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NAME:
say
CALLING SEQUENCE:
PRO say, str, silent=silent, threshold=threshold
INCLUDE:
@compile_opt.pro
CALLS: ***
InitVar, who_am_i
CALLED BY:
InsituTimeSeries, PlotEarthSkymap [1], forecast, forecast_env, forecast_ftp
getipssources, getnagoyasources, getootyasources, is_running, mk_flick
vu_correlate, vu_earthskymap, vu_get_page, vu_getdata, vu_gettime, vu_header
vu_image, vu_insitu_raw, vu_lineofsight, vu_localskymap, vu_mean, vu_movie
vu_nagoyasourcemap, vu_new_time, vu_planarcut, vu_prefix, vu_quick_movie
vu_radialcut, vu_read, vu_remoteview, vu_select, vu_solardisk, vu_spherecut
vu_syncgrid, vu_synopticmap, vu_timeseries, vu_update_hours, vu_update_marker
vu_vox_sequence, vu_vox_write, vu_write
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NAME:
scalarproduct
PURPOSE:
Calculate scalar product for two vectors
CATEGORY:
gen/idl/toolbox/math
CALLING SEQUENCE:
FUNCTION scalarproduct, r1, r2, $
cylin = cylin , $
sphere = sphere , $
rect = rect , $
degrees = degrees , $
angle = angle
INPUTS:
r1 arrays[3,*]; type: int or float
r1 arrays[3,*]; type: int or float
vectors for which the product is to be taken.
the first dimension identifies the three coordinates: Cartesian (default),
cylindrical or spherical.
OPTIONAL INPUT PARAMETERS:
/angle if set then information about the angle between the two vectors is returned:
i.e. cos(angle) = |r1.r2|/|r1||r2|
/cylin, /sphere, /rect
indicates whether input vectors are in cylindrical, spherical or rectangular
coordinates. If none is set then rectangular is assumed.
/degrees if set, and spherical or cylindrical coordinates are used, then the angles
are assumed to be in degrees (default: radians)
OUTPUTS:
result array[*] same type as input
scalar products or angle information are returned as array[n]
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CV_COORD, InitVar, SyncArgs, SyncDims
CALLED BY:
RotationMeasure, haystack_2006, jpl_phase
PROCEDURE:
> The arrays r1 and r2 do not necessarily have the same dimensions, i.e.
if r1 is an array[3,n] and r2 is an array[3] then r2 is interpreted as an array[3,n]
with all n vectors the same (SyncArgs is used to synchronize the array dimensions).
> Arrays r1 and r2 can have more than two dimensions, i.e. if r1 and r2 are both
arrays[3,n,m] then the scalar products will be returned as array[n,m]
MODIFICATION HISTORY:
AUG-1999, Paul Hick (UCSD/CASS)
NOV-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Extracted from vectorproduct procedure.
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NAME:
set_page
PURPOSE:
Setup procedure for controlling output to plot device or graphics file
The output procedure is completed by a call to get_page
CALLING SEQUENCE:
PRO set_page, $
eps = eps , $
gif = gif , $
bmp = bmp , $
png = png , $
xysize = xysize , $
scale_factor= scale_factor, $
aspect = aspect , $
fullsize = fullsize , $
winaspect = winaspect , $
landscape = landscape , $
portrait = portrait , $
silent = silent , $
setup_only = setup_only, $
file = file , $
zbuffer = zbuffer , $
printer = printer , $
display = display , $
ctable = ctable , $
old_device = old_device, $
new = new , $
bigsize = bigsize , $
xoff = xoff , $
yoff = yoff , $
smallsize = smallsize , $
notwin = notwin , $
font = font , $
flip_bw = flip_bw , $
flip_ct = flip_ct
OPTIONAL INPUT PARAMETERS:
The following keywords control the size and orientation of the output page.
They only affect EPS, PS, HP or PRINTER devices (as keywords in the 'device'
call). EPS is selected with the /eps keyword. PS, HP and PRINTER is used
depending on !ThePrinter (initialized during startup).
/landscape plot in landscape mode
/portrait plot in portrait mode
If neither of these is set then /landscape is used
Only used to set up PS, EPS or default PRINTER.
xysize=xysize scalar, or array[2]; type: float
horizontal and vertical size of page (in cm for printer,
in pixel for display and z-buffer). If a scalar is
specified it is assumed to be the horizontal size
/fullsize overrides 'xysize' keyword. For the printer xysize is set
to the full page size, for other devices [!d.x_size,
!d.ysize] is used
If xysize is not specified then default values are selected
depending on whether /landscape of /portrait is used.
If specified then aspect (or /winaspect) overrides either
xsize of ysize to establish the proper aspect.
aspect=aspect scalar; type: float
aspect ratio (=ratio vertical/horizontal size
/winaspect same as: aspect = !d.y_size/!d.x_size
i.e. the aspect ratio of the active window is used
/silent suppresses informational messages
/setup_only the command 'set_page, /setup, /silent' is used during
IDL_startup to set up the default printer. The plot
device is NOT changed, and !ThePlotFile is NOT set (i.e.
is set to the null string)
/eps sets the plot device to PS and opens an EPS file
!ThePlotFile is set to IDL.EPS or 'File'
/gif sets the plot device to !TheTerminal
!ThePlotFile is set to IDL.GIF or 'File'
/png sets the plot device to !TheTerminal
!ThePlotFile is set to IDL.PNG or 'File'
/bmp sets the plot device to !TheTerminal
!ThePlotFile is set to IDL.BMP or 'File'
/zbuffer NOT WORKING YET
OUTPUTS:
xysize=xysize array[2]; type: integer
[!d.x_size, !d.y_size] on return
old_device=old_device
scalar; type: string
original graphics device (i.e. value of !d.name when
this procedure is called)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, GetFileSpec, InitVar, IsType, LOADCT, destroyvar, do_file, flip_colors, twin
CALLED BY:
GetColors [2], GetColors [3], IDL_postop_linux, IDL_postop_vms, IDL_postop_win
PlotEarthSkymap [2], PlotEarthSkymap [3], PlotEarthSkymap [4], allsky [1]
allsky [2], allsky [3], allsky_f, ark_duty_cycle, coriolis_map, dusan_earth
even_light_corrections, even_light_photometry, even_light_registration
fileset_sizes, grdout, ips_exit, ipv6_packets, ipv6_traffic, krill_request_bars
krill_request_stats, miscfig, packet_size_graphs, packet_size_update
qset_page_submit, show_wso, smei_frm_summary, smei_hdr_plot, smei_sky
smei_star_show, smei_zldsky, smeifig, telescope_sizes, thomsonfig, vu_coronagraph
vu_earthskymap, vu_elotime, vu_insitu, vu_insitu_persist, vu_planarcut
vu_solardisk, vu_spherecut, vu_synopticmap, vu_thomson_antifish
vu_thomson_hammer
SEE ALSO:
qset_page
PROCEDURE:
Pretty darn ugly.
The plot device is set to !ThePrinter, or PS (if /eps is set) or
!TheTerminal (if /gif or /bmp are set).
!ThePlotFile is always set. Unless argument 'File' is used
the file name will be IDL.EPS, IDL.GIF or IDL.BMP (if /eps, /gif or /bmp are
set) or IDL.HP, IDL.PS or IDL.PRINTER (depending on the value of
!ThePrinter). Note that in the last case (IDL.PRINTER) no plot file is used
since the output goes directly to the printer.
For HP and PS the graphics output is collected in the output file, which is
then send to the printer using get_page
MODIFICATION HISTORY:
MAR-1995, Paul Hick (UCSD/CASS)
MAR-1998, Paul Hick (UCSD/CASS); added PRINTER device
MAR-2000, Paul Hick (UCSD/CASS)
added /gif and /bmp keywords, updated documentation
???-2002, Paul Hick (UCSD/CASS)
added /png keyword
AUG-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
added /color to device call for EPS
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NAME:
SetFileSpec
PURPOSE:
Split file names into file components.
Optionally parse the file names.
CATEGORY:
gen/idl/toolbox/files
CALLING SEQUENCE:
PRO SetFileSpec, FileSpec, FileParts, $
parse = Parse , $
nosave = NoSave, $
strict = strict, $
status = Status
INPUTS:
FileSpec string array or scalar, containing file names
(read-only)
OPTIONAL INPUT PARAMETERS:
/parse if set, the file names are parsed.
parsing is successful if
- The directory exists
- There is write access to the directory
- The file name is valid (the file may or may not exist)
(if no file name is specified this step is skipped)
If the parsing is succesful, missing file parts will
be added to the FileParts array; if not all parts are
set to the null string.
/nosave by default, the FileParts array returned as ouput
is saved internally in a common block (which can
be accessed with GetFileSpec and PutFileSpec).
if nosave is set, the internal data are not overwritten.
/strict by default the file type is the part of the
filename trailing the last dot, i.e. if the file name
is file.txt.gz, the file type is .gz.
If /strict is set the type becomes the part following
the first dot, i.e. the type is .txt.gz.
OUTPUTS:
FileParts string array with one dimension more than
FileSpec; the extra first dimension has 6 elements,
containing node, device, directory, name, type, version
!!! the FileParts argument is sometimes useful in
combination with the /nosave keyword. Preferably this
argument should not be used; instead use GetFileSpec
and PutFileSpec to manipulate the same information.
OPTIONAL OUTPUT PARAMETERS:
status=Status long integer array with same dimensions as FileSpec.
If keyword Parse set:
0 : indicates that parsing failed
1 : indicates that parsing was succesfull
If keyword Parse not set, all values are set to 1
CALLS: ***
CheckDir, FILEPATH, FindAllFiles, InitVar, IsType, SyncDims, os_separator, strposn
INCLUDE:
@compile_opt.pro ; On error, return to caller
@filespec_common.pro ; Common block with arrays File and Parts
CALLED BY:
FindAllFiles, FindAllSubDirs, GetFileSpec, PlotEarthSkymap [2], PutFileSpec
allsky [1], allsky [2], allsky [3], allsky_f, aurora, badpix, bin_read, bin_write, clean
cvgrd, cvgrd_skymap, do_file, findfile_fix, forecast_ftp, get_page, gunzip_file
makediff, makemovie [1], makemovie [2], mk_flick, nso_fe_read, qImage, qImage_Pick
qImage_cw_SmeiMask, qRemoteView_Pick, qSave2File_Save, qView, qView_FileFilter
qView_PickFiles, qView_Save2File, qView_TMO_tracksky, qset_page_pick, smei_buf
smei_frm_update, smei_www_skymaps, test_td, tolowcase, usno_body, vu_check
vu_coronagraph, vu_earthskymap, vu_extract, vu_get_page, vu_getdata, vu_header
vu_image, vu_insitu, vu_lineofsight, vu_movie, vu_quick_movie, vu_remoteview
vu_vox_write, www_help_crosslinks, www_help_files, www_help_get_header
www_help_get_info
SIDE EFFECTS:
Internal data are maintained internally (a copy of FileParts)
RESTRICTIONS:
FileSpec containing relative directory specifications
(e.g. [], [-] on VMS, or . and .. on Win32 and Unix), cause
problems for GetFileSpec. If these are present, then /parse
should be used to remove them.
PROCEDURE:
> Parsing: the existence check for the directory is done using CheckDir.
The fully-parsed directory returned by CheckDir is used, so the parse
keyword can be used to expand environment variables, e.g.
SetFileSpec, '$dat/tmo/*.nic', /parse
print, GetFileSpec()
would print (provided the directory exists):
/big/oftp/dat/tmo/*.nic
> If a wildcard is specified in the file name then only the directory
is parsed.
> For an existing file the full file name is obtained using FindAllFiles.
If the file does not exist, an attempt is made to open
the file with OPENW to establish that the syntax is valid;
FindAllFiles is used to obtain the full file name before closing and
deleting the file again.
> The filenames are split up into parts by a series of strposn calls
> FileSpec='' (null string) is interpreted as the current working directory,
and will always return status=1.
MODIFICATION HISTORY:
DEC-1997, Paul Hick (UCSD/CASS)
FEB-2002, Paul Hick (UCSD/CASS)
Remove bug which caused problems when multidimensional arrays
of filenames were processed.
JAN-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
If a wildcard (*) is specified in the filename part then only the
directory is checked when the /parse keyword is set.
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NAME:
SetRange
PURPOSE:
Set range of values, checking against a default range
CATEGORY:
Tricks
CALLING SEQUENCE:
new = SetRange(default, range [, /lower_limit])
INPUTS:
default array[2]; type: any
upper and lower limits on allowed values
OPTIONAL INPUT PARAMETERS:
range scalar or array[2]
range to be checked against 'default'
/lower_limit if set then a scalar 'range' is interpreted as
a lower limit (default is upper limit)
OUTPUTS:
new array[2]
updated range of values
if 'range' undefined then 'new' is set to 'default'
if 'range' is scalar then new = [range,default[1]] is
returned (/lower_limit is set), or new = [default[0],range[1]]
is returned (/lower_limit not set
Always 'range' is constrained to stay inside the limits set by 'default'
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar
CALLED BY:
RemoteView_rgbo
PROCEDURE:
Trivial
MODIFICATION HISTORY:
JUN-2000, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
setup3d
PURPOSE:
Sets up scaling (!x.s, !y.s, !z.s) and transformation matrix (!p.t)
CATEGORY:
CALLING SEQUENCE:
setup3d, d0, d1, n0, n1 [, /rotate, /oblique]
setup3d, d0, d1, n0, n1 [, rotate=[[a,b,c],[d,e,f]], oblique=[p,q] ]
INPUTS:
d0 scalar or array[3]; default: -1.5*[1,1,1]
d1 scalar or array[3]; default: 1.5*[1,1,1]
begin and end of data coordinate range
scalars are interpreted as scalar*[1,1,1]
n0 scalar or array[3]; default: 0.0*[1,1,1]
n1 scalar or array[3]; default: 1.0*[1,1,1]
begin and end of normal coordinate range
scalars are interpreted as scalar*[1,1,1]
!x.s, !y.s and !z.s are set up to map data ranges [d0,d1] to normal ranges [n0,n1]
OPTIONAL INPUT PARAMETERS:
rotate=rotate
array[3,n] or array[3*n]; type: float
The special form /rotate is identical to rotate=[ [ 0.,-20.,0.], [20., 0. ,0.] ]
Set of rotations to be set up in !p.t matrix
rotations are processed left to right; rotate[0,*], rotate[1,*] and rotate[2,*]
are rotations around x,y and z-axis respectively
oblique=oblique
array[2]; type: float
The special form /oblique is identical to oblique=[.4,-125]
Parameters for an oblique projection
/xyplane Puts x-y plane in plane of screen
/yzplane Pust y-z plane in plane of screen
/xzplane Puts x-z plane in plane of screen
OUTPUTS:
Sets !x.s, !y.s, !z.s and !p.t
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
T3D, t3d_oblique
CALLED BY:
PlotPlanarCut, PlotSolarDisk, RemoteView_PlotVertices, brachistochrone
cvplot_figures, even_light_figures, losgeometry, miscfig, projfig, qimage_fig
qvu_draw, smeifig, ss_map, thomsonfig, tomography_sp
RESTRICTIONS:
PROCEDURE:
!p.t is first reset. Then clockwise rotations around y and z-axis over 90 degrees are
executed to point the x-axis perpendicular to the screen, the y-axis pointing right and the
z-axis pointing up in the plane of the screen.
After that the rotations supplied as keywords are applied, followed by the oblique projection.
MODIFICATION HISTORY:
AUG-1999, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
sgp4_eph
PURPOSE:
Get location of Coriolis spacecraft in ECI coordinates
CATEGORY:
gen/idl/ephem
CALLING SEQUENCE:
FUNCTION sgp4_eph, tt_obs, body_, $
km = km , $
location= location , $
source = source , $
precess = precess
INPUTS:
tt_obs array[n]; type: time structure
UT time
OPTIONAL INPUTS:
body_ scalar; type: string; default: 'sat27640'
spacecraft designation
The default sat27640 is Coriolis.
km=km if set, return distance in km instead of AU
source=source scalar; type: string; default: who_am_i(/dir)/sgp
directory where TLE file is located (by default the
subdir sgp of the dir where this file is located.
/precess precess position and velocity vector to J2000 coordinates
(used by big_eph)
OUTPUTS:
rr[6,n] location and velocity
Coordinates are valid for the current epoch and equinox,
unless /precess is set (see PROCEDURE).
If /location is set only r[0:2,n] is returned.
If the required file with TLEs is not found
then the output vector contains NaNs.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, BadValue, CvPrecess, FILEPATH, InitVar, SuperArray, TimeFixYear
TimeLimits, TimeOp, TimeSet, TimeUnit, hide_env, sgp_alias, txt_read, who_am_i
CALLED BY:
big_eph, coriolis_map, sgp4_orbit_axis, smei_frm_cvhdr, smei_frm_where
smei_sgp4_orbits, smei_sgp4_quat
PROCEDURE:
The file with orbital elements is 'body.txt' i.e. sat27640.txt for
Coriolis. The file is looked for in the subdirectory sgp of the
directory where this source code is located. Used keyword 'source'
to point to another subdirectory.
Orbital elements can be retrieved from www.space-track.org
Excerpt from http://celestrak.com/columns/v02n01/:
"As it turns out, the NORAD SGP4 orbital model takes the standard
two-line orbital element set and the time and produces an ECI
position and velocity for the satellite. In particular, it puts it
in an ECI frame relative to the "true equator and mean equinox of
the epoch" of the element set. This specific distinction is
necessary because the direction of the Earth's true rotation axis
(the North Pole) wanders slowly over time, as does the true direction
of the vernal equinox. Since observations of satellites are made
by stations fixed to the Earth's surface, the elements generated
will be referenced relative to the true equator. However, since the
direction of vernal equinox is not tied to the Earth's surface, but
rather to the Earth's orientation in space, an approximation must
be made of its true direction. The approximation made in this case is
to account for the precession of the vernal equinox but to ignore the
nutation (nodding) of the Earth's obliquity (the angle between the
equatorial plane and the ecliptic)."
MODIFICATION HISTORY:
MAR-2005, Paul Hick (UCSD/CASS)
SEP-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Reduced memory requirements by extracting TLE bracketing the
input time range tt_obs
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NAME:
sgp4_orbit_axis
PURPOSE:
Gets ECI coordinates for Coriolis orbital axis (i.e. the normal
to the orbital plane, close to the sunward direction).
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
FUNCTION sgp4_orbit_axis, tt, $
degrees = degrees , $
to_sphere = to_sphere , $
precess = precess
INPUTS:
tt array; type: time structure
OPTIONAL INPUT PARAMETERS:
/to_sphere if set return spherical (RA,dec) coordinates
/degrees if set, angles are in degrees (default: radians)
/precess (passed to sgp4_eph)
precess to J2000 coordinates
OUTPUTS:
rr array[3,*]; type: double
coordinates of a unit vector along the normal
to the SMEI orbital plane in rectangular (/to_sphere
NOT set) or spherical (RA,dec) coordinates
(/to_sphere) SET.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, CV_COORD, InitVar, IsTime, TimeOp, TimeSet, TimeSystem, TimeUnit, gridgen
sgp4_eph, vectorproduct
CALLED BY:
cv, smei_normal, smei_sgp4_orbits, smei_zld_weekly
PROCEDURE:
Viewed from the Sun SMEI circles the Earth close to the terminator
in anti-clockwise direction (going north towards the east (dusk
terminator) and south in the west (dawn terminator).
The normal, defined as the cross produce of position and velocity
vector points towards the Sun.
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS)
MAR-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added more documentation.
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NAME:
sgp4_orbit_period
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS: ***
BadValue, SyncArgs, sgp4_tle
CALLED BY:
smei_sgp4_orbits
PROCEDURE:
MODIFICATION HISTORY:
JUNE-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
sgp4_tle
PURPOSE:
Extract orbital elements covering bracketing tt_obs from
tle data base file
CATEGORY:
gen/idl/ephem
CALLING SEQUENCE:
status = sgp4_tle(tt_obs,body_,source=source,tle=tle,tt_tle=tt_tle)
INPUTS:
tt_obs array[n]; type: time structure
UT time
OPTIONAL INPUTS:
body_ scalar; type: string; default: 'sat27640'
spacecraft designation
The default sat27640 is Coriolis.
source=source scalar; type: string; default: who_am_i(/dir)/sgp
directory where TLE file is located (by default the
subdir sgp of the dir where this file is located.
OUTPUTS:
status scalar; type: integer
0: the ephemeris find is not found or there
is a read error. In this case tle and tt_tle
won't exist
1: tles found
tle=tle array[2,ntle]; type: string
tle (each tle consists of two records)
the tles will bracket the input time period tt_obs
tt_tle array[ntle]; type: time structure
times extracted from tle records
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, FILEPATH, InitVar, SuperArray, TimeFixYear, TimeLimits, TimeOp, TimeSet
TimeUnit, hide_env, sgp_alias, txt_read, who_am_i
CALLED BY:
sgp4_orbit_period
PROCEDURE:
The file with orbital elements is 'body.txt' i.e. sat27640.txt for
Coriolis. The file is looked for in the subdirectory sgp of the
directory where this source code is located. Used keyword 'source'
to point to another subdirectory.
Orbital elements can be retrieved from www.space-track.org
MODIFICATION HISTORY:
DEC-2005, Paul Hick (UCSD/CASS)
Extracted from sgp4_eph
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NAME:
sgp_alias
PURPOSE:
Translates aliases for satellite names to their sgp names
CATEGORY:
gen/idl/ephem
CALLING SEQUENCE:
name = alias_sgp(body)
INPUTS:
body array: type: string
alias for satellite name
OUTPUTS:
name array: type: string
sgp name for satellite
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
big_body, big_eph, sgp4_eph, sgp4_tle
PROCEDURE:
Currently only aliases 'coriolis','windsat' and 'smei' are
converted to sgp name 'sat2740'
MODIFICATION HISTORY:
JUN-2006, Paul Hick (UCSD/CASS)
SEP-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Bugfix? Unidentified bodies would be returned in lowercase.
Now they remain untouched.
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NAME:
sgp_body
PURPOSE:
Get list of bodies for which SGP ephemerides are available
CATEGORY:
smei/gen/idl/ephem
CALLING SEQUENCE:
sgp_nams = sgp_body([body, files=files, numbers=numbers, count=count])
OPTIONAL INPUT PARAMETERS:
body scalar or array; type: integer or string
integer: list of body numbers
string : list of body names
only valid entries on this list are processed
If not specified then all bodies are processed
OUTPUTS:
names array[count]; type: string
list of body names for which ephemeris files
are available; if none exist (count=0) then names=''
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
# requested bodies for which ephemeris files are present
i.e. # elements in input 'body' with invalid entries removed
file=file array[count]; type: string
file names of the ephemeris files; null-string if count=0
number=number array[count]; type: integer
body numbers; -1 if count=0
index=index array[count]; type: integer
index numbers between 0, and total_count-1; -1 if count=0
total_count=total_count
scalar; type: integer
total # bodies for which ephemeris files are present
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, GetFileSpec, IsType, hide_env, where_common, who_am_i
CALLED BY:
RemoteView_BodyLoc, big_body, big_eph
PROCEDURE:
> Currently only 9P/Tempel (comet Tempel 1 around 'deep impact' time) is available
> The SGP files are searched for in the subdirectory 'sgp' of the directory
where this procedure is located.
MODIFICATION HISTORY:
JUL-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Based on usno_body()
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NAME:
show_wso
PURPOSE:
CALLS: ***
FILEPATH, InitVar, PlotSynopticMap, SuperArray, WhatIs, get_page, gridgen, set_page
view, wso_read
MODIFICATION HISTORY:
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NAME:
Sky_ColorView
PURPOSE:
Calculates image of sky from 3D density matrix for a given viewer location
and viewing direction.
CATEGORY:
Image construction
CALLING SEQUENCE:
Sky_ColorView, F3D, R3D, $
rotation = Rotation, $
states = States, $
dostates = DoStates, $
/heliographic, $
/degrees, $
/cartesian, $
eqdistance = EqDistance, $
eqangle = EqAngle, $
eqarea = EqArea
INPUTS:
F3D array[N,L,M]; type: float
3D data array
Cartesian: N=L=M; cube of data with Sun in the center
Spherical: N=# longitudes covering 360 deg
L=# latitudes covering -90,90 deg
M=# heliocentric distances covering [R3D[0],R3D[1]]
R3D scalar, array[2]; type: float; default: [0,1.5]
A scalar is interpreted as [0,R3D]
Determines size of volume covered by F3D (in AU)
Cartesian: R3D[1] is half the size of the cube covered by F3D
(R3D[0] is not used)
Spherical: heliocentric distance range covered by F3D
rotation=Rotation scalar; type: float
The density matrix is assumed to reflect the heliospheric density
for a whole Carrington rotation (360 degree in heliographic longitude)
starting at the value 'rotation'.
The value of Rotation is used in three ways:
1. the fractional part is used to set the starting heliographic longitude,
e.g. 1884.0 starts at 0 degrees; 1884.25 at 270 degrees.
2. if the image time in the States array is set to !values.f_nan, it is
assumed to be the time at which the longitude corresponding to 'Rotation'
crossed the central meridian (i.e. it is set to CarringtonT(Rotation))
3. Rotation is passed to ReadSynopticMap to read in a map to be wrapped around
the surface of the Sun
states = States float array[8,*]
Each state is processed separately, and results in an image
All angles are in radians unless /degrees is set.
State[0] time of image in days since 2000 Jan 1.5 (mjd2).
if equal to !values.f_nan it is set to the start of the
rotation specified in the rotation keyword
State[1:3] position of viewer (longitude, latitude, heliocentric distance)
By default, ecliptic coordinates are assumed.
Set /heliographic keyword to input heliographic coordinates.
The heliocentric distance is in AU.
State[4:5] viewing direction corresponding to center of image
(longitude, latitude) in the same coordinate system as used for
the viewer location, but with the viewer in the origin.
State[6] Angular width of rectangular field of view
State[7] ??? Tilt angle of field of view. Zero tilt means that the horizontal
direction in the image is parallel to the ecliptic or solar
equator (depending on the setting of keyword /heliographic)
Tilt angle increases counterclockwise.
OPTIONAL INPUT PARAMETERS:
dostates = DoStates
scalar, or array[2]; type: integer; default: all states
defines subset of States array to be processed in terms of
index to States array (0,..,n_elements(States)-1)
if scalar: process states from DoStates to n_elements(States)-1
if array : process states from DoStates[0] to DoStates[1]
/heliographic if set, angles specified in the state array are assumed to
in heliographic coordinates (default: ecliptic coordinates)
/degrees if set, angles used in viewer location and viewing direction
are assumed to be in degrees (default: radians)
/cartesian if set, the array F3D is assumed to refer to
a Cartesian coordinate system with linear dimensions [N,L,M].
x-coord = n, n=0,N-1
y-coord = l, l=0,L-1
z-coord = m, m=0,M-1
/stereo
stereo=[Angle,Distance]
/stereo if set, stereo pairs are produced using default
settings for stereo angle (6 degrees) and
distance (Sun-viewer distance)
stereo=[Angle, Distance]
if specified as a two-element array, the first
element is used as stereo angle, the second as
stereo distance. If the distance is set to zero
then the viewer-origin distance Loc[2,*] is used.
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
states = States
array[8,*]; type: float or double
times set to 'bad value' !values.f_nan will be filled in using
the start time of 'rotation'
CALLS:
CMEDensity, CarringtonT, CubeFrame, CvSky, EarthOrbit, FILEPATH, GlobePosition
GlobeSize, ReadSynopticMap, SkyDisplay, SkyFOVTilt, SkyGrid, SkyStereoStates
Sky_BodyColors, TimeBuild, TimeGet, TimeSet, TimeString, UTSystem, VertexMap
VertexSphere, ZEclipticPlane, skycolors
CALLED BY:
SkyForecast, test_td
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
NOV-1999, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added nGrid keyword to allow specification of viewing space dimensions
for each of the three dimensions separately.
Added rInner keyword to allow specification of inner boundary for a
density matrix specified in spherical coordinates (was always set to zero before).
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NAME:
Sky_ColorView
PURPOSE:
Calculates image of sky from 3D density matrix for a given viewer location
and viewing direction.
CATEGORY:
Image construction
CALLING SEQUENCE:
Sky_ColorView, F3D, R3D, $
rotation = Rotation, $
states = States, $
dostates = DoStates, $
/heliographic, $
/degrees, $
/cartesian, $
eqdistance = EqDistance, $
eqangle = EqAngle, $
eqarea = EqArea
INPUTS:
F3D array[N,L,M]; type: float
3D data array
Cartesian: N=L=M; cube of data with Sun in the center
Spherical: N=# longitudes covering 360 deg
L=# latitudes covering -90,90 deg
M=# heliocentric distances covering [R3D[0],R3D[1]]
R3D scalar, array[2]; type: float; default: [0,1.5]
A scalar is interpreted as [0,R3D]
Determines size of volume covered by F3D (in AU)
Cartesian: R3D[1] is half the size of the cube covered by F3D
(R3D[0] is not used)
Spherical: heliocentric distance range covered by F3D
rotation=Rotation scalar; type: float
The density matrix is assumed to reflect the heliospheric density
for a whole Carrington rotation (360 degree in heliographic longitude)
starting at the value 'rotation'.
The value of Rotation is used in three ways:
1. the fractional part is used to set the starting heliographic longitude,
e.g. 1884.0 starts at 0 degrees; 1884.25 at 270 degrees.
2. if the image time in the States array is set to !values.f_nan, it is
assumed to be the time at which the longitude corresponding to 'Rotation'
crossed the central meridian (i.e. it is set to CarringtonT(Rotation))
3. Rotation is passed to ReadSynopticMap to read in a map to be wrapped around
the surface of the Sun
states = States float array[8,*]
Each state is processed separately, and results in an image
All angles are in radians unless /degrees is set.
State[0] time of image in days since 2000 Jan 1.5 (mjd2).
if equal to !values.f_nan it is set to the start of the
rotation specified in the rotation keyword
State[1:3] position of viewer (longitude, latitude, heliocentric distance)
By default, ecliptic coordinates are assumed.
Set /heliographic keyword to input heliographic coordinates.
The heliocentric distance is in AU.
State[4:5] viewing direction corresponding to center of image
(longitude, latitude) in the same coordinate system as used for
the viewer location, but with the viewer in the origin.
State[6] Angular width of rectangular field of view
State[7] ??? Tilt angle of field of view. Zero tilt means that the horizontal
direction in the image is parallel to the ecliptic or solar
equator (depending on the setting of keyword /heliographic)
Tilt angle increases counterclockwise.
OPTIONAL INPUT PARAMETERS:
dostates = DoStates
scalar, or array[2]; type: integer; default: all states
defines subset of States array to be processed in terms of
index to States array (0,..,n_elements(States)-1)
if scalar: process states from DoStates to n_elements(States)-1
if array : process states from DoStates[0] to DoStates[1]
/heliographic if set, angles specified in the state array are assumed to
in heliographic coordinates (default: ecliptic coordinates)
/degrees if set, angles used in viewer location and viewing direction
are assumed to be in degrees (default: radians)
/cartesian if set, the array F3D is assumed to refer to
a Cartesian coordinate system with linear dimensions [N,L,M].
x-coord = n, n=0,N-1
y-coord = l, l=0,L-1
z-coord = m, m=0,M-1
/stereo
stereo=[Angle,Distance]
/stereo if set, stereo pairs are produced using default
settings for stereo angle (6 degrees) and
distance (Sun-viewer distance)
stereo=[Angle, Distance]
if specified as a two-element array, the first
element is used as stereo angle, the second as
stereo distance. If the distance is set to zero
then the viewer-origin distance Loc[2,*] is used.
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
states = States
array[8,*]; type: float or double
times set to 'bad value' !values.f_nan will be filled in using
the start time of 'rotation'
CALLS:
CMEDensity, CarringtonT, CubeFrame, CvSky, EarthOrbit, FILEPATH, GlobePosition
GlobeSize, ReadSynopticMap, SkyDisplay, SkyFOVTilt, SkyGrid, SkyStereoStates
Sky_BodyColors, TimeBuild, TimeGet, TimeSet, TimeString, UTSystem, VertexMap
VertexSphere, ZEclipticPlane, skycolors
CALLED BY:
SkyForecast, test_td
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
NOV-1999, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added nGrid keyword to allow specification of viewing space dimensions
for each of the three dimensions separately.
Added rInner keyword to allow specification of inner boundary for a
density matrix specified in spherical coordinates (was always set to zero before).
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NAME:
skycolors
CALLED BY:
Sky_ColorView [1], Sky_ColorView [2]
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NAME:
skyd_cat
PURPOSE:
Creates the initial orbit catalogues needed by the
SMEI skyd daemon.
CALLING SEQUENCE:
PRO skyd_cat, range, $
camera = camera , $
mode = mode , $
source = source , $
dig = dig , $
destination = destination,$
to_smeidb = to_smeidb , $
full_count = full_count, $
keepskip = keepskip , $
smoothdark = smoothdark, $
reverse_order= reverse_order
INPUTS:
range array[2]; type: time structure
time range for which to produce a catalogue.
If omitted the entire mission time is used.
OPTIONAL INPUTS:
camera=camera array or scalar; type: integer; default: [1,2,3]
SMEI cameras to be processed
mode=mode array or scaler; type: integer; default: [0,1,2]
modes to be processed
source=source scalar or array; type: string; default: SMEISKY?
list of directories with skymaps.
The default SMEISKY? is translated to all
directories assigned to env vars $SMEISKYn
/dig If /dig is set then the skymaps should be located
in subdirectories c1,c2,c3.
IF source=SMEISKY? then always /dig is assumed
destination=destination
scalar; type: string; default: $TUB
destination directory for the skyd catalogues
/to_smeidb forces destination=$SSWDB_SMEI/cat/list
(see PROCEDURE)
/full_count by default the sky catalogues are based on the frame
counts for frames satisfying the default conditions
used by smeidb_sky for frame selection (not a "just-bad"
frame, good quaternion, shutter open and base OK;
this is the second set of 4 columns in
the smei_frm_orb_m<mode>.txt files).
If full_count is set then the unrestricted counts for
all frames per orbit (the first set of 4 columns in the
smei_frm_orb_m<mode>.txt files) is used.
/keepskip by default, orbits marked 'skip' are not written
into the catalogue files. Set /keepskip to override.
/smoothdark create catalogues for the skymaps based on smoothed
dark currents (cam 3 only).
(By default, skyd_cat looks in the c1,c2,c3 directories
of $SMEISKY0/sky. Setting this keyword forces it to
look in the c3s directory).
/reverse_order by default, catalogues are written in reverse
chronological order (i.e. the most recent data get
processed first). To reverse this, and process data
chronologically set this keyword.
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FILEPATH, FXPAR, FindAllFiles, HEADFITS, InitVar, IsTime, IsType, TimeGet
TimeOp, TimeSet, TimeUnit, boost, destroyvar, flt_string, hide_env, smei_filename
smei_filepath, timeposn, txt_read
CALLED BY:
smei_mksky
PROCEDURE:
The skyd catalogues are derived from the files
smei_frm_orb_m0.txt, smei_frm_orb_m1.txt and smei_frm_orb_m2.txt
in directory $SSWDB_SMEI/cat/list. These files list the numbers
of frames for each camera in each of three modes. They are
created and maintained by the IDL procedure
smei_orbit_stats (through a daily cronjob).
The skyd_catalogues will have names skyd_c<cam>m<mode>.txt
where <cam> is the camera id (1,2,3) and <mode> the mode id
<0,1,2>. The files are written to directory 'destination'.
If /to_smeidb is set the destination directory is the same
as for the smei_frm_orb_m*.txt files ($SSWDB_SMEI/cat/list).
These catalogues are accessed by the Python script
skyd_orbit (which in turn is used by the SMEI
skyd daemon skyd_wait).
MODIFICATION HISTORY:
DEC-2005, Paul Hick (UCSD/CASS)
MAR-2007, Paul Hick (UCSD/CASS)
Added keyword /full_count
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword /reverse_order
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NAME:
skyd_pass2make
PURPOSE:
Runs through SKYD orbit catalogues to replace
orbits marked "pass" back to "make"
CATEGORY:
skyd
CALLING SEQUENCE:
PRO skyd_pass2make
INPUTS:
OUTPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
destroyvar, txt_read
PROCEDURE:
MODIFICATION HISTORY:
DEC-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
skyd_reverse
CALLING SEQUENCE:
PRO skyd_reverse, f
INCLUDE:
@compile_opt.pro
CALLS: ***
InitVar, txt_read
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NAME:
skyd_version
PURPOSE:
Creates catalogue with software version numbers used
to create skymap database
CALLING SEQUENCE:
PRO skyd_version, $
camera = camera , $
destination = destination,$
to_smeidb = to_smeidb
OPTIONAL INPUTS:
camera=camera array or scalar; type: integer; default: [1,2,3]
SMEI cameras to be processed
destination=destination
scalar; type: string; default: $TUB
destination directory for the skyd_equ catalogues
/to_smeidb forces destination=$SSWDB_SMEI/cat/list
(see PROCEDURE)
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FILEPATH, FXPAR, HEADFITS, InitVar, SFLOAT, TimeGet, TimeSet, TimeUnit, hide_env
smei_filepath, smei_getfile, smei_star_readpnt
PROCEDURE:
MODIFICATION HISTORY:
JUN-2008, Paul Hick (UCSD/CASS)
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NAME:
SkyDriveIn
CALLING SEQUENCE:
pro SkyDriveIn, distance, $
rotation = Rotation, $ ; Defines 3D data set
resolution = Resolution, $
cube = Cube, $
drawecliptic= DrawEcliptic, $
meshecliptic= MeshEcliptic, $
tiff8 = Tiff8, $
tiff24 = Tiff24, $
bmp8 = Bmp8, $
bmp24 = Bmp24, $
interleave = Interleave, $
fov = fov, $
firststate = FirstState, $
fire = Fire, $
helios = Helios, $
smex = Smex, $ ; Single s/c east of Earth
twinsc = Twinsc, $ ; Two s/c on either side of Earth
cartesian = Cartesian, $
eqdistance = eqdistance, $
eqangle = eqangle, $
eqarea = eqarea, $
cme = cme, $
noplot = noplot, $
stereo = stereo, $
xsize = xsize, $
ysize = ysize
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, NewcombSun, SKYIMAGE, TimeGet, TimeSet, flt_read
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NAME:
SkyForecast
CALLING SEQUENCE:
pro SkyForecast, file, $
rotation = Rotation, $ ; Defines 3D data set
ngrid = ngrid, $
cube = Cube, $
drawecliptic= DrawEcliptic, $
meshecliptic= MeshEcliptic, $
tiff8 = Tiff8, $
tiff24 = Tiff24, $
bmp8 = Bmp8, $
bmp24 = Bmp24, $
interleave = Interleave, $
fov = fov, $
firststate = FirstState, $
fire = Fire, $
helios = Helios, $
smex = Smex, $ ; Single s/c east of Earth
twinsc = Twinsc, $ ; Two s/c on either side of Earth
eqdistance = eqdistance, $
eqangle = eqangle, $
eqarea = eqarea, $
cme = cme, $
noplot = noplot, $
stereo = stereo, $
xysize = xysize
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CARRINGTONT, FILEPATH, MEAN, Sky_ColorView [1], Sky_ColorView [2], TimeGet, TimeOp
TimeSet, vu_read
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NAME:
smei_base_testcase
PURPOSE:
Runs test case for smei_base program and validates results
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_base_testcase, make=make, db=db, keep=keep, $
source=source, digsource=digsource
OPTIONAL INPUT PARAMETERS:
/make if set, the testcase results are regenerated
source=source passed to smei_base
/digsource passed to smei_base
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, FindAllFiles, GetFileSpec, InitVar, IsType, TimeGet, TimeOp, TimeSet
TimeUnit, flt_string, smei_getfile, smei_property, txt_read, who_am_i
PROCEDURE:
The testcase results are stored in an ASCII file in the
same directory as this procedure (smei_base_testcase.txt).
The file contains frame names and values for pedestal and
dark current.
The executable smei_base is run for all frames in the testcase.
Resulting Fits frames are written to $TUB/smei_base_testcase.
These files are cleaned up afterward.
Differences between pedestal and dark current should be at
the single precision level.
MODIFICATION HISTORY:
DEC-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_blocked
PURPOSE:
Used to temporary block the real-time SMEI pipeline
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
FUNCTION smei_blocked, ignore_block=ignore_block
OPTIONAL INPUT PARAMETERS:
/ignore_block return values always 0
(pipeline NOT blocked)
OUTPUTS:
Result 0: pipeline not blocked
1: pipeline blocked
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, hide_env, smei_filepath, txt_read
CALLED BY:
smei_mkbase, smei_mkcal_auto, smei_mkorb_auto, smei_mksky
PROCEDURE:
File $SMEIDB/cat/sts/block/block_file.txt should contain 0 or 1
(the file needs to be edited manually).
1 means that the pipeline is blocked.
The caller presumably will abort (unless /ignore_block is set)
MODIFICATION HISTORY:
DEC-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_buf
PURPOSE:
Main procedure for processing l1a files
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
PRO smei_buf, tmp_list
INPUTS:
tmp_list scalar; type: string; default: $TUB/l1a_list.txt
name of ascii file created by Python script l1a.py
(the file will be deleted after it has been read)
OUTPUTS:
.nic files to $dat/smei/nic
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, GetFileSpec, InitVar, SetFileSpec, TimeGet, TimeOp, TimeSystem
TimeUnit, destroyvar, do_file, hide_env, smei_buf_get, smei_buf_getframe
smei_buf_mget, txt_read
PROCEDURE:
> This procedure is accessed primarily through the Python script
l1a.py, which creates the main IDL main program and the input
file 'tmp_list'.
> All frames are extracted from the specified list of *.buf files
and written to disk as *.nic files.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
FEB-2004, Paul Hick (UCSD/CASS)
Added option for 'noclones' check.
Added option to move processed L1A files to other directory
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added option to allow writing of Fits files and Nic files.
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NAME:
smei_buf_get
PURPOSE:
Extracts data area for specified frames
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
PRO smei_buf_get, frame_headers, $
source = source , $
destination = destination , $
nic = nic , $
fits = fits , $
ptr_data = ptr_data , $
gzip = gzip , $
trange = trange , $
count = count , $
silent = silent , $
email = email , $
_extra = _extra
INPUTS:
frame_headers array; type: smei_frm_hdr structure
frame header array (as returned by smei_buf_getframe)
OPTIONAL INPUT PARAMETERS:
trange=trange array[n]; type: time structure
time info for tracking down SMEI frames.
See smei_buf_getframe for more information.
source=source scalar; type: string; default: /media/cdrecorder
directory where the L1A files are located.
If trange is used this is passed to smei_buf_getframe.
If frame_headers is specified than this is added to
frame_headers.l1a_file (which does not include a
directory).
destination=destination
scalar; type: string
directory into which to write the individual frame files
Output files have form c#frm_YYYY_DDD_HHMMSS (for padded
frames) or c#roi_YYYY_DDD_HHMMSS (for unpadded ROI
frames). # is the camera number (1,2 or 3).
/nic if set (and a valid destination is specified) then frame are
written in NIC file format (i.e. the data are stored in
the same way as for the TMO data, but the trailer has
a totally different structure)
/fits if set (and a valid destination is specified) then a fits
file is written
(at this point the frame headers are not written into
the fits file.
/split_dir if writing out lots and lots of frames it is probably better
to distribute the frames over multiple directories.
If /split_dir is set then each day of data is split in
4-hour intervals over 6 directories with names
destination/YYYY_DDD/HH with HH=00,04,08,12,16,20
email=email list of email addresses to be notified of errors
(used in smei_buf_read and smei_frm_cvhdr).
If the output keyword ptr_data is set, and /nic, /fits are not set
then the frame data ar returned as a heap variable.
/overwrite will unconditionally overwrite existing files when
writing individual frames to disk
/gzip gzip directories
OPTIONAL OUTPUT PARAMETERS:
count=count # frames found
ptr_data=ptr_data
array; type: pointer
the frame data corresponding to 'hdr'
i.e. *ptr_data[i] is the 2D frame data array.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, InitVar, IsTime, IsType, TimeGet, TimeSet, TimeUnit, hide_env
smei_buf_getframe, smei_buf_gzip, smei_buf_prep, smei_buf_read, smei_frm_write
smei_property, smei_setup_roi, txt_read
CALLED BY:
smei_buf
EXAMPLE:
The most efficient way to replace a damaged frame in the SMEI database from a DVD
is the following command:
smei_buf_get, timeset('2005_006_160819'), cam=2, /fits, dest=getenv('TUB'), /usedb
This requires that the proper DVD is mounted on /media/cdrecorder (specify
source=<source> to override the default) and that the SMEI database is accessible.
Note: dest='SMEIDB?' will NOT work.
PROCEDURE:
If either /fits or /nic is set then data are saved to binary files in
the destination directory (no pointer data will be returned).
File names will have the form c#frm_YYYY_DDD_HHMMSS.ext:
# = camera id (1,2 or 3)
ext = 'fts' or 'nic'
If neither /nic nor /fits is specified then data can be extracted in
ptr_data.
/fits SET:
Writes bare fits file (no extra frame header info is put in the file yet,
just the data are stored).
/nic SET (obsolete; we don't use .nic files anymore):
A 512 byte trailer is added after the data array.
The first 3 bytes are the characters 'buf' (to distinguish these
files from e.g. the TMO data files). The next 256 is the unmodified
header from the original frame (except for byte swapping to put the
data in native machine format.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
MAY-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Changed default source from /media/cdrecorder to /media/CDROM
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NAME:
smei_buf_getframe
PURPOSE:
Extracts individual frames from all *.buf files in the specified
source directory.
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
FUNCTION smei_buf_getframe, trange, $
source = source , $
camera = camera , $
count = count , $
dups_too= dups_too , $
usedb = usedb , $
silent = silent
INPUTS:
trange array[n]; type: time structure
n=0: if not specified than all frames in all L1A files in
'source' are extracted.
n=1: extract frame for specified time
n=2: extract all frames between trange[0] and trange[1]
n>2: extract frames for specified times
OPTIONAL INPUT PARAMETERS:
source=source scalar, array; type: string
scalar: source directory containing L1A *.buf files
array : list of fully-qualified names of L1A files
camera=camera scalar, array[2], array[3]
numbers 1, 2, or 3, identifying the cameras to be extracted
if 'camera' not set then all cameras are extracted.
/usedb if set then an attempt is made to find a file pointer in the
first L1A file to be accessed close to trange[0] (by
looking for nearby frames in the SMEI data base).
(this is primarily used to replace corrupted frames in the
SMEI data base).
OUTPUTS:
hdr array; type: smei_frm_hdr structure
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
# frames returned in 'hdr'
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FindAllFiles, GetFileSpec, InitVar, IsTime, IsType, TimeGet, TimeLimits
TimeOp, TimeSet, TimeUnit, UNIQ, boost, destroyvar, hide_env, smei_buf_read
smei_getfile, smei_property, where_common
EXTERNAL:
smei_buf_hdr__define, smei_frm_hdr__define
CALLED BY:
smei_buf, smei_buf_get
PROCEDURE:
Frame headers are stored in the same order as they are read from the
L1A files, i.e. there will be contiguous groups of frames from each
L1A files. Each L1A file appears to be chronological, but subsequent
files overlap (because of the double dump?). As a result the frame
header array as a whole (from more than one L1A file) is probably not
chronological.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_buf_gzip
PURPOSE:
Controls gzipping of new frames in SMEI data base.
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
PRO smei_buf_gzip, last_dir, need_gzip
INPUTS:
need_gzip scalar; type: integer
# frames to be gzipped
last_dir scalar; type: string
name of directory to be gzipped
OUTPUTS:
need_gzip scalar; type: integer
reset to zero
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType, hide_env
CALLED BY:
smei_buf_get, smei_buf_mget, smei_buf_prep
PROCEDURE:
MODIFICATION HISTORY:
OCT-2004, Paul Hick (UCSD/CASS)
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NAME:
smei_buf_hdr__define
PURPOSE:
Structure definition for file header of SMEI .buf files
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
hdr = {smei_buf_hdr}
INPUTS:
(none)
OUTPUTS:
(none)
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_buf_getframe, smei_buf_splitfile
PROCEDURE:
See Don Mizuno's, SMEI_CONVERT memo
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_buf_mget
PURPOSE:
Extracts all frames from specified l1a_files
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
PRO smei_buf_mget, l1a_files, $
destination = destination , $
nic = nic , $
fits = fits , $
nowrite = nowrite , $
gzip = gzip , $
silent = silent , $
email = email , $
_extra = _extra
INPUTS:
l1a_files array; type: string
fully-qualified names of l1a_files
OPTIONAL INPUT PARAMETERS:
destination=destination
scalar; type: string
directory into which to write the individual frame files
Output files have form c#frm_YYYY_DDD_HHMMSS (for padded
frames) or c#roi_YYYY_DDD_HHMMSS (for unpadded ROI
frames). # is the camera number (1,2 or 3).
/nic if set (and a valid destination is specified) then frames are
written in NIC file format (i.e. the data are stored in
the same way as for the TMO data, but the trailer has
a totally different structure)
/fits if set (and a valid destination is specified) then a fits
file is written
(at this point the frame headers are not written into
the fits file).
/split_dir if writing out lots and lots of frames it is probably better
to distribute the frames over multiple directories.
If /split_dir is set then each day of data is split in
4-hour intervals over 6 directories with names
destination/YYYY_DDD/HH with HH=00,04,08,12,16,20
/nowrite if set then no frames are written (all frames are listed as 'rejected')
This allows for testing of reading L1A files.
/overwrite if set existing frames are overwritten
(passed to smei_buf_prep)
email=email list of email addresses to be notified of errors
(used in smei_buf_read and smei_frm_cvhdr).
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
smei_buf
SEE ALSO:
smei_buf_get, smei_buf_getframe
CALLS: ***
CheckDir, InitVar, IsType, hide_env, smei_buf_gzip, smei_buf_prep, smei_buf_read
smei_frm_write, smei_property, smei_setup_roi
PROCEDURE:
This is a faster alternative to smei_buf_get. It processes all
l1a_files in sequence and extracts/writes to disk all frame data.
If either /nic of /fits is set then data are saved to binary files in
the destination directory (no pointer data will be returned).
File names will have the form c#frm_YYYY_DDD_HHMMSS.ext:
# = camera id (1,2 or 3)
ext = 'nic' or 'fts'
/nic SET:
A 512 byte trailer is added after the data array.
The first 3 bytes are the characters 'buf' (to distinguish these
files from e.g. the TMO data files). The next 256 is the unmodified
header from the original frame (except for byte swapping to put the
data in native machine format.
/fits SET:
STILL NEEDS WORK
Writes bare fits file (no extra frame header info is put in the file yet,
just the data are stored).
MODIFICATION HISTORY:
APR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_buf_prep
PURPOSE:
Decide whether a frame extracted from an L1A file needs to be
written to disk.
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
FUNCTION smei_buf_prep, hdri, destination, $
nic = nic , $
fits = fits , $
last_dir = last_dir , $
filelist = filelist , $
split_dir = split_dir , $
overwrite = overwrite , $
count = count , $
last_time = last_time , $
noclones = noclones , $
comment = comment , $
gzip = gzip , $
need_gzip = need_gzip , $
status = status
INPUTS:
hdri array[1]; type: frame header structure
frame header
destination scalar; type: string
name of existing directory where to write the file
If split_dir is NOT set then frames will be written
directly to 'destination'
If split_dir is SET then files are written into subdirectories
destination/year_doy/c1, destination/year_doy/c2 or
destination/year_doy/c3
count array[4]; type: integer
Counters to be updated.
OPTIONAL INPUT PARAMETERS:
/nic write nic file
/fits write fits file
/split_dir if writing out lots and lots of frames it is probably better
to distribute the frames over multiple directories.
If /split_dir is set then each day of data is split in
4-hour intervals over 6 directories with names
destination/YYYY_DDD/HH with HH=00,04,08,12,16,20
/overwrite by default frames are not written to drive if a file for
the frame already exists, UNLESS the new frame was from
the 1st telemetry dump. Set this keyword to
unconditionally overwrite existing files.
(setting -overwrite speeds up processing by a factor 2).
count=count array[4]; type: integer
The count array MUST EXIST on input for updates to
occur. One or more of the counters are incremented by 1.
count[0]: # frames written to disk as .nic or .fts
file (updated in smei_frm_write)
count[1]: # frames skipped because file already exists
(updated here)
count[2]: # frames with times earlier than the most
recent frame (updated here) that are written to
disk (these should be frames from the second dump;
if the second dump contains the same frames as the
first the number of these frames should be small)
count[3]: # clone frames (updated here)
last_time=last_time
array[1]; type: time structure
time of most recent frame processed
status=status if set, then status files for each day are created in
$SSWDB_SMEI/cat/sts. This keyword is used only
in the SMEI pipeline.
OUTPUTS:
filename scalar; type: string
fully-qualified file name to be used for output file.
If /overwrite is NOT set and the file exists already
then the null-string is returned.
count array[3]; type: integer
updated file counters
last_time array[1]; type: time structure
updated frame time
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
smei_buf_get, smei_buf_mget
COMMON BLOCKS:
common save_three_clones, last_hdrs, last
common save_double_dump , overlap_on, overlap_l1a, first_dump
CALLS: ***
CheckDir, FILEPATH, GetFileSpec, InitVar, IsType, TimeGet, TimeLimits, TimeOp, TimeSet
TimeUnit, UNIQ, boost, destroyvar, hide_env, smei_buf_gzip, smei_filename
smei_filepath, smei_frm_read, smei_property, txt_read
RESTRICTIONS:
If /split_dir is set then a 'mkdir --parents' is spawned to to create
subdirectories, and gzip is spawned to compress files. This works in
Linux, but not in Windows without some modifications.
PROCEDURE:
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
MAY-2003, Paul Hick (UCSD/CASS)
If /overwrite is NOT and a frame exists already the telemetry times are
compared. If the new frame is earlier than the one already on disk,
then it is still overwritten.
This determination is made from the name of the original telemetry file
which is stored in the frame header.
JUL-2003, Paul Hick (UCSD/CASS)
Force overwrite if there is read error on an existing .nic file.
FEB-2004, Paul Hick (UCSD/CASS)
Added /noclones keyword
Added new code to deal with double dump frames. Should reduce disk I/O
considerably.
AUG-2004, Paul Hick (UCSD/CASS)
Introduced error handler bracketing calls to smei_property(hdr,/tlm_time).
Occasionally the tlm_file name is screwy enough to crash
smei_property. If this happens continue assuming that the new frame
is from a second dump.
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword "status". This triggers writing of "status" files
to $SSWDB_SMEI/cat/sts each time the last frame for a given
day has been written. Used in pipeline.
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NAME:
smei_buf_read
PURPOSE:
Read Level 1A file in 'buf' format
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
FUNCTION smei_buf_read, l1a_file, pointer, $
get_file_header = get_file_header, $
file_header = file_header , $
frame_headers = frame_headers , $
frame_nr = frame_nr , $
frame_data = frame_data , $
get_next_frame = get_next_frame , $
silent = silent , $
force_close = force_close , $
trunc_time = trunc_time , $
start_pointer = start_pointer , $
email = email
INPUTS:
l1a_file scalar; type: string
fully-qualified file name of SMEI l1a*.buf file.
To close an open file, set l1a_file = ''
pointer scalar; type: integer
file pointer in l1a_file where the requested frame starts.
This argument is optional, but if known, speeds up
the process of finding a frame in the L1A file.
OPTIONAL INPUT PARAMETERS:
/get_file_header only fill file_header structure
/get_next_frame get next frame from file
If this keyword is set then the data file is kept open
with the file pointer after the current frame.
frame_nr=frame_nr
get frame with number 'frame_nr'
The frame number specified here should be taken
from the header array returned in a previous call
(this is a 1-based frame number).
trunc_time array[1]; type: time structure
used only when collecting all frame headers (i.e.
keywords frame_nr_defined and get_next_frame NOT set,
and argument have_pointer NOT set). The collection of
frames stops at the indicated time instead of
continuing until the end-of-file is reached.
start_pointer scalar; type: integer
when new l1a_file is opened move to file pointer
to start_pointer and start processing from there
instead of from the beginning of the file.
'start_pointer' is destroyed to avoid using
in another l1a_file.
email=email list of email addresses to be notified of errors
(used in smei_buf_read and smei_frm_cvhdr).
OUTPUTS:
status scalar; type: integer
0: failure; 1: success
OPTIONAL OUTPUT PARAMETERS:
file_header=file_header
array[1]; type: file header structure
frame_headers=frame_headers
array[n]; type: frame header structure array
an array with with headers for all frames is returned
array[1]; type: frame header structure
if 'frame_nr' is specified than the
header for the matching frame is returned
frame_data=frame_data
array[n], array[n,m]; type: unsigned int, long or float
if 'frame_nr' is set then the matching frame
data are returned here.
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; ROI mask common block
CALLED BY:
smei_buf_get, smei_buf_getframe, smei_buf_mget
COMMON BLOCKS:
common smei_read_buf_file, iu, open_file, open_hdr, pntr, last_frm, frm_count
CALLS: ***
InitVar, IsTime, IsType, TimeGet, TimeLimits, TimeOp, TimeUnit, boost, destroyvar
hide_env, smei_buf_splitfile, smei_filename, smei_frm_cvhdr, smei_property
smei_setup_roi, who_am_i
PROCEDURE:
The content of SMEI .buf files is described in Don Mizuno's memo:
The data area is padded to a 2D frame using the mask stored in
the ASCII file smei_buf_roi.txt. This file contains a 318 x 64 array with values 0,1,2 and 3.
0: pixels outside the region of interest
1: pixels in the smei fov
2: pixels in the covered columns left and right
3; pixels in the square open areas outside the smei fov
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
APR-2003, Paul Hick (UCSD/CASS)
Fixed bug in frame header structure. The naxes values in the raw
header were not updated when the ROI was applied (so the nic files
prior to today (Apr 20) have naxes=[0,0] in the trailer).
MAR-2003, Paul Hick (UCSD/CASS)
Entry frame_header.n_satured is filled here using the
data extracted from the L1A file.
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added checks for corrupted frames (as identified by
smei_frm_cvhdr).
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NAME:
smei_buf_splitfile
PURPOSE:
Analyze content of 256-ascii file header in SMEI L1A *.buf file
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
FUNCTION smei_buf_splitfile, byte_hdr
INPUTS:
ascii_hdr array[256]; type: byte
256-byte header
OUTPUTS:
Result array[1]; type: smei_buf_hdr structure
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_buf_hdr__define
CALLS: ***
GetFileSpec, TimeOp, TimeSet, timeposn
CALLED BY:
smei_buf_read
PROCEDURE:
The file header is actually stored in ascii form, so the input byte
array is converted to string before processing
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Based on SMEI Convert 1.0
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NAME:
smei_cam2angle
PURPOSE:
Get angles from unit vector in SMEI camera frame
CATEGORY:
camera/idl
CALLING SEQUENCE:
angle = smei_cam2angle(runit [,stheta=stheta, rtheta=rtheta])
INPUTS:
runit array[3,n]; type: float or double
x,y,z components of unit vector in UCSD camera frame
OPTIONAL INPUT PARAMETERS:
/stheta if set, then the direction cosine angles are returned
this is the default if no keywords are specified.
/rtheta if set, then the rotation angles from
Buffington et al., SPIE 4853, 490, 2002.
are returned
OUTPUTS:
angle array[2,n]; type: double
requested theta-x and theta-y angles
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, ToRadians
CALLED BY:
smei_findcrazy, smei_frm_hbar, smei_frm_where
SEE ALSO:
PROCEDURE:
/stheta set
locations in the sky as direction cosine angles theta-x and
These are the direction cosine angles required by Andy's formulae for
mapping sky locations to CCD positions ('Defining the field of
view for the SMEI cameras', A. Buffington, 11 July 2001.)
!!! These are not the same as the theta-x, theta-y angles
in Buffington et al., SPIE 4853, 490, 2002.
/rtheta
!!! These are the theta-x, theta-y angles
in Buffington et al., SPIE 4853, 490, 2002.
i.e. angles used in determining the performance of the baffle,
incl. the glare.
MODIFICATION HISTORY:
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_cam_quaternion
PURPOSE:
Get quaternion that rotates from ECI (=J2000) frame to UCSD
camera frame for given Coriolis s/c quaternion and camera.
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
qcam = smei_cam_quaternion(hdr)
qcam = smei_cam_quaternion(quaternion, camera)
qcam = smei_cam_quaternion(uttime, camera)
INPUTS:
hdr array[n]; type: SMEI_FRM_HDR structure
hdr.quaternion and hdr.camera are used
to calculate the camera quaternion.
array[n]; type: time structure
UT time is used to get the quaternion
assuming the Coriolis is in its
nominal attitude.
array[4] or array[4,n]; type: double
Coriolis quaternion (as extracted from
frame header). If 'hdr' is a quaternion
then 'camera' needs to specified too.
OPTIONAL INPUTS:
camera scalar or array[n]; type: integer
camera number (as extracted from frame header)
OUTPUTS:
qcam array[4] or array[4,n]; type: double
camera quaternion (relative to same coord
system as Coriolis quaternion)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CombineRotations, IsTime, IsType, smei_camera, smei_property, smei_sgp4_quat
CALLED BY:
cvsmei, smei_ccd2sky, smei_frm_where, smei_sky2cam
SEE ALSO:
smei_orient_test
PROCEDURE:
Camera quaternion rotates from J2000 equatorial coordinates to
UCSD camera coordinates.
MODIFICATION HISTORY:
JUN-2003, Paul Hick (UCSD/CASS
FEB-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added option to input time and retrieve the
the nominal quaternion.
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NAME:
smei_camera
PURPOSE:
Defines parameters for the SMEI fov
CATEGORY:
SMEI
CALLING SEQUENCE:
R = smei_camera(/get_center)
INPUTS:
nsize = nsize array[2]; type: long integer; default:[1280,360]
CCD frame size (pixels)
center= center array[2]; type: float; default: [631.65, 1233.03]
x- and y-coordinate of center of field of view arc
optical_axis array[2]; type: float; default: [-89.5 (deg), 1179.50 (pix)]
azimuth and radius of optical axis
identifies the location of the optical axis relative
to the fov center in terms of polar coordinates. By
default. The optical axis is near azimuth 270
(vertically below the center) at ~ 1200 pixels
distance.
fov_size array[2,2]; type: float: default:[30 (deg), 42.5 (pix)]#[-1,1]
the size of the SMEI fov in polar coordinates
The fov is ~ 60 degrees in azimuth by 85 pixels
in the radial direction, and is centered on the
optical axis.
quaternion array[4]; type: double: default
quaternion describing orientation of cameras
relative to the spacecraft structure.
fov_tosky array[2,2] type: float
scaling from CCD coordinates to sky coordinates
fov_toccd
OPTIONAL INPUT PARAMETERS:
/get_nsize retrieve frame size
/get_center retrieve center of field of view arc
/get_optical_axis retrieve optical axis coordinates
/get_fov_size retrieve field of view size
/get_fov_limits retrieve limits of field of view
/get_quaternion retrieve camera quaternions
/get_fov_tosky retrieve CCD-to-sky transformation constants
/get_fov_toccd
/get_structure retrieve structure containing all field of view information
/degrees if set then all angles (input and output) is in degrees
(default: radians)
OUTPUTS:
Output depends on the keyword selection.
If /get_fov_limits is set the limits of the field of view are returned:
R array[2,2]; type: float
limiting values in azimuth and radius of the fov
in the form [[angle1,radius1],[angle2,radius2]].
Angle1 and angle2 are in radians between [-!pi,+!pi].
The fov runs counterclockwise from 'angle1' to 'angle2'.
If /get_structure is set then a structure is returned containing all
field of view information:
R array[1]; type: structure
{SMEI_fov, $
camera : camera,
nsize : nsize,
center : center,
axis : optical_axis,
size : fov_size,
limits : fov_limits,
quaternion : quaternion,
tosky : fov_tosky,
radial_profile: ptr to radial_profile}
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CombineRotations, InitVar, IsType, ToDegrees, ToRadians
CALLED BY:
SMEI_cr_removal, TMO_tracksky, cvsmei, qGlitch_Run, qImage_cw_SMEI
smei_cam_quaternion, smei_ccd2sky, smei_sky2cam, smei_sky2ccd, stardistance
test_tmo
SEE ALSO:
smei_orient_test
PROCEDURE:
Default values are used unless other values are specified as input arguments
The fov limits are calculated from the location of the optical axis and
the size of the field of view.
MODIFICATION HISTORY:
FEB-2000, Paul Hick (UCSD/CASS)
MAR-2003, Paul Hick (UCSD/CASS)
Added numbers for flight cameras.
JAN-2004, Paul Hick (UCSD/CASS)
Added camera values from Aarons indexing program. These used the center
values from Andys memo, and camera quaternions obtained by trial-and-error.
These numbers are now the default.
FEB-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Update camera quaternions with values used by the Fortran
SMEI programs. Presumably these are the best we have.
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NAME:
smei_camera_gain
PURPOSE:
Returns the camera gain at specified time
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_camera_gain, tt, $
camera = camera , $
zero_time = zero_time , $
zero_gain = zero_gain , $
delta_gain = delta_gain
INPUTS:
tt array[n]; type: time structure
UT time
OPTIONAL INPUTS:
camera=camera scalar or array[n]; type: integer; default: 2
camera number, 0,1,2,3
camera=0 will always return gain=1.00
zero_time=zero_time
array[1]; type: time structure;
default: TimeSet(yr=2003,doy=0)
Time origin for gain correction
zero_gain=zero_gain
array[4]; type: float; default: 1.0/[0.00,0.97,1.00,0.92]
gains for "camera 0" and three cameras at time zero_time
delta_gain=delta_gain
array[4]; type: float; default: [0.00,-0.005,-0.01,-0.01]
gain change per year for "camera 0" and three cameras
OUTPUTS:
gain array[n]; type: float
gain correction at specified times
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, TimeOp, TimeSet, TimeUnit
CALLED BY:
smei_sky_read, smei_star_fit, smei_star_remove, smei_zld_remove [1]
smei_zld_remove [2]
PROCEDURE:
The sensitivity of the cameras appears to be decreasing at a
rate of about 1% per year. (But see next paragraph)
JUL-2008:
From looking at a timeseries of a patch of 31x31 skybins centered on the
galactic center for the period 2003-2008 we found that the gain for
camera 1 is decreasing by about 0.5%/year. For camera 2 the original
number of 1%/year is still acceptable, but may actually be closer to
1.1%/year. For camera 3 the current 1%/year may be a bit large, but
it is not clear by how much.
NOV-2008:
It was decided to set the gain decrease for camera 1 back to 0.1%/year.
Andy set the time origin for the gain to 2003, doy 0 (NOT doy 1).
So the time origin is at 2002 Dec 31, 0 UT.
MODIFICATION HISTORY:
JUL-2006, Jordan Vaughan, Paul Hick (UCSD/CASS)
NOV-2007, Paul Hick (UCSD/CASS)
zero_gain was defined wrong. The gain for camera 1 at zero_time
is 1.0/0.97 (NOT 0.97); for camera 3 it is 1.0/0.92 (NOT 0.92).
I.e., cameras 1 and 3 are MORE sensitive than camera 2;
NOT less sensitive as originally coded.
DEC-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Gain for camera 1 was set to 0.5% per year for a while.
On Dec 1 the gain was set back to old value of 1% per year.
Default tt is now the time origin zero_time (used to crash
with undefined tt).
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NAME:
smei_ccd2sky
PURPOSE:
Convert from CCD coordinates to positions in the sky
CATEGORY:
SMEI
CALLING SEQUENCE:
R = smei_ccd2sky( rvec, [ camera=camera, quaternion=quaternion, /degrees])
INPUTS:
rvec array[2,*]; type: float
x- and y- coordinates of locations on the CCD
These are converted to sky coordinates if inside the
field of view. If no points lie inside the field of
view then the scalar BadValue(rvec) is returned.
If rvec is not specified then all pixels in a
frame are processed.
OPTIONAL INPUT PARAMETERS:
/rectangular if set then the return value is in rectangular coordinates
(with 1st dimension of 3).
camera=camera This keyword can be any one of the following three.
array[1]; type: smei_buf_frm structure
this determines the camera and the quaternion.
The keywords 'quaternion' and 'qcamera' are ignored.
array[1]; type: smei_camera_fov structure
structure containing information about SMEI field of
view; usually the return value of smei_camera
with the /get_structure keyword set.
scalar; type: integer
camera number (1,2 or 3).
If not specified then camera=1 is assumed.
The camera number is used as argument to smei_camera to
obtain the fov structure.
quaternion=quaternion
array[4]; type: float
Coriolis quaternion, or (if /qcamera is set) the
camera quaternion (i.e. the quaternion
constructed by smei_cam_quaternion).
/qcamera indicates that 'quaternion' already is the camera
quaternion for the camera specified in 'camera'.
/degrees if set, all in- and output angles are in degrees
(default: radians). Note that the 'fov' structure
must be consistent with the setting of /degrees.
/boolean if set then the output array 'inside' is returned as an
2D array of indices. (set this keyword only if rvec
is NOT specified, i.e. when processing a whole frame.
distort=distort
NOT IMPLEMENTED YET
OUTPUTS:
R array[2,n]; type: float
spherical coordinates (longitude, latitude)
for all pixels inside the SMEI fov
OPTIONAL OUTPUT PARAMETERS:
inside=inside
array[ n]; type: long integer (if /twod NOT set)
array[2,n]; type: long integer (if /twod set0
one- or two-D CCD pixel indices for all the pixels
listed in R
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, BadValue, CV_COORD, CvRotation, InitVar, Inside_Wedge, IsType, SubArray
SyncDims, ToDegrees, ToRadians, boost, gridgen, smei_cam_quaternion, smei_camera
smei_radial2theta
PROCEDURE:
MODIFICATION HISTORY:
OCT-1998, Paul Hick (UCSD/CASS)
FEB-2001, Paul Hick (UCSD/CASS; pphick@ucsd.edu); added quaternion keyword
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NAME:
smei_coriolis
PURPOSE:
Returns time at which Coriolis was in specified orbit
CALLING SEQUENCE:
FUNCTION smei_coriolis, tt_or_orbit , $
orbital_period = orbital_period, $
number = number , $
fraction = fraction , $
doublex = doublex
INPUTS:
tt_or_orbit array; type: time structure or any numerical type
if input are times then output is the
orbit number; if input is numerical then
output is the orbit time.
OPTIONAL INPUTS:
/orbital_period return orbital period
if set then the orbital period at the specified
time or orbit number is returned
(if tt_or_orbit is not specified then
tt_or_orbit=0 is assumed)
/number these three keywords are used only if a time
/fraction structure is specified as input (the keywords
/doublex are passed to smei_orbit_get.
OUTPUTS:
smei_coriolis array; type: numerical or time structure
orbit number or orbit time (depending on input
tt_or_orbit
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, IsTime, IsType, TimeGet, TimeLInterpol, TimeOp, TimeSet
smei_orbit_get, smei_orbit_set, timeposn, txt_read, who_am_i
CALLED BY:
FUNCTION smeilatest lastorbit, PlotEarthSkymap [2], TimeGet, TimeSet, allsky [1]
allsky [2], allsky [3], allsky_f, orb_comp, smei_frm_findpoint, smei_getfile
smei_orbit_stats, smei_shutterwrong, smei_star_fit, smei_www_skymaps
PROCEDURE:
Orbit n0(=0) starts at t0 = 2002/12/31 23:56:41.900.
The orbital period at this time was p0=0.0705612268519d0 days (6096.490 s),
and has been decreasing since with dp=0.084 msec per orbit.
(0.42s reduction in SMEI period per 365 days).
The effective orbital period for orbit n is p0-(n-n0)*dp.
The start times for each orbit becomes:
t(n0+0) = t0
t(n0+1) = t(n0+0)+p0-1*dp
t(n0+2) = t(n0+1)+p0-2*dp
...
t(n0+n) = t(n0+n-1)+p0-n*dp = t0+n*p0-0.5*n*(n+1)*dp
MODIFICATION HISTORY:
JUN-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SMEI_cr_removal
CALLING SEQUENCE:
pro SMEI_cr_removal, files, $
nbuffer = nbuffer , $
sigmathreshold = SigmaThreshold, $
minthreshold = MinThreshold , $
remove = Remove , $
silent = silent
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, BadValue, CV_COORD, Find2DGlitch, GroupPixels, Inside_Wedge
SuperArray, TMO_skymotion, bin_read, destroyvar, gridgen, smei_camera
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NAME:
smei_cv_catalogue
PURPOSE:
Modifies formatting in bright star catalogue
CATEGORY:
camera/idl
CALLING SEQUENCE:
PRO smei_cv_catalogue
INPUTS:
Text file brightstars.txt in same directory as this routine.
OUTPUTS:
updata catalogue (overwrites old one)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, txt_read, who_am_i
PROCEDURE:
Fixes format problem with small negative latitudes. The minus sign
in front of zero degrees is moved to the minute (or even the seconds
field) e.g. entry -0 20 20 is changed to 0 -20 20
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_filename
PURPOSE:
Construct or deconstructs file name for SMEI data files from/into its
components (time,camera,file extension, and map mode)
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_filename, tt, $
camera = camera, $
mode = mode , $
postfix = postfix,$
upto = upto , $
pos_tt = pos_tt, $
type = type , $
dir = dir , $
ccd = ccd
INPUTS:
tt array[n]; type; time structure or string
time or file name
If tt is a file name, two conditions must
be met for a successfull deconstruction:
- it must contain a valid time string
(see timeposn).
- the time must be preceeded by an
underscore
If these are not met then the 'camera'
'mode' and 'postfix' fields are not set
(i.e. camera=-1, mode=postfix='')
OPTIONAL INPUT PARAMETERS:
If input 'tt' is a time structure, the file name is
constructed using the following additional input:
camera=camera scalar or array[n]; type: integer; default: 1
camera number (1,2, or 3)
type=type scalar or array[n]; type: string; default: '.fts.gz'
file type
mode=mode scalar or array[n]; type: string or integer; default: 0
file mode, e.g. 'frm', 'cal','sky','equ'
If an integer is specified it is assumed to be the
frame binning mode 0 (1x1), 1 (2x2) or 2 (4x4),
in which case the mode will be 'm'+mode
upto=upto scalar; type: integer; default: TimeUnit(/sec)
sets time unit where file name is truncated
(only used if input 'tt' is time structure)
OUTPUTS:
If input 'tt' is time structure:
result array[n]; type: string
name of SMEI file
If input 'tt' is a file name
result array[n]; type: time structure
time coded into SMEI file (e.g. time of
frame or start time of orbit)
OPTIONAL OUTPUT PARAMETERS:
If input 'tt' is a filename several parameters coded into
the file are extracted:
camera=camera array[n]; type: integer
camera number (1,2, or 3)
ccd=ccd set to 1 if all entries are CCD frames
(i.e. 'm0','m1','m2' and 'cal' files
mode=mode array[n]; type: string or integer; default: 0
file mode, e.g. 'frm', 'cal','sky','equ',
'l1a', 'm0', 'm1', 'm2'.
If ccd=1, and all files are 'm0','m1' or
'm2' (i.e. no 'cal' files), then mode is
returned as integers (0,1 or 2).
Otherwise the mode is returned as a string,
i.e. for CCD frames it will be 'm0','m1','m2'.
pos_tt=pos_tt array[n]; type: integer
position where time string starts in file name
(-1 if no time string is found)
pos_tt applies to the file name only (i.e.
after the directory spec has been removed).
type=type array[n]; type: string
file type (may be a double type
e.g. .fts.gz)
directory=directory
array[n]; type: string
directory (null-string if not present)
postfix=postifx array[n]; type: string
null-string, 'm0' or 's'
Set to 'm0' (if the directory name
ends in 'c#m0') or 's' (if the directory name
ends in 'c#s' (where # is the camera
number).
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
GetFileSpec, InitVar, IsTime, IsType, SyncArgs, TimeGet, TimeSet, TimeUnit, UNIQ
strreverse, timeposn
CALLED BY:
img_read, orb_comp, psfn, qImage_cw_Property, qsmei_sky_pick, skyd_cat
smei_buf_prep, smei_buf_read, smei_filepath, smei_findpnt, smei_getfile
smei_hdr_get, smei_hdr_plot, smei_mkbase, smei_mkcal, smei_mkcal_auto
smei_mkorb_auto, smei_mksky, smei_property, smei_rewind, smei_sky_field
smei_sky_getmask, smei_sky_read, smei_sky_track, smei_star_remove
smei_zld_remove [1], smei_zld_remove [2]
PROCEDURE:
Uses the standard SMEI template for file names:
c1m0_2003_123_123456.fts.gz
MODIFICATION HISTORY:
MAY-2004, Paul Hick (UCSD/CASS)
JUL-2004, Paul Hick (UCSD/CASS)
Modified to deal with new frame name syntax with mode coded
into the file name
JUL-2004, Paul Hick (UCSD/CASS)
Updated documentation
MAR-2008, Paul Hick (UCSD/CASS)
Substantial rewrite of deconstruction section.
Added pos_tt and ccd keywords.
JUN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
The filename of a calibration patter (mode='cal') is now
recognized as a CCD frame.
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NAME:
smei_filepath
PURPOSE:
Construct path to SMEI file (frame or skymap)
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_filepath, tf, $
base = base , $
source = source, $
camera = camera, $
mode = mode , $
postfix = postfix,$
type = type , $
upto = upto , $
full = full
INPUTS:
tf undefined; scalar, or array[1]
if defined then either a time (in the form of a standard
time structure), or the name of a SMEI frame or skymap
(e.g. 'c2m0_2003_123_456789')
NOTE: if tf is NOT defined than keyword source MUST be
set to an existing directory.
OPTIONAL INPUT PARAMETERS:
source=source scalar; type: string; default: SMEIDB?
directory where to look for SMEI frames.
If the directory does not exist then the current SMEI
drive is used. The default value SMEIDB? will result
in an automatic determination of a source directory
using the information in file smei_drives.txt.
The SMEI frames are stored in directories of the form
$SMEIDB#/yyyy_doy/hh. By default the name of the full directory
where the frames for time 'tf' are located is returned.
/base if set only the part $SMEIDB# is returned
/day if set only the part $SMEIDB#/yyyy_doy is returned
mode scalar; or array[2]
mode[0] is used in construction of directory
(e.g. $SMEIDB/orb for orbital patterns (mode='orb')
mode[1] is used in construction of filename (/full set)
(e.g. mode=['orb_003','orb'] results in
$SMEIDB/orb_003/c3orb_2000_001_000000.fts.gz)
OUTPUTS:
ff scalar; type: string
directory where frame(s) for specified time are located
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
skyd_cat, skyd_version, smei_blocked, smei_buf_prep, smei_findpnt, smei_frm_mask
smei_frm_read, smei_getfile, smei_hdr_get, smei_hdr_plot, smei_hdr_update
smei_mkbase, smei_mkc3mask, smei_mkcal, smei_mkcal_auto, smei_mkmask, smei_mkorb
smei_mkorb_auto, smei_mksidereal, smei_mksky, smei_orbit_stats, smei_property
smei_rewind, smei_sky_getmask, smei_sky_read, smei_star_remove
smei_zld_remove [1], smeidb_mounted
COMMON BLOCKS:
common smei_filepath_save, checkdrives, sdat
CALLS: ***
CheckDir, FILEPATH, InitVar, IsTime, IsType, TimeGet, TimeOp, TimeSet, TimeUnit
destroyvar, flt_read, smei_filename, who_am_i
PROCEDURE:
The SMEI data are distributed across several hard drives.
Env variables SMEIDB1, SMEIDB2, etc. exist pointing to the mount
points of each drive. Each drive contains data for the time range
specified in the file 'smei_drives.txt'.
SMEI data are organized in separate folders for each day. E.g. the
folder $SMEIDB1/2003_100/c2 contains all SMEI frames
day of year 100 (in year 2003) for camera 2.
If tf is NOT defined then the YYYY_DOY part in the returned path
will be missing. This is useful to locate skymaps (which usually are
split up by camera only, not by time).
MODIFICATION HISTORY:
JUN-2003, Paul Hick (UCSD/CASS)
Introduced to deal with multiple hard drives containing
SMEI data frames.
MAY-2004, Paul Hick (UCSD/CASS)
Modified to reflect new directory structure of SMEI data base
(frames are now organized in a separate directory for each
doy of year, with subdirectories for each of the cameras)
AUG-2006, Paul Hick (UCSD/CASS)
Modified to do something useful when tf is not defined.
FEB-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Generalized to work with data other than CCD frames
(skymaps, hdr and png files)
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added 'cal', 'orb', 'orb_003', 'sts' to mode options.
' 'mode' can now be a 2-element array with mode[0] used
in the directory name and mode[1] in the filename
(if /full is set)
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NAME:
smei_findcrazy
PURPOSE:
Look for 'crazy frames'
CATEGORY:
CALLING SEQUENCE:
PRO smei_findcrazy, trange, source=source, camera=camera, mode=mode, copy=copy
INPUTS:
trange passed to smei_hdr_get
OPTIONAL INPUT PARAMETERS:
camera
mode
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS: ***
GetFileSpec, InitVar, boost, destroyvar, do_file, smei_cam2angle, smei_frm_hbar
smei_hdr_get
SEE ALSO:
PROCEDURE:
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_findobj
PURPOSE:
WORK IN PROGRESS
Analyzes output from smei_findpnt
CATEGORY:
smei/ucsd/camera/idl/star
CALLING SEQUENCE:
PRO smei_findobj , $
eq_objects = eq_objects , $
np_objects = np_objects , $
sp_objects = sp_objects , $
camera = camera , $
source = source , $
from_mode = from_mode , $
binfactor = binfactor
OPTIONAL INPUT PARAMETERS:
eq_objects=eq_objects array; type: structure
np_objects=np_objects array; type: structure
sp_objects=sp_objects array; type: structure
source=source scalar; type: string; default: $TUB
fromn_mode=from_mode scalar; type: string; default: 'bol'
camera=camera scalar; type: integer; default
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS: ***
AngleRange, AngleUnits, ArrayLocation, FILEPATH, HIST_2D, InitVar, IsType, MEAN, REVERSE
STDDEV, WhatIs, boost, cvsmei, cvsmei_init, destroyvar, smei_i2m, smei_star_list
smei_star_readpnt, view
SEE ALSO:
COMMON BLOCKS:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
STATE INFO USED:
STATE INFO MODIFIED:
PROCEDURE:
MODIFICATION HISTORY:
NOV-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_findpnt
PURPOSE:
Originally created to look for point sources in the star-subtracted
equ files to find unknown objects (i.e. objects not included in the
SMEI star catalogues).
To run this program access is needed to the 'equ' files, If keyword
/use_catalogue is set then also access to the 'sky' files is required.
CATEGORY:
smei/ucsd/camera/idl/star
CALLING SEQUENCE:
PRO smei_findpnt, wanted_map , $
camera = camera , $
from_mode = from_mode , $
to_mode = to_mode , $
destination = destination , $
fix_centroid= fix_centroid , $
cvmin = cvmin , $
use_catalogue= use_catalogue, $
npeak = npeak , $
silent = silent , $
_extra = _extra
INPUTS:
wanted_map array[n]; type: string, time structure or integer
passed to smei_getfile.
Selects skymap files to be processed.
Usually this is a pair of times (start time and
stop time) to process all maps inside a period
of time.
OPTIONAL INPUT PARAMETERS:
camera=camera scalar; type: integer; default: 2
camera id (1,2,3). The default camera 2 has the most
sky real estate.
from_mode=from_mode
scalar; type: string; default: 'equ'
selects the type of skymap to be used.
Can also be used for 'sky' to work from the
unsubtracted maps, but that doesn't make much sense
since these maps still contain all the catalogue stars.
to_mode=to_mode
scalar; type: string; default: 'bol'
This is only used in the naming convention for the
output 'pnt' files: the names will look like:
c2bol_YYYY_DOY_hhmmss.pnt
where YYYY_DOY_hhmmss is the start time of a SMEI
orbit, taken from the associated 'equ' file
destination=destination
scalar; type: string; default: $TUB
destination directory of output file(s)
fix_centroid=fix_centroid
if set, this turns on the 'fix_centroid' option in the
smei_star_fit, i.e. the centroid position of the new
object is iteratively improved. This gives better results
at the expense of a substantial increase in processing time.
cvmin=cvmin scalar; type: float; default: 0.7
Only new objects with a PSF correlation coefficient
greater than cvmin will be written to the output files
/use_catalogue if set, an attempt is made to match unknown objects against
objects in the SMEI catalogue. This will pick up 'unknown'
objects at the location of a SMEI catalogue object, usually
indicating that the catalogue star was imperfectly subtracted.
This keyword can increase processing time significantly
especially if combined with a low cvmin value.
npeak=npeak scalar; type: integer; default: none, i.e. no limit
passed to FindPeaks.
Can be used to limit the number of objects on the initial
list of local maxima in the skymap, that are further
investagated by smei_star_fit.
Probably best avoided (see PROCEDURE)
silent=silent scalar; type: integer; default: 0
higher values suppress more informational messages
OUTPUTS:
Files in destination directory
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, AngleUnits, ArrayLocation, BadValue, FILEPATH, FXPAR, FindPeaks, HEADFITS
InitVar, REVERSE, SuperArray, TimeSet, TimeSystem, boost, cvsmei, destroyvar, hide_env
smei_filename, smei_filepath, smei_getfile, smei_sky, smei_star_fit
smei_star_info, smei_star_writepnt, sphere_distance
PROCEDURE:
The equ files have all SMEI catalogue stars (presumably all stars
brighter than 6th magnitude), the sidereal background and the
zodiacal dust cloud subtracted.
The search procedure consists of the following steps:
1. Smoothing of skymaps.
First the map is smoothed by subtracting a running mean for an 8 degree wide box.
This takes out variations over spatial scales much larger than the PSF. This step
mainly serves to create local maxima that are more easily sorted, i.e. it makes
it easier to process maxima starting with the highest and working down from there.
The second step is to apply a smoothing using a running mean of 1 degree, the full
width of the SMEI PSF. This reduces the noise in the maps, and avoids picking
up every noise spike as a separate local maxima.
2. Prepare a list of candidate objects.
In this step the procedure FindPeaks is used to make a list of all the local
maxima in the skymap, listing the highest ones first.
The number of local maxima can be controlled with a number of keywords
(see FindPeaks for details). This should not really be necessary:
step 1 has proven to be the simplest way to control the output from
FindPeaks.
3. Fit all the candidate maxima to the PSF using smei_star_fit.
This step uses the default star fitting procedure for SMEI to identify
those objects on the candidate list that look like point sources (i.e.
look like the SMEI PSF).
The main keyword to control this step is /fix_centroid.
The default mode is NOT to use this keyword. In that case the PSF is fit
once at the location of each candidate maximum. If /fix_centroid is ON,
then an iterative procedure is used to find the location in the skymap
near the candidate maximum that provides the best fit (the highest
correlation between the object in the skymap and the standard SMEI PSF).
The advantage of NOT setting /fix_centroid is a significant reduction
in processing time (close to a factor of 10). The disadvantage is that
the quality of the PSF fitting is worse, which might lead to good objects
going unnoticed because the correlation is much worse.
The result of step 3 is that all the candidate objects from step 2
can be classified by sorting on the correlation coefficient of
of the PSF fit. The difference between using (or not using) /fix_centroid
is that the candidates will be sorted differently.
4. Retain the best fitting objects only
At this stage the keyword cvmin is used to only retain objects that
resulted in a correlation coefficient higher than cvmin (0.7 by default).
The total list of candidates for one skymap can easily be on the order
of 1000 or so. A significant fraction of the correlation coefficient
(often 70-80%) of the candidates will be quite low, so it makes sense
to reduce the search space by focusing on the higher correlations.
Note that at this stage the effect of using (or not using) fix_centroid
in step 3 becomes evident: since the correlation coefficients are different
(lower when fix_centroid is not used), a different set of candidate objects
is retained. Note that if cvmin=-1 is used, all objects are retained.
This results in significantly larger output files though.
[Rebekah, could you summarize your tests with /fix_centroid and cvmin here.
This is what I remember]
For cvmin=0.7 a testrun indicates that approximately the same amount of
objects remain for runs with /fix_centroid ON and OFF, with about 2/3 of
the objects the same in both lists.
4. Match against catalogue stars
This step is optional. By default it is not done, but it can be switched
on with keyword /use_catalogue.
The locations of the candidate maxima from step 4 (after trimming the list
using cvmin), is compared against the locations in the SMEI star
catalogues. If a catalogue star is found whitin 0.5 degrees of a
candidate object, most likely the object found is the results of
a badly-subtracted catalogue star. In this case the candidate
object will be listed in the output file under the name of the candidate
object. Note that this is not a positive indentification; it just indicates
the proximity of a catalogue star.
Using a low value of cvmin in combination with /use_catalogue keyword is
not advisable: checking a long list of candidate objects against the SMEI
star catalogue will drastically increase processing time.
5. Write output file
The output files contains the results of the fits for all candidate
objects, sorted by correlation (the best one first).
Note that for objects located in the overlapping area between the polar
maps and the equatorial map (approximately between 50 and 60 degrees
declination north and south there will be two records in the output file:
one for the object seen in the equatorial map, the other in one of the
polar maps. This needs to be taken into account when analyzing the
content of the input file (e.g. when counting the number of hits for
a given object in a sequences of skymaps).
The names of the objects indicated in which map the object was detected,
EQ (for the equatorial map), NP and SP for north and south polar map,
respectively; followed by an integer that counts the number of objects.
Note that the same object will have a different name in output files
for different skymaps. Entries will need to be matched by RA and dec.
MODIFICATION HISTORY:
FEB-2008, Paul Hick (UCSD/CASS)
NOV-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Thorough review of code; added documentation.
Most significant change to the code was the removal of the zodiacal
dust cloud subtraction. The equ file now contain maps with the zld
already subtracted, so this is not needed anymore.
Reduced dependence on 'sky' files. These are needed now only if
keyword /use_catalogue is used.
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NAME:
smei_fixpnt
CALLING SEQUENCE:
PRO smei_fixpnt, file, version=version
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, FindAllFiles, InitVar, hide_env, smei_star_formatpnt, smei_star_info
txt_read
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NAME:
smei_frm_base
PURPOSE:
Calculate pedestal and dark current for frame
CATEGORY:
smei/camera/idl/misc
CALLING SEQUENCE:
PRO smei_frm_base, hdr, img, silent=silent, $
cam_full=cam_full, cam_ok=cam_ok, init=init, reset=reset, $
clear=clear, frm=frm, step=step, status=status, $
nfill_control=nfill_control, nbad_control=nbad_control
INPUTS:
hdr array[1]; type: structure
frame header
img array; type: integer
frame data
OPTIONAL INPUT PARAMETERS:
nfill_control=nfill_control
scalar; type: integer; default: 10
/init initialize all camera/mode combinations
/reset re-initialize the current camera/mode combination only
/clear clear all variables stored internally in common block
silent =0: display all messages
=1: suppress non-essential messages
=2: suppress all messages
OUTPUTS:
hdr array[1]; type: structure
frame header with a number of values filled, in particular
hdr.pedestal, hdr.dark current, hdr.squares, hdr.centerpix
img array; type: float
image with pedestal and dark current subtracted
Any negative elements after subtraction are set to zero
(these will mostly be pixels in the semi-covered columns
(5 and 315 for mode 2 data)
OPTIONAL OUTPUT PARAMETERS:
cam_ok=cam_ok
scalar; type: byte
0: failed to determine pedestal and/or dark current
1: pedestal and dark current determined successfully
nfill_control=nfill_control
scalar; type: integer
# good frames used to build reference base values
cam_full=cam_full
0: still busy accumulating reference base data (based on
nfill_control preceeding good frames) for current
camera/mode combination
1: reference data for preceeding nfill_control good frames
available
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; SMEI masks
CALLED BY:
smei_frm_track
COMMON BLOCKS:
common smei_frm_base_save, ped_threshold, drk_threshold, $
ped_mean_init, drk_mean_init, ped_sigma_init, drk_sigma_init, $
nfull, nbads, ifull, bfull, nbad, badv, $
peds_mean, peds_sigma, drks_mean, drks_sigma,$
ped_mean , ped_sigma , drk_mean , drk_sigma , $
drk_nout_init, drk_dout_init, drks_nout, drk_nout, drk_dout, $
drk_lr_ratio
CALLS: ***
ArrayLocation, BadValue, InitVar, IsType, MEAN, STDDEV, TimeGet, TimeUnit, destroyvar
smei_property, smei_setup_roi, where_common, who_am_i
PROCEDURE:
MODIFICATION HISTORY:
MAY-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_comments
PURPOSE:
Returns comments for Fits header in SMEI frame
CATEGORY:
CALLING SEQUENCE:
FUNCTION smei_frm_comments, hdr
INPUTS:
hdr array[1]; type: SMEI__FRM_HDR structure
SMEI frame header
OUTPUTS:
str array[n]; type: string
list of comments (one for each tag name
in the SMEI__FRM_HDR structure
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
smei_frm_cvhdr
PROCEDURE:
MODIFICATION HISTORY:
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_cp
PURPOSE:
Copy SMEI frames from SMEI data base
CATEGORY:
ucsd/camera/idl/frm
CALLING SEQUENCE:
PRO smei_frm_cp, trange, destination=destination, unzip=unzip, camera=camera, mkdir=mkdir, _extra=_extra
INPUTS:
trange array[2]; type: time structure
time range to be copied (see TimeSet)
OPTIONAL INPUT PARAMETERS:
camera=camera scalar, or array[n] (n=1,2,3); default: [1,2,3]
cameras to be copied
/unzip if set files are unzipped
/mkdir if set then the destination directory specified using
the'destination' keyword is created if it doesn't exist already
Passed to smei_getfile:
silent=silent controls informational messages
mode=mode scalar, or array[n] (n=0,1,2); default: none
if set only the specified modes are selected
OUTPUTS:
(none)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, GetFileSpec, InitVar, IsTime, TimeGet, TimeOp, TimeSet, TimeUnit
do_file, hide_env, smei_getfile
RESTRICTIONS:
Files are copied in groups of typically about 4000 frames at a time.
See do_file for more details. The limitation arises from a restriction
on the length of a shell command (usually 128 kB).
PROCEDURE:
> Files for camera 1 are copied into subdirectory c1 of destination
directory (the subdirectory is created if it does not exist yet).
Same for cameras 2 and 3.
> Specifying the mode keyword requires that file headers need to be read
to determine the mode (the camera number is coded into the file name).
This slows down the copy operation considerably.
EXAMPLES:
Copy files for cameras 1 and 2 from between 0 UT on doy 110 to 0 UT on doy 115
for 4x4 binning (mode 2) to the $TUB directory: Unzip files after copy
is complete.
tt = TimeSet(yr=2004,doy=[110,115])
smei_frm_cp, tt,destination=getenv('TUB'), /unzip, camera=[1,2], mode=2
Copy all frames for the specified time period for all cameras to
'/zulu/zone/2003_110_115', creating the subdirectory 2003_110_115 if it
doesn't exist already; suppress informational messages:
tt = TimeSet(yr=2004,doy=[110,115])
smei_frm_cp, tt,destination=getenv('TUB'), /unzip, silent=1
See TimeSet for other ways to specify begin and end time.
MODIFICATION HISTORY:
JUL-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_cvhdr
PURPOSE:
Convert frame headers between various formats
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_frm_cvhdr, $
from_hdr = from_hdr , $
from_byte = from_byte , $
from_fits = from_fits , $
to_ascii = to_ascii , $
to_fits = to_fits , $
to_byte = to_byte , $
to_hdr = to_hdr , $
swap_bytes = swap_bytes, $
tlm_file = tlm_file , $
l1a_file = l1a_file , $
l1a_pntr = l1a_pntr , $
length = length , $
allow_bad = allow_bad , $
corrupt_frame = corrupt_frame , $
error_message = error_message
OPTIONAL INPUT PARAMETERS:
from_hdr=from_hdr array[1]; type: smei_frm_hdr structure
frame header
from_byte=from_byte array[256] or array[512]; type: byte
binary header from L1A file (256 bytes) or
trailer from .nic file (512 bytes).
A trailer from .nic file should have the
starting byte('buf') removed already.
from_fits=from_fits array[n]; type: string
fits header extracted from SMEI frame fits file
/to_hdr return header as a smei_frm_hdr structure
/to_byte return header as a 256 or 512 byte array
/to_fits return header as a fits header string array
if the fits header is not from a SMEI camera frame
then the integer -1 is returned.
/to_ascii return a single string with an ascii representation
of selected information from the header (used primarily
for display in widgets).
/swap_bytes if set, then bytes are swapped in the byte header
(used if from_byte=from_byte or /to_byte is used.
OUTPUTS:
rtn_hdr header in format selected with /to_* keywords
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, CV_COORD, FXADDPAR, FXPAR, GetFileSpec, InitVar, IsType, MKHDR, TimeGet
TimeOp, TimeSet, TimeUnit, cvsmei, eclipsed_area, jpl_body, jpl_eph, sgp4_eph
smei_frm_comments, smei_frm_flag, smei_property
CALLED BY:
img_read, smei_buf_read, smei_frm_read, smei_frm_write
PROCEDURE:
Only a selection of the data in the header are put in the string,
separated by the newline character (10B).
The binary frame header in the Hanscom L1A*.buf files binary header
has 256 bytes. These are in Unix format (big-endian), i.e. byte swapping
is necessary on i386 machines (which are little-endian).
The .nic files contain a 512 byte trailer.
The first 3 bytes in the .nic files are used to store the ASCII string 'buf'
(to distinguish them from other .nic files, e.g. the TMO data).
The next 256 bytes in the .nic trailer (bytes 3-258) are a copy
of the frame header found in the Hanscom L1A*.buf files, except for byte
swapping when necessary (i.e. they are little-endian).
The remaining 253 bytes are partially filled with UCSD extensions:
259 +
byte 0- 59 (60) name of original telemetry file
byte 60-119 (60) name of original L1A file
byte 120-123 ( 4) file pointer into L1A file
byte 184-187 ( 4) # pixels contributing to pedestal
byte 188-191 ( 4) # pixels contributing to dark current
byte 192-196 ( 4) # pixels in negative measles
byte 196-199 ( 4) # pixels in positive measles
byte 200-203 ( 4) # pixels in big measles
byte 204-207 ( 4) # pixels in cosmic rays
byte 208-211 ( 4) # pixels in big cosmic rays
byte 212-215 ( 4) residual intensity in squares
byte 216-219 ( 4) residual intensity in center group
byte 220-223 ( 4) standard deviation of pedestal
byte 224-227 ( 4) standard deviation of dark current
byte 228-231 ( 4) flags
MODIFICATION HISTORY:
OCT-2003, Paul Hick (UCSD/CASS)
Extracted from smei_buf_splitframe
JUN-2004, Paul Hick (UCSD/CASS)
Added room for name of another pattern file name.
Rearranged to put everything at proper boundaries.
MAR-2005, Paul Hick (UCSD/CASS)
Added code to fill hdr.sun,hdr.moon,hdr.venus,hdr.ra,hdr.dec
and hdr.angle, hdr.eclipse and hdr.shadow using JPL ephemeris
and Coriolis orbital elements run through sgd4.
Note that for the first real-time downloads of the
SMEI data the orbital elements will probably be out of date, so
especially hdr.moon and hdr.eclipse should be treated with suspicion
until this has been rerun with valid orbital elements.
MAR-2009, Paul Hick (UCSD/CASS)
Added checks for valid camera and mode values, and a check on
valid time when converting from binary header to a hdr structure.
When an invalid value is found, the integer -1 is returned
instead of a structure.
MAR-2011, Paul Hick (UCSD/CASS)
Bug fix. The julian_date entry in a binary header from an L1A file
was tested for equality against the time specified in the year,doy,
hour,min,sec fields. This led to the occasional rejection of
a header (testing real numbers for equalitiy is a bad idea after all).
The test now is that julian date needs to within 10 msec.
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added corrupt_frame keyword to be able to suppress printing of
of error_messages while recovery from corrupt frame is in progress
(this would potentially generate truckloads of messages.
Added error_message keyword.
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NAME:
smei_frm_darkfit
CALLING SEQUENCE:
PRO smei_frm_darkfit, tt, plotx=plotx
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CURVEFIT, FILEPATH, FindAllFiles, GetFileSpec, InitVar, IsTime, PlotCurve, TimeOp
TimeSet, TimeUnit, boost, flt_read, smei_frm_darkfnc, who_am_i
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NAME:
smei_frm_darkfnc
CALLING SEQUENCE:
PRO smei_frm_darkfnc, x, a, f, p
INCLUDE:
@compile_opt.pro
CALLED BY:
smei_frm_darkfit
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NAME:
smei_frm_drive
PURPOSE:
Return time range for content of SMEI data base
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_frm_drive, drive
INPUTS:
drive scalar or array[n]; type: integer or string
identified SMEI drive as integer n
or as string of type 'SMEIDBn'
If omitted all drives are used
OUTPUTS:
t array[2,n]; type: time structure
begin and end time of data on each drive
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, IsType, TimeSet, destroyvar, flt_read, flt_string, who_am_i
CALLED BY:
smei_hdr_update
COMMON BLOCKS:
common smei_filepath_save, checkdrives, sdat
PROCEDURE:
MODIFICATION HISTORY:
AUG-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_eclipse
PURPOSE:
Eclipse calculations
CATEGORY:
smei_frm_eclipse, hdr, /may2003
CALLING SEQUENCE:
PRO smei_frm_eclipse, hdr, $
may2003 = may2003 , $
nov2003 = nov2003 , $
jun2003 = jun2003 , $
apr2004 = apr2004 , $
oct2004 = oct2004 , $
apr2005 = apr2005 , $
mar2006 = mar2006 , $
sep2007 = sep2007 , $
aug2008 = aug2008 , $
jan2009 = jan2009 , $
jan2010 = jan2010 , $
earth = earth , $
orbit = orbit , $
loc = loc , $
runit = runit , $
area = area , $
camera = camera , $
_extra = _extra
INPUTS:
hdr array; type: structure
headers of SMEI frames returned from a
previous call. If hdr exists than the
optional input parameters are ignored.
OPTIONAL INPUT PARAMETERS:
/may2003, orbit=0 for eclipse on 31 May 2003 04:13
/may2003, orbit=-1 for eclipse on 31 May 2003 02:42
/nov2003 for eclipse on 23 Nov 2003 22:53
/apr2004 for eclipse on 19 Apr 2004 15:24
/apr2005 for eclipse on 08 Apr 2005 20:35
/mar2006 for eclipse on 29 Mar 2006 10:10
/sep2007
/aug2008 includes full eclipse
/jan2009
/jan2010
/jun2003 Coriolis in Earth shadow from 13:58:19 until 14:14:51
orbit=0 plots several orbits around time of maximum eclipse
orbit=-1 plots the earlier of the two eclipses usually seen by SMEI
orbit=1 plots the later of the two eclipses
OUTPUTS:
(Plot to screen)
hdr array; type: structure
headers of all SMEI frames processed
This can be used as input for subsequent
call to to bypass rereading of the frames.
OPTIONAL OUTPUT PARAMETERS:
loc=loc output from smei_frm_where
runit=runit output from smei_frm_where
area=area output from eclipsed_area
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, TimeGet, TimeLimits, TimeSet, TimeUnit, eclipsed_area, jpl_body
smei_frm_where, smei_property
PROCEDURE:
MODIFICATION HISTORY:
OCT-2004, Paul Hick (UCSD/CASS)
FEB-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added eclipses in sep 2007 and later.
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NAME:
smei_frm_findpoint
PURPOSE:
Return frames with specified locations in the fov
CATEGORY:
ucsd/camera/idl
CALLING SEQUENCE:
PRO smei_frm_findpoint, trange, $
_extra = _extra , $
hdr = hdr , $
theta = theta , $
ccd = ccd , $
list = list , $
camera = camera
INPUTS:
trange array[2]; type: time structure
time range of target frames
OPTIONAL INPUT PARAMETERS:
/degrees if set all angles are in degrees (default: radians)
The sky locations can be specified using any one of the methods
used in smei_frm_where. The simplest is:
points_radec array[2]; type: float
J2000 RA and dec of locations in the sky.
The units are degrees or radians depending on the
setting of keyword /degrees.
list=list scalar; type: string; default: none
name of an output file where to write the fully-qualified
file names of all SMEI frames containing the sky location.
OUTPUTS:
hdr=hdr array; type: structure
headers for all identified SMEI frames
theta=theta see smei_frm_where
ccd=ccd see smei_frm_where
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, InitVar, IsType, MEAN, TimeGet, TimeLimits, TimeOp, TimeSet, TimeUnit, boost
destroyvar, do_file, smei_coriolis, smei_frm_where, smei_property
CALLED BY:
grayburst
PROCEDURE:
> Check whole orbit starting at trange[0] for frames with the sky location
in it. If no frames are found, try the next orbit.
> If a transit of the sky location is found then determine the start
and duration of the transit. Use this to estimate when the transit
in the next orbit is.
MODIFICATION HISTORY:
NOV-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_flag
PURPOSE:
Manipulates hdr.flags entry in SMEI frm header
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
result = smei_frm_flag(flag [,flag=flag, names=names])
INPUTS:
hdr array; SMEI__FRM_HDR structure
OPTIONAL INPUTS
flag=flag array; type: SMEI_FRM_HDR structure or integer
OPTIONAL INPUT PARAMETERS:
The following flags are processed:
base_done
base_ok
eclipse
shadow
bad_quat
just_bad
anneal
tagmode
full_frame
shutter
dark_offset
flatfield
cosmic_rays
calibration
flat_enabled
led_enabled
bos_alert
OUTPUTS:
results array: type: SMEI_FRM_HDR structure or integer
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType, ibsetf, ibtestf
CALLED BY:
smei_frm_cvhdr, smei_frm_update
PROCEDURE:
Each keyword corresponds to a bit in the hdr.flags entry.
The values used here should be consistent with the value
in the Fortran include value smei_frm_hdr.h
MODIFICATION HISTORY:
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_flatfield
PURPOSE:
Get small or large-scale flatfield for the SMEI cameras.
CATEGORY:
camera/idl/field
CALLING SEQUENCE:
ff = smei_frm_flatfield(camera=camera [, /lsff)
INPUTS:
OPTIONAL INPUT PARAMETERS:
camera=camera scalar; type: integer; default: 1
camera number (1,2, or 3)
/lsff get large scale flatfield instead of
small scale flatfield.
OUTPUTS:
ff array[1272,256]; type: double
flatfield value; the flatfield is applied
by multiplying the uncorrected value by ff.
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; ROI definition
CALLS: ***
FILEPATH, InitVar, IsType, MagnifyArray, READFITS, SuperArray, smei_setup_roi
who_am_i
PROCEDURE:
SMALL SCALE (ON BOARD) FLAT FIELDS:
c1_ssff.fts.gz, c2_ssff.fts.gz, c3_ssff.fts.gz
For the small-scale flatfields, if the uncorrected CCD-readout is N ADUs,
then the flat field corrected read-out M follows by adding one to the
flatfield values and multiplying, i.e. with ff the array read from the
FTS file:
M = (1+ff)*N
The addition of 1 is already done in the output array
(i.e. 1+ff is returned).
LARGE SCALE FLAT FIELDS:
c1_lsff.fts.gz, c2_lsff.fts.gz, c3_lsff.fts.gz
For the large-scale flatfields, if the uncorrected readout is N ADUs, then
the flat field corrected readout M follows by dividing by the flat field
value, i.e. with ff the array from the FTS file:
M = N/ff
The inversion is already done in the output array (i.e. 1/ff is returned).
RAL TO SMEI MAPPING (applies to ssff and lsff files, NOT the lsffc files):
All FTS files contain float arrays of size 1280x600 ('RAL frame'). The SMEI
engineering mode (mode 0) frames have dimensions 1272x256. The pixels in a
SMEI frame are a subset of the pixels in a RAL frame. The RAL frame is
mapped to the SMEI frame by dropping the first 5 columns, then extracting
the next 1272 columns; and dropping the first 65, 59 and 61 rows for
cameras 1, 2 and 3, resp., then extracting the next 256.
Let:
n = 5, m = 65 for camera 1
n = 5, m = 59 for camera 2
n = 5, m = 61 for camera 3
Then in IDL (with 0-based array indices):
SMEI = RAL[n:n+1271,m:m+255]
or pixel-by-pixel:
SMEI[i,j] = RAL[n+i,m+j]
In Fortran (1-based array indices):
for j=1,256
for i=1,1272
SMEI[i,j] = RAL[n+i,m+j]
end for
end for
NORMALIZED FLAT FIELD CORRECTION (clsff):
c1_clsff.fts.gz, c2_clsff.fts.gz, c3_clsff.fts.gz
Contain arrays of size 1280x301 with numbers of order 1. As far as I can
tell these are based on the large-scale flat field files with a couple of
modifications:
- geometrical effects are taken out (cosine effect along long dimension due
to changing effective aperture size, and radial effect along the narrow
dimension
- a couple of 'bad pixels' are stamped out
Even though the arrays suggest they are in engineering mode they are
effectively in mode 2 (4x4 binning): numbers are identical in groups of 4x4.
To use them with the SMEI an offset needs to be taken into account different
from the large-scale flatfield discussed above: the first two columns need
to be dropped, and the first 16, 10 and 12 rows for cameras 1,2 and 3,
respectively.
So let:
n = 2, m = 16 for camera 1
n = 2, m = 10 for camera 2
n = 2, m = 12 for camera 3
Then use the same code as above for the large-scale flatfields.
MODIFICATION HISTORY:
JAN-2004, Paul Hick (UCSD/CASS)
NOV-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added the normalized flatfield corrections.
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NAME:
smei_frm_hbar
PURPOSE:
Detects horizontal features in SMEI frames with readout
lower than neigbouring rows (i.e. 'crazy frames')
CATEGORY:
ucsd/camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_frm_hbar, trange, $
length = length , $
_extra = _extra , $
roi_map = roi_map , $
moon = moon , $
sun = sun , $
venus = venus , $
bpos = bpos , $
bmap = bmap , $
hdr = hdr , $
bdepth = bdepth , $
blength = blength , $
dlength = dlength , $
pcount = pcount , $
excl_moon = excl_moon , $
excl_sun = excl_sun , $
excl_venus = excl_venus, $
degrees = degrees
INPUTS:
trange array[2]; type: time structure
array; type: string
if time structure of array this is passed to
smei_getfile to get a list of frame file names.
array[*,*,n]; type: numerical
image cube of n SMEI frames
OPTIONAL INPUT PARAMETERS:
length scalar; type: integer; default: 100
maximum length of horizontal feature searched for
blength scalar; type: integer; default: length
the return arrays bmap, bpos
provide information about horizontal features
of length 'blength' pixels and longer.
(if the maximum length horizontal feature is less
than 'blength' than the maximum length is used
for 'blength').
dlength scalar; type: integer: default: length
excl_moon array[4]; type: float or double
excl_sun array[4]; type: float or double
excl_venus array[4]; type: float or double
if the respective body is inside this exclusion zone
the tx-ty (direction cosine) plane then no check is
performed (and result -1 is returned)
Default units are radians (unless /degrees is set)
/degrees sets units of exclusion zones to degrees
If a 2D array is input as trange then additional header information
can be provided with the following keywords:
(these are ignored if trange is a time structure or string:
the information is extracted from the frame headers):
roi_map identifier for region of interest map used (usually 4)
moon location Moon
sun location Sun
venus location Venus
OUTPUTS:
result array[n]; type: long
length of longest horizontal feature in frame
OPTIONAL OUTPUT PARAMETERS:
pcount array[*,n]; type: long
number of pixels in horizontal bars at each stage
of the detection process
pcount[0,n]: # pixels with length 1 and longer
pcount[1,n]: # pixels with length 2 and longer
etc.
These output arguments refer to the last frame processes, so they are
useful only when processing a single frame:
bmap=bmap array[*,*]; type: bytarr
map of horizontal features with length 'blength' or
longer marked by one; zero everywhere else.
bpos=bpos array[*,*,n]; type: long
starting pixels of hor features with length 'blength'
or longer
If a bar is n > blength then n+1-blength
consecutive pixels will be marked in bmap.
bdepth=bdepth scalar; type: float
blength=blength scalar; type: integer
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro
CALLS: ***
ArrayLocation, InitVar, IsTime, IsType, LocalExtrema, MEAN, STDDEV, TimeUnit, destroyvar
smei_cam2angle, smei_frm_hbar_inside, smei_frm_read, smei_getfile, smei_property
smei_setup_roi, who_am_i
CALLED BY:
smei_findcrazy
PROCEDURE:
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_hbar_inside
PURPOSE:
(internal use by smei_frm_hbar only)
CALLING SEQUENCE:
FUNCTION smei_frm_hbar_inside, txy, tbox, body
INCLUDE:
@compile_opt.pro
CALLED BY:
smei_frm_hbar
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_hdr__define
PURPOSE:
Structure definition for frame header of SMEI .buf files
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
hdr = {smei_frm_hdr}
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_buf_getframe, smei_frm_summary, smei_frm_track, smei_getfile, smei_hdr_plot
PROCEDURE:
See Don Mizuno's, SMEI_CONVERT memo
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
Based on SMEI Convert 1.0 and 1.1
FEB-2005, Paul Hick (UCSD/CASS)
Rearranged order. Merged all times in single structure
elements. Added entry for exposure time. Added location
of venus. Removed all blank_double, blank_float,
blank_long and blank_short.
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added dark_average
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NAME:
smei_frm_info
PURPOSE:
Compiles statistics for list of frames
CATEGORY:
camera/idl/misc
CALLING SEQUENCE:
PRO smei_frm_info, hdrs, day_by_day=day_by_day
INPUTS:
hdrs array; type: smei_frm_hdr structure
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
(to screen)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, TimeGet, TimeOp, TimeUnit, smei_property
PROCEDURE:
Counts frames for each camera and mode.
Also distinguished between padded 'full-frame' data
and unpadded 'ROI' data.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_mask
PURPOSE:
Check whether camera 3 mask is active at specified time
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_frm_mask, tframe, mask=mask
INPUTS:
tframe character*(*) SMEI frame time in format YYYY_DOY_hhmmss
OUTPUTS:
smei_frm_mask_active
logical .TRUE. : bad pixel mask in use for specified time
.FALSE.: no bad pixel mask in use for specified time
cmask character*(*) mask time in format YYYY_DOY
This is used in the construction of the file
name for the mask.
CALLS: ***
FILEPATH, IsTime, SyncArgs, TimeSet, smei_filepath, txt_read
PROCEDURE:
A bad pixel mask is in effect during time periods hardcoded in this routine.
If the specified frame time tframe is inside one of these time periods then
the appropriate mask is returned. If not inside any one of the time periods
then a mask containing only the value 1 is returned.
MODIFICATION HISTORY:
MAR-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_ped
PURPOSE:
Calculate electronic pedestal offset for SMEI frames
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
R = smei_frm_ped,
INPUTS:
hdr
ff
OPTIONAL INPUT PARAMETERS:
pattern=pattern
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType, smei_property
SEE ALSO:
COMMON BLOCKS:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
OCT-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_read
PURPOSE:
Read SMEI frame
CATEGORY:
camera/idl/misc
CALLING SEQUENCE:
FUNCTION smei_frm_read, ff , $
source = source , $
head_room = head_room , $
hdr = hdr , $
silent = silent , $
error = error , $
nodata = nodata , $
ramdisk = ramdisk , $
raw = raw , $
allow_bad = allow_bad , $
ls_corrupt = ls_corrupt, $
rm_corrupt = rm_corrupt
INPUTS:
ff scalar; type: string
file name of SMEI frame
If no file type is specified then .fts.gz is assumed
If no directory is specified then the main
SMEI data base on smeidb is used.
OPTIONAL INPUT PARAMETERS:
source=source scalar; type: string
source directory of SMEI frames
/nodata if set, only read the frame header
(return value of img will be -1).
OUTPUTS:
img array[n,m]; type: integer
SMEI frame data
OPTIONAL OUTPUT PARAMETERS:
hdr=hdr array[1]; type: structure
frame header
error=error scalar; type: string
error string. Will be the null string if
file was read successfully.
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; ROI mask common block
CALLS: ***
FILEPATH, GetFileSpec, HEADFITS, InitVar, IsType, READFITS, TimeGet, TimeOp, TimeUnit
bin_read, do_file, hide_env, smei_filepath, smei_frm_cvhdr, smei_property
smei_setup_roi, timeposn, who_am_i
CALLED BY:
aurora, img_read, smei_buf_prep, smei_frm_hbar, smei_frm_track, smei_getfile
stardistance
SEE ALSO:
SIDE EFFECTS:
RESTRICTIONS:
Andy renames .nic files to .raw to look at them in Adobe Photoshop.
For now we assume that all .raw files are indeed .nic files in disguise.
PROCEDURE:
MODIFICATION HISTORY:
MAY-2003, Paul Hick (UCSD/CASS)
JUN-2003, Paul Hick (UCSD/CASS)
Added check for missing file extension.
JUL-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added /ramdisk keyword
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NAME:
smei_frm_rebin
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; ROI mask common block
EXTERNAL:
CALLS: ***
InitVar, MagnifyArray, smei_setup_roi, who_am_i
SEE ALSO:
COMMON BLOCKS:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
APR-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_smoothdark
PURPOSE:
Add extra Fits keyword to frame header containing
smoothed dark current (boxcar average in the time domain)
CATEGORY:
ucsd/camera/idl/frm
CALLING SEQUENCE:
PRO smei_frm_smoothdark, trange, $
dbsource = dbsource , $
test = test , $
silent = silent
INPUTS:
trange array[2]; type: string or time structure
time range to be smoothed
(internally the range is extended to include
enough frames to get the averages near the
beginning and end of the time range)
OPTIONAL INPUT PARAMETERS:
dbsource = dbsource
scalar; type: string; default; SMEIDB?
indicates location of frames (either SMEIDB? or SMEIDB?)
passed to smei_hdr_update and smei_hdr_get
/test if set, the SMEI frames are not updated
(i.e. nothing is modified, just output is written
to screen)
OUTPUTS:
(Keyword SDARK0 added to Fits header)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FXHMODIFY, GetFileSpec, InitVar, IsType, MEAN, POLY_FIT, TimeGet, TimeLimits, TimeOp
TimeSet, TimeUnit, hide_env, smei_hdr_get, smei_hdr_update
CALLED BY:
smei_mkbase
PROCEDURE:
TimeSet(['2006_004','2007_003']
Note that the frame names and dark currents are pulled out
of the header database. This means that, after a period
has been "based" using smei_base, the corresponding
header files need to be updated first with
smei_hdr_update before this procedure is run to
calculate the smoothed dark currents (which are than
inserted into the frames).
MODIFICATION HISTORY:
AUG-2008, Paul Hick (UCSD/CASS)
OCT-2008, Paul Hick (UCSD/CASS)
Added call to smei_hdr_update to ensure that the
header files are up-to-date before calculating
smoothed dark currents
JAN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added silent=silent to smei_hdr_update call
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NAME:
smei_frm_summary
PURPOSE:
Plots time series for various basic parameters in SMEI data frames
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
PRO smei_frm_summary, frame, printer=printer, zbuffer=zbuffer, $
destination=destination, _extra=_extra, $
nfill_control=nfill_control, nbad_control=nbad_control, $
hdr=hdr, silent=silent
INPUTS:
frame array[1], or array[2]; type: time structure
begin and end time for time range to be plotted.
If only a start time is given then the end time is taken
to be the start time, plus one day.
OPTIONAL INPUT PARAMETERS:
source=source
destination=destination
camera=camera
OUTPUTS:
(to png file)
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_frm_hdr__define
CALLS: ***
AngleRange, BadValue, CheckDir, FILEPATH, InitVar, IsTime, IsType, MEAN, PlotCurve, STDDEV
TimeGet, TimeLimits, TimeOp, TimeScale, TimeSet, TimeSystem, TimeUnit, TimeXAxis, WhatIs
destroyvar, get_page, jpl_body, jpl_phase, set_page, smei_frm_track, smei_frm_where
smei_getfile, smei_property, sphere_distance
COMMON BLOCKS:
PROCEDURE:
TO DO:
- Dark current subtraction does not take slope from row to row into account
(especially important for camera three)
- Definition of SAA needs improvement
MODIFICATION HISTORY:
APR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_track
PURPOSE:
Calculates frame baseline (pedestal, dark current,
average intensity in squares and center group) using
information from previously processed frames.
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
FUNCTION smei_frm_track, frm, count , $
nfill_control = nfill_control , $
nbad_control = nbad_control , $
ff = ff , $
hdr = hdr , $
img = img , $
reset = reset , $
status = status, $
silent = silent
INPUTS:
frm scalar; type: integer
frame number to be processed
count scalar; type: integer
total # frames to be processed
(used to dimension a several arrays maintained internally
in common block, and used to clear the common block whe
frm becomes equal to count (i.e. when all frames have been
processed).
OPTIONAL INPUT PARAMETERS:
/silent suppress run-time information
(passed to smei_frm_base)
/reset re-initialize the current camera/mode combination
nfill_control=nfill_control
scalar; type: integer; default: (set in smei_frm_base)
# good frames used to build reference base values
(passed to smei_frm_base)
ff=ff
hdr=hdr
img=img
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
hdr = hdr
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_frm_hdr__define
CALLS: ***
ArrayLocation, InitVar, IsType, TimeGet, TimeUnit, destroyvar, smei_frm_base
smei_frm_read, smei_property
CALLED BY:
smei_frm_summary
COMMON BLOCKS:
common smei_frm_track_save, ncount, cam_fulls, cam_start, cam_nail, frm_ok, cameras, modes, step
PROCEDURE:
MODIFICATION HISTORY:
MAY-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_frm_update
PURPOSE:
Update headers of SMEI Fits frames
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
PRO smei_frm_update, cframe, $
shutter_open=shutter_open, $
bad_quat=bad_quat, $
new_quat=new_quat, $
just_bad=just_bad, $
on=on, $
off=off
INPUTS:
cframe scalar; type: string
fully-qualified name of SMEI frame
OPTIONAL INPUT PARAMETERS:
/shutter_open if set the value of the 'shutter-open' flag is changed
/just_bad if set the value of the 'just_bad' flag is changed
/on by default the flag setting is reversed.
/on explicitly sets the flag to 'on'
/off /off explicitly sets the flag to 'off'
new_quat=new_quat
array[4]; type: double
new quaternion to be put in frame header.
(if new_quat is set, then the bad_quat flag is
explicitly set to zero).
OUTPUTS:
Changes are written directly into the disk file
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FXHMODIFY, GetFileSpec, InitVar, IsType, SetFileSpec, smei_frm_flag, smei_getfile
CALLED BY:
qnew_2007_013
PROCEDURE:
Only one header entry can be changed in one frame at a time.
MODIFICATION HISTORY:
MAR-2004, Paul Hick (UCSD/CASS)
JUL-2006, Paul Hick (UCSD/CASS)
Added /on and /off keywords
Added /bad_quat keyword
OCT-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added new_quat keyword
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NAME:
smei_frm_where
PURPOSE:
Calculate location of Coriolis and pointing of cameras
for specified time and spacecraft quaternion.
Check whether specified location (RA,dec in J2000) is
inside the field of view.
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
smei_frm_where, hdr
INPUTS:
hdr can be one of the following
array[n]; type: frame header structure
array of headers for target frames
array[2]; type: time structure
time range (passed to smei_getfile)
scalar or array; type: string
list of file names of target frames. These can
be fully-qualified. If it only consists of a filename
(e.g. c2m2_2004_101_121212) then the SMEI data base
is used.
if 'hdr' is not specified then the dialog_pickfile
dialogis used to select files. If two files are
selected, then the file names are passed to
smei_getfile to find all frames in between the
implied time range. If only one file or more than two
files are selected, then the indicated frames are
processed.
OUTPUT PARAMETERS:
hdr array[n]; type: frame header structure
array of headers for target frames
(if the input 'hdr' was a time range or a list of
fully-qualified filenames)
OPTIONAL INPUT PARAMETERS:
/open_shutter selects frames with shutter open
/closed_shutter selects frames with shutter closed
(this checks the 'shutter_open' flag in the frame
header; by default the 'shutter_open' flag is NOT checked)
mode=mode selects data for specified mode (0,1 or 2) only.
/degrees if set all angles are in degrees (default: radians)
/spacecraft if set then sky locations of all bodies in the planetary
JPL ephemeris and asteroid USNO ephemeris are calculated
from a spacecraft-centric perspective (by default the locations
are geocentric). The difference is probably only significant
for the Moon (e.g. it matters for eclipse calculations).
The location of the spacecraft is approximate only. It assumes
that the spacecraft is at geocentric distance of 6367+850 km.
The location in geocentric RA and dec is derived from the
spacecraft quaternion assuming the spacecraft is in its default
attitude with the s/c axis along the nadir-zenith direction (i.e.
if breaks down during attitude changes.
source=source scalar; type: string
passed to smei_getfile
camera=camera scalar; type: integer
passed to smei_getfile
show=show scalar; type: integer: default: 0
1: print info for frames and all bodies for all frames
2: print info for frames and all bodies, but only for
frames that contain one or more bodies.
3: print SMEI frame info only for all frames
-1:
outfile=outfile scalar; type: string
fully-qualified name of output file
Captures same output of 'show' to the specified file
If outfile is specified and 'show' is not set then
show=1 is assumed.
points_radec array[2,n]; type: float
J2000 RA and dec of locations in the sky.
The units are degrees or radians depending on the
setting of keyword /degrees.
points_name array[n]; type: string
list of ascii names for all sky locations
in 'points_radec'. If not specified, then '1','2',
etc. is used.
Instead of specifying points_radec sky locations can be identified by
the following keywords. /jpls depends on the JPL planetary ephemeris.
/stars depends on the bright star list compiled by Susan Rappoport and
Andy Buffington, /usnos depends on the USNO ephemeris,and
/mpcs depends on ephemerides from the Minor Planet Center homepage.
Locations in the sky are specified as J2000 RA and dec.
/jpls checks for planets, Sun and Moon (using JPL ephemeris)
Optional if jpl_list is specified.
/stars checks for stars on SMEI star list (currently cut off at
SMEI magnitude 'm_max' (default: 4.5,
which leaves about 1000 stars).
Optional if star_list is specified.
/usnos checks for asteroids on the USNO ephemeris
Optional if usno_list is specified.
jpl_list=jpl_list array; type: integer; default: sun,planets and moon
list of planets to check.
Usually set up by a call to jpl_body
star_list=star_list array; type: structure
list of stars to check. Usually set up by call to
smei_star_info(/get_struct)
usno_list=usno_list array; type: integer or string; default: all asteroids
list of asteroids to be checked. Usually set up by
call to usno_body
mpc_list=mpc_list array; type: integer or string; default: all MPC bodies
list of MPC bodies to be checked. Usually set up by
call to mpc_body
/all by default only information about points strictly inside
the fov is given (and output in the OPTIONAL OUTPUT
PARAMETERS). Setting /all will return
information about all points.
m_max=m_max scalar or array[2]; type: float
if scalar then only stars from the SMEI catalogue
brighter then this cut-off SMEI magnitude are used.
OPTIONAL OUTPUT PARAMETERS:
sc_loc = sc_loc array[3,n]; type: double
best guess at Coriolis location in geographic
coordinates (derived from quaternion, assuming that
the spacecraft is in its default attitude with
z-axis pointing to nadir and x-axis along the
velocity vector).
array[0,*]: geographic longitude
array[1,*]: geographic latitude
array[2,*]: don't know exactly, but it's
positive when Coriolis is heading north;
negative when heading south.
pointing = pointing array[3,n]; type: double
camera pointing in equatorial coordinates
array[0,*]: right ascension of optical axis
array[1,*]: declination of optical
array[2,*]: camera tilt relative to equat north
nobject=nobject scalar; type: integer
# sky objects
if nobject=0 then none of the output arguments
below will exist.
name = name array[nobject]; type: string
names of bodies for which information is given
inside = inside array[nobject,n]; type: byte
0 if inside fov; 1 if outside fov
loc = loc array[3,nobject,n]; type: float
equatorial coordinates of all bodies in 'name'
array[0,*,*]: right ascension
array[1,*,*]: declination
array[2,*,*]: distance (for stars and RA-dec
pairs this will be 1)
runit = runit array[3,nobject,n]; type: double
locations in the sky of planets, asteroids or stars,
as unit vectors in the UCSD camera frame
ccd = ccd array[2,nobject,n]; type: double
CCD locations of points in the sky. These are the
values after applying Andys' formulae.
array[0,*,*]: x coordinate
array[1,*,*]: y coordinate
mags = mags array[nobject,n]; type: float
apparent SMEI magnitude. This is only available
for the stars in the SMEI star catalogue.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, AngleUnits, CV_COORD, CombineRotations, CvRotation, CvSky, InitVar, IsTime
IsType, REVERSE, SuperArray, TimeGet, ToDegrees, ToRadians, WhatIs, boost, cvsmei
destroyvar, jpl_body, jpl_eph, mpc_body, mpc_eph, sgp4_eph, smei_cam2angle
smei_cam_quaternion, smei_getfile, smei_hdr_get, smei_property, smei_star_info
usno_body, usno_close, usno_eph
CALLED BY:
grayburst, maygeometry, qImage_cw_DrawEphem, qImage_cw_Where, smei_frm_eclipse
smei_frm_findpoint, smei_frm_summary, smei_hdr_plot, stardistance
EXAMPLE:
EXAMPLE 1:
Check where Mars is inside FOV between 2:00 and 2:30 on 2003 doy 67.
The frames are read from the default location for the SMEI data.
hdr = timeset(yr=2003, doy=67, hr=2, min=[0,30])
smei_frm_where, hdr, show=1, jpl_list=jpl_body(/mars)
hdr is now filled with the headers for all frames in the specified
time range. Subsequent calls with this header will bypass reading of frames.
EXAMPLE 2:
Given an array with frame names (e.g. read from a file), create a file
with information about the position of the Sun.
If 'file' contains records of the form c2m2_2003_101_121212 with frames
for camera 2 only:
status = txt_read(file, frames)
smei_frm_where, frames, jpl_list=jpl_body(/sun), /all, $
/longformat, outfile='sun.txt'
The file sun.txt is created in the working directory.
PROCEDURE:
For single frames retrieve the header first with smei_frm_read, and
use it as input. This circumvents the potentially very slow
call to smei_getfile.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
OCT-2004, Paul Hick (UCSD/CASS)
Added rtheta keyword.
OCT-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Replaced approximate calculation of spacecraft location based
on quaternion to more accurate location based on orbital elements.
Replaced stheta and rtheta by runit keyword. The function
smei_cam2angle can be used to convert the unit vectors to angles.
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NAME:
smei_frm_write
PURPOSE:
Write SMEI data into nic file
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
status = smei_frn_write(hdri, data, filename, count=count)
INPUTS:
hdri array[1]; type: frame header structure
frame header for frame to be written to file
data array[n,m]; type: unsigned integer (??)
data to be written
filename scalar; type: string
fully-qualified name for output file
OPTIONAL INPUT PARAMETERS:
count array[3]; type: integer
file counters; one or more of the counters are incremented by one
count[0]: # frames written to disk as .nic or .fits file
count[1]: # frames skipped because file already exists
count[2]: # frames with times earlier than the most recent frame
that are written to disk (these should be frames from the second dump;
if the second dump contains the same frames as the first the number
of these frames should be small)
OUTPUTS:
count array[3]; type: integer
updated file counters (only count[0] is updated)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, GetFileSpec, IsType, WRITEFITS, hide_env, smei_frm_cvhdr
CALLED BY:
smei_buf_get, smei_buf_mget
RESTRICTIONS:
If /split_dir is set then a 'mkdir --parents' is spawned to to create subdirectories,
and gzip is spawned to compress files. This will probably work under Linux, but not
in Windows without some modifications.
PROCEDURE:
This thing still needs an I/O error handler
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS)
MAY-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added explicit check for existence of directory
and create it if not.
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NAME:
smei_fts_read
PURPOSE:
Read Fits file
CALLING SEQUENCE:
status = smei_fts_read(File, Array, errormessage=errormessage)
INPUTS:
File string file name
OPTIONAL INPUT PARAMETERS:
header=header
if set then only the Fits header is read and returned
in 'Hdr'. The data array is set to -1.
OUTPUTS:
status 0: some error occurred (check 'errormessage')
1: file properly read
Array array[n,m]
2D array of requested type
if something goes wrong or /header was set then
Array = -1 is returned
Hdr Fits header array
OPTIONAL OUTPUT PARAMETERS:
errormessage
scalar; type: string
Contains null string if file was read succesfully
Contains error message if an error occurred
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
HEADFITS, InitVar, IsType, READFITS, do_file, gunzip_file
PROCEDURE:
Wrapper for the readfits.pro procedure in SSW.
The SSW version decompresses Fits file in place, which won't work
if the gzipped version is stored on a read-only file system.
This wrapper unzips the file into a temporary file using
gunzip_file and takes care of cleaning up the temporary file.
MODIFICATION HISTORY:
JUL-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_getfile
PURPOSE:
Get list of file names for all files (CCD frames or skymaps)
in specified time range
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
FUNCTION smei_getfile, wanted_file, $
nodialog= nodialog , $
usetime = usetime , $
exists = exists , $
exact = exact , $
camera = camera , $
mode = mode , $
count = count , $
tt = tt , $
source = source , $
nodig = nodig , $
science_mode = science_mode , $
engineering_mode = engineering_mode , $
smoothdark = smoothdark , $
prefer_smoothdark= prefer_smoothdark, $
chronological = chronological , $
get_hdr = get_hdr , $
hdr = hdr , $
get_map = get_map , $
map = map , $
silent = silent , $
ramdisk = ramdisk , $
ls_corrupt=ls_corrupt,$
rm_corrupt=rm_corrupt
INPUTS:
wanted_file array[1], or array[2]; type: time structure
begin and end time for requested time range
If only a start time is given then the end time is
taken to be the start time, plus one day.
If "wanted_file" is not defined than the IDL pickfile
dialog is called
OPTIONAL INPUT PARAMETERS:
/exists should only be used if "wanted_file" contains names
of files known to exist (the procedure skips
straight to the read section).
/usetime should only be used with "wanted_file" containing
sensible SMEI file names. The times, mode and
camera fields are extracted, and used as if
input through "wanted_file" (time), "camera" and
"mode" (override by explicitly setting mode and
camera, if necessary)
/nodialog for string input of file names (possible a scalar
containing a wildcard) the dialog_pickfile is
used to select file. If /nodialog is set then
file_search is used instead).
source=source scalar; type: string; default: SMEIDB?
root directory of smei data
camera=camera scalar, or array[n]; type: integer
camera number (1,2 or 3); if set only filees for the
specified camera(s) are extracted.
mode=mode scalar, or array[n]; type: integer or string; default: [0,1,2]
if set then only retrieve files for specified mode(s).
/get_hdr return file headers
/get_map return a pointer to the maps (CCD frames or skymaps)
/science_mode (for skymaps only)
selects science mode orbits only
/engineering_mode selects engineering mode orbits only
/smoothdark selects orbits with smoothed dark current
(only can pick up camera 3 science_mode orbits)
/prefer_smoothdark removes orbits with dark current NOT smoothed if
the matching orbit with dark current smoothed
is also present
OUTPUTS:
Result array[count]; type: string or smei_frm_hdr structure
fully-qualified file names for all files
if no files are found (count=0) then ff is the null string
if /get_hdr is set then the headers are returned instead.
if /get_map is set then the file data are returned instead
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
# files located
tt=tt array[count]; type: time structure
file times (i.e. the return value of
timeposn(Result,/extract))
hdr=hdr array[count]; smei_frm_hdr structure
file headers
map=map array[count]; heap pointer
file data
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, FindAllFiles, GetFileSpec, InitVar, IsTime, IsType, TimeGet
TimeLimits, TimeOp, TimeSet, TimeSystem, TimeUnit, boost, destroyvar, flt_string
hide_env, os_separator, smei_coriolis, smei_filename, smei_filepath, smei_frm_read
smei_orbit_get, smei_sky_read, timeposn, unique_only, where_common
EXTERNAL:
smei_frm_hdr__define
CALLED BY:
maygeometry, psfn, qImage_cw_Property, qsmei_hdr, skyd_version, smei_base_testcase
smei_buf_getframe, smei_findpnt, smei_frm_cp, smei_frm_hbar, smei_frm_summary
smei_frm_update, smei_frm_where, smei_hdr_make, smei_orbit_stats
smei_shutterwrong, smei_sky, smei_sky_atlocation, smei_sky_read, smei_sky_track
smei_star_fitone, smei_star_remove, smei_zld_remove [1]
PROCEDURE:
MODIFICATION HISTORY:
APR-2003, Paul Hick (UCSD/CASS)
OCT-2003, Paul Hick (UCSD/CASS)
Added /get_hdr and hdr=hdr keywords
FEB-2004, Paul Hick (UCSD/CASS)
Added /get_map and map=map keywords
MAY-2004, Paul Hick (UCSD/CASS)
Fairly substantial rewrite of a crappy routine.
Modified to reflect new directory structure of SMEI data base
(frames are now organized in a separate directory for each
doy of year, with subdirectories for each of the cameras)
JUL-2004, Paul Hick (UCSD/CASS)
Added /ramdisk keyword. Bug fix on processing of mode keyword.
SEP-2004, Paul Hick (UCSD/CASS)
Added code to select frames for a specific mode by checking the
file name first. If the mode is encoded in the file name this
speeds up the selection considerably.
AUG-2006, Paul Hick (UCSD/CASS)
Removed some dead code that dates back to when the mode was not
yet encoded in the filename for SMEI CCD frames.
Generalized interpretation of mode keyword: if set to a string
than skymaps will be processed, instead of SMEI CCD frames.
OCT-2007, Paul Hick (UCSD/CASS)
Changed loop variable from short to long integer.
FEB-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Fairly substantial revision. The procedure now also locates
skymaps, hdr and png files efficiently.
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NAME:
smei_hdr_c3maskupload
PURPOSE:
Best effort at determining upload times for C3 "bad-pixel" masks
CATEGORY:
camera/idl/hdr
CALLING SEQUENCE:
FUNCTION smei_hdr_c3maskupload, trange, time=time, name=name, status=status
INPUTS:
trange array[2]; time structure or valid time string
start and end time
OUTPUTS:
result scalar; type: integer
number of uploads in specified time period
OPTIONAL OUTPUT PARAMETERS:
time array[result]; type: time structure
upload times
name array[result]; type: string
name of "bad-pixel" mask
status array[result]; type: byte
0: upload failed
1: upload succesfull
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType, TimeGet, TimeSet, TimeUnit, destroyvar
CALLED BY:
smei_hdr_plot
PROCEDURE:
Information mostly from SMEI logs, plus some additional
information scattered around in the code, primarily
the Fortran routine smei_frm_c3mask_active.f
MODIFICATION HISTORY:
JUN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_hdr_get
PURPOSE:
Reads Fits binary tables containing all SMEI frame headers
CATEGORY:
ucsd/camera/idl/frm
CALLING SEQUENCE:
PRO smei_hdr_get, tt , $
source = source , $
destination = destination , $
camera = camera , $
mode = mode , $
get = get , $
time = time , $
hdr = hdr , $
one = one , $
two = two , $
three = three , $
four = four , $
five = five , $
six = six , $
seven = seven , $
dbname = dbname , $
dbsource = dbsource , $
count = count , $
silent = silent , $
exact = exact
;_extra = _extra
INPUTS:
tt array[2]; standard time structure
indicates time range for which SMEI frame are to
be processed. Can be a time structure, valid time string,
or SMEI orbit numbers.
OPTIONAL INPUT PARAMETERS:
source=source scalar; type: string
either a single Fits file containing frame headers in binary
table form, or a directory where these files are located.
If a directory is specified then the Fits files MUST contain
frame headers organized in daily files
destination=destination
scalar; type: string
only used if /write or /overwrite are set
destination directory for Fits binary table file
camera=camera scalar; type: integer (1,2,3)
camera for which headers are to be extracted
If not specified, camera 1 is used.
mode=mode scalar; type: integer (0,1,2); default: none
only frames for specified mode are extracted
get=get scalar or array; type: string
list of tag names of the {smei_frm_hdr} structure
to be extracted in the one,..,seven keywords
(to get a list of valid entry, type 'smei_hdr_get' at
the IDL prompt).
dbsource=dbsource
only used if output arg 'dbname' is requested
passed to smei_filepath
scalar; type: string; default: SMEIDB?
location of SMEI data frames (usually SMEIDB? or SMEIDC?)
OUTPUTS:
time=time array; type: standard time structure
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
number of frames found
hdr=hdr complete header
one=one Extracted keywords in the order specified in 'get'
two=two
three=three
four=four
five=five
six=six
seven=seven
dbname array; type: string
list of fully-qualified frame file name in SMEI database
specified in 'dbname'.
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_frm_hdr
CALLS: ***
BadValue, CheckDir, FILEPATH, FXBCLOSE, FXBOPEN, FXBREAD, InitVar, IsTime, IsType, TimeGet
TimeLimits, TimeOp, TimeSet, TimeUnit, boost, destroyvar, hide_env, smei_filename
smei_filepath
CALLED BY:
qnew_2007_013, qsmei_hdr, smei_findcrazy, smei_frm_smoothdark, smei_frm_where
smei_hdr_plot, smei_mkcal, smei_mkorb, smei_orbit_stats, smei_shutterwrong, tbad
tplot
SEE ALSO:
smei_hdr_make
PROCEDURE:
MODIFICATION HISTORY:
JUN-2005, Paul Hick (UCSD/CASS)
FEB-2007, Paul Hick (UCSD/CASS)
Bug fix(?). Variable mode was used in two different roles
when dbname was set.
SEP-2008, Paul Hick (UCSD/CASS)
Added check for presence of requested "get" keyword.
If not present, then an array of NaNs is returned.
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Modified processing of input time range to allow
specification of SMEI orbit numbers.
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NAME:
smei_hdr_make
PURPOSE:
Writes Fits binary tables containing all SMEI frame headers
CATEGORY:
ucsd/camera/idl/frm
CALLING SEQUENCE:
PRO smei_hdr_make, tt, $
overwrite = overwrite , $
source = source , $
destination = destination , $
camera = camera , $
get = get , $
count = count , $
remote = remote , $
silent = silent
;_extra = _extra
INPUTS:
tt array[2]; standard time structure
indicates time range for which SMEI frame are to
be processed
OPTIONAL INPUT PARAMETERS:
/overwrite if SET a binary Fits table is overwritten if it exists
By default existing files are NOT overwritten.
The file name will have the form c#hdr_YYYY_DOY_hhmmss.fts
where #=1,2,3 is the camera number.
Existing files are overwritten
source scalar; type: string
source of SMEI frame files (passed to smei_getfile)
(usually set to SMEIDB? or SMEIDC?)
destination scalar; type: string
destination directory for Fits binary table file
remote=remote scalar; type: string; default: none
if present, is combined with destination to build
the destination as <remote>:<destination>
(usually "remote" is set to the computer hosting
the header database when this routine is executed
on another computer)
camera scalar; type: integer (1,2,3)
only camera one frames are processed. By default all three
cameras are processed and headers are written into three
separate files, one for each camera.
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
number of headers written into Fits binary table (all cameras
combined, if more than one camera was processed).
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_frm_hdr
CALLS: ***
CheckDir, FILEPATH, FXADDPAR, FXBADDCOL, FXBCREATE, FXBFINISH, FXBHMAKE, FXBWRITM
FXHMAKE, FXWRITE, GetFileSpec, InitVar, IsTime, IsType, TimeGet, TimeOp, TimeSet, TimeUnit
hide_env, smei_getfile, smei_property
CALLED BY:
smei_hdr_update
SEE ALSO:
smei_hdr_get
PROCEDURE:
MODIFICATION HISTORY:
JUN-2005, Paul Hick (UCSD/CASS))
JAN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword silent=silent to smei_getfile call
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NAME:
smei_hdr_plot
PURPOSE:
Plots time series for various basic parameters in SMEI data frames
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
PRO smei_hdr_plot, tt , $
destination = destination , $
camera = camera , $
silent = silent , $
printer = printer , $
remote = remote , $
_extra = _extra
INPUTS:
tt array[2]; type: time structure
time range to be updated
OPTIONAL INPUT PARAMETERS:
destination=destination
remote=remote scalar; type: string; default: none
if present, is combined with destination to build
the destination as <remote>:<destination>
(usually "remote" is set to the computer hosting
the header database when this routine is executed
on another computer)
camera=camera
OUTPUTS:
(to png file)
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_frm_hdr__define
CALLS: ***
AngleRange, BadValue, CheckDir, FILEPATH, FXPAR, HEADFITS, InitVar, IsType, MEAN
PlotCurve, PlotCurves, SFLOAT, STDDEV, TimeGet, TimeLimits, TimeOp, TimeScale, TimeSet
TimeSystem, TimeUnit, TimeXAxis, UNIQ, boost, destroyvar, do_file, get_page, gridgen
hide_env, init_contiguous_group, jpl_body, jpl_phase, next_contiguous_group
set_page, smei_filename, smei_filepath, smei_frm_where, smei_hdr_c3maskupload
smei_hdr_get, smei_orbit_get, smei_orbit_set, smei_property, sphere_distance
CALLED BY:
smei_hdr_update
PROCEDURE:
- Definition of SAA needs improvement
MODIFICATION HISTORY:
SEP-2005, Paul Hick (UCSD/CASS)
OCT-2007, Paul Hick (UCSD/CASS)
Added PlotCurve calls to shade periods with
bad quaternions.
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added markers for mask uploads (cam 3 only) and anneals.
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NAME:
smei_hdr_update
PURPOSE:
Update Fits binary tables containing SMEI frm headers or time series plots based
on Fits binary tables.
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
PRO smei_hdr_update, tt , $
source = source , $
pscmd = pscmd , $
destination = destination , $
camera = camera , $
silent = silent , $
all = all , $
drive = drive , $
update = update , $
plotx = plotx , $
force = force , $
remote = remote
INPUTS:
tt array[2]; type: time structure
time range to be updated
OPTIONAL INPUT PARAMETERS:
all=all if set the whole SMEI data base is updated (overrides 'tt')
drive=drive scalar; type: integer
if set the corresponding drive is processed (overrides 'tt' and /all)
source=source scalar; type: string; default: SMEIDB?
directory indicating source of SMEI data frames (parameter is
passed to smei_filepath)
(usually SMEIDB? or SMEIDC?)
destination=destination
scalar; type: string; default: $SSWDB_SMEI/cat/hdr
directory where Fits binary tables are stored
remote=remote scalar; type: string;
defaults: none if $HOST != smei.ucsd.edu
'soft@smei' if $HOST == smei.ucsd.edu
if present, is combined with destination to build
the destination as <remote>:<destination>
(usually "remote" is set to the computer hosting
the header database when this routine is executed
on another computer; passed to smei_hdr_make and
smei_hdr_plot)
camera=camera scalar or array[n]; type: integer; default: [1,2,3]
cameras to be updated
plotx=plotx 0: update hdr data base of Fits binary tables
1: update time series plots based on the Fits binary tables
(the "png" files)
2: do both
/force will unconditionally update Fits tables or png files
silent=silent suppresses informational messages if set to > 0
OUTPUTS:
Updated Fits binary tables.
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXPAR, FindAllFiles, HEADFITS, InitVar, IsType, TimeGet, TimeLimits, TimeOp
TimeSet, TimeSystem, TimeUnit, hide_env, is_running, smei_filepath, smei_frm_drive
smei_hdr_make, smei_hdr_plot, timeposn
CALLED BY:
smei_frm_smoothdark, smei_mkbase, smei_mkcal, smei_mkorb_auto, tplot
PROCEDURE:
MODIFICATION HISTORY:
AUG-2005, Paul Hick (UCSD/CASS)
OCT-2006, Paul Hick (UCSD/CASS)
Added pscmd keyword
FEB-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Default destinations are now set through calls to
smei_filepath instead of hardcoding them here.
JAN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
For cam 3, added check of timestamp of orb files
to decide whether an update is required for a png file.
If $HOST != smei.ucsd.edu then keyword remote is now
initialized to 'soft@smei', if not specified explicitly.
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NAME:
smei_i2m
CALLING SEQUENCE:
FUNCTION smei_i2m, from_ms=from_ms, from_bb=from_bb
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType
CALLED BY:
PRO bold, smei_findobj, smei_star_fit, smei_star_show
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NAME:
smei_last_tle
PURPOSE:
Retrieves time of most recent Coriolis tle
CALLING SEQUENCE:
FUNCTION smei_last_tle
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, SFLOAT, TimeFixYear, TimeSet, hide_env, txt_read
CALLED BY:
smei_mkbase, smei_mkcal_auto, smei_mkorb_auto, smei_mksky
RESTRICTIONS:
PROCEDURE:
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_mkbase
PURPOSE:
Used to run smeidb_base and smei_hdr-update
for whole days of frames in $SSWDB_SMEI
CALLING SEQUENCE:
PRO smei_mkbase, $
camera = camera , $
lastdays = lastdays , $
days_to_cal = days_to_cal , $
ignore_block= ignore_block, $
force = force , $
test = test
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, FindAllFiles, InitVar, IsType, TimeGet, TimeOp, TimeSet, TimeUnit, boost
destroyvar, hide_env, smei_blocked, smei_filename, smei_filepath
smei_frm_smoothdark, smei_hdr_update, smei_last_tle, smei_orbit_stats, txt_read
RESTRICTIONS:
Status files are written to $SSWDB_SMEI on the smei server
over ssh. If this procedure is run as part of a cronjob
then login without password to the smei server should
be possible
PROCEDURE:
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
JUN-2010, John Clover (UCSD/CASS)
Increasing default threshold for camera 2
ped_median_excess from 6 to 8.
SEP-2010, John Clover (UCSD/CASS)
Changed defaults for camera 1 and camera 2
ped_median_excess 8 8
dark_cut 14 14
dark_max_ratio 1.05 1.05
These likely still need tweaking
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NAME:
smei_mkc3mask
PURPOSE:
Converts J. Tappins mask file into format needed by smei_cal
CATEGORY:
CALLING SEQUENCE:
PRO smei_mkc3mask, last_only=last_only
OPTIONAL INPUTS:
/last_only processes only the most recent mask
(useful when adding a mask)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, WhatIs, flt_read, flt_string, smei_filepath
PROCEDURE:
The first line in James' files contain the array dimensions
(1272 by 256). This line should be commented with a semi-colon first.
The files have rows of 19 numbers (values 0 and 1 only)
Each row of 1272 mask values is stored in 67 rows with the last
row missing one number: 66*19+18=1272
Files are written in format (1272I1)
MODIFICATION HISTORY:
FEB-2007, Paul Hick (UCSD/CASS)
SEP-2007, Paul Hick (UCSD/CASS)
Added mask 2007_237.
MAR-2007, Paul Hick (UCSD/CASS)
Added mask 2008_023.
OCT-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added mask 2008_226. Added /last_only keyword
OCT-2009, John Clover (UCSD/CASS; jclover@ucsd.edu)
Added mask 2009_260
XXX-2010, John Clover
Added mask 2010_098
OCT-2010, John Clover
Added mask 2010_259
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NAME:
smei_mkcal
PURPOSE:
Create "closed shutter" calibration pattern
CALLING SEQUENCE:
PRO smei_mkcal, tt, $
camera = camera , $
generate= generate , $
name = name , $
template= template , $
force = force
INPUTS:
tt array[1]; time structure; default: TimeSystem()
day on which to look for mode 0 frames
(fraction of day is ignored)
OPTIONAL INPUTS:
camera=camera
scalar or array; type: integer; default: [1,2,3]
cameras to be processed
template=template
scalar; type: integer
fully-qualified file name of an existing
calibration ASCII template. This keywords overrides
input 'tt' and 'camera'
/generate by default only the ASCII file describing the
pattern (input for smei_cal) is made.
If /generate is set then the calibration pattern
itself is made.
/force if set, then existing patterns are overwritten
OPTIONAL OUTPUTS:
name=name scalar or array; type: string
fully-qualified names of created patterns
(null-string if no pattern is created)
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, FXPAR, GetFileSpec, InitVar, IsTime, IsType, READFITS, TimeGet, TimeLimits
TimeSet, TimeSystem, TimeUnit, boost, destroyvar, hide_env, smei_filename
smei_filepath, smei_hdr_get, smei_hdr_update, txt_read
CALLED BY:
smei_mkcal_auto
RESTRICTIONS:
Should only be run on smei.ucsd.edu or smeidb.smei.ucsd.edu
PROCEDURE:
Creates the ASCII calibration template (unless this is specified
as input). This is stored in $SMEIDB/cal/txt.
In addition to the pattern itself, a sequence of png files is generated
for the pattern itself and the individual frames on which the
pattern is based. These are stored in subdirectories of $SMEIDB/cal.
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS)
DEC-2009, Paul Hick (UCSD/CASS)
Allow execution on smeidb. When running on smeidb
all output files are created locally, and then are scp'd
to $SMEIDB on smei, to avoid problems in case
smei exports $SMEIDB in read-only mode.
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword 'template' to allow input of an existing
ASCII calibration templates. This allows (re-)creation
of cal pattern file and associated images.
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NAME:
smei_mkcal_auto
PURPOSE:
CALLING SEQUENCE:
PRO smei_mkcal_auto, $
camera = camera , $
lastpat = lastpat , $
ignore_block=ignore_block, $
force = force
OPTIONAL INPUTS:
camera = camera scalar or array; type: integer; default [1,2,3]
camera number(s): 1, 2 and/or 3
lastpat = lastpat scalar; type: integer; default: 0
indicates the number of status files to be
checked starting from the most recent one.
Special values:
lastpat = -1: check all status files
lastpat = 0: check all status files, starting
with the status file matching the doy
for the most recent cal pattern available
(used in SMEI data pipeline)
/ignore_block passed to smei_blocked
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FindAllFiles, InitVar, TimeGet, TimeUnit, hide_env, smei_blocked
smei_filename, smei_filepath, smei_last_tle, smei_mkcal, txt_read
RESTRICTIONS:
Can only be run on smei.ucsd.edu and smeidb.smei.ucsd.edu
PROCEDURE:
Sets "cal = 1" field in status file if cal pattern is successfully generated.
The "cal" field is always zero if the "mode 0" frame count is zero.
If the "mode 0" count is non-zero then "cal=0" means that the calibration
pattern for the set of mode 0 frames on this doy has not been created
yet. "cal=1" means that the cal patterns already exists.
This routine is usually run as a cronjob with keyword
lastpat=0. This looks for the most recent status file with
"cal=1" (pointing to the most recent existing cal pattern). It then
processes status files from that doy onward looking for status files
with a non-zero "mode 0" frame count and "cal=0". It the creates the
calibration pattern, and updates the status file by setting "cal=1".
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS)
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Also allow execution from smeidb.
Added documentation.
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NAME:
smei_mkdrives
PURPOSE:
Rewrites the file smei_drives.txt
CATEGORY:
camera/idl/frm
CALLING SEQUENCE:
PRO smei_mkdrives
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS: ***
FILEPATH, FindAllSubDirs, TimeGet, TimeOp, TimeSet, TimeUnit, hide_env, who_am_i
PROCEDURE:
MODIFICATION HISTORY:
JUL-2007, G. Megally, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_mkglare
PURPOSE:
Converts glare related grd files to Fits files
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_mkglare
INPUTS:
From $SSWDB_SMEI/glare
OUTPUTS:
To $SSWDB_SMEI
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXADDPAR, IsType, MKHDR, WRITEFITS, do_file, grd_read
PROCEDURE:
MODIFICATION HISTORY:
JUL-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_mki2m
CALLING SEQUENCE:
PRO smei_mki2m, f
INCLUDE:
@compile_opt.pro
CALLS: ***
LINFIT, gridgen, smei_star_list, smei_star_readpnt
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NAME:
smei_mklsff
CALLING SEQUENCE:
pro smei_mklsff
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, WRITEFITS, grd_read
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NAME:
smei_mkmask
PURPOSE:
Produces a daily "sky mask" indicating which parts of the sky were seen
by SMEI on a given day (1=always seen; 0=never seen; between 0 and 1:
seen in some but not all skymaps).
CALLING SEQUENCE:
PRO smei_mkmask, range, $
nbin = nbin , $
to_smeidb = to_smeidb , $
norbit = norbit , $
remote = remote , $
silent = silent
INPUTS:
range array[2]; type: time structure or valid time strings
default: ['2006_033','2008_318']
time range (start and end day)
OPTIONAL INPUTS:
/to_smeidb if set then write Fits file to standard
directory $SMEIDB/msk
norbit=norbit scalar; type: integer; default: 15
number of consecutive orbits to be used for
the creation of a mask (the default 15 covers
about one day).
nbin=nbin scalar; type: integer; default: 5
Sets the resolution of the mask
Must be a factor of 1800.
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FILEPATH, FXADDPAR, InitVar, IsType, MKHDR, TimeGet, TimeSet, TimeUnit
WRITEFITS, gridgen, hide_env, smei_filepath, smei_orbit_get, smei_sky
CALLED BY:
smei_mksky
PROCEDURE:
The size of the mask array is [3600,1800]/nbin. For nbin=5 (default)
this gives a 720x360 mask with a resolution of 0.5 degrees,
covering [0,360] in RA and [-90,+90] in declination.
The mask value for each skybin is a value between 0 and 1.
1 means that the skybin has a value in each of the morbit orbits
tested (where morbit <= norbit, is the number of skymaps found);
0 means that the skybin did not contain anything in all skymaps.
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_mkorb
PURPOSE:
Calculates approximations for parameters needed to
create orbital "on-the-fly" patterns
CATEGORY:
ucsd/camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_mkorb, ut_frac , $
lastpat = lastpat , $
firstorb= firstorb , $
lastorb = lastorb , $
generate= generate , $
truncpat= truncpat , $
filecmd = filecmd , $
threshold=threshold , $
force = force , $
silent = silent
OPTIONAL INPUTS:
lastpat=lastpat
scalar; type: integer; default: nr cal patterns, minus one.
defines the pair of "closed-shutter" calibration patterns
where to start calculating, i.e. the last "lastpat" pairs
of calibration patterns are processed.
lastpat=0: look at orbits more recent than last cal pattern
this is used in the real-time data pipeline
lastpat=1: look at orbits between last pair of cal patterns
lastpat>1: look further back for last 'lastpat' pairs of cal patterns
firstorb=firstorb
scalar; type: integer
overrides the internally determined start orbit
lastorb=lastorb
scalar; type: integer
overrides the internally determined stop orbit
/generate (only used if lastpat=1, and if run on
SMEI server smei.ucsd.edu)
if set then generate the "on-the-fly" orbital
patterns.
/filecmd (only used if lastpat=1, and if run on
SMEI server smei.ucsd.edu)
append result to file $SMEIDB/cat/list/c3orb
threshold=threshold
scalar; type: integer; default: 800
minimum on nr of frames required for "on-the-fly" pattern
(if there are less frames no pattern is created)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, FindAllFiles, GetFileSpec, InitVar, IsTime, IsType, REVERSE, TimeGet
TimeLInterpol, TimeLimits, TimeOp, TimeSet, TimeUnit, do_file, flt_read, hide_env
smei_filepath, smei_hdr_get, smei_orbit_get, timeposn, txt_read
CALLED BY:
smei_mkorb_auto
RESTRICTIONS:
Needs access to
$SMEIDB/cat/list/c3orb
file with previously used smeidb_orb calls
(the first 3-years of calls are used to get values for
min and max orbital fractions)
$SMEIDB/cat/list/smei_frm_orb_m1.txt
contains frame counts per orbit
and directory $SMEIDB/cal
contains the "closed-shutter" calibration patterns.
PROCEDURE:
For camera 3 a sequence of "on-the-fly" patterns needs to be defined
between each pair of successive "closed-shutter" calibration patterns.
Each sequence is created by a call to the Fortran program
smei_orb. The main parameters needed for this program are
minimum orbit, start orbit, stop orbit, minimum orbital fraction, and
maximum orbital fraction.
minimum orbit: usually the first full science mode orbit following
a "closed-shutter" calibration pattern.
NOTE that this probably will be wrong near anneals, when the
proper minimum patterns may be the one close to the trailing
calibration pattern.
start orbit: first orbit for which an "on-the-fly" patterns is needed
Usually the same as the minimum orbit)
stop orbit: last orbit for which an "on-the-fly" pattern is needed.
Usually the last science mode orbit preceding the next-following
calibration pattern.
minimum orbital fraction (between 0 and 1)
maximum orbital fraction (between 0 and 1)
restricts the range of CCD frames to be used in the construction
of "on-the-fly" patterns.
For the first three years of SMEI these parameters were determined
"by hand". This information is stored in the bash script $SMEIDB/cat/list/c3orb
in the form of calls to smei_orb. More recent data in this script are based
on the output of this program.
Minimum, start and stop orbit are set using the frame counts stored
in $SMEIDB/cat/list/smei_frm_orb_m1.txt. The main constraint is that the
number of valid frames needs to be above a specified threshold.
The minimum and maximum fraction are calculated by mapping back to
the first three assuming that the fractions have a periodicity of 1 year.
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS)
JAN-2010, Paul Hick (UCSD/CASS)
Prevent last_orbit return value to be larger than
orbit number of following cal
Bugfix. Do not use redirection over ssh to send modified
c3orb script back to soft@smei.
Changed definition for min_orbit. It now is one orbit later
than first_orbit to avoid using a partial orbit as min_orbit.
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added check for multiple cal patterns in the same orbit.
Script will abort when this happens.
Bugfix: the c3orb script was not updated correctly.
Updates are now done to file $SMEIDB/cat/list/c3orb_pipeline
Improved algorithm to calculate start, stop and minimum orbit.
The old algorithm put the start and minimum orbit very often
one orbit too high.
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NAME:
smei_mkorb_auto
PURPOSE:
Wrapper for smei_mkorb for creating "on-the-fly" orbital
patterns. Used in real-time data pipeline only.
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_mkorb_auto, $
threshold = threshold , $
ignore_block= ignore_block , $
force = force
OPTIONAL INPUT PARAMETERS:
threshold passed to smei_mkorb
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FindAllFiles, IsType, TimeGet, TimeOp, TimeSet, TimeUnit, boost, hide_env
smei_blocked, smei_filename, smei_filepath, smei_hdr_update, smei_last_tle
smei_mkorb, smei_orbit_get, txt_read
RESTRICTIONS:
Can only be run on the SMEI servers (smei.ucsd.edu or smeidb.smei.ucsd.edu)
PROCEDURE:
MODIFICATION HISTORY:
DEC-2008, Paul Hick (UCSD/CASS)
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Allow for execution on smeidb
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NAME:
smei_mksidereal
PURPOSE:
Combine three grid files
eq_allskymeed.grd.gz
np_allskymeed.grd.gz, and
sp_allskymeed.grd.gz
into one compressed Fits file
$SSWDB_SMEI/sid/c0sid_2002_365_000000.fts.gz.
The resulting FITS file represents sidereal background information
useful for star removal algorithms.
CALLING SEQUENCE:
PRO smei_mksidereal, version
INPUTS:
None
OPTIONAL INPUT PARAMETERS:
None
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FILEPATH, FXADDPAR, InitVar, IsType, MKHDR, TimeGet, TimeSet, TimeUnit
WRITEFITS, grd_read, gzip_file, hide_env, smei_filepath
RESTRICTIONS:
The input grid file paths and output FITS file path are hardcoded
into the program.
PROCEDURE:
The three grid files mentioned above are assumed to be valid grid
files. Additional FITS header information is added to each map as
they are written to the output FITS file.
A special version number header keyword, BKGNDVER, is added to the
main FITS header.
MODIFICATION HISTORY:
JUL-2006, Jordan Vaughan (UCSD)
DEC-2007, Paul Hick (UCSD/CASS)
Introduced WCS-compliant keywords to describe coordinate system.
APR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added new skymap version (2.0; not quite final yet).
OCT-2009, John Clover (UCSD/CASS)
Added new maps, all sky median for v4 background
JUL-2010, John Clover (UCSD/CASS; jclover@ucsd.edu)
Added newer maps, fixes error caused by star removal
that manifested in the over all background maps
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NAME:
smei_mksky
PURPOSE:
Create skymaps from most recent SMEI data
CATEGORY:
ucsd/camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_mksky, $
camera = camera , $
ignore_block= ignore_block , $
force = force , $
make_mask = make_mask , $
make_www = make_www , $
remote = remote , $
boss = boss
OPTIONAL INPUTS:
camera scalar or array; type: integer; default: [1,2,3]
camera numbers
/ignore_block if the SMEI pipeline is blocked (by putting a 1 in
file $SSWDB_SMEI/cat/sts/block/block_pipeline.txt)
this procedure will abort by default.
Setting this keyword will ignore this block.
/force if set then the "overwrite" flag is set for the "skyd"
daemon (resulting in overwriting existing skymaps)
/make_mask if set then the "msk" daily skymasks are calculated
and written to $SSWDB_SMEI/msk
/make_www creates html tables for available SMEI skymaps
(see smei_www_skymaps)
remote=remote scalar; type: string: default: soft@smei
if /make_mask is SET, and this procedure has no write
access to $SSWDB_SMEI, then remote should be set to a
username/host on a machine that does have write
access. The "msk" files are copied using scp.
boss scalar; type: string: default: smeidb.smei.ucsd.edu
set hostname of 'boss'. previously only ran on sun
this should let it run on any machine, use with
caution
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, FindAllFiles, InitVar, IsType, STRSPLIT, TimeGet, TimeOp, TimeSet, TimeSystem
TimeUnit, UNIQ, boost, hide_env, skyd_cat, smei_blocked, smei_filename, smei_filepath
smei_last_tle, smei_mkmask, smei_orbit_get, smei_www_skymaps, txt_read
RESTRICTIONS:
-Can only be run on smei.smei.ucsd.edu on the "skyd" account.
unless boss is specified
Depends on the collection of "status" files in $SSWDB_SMEI/cat/sts.
- Will not run if a skyd daemon is already running.
- To update the sts files on the smei server over ssh login using
public/private key pair needs to be set up.
PROCEDURE:
Processes days for which the sts files has flag "summary" ON
(i.e. pedestal/dark current have been calcalate and the header
files have been updated); and (camera 3 only) the flag "orb" is
ON (i.e. "on-the-fly" orbital patterns are available; the flag
"sky" of OFF (i.e. no skymaps have been made yet.
- skyd_cat is called to create the catalogues in $SKYD/list.
- the cf file $SKYD/cf/skyd_sun.cf is modified
- launches the skyd daemon
- sets the flag "sky" in the appropriate sts files.
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_mkstarmask
PURPOSE:
Creates the star mask file used in the creation of
skymaps by smei_skyd
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_mkstarmask, notest=notest
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXADDPAR, InitVar, MKHDR, WRITEFITS, grd_read
PROCEDURE:
Uses grd files in $SSWDB_SMEI as input, and creates
starmask.fts.gz in the same directory.
starmask.fts needs to be moved to $SMEIDB
where the Fortran routine smei_get_starmask looks for it.
MODIFICATION HISTORY:
DEC-2008, Paul Hick (UCSD/CASS)
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Bugfix: maps were stored in wrong coordinate system. The new
version converst from Andy's convention used in the grd file
to the SMEI skymap convention (the same is done for the
sidereal background maps in smei_mksidereal.pro)
Bugfix: resolution (bins/degrees) was specified wrong in Fits header.
Made Fits header WCS compliant.
Added Fits header keyword for star mask version number (now 2.0)
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NAME:
smei_mkstdstar
PURPOSE:
Convert grd files for standard stars to Fits files
used by smei_skyd
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_mkstdstar
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXADDPAR, IsType, MKHDR, WRITEFITS, grd_read, gzip_file, who_am_i
MODIFICATION HISTORY:
JUN-2006, Paul Hick (UCSD/CASS)
SEP-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
In addition to old PSF there now is an alternative PSF
(presumably with the background removed more accurately)
The old standard_star.fts is now standard_star_fixd.fts;
the new PSF is in standard_star_fill.fts.
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NAME:
smei_mkzldresidue
PURPOSE:
Stores Andy's zld correction map (1 static and 52 weekly
corrections) in a single Fits file
CATEGORY:
camera/idl/zld
CALLING SEQUENCE:
PRO smei_mkzldresidue
INPUTS:
(none)
OUTPUTS:
c3zldresidue.fts.gz
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXADDPAR, GetFileSpec, IsType, MKHDR, REVERSE, WRITEFITS, grd_read, hide_env
PROCEDURE:
The Fits headers should be WCS-compliant.
The coordinate system used is helioecliptic J2000.
Each of Andys maps is 360 x 360 with 0.5 degree resolution.
covering [-90,+90] in helioecliptic longitude. This is expanded
with zeroes to [-180,+180] making a standard helioecliptic
low-res map.
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_normal
CALLING SEQUENCE:
PRO smei_normal, _extra=_extra
INCLUDE:
@compile_opt.pro
CALLS: ***
AngleRange, AngleUnits, PlotCurve, TimeGet, TimeOp, TimeSet, TimeUnit, WhatIs, gridgen
ra_fictitious_sun, sgp4_orbit_axis
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NAME:
smei_orbit_get
PURPOSE:
Extracts fields from orbit structure
CATEGORY:
camera/gen/idl/toolbox
CALLING SEQUENCE:
FUNCTION smei_orbit_get, orb, $
number = number , $
fraction = fraction , $
doublex = doublex , $
roundx = roundx , $
ceilx = ceilx , $
floorx = floorx
INPUTS:
orb array; type: orbit structure
orbit structure as created by smei_orbit_set
OPTIONAL INPUTS:
/number extract integer orbit number
/fraction extract double precison fraction
/doublex extract orbit as double precision number, i.e. the
sum of number and fraction part. Note that this number
looses precision pretty quick for high orbit numbers.
/roundx extract orbit rounded to nearest integer orbit number
OUTPUTS:
rtn scalar or array
integer orbit number of double precision
fraction depending on setting of /number
or /fraction
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar
CALLED BY:
getsmeisources, smei_coriolis, smei_getfile, smei_hdr_plot, smei_mkmask
smei_mkorb, smei_mkorb_auto, smei_mksky, smei_orbit_stats, smei_sky_track
smei_star_show
PROCEDURE:
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_orbit_set
PURPOSE:
Creates structure for manipulating SMEI orbit numbers
CATEGORY:
camera/gen/idl/toolbox
CALLING SEQUENCE:
rtn = smei_orbit_set(number, [fraction])
INPUTS:
number scalar or array; any numerical type
fraction scalar or array; any numerical type
number and fraction are added together
and put in the structure
OUTPUTS:
rtn array; type: orbit structure
rtn.number is integer orbit number
rtn.fraction is double precision orbital fraction
with 0 <= fraction < 1
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType
CALLED BY:
smei_coriolis, smei_hdr_plot, smei_sky_track
PROCEDURE:
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_orbit_stats
PURPOSE:
Extracts information about frame counts and state changes from
the SMEI data base. The information is stored in ASCII files.
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_orbit_stats, trange , $
source = source , $
destination = destination , $
to_smeidb = to_smeidb , $
update = update , $
state_changes = state_changes , $
camera = camera , $
mode = mode , $
ndoy_lag = ndoy_lag , $
silent = silent , $
usedb = usedb , $
instant_write = instant_write , $
remote = remote
INPUTS:
trange array[2]; type: time structure; default: ['2003_001',Current time]
time range to be processed
If /update is set, then trange should NOT be specified
OPTIONAL INPUT PARAMETERS:
/state_changes if NOT set then frame counts are made only.
if SET then a log of state changes over time is made
source=source scalar; type: string; default: SMEIDB?
specifies the location of the SMEI data base
(passed to smei_getfile).
/update /update is ignored if trange is set.
If set then also /to_smeidb is assumed.
If set then the existing ASCII files in $SSWDB_SMEI/cat/list
are updated (i.e. /to_smeidb is assumed).
If NOT set then new ASCII files covering time range trange
are created in the specified destination; if no trange is
specified then the whole SMEI mission is covered.
/to_smeidb sets the destination to $SSWDB_SMEI/cat/list
destination=destination
scalar; type: string
destination directory for the ASCII data base files.
/to_smeidb NOT set: default: $TUB
/to_smeidb SET : default: $SSWDB_SMEI/cat/list
camera=camera scalar or array[2]; type: integer; default: [1,3]
ignored if /state_changes is NOT set
create/update state changes for specified cameras only
mode=mode scalar; type: integer
ignored if /state_changes is SET
if set the frame counts are for the specified mode
only (by default all three modes are combined)
tnow=tnow array[1]; type: time structure; default: TimeSystem()
ignored when /state_changes is set
sets the end time when /update is set
ndoy_lag scalar; type: integer; default: -3
sets overlap with existing ASCII files when /update
is set (i.e. the last ndoy_lag days in the ASCII
files is redone).
/usedb by default the header data base is used.
If /usedb is set the frame data base is used
(this takes a lot longer)
silent=silent scalar; type: integer; default: 0
controls level of informational messages
/instant_write only used is /state_changes is set
forces write of results as they are accumulated, instead
of storing into potentially gigantic arrays that are
written at the end.
OUTPUTS:
(to ASCII files; see PROCEDURE)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CheckDir, FILEPATH, GetFileSpec, InitVar, IsType, REVERSE, SMEI_ORBIT_BAD, TimeGet
TimeOp, TimeSet, TimeSystem, TimeUnit, boost, destroyvar, do_file, flt_string
smei_coriolis, smei_filepath, smei_getfile, smei_hdr_get, smei_orbit_get
smei_property, smeidb_mounted, txt_read
CALLED BY:
smei_mkbase
PROCEDURE:
/state_changes NOT set (i.e. frame counts only)
if no mode is specified then create/update files
destination/smei_frm_day.txt and destination/smei_frm_orb.txt
if mode is specified then create/update files
destination/smei_frm_day_m#.txt and destination/smei_frm_orb_m#.txt
(where # is 0,1,2)
/state_changes SET (i.e. state changes only)
create/update files destination/smei_state_cam#.txt'
where # is 1,2,3
MODIFICATION HISTORY:
SEP-2005, Paul Hick (UCSD/CASS)
MAR-2007, Paul Hick (UCSD/CASS)
Added counters for frames that satisfy the default test
criteria used by smeidb_sky to select frames for skymap
construction.
APR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added timestamp to header
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NAME:
smei_orient_test
PURPOSE:
Check orientation of cameras
CATEGORY:
camera/idl/tricks
CALLING SEQUENCE:
smei_orient_test
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, CombineRotations, CvRotation, HAFB_GET_CAMERA_DATA, WhatIs
RESTRICTIONS:
Probably need to compile smeipoint.pro explicitly to get access to
Don's get_camera_data
SEE ALSO:
smei_camera
PROCEDURE:
The UCSD s/c coordinate system:
X-axis along velocity vector
Y-axis along rotation axis spacecraft
Z-axis to zenith
The HAFB s/c coordinate system (as in Don's smeipoint.pro routine):
X-axis along velocity vector
Y-axis opposite to rotation axis spacecraft
Z-axis pointing to nadir (i.e. down to Earth)
To go from UCSD to HAFB s/c coordinate system, rotate around
x-axis by 180 degrees:
R[sc UCSD -> s/c HAFB]: Euler angles: [0,!pi,!pi]; quaternion: [1,0,0,0].
The UCSD camera coordinate system:
X-axis along long dimension (on CCD positive X goes to larger pixel indices)
Y-axis along narrow dimension (on CCD positive Y goes to smaller radius)
Z-axis along optical axis
The HAFB camera coordinate system (as in Don's smeipoint.pro routine):
X-axis is UCSD Z-axis (along optical axis)
Z-axis is UCSD Y-axis
Y-axis is UCSD X-axis
To go from HAFB to UCSD camera coordinate system, apply
Euler angles:
R[camera HAFB -> camera UCSD]: [0,!pi/2,!pi/2]; quaternion: [1,1,1,1]/2.
(this is a rotation of 120 degrees around a unit vector with equal components
along positive x,y and z axes).
The Euler angles provided to Spectrum Astro rotate from the UCSD
s/c coordinate system to the UCSD camera coordinate system.
R[sc UCSD -> camera UCSD]
The Euler angles provided to Spectrum Astro apply rotations to Z,X and
Z axes. We want Euler angles applied to Z,Y,Z axes. To go from Z,Y,Z angles
to Z,X,Z angles add 90 deg to the first and subtract 90 deg from the
last Euler angle.
The HAFB camera quaternions rotate from the HAFB camera coordinate
system to the HAFB s/c coordinate system.
R[camera HAFB -> sc HAFB]
To retrieve the equivalent Spectrum Astro angles from the HAFB quaternions
apply the following rotations in sequence:
R[sc UCSD -> s/c HAFB] quaternion [1,0,0,0]
Inverse of R[camera HAFB -> sc HAFB] (inverse of smeipoint quaternion)
R[camera HAFB -> camera UCSD] quaternion: [1,1,1,1]/2.
Convert the resulting quaternion to Z,Y,Z angles, i.e.
add 90 to first and -90 to third to get Z,X,Z angles:
The Euler angles given to Spectrum Astro are:
camera 1: -28.207646 69.541377 -21.4776600
camera 2: -86.023031 58.285313 -6.5798011
camera 3: -143.782150 62.553932 0.3674422
We frequently need to convert from equatorial coordinates to UCSD
camera coordinates. The quaternions provided to us in the SMEI data
rotate from the ECI (J2000 equatorial) to the HAFB s/c frame.
So to go from UCSD camera frame to the ECI frame apply the following
rotations
R[camera UCSD -> camera HAFB] quaternion [-1,-1,-1,1/2
R[camera HAFB -> s/c HAFB] (from smeipoint)
Inverse of R[sc HAFB -> ECI] (inverse of quaternion from SMEI data)
The first two of these (rotating from UCSD camera to HAFB s/c frame)
is returned by smei_camera. The inverse of all three combined
rotations is returned by smei_cam_quaternion.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_pick_stars
PURPOSE:
Select stars to be used for frame registration
CATEGORY:
camera/idl
CALLING SEQUENCE:
FUNCTION smei_pick_stars, pp, mag, dmin=dmin, magmax=magmax, count=count
INPUTS:
pp array[2,*]; type: float
x,y pixel coordinates
OPTIONAL INPUT PARAMETERS:
dmin=dmin only entries at least dmin pixels
removed from the nearest neighbour are put in 'list'
magmax=magmax only entries with magnitudes less then magmax
are put in 'list'
OUTPUTS:
pp array[2,*]; type: float
subset of input for stars fitting criterion
pp will not exist on return if no stars fit.
list array; type: integer
list of stars fitting the criterion
If no stars fit then list = -1 is returned
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
# stars in 'list'
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType
CALLED BY:
stardistance
PROCEDURE:
MODIFICATION HISTORY:
FEB-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_plot_timeseries
PURPOSE:
Plots SMEI timeseries from one of the points files generated
by the SMEI tomography program.
CATEGORY:
CALLING SEQUENCE:
PRO smei_plot_timeseries, file, nr=nr, $
nvalid_los = nvalid_los , $
xrange = xrange , $
refresh = refresh , $
path = path , $
_extra = _extra
INPUTS:
file scalar; type: string
fully-qualified file name.
If not specified the IDL dialog_pickfile is used.
OPTIONAL INPUT PARAMETERS:
nr=nr array; type: integer; default: 0
list of timeseries to be plotted
nvalid_los=nvalid_los
scalar; type: integer; default: 1
threshold for plotting timeseries: only timeseries with
more than "nvalid_los" points are displayed.
/refresh if set, forces reading of new file, instead of using
data still in memory
path=path scalar; type: string
directory name passed to dialog_pickfile
Only used if 'file' is not defined
xrange=xrange array[2]; type: time structure
range of time axis (passed to PlotCurver)
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
COMMON BLOCKS:
common smei_plot_timeseries_common, old_file, d
CALLS: ***
BadValue, InitVar, IsType, PlotCurve, TimeGet, TimeSet, TimeUnit, destroyvar, flt_read
hide_env
PROCEDURE:
Once read, information from the last read file is kept in memory
for replotting, except when /refresh is set (which forces reading
of a new file.
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_property
PURPOSE:
Get some property of a SMEI frame
CATEGORY:
camera/idl/misc
CALLING SEQUENCE:
FUNCTION smei_property, frame , $
uncovered = uncovered , $
inroi = inroi , $
pedestal = pedestal , $
dark_current= dark_current , $
dark_median = dark_median , $
dark_average= dark_average , $
squares = squares , $
centerpix = centerpix , $
left = left , $
right = right , $
high = high , $
low = low , $
sandwich = sandwich , $
average = average , $
threshold = threshold , $
exclude_value=exclude_value , $
ceiling_value=ceiling_value , $
floor_value = floor_value , $
rejected = rejected , $
silent = silent , $
sigma = sigma , $
stdev = stdev , $
time = time , $
exposure = exposure , $
name = name , $
path = path , $
camera = camera , $
mode = mode , $
frame_nr = frame_nr , $
onboard_ff_enabled=onboard_ff_enabled, $
shutter_open= shutter_open , $
led_enabled = led_enabled , $
roi_map = roi_map , $
bos_alert = bos_alert , $
bos_change = bos_change , $
sun = sun , $
moon = moon , $
venus = venus , $
ccd_temp = ccd_temp , $
tlm_time = tlm_time , $
l1a_time = l1a_time , $
tlm_file = tlm_file , $
l1a_file = l1a_file , $
l1a_pntr = l1a_pntr , $
quaternion = quaternion , $
n_pedestal = n_pedestal , $
n_dark_current = n_dark_current , $
base_done = base_done , $
base_ok = base_ok , $
in_eclipse = in_eclipse , $
in_earth_shadow = in_earth_shadow, $
bad_quaternion = bad_quaternion, $
just_bad = just_bad , $
anneal = anneal , $
bad_data = bad_data , $
version = version , $
cal_pattern = cal_pattern , $
orb_pattern = orb_pattern , $
orbit = orbit , $
naxes = naxes , $
crpix = crpix , $
cdelt = cdelt , $
crval = crval , $
lonpole = lonpole , $
count = count
INPUTS:
frame array[n,m,k]; type: short integer ??
sequence of k SMEI frames of dimension n x m
array[n]; type: structure
header structure of SMEI frame(s)
OPTIONAL INPUT PARAMETERS:
If input 'frame' are 2D-arrays with SMEI frame data:
/uncovered Get uncovered arrea of CCD (between dark columns)
/inroi Only get pixels inside ROI
/pedestal Get pedestal value
(based on a subset of the pixels in the pedestal columns)
/dark_current
/dark_median
/dark_average
/dark_columns Get dark columns
/ccd_squares Get CCD squares
/sngle_pix Get single pixel in center of fov
If input 'frame' is a header structure:
/time returns time of array as time structure
/name returns file name of frame (name+extension)
/path returns fully-qualified path
/onboard_ff_enabled returns 1 if ff was enabled
/tlm_time returns name of original telemetry file
OUTPUTS:
If input 'frame' are 2D-arrays with SMEI frame data:
out /pedestal set:
array[k]; type: double
Currently the pedestal is the average over the top
half of dark columns (pixels 32 and up) away from the
field of view
/dark_columns set:
array[nn,m,k]; type: same as input 'frame'
dark columns (nn=2,4, or 8 depending on binning)
/ccd_squares set:
array[2*nn,nn,k]; type: same as input 'frame'
squares on either side of fov (nn=10,20,40 depending on binning)
/single_pix set
array[nn,nn,k]; type: same as input 'frame'
single pixel in center above field of view
(nn=1,2,4 depending on binning)
dark_column=dark_columns
array[2,64] (mode 2); type: unsigned int, long or float
(multiply array dims by 2^(2-mode) for mode 0,1)
pixels in covered columns on eithe side of the frame
(with a width of 'a' pixels)
ccd_squares=ccd_squares
array[10,10]; type: unsigned int, long or float
(multiply array dims by 2^(2-mode) for mode 0,1)
pixels in open areas outside of the smei fov
(two squares of 10 x 10 telemetry pixels)
single_pix=single_pix
array[1,1]
(multiply array dims by 2^(2-mode) for mode 0,1)
pixels horizontally centered in frame above fov
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro ; ROI mask common block
CALLS: ***
ArrayLocation, BadValue, FILEPATH, GetFileSpec, InitVar, IsType, STDDEV, TimeSet, UNIQ
boost, smei_filename, smei_filepath, smei_setup_roi, timeposn, where_common
who_am_i
CALLED BY:
img_read, maygeometry, qImage_cw_Property, qImage_cw_Where, qsmei_hdr
smei_base_testcase, smei_buf_get, smei_buf_getframe, smei_buf_mget
smei_buf_prep, smei_buf_read, smei_cam_quaternion, smei_frm_base, smei_frm_cvhdr
smei_frm_eclipse, smei_frm_findpoint, smei_frm_hbar, smei_frm_info, smei_frm_ped
smei_frm_read, smei_frm_summary, smei_frm_track, smei_frm_where, smei_hdr_make
smei_hdr_plot, smei_orbit_stats, smei_shutterwrong, smei_sky2cam, stardistance
SEE ALSO:
RESTRICTIONS:
The file smei_buf_roi.txt must exist in the same directory as this source
code file.
PROCEDURE:
The dark_columns, ccd_squares and single pix are identified by checking for values
2,3 and 4, respectively in the mask read from smei_buf_roi.txt.
MODIFICATION HISTORY:
MAR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_radial2theta
PURPOSE:
Converts a radial offset Rccd-R0 to an angle thetay
CATEGORY:
camera
CALLING SEQUENCE:
thetay = smei_radial2theta(delta_r[, thetax, tol=tol])
INPUTS:
delta_r array; type: float
radial offsets in left-hand side of Eq. 3
in pixels
OPTIONAL INPUT PARAMETERS:
thetax scalar or array with structure type as 'delta_r';
type: same as 'delta_r'; default: 0.0
thetax value in right-hand side of Eq. 3
in degrees
OUTPUTS:
thetay array with same structure as 'delta_r'; type: same as 'delta_r'
thetay value that satisfies Eq. 3 for specified
radial offset and thetax in degrees.
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_theta2radial
CALLS: ***
InitVar, SubArray, SuperArray, nrZBrent, nrZbrac
CALLED BY:
cvsmei, smei_ccd2sky
PROCEDURE:
See Andy's memo "Defining the field of view for the SMEI cameras" (11-July-2001)
This function inverts Equation 3.
MODIFICATION HISTORY:
FEB-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_rewind
PURPOSE:
Rewinds SMEI pipeline by clearing entries in status files
in $SSWDB_SMEI/cat/sts
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_rewind, tt , $
cal = cal , $
base = base , $
orb = orb , $
sky = sky , $
camera = camera , $
notest = notest
INPUTS:
tt scalar or array[1]; time in the form of a
string or standard time structure. The input time is
truncated to the beginning of the day (0 UT).
Usually specified in the form YYYY_DOY. This rewinds
the pipeline back to (and including) the indicating
day.
OPTIONAL INPUT PARAMETERS:
Four keywords are available to indicate which part of the
pipeline processing is to redone.
One and only one of the following four keyword must be set:
/cal Redo everything starting with the calibration patterns
/base Rebase all frames, redo "on-the-fly" patterns and skymaps
/orb Redo the orbital "on-the-fly" pattern, and the skymaps
/sky Redo only the skymaps
camera=camera scalar, or array; type: integer; default: [1,2,3]
list of cameras for which status are updated
/notest no actual updates of the status files are made
UNLESS this keyword is set. If /notest is NOT set
then the content of the updated status files is
written to screen only.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FindAllFiles, InitVar, IsTime, IsType, TimeGet, TimeOp, TimeSet, TimeUnit, hide_env
smei_filename, smei_filepath, txt_read
SIDE EFFECTS:
Updates status files
PROCEDURE:
The status files are used in the script smei_pipeline.sh, and
the IDL programs it calls to decide which steps to executed.
Rewinding the pipeline with this procedure only will clear
(set to zero) the appropriate flags in the status file, forcing
the indicated steps to be redone.
Note that this will only work if smei_pipeline.sh is set up
in such a way that existing files are overwritten. In particular,
this means that the /force keyword must be used on all IDL
procedures executed.
MODIFICATION HISTORY:
MAR-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added documentation
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NAME:
smei_rmdups
CALLING SEQUENCE:
PRO smei_rmdups
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, FindAllFiles, GetFileSpec, WhatIs, where_common
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NAME:
smei_roi_mask
PURPOSE:
Common block definition with ROI information
CATEGORY:
camera/idl/buf
CALLING SEQUENCE:
@smei_roi_mask.pro
INPUTS:
From text file smei_buf_roi.txt
OUTPUTS:
Stored in common block
COMMON BLOCKS:
common smei_roi_mask, roi_siz, roi_frm, roi_drk, roi_sqr, roi_pix, roi_ped, roi_col, roi_fov, roi_bad
CALLS:
smei_setup_roi, who_am_i
MODIFICATION HISTORY:
APR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_setup_roi
PURPOSE:
Fill common block with ROI information
CATEGORY:
camera/idl
CALLING SEQUENCE:
smei_setup_roi
INPUTS:
(from text file smei_roi.txt)
OPTIONAL INPUTS:
/destroy destroys ROI heap variables
OUTPUTS:
CALLS: ***
ArrayLocation, FILEPATH, InitVar, IsType, MagnifyArray, destroyvar, txt_read, who_am_i
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_roi_mask.pro
CALLED BY:
qImage_cw_Where, qView_Destroy, smei_buf_get, smei_buf_mget, smei_buf_read
smei_frm_base, smei_frm_flatfield, smei_frm_hbar, smei_frm_read, smei_frm_rebin
smei_property, smei_roi_mask
PROCEDURE:
Sets up pointers to list of array indices into SMEI frames for each of the modes
For i=0,1,2 (three different modes):
*roi_siz[i] 2-element array with image dimension
*roi_frm[i] list of pixels included in the SMEI roi
*roi_fov[i] list of pixels inside the field of view (incl. *roi_bad[i])
*roi_drk[i] list of pixels in dark current columns
*roi_sqr[i] list of pixels in two squares outside fov arc
*roi_pix[i] list of pixels in center square inside fov arc
*roi_ped[i] list of pixels in pedestal columns
*roi_col[i] list of pixels in pedestal and dark current columns
*roi_bad[i] list of pixels with partially covered pixels
(i.e. the column to the right of the dark columns on the left, and
the column to the left of the dark columns on the right of the frame)
MODIFICATION HISTORY:
APR-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sgp4_orbits
PURPOSE:
Build list of start times for all orbits using TLE data base.
CALLING SEQUENCE:
PRO smei_sgp4_orbits, input_sgp4_file, new=new, smeitree=smeitree, silent=silent
INCLUDE:
@compile_opt.pro ; On error, return to caller
INPUTS:
input_sgp4_file
existing file with start times.
By default the file in the SMEI tree is used
(if /new is NOT set)
OPTIONAL INPUTS:
/new creates a new file from scratch. In this case
input_sgp4_file is ignored
/smeitree The output file is created as $TUB/smei_sgp4_orbits.tmp
If /smeitree is set then the file in $TUB is copied to
the SMEI master tree and to the SMEI tree on smei.ucsd.edu
(requires that env $SMEIMASTER is defined)
CALLS: ***
AngleRange, CV_COORD, FILEPATH, INTERPOL, InitVar, TimeGet, TimeOp, TimeSet, TimeUnit
big_eph, destroyvar, hide_env, ra_fictitious_sun, sgp4_eph, sgp4_orbit_axis
sgp4_orbit_period, sphere_distance, txt_read, who_am_i
PROCEDURE:
sgp4_eph returns rectangular ECI coordinates relative to the
current equinox. Essentially this means equatorial coordinates
relative to the current equinox. So the declination is
effectively the geographic latitude.
Currently (March 2011) this procedure is called as part of
smei_pipeline.sh (executed hourly as cronjob on smeidb).
The file is used in IDL only by the procedure smei_coriolis.pro.
In Fortran the only function calling it is smei_orbit_info2.f.
Content of file:
1. SMEI orbit number
2. Orbit start time in format YYYY_DOY_hhmmssmss
The orbital start time in format hh:mm:ss.mss
Defined as the time Coriolis crosses a fixed geographic
latitude (~ -31.1 degrees; close to the latitude of the
SAA) going north.
3. Orbital period, defined as time difference between two
successive orbital start times
4. Orbital period used in sgp4 software
I think this is some sort of Keplerian orbital period;
not particulary useful.
5. Precision of geographic latitude calculation
The remaining columns are related to the normal of the SMEI orbital
plane (pointing towards the Sun).
6. Solar elongation (in degrees) of the normal
7. RA (in degrees) of the fictitious Sun
This progresses stricly linear with UT going through
360 degrees in 365.25 days (one Julian year).
This is approximate, but good enough for government work)
8. RA difference (J2000, in degrees) of the normal with the
RA of the fictitious Sun.
9. Declination of the normal (J2000, in degrees)
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS)
OCT-2006, Paul Hick (UCSD/CASS)
Replaced NewcombSun by big_eph calls
MAR-2007, Paul Hick (UCSD/CASS)
Eliminated big_eph. Now only sgp4_eph is used.
APR-2007, Paul Hick (UCSD/CASS)
Added check to avoid calculating start times past
the time of the last TLE available to sgp4_eph.
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added column for elongation of normal to Coriolis
of orbital plane.
MAR-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added columns for RA,dec of orbit normal
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NAME:
smei_sgp4_quat
PURPOSE:
Calculates quaternion for nominal SMEI attitude at indicated times.
CATEGORY:
CALLING SEQUENCE:
FUNCTION smei_sgp4_quat, tt
INPUTS:
tt array; type: time structure
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
qq array[4,*]; type: double
spacecraft quaternion
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CV_COORD, CvRotation, sgp4_eph
CALLED BY:
qImage_cw_Where, smei_cam_quaternion
PROCEDURE:
Should match the quaternion specified in the SMEI frame header.
MODIFICATION HISTORY:
JUL-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_shutterwrong
PURPOSE:
Detect frames that may have the shutter flag set wrong
CALLING SEQUENCE:
PRO smei_shutterwrong, trange, camera=camera, mode=mode, dbsource=dbsource
INCLUDE:
@compile_opt.pro
CALLS: ***
FILEPATH, GetFileSpec, InitVar, IsType, MEAN, STDDEV, TimeGet, TimeUnit, smei_coriolis
smei_getfile, smei_hdr_get, smei_property
MODIFICATION HISTORY:
JAN-2006, Paul Hick (UCSD/CASS)
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NAME:
smei_sky
PURPOSE:
View orbital sky maps
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
PRO smei_sky, wanted_map, _extra=_extra, $
source = source , $
allraw = allraw , $
allcnt = allcnt , $
allflat = allflat , $
allstars = allstars , $
two_eyes = two_eyes , $
timesun = timesun , $
degrees = degrees , $
maxelo = maxelo , $
ndim = ndim , $
equator = equator , $
range = range , $
ctable = ctable , $
breakval = breakval , $
antisolar = antisolar , $
silent = silent , $
zero_point = zero_point, $
difference = difference, $
xysize = xysize , $
rawmap = rawmap , $
sidereal = sidereal , $
noplot = noplot , $
skymap = skymap , $
hdrs = hdrs , $
count = count , $
imgfile = imgfile , $
logo = logo , $
charsize = charsize , $
exten_no = exten_no , $
compose = compose , $
naked = naked , $
legend = legend , $
logscale = logscale , $
get_camera_map = get_camera_map, $
min_map = min_map , $
flip_ct = flip_ct , $
flip_bw = flip_bw , $
timeavgcam = timeavgcam
INPUTS:
wanted_map scalar; type: integer
OPTIONAL INPUT PARAMETERS:
timesun=timesun array[1]; type: time structure
overrides the time extracted from the
file header as the time determining the position
of the Sun in the sun-centered maps.
/degrees if set, all angles are in degrees
default: radians
mode = 'sky','equ':
The all* keywords force display of all three 'raw' (hires) skymaps in one
image. (i.e. the equatorial and the two polar maps):
/allraw ('sky' and 'equ')
if set, plot brightness maps (1st 3 Fits extensions)
in three separate panels: north pole, equatorial
region and south pole.
/allcnt ('sky' only)
if set, plot frame counts (2nd 3 Fits extensions in 'sky' maps)
in three separate panels: north pole, equatorial
region and south pole.
/allflat ('equ' only)
if set, plot star-subtracted "flat" brightness maps
(2nd 3 Fits extension in "equ" maps)
in three separate panels: north pole, equatorial
region and south pole.
/allstars ('equ' only)
if set, plot subtracted stars (3rd 3 Fits extensions in "equ" maps)
in three separate panels: north pole, equatorial
region and south pole.
A number of keywords force display of a single Fits extension.
Hires equatorial maps are always in equi-rectangular projection:
/equatraw ('sky' and 'equ')
/equatcnt ('sky')
/equatflat ('equ')
/equatstars ('equ')
Hires polar maps are always in polar projection.
/northraw ('sky' and 'equ')
/northcnt ('sky')
/northflat ('equ')
/northstars ('equ')
/southraw ('sky' and 'equ')
/southcnt ('sky')
/southflat ('equ')
/southstars ('equ')
Remaining keywords refer to lores maps. The lores maps are always full-sky.
/dirtysky ('sky')
/orbtime ('sky', 'equ')
/orbsecs ('sky', 'equ')
/psfn ('sky', 'equ')
/psfe ('sky')
/badsky ('sky')
/badhtm ('sky')
/fovx ('sky', 'equ')
/thetax ('sky')
/thetay ('sky')
If none of these keywords are specified than the equatorial
and two polar maps are assembled into a single map covering the full
sky.
/difference ??
/compose ??
Full-sky maps (i.e. the lores maps and composite hires maps) are by
default plotted in a sun-centered (or centered anti-solar if /antisolar
is set). The map projection is controlled by the maxelo keyword.
/equator passed to PlotEarthSkymap. Puts the equatorial plane on the
horizontal instead of the ecliptic.
Used only for sun-centered (composite) maps.
/rawmap This displays the sun-centered map without interpolation
to obtain the map values. In this case the keyword
/equator is set in PlotEarthSkymap.
Used only for sun-centered (composite) maps.
/sidereal forces display in a sidereal (equatorial)
coordinate system.
maxelo=maxelo passed to PlotEarthSkymap. Determines the map projection
(Hammer-Aitoff, equi-rectangular or fish-eye)
/antisolar shifts from sun-centered map to map centered on
anti-solar direction.
Other keywords passed to smei_sky_read
camera=camera scalar, or array[n]; type:integer; default: 2
camera numbers
nbin=nbin
/noplot suppresses plotting
mostly used to pull out the skymap array
ignored if keyword allraw is set
OUTPUTS:
skymap=skymap skymap array as returned by smei_sky_read
hdrs=hdrs scalar or array; type: string
list of fully-qualified filenames read
by smei_sky_read
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, BadValue, CvPrecess, CvSky, InitVar, IsType, LOADCT, PlotEarthSkymap [1]
PlotEarthSkymap [2], PlotEarthSkymap [3], PlotEarthSkymap [4], PlotPolarSkymap
REVERSE, SuperArray, TimeLimits, TimeSet, ToDegrees, ToRadians, UNIQ, WhatIs, big_eph
destroyvar, get_page, gridgen, jpl_body, set_page, smei_getfile, smei_sky_cleantime
smei_sky_field, smei_sky_hdr2range, smei_sky_hdr_check, smei_sky_read
CALLED BY:
FUNCTION smeilatest lastorbit, qsmei_sky_pick, smei_findpnt, smei_mkmask
smei_sky_cleanedge_map, smei_sky_track, smei_star_fit, smei_star_remove
smei_zld_remove [1], smei_zld_remove [2]
PROCEDURE:
MODIFICATION HISTORY:
DEC-2004, Paul Hick (UCSD/CASS)
JUL-2006, Paul Hick (UCSD/CASS)
Added time keyword
APR-2008, Paul Hick (UCSD/CASS)
Added code to handle input of 2-element 'source'.
Fixed bug in making of difference maps for raw maps
MAY-2008, Paul Hick (UCSD/CASS)
All full-sky maps are now by default sun-centered.
Added /sidereal keyword to force display in sidereal
equatorial in equi-rectangular projection.
JUL-2008, Paul Hick (UCSD/CASS)
Improved interpolation procedure on equatorial map
for points close to edge of map. Primarily needed
to overcome limitation in IDL interpolate procedure
for point just outside the array limits.
FEB-2010, Paul Hick (UCDS/CASS)
Removed ambiguity between keywords 'time' and 'timeavgmap'
(made keyword time inaccessible) by renaming 'time' to
'timesun'
JUN-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Bugfixes: added safeguards against completely empty skymaps
to avoid crash because of invalid array index -1.
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NAME:
smei_sky2cam
PURPOSE:
Convert from equatorial coordinates to coordinates in the UCSD
SMEI camera frame.
CATEGORY:
camera/idl
CALLING SEQUENCE:
R = smei_sky2cam( rvec, [ camera=camera, quaternion=quaternion, /degrees] )
INPUTS:
rvec array[2,n] or array[3,n]; type: float
positions in the sky as spherical or rectangular
equatorial coordinates.
/rect NOT SET: spherical coordinates
rvec[0,*] is RA;
rvec[1,*] is declination
rvec[3,*] (usually the distance)
/rect SET: rectangular coordinates
rvec[0,*] is x-coordinate (toward vernal equinox
rvec[1,*] is y-coordinate
rvec[3,*] is z-coordinate (toward equatorial north)
The units of the angles are determined by the setting of /degrees.
OPTIONAL INPUT PARAMETERS:
/degrees if set, all in- and output angles are in degrees
(default: radians). Note that the input 'camera' structure,
if specified, must be consistent with the setting of /degrees.
/rectangular if set then rvec is in rectangular Cartesian coordinates.
The 1st dimension in rvec MUST be 3; if it is not then
this keyword is ignored.
camera=camera Identifies the SMEI camera
Can be any one of the following three.
array[1]; type: SMEI_FRM_HDR structure
this determines the camera and the quaternion.
The keyword 'quaternion', if present,
will be ignored.
array[1]; type: SMEI_CAMERA_FOV structure
structure containing information about SMEI field of
view; usually the return value of smei_camera
with the /get_structure keyword set.
This determines the fixed S/C-to-camera quaternion. The
Coriolis quaternion must be specified using the
'quaternion' keyword.
scalar; type: integer
camera number (1,2 or 3).
This determines the fixed S/C-to-camera quaternion. The
Coriolis quaternion must be specified using the
'quaternion' keyword.
If not specified then camera=1 is assumed.
The camera number is used as argument to smei_camera to
obtain the fov structure.
quaternion=quaternion
array[4]; type: float
Coriolis S/C quaternion
OUTPUTS:
R array[3,n]; type: float
x,y,z coordinates of unit vector in the UCSD camera
frame
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CV_COORD, CvRotation, InitVar, IsType, SyncDims, ToRadians, boost, smei_cam_quaternion
smei_camera, smei_property
PROCEDURE:
MODIFICATION HISTORY:
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Extracted from smei_sky2ccd.
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NAME:
smei_sky2ccd
PURPOSE:
Convert from positions in the sky to CCD coordinates
CATEGORY:
camera/idl
CALLING SEQUENCE:
R = smei_sky2ccd( runit, [ camera=camera, /degrees] )
INPUTS:
runit array[3,n]; type: float
positions in the sky as unit vectors in the UCSD camera
frames (as output by smei_frm_sky2ccd)
These are converted to CCD coordinates if inside the FOV
If no points lie inside the
field of view then the scalar BadValue(rvec) is returned.
OPTIONAL INPUT PARAMETERS:
camera=camera scalar; type: integer
camera number (1,2 or 3).
If not specified then camera=1 is assumed.
The camera number is used as argument to smei_camera to
obtain the fov structure.
/degrees if set, all in- and output angles are in degrees
(default: radians). Note that the 'camera' structure
must be consistent with the setting of /degrees.
/boolean if set then the output array 'inside' is a byte array of zeros
and ones indicating whether the corresponding vectory is
outside/inside the field of view (instead of a list of
indices from the IDL 'where' function identifying vectors
inside the field of view).
scalefov=scalefov
scalar; type: float; default=3.0 (covers essentially the whole
hemisphere centered on the camera optical axis).
Only locations closer then fov.size[0]/2 (= 30 degrees) to the
pole potentially lie inside the fov. The multiplier scalefov
extends the search to at most 89.5 degrees (essentially the
whole hemisphere centered on the pole. See PROCEDURE.
distort=distort
NOT IMPLEMENTED YET
OUTPUTS:
R array[2,n]; type: float
x and y pixel coordinates inside the SMEI fov
OPTIONAL OUTPUT PARAMETERS:
inside=inside array; type: long int (/boolean NOT set) or byte (/boolean set).
if /boolean is not set then 'inside' is a list of indices of
vectors inside field of view
if /boolean is set then 'inside' is a byte array with 0 for
vectors inside or 1 for vectors inside the field of view.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, CV_COORD, InitVar, Inside_Wedge, IsType, SyncDims, ToDegrees, ToRadians
smei_cam2ccd, smei_camera, smei_theta2radial
PROCEDURE:
The determination of sky locations inside the field of view is done in
two cuts. The first cut retains only points within scalefov*30 deg from
the optical axis. The default scalefov=3.0 so all points within 90 deg
are retained (actually 89.5 degrees).
The second cut retains only points strictly inside the field of view as
defined in the 'camera' structure. Only CCD coordinates for these points are
returned and are marked in the 'inside' array.
MODIFICATION HISTORY:
FEB-2003, Paul Hick (UCSD/CASS)
FEB-2005, Paul Hick (UCSD/CASS)
Added keyword runit
MAR-2005, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Split smei_sky2ccd into two parts: smei_sky2cam and smei_cam2ccd.
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NAME:
smei_sky_atlocation
PURPOSE:
Good question
CATEGORY:
Extract function values at specified sky locations from a SMEI
skymaps. Put together in kinda adhoc fashion. So sorry.
CALLING SEQUENCE:
FUNCTION smei_sky_atlocation, wanted_map, $
show = show , $
time = time , $
_extra = _extra
INPUTS:
wanted_map passed to smei_getfile
OPTIONAL INPUT PARAMETERS:
/show prints the locations and function values extracted
from the skymap on the screen for all extensions
in the selected skymap.
_extra=_extra /show SET:
One of the from_* keywords to cvsmei is used here to
specify one or more skymap locations
(just a single location should be specified, I think, otherwise
the screen will be flooded with too much output).
/show NOT set:
keywords are passed to smei_sky_field to determine
whether a skymap is requested, and what extension to read,
if it is a skymap.
Also, one of the from_* keywords to cvsmei is used
to specify the sky locations
OUTPUTS:
R function value
OPTIONAL OUTPUT PARAMETERS:
time=time array[1]; type: time structure
if /show is set, then the time at which SMEI observed the
sky location is returne here.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, FXPAR, InitVar, READFITS, TimeGet, TimeOp, TimeSet, TimeUnit, cvsmei
smei_getfile, smei_sky_field, smei_sky_hdr2mode
CALLED BY:
qImage_cw_Where
PROCEDURE:
MODIFICATION HISTORY:
APR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_cleanedge_fix
PURPOSE:
Applies a correction to a hires skymap (equatorial
north pole or south pole) for straylight contribution
from sky just outside the fov.
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_sky_cleanedge_fix , $
lo_fovx , lo_time , $ ; Lores direction cosine angle and time maps
hi_sky , $ ; Hires sky map
lo_edge , hi_edge , $ ; Inner and outer edge of band in need of fixing
fraction , time_sample , $ ; Max fraction of sample time series subtracted
left_sample , right_sample , $
mode = mode
INPUTS:
lo_fovx array[720,360]; type: float
lo_time array[720,360]; type: float
2D lores skymaps: time and fovx angle
hi_sky array[3600,1200,n] or array[800,800]
2D hires skymap to be corrected
If n=1 the 3rd dimension may be absent
lo_edge scalar; inner edge of fov area that needs
to be corrected (lo_edge=20 degrees)
hi_edge scalar: outer edge of fov area that needs
to be corrected (hi_edge=30 degrees)
time_sample array[n]; type: float
times (as seconds since start of orbit)
covering the entire orbit
left_sample array[n]; type: float
sky brightness at "left edge" of fov
(negative direction cosine angles)
set by smei_sky_cleanedge_median)
right_sample array[n]; type: float
sky brightness at "right edge" of fov
(positive direction cosine angles)
set by smei_sky_cleanedge_median)
OUTPUTS:
hi_sky array[3600,1200] or array[800,800]
corrected 2D hires skymap
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
INTERPOL, IsType, cvsmei
CALLED BY:
smei_sky_cleanedge_fov
RESTRICTIONS:
The units of the angles (degrees or radians) must be the
same for lo_fovx, lo_edge and hi_edge
PROCEDURE:
All bins in the hires sky map with direction cosine angle
greater than lo_edge in absolute value are corrected by
subtracted a fraction of the left_sample or right_sample
array.
The correction is largest at the edge of the fov
and drops of linearly with direction cosine angle to zero
at direction cosine angle lo_edge.
At direction cosine angle hi_edge the correction is
'fraction' times left_sample or right_sample.
For each skybin the time is used to determine the
appropriate left_sample or right_sample value by
linear interpolation on the two sample time series.
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_cleanedge_fov
PURPOSE:
Remove straylight from sky just outside edge
of camera field of view
CATEGORY:
ucsd/camera/idl/stars
CALLING SEQUENCE:
PRO smei_sky_cleanedge_fov, $
eq_sky = eq_sky , $
np_sky = np_sky , $
sp_sky = sp_sky , $
time_map = time_map , $
fovx_map = fovx_map , $
degrees = degrees , $
silent = silent
OPTIONAL INPUT PARAMETERS:
/degrees if set then the angles in fovx_map are in
degrees (default: radians)
/silent controls informational messages
eq_sky=eq_sky array[3600,1200]; type: float
np_sky=np_sky array[ 800, 800]; type: float
sp_sky=sp_sky array[ 800, 800]; type: float
2D hires sky maps: equatorial, north pole and
south pole
time_map=time_map array[720,360]; type: float
fovx_map=fovx_map array[720,360]; type: float
2D lores skymaps: time and fovx angle
OUTPUTS:
eq_sky=eq_sky array[3600,1200]; type: float
np_sky=np_sky array[ 800, 800]; type: float
sp_sky=sp_sky array[ 800, 800]; type: float
2D hires sky maps: equatorial, north pole and
south pole
with the straylight contribution from sky
just outside the fov removed
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, ToDegrees, ToRadians, destroyvar, gridgen, smei_sky_cleanedge_fix
smei_sky_cleanedge_median, smei_sky_cleanedge_sample
CALLED BY:
smei_sky_cleanedge_map, smei_star_remove
PROCEDURE:
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS)
MAY-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added check for number of valid lores element in time map.
There should be at least two valid elements in time_sample
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NAME:
smei_sky_cleanedge_map
PURPOSE:
Wrapper for smei_sky_cleanedge_fov for processing
a single Fits skymap.
CATEGORY:
ucsd/camera/idl/stars
CALLING SEQUENCE:
PRO smei_sky_cleanedge_map, file, $
overwrite = overwrite , $
degrees = degrees , $
silent = silent
INPUTS:
file scalar; type; string
fully-qualified file name of sky map
OPTIONAL INPUTS:
/degrees
/silent
/overwrite
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXADDPAR, FXPAR, GetFileSpec, HEADFITS, InitVar, READFITS, WRITEFITS, do_file
hide_env, smei_sky, smei_sky_cleanedge_fov
PROCEDURE:
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS)
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NAME:
smei_sky_cleanedge_median
PURPOSE:
Converts the data for sky bins in a one-degree strip
of sky along the left or right edge of the fov
(collected by smei_sky_cleanedge_sample) into
a time series at times time_sample
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
FUNCTION smei_sky_cleanedge_median, time, sky, time_sample, time_hbox
INPUTS:
time array[n]; type: float
times (as seconds since start of orbit)
for sky bins along left edge of fov.
sky array[n]; type: float
sky brightness for sky bins along left
edge of fov.
These arrays are output from smei_sky_cleanedge_sample
time_sample array[m]; type: float
equal-step array of times covering
entire orbit.
OUTPUTS:
sky_sample array[m]; type: float
sky brightness at times time_sample
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue
CALLED BY:
smei_sky_cleanedge_fov
PROCEDURE:
The sky_sample values are the median of all skybins
within time_hbox seconds of time_sample.
If no sky bins are present then sky_sample is set to
BadValue(0.0).
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS)
OCT-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Changed loop variable from short to long integer
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NAME:
smei_sky_cleanedge_sample
PURPOSE:
(for internal use by smei_sky_cleanedge_fov)
Accumulates bins from hires skymaps along strip of
sky close to edge of fov.
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
PRO smei_sky_cleanedge_sample , $
lo_fovx , lo_time , $ ; Lores direction cosine angle and time maps
hi_sky , $ ; Hires sky map
lo_edge , hi_edge , $ ; Inner and outer edge of strip used to make sample brightness
left_time , left_sky , $
right_time , right_sky , $
mode = mode
INPUTS:
lo_fovx array[720,360]; type: float
lo_time array[720,360]; type: float
2D lores skymaps: time and fovx angle
hi_sky array[3600,1200] or array[800,800]
2D hires skymap to be corrected
lo_edge scalar; inner edge of strip along edge fov
(lo_edge=29 degrees)
hi_edge scalar: outer edge of strip along edge fov
(hi_edge=30 degrees)
OUTPUTS:
left_time array[n]; type: float
times (as seconds since start of orbit)
for sky bins along left edge of fov.
left_sky array[n]; type: float
sky brightness for sky bins along left
edge of fov.
right_time array[n]; type: float
sky brightness for sky bins along right
edge of fov.
right_sky array[n]; type: float
sky brightness for sky bins along right
edge of fov
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
boost, cvsmei
CALLED BY:
smei_sky_cleanedge_fov
RESTRICTIONS:
The units of the angles (degrees are radians) must be the
same for lo_fovx, lo_edge and hi_edge
PROCEDURE:
Collects sky bins inside 1-degree strip along "left edge"
(negative direction cosine angles) and "right edge" (positive
direction cosine angles) of fov, and stores times in
left_time and right_sky, and sky brightnesses in
right_time and right_sky.
Bin times and brightnesses are tagged to the end of the
*_time and *_sky arrays, i.e. these arrays need to be
destroyed by the calling procedure prior to accumulating
sky bins for the three hires maps (equatorial, north pole
and south pole).
MODIFICATION HISTORY:
APR-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_cleantime
PURPOSE:
Removes averages from slices of a skymap that are between
two orbital time intervals, determined by the number of
slices. (default 360 slices)
CATEGORY:
camera/idl/toolbox
CALLING SEQUENCE:
FUNCTION smei_sky_cleantime , $
skymap , $ ; equatorial map
timemap , $ ; low-res orbtime map
cammap=cammap , $ ; low-res camera coverage map
camavg=camavg , $ ; camera or cameras to average
slices=slices ; number of time slices
INPUTS:
skymap array[720,360]; type: float
low res equatorial skymap
timemap array[720,360]; type: float
orbtime map
OPTIONAL INPUTS:
slices=slices scalar; type: float
number of slices to cut map
into for averaging times
camavg=camavg scalar or array; type: integer
camera or cameras to remove
average values from (default: 3)
must only contain integer values
1 2 or 3, or an array of those
eg. [1,2,3]
cammap=cammap array[720,360]; type: integer
map of camera coverage
(if either camavg or cammap are
not provided, then the entire
skymap will have the average
removed in slices
OUTPUT:
skymap array[720,360]; type: float
same as input map but with
time-slice averages removed
in specified camera only
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CONGRID, InitVar, MEAN
CALLED BY:
smei_sky
MODIFICATION HISTORY:
JAN-2010, John Clover (UCSD/CASS; jclover@ucsd.edu)
OCT-2010, John Clover
Added more flexibility, if nbin is changed in smei_sky, this should
catch it and adjust appropriately.
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NAME:
smei_sky_field
PURPOSE:
Maps keywords to Fits extension numbers in the
various types of SMEI skymaps
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_sky_field, files, $
exten_no = exten_no , $
equatraw = equatraw , $ ; sky, equ
northraw = northraw , $ ; sky, equ
southraw = southraw , $ ; sky, equ
equatcnt = equatcnt , $ ; sky
northcnt = northcnt , $ ; sky
southcnt = southcnt , $ ; sky
equatflat = equatflat , $ ; equ
northflat = northflat , $ ; equ
southflat = southflat , $ ; equ
equatstars = equatstars, $ ; equ
northstars = northstars, $ ; equ
southstars = southstars, $ ; equ
dirtysky = dirtysky , $ ; sky : SKYD__LO_SKY = 1
orbtime = orbtime , $ ; sky, equ, ecl : SKYD__LO_TIME = 2
orbsecs = orbsecs , $ ; sky, equ, ecl : SKYD__LO_SECS = 9
psfn = psfn , $ ; sky : SKYD__LO_PSFN = 3
psfe = psfe , $ ; sky : SKYD__LO_PSFE = 4
badsky = badsky , $ ; sky : SKYD__LO_CUT = 5
badhtm = badhtm , $ ; sky : SKYD__LO_FRAC = 6
fovx = fovx , $ ; sky, equ : SKYD__LO_FOVX = 10 Added in version 5.1
thetax = thetax , $ ; sky : SKYD__LO_ROTX = 7
thetay = thetay , $ ; sky : SKYD__LO_ROTY = 8
hits = hits , $ ; sky, equ, ecl : SKYD__LO_HIT = 11 Added in version 6.0
badpixels = badpixels , $ ; sky
sunsky = sunsky , $ ; ecl: helioecliptic sky map
sunflat = sunflat , $ ; ecl: helioecliptic sky map (flat)
suntime = suntime , $ ; ecl: helioecliptic orbit fraction
sunsecs = sunsecs , $ ; ecl: helioecliptic orbit time
sunhits = sunhits , $ ; ecl: helioecliptic contr pix count
fullsky = fullsky , $ ; ecl: equatorial lores skymap
fullflat = fullflat , $ ; ecl: equatorial lores skymap (flat)
hires_map = hires_map , $
lores_map = lores_map , $
eclsun_map = eclsun_map, $
frame_map = frame_map , $
adus_map = adus_map , $
angle_map = angle_map , $
cvsmei_mode = cvsmei_mode,$
droplist = droplist , $
count = count , $
map_types = map_types
INPUTS:
files array[n]; type: string
file names
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
result array[n]; type: integer
extension number (-1 if keyword does
not match an extension number)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, SyncArgs, SyncDims, smei_filename
CALLED BY:
qImage_cw_Property, qImage_cw_Where, qsmei_sky, qsmei_sky_pick, smei_sky
smei_sky_atlocation, smei_sky_read, smei_sky_track
PROCEDURE:
MODIFICATION HISTORY:
MAR-2008, Paul Hick (UCSD/CASS)
APR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keywords /sun*
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NAME:
smei_sky_getmask
PURPOSE:
Get SMEI mask at specified time and sky location(s)
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_sky_getmask, ut, ra, dec, $
equator = equator , $
degrees = degrees , $
scalar = scalar , $
silent = silent
INPUTS:
ut array[1]; type: time structure or valid time string
ra array[n]; type: float
right ascensions or ecliptic longitudes
dec array[m]; type: float
equatorial declinations or ecliptic latitudes
OPTIONAL INPUT PARAMETERS:
/equator if set, ra,dec are intepreted as equatorial coordinates
(default: ecliptic coordinates)
/degrees if set, all angles are in degrees (default: radians)
/scalar if set, a single position is returned as a scalar
instead of a 1-element array
silent=silent scalar; type: integer
larger numbers suppress more messages.
OUTPUTS:
R array[n.m]; type: float
mask values
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, CvSky, FILEPATH, InitVar, IsType, READFITS, TimeGet, TimeUnit, cvsmei, gridgen
hide_env, smei_filename, smei_filepath
CALLED BY:
vu_coronagraph, vu_earthskymap
PROCEDURE:
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_grd2fts
CALLING SEQUENCE:
PRO smei_sky_grd2fts, f
INCLUDE:
@compile_opt.pro
CALLS: ***
FXADDPAR, InitVar, IsType, MKHDR, REVERSE, WRITEFITS, grd_read
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NAME:
smei_sky_hdr2mode
PURPOSE:
Determines value of skymap 'mode' from Fits header
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_sky_hdr2mode, hdr
INPUTS:
hdr array[1]; type structure
OUTPUTS:
R scalar; type: string
one of ['npmap','spmap','eqmap','lores']
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FXPAR, IsType
CALLED BY:
smei_sky_atlocation, smei_sky_read
PROCEDURE:
Usually used to determine the value for the 'mode'
keyword for cvsmei.
MODIFICATION HISTORY:
MAR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_hdr2range
PURPOSE:
Determines break values for display of skymaps from Fits header
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_sky_hdr2range, hdr, difference=difference, degrees=degrees
INPUTS:
hdr array[1]; type structure
OUTPUTS:
R array; type: float
array[3]
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, FXPAR, InitVar, IsType, ToDegrees
CALLED BY:
smei_sky
PROCEDURE:
MODIFICATION HISTORY:
APR-2008, Paul Hick (UCSD/CASS)
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added ranges for star-subtracted maps in equ files, and
helioecliptic maps in ecl files.
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NAME:
smei_sky_hdr__define
PURPOSE:
Defines hdr structure or skymaps
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
PRO smei_sky_hdr__define
INPUTS:
(none)
OUTPUTS:
(none)
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_sky_read
PROCEDURE:
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
Extracted from smei_sky_read
JUL-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added ccd_mode (is filled only when reading
a hires equatorial map.
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NAME:
smei_sky_hdr_check
PURPOSE:
Align sky map headers for various routines
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
PRO smei_sky_hdr_check, hdrs, hdr
INPUTS:
hdrs structure; type: smei_sky_hdr
hdr structure; type: smei_sky_hdr
OUTPUTS:
hdrs=hdrs structure or array; type: smei_sky_hdr
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
boost
CALLED BY:
smei_sky
PROCEDURE:
smei_sky_hdr_check, hdrs, hdr
two headers to be compared
MODIFICATION HISTORY:
FEB-2010, John Clover (UCSD/CASS)
Compares two hdr structures for matching cameras and
returns them with the same dimensions
Still ignorant of modes, and prefers c3 to c3s unless
/prefer_smoothdark was used in caller (smei_sky)
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NAME:
smei_sky_read
PURPOSE:
Reads orbital skymaps
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
FUNCTION smei_sky_read, wanted_map, $
source = source , $
nbin = nbin , $
silent = silent , $
xgrid = xgrid , $
ygrid = ygrid , $
xedge = xedge , $
yedge = yedge , $
degrees = degrees , $
hdrs = hdrs , $
fixgain = fixgain , $
rmbkgnd = rmbkgnd , $
rmzld = rmzld , $
exten_no = exten_no , $
use_flat = use_flat , $
use_stars = use_stars , $
num = num , $
_extra = _extra
INPUTS:
wanted_map scalar, array[1]; type: numerical, time structure, or string
indicates the orbit(s) to be processed
(passed to smei_getfile together with _extra).
OPTIONAL INPUT PARAMETERS:
source=source scalar; type: string
source directory for skymaps
(the following keywords are processed by smei_sky_field)
/equatraw
/northraw
/southraw
/equatflat
/northflat
/southflat
/equatcnt
/northcnt
/southcnt
/equatstars
/northstars
/southstars
/dirtysky
/orbtime
/orbsecs
/psfn
/psfe
/badsky
/badhtm
/fovx
/thetax
/thetay
/hit
/badpixels
if none of these map types is selected then the hires maps
(equatorial,south and north pole) are put together into a
single equatorial map covering [-90,+90] degrees declination.
Note that this option also handles skymaps that contains
a single equatorial map covering the full latitude range.
nbin scalar; type: integer; default: 5
rebinning factor applied to high-resolution maps.
A rebinning with factor 5 results in maps
with 5 deg bins in RA and Dec.
/fixgain if set then sky brightnesses are corrected for changing
camera gain (see smei_camera_gain)
/use_flat if set for 'equ' and 'ecl' files then the
maps with subtracted stars replaced by a flat background
are used
OUTPUTS:
Result array; type: float
skymap (-1 if no skymap was read)
OPTIONAL OUTPUT PARAMETERS:
orbit scalar; type: integer
actual orbit number used
xgrid horizontal grid (bin centers)
ygrid vertical grid (bin centers)
xedge horizontal grid (bin edges)
yedge vertical grid (bin edges)
num=num array; type: integer
array of same size as returned skymap
Contains 1,2 or 3 identifying camera
that observed correspondig skybin
(contains 0 where skymap is empty).
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, BadValue, FILEPATH, FXPAR, HEADFITS, InitVar, IsType, MEAN, READFITS
TimeOp, TimeSet, ToDegrees, ToRadians, boost, cvsmei, destroyvar, gridgen, hide_env
smei_camera_gain, smei_filename, smei_filepath, smei_getfile, smei_sky_field
smei_sky_hdr2mode, smei_zld_model
EXTERNAL:
smei_sky_hdr__define
CALLED BY:
smei_getfile, smei_sky
PROCEDURE:
Way too complicated.
MODIFICATION HISTORY:
DEC-2004, Paul Hick (UCSD/CASS)
JUL-2006, Paul Hick (UCSD/CASS)
Added /fovx to extract Fits extension containing direction cosine
angle in long dimension. If the extension is not present then an
array with value of 15 degree everywhere is returned.
DEC-2007, Paul Hick (UCSD/CASS)
Added keyword /fixgain
APR-2008, Paul Hick (UCSD/CASS)
Added keyword /rmbkgnd and /rmzld to be able to remove
sidereal background and zodiacal light distribution.
MAY-2008, Paul Hick (UCSD/CASS)
Bugfixes in ZLD removal (missing degrees=degrees).
JUN-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added "num" keyword
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NAME:
smei_sky_testcase
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
PRO smei_sky_testcase
INPUTS:
OUTPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FXPAR, InitVar, READFITS, WhatIs, hide_env, who_am_i
PROCEDURE:
MODIFICATION HISTORY:
DEC-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_sky_track
PURPOSE:
Track location on sky
CATEGORY:
camera/idl/sky
CALLING SEQUENCE:
PRO smei_sky_track, wanted_map , $
body = body , $
degrees = degrees , $
rmbkgnd = rmbkgnd , $
rmzld = rmzld , $
range = range , $
destination = destination , $
equator = equator , $
fix_sun = fix_sun , $
step = step , $
rm_min_count= rm_min_count , $
_extra = _extra
INPUTS:
wanted_map scalar, array[1]; type: numerical, time structure,
or string
indicates the orbit(s) to be processed
(passed to smei_getfile together with _extra).
OPTIONAL INPUT PARAMETERS:
body=body array[2], type: float
ecliptic or equatorial coordinates
of fixed point on sky
scalar; type: string
name of one of the bodies for which
an ephemeris is available from big_eph
/degrees if set, all angles are in degrees
(default: radians)
/rmbkgnd if set, subtract sidereal background
(for 'sky' maps this is SET by default;
for 'equ' map this is NOT set by default)
/rmzld if set, subtract zodiacal light distribution
by default this is SET for both 'sky'
and 'equ' maps
range=range array[2]; type: float;
default: [-30,390] for 'sky' maps;
[-10, 10] for 'equ' maps
brightness range in ADUS
destination=destination
name of existing directory. If set this is
where gif images will be written
/equator keep horizontal parallel to equatorial plane
(default: parallel to ecliptic plane)
/fix_sun if set the direction to the Sun is kept on
the x-axis (left in a fish-eye plot)
step=step scalar; type: integer; default: 1
step size for processing the selected
map: only one of every 'step' maps is processed
rm_min_count=rm_min_count
scalar; type: integer: default: 0
the first 'rm_min_count' maps are used to create
a 'minimum skymap'. The minimum map is then
subtracted from the displayed map for all subsequent
skymaps.
_extra=_extra
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleUnits, BadValue, CheckDir, FILEPATH, FXPAR, InitVar, IsType, READFITS, SuperArray
TimeGet, TimeOp, TimeSet, TimeUnit, ToDegrees, ToRadians, UNIQ, big_eph, cvsmei, jpl_body
smei_filename, smei_getfile, smei_orbit_get, smei_orbit_set, smei_sky
smei_sky_field, smei_star_info
CALLED BY:
smei_star_show
PROCEDURE:
mei_sky_track,dest=getenv('PWD'),mode='equ',maxelo=10,/deg, $
chars=1.2,range=[-8,29.9],xysize=[400,400],nbin=1, /use_flat
MODIFICATION HISTORY:
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star__define
PURPOSE:
Defines structure to store fit parameters for stars
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star__define
INPUTS:
(none)
OUTPUTS:
(none)
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_star_fit
RESTRICTIONS:
If this structure is modified then the format statements in
smei_star_formatpnt need to be updated accordingly.
PROCEDURE:
The standard star is defined as a 200 x 200 array with bins
of 0.025 x 0.025 degrees (5 x 5 degree total).
The skymaps have bins of 0.1 x 0.1 degrees.
When a star is fitted to the 'standard star' locations in
a box of 50 x 50 bins (5 x 5 degrees) around the star are mapped into the
'standard star' map where 'standard brightnesses' are determined
by linear interpolation on the 'standard star' array. Fitting
the star involves matching observed 50 x 50 observed skymap brightnesses
against the 50 x 50 'standard brightnesses'.
The fit is done using skybins inside an area defined by the core PSF, and
(if wing_radius is used, instead of bkgnd_radius) additional bins
extending out to the selected wing_radius).
Let there be 'n' 0.1 x 0.1 bins in the skymap inside the (extended) PSF,
and let the skymap brightness in these bins be
(1) v(i) i=1,n
These values can be symbolically represented as:
(2) v(i) = a(i) + I(i) i=1,n
where a(i) is the background component, and I(i) the brightness
attributed to the star.
The locations in the skymap are mapped into the 'standard star' reference
frame. By linear interpolation the 'standard brightnesses' are:
(3) I_std(i) i=1,n
The fitting procedure generates an lsq 'model' for the star from
'standard star' values:
(4) v_model(i) = A(i) + B * I_std(i)
Here A(i) represents a planar fit to the background, and B is the
star brightness normalized to the 'standard star' brightness.
These fit quantities are stored in structure tags:
back_const
back_slope
bright
Let the extended PSF, mapped to the 'standard star' reference frame,
cover a total of 'N' 0.025 x 0.025 bins and let the 'standard
brightness' in these bins be
(5) J_std(N) i=i,N
The total number of ADUs in this area then is
(6) T(std) = Sum(i=1,N) {J_std(i)}
A similar sum can be defined from (3), based on 0.1 x 0.1 deg bins:
(7) U(std) = Sum(i=1,n) {I_std(i)}
Since
(8) N = (0.1/0.025)^2 x n = 16 x n
it follows
(9) U(std) = T(std)/16
or
U(std) x 0.1^2 = T(std) x 0.025^2
The quantity T(std) x 0.025^2 is stored in the structure tag 'total_adus'.
It is calculated in smei_star_stdmaps in the 'standard star'
reference frame (the right side of Eq. (9)).
There are two indirect ways to calculate the quantity 'B' in (4).
The first one is fairly trivial. v_model in Eq (4) is calcaluted as a
50 x 50 array, matching the box in the skymap. Looking at Eqs. (4)
and (9):
(10) B1 = Sum(i=1,n) {v_model(i)-A(i)) / U(std)
The second is an estimate based on the actual data 'v(i)' in Eq. (1),
and assuming that the fit worked:
(11) Sum(i=1,n) {v(i)} = Sum(i=1,n) {v_model(i)}
From (10) and (11) it follows:
(12) B2 = Sum(i=1,n) {v(i)-A(i)} / U(std)
B1 is stored in tag 'bright_mdl'; B1 is stored in tag 'bright_raw'.
If the bins used in the lsq fit would be the same set of bins used
to calculate the sum in Eq. (10), then B1 would be identical to
B in Eq. (4). For a number of reasons only a subset of the bins in
Eq (1) are actually used in the lsq fit. So B1 and B will not be
identical.
B2 in some sense is an indicator of the quality of the lsq fit. For
a perfect fit, B2 would be the same as B (Eq. 4). In reality, there
are systematic differences between B2 and B that are not understood.
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
Extracted from smei_star_fit
NOV-2006, Jordan Vaughan (UCSD; jtvaugha@ucsd.edu)
Added gain field to stars_fit
MAY-2007, Paul Hick (UCSD/CASS)
Changed scalar fovxangle to 2-element array fovangle
Added 2-element array dfovangle
JUL-2007, Paul Hick (UCSD/CASS)
Added psfstretch, renamed dfovangle to dpsfstretch
FEB-2008, Paul Hick (UCSD/CASS)
Added "remove" entry.
NOV-2011, Paul Hick (UCSD/CASS)
Expanded information in header considerably.
JUL-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added structure key 'total_area'
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NAME:
smei_star_alias
PURPOSE:
Translates aliases for star names to catalogue names
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_alias, alias
INPUTS:
alias scalar or array; type: string
star alias
OUTPUTS:
smei_star_alias same dimensions as 'alias'; type: string
name from SMEI catalogue
if the alias is not known the input
value is left unchanged.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
where_common
CALLED BY:
big_eph, smei_star_fitone, smei_star_list, smei_star_show
EXAMPLE:
name = smei_star_alias('Sirius')
returns
name = 'HD 48915'
PROCEDURE:
List of aliases and real names are hardcoded
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_box
PURPOSE:
Set up box around star centroid of about the same
size as the standard star map.
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_box, $
fullmap , $
maptype , $
std_ndim, $
ndim , $
xystar , $
ibeg , $
iend , $
jbeg , $
jend , $
rr , $
ibeg0=ibeg0, $
jbeg0=jbeg0
INPUTS:
fullmap scalar; type: integer
1 if array size 'ndim' is for a full skymap
0 if not.
Matters only for equatorial maps (maptype=0). For
full maps, if the box around the stars partly falls
outside the map (RA < 0 or RA > 360) then the box
can be filled using the opposite side of the map.
maptype scalar; type: integer
-1: south-polar map
0: equatorial map
1: north-polar map
Only used to test for equatorial map (for full maps,
see description of 'fullmap' argument.
std_ndim array[2]; type: integer
size of the standard star map (50x50)
ndim array[2]; type: integer
size of the skymap
xystar array[2]; type: double
array indices into the skymap (of size 'ndim')
of the star centroid
OUTPUTS:
result array[m], m <= std_ndim[0]; type: integer
see PROCEDURE
ibeg scalar; type: integer
jbeg scalar; type: integer
horizontal and vertical index values in the
returned 'rr' array for the lower-left corner
iend scalar; type: integer
jend scalar; type: integer
same for the upper-right corner
rr array[2,n], n <= std_ndim[0]*std_ndim[1]; type: double
see PROCEDURE
OPTIONAL OUTPUT PARAMETERS:
ibeg0=ibeg0 scalar; type: integer
jbeg0=jbeg0 scalar; type: integer
horizontal and vertical index values in 'rr' for
the lower-left corner before rows/columns
outside the map were truncated.
ibeg0=ibeg and jbeg0=jbeg if the lower-left corner
of the 'std_ndim' sized box lies inside the map;
if not then at least one of ibeg0 or jbeg0 will
be an invalid negative index into the skymap.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
gridgen
CALLED BY:
smei_star_corepsf, smei_star_fit
PROCEDURE:
rr[2,n] provides horizontal (xx[0,*]) and vertical (xx[1,*]) indices into
a skymap of dimensions 'ndim' for a square box of skylocations centered on
the star centroid 'xystar'. The size of the box is usually 'std_ndim', but is
smaller if part of the box falls outside the skymap.
result[n] is an array of horizontal indices into the skymap across the box.
If the whole box of size 'std_ndim' lies inside the skymap then
rr[2,n] gives locations for a box of size `std_ndim`; result[n] is of size
std_ndim[0]: result = reform(rr[0,std_ndim[0]) (i.e. a monotonic increasing
sequence for the horizontal locations of the bottom row of the box).
If part the box of size 'std_ndim' sticks out 'above' or 'below' of the map,
then the rows outside the map are removed and only coordinates of rows
inside the map are returned in rr[2,n]; n=nx x ny with ny < std_ndim[1].
If part of the box of size 'std_ndim' sticks out 'left' or 'right' of the map
then, for polar maps (maptype=+/-1) and for incomplete (fullmap=0) equatorial
(maptype=0) maps, the columns outside the map are remove, and only coordinates
for columns inside the map are returned in rr[2,n]; n = nx x ny with nx < std_ndim[0].
In this case it is still true result[nx] = rr[0:nx-1] (i.e. still a monotonic
increasing sequence of horizontal locations of the bottom row of the box.
For a complete (fullmap=1) equatorial (maptype=0) map, instead of truncating
columns from the box of size 'std_ndim' that extend below RA=0 or above RA=360,
the columns 'outside' the map are filled in by picking up colmns from the
opposite side of the map. In this case rr[2,n]; n=nx x ny with nx=std_ndim[0], and
result[nx] with nx=std_ndim[0]. rr[2,n] will contain invalid horizontal
indices for the columns outside the map. However, the locations in result[nx]
have been adjusted to reflect the 'wrap'-operation, and will contain valid
horizontal indices only. This 'result' array should be used by caller to index
the skymaps.
MODIFICATION HISTORY:
JUL-2007, Paul Hick (UCSD/CASS)
FEB-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added documentation
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NAME:
smei_star_cleanlist
CALLING SEQUENCE:
PRO smei_star_cleanlist
INCLUDE:
@compile_opt.pro
CALLS: ***
txt_read
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NAME:
smei_star_cleanup
PURPOSE:
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_cleanup, file, silent=silent
INPUTS:
OPTIONAL INPUTS:
OUTPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
GetFileSpec, SFLOAT, boost, flt_format, hide_env, smei_star_formatpnt
smei_star_info, smei_star_list, smei_star_standard, txt_read
PROCEDURE:
MODIFICATION HISTORY:
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NAME:
smei_star_corepsf
PURPOSE:
Create a skymap identifying the bins lying
inside the "core" PSF for the specified stars
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_corepsf, $
fullmap , $
camera , $
maptype , $
origin , $
scale , $
sky_ndim , $
std_ndim , $
ndim , $
nvalid , $
valid , $
stars_list, $
stars_fit , $
xystar , $
rastar , $
degrees = degrees , $
use_filled_psf = use_filled_psf, $
wing_radius = wing_radius , $
magnify = magnify
INPUTS:
fullmap scalar; type: integer
1 if array size 'ndim' is for a full skymap
0 if not
passed to smei_star_box
camera scalar; type: integer
camera number (1,2,3)
maptype scalar; type: integer
-1: south-polar map
0: equatorial map
1: north-polar map
passed to smei_star_box and smei_star_stdmaps
origin array[2]
passed to smei_star_stdmaps
scale scalar
passed to smei_star_stdmaps
sky_ndim array[2]; type: integer
size of output array 'result'
(usually the same as 'ndim' ????)
std_ndim array[2]; type: integer
size of standard star map (50x50)
passed to smei_star_box
ndim array[2]; type: integer
size of full skymap (see also 'fullmap')
nvalid scalar; type: integer
number of stars in 'valid' (i.e. n_elements(nvalid))
valid array[nvalid]; type: integer
(if nvalid=0 then valid=-1)
indices into the star arrays (stars_list, stars_fit, xystar
and rastar). Only stars in these arrays with indices
valid[i], i=nvalid-1,0,-1 are processed
stars_list array[n]; type: structure
contains general star info; only SMEI magnitude is used)
stars_fit array[n]; type: structure
contains skymap dependent star info; only psfangle and
fovangle are used.
xystar array[2,n]
star centroids as indices into skymap of size 'ndim'
rastar array[2,n]
star centroids in RA and dec
OPTIONAL INPUT PARAMETERS:
/degrees
/use_filled_psf
passed to smei_star_stdmaps
wing_radius = wing_radius
passed to smei_star_stdmaps
magnify = magnify
scalar; type: float; default: 0.0
some sort of offset applied to cos(fovangle)
OUTPUTS:
results array[sky_ndim[0],sky_ndim[1]]; type: float
skymap where the location of bright stars are marked
with there SMEI magnitude (see PROCEDURE).
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, ToRadians, smei_star_box, smei_star_info, smei_star_stdmaps
CALLED BY:
smei_star_fit
PROCEDURE:
The returned skymap is initialized to SMEI magnitude 100.
Then all stars in the 'valid' list are processed from faintest
to brightest star (as indicated by the SMEI magnitude in the
'star_list' structure. For each star all skybins in the 'core' PSF
(as determined by smei_star_stdmaps) are set to the SMEI magnitude.
Note that in overlapping PSF cores, the brightest magnitude will win.
MODIFICATION HISTORY:
JUL-2007, Paul Hick (UCSD/CASS)
FEB-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added documentation. Changed top_mags from 10 to 100.
The earlier value caused problem when fitting faint stars
that were given the wrong SMEI magnitude in the star catalogues.
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NAME:
smei_star_enough_bins
PURPOSE:
Used in smei_star_fit.pro to test whether the lsq fit
for a star needs to be executed or not.
CATEGORY:
ucsd/camera/idl/stars
CALLING SEQUENCE:
FUNCTION smei_star_enough_bins, $
fit_bkgnd , $
n_fitpsf , $
n_bkgnd , $
min_psf_bins = min_psf_bins , $
min_bkgnd_bins = min_bkgnd_bins
INPUTS:
fit_bkgnd scalar; type: integer
0: background and PSF fitted simultaneously
1: background fitted simultaneously from PSF
n_fitpsf scalar; type: integer
number of sky bins in PSF
n_bkgnd scalar; type:integer
number of sky bins in background area
(only relevant if fit_bkgnd=1)
OPTIONAL INPUT PARAMETERS:
min_psf_bins = min_psf_bins
scalar; type: integer; default: 25
lower limit on number of sky bins in PSF needed
for lsq fit to proceed
min_bkgnd_bins = min_bkgnd_bins
scalar; type: integer; default: 5
lower limit on number of background bin needed
for lsq fit to proceed
OUTPUTS:
result scalar; type: integer
0: do not do lsq fit
1: proceed with lsq fit
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar
CALLED BY:
smei_star_fit
MODIFICATION HISTORY:
APR-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_filename
PURPOSE:
Construct file name from star name, and v.v.
CATEGORY:
ucsd/camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_filename, star, reverse=reverse
INPUTS:
star array; type: string
star name, or file name (if /reverse SET)
OPTIONAL INPUT PARAMETERS:
/reverse if set, reverse translation
(from file name back to star name)
OUTPUTS:
result array; type: string
file name, or star name (if /reverse SET)
File names are 12 chars long
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar
CALLED BY:
smei_star_fitone, smei_star_show, smei_star_writepnt
PROCEDURE:
MODIFICATION HISTORY:
DEC-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_fit
PURPOSE:
Fit bright stars in sky map
CATEGORY:
ucsd/camera/idl/stars
CALLING SEQUENCE:
PRO smei_star_fit, file , $
hdr = hdr , $
sky = sky , $
camera = camera , $
ccd_mode = ccd_mode , $
origin = origin , $
scale = scale , $
southpole = southpole , $
northpole = northpole , $
torigin = torigin , $
time_map = time_map , $
psf_map = psf_map , $
fovx_map = fovx_map , $
nofovx = nofovx , $
stime = stime , $
etime = etime , $
final_sky = final_sky , $
flat_sky = flat_sky , $
star_sky = star_sky , $
star_fit = star_fit , $
star_info = star_info , $
count = count , $
upto_mags = upto_mags , $
bkgnd_origin= bkgnd_origin , $
bkgnd_radius= bkgnd_radius , $
bkgnd_count = bkgnd_count , $
wing_origin = wing_origin , $
wing_radius = wing_radius , $
auto_wing = auto_wing , $
star_list = star_list , $
star_remove = star_remove , $
star_index = star_index , $
catalogues = catalogues , $
degrees = degrees , $
kill_one = kill_one , $
fix_centroid= fix_centroid , $
fix_fovangle= fix_fovangle , $
fix_psfangle= fix_psfangle , $
fix_pattern = fix_pattern , $
noplane = noplane , $
noyzero = noyzero , $
use_filled_psf=use_filled_psf,$
use_weights = use_weights , $
weights = weights , $
skip_dist = skip_dist , $
incl_dist = incl_dist , $
max_stars = max_stars , $
badfit = badfit , $
show = show , $
area_show = area_show , $
max_show = max_show , $
min_show = min_show , $
silent = silent , $
sigma = sigma , $
magnify = magnify , $
;no_stars_mask = no_stars_mask , $
no_corepsf_mask = no_corepsf_mask, $
rmbkgnd = rmbkgnd , $
rmzld = rmzld , $
known_stars = known_stars , $
known_names = known_names , $
known_mags = known_mags
INPUTS:
file scalar; type; string
fully-qualified file name of sky map
OPTIONAL INPUT PARAMETERS:
/degrees if set then all angles are in degrees (default: radians)
hdr=hdr array[1]; type: structure
sky map header
sky=sky array[n,m]; type: float
2D sky map
camera=camera
ccd_mode=ccd_mode
origin=origin
scale=scale
/southpole if set, then fit stars in north polar map
/northpole if set, then fit stars in south polar map
By default stars are fit in the equatorial map
star_list=star_list array; type: SMEI_STAR_LIST structure
list of stars to be fitted
These can be extracted from the SMEI
star catalogues with smei_star_list.
array: type: string
alternatively a list of star names are specified
A call to smei_star_list is made to convert
the list to a SMEI_STAR_LIST structure
catalogues=catalogues scalar or array; type: string;
list of star catalogues to be used
Passed to smei_star_list.
NOT used if keyword star_list is set.
upto_mags=upto_mags scalar; type: float; default: 6.0
maximum SMEI magnitude; only stars
brighter than this are removed.
All other objects are fitted, but NOT removed
from the skymaps
bkgnd_origin=bkgnd_origin
array[2]; type: float
eventually processed by smei_star_standard.
bkgnd_radius=bkgnd_radius
scalar or array[2]; type: float
eventually processed by smei_star_standard.
bkgnd_count=bkgnd_count
scalar; type: float (<= 1.0) or integer (> 1)
passed to smei_star_lsqbins.
wing_origin=wing_origin array[2]; type: float
eventually processed by smei_star_standard.
wing_radius=wing_radius array[2]; type: float
eventually processed by smei_star_standard.
/auto_wing if set, then wing_radius varies with the SMEI magnitude as
wing_radius+0.1*(3-m_SMEI) degrees
i.e. the wing radius is smaller for fainter stars by
one high-res skybin (0.1 degrees) per magnitude.
wing_radius is set to 1.4 degrees if it is not defined.
(note that smei_star_standard will prevent the
wing_radius to drop below a minimum value though).
This keyword was added for use in the SMEI pipeline only,
to define a larger wing radius for very bright stars.
/fix_centroid if set, then the star centroid is included in the fit.
If multiple stars are fitted simultaneously then this will
adjust the centroid of the group of stars while keeping the
relative locations of the stars fixed (as implied by the
catalogue positions).
This keyword is primarily useful for correcting for pointing
errors, which affect all stars in a group in the same way.
/fix_pattern /fix_pattern implies /fix_centroid.
/fix_pattern has no effect for stars fitted individually.
if set, then for stars fitted simultaneously the centroids
of all stars in the group are adjusting individually
(changing the relative locations of the stars) to improve the fit.
/fix_psfangle if set, then the PSF angle is included in the fit
/fix_fovangle if set, then the direction cosine angles are included
in the fit.
(this slows down the star fitting considerably).
/noplane if set, suppress fit of planar background, and fit a
constant background instead (default: fit
planar background).
/noyzero passed to smei_star_lsqfit
/use_filled_psf passed to smei_star_standard
/use_weights passed to smei_star_lsqfit
weights=weights array[n,m]; type: float
Only used if /use_weights SET.
Weights to be used for skybins
/no_corepsf_mask by default, when a star is fitted, all skybins in the core PSF
of stars brighter then m_smei+2 are excluded from being
using in the fitting procedure.
Set this keyword to bypass this (bad idea!)
/kill_one by default, when multiple (nearby) stars are fitted simultaneously
all stars in the group are subtracted. If /kill_one is set the
group is fitted as a whole, but only the brightest star is subtracted
and the other stars will be fitted separately later.
skip_dist=skip_dist scalar; type: float; default: 0.25 degrees
nearby fainter stars at angular distances less
then 'skip_dist' away are not fit
incl_dist=incl_dist scalar; type: float; default: 0.75 degrees
nearby fainter stars at angular distances
less than 0.75 degrees (and more than /skip_dist)
are included when fitting a star.
max_stars=max_stars scalar; type: integer; default: 4
maximum number of stars fitted simultaneously.
If more than 'max_stars' stars pass the
'incl_dist' criterion, than only the
brightest 'max_stars-1' are included in the fit
(for a fit of max_stars stars).
sigma=sigma scalar; type: float
?
show=show scalar; type: star
name of star for which results are displayed
This should be one of the names from the
SMEI star catalogue.
Set show='*' to display results for all stars
Five views of the star are displayed:
- the area around the star in the original skymap
- the same area after the fit is subtracted
- the same area with the PSF replaced by the fitted background
- the same area showing the bins used in the fit
- a scatter plot of model vs. data
min_show scalar or array[2]; type: numeric; default: none
max_show scalar or array[2]; type: numeric; default: none
when keyword 'show' is set the display is auto-scaled
by default. These two keywords can be used to
set the dynamic range. If a scalar is set then the
value is used for all three diplays of the area around the
star. If a 2-element array is specified then the
1st value is used for the first display (the original
skymap), and the 2nd is used for the two subtracted
displays.
Sometimes it is convenient to be able to specify characteristics of certain 'known' stars,
rather than fitting them. There are two mechanisms in place to do this.
known_stars = known_stars
array[3,*]; type: float
specifies RA, dec and SMEI magnitude of a list of 'known' stars.
These stars are removed from the map prior to fitting other
stars by subtracting the standard star multiplied by the SMEI
brightness (as determined by smei_i2m from the SMEI magnitude)
at the specified location in the skymap.
Note that it is the responsibility of the user to find the
correct location and SMEI magnitude of the star. Note also
that these star do not need to be in one of the SMEI
star catalogues.
known_names array; type: string
known_mags array, same size as 'known_names'; type: numeric
list of stars (catalogue names and SMEI magnitudes)
of stars for which the brightness is considered
known. The brightness for these stars is not fitted.
Typically used when a non-variable star (with known
brightness), intrudes on the location of a variable
star of interest. Both stars can be fit simultaneously,
while keeping the brightness of the non-variable star
fixed, i.e. only the background and brightness of the
variable star is fit.
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
number of stars fitted (but not necessarily
subtracted)
count=0 if the skymap was not found or if
no stars with valid intensity or psf angle
were found.
If count=0 then star_fit will not exist.
star_fit=star_fit array[count]; SMEI_STAR_FIT structure
contains the fit results for all stars
star_index=star_index array[count]; integer
position of fitted star in original
star_list (useful only if star_list is
is one of the input arguments)
If count=0 then star_index = -1
final_sky=final_sky array[3600,1200] or array[800,800]
skymap with stars subtracted
flat_sky=flat_sky array[3600,1200] or array[800,800]
skymap with stars subtracted, but also with
the core PSF for each fitted star explicitly
replaced by the background model
star_sky=star_sky array[3600,1200] or array[800,800]
skymap containing the subtracted stars
If there is a problem reading the skymap Fits files
these variables will contain a scalar -1
If count=0 then final_sky and sky will contain the
unmodified input skymap, and star_sky will contain
zeroes.
area_show=area_show array[50,50,4]; type: float
If keyword 'show' is used, this returns the content
of the the four displays showing the area around
the star (after applying the min_show and max_show
keywords). Note that only the last display is saved,
so this keyword only makes sense if a single star
is specified in the 'show' keyword.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, AngleUnits, BadValue, CORRELATE, FXPAR, HEADFITS, InitVar, IsTime, IsType
MEAN, MagnifyArray, STDDEV, TimeGet, TimeLimits, TimeOp, TimeSet, TimeUnit, ToDegrees
ToRadians, boost, cvsmei, destroyvar, hide_env, jpl_body, jpl_eph, jpl_mag
smei_camera_gain, smei_coriolis, smei_i2m, smei_sky, smei_star_box
smei_star_corepsf, smei_star_enough_bins, smei_star_formatpnt, smei_star_info
smei_star_list, smei_star_lsqbins, smei_star_lsqfit, smei_star_standard
smei_star_stdmaps, sphere_distance, twin, usno_body, usno_eph, view, where_common
EXTERNAL:
smei_star__define
CALLED BY:
smei_findpnt, smei_star_fitone, smei_star_remove
PROCEDURE:
The information needed for the star removal is:
sky 2D-sky map
map type type of sky map (south pole, north pole, equatorial map)
origin array indices for RA=dec=0 (eq map) or indices of pole (polar map)
resolution number of degrees/radians per bin
camera SMEI camera (each camera has its own standard star map)
psf_map equatorial 2D-sky map with rotation angles for the stars
time_map equatorial 2D-sky map with times (secs since start of orbit)
This information can be supplied in a number of different ways:
1. Set 'file' to the fully-qualified file name of a sky map
All information is extracted from the file by smei_sky.
Information in other keywords is ignored.
Note that by default the equatorial map is processed, unless
/southpole or /northpole is set.
2. Set keyword 'hdr' to the header of a sky map previously read by
smei_sky. 'hdr' provides all the information needed,
include the map type (equatorial, south- or northpole).
The skymap itself can be supplied in keyword 'sky' (it probably
is available from the same smei_sky call that set 'hdr'. If absent
then the original skymap is read (the file name is in 'hdr').
All other keywords are ignored. The psf and time maps are always
read from file by smei_sky.
3. Explicitly provide all information in the appropriate keywords.
Defaults are set to the values currently used for the sky maps
produced by smei_skyd.
Stars are fitted and subtracted starting with the brightest stars
and working down to the fainter stars down to the cutoff magnitude
'upto_mags'.
Groups of upto 'max_stars' stars are fitted simultaneously. This group
is selected as follows:
- the first star in the group is the brightest star in the sky
that has not been fit yet.
- all stars within 'incl_dist' are added to the group
- the same is done iteratively for stars added to the group in this
way: for each a neighbourhood of 'incl_dist' is searched, and if
stars are found these are added to the group
- stop if no more stars are found within 'incl_dist' of any star
in the group, or if the group size exceeds 'max_crowd' members
- pass through all group members in order of decreasing brightness
and remove fainter stars that lie within 'skip_dist'. These
stars are marked as "done" immediately.
- only keep at most 'max_star' of the remaining stars are not
fitted on the assumption that its psf is indistinguishable from
the psf of the brighter star.
The results of the fit are by default subtracted for all the stars
in the group simultaneously. If /kill_single is set then only the
fit for the bright star is subtracted. The fainter stars will be
fitted again separately (after the bright star has been removed).
By default a planar (sloped) background is fitted. If keyword
/noplane is set then a constant background is fitted.
By default the star locations in the SMEI star catalogue are used
as fixed centroids. If keyword /fix_centroid is set then a brute
force iteration scheme is used to improve the fit by fitting the
centroid location also. This is mainly useful for detecting 'bad
quaternion' episodes in the SMEI data. Setting /fix_centroids
slows the program down considerably.
Fitting of the plane background and the star brightnesses is done
using linear least squares fits. lsqLinearFit implements fits
upto four dimension as analytic expressions, allowing for fitting
of two stars with a planar background of three stars with a constant
background. For fits in more dimension a matrix inversion is used.
The planets Mercury,Venus,Mars,Jupiter,Saturn and Uranus are
subtracted using their apparent visual magnitudes to control
the order of subtraction.
MODIFICATION HISTORY:
NOV-2005, Paul Hick (UCSD/CASS)
FEB-2006, Paul Hick (UCSD/CASS)
Replaced keyword /plane by keyword /noplane. By default
a sloped background is fitted unless suppressed by /noplane.
AUG-2006, Paul Hick (UCSD/CASS)
Keyword star_list can now also be a list of star names from
the SMEI catalogues.
If no stars are left to be fitted the procedure will now always
return with count=0 and final_sky and star_sky existing.
(it used to abort in some situations).
SEP-2006, Paul Hick (UCSD/CASS)
Added /use_filled_psf keyword
Added star_info keyword
NOV-2006, Jordan Vaughan (UCSD; jtvaugha@ucsd.edu)
Added gain field to star_fit
Set star_fit.close to '-' by default
FEB-2007, Jordan Vaughan, Paul Hick (UCSD/CASS)
Added stars_mask array, passed to smei_star_stdmaps
to exclude skybins from previously-subtracted star
from the background skybins.
APR-2007, Paul Hick (UCSD/CASS)
The lowres time map is now used as is (i.e. we do not
take the absolute value anymore).
MAY-2007, Paul Hick (UCSD/CASS)
Added keyword fix_psfangle fix_fovangle
In the iterative fitting a point far away from the
current best fit is now used in an attempt to speed up
the iteration when the starting point is far away from
the correct solution (seems to be most useful if
keyword /fix_fovangle is set).
JUN-2007, Paul Hick (UCSD/CASS)
Bug fix. psfwidth calculation for case with only one
skybin insided psf would crash.
JUL-2007, Paul Hick (UCSD/CASS)
Substantial rewrite of section that selects the
group of stars to be fitted simultaneously.
JAN-2008, Paul Hick (UCSD/CASS)
Modified storage of planet names in star_list
structure (left-adjusted, instead of right-adjusted)
FEB-2008, Paul Hick (UCSD/CASS)
Added star_fit.remove entry.
Added USNO asteroids and the 'stars_not_subtracted'
catalogue to list of point sources. These are fitted but
not subtracted from the sky map.
Bug fix in calculation of psfwidth (sometimes gave NaN).
MAR-2008, Paul Hick (UCSD/CASS)
Bugfix. The return arrays final_sky, flat_sky and
star_sky would not exist if count=0 (no stars subtracted).
Now final_sky and flat_sky contain the input map,
and star_sky contains zeroes.
APR-2008, Paul Hick (UCSD/CASS)
Made sure that dradec is really zero when no centroid
fitting is done (used to be a really small number
sometimes instead of identical to zero).
Added keyword weights. Added keyword original_weights
to all smei_star_lsqfit calls.
JUL-2008, Paul Hick (UCSD/CASS)
Added keyword /fix_pattern to allow adjusting of centroids
of individual stars when multiple stars are fitted
simulataneously.
FEB-2010, Paul Hick (UCSD/CASS)
Added keyword area_show. Added documentation.
Fixed bug in processing of keyword star_list (would crash
if none of the stars on the list would be in one of
the selected SMEI star catalogues).
JUN-2010, Paul Hick (UCSD/CASS)
Fixed bug in the construction of flat_sky array (pieces
of final_sky were erroneously copied into flat_sky)
JUN-2010, John Clover (UCSD/CASS)
Bumped incl_dist to 1.0 degrees
APR-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added more checks in the iteration procedures to pick up
cases where there are not enough bins left for an lsq fit
(also prevents crashes due to an 'array index out of
range' error on an empty index array when no bins are
left at all)
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NAME:
smei_star_fitone
PURPOSE:
Fit specified star(s) for all skymaps in specified
time range, and write results to file
CATEGORY:
sat/idl/star
CALLING SEQUENCE:
PRO smei_star_fitone, name, tt , $
camera = camera , $
mode = mode , $
rmbkgnd = rmbkgnd , $
destination = destination , $
show_ = show_ , $
movie = movie , $
_extra = _extra
INPUTS:
name scalar, array[n]; type: string; default: Sirius
name(s) of star
tt array[2]; type: time structure
time range
OPTIONAL INPUT PARAMETERS:
camera=camera
scalar; type: integer
camera number (1,2,3)
mode=mode
scalar; type: string; default: 'sky'
skymap type: 'sky' or 'equ'
/rmbkgnd
destination=destination
scalar; type: string; default: none
name of existing directory where output
file is written
/movie if set, create an animated gif
(requires that 'destination' is set)
_extra=_extra
additional keywords for smei_star_fit
OUTPUTS:
(to file)
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
smei_star_fit__define
CALLS: ***
CheckDir, FILEPATH, GetFileSpec, InitVar, IsType, MagnifyArray, WhatIs, boost, mk_flick
smei_getfile, smei_star_alias, smei_star_filename, smei_star_fit, smei_star_info
smei_star_list, smei_star_writepnt
EXAMPLE:
smei_star_fitone,['V598 Puppis','HD 54153'],cat='*',skip_dist=0.1, /degrees,/fix_centroid,rmbkgnd = 0, $
known_stars=[106.51,-38.40,5.68]
PROCEDURE:
MODIFICATION HISTORY:
SEP-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_formatpnt
PURPOSE:
Controls formatting of time series files
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_formatpnt , $
get_titles = get_titles , $
get_format = get_format , $
get_timefmt = get_timefmt , $
old_format = old_format
OUTPUTS:
/get_titles if set then return string of column titles that preceeds the numbers
in the time series files
/get_format if set then return the format string used to write the smei_star_fit
structures produced by smei_star_fit
/get_timefmt if set then return the format used to write the time of observation
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar
CALLED BY:
smei_fixpnt, smei_star_cleanup, smei_star_fit, smei_star_readpnt
smei_star_writepnt
PROCEDURE:
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
NOV-2006, Jordan Vaughan (UCSD; jtvaugha@ucsd.edu)
Added gain column to PNT titles, formatc, and format
MAY-2007, Paul Hick (UCSD/CASS)
Modified to take changes in smei_star__define into
account (changed scalar fovxangle to 2-element
array fovangle; added dfovangle)
JUL-2007, Paul Hick (UCSD/CASS)
Modified to take changes in smei_star__define into
account
JAN-2008, Paul Hick (UCSD/CASS)
Fixed bug in format (star name has 12 chars, not 11)
FEB-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added X column (point source removed from skymap)
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NAME:
smei_star_info
PURPOSE:
Retrieves info about stars from the SMEI star catalogue
CATEGORY:
CALLING SEQUENCE:
FUNCTION smei_star_info, star, $
degrees = degrees , $
count = count , $
get_ra_dec = get_ra_dec, $
rectangular = rectangular,$
get_struct = get_struct, $
get_number = get_number, $
get_name = get_name , $
get_obafg = get_obafg , $
get_magv = get_magv , $
get_magb = get_magb , $
get_mags = get_mags , $
_extra = _extra
INPUTS:
star array; type: structure
smei_star_list structure returned by smei_star_list.
OPTIONAL INPUT PARAMETERS:
/get_number get number from smei catalogue
/get_ra_dec get RA and declination (this is also the default)
/get_name get ascii name for star
/get_obafg get spectral class
/get_magv get visual magnitude
/get_magb get blue magnitude
/get_mags get SMEI magnitude
If 'star' does not exist on input, or is not specified then smei_star_list
is called to read the star catalogues. All keywords to smei_star_list can be
used to control which star catalogues are read.
OUTPUTS:
result array[2,*] or array[*]; type: depends on keywords
if none of the /get* keywords is set then the
equatorial location of the stars are returned in
radians or degrees
(depending on setting of /degrees keyword).
array[0,*] is the right ascension
array[1,*] is the declination
Otherwise the quantity indicated by the get* keyword
is returned.
OPTIONAL OUTPUT PARAMETERS:
star if 'star' does not exist on input then the result from a
call to smei_star_list is returned
count=count # stars in 'star' structure
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleUnits, CV_COORD, InitVar, IsType, smei_star_list
CALLED BY:
PRO bolstrip, big_eph, qEphem_State, smei_findpnt, smei_fixpnt, smei_frm_where
smei_sky_track, smei_star_cleanup, smei_star_corepsf, smei_star_fit
smei_star_fitone, smei_star_list, smei_star_show, smei_star_test, stardistance
PROCEDURE:
Returns fields from the 'star' structure
MODIFICATION HISTORY:
FEB-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_list
PURPOSE:
Reads content of star catalogues used for star subtraction in SMEI frames
CATEGORY:
camera
CALLING SEQUENCE:
FUNCTION smei_star_list , $
root = root , $
silent = silent , $
count = count , $
name = name , $
catalogues = catalogues, $
get_format = get_format, $
rmstar = rmstar
OPTIONAL INPUT PARAMETERS:
root=root scalar; type: string
directory where star catalogue files are located.
By default, this is the directory where this
file is located.
name=name array; type: string
list of star names; only the data for the
specified stars are returned. These MUST be names
present in the SMEI star catalogues.
catalogues scalar or array; type: string;
default: ['brightstars','variables_4th','big_variables','duhstars']
list of catalogues to be used. Must be one or more of
the entries on the defaults list (lowercase! and NO typos!).
/silent suppresses informational messages
/get_format if set, return the format used for the bright star catalogue
OUTPUTS:
star array; type: SMEI_STAR_LIST structure
if 'name' NOT specified:
all stars in the selected catalogues
if 'name' specified:
array of length n_elements(name)
OPTIONAL OUTPUT PARAMETERS:
count=count scalar; type: integer
# stars in return array 'star'
rmstar=rmstar array; type: byte
0: star should be fitted but not subtracted from skymap
1: star should be fitted and subtracted from skymap
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, GetFileSpec, InitVar, IsType, UNIQ, destroyvar, smei_star_alias
smei_star_info, txt_read, where_common, who_am_i
EXTERNAL:
smei_star_list__define
CALLED BY:
PRO bold, qEphem_State, smei_findobj, smei_mki2m, smei_star_cleanup, smei_star_fit
smei_star_fitone, smei_star_info, smei_star_test, stardistance
RESTRICTIONS:
Small declinations (-1<lat<0) need special attention: the minus sign
needs to be put in front of the first non-zero component (i.e. minutes
or arcseconds)
PROCEDURE:
MODIFICATION HISTORY:
JAN-2003, Paul Hick (UCSD/CASS)
MAR-2003, Paul Hick (UCSD/CASS)
Rewrite to deal with single bright star catalogue
JAN-2004, Paul Hick (UCSD/CASS)
Added big_variables.txt and variables_4th.txt
NOV-2005, Paul Hick (UCSD/CASS)
Removed duplicate entries from list of stars (this should take
care of the overlap between 'brightstars' and 'big_variables'
catalogues.
MAR-2008, Paul Hick (UCSD/CASS)
Removed keyword 'pos'. Added 'duhstars' catalogue.
DEC-2008, Paul Hick (UCSD/CASS)
Added 'nova_list' catalogue.
Edited 'big_variables' catalogue to make format the same as
all other catalogues
MAY-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added some code to report detection of duplicate names in the
star catalogues. These are removed (but this was done quietly
before).
Also merged big_variables.txt and variables_4th.txt with the
main brightstars.txt catalogue. Almost all of the variables
already were present in brightstars already. The original
brightstars.txt file is saved as brightstars_original.txt.
JUL-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Bugfix. The default value for keyword 'catalogues' after
merging of three catalogues is the first two (instead of
four) catalogues hardcoded.
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NAME:
smei_star_list__define
PURPOSE:
Defines structure for star in SMEI star catalogues
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_list__define
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_star_list
PROCEDURE:
MODIFICATION HISTORY:
FEB-2008, Paul (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_lsqbins
PURPOSE:
Refine PSF and background area definition based on
properties of the original star.
CATEGORY:
CALLING SEQUENCE:
PRO smei_star_lsqbins, original_star, rr, rr0, in_psf, in_bkgnd, bkgnd_count=bkgnd_count
INPUTS:
original_star array[nx,ny]; type: float
area from original skymap around the star to be subtracted
(current a 50x50 box i.e 5x5 degrees)
rr array[2,nx*ny]; type: integer??
column and row indices into original skymap for all bins
in original_star
rr0 array[2,nx*ny]; type: float
x,y locations relative to the centroid of the star
(in the same units as rr, i.e. bin spacings)
in_psf array[nx,ny]; type: byte
1: bin is inside the PSF
0: bin is outside the PSF
in_bkgnd array[nx,ny]; type: byte
1: bin is included in background area
0: bin is not included in background area
OPTIONAL INPUT PARAMETERS:
bkgnd_count=bkgnd_count
scalar; type: float (<=1.0) or integer (n > 1)
sets the maximum number of pixels to be retained for
the background area (in the in_bkgnd array).
bkgnd_count > 1 : maximum number of bins to be retained
bkgnd_count <= 1.0: maximum fraction of current number of
background bins to be retained
OUTPUTS:
in_psf updated, bins where original_star is NaN are set to zero
in_bkgnd updated, bins where original_star is NaN are set to zero, and
the number of bins in in_bkgnd is reduced to match the input
given in bkgn_count
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType
CALLED BY:
smei_star_fit
PROCEDURE:
The first filter on in_psf and in_bkgnd is that only bins with finite
values in original star are left non-zero.
If bkgnd_count is defined then the background array in_bkgnd is modified
so that at most bkgnd_count bins are left non-zero. These will be the bins
in the background with the lowest value in original_star.
Note that in_bkgnd is NOT modified if there are already less than
bkgnd_count bins in it.
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_lsqfit
PURPOSE:
Performs multi-dimensional least-squares fit between
observed star and standard star
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_lsqfit, $
rr , $
standard_stars , $
original_star , $
in_fullpsf , $
in_fitpsf , $
in_bckgnd , $
back , $
bright , $
sigma = sigma , $
only = only , $
noplane = noplane , $
noyzero = noyzero , $
bkgnd_model = bkgnd_model , $
one_star_model = one_star_model, $
use_weights = use_weights , $
original_weights= original_weights,$
fixed_bright = fixed_bright
INPUTS:
rr array[2,n]; type: float
position vectors for all bins in the box around
the star, relative to the star centroid
(in units of the bin size of the skymap from
which the star was extracted).
standard_stars array[n,m]; type: float
intensities in equivalent locations in standard
star for all bins around star
The 2nd dimension indicates the m stars fitted
simultaneously (absent if m=1)
original_star array[nx,ny] (with nx*ny=n); type: float
intensities in box around star as extracted
from the original skymap.
in_fullpsf array; type: long
list of array indices into rr, standard_stars and
original_star that defines the full area of the
PSF used to define the star model.
in_fullpsf is almost, but not quite,
in_fullpsf = total(standard_stars GT 0.0,2) GT 0
in_fitpsf array; type: long
list of array indices into rr, standard_stars and
original_star that should be used to fit the star.
in_fitpsf is a subset of in_fullpsf
(see smei_star_stdmaps).
in_bckgnd array; type: long
list of array indices to be used to fit the background.
If this is a valid list of indices (i.e. if
in_bckgnd[0] NE -1 then these pixels are used to fit
a background separately from the fit to the PSF.
The fit is to a plane or, if /noplane, is SET the
mean of the background pixels is used.
OPTIONAL INPUTS:
sigma=sigma scalar; type: float
if set then a second fit is made after discarding
bins that are more than 'sigma' standard deviations
in the residual after the first fit.
only=only array; type: integer
set of indices into the 'in_fitpsf' array
Only the subset of bins in 'only' are used in the fit
(this is only used in this procedure for a recursive
call when keyword sigma is used).
/noplane if set, then fit constant background (i.e. do
not fit a sloped background
/noyzero passed to lsqLinearFit for fitting of PSF only if
background and PSF are fitted separately (i.e. if
in_bckgnd contains a valid list of background bins)
original_weights=original_weights
array[nx,ny] (with nx*ny=n); type: float;
default: 1.0/(50.0+original_star) (See PROCEDURE)
Only used if /use_weights SET.
Weights to be used for each skybin in the lsq fit.
/use_weights if set, the fit is done using weights specified in
keyword original_weights.
fixed_bright=fixed_bright
array[m]; type: float
can be used to fix the brightness for one or more of the
m stars. Should be set to the brightness of the star(s)
that need to be 'frozen'. All other values should be set
to NaN (i.e. BadValue(0.0))
Usually output values from the keyword 'bright' of this
procedure obtained from previous fit are used. This can
be used for instance to separate a variable star (say a nova)
from a non-variable close neighbour. The close neighbour
can be fit from pre-nova data, and the result can then be
used to freeze the brightness during the nova outburst.
OUTPUTS:
Result array[nx,ny]; type: float
the resulting lsq fit to the PSFs of all stars fitted
simultaneously. This is the 'best fit' model for the
m stars combined:
star_model[nx,ny] = (Sum(m))bright[m]*standard_stars[n,m]
back array[3]; type: float
constants for fit of background
back[0] intensity at the centroid of the star
(i.e. at the origin of the rr position vectors)
back[1:2] horizontal and vertical slope of the background
bright array[m]; type: float
brightness fit for all stars
OPTIONAL OUTPUTS:
bkgnd_model=bkgnd_model
array[nx,ny]; type: float
the resulting lsq fit for the planar background
one_star_model=one_star_model
array[nx,ny,n]; type: float
the resulting lsq fit to the brightest of the stars
one_star_model[nx,ny,i] = bright[i]*standard_stars[n,i]
This is equal to the return value if only one star is fitted
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, MEAN, MagnifyArray, STDDEV, destroyvar, lsqLinearFit, view
CALLED BY:
smei_star_fit
PROCEDURE:
Note if /use_weights is set then the default weight used
is 1.0/(50.0+original_star).
The 50.0 is an estimate for the brightness of the darkest sky.
The reason for using it is to avoid extremely large weights for
background skybins when original_star already has the sidereal
background and the zodiacal light removed (resulting in a
residual background that is essentially zero).
MODIFICATION HISTORY:
DEC-2006, Paul Hick (UCSD/CASS)
AUG-2006, Paul Hick (UCSD/CASS)
Added in_bckgnd argument to be able to fit background and
star separately
APR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword original_weights.
Changed default weights from 1/original_star
to 1/(50+original_star).
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NAME:
smei_star_make
PURPOSE:
Create star structure from RA,Dec
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_make, radec, $
name = name , $
mags = mags , $
magv = magv , $
magb = magb , $
degrees = degrees
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleUnits, IsType
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
MAY-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_readpnt
PURPOSE:
Reads time series files into smei_star_fit structure
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_readpnt, filename, stars, $
hdr = hdr , $
nohdr = nohdr , $
error_message = error_message, $
silent = silent
INPUTS:
filename scalar; type: string
fully-qualified filename
OUTPUTS:
smei_star_readpnt
OPTIONAL OUTPUT PARAMETERS:
hdr=hdr array; type: string
header (lines at beginning of file starting
with semi-colon)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, boost, destroyvar, do_file, gunzip_file, hide_env, smei_star_formatpnt
EXTERNAL:
smei_star_fit__define
CALLED BY:
PRO bold, skyd_version, smei_findobj, smei_mki2m, smei_star_show, smei_star_split
smei_star_test
PROCEDURE:
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
SEP-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added hdr keyword
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NAME:
smei_star_remove
PURPOSE:
Removes bright stars from SMEI orbital sky maps
CATEGORY:
ucsd/camera/idl/star
CALLING SEQUENCE:
PRO smei_star_remove, wanted_map, $
destination = destination , $
to_smeidb = to_smeidb , $
checkversion = checkversion , $
overwrite = overwrite , $
force = force , $
silent = silent , $
keepbkgnd = keepbkgnd , $
fit_with_nobkgnd = fit_with_nobkgnd , $
cleanedge = cleanedge , $
version = version , $
get_version = get_version , $
reverse_loop = reverse_loop , $
use_bkgnd_version = use_bkgnd_version , $
use_zld_version = use_zld_version , $
_extra = _extra
INPUTS:
wanted_map array[n]; type: string, time structure or integer
passed to smei_getfile
Selects skymap files to be processed
OPTIONAL INPUT PARAMETERS:
/to_smeidb if set, write to directory structure as used
for SMEI data base (separate subdirs for mode
and camera) with 'destination' as the base dir.
destination scalar; type: string; default: $TUB
array[2]; type: string
destination directory for skymaps and time series file
if /to_smeidb NOT set then maps are written
directly to 'destination'.
The default in this case is $TUB
if /to_smeidb SET then files are written to
a directory structure as used for the
SMEI data base with 'destination' as the
base directory.
The default in this case is 'SMEIDB?' (the
SMEI database).
If two directories are specified the first is used
for the skymap and the second for the time series
If destination includes a "user@host:" identifier then
the output is created locally in $TUB
and is then transferred to the remote host using scp;
the local files are deleted after the transfer;
note that this will only work if the remote host has
been configured for ssh using private/public keys
allowing login without passwords.
/overwrite forces overwriting of existing skymaps and timeseries files
(by default no files are overwritten)
/checkversion if present, files will be overwritten only if the current
star subtraction version number and the current sidereal
background version is higher then the version in the Fits
header of the skymap.
(if /keepbkgnd is set then the background version is not
checked)
silent=silent if set, suppresses informational messages
upto_mags=upto_mags
scalar; type: float; default: 6.0
maximum SMEI magnitude; only stars brighter than this
are removed. (passed to smei_star_fit)
/keepbkgnd if set, the sidereal background (Milky Way, faint stars,
etc.) is not subtracted from the skymaps after
the bright stars are subtracted.
/cleanedge if set, a correction is made for straylight from sky
just outside the fov into the outer areas (direction
cosine angles larger than 20 deg) of the camera fov.
/fit_with_nobkgnd if set, stars are fit with the sidereal background removed
_extra=_extra The _extra keyword is passed to smei_star_fit,
and smei_getfile, so check those for
additional input keywords.
/get_version retrieve software version number
(returned in keyword "version")
use_bkgnd_version=use_bkgnd_version
scalar; type: integer 1,2 or 3; default: 3
selects the sidereal background map
use_zld_version=use_zld_version
scalar; type: integer 1,2,3,4; default: 4
selects the zodiacal brightness model
(passed to smei_zld_model)
OUTPUTS:
Files in destination directory
OPTIONAL OUTPUTS:
version=version Only defined if /get_version is set
array[2]; type: float
version[0]: version of bright star subtraction
version[1]: version of sidereal background map
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, CheckDir, FILEPATH, FXADDPAR, FXPAR, GetFileSpec, HEADFITS, InitVar
IsType, MKHDR, READFITS, TimeGet, TimeOp, TimeSystem, TimeUnit, WRITEFITS, boost, cvsmei
destroyvar, do_file, gzip_file, hide_env, smei_camera_gain, smei_filename
smei_filepath, smei_getfile, smei_sky, smei_sky_cleanedge_fov, smei_star_fit
smei_star_writepnt, smei_zld_model
CALLED BY:
remove_stars, remove_stars_c3s, remove_stars_m0, smei_star_update
EXAMPLE:
smei_star_remove, 1500
Subtract stars for orbit 1500 (specified as integer) for camera 1
smei_star_remove, smei_coriolis([1500,1501]), camera=1
Subtract stars for orbits 1500 and 1501 (specified as time
structure) for camera 1
smei_star_remove, '2003/04/16 18:25:57'
Subtract stars for orbit 1500 specified as time string
smei_star_remove, '*.fts.gz'
Use dialog_pickfile to select single skymap
smei_star_remove, 'c1sky_2006_045_021031.fts.gz'
Subtract stars for specified map
PROCEDURE:
For each skymap a new skymap (Fits file) with the star-subtracted
maps is created, and an ASCII file with information about the
fitted stars. Both files are created in the directories
specified in keyword 'destination'.
The current star subtraction is build around the following
set of keywords:
smei_star_remove, f, /cleanedge, /use_weights, /auto_wing
This implies a wind_radius value of 1.4 degrees.
A good way to redo a section of maps in a time range 'trange' in the SMEI
skymap data base on $SMEISKY0 is the command:
smei_star_remove, trange,cam=3,/cleanedge,/use_weights,/auto_wing, $
/checkversion,silent=3,/to_smeidb
MODIFICATION HISTORY:
NOV-2005, Paul Hick (UCSD/CASS)
JUN-2006, Paul Hick (UCSD/CASS)
Modified to accept arrays as input in wanted_map argument.
JUN-2006, Paul Hick (UCSD/CASS)
Added Fits keyword VERSION to sky map
Added NAME, CREATED and VERSION keywords to time series file
Added keyword /overwrite
JUL-2006, Jordan Vaughan, Paul Hick (UCSD/CASS) V2.0
Added subtraction of sidereal background map (can be disabled
by keyword /keepbkgnd)
Added two extensions (copied from original skymap):
-extension 6: fraction of orbit (extension 7 from original skymap)
-extension 7: time in sec since first frame used
(extension 14 from original skymap)
Keyword VERSION is now called BSTARVER (to distinguish it from
keyword BKGNDVER (the version of the sidereal background map)
Keyword MILKYWAY is now called BKGND
If the sidereal backgound is subtracted keyword BKGND is set
to 1, and two more keywords are added:
BKGNDVER is the version of the sidereal background map
BKGAIN is the gain correction (multiplicative factor) applied
to the sidereal background map before subtracting it.
Fixed problem with header for extension 4 (map of removed stars
in equatorial map.
AUG-2006, Paul Hick (UCSD/CASS) V3.0
Modifications related to separate fitting of background and PSF.
Added couple of entries to smei_star_fit structure.
Time series file is now written by procedure smei_star_writepnt
AUG-2006, Paul Hick (UCSD/CASS) V3.0
Padded records in time series file with 5 spaces to make them
exactly the same length as the titles record.
SEP-2006, Paul Hick (UCSD/CASS) V3.1
Added /use_filled_psf keyword
Added star_info keyword to smei_star_fit and smei_star_writepnt
NOV-2006, Paul Hick (UCSD/CASS) V4.0
Rearranged layout of time series file
Added extension (lowres map copied from original skymap)
-extension 8: number of pixels per skybin
(extension 16 from original skymap)
MAR-2007, Paul Hick (UCSD/CASS) V4.1
Added extension (lowres map copied from original skymap)
-extension 8: direction cosine angle
(extension 15 from original skymap)
-extension 9: old extension 8 (pixels per skybin)
APR-2007, Paul Hick (UCSD/CASS) V4.2
Added cleanedge keyword to allow removal of straylight
from sky just outside the camera fov.
MAY-2007, Paul Hick (UCSD/CASS) V4.3
Modified fovangle field and added dfovangle field
to star_fit structure
MAY-2007, Paul Hick (UCSD/CASS) V4.31
If keywords /cleanedge is set and /keepbkgnd NOT set,
then the sidereal background is added again AFTER
the star subtraction, and PRIOR to the removal of
the scattered light along the edge of the FOV. After
the scattered light correction the sidereal background
is taken out again.
Added keyword /to_smeidb to write directly into SMEI data base
Added keyword remote to do transfers to remote host
JUN-2007, Paul Hick (UCSD/CASS)
Added keyword /from_smeidb
JUL-2007, Paul Hick (UCSD/CASS)
Bug fix. removebkgnd was written into Fits file as byte
instead of short int.
JUL-2007, Paul Hick (UCSD/CASS), V5.01
Added three extensions to output Fits file.
These contain 3 skymaps (equatorial,north and south pole)
with the stars subtracted and the core PSF replaced by
the background model.
Modified use of area defined with wing_radius. Bins in this
area that are part of the core PSF of a brighter neighbour
star (which has been subtracted already) are excluded from
being used in the lsq fit. They are still used when the
star model is subtracted.
Removed keywords wing_radius and use_filled_psf
(now passed to smei_star_fit using _extra keyword).
NOV-2007, Paul Hick (UCSD/CASS), V5.02
Fixes bug in calculation of camera gain for cameras 1 and 3
smei_camera_gain.
DEC-2007, Paul Hick (UCSD/CASS), V5.03
Added /inside_range keyword to be able to process
files in a specified time range (specified as a 2-element
time array in 'wanted_map')
Changed keyword CREATED in time series file to DATE.
Shortened header for equatorial maps in ext 3 and 6
(TX1MOON, TX2MOON, TX3MOON removed).
DEC-2007, Paul Hick (UCSD/CASS), V5.04
Added two lines to header for timeseries files
(clean edge and remove bkgnd keywords)
DEC-2007, Paul Hick (UCSD/CASS), V5.05
Added some more keyword to timeseries header:
BSTAR,BSTARVER,BKGNDVER,BKGAIN,CLNEDGE
(these are also present in the Fits file with the
star-subtracted skymaps).
DEC-2007, Paul Hick (UCSD/CASS), V5.06
Added keywords ONEORBIT and ORBIT to timeseries header.
JAN-2008, Paul Hick (UCSD/CASS), V5.07
Fixed some format issues in pnt file.
Star name was truncated at 11 char, should be 12.
Planet names were print right-adjusted, should be
left-adjusted
FEB-2008, Paul Hick (UCSD/CASS)
Location of files now done using smei_getfile.
Removed keyword remote (functionally is now provided by
keyword destination).
FEB-2008, Paul Hick (UCSD/CASS), V5.10
Added star_fit.remove entry.
Bug fix in calculation of psfwidth (sometimes gave NaN).
FEB-2008, Paul Hick (UCSD/CASS), V5.11
Added USNO asteroids and 'stars_not_subtracted' catalogue to
list of point sources (these are fitted, but not subtracted).
MAR-2008, Paul Hick (UCSD/CASS), V5.12
Added keyword SMEI_SKY, SMEI_CAL and SMEI_ORB to pnt header
MAR-2008, Paul Hick (UCSD/CASS), V5.13
Fixed problem with two DATE keywords in header of output
Fits file.
MAR-2008, Paul Hick (UCSD/CASS), V5.2
Bug fix in edge-clean procedure. The bug may have been
introduced with V5.01 (JUL-2007) with the inclusion of the
'flat' star-subtracted maps.
APR-2008, Paul Hick (UCSD/CASS), V5.3
Both sidereal background and zodiacal dust brightness
are now subtracted prior to fitting stars.
The weighting in smei_star_lsqfit was changed to
from 1/b to 1/(50+b), where b is the residual brightness
(after background and zodiac subtraction).
Added keyword removezld.
Added header keywords ZLD, ZLDVER to output files.
Renamed header keyword gain from BKGAIN to SKYGAIN
APR-2008, Paul Hick (UCSD/CASS), V5.31
Replaced sidereal background map with new version.
JUN-2008, Paul Hick (UCSD/CASS)
Added PSF angle to output Fits file.
JUL-2008, Paul Hick (UCSD/CASS), V5.32
Changed gain decrease for camera 1 from 1%/yr to 0.5%/yr
(in smei_camera_gain)
OCT-2008, Paul Hick (UCSD/CASS), V5.33
Fixed bug in calculation of observation time (used stime as
time origin instead of extracted the origin from the header
for the time map (keyword TORIGIN).
DEC-2008, Paul Hick (UCSD/CASS), V6.00
New sidereal background map (version 3)
New zodiacal dust cloud model (model 4.01)
Gain change for camera 1 set back to -1% per year.
AUG-2009, Paul Hick (UCSD/CASS)
Added keyword use_bkgnd_version to be able to change the
selected sidereal background map.
SEP-2009, Paul Hick (UCSD/CASS)
Added keyword use_zld_version to be able to change the
selected zld model.
OCT-2009, John Clover (UCSD/CASS; jclover@ucsd.edu), V6.01
Changed the default behavior of star fitting, the sidereal
background is no longer removed prior to the star fit
if background is removed, it is done so after star fit.
Also changed default background to version 4.
DEC-2009, Paul Hick (UCSD/CASS), V6.02
The star_sky array returned from smei_star_fit is now
contains "flat" stars, i.e. the fitted stars with the
fitted background model subtracted
MAY-2010, John Clover (UCSD/CASS), V7.01
Updated to include ZLD removed FTS headers.
1, 2, 3 contain star removed "flat" maps (eq, np, sp)
with ZLD removed
4, 5, 6 contain star removed "flat" maps (eq, np, sp)
with ZLD not removed (unchanged from previous version)
Removed keyword removezld (zld now always removed)
Added keyword fit_with_nobkgnd (default off)
JUN-2010, Paul Hick (UCSD/CASS), V7.02
After bugfix in construction of flat_sky in smei_star_fit
JUL-2010, John Clover (UCSD/CASS)
Incrimented use_bkgnd_version to 5, new background maps
have been from engineering mode maps with the bugfix
applied
AUG-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu), V7.03
Added two columns (for ccd_mode and area of (exteneded)
PSF. Changed format of column Istd. Allowed value 2
in last column to indicate stars not fitted because there
are not enough good bins.
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NAME:
smei_star_show
PURPOSE:
Plot star time series
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_show, star_name, pnt_, $
source = source , $
xname = xname , $
xtype = xtype , $
yname = yname , $
ytype = ytype , $
ttrange = ttrange , $
cvrange = cvrange , $
fixgain = fixgain , $
magnitude=magnitude , $
pnt = pnt , $
camera = camera , $
track = track , $
yaxis = yaxis , $
newyaxis= newyaxis , $
dtsmooth= dtsmooth , $
tsmooth = tsmooth , $
xysize = xysize , $
zbuffer = zbuffer , $
imgfile = imgfile , $
logo = logo , $
silent = silent , $
_extra = _extra
INPUTS:
star_name scalar; type: string; default: Polaris
name of star
used only if 2nd argument (pnt_) is not specified
star_name is run through smei_star_alias
and smei_star_info to translate the specified
name to a star_name on one of the SMEI star catalogues
(set keyword cat='*' to scan all available catalogues).
If no match is found then 'star_name' is used (after
replacing spaces with underscores) to locate a time
series file <star_name>.txt or <star_name>.txt.gz.
If a match is found than the standard naming convention
for naming pnt files is followed to locate a pnt file
(see smei_star_filename).
pnt_ array; type: structure
time series info read from pnt file.
If this argument is specified (obtained from a previous
call to smei_star_show) then 'star_name' is ignored
and this argument is used instead of reading the
time series from file.
OPTIONAL INPUT PARAMETERS:
source=source scalar; type: string; default: $SMEISKY0/star
name of directory where pnt file for 'star_name'
timeseries is located
Any of the quantities in the time series ('pnt') file can be plotted.
These are selected by specifying field names in the xname and yname
keywords. Valid entries are:
NAME
RADEC 2-element vector
MAPTYPE
CAMERA
TIME
PSFANGLE
FOVANGLE 2-element vector
PSFSTRETCH 2-element vector
GAIN
NAME_CLOSE
TOTAL_ADUS
BRIGHT_RAW
BRIGHT_MDL
BRIGHT
BACK_CONST
BACK_SLOPE 2-element vector
N_BKGND
N_FITPSF
STDEV_BKGND
STDEV_PSF
CVFIT
DRADEC 2-element vector
DPSFANGLE
DPSFSTRETCH 2-element vector
PSFWIDTH 2-element vector
REMOVE
DONE
xname=xname scalar; type: string; default: 'TIME'
selects the quantity on the horizontal axis
yname=yname scalar or array; type: string; default: 'BRIGHT'
selects one or more quantities for the vertical axis
Note: if more than one quantity for the y-axis is
specified then probably keywords newyaxis and yaxis
will be needed to get a decent plot
(see PlotCurve).
xtype=xtype scaler; type: integer; default: 0
ytype=ytype scalar; type: integer; default: replicate(0,n_elements(yname)
either 0 or 1; selects the vector component if one of the
vector fields is used for xname and/or yname
Special cases:
- If one of the vector fields is used for xname, then the second vector
component is used for the y-axis, e.g.
xname='RADEC' is the same as xname='RADEC, xtype=0, yname='RADEC', ytype=1
camera=camera scalar or array; type: integer; default: none
list of cameras (value 1,2 or 3). If present, only
data points for the indicated cameras are plotted.
ttrange=ttrange array[2]; type: string or time structure; default: none
limits time series to specied time range
If only one time is specified than the time series
from that time to the end of the time series is plotted.
cvrange=cvrange scalar or array[2]; type: numeric; default: none
only plots data points for which the correlation of the
PSF fits was in the specified range.
If a scalar is specified then [cvrange,1.0] is assumed,
i.e. all points with fits better than the indicated
threshold are used.
/magnitude converts the brightness to a SMEI magnitude scale
(Note: this is a very coarse conversion)
/fixgain if set, then the gain information in the pnt file is used
to correct the timeseries for camera gain.
/track calls smei_sky_track instead of plotting time series info
(Does this work? What does it do anyways?)
_extra=_extra extra keywords passed to smei_star_info, smei_sky_track,
PlotCurve and xyouts
OUTPUTS:
pnt_ array; type structure
the content read from the pnt file. This can be used
in subsequent calls to bypass reading the file
again. In this case the 'star_name' argument is ignored.
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, InitVar, IsTime, IsType, PlotCurve, TimeGet, TimeLimits, TimeSet, TimeUnit
destroyvar, get_page, set_page, smei_i2m, smei_orbit_get, smei_sky_track
smei_star_alias, smei_star_filename, smei_star_info, smei_star_readpnt
smei_star_showsmooth, smei_star_title, where_common
PROCEDURE:
MODIFICATION HISTORY:
JAN-2008, Paul Hick (UCSD/CASS)
FEB-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_showsmooth
PURPOSE:
Internal use only (by smei_star_show)
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_showsmooth, time, fnc, $
dtsmooth = dtsmooth , $
tsmooth = tsmooth , $
sigma = sigma
INPUTS:
time
fnc
OPTIONAL INPUT PARAMETERS:
dtsmooth=dtsmooth
OUTPUTS:
Result
OPTIONAL OUTPUT PARAMETERS:
sigma=sigma
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, IsTime, IsType, MEAN, STDDEV, TimeGet, TimeOp, TimeSet, TimeUnit
CALLED BY:
smei_star_show
PROCEDURE:
MODIFICATION HISTORY:
OCT-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_split
PURPOSE:
Processes all individual star files (as created by Python
script smei_star_split.py) and sorts their content into
chronological order.
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_split, wildcard, $
source = source , $
remove = remove , $
silent = silent , $
force = force
INPUTS:
wildcard scalar; type: string; default: '*'
OPTIONAL INPUTS:
source scalar; type: string; default: '.'
source directory of files for individual stars
OUTPUTS:
Rewrites all the files for individual stars
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FindAllFiles, GetFileSpec, InitVar, SMEI_STAR_TESTPNT, TimeOp, TimeSet, TimeUnit
do_file, hide_env, smei_star_readpnt, smei_star_writepnt
PROCEDURE:
For each star a separate file is created in $SMEISKY0/star
containing all the records for that star found in the
pnt files stored in $SMEISKY0/pnt.
MODIFICATION HISTORY:
JAN-2007, Paul Hick (UCSD/CASS)
JUL-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Removed the part that creates the individual star files.
This is now done with Python script smei_star_split.py
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NAME:
smei_star_standard
PURPOSE:
Read in the standard star map
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_standard, camera , $
bkgnd_origin = bkgnd_origin , $
bkgnd_radius = bkgnd_radius , $
wing_origin = wing_origin , $
wing_radius = wing_radius , $
wing_delta = wing_delta , $
min_wing_radius = min_wing_radius , $
psfstretch = psfstretch , $
degrees = degrees , $
get_origin = get_origin , $
get_ndim = get_ndim , $
get_fov = get_fov , $
get_scale = get_scale , $
get_nomansland_id = get_nomansland_id , $
get_background_id = get_background_id , $
get_wayoutside_id = get_wayoutside_id , $
use_filled_psf = use_filled_psf , $
in_psf = in_psf , $
show = show , $
scale = scale , $
origin = origin , $
extend_corepsf = extend_corepsf , $
silent = silent
INPUTS:
camera scalar; type: integer; default: 2
camera number (1,2,3)
OPTIONAL INPUT PARAMETERS:
!!! DO NOT MIX the bkgnd_* and wing_* keywords: results will be unpredictable.
/degrees all angles are in degrees (default is radians)
This includes bkgnd_radius, wing_radius, psfstretch
bkgnd_origin, wing_origin, wing_delta and min_wing_radius
bkgnd_origin=bkgnd_origin
array[2]; type: float; default: [0,0]
only used if bkgnd_radius is set.
Shifts the origin of the ellipsoidal background area
The units are the same as bkgnd_radius (i.e. radians or
degrees, depending on setting of /degrees).
bkgnd_radius=bkgnd_radius
scalar or array[2]; type: float; default: none
Radius of circular or ellipsoidal area around centroid
of standard star used to define the background area around the PSF
If two radii are specified than the ring in between
the two circles/ellipses is used to define the background area.
(an ellipse results from the use of 'psfstretch' see below.)
wing_origin=wing_origin
array[2]; type: float; default: [0,0]
only used if wing_radius is set.
Shifts the origin of the ellipsoidal wing area
The units are the same as wing_radius (i.e. radians or
degrees, depending on setting of /degrees).
wing_radius=wing_radius
scalar or array[2]; type: float; default: none
Axes of ellipse defining a wing area around the PSF
If scalar then the ellipse becomes a circle.
Inside this area the PSF is extended using an
exponential dropoff in directions along and
perpendicular to the PSF symmetry axis.
wing_delta=wing_delta
scalar or array[2]; type: float; default: none
correction to wing_radius
min_wing_radius=min_wing_radius
scalar; type: float; default: 0.5 degrees
sets a lower value on the effective wing radius
(wing_radius+wing_delta) to avoid using too low
values (wing_delta is used to scale the effective
wing radius with magnitude; this could lead to
small, or even negative values for very faint stars).
psfstretch=psfstretch
array[2]; type: float: default: [0.0,0.0]
Only used if bkgnd_radius or wing_radius is set
to non-zero value
Setting psfstretch to a value other than one will turn the
background (if bkgnd_* keywords are uses) or wing (if wing_*
keywords are used) area into an ellipse with a semi-major
axis of bkgnd_radius/psfstretch, i.e. larger values of
psfstretch shrink the axes.
(usually psfstretch=cos(fovangle) where fovangle is the
direction cosine angle in the long fov dimension)
/get_origin if set return origin (array indices for RA=0, dec=0) of
standard star map
/get_ndim if set return dimensions of standard star map
/get_fov if set return width of standard map in angular units
This is the product of the return values for the /get_ndim
and /get_scale keywords.
/get_scale if set return scale (angular units per bin) of standard
star map
/show if set display standard star map
/use_filled_psf if set, use the alternative PSF map
OUTPUTS:
See /get_origin, /get_scale, /get_ndim
for return value if one of these keywords is set. If no keyword is set:
std_map array[n,n]; type: float
2D standard star map of 200x200 bins
map > 0 inside PSF (brightness of standard star)
map = -1 inside inner radius, but outside PSF
(not present if bkgnd_radius is a scalar (outer radius only),
or if wing_radius is used)
map = -2 inside outer radius, but outside PSF and outside
inner radius (if specified);
or inside wing_radius but outside PSF.
map = -3 outside outer radius, and outside PSF
in_psf array[n,n]; type: byte
1 inside the non-zero area of the PSF; 0 outside
This is the effective non-zero area of the PSF, or 'core PSF'
!!! If keyword wing_radius is set this EXCLUDES the circular
!!! area out to radius 'wing_radius', but only covers the part
!!! that is non-zero in the standard_star file.
origin=origin array[2]; float
array indices for RA=0,dec=0) of the standard star map
scale=scale scalar; type: float
scale (angular units per bin) of standard star map
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
smei_star_cleanup, smei_star_fit, smei_star_stdmaps, smei_star_writepnt
COMMON BLOCKS:
common smei_star_standard_save, $
std_psf , $
std_wing , $
std_cam , $
std_origin , $
std_scale , $
std_adus , $
std_map , $
std_in_psf
CALLS: ***
FILEPATH, FXPAR, InitVar, IsType, READFITS, ToDegrees, destroyvar, gridgen, view, who_am_i
PROCEDURE:
The standard star is stored in the Fits file standard_star.fts.gz
in the same directory as this procedure.
The standard map is a 200x200 array covering a 5x5 deg area
(0.025 deg/bin). for each camera. It contains positive-definite
values defining the PSF and is zero everywhere else.
The center of the map (at array indices [99.5,99.5] is the
centroid of the PSF. The standard star represents the shape of a star
with its centroid located at RA=0, dec=0 (i.e. on the equator).
Either the bkgnd_* or the wing_* are used to fill the return
array:
Only outer radius specified in bkgnd_radius:
The input values bkgnd_radius, bkgnd_origin and psfstretch are
used to define an ellipsoidal area around the center of the map.
Bins outside the ellipse are set to -3.
Bins inside the ellipse (but not in the PSF) are set to -2.
The output map contains -3, -2, and positive-definite values.
Both inner and outer radius specified in bkgnd_radius:
The input values bkgnd_radius, bkgnd_origin and psfstretch are
used to define an ellipsoidal ring around the center of the map.
Bins outside the outer ellipse are set to -3.
Bins inside the ring between inner and outer ellipse
(but not in the PSF) are set to -2.
Bins inside the inner ellipse (but not in the PSF) are set to -1
The output map contains -3, -2, -1, and positive-definite values
Single radius or semi-major axes specified in wing_radius:
The input values wing_radius (and wing_delta), wing_origin, and
psfstretch are used to define an ellipsoidal ring around the
center of the map.
Bins outside the ellipse (but not in the PSF) are set to -3.
The output map contains -3, and positive-definite values
The bins with value -2 in the output map can be used to define
a background area around the PSF.
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
AUG-2006, Paul Hick (UCSD/CASS)
Added /use_filled_psf keyword to work with alternative PSF map
MAR-2007, Paul Hick (UCSD/CASS)
Change bkgnd_radius and fovxangle from argument to keyword.
Added keywords wing_radius and wing_origin
MAY-2007, Paul Hick (UCSD/CASS)
Changed scalar fovxangle keyword to 2-element array psfstretch
Changed keyword /get_adus to /get_psfadus.
Added keyword /get_psfarea
JUL-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword in_psf
Removed keywords get_psfarea and get_psfadus.
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NAME:
smei_star_stdmaps
PURPOSE:
Get brightness in standard star at indicated locations
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_stdmaps, camera, $
maptype , $
rr , $
origin , $
scale , $
radec , $
psfangle , $
psfstretch , $
degrees = degrees , $
bkgnd_origin = bkgnd_origin , $
bkgnd_radius = bkgnd_radius , $
wing_origin = wing_origin , $
wing_radius = wing_radius , $
wing_delta = wing_delta , $
in_fullpsf = in_fullpsf , $
in_fitpsf = in_fitpsf , $
in_corepsf = in_corepsf , $
in_bkgnd = in_bkgnd , $
std_rr = std_rr , $
use_filled_psf=use_filled_psf,$
stars_mask = stars_mask , $
corepsf_mask = corepsf_mask , $
stdarea = stdarea , $
stdadus = stdadus
INPUTS:
camera scalar; type: integer
camera id (1,2,3)
maptype scalar; type: integer
-1: map of south pole
0: equatorial map
+1: map of north pole
rr array[2,n]; type: integer
position vectors for all bins in the box around
the star as column and row indices into the original skymap
for all bins in box around star
origin array[2]; type: float
array indices of RA=0, dec=0 (equatorial map),
position of north pole, dec=90 (north polar map) or
position of south pole, dec=-90 (south polar map)
scale scalar; type: float
map resolution (radians/degrees per bin)
radec array[2,m]; type: float
RA and dec of the star centroids for m stars
psfangle array[m]; type: float
orientations of PSF relative to equatorial north
for m stars
psfstretch array[2,m]; type: float
'stretch' factors along long and narrow dimension of the
SMEI field of view for m stars. Larger stretch factors
will shrink the PSF size (similar to the geometric effect
of the shrinking aperture size when viewed from a direction
away from the optical axis (the fov direction cosine angle)).
OPTIONAL INPUTS:
/degrees if set, all angles are in degrees (default: radians)
stars_mask=stars_mask
array[n]; type: float
box around star with results for previously-
subtracted stars.
This is a box extracted from the "stars_sky"
array in smei_star_fit: it is zero in skybins
where nothing has been subtracted yet, and
positive-definite when subtraction has taken
place (the content is the intensity that was
subtracted from the original skymap).
If present this affects 'in_fit_psf' and 'in_bkgnd':
in_bkgnd: skybins that are part of an already-subtracted
star are excluded.
in_fitpsf: skybins that that are part of an already-subtracted
star and are in the core PSF of one of the m stars
are excluded.
corepsf_mask=corepsf_mask
array[n]; type: byte
0 where bins are inside the core PSF of bright stars.
This mask affects 'in_fit_psf':
skybins inside the core PSF of bright stars, but outside
the core PSF of the m stars are excluded
Passed to smei_star_standard:
bkgnd_origin=bkgnd_origin
array[2]; type: float
bkgnd_radius=bkgnd_radius
scalar or array[2]; type: float
wing_origin=wing_origin
array[2]; type: float
wing_radius=wing_radius
scalar or array[2]; type: float
wing_delta=wing_delta
scalar or array[2]; type float
/use_filled_psf if set, use the alternative PSF map
OUTPUTS:
Result array[n,m]; type: float
'standard star' brightnesses at the locations rr for m stars.
The 'standard star' gives the brightness of a star located
at RA=0, dec=0 with PSF angle of zero.
The sky locations rr are transformed to locations in the
'standard star' reference frame; 'standard star' brightnesses
are obtained by interpolation.
in_fullpsf=in_fullpsf
array[n]; type: byte
1B identifies locations inside combined PSF of
m stars (i.e. the union of the non-zero location
for the individual stars).
This includes locations inside the "core" PSF, and
(if wing_radius is used) additional locations where
the core PSF is extended out to the specified
wing_radius.
in_fitpsf=in_fitpsf
array[n]; type: byte
subset of in_fullpsf
excludes bins set to 1B in in_fullpsf based
on info provided in keyword stars_mask
and corepsf_mask
in_corepsf=in_corepsf[n,m]
array[n]; type: byte
1B identifies locations inside the "core" PSF
(stored in the standard star map) for each of the
m fitted stars individually.
If wing_radius is set this is NOT the same as in_fitpsf
(in_corepsf is a subset of in_fitpsf, identifying the
PSF before it was extended out to wing_radius)
in_bkgnd=in_bkgnd
array[n]; type: byte
1B identifies locations in background area
Is affected by stars_mask, if specified
std_rr=std_rr array[2,n,m]; type: float
equivalent RA,dec in the 'standard star' reference frame
(centered on RA=0, dec=0) with abs(RA) < 180 degrees
stdarea=stdarea array[m]; type: float
total angular size of the PSF for all m stars.
Calculated in the 'standard star' reference frame, and
includes all bins with non-zero brightness (i.e. if
wing_radius is used this includes the bins outside the
core PSF filled with an exponential dropoff out to
wing_radius. (!!! Not sure this is the right way to
do it: maybe should use core PSF only)
stdadus=stdadus array[m]; type: float
Total adus in the 'standard star' in the same set of
bins used to calculate 'stdarea'.
The sum is defined as the sum of the ADUs in the
standard star skybins, times the binarea (0.025^2 deg).
(this makes totaladus independent of bin size, making
it easier to compare with the same quantity calculated
in the fullsky maps (with 0.1 deg resolution).
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, BILINEAR, EulerRotate, IsType, ToDegrees, ToRadians, smei_star_standard
CALLED BY:
smei_star_corepsf, smei_star_fit
PROCEDURE:
See Section 6 in http://supercat.ucsd.edu/reports/smei.pdf
MODIFICATION HISTORY:
JUN-2006, Paul Hick (UCSD/CASS)
JUL-2006, Jordan Vaughan (jtvaugha@ucsd.edu)
Added costhetax argument
JUL-2006, Paul Hick (UCSD/CASS)
Modified the linear interpolation on the standard map.
The 'missing data' value now is -1.0 instead of 0.0.
The value 0.0 is now used to indicate bins used to sample
the background.
JUL-2006, Paul Hick (UCSD/CASS)
Added /use_filled_psf keyword
FEB-2007, Jordan Vaughan, Paul Hick (UCSD/CASS)
Added stars_mask keyword to be able to exclude skybins
in already-subtracted stars from the background.
JUL-2007, Paul Hick (UCSD/CASS)
Added keyword in_corepsf
NOV-2011, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added more documentation.
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NAME:
smei_star_test
PURPOSE:
Test integrity of star time series files
Works for pnt files, and for files made for
individual stars (if /nohdr) is set.
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
FUNCTION smei_star_testpnt, files, $
nohdr = nohdr , $
silent = silent
INPUTS:
files scalar or array; type: none
OPTIONAL INPUTS:
/nohdr
OUTPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
SMEI_STAR_TESTPNT, TimeOp, TimeSet, TimeUnit, UNIQ, hide_env, jpl_body, smei_star_info
smei_star_list, smei_star_readpnt, sphere_distance, usno_body, where_common
PROCEDURE:
Checks for duplicate times
Checks for times before start of mission (this catches
data points without a valid time for which the time
is set to 2000/01/01
Checks for timea after end of mission (should never happen)
MODIFICATION HISTORY:
JUL-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_title
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
FUNCTION smei_star_title, xtag, itag
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS:
CALLED BY:
smei_star_show
PROCEDURE:
MODIFICATION HISTORY:
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_update
PURPOSE:
Update star subtractions in SMEI data base
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_update, camera=camera, mode=mode
INPUTS:
(none)
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, FindAllFiles, InitVar, IsType, smei_star_remove
PROCEDURE:
MODIFICATION HISTORY:
NOV-2006, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smei_star_writepnt
PURPOSE:
Write fit informations for bright star to file
CATEGORY:
camera/idl/star
CALLING SEQUENCE:
PRO smei_star_writepnt, filename, star_fit , $
dec_cutoff = dec_cutoff, $
camera = camera , $
append = append , $
star_info = star_info , $
degrees = degrees , $
single_star = single_star
INPUTS:
filename scalar; type: string
Fully-qualified filename
star_fit array; type: structure
Structure with information from fits of bright star
(from output keyword star_fit in smei_star_fit.
If star_fit is NOT defined and /append is NOT set then
just the header is written.
OPTIONAL INPUT PARAMETERS:
append=append if set, the append to existing file
if NOT set, a new file is created. The file
starts with a header.
camera=camera scalar; type: integer; default: none
camera ID (1,2 or 3)
If present, a line is added to the header with the
mean intensity (in adus) in the standard star
dec_cutoff scalar; type: float; default: none
If present, stars are written to file only if:
abs(dec(star) LE dec_cutoff in equatorial map
dec_star GT dec_cutoff in north polar map
dec_star LT -dec_cutoff in south polar maps
If NOT present, all stars are written to file
Note that the units of dec_cutoff (degrees or radians)
must be consistent with the units for RA,dec stored
in the 'star_fit' structure.
star_info=star_info array; type: string
string array containg fit parameters used by smei_star_fit.
This is added to the header (if /append NOT set).
OUTPUTS:
(to ASCII file)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
GetFileSpec, InitVar, IsType, TimeGet, TimeSystem, boost, flt_format, hide_env
smei_star_filename, smei_star_formatpnt, smei_star_standard
CALLED BY:
smei_findpnt, smei_star_fitone, smei_star_remove, smei_star_split
PROCEDURE:
MODIFICATION HISTORY:
AUG-2006, Paul Hick (UCSD/CASS)
SEP-2006, Paul Hick (UCSD/CASS)
Added /use_filled_psf keyword
JUL-2007, Paul Hick (UCSD/CASS)
Removed wing_radius and use_filled_psf keywords
DEC-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Changed keyword CREATED to DATE (consistent with IDL)
Removed version keyword (version is now added to header in smei_star_remove)
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NAME:
smei_theta2radial
PURPOSE:
Converts from angle thetay in the sky to radial offset
Rccd-R0 on the CCD
CATEGORY:
camera
CALLING SEQUENCE:
R = smei_theta2radial(thetay [, thetax])
INPUTS:
thetay array[*]; type: any
thetay argument for Eq. 3
OPTIONAL INPUT PARAMETERS:
thetax array[*] or array[2,*]; type: same as thetay
if thetax is absent then Equation 2 from the memo is
used (= Eq. 3 with thetax=0)
CASE 1: array[*]: if thetax is an array with the same structure
as thetay then the radial offset from Eq. 3 is returned
CASE 2: array[2,*]: this is used by smei_radial2theta to determine the
zero for Eq 3 for given thetax and radial offset.
thetax[0,*]: stores the thetax values
thetax[1,*]: stores the radial offset values
OUTPUTS:
R array[*]; type: same type as thetax
CASE 1: radial offset from Eq 3 in pixels
CASE 2: radial offset from Eq 3, minus radial offset specified in
thetax[1,*] (the value of thetay that makes this difference zero is
the value that smei_radial2theta is after).
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL BY:
smei_radial2theta
CALLS: ***
IsType, SubArray
CALLED BY:
cvsmei, smei_sky2ccd
PROCEDURE:
See Andy's memo "Defining the field of view for the SMEI cameras" (11-July-2001)
This function implements Equation 3. All angles are in degrees.
MODIFICATION HISTORY:
FEB-2003, Paul Hick (UCSD/CASS)
JAN-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Modification to intercept large thetay values
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NAME:
smei_www_skymaps
PURPOSE:
Creates the html tables showing available skymaps
on SMEI website.
CALLING SEQUENCE:
PRO smei_www_skymaps, mode, $
supercat = supercat , $
update = update , $
lastmonths = lastmonths, $
remote = remote , $
silent = silent
OPTIONAL INPUTS:
mode array or scaler; type: integer; default: 'sky'
modes to be processed
INCLUDE:
@compile_opt.pro
CALLS: ***
CheckDir, FILEPATH, FindAllFiles, GetFileSpec, InitVar, IsType, SetFileSpec, TimeGet
TimeMonth, TimeSet, TimeSystem, TimeUnit, boost, destroyvar, hide_env, smei_coriolis
txt_read
CALLED BY:
smei_mksky
PROCEDURE:
MODIFICATION HISTORY:
OCT-2006, Paul Hick (UCSD/CASS)
JAN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Bug fix in construction of index.html with /update set when
crossing from one year to the next.
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NAME:
smei_zld_dumbbell
PURPOSE:
Calculates analytic dumbbell-shaped correction to the zodiacal light
distribution seen by SMEI
CATEGORY:
ucsd/camera/idl/zld
CALLING SEQUENCE:
FUNCTION smei_zld_dumbbell, r, $
degrees = degrees , $
silent = silent , $
zld_component = zld_component
INPUTS:
r array[2] or array[2,n]; type: double
Sun-centered ecliptic coordinates (longitude and
latitude for points where correction is needed).
OPTIONAL INPUT PARAMETERS:
/degrees if set, all angles are in degrees (default: radians)
zld_component = zld_component
array; type: integer; default: none
By default, both components (analytic and residue
map) are returned.
The values ZLD_MDL__FNC_DUMBBELL and ZLD_MDL__RES_DUMBBELL
can be used in zld_component to extract either one
of both components. The constants are defined in
include file smei_zld_parts.pro
OUTPUTS:
Result scalar or array[n]
brightness of zodiacal light correction in
ADUs at nominal gain.
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_zld_parts.pro
CALLS: ***
AngleRange, EulerRotate, InitVar, IsType, SyncDims, ToDegrees, ToRadians, WhatIs
CALLED BY:
smei_zld_model, test_dumbbell
PROCEDURE:
There is a discontinuity of < 0.6 ADUs on the ecliptic.
The residual map is stored in $SMEIDB/c3zldresidue.fts.gz
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS)
APR-2009, Paul Hick (UCSD/CASS)
Added /add_residue to add interpolated value from residue
zld map to analytic zld correction.
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Couple of bugfixes. Fairly substantial rewrite.
Removed /add_residue, and instead added keyword zld_component
MAR-2010, John Clover (UCSD/CASS; jclover@ucsd.edu)
Bugfix with Sun centered ecliptic domain. Coords were 0
and positive in array to rightmost column, and 0 to negative
to leftmost column, causing some issue, latitudes are
shifted to be -180 to 180 degrees.
Added exclusion zone for 0-15 degrees elongation
from Sun and added dropoff starting at 75 degrees
elongation and added exclusion outside of 90 degrees
elongation from the Sun
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NAME:
smei_zld_model
PURPOSE:
Implements the current analytic fit to the zodiacal light
distribution for the SMEI observations
CATEGORY:
camera/idl/dust
CALLING SEQUENCE:
FUNCTION smei_zld_model, tt, rr, $
ndim = ndim , $
range = range_ , $
degrees = degrees , $
ecliptic = ecliptic , $
equatorial = equatorial, $
model_1 = model_1 , $
model_2 = model_2 , $
model_3 = model_3 , $
model_4 = model_4 , $
use_zld_version=use_zld_version, $
version = version , $
get_version = get_version,$
silent = silent , $
camera = camera , $
zld_component = zld_component, $
minelo = minelo , $
noslab = noslab ; Obsolete (not used in model 4)
INPUTS:
tt array[1]; type: time structure
UT time at which zodiacal light brightness is required
rr array[2,*]; type: float or double
angles defining the lines of sight for which brightness is required
rr[0,*] is ecliptic longitude of los relative to Sun
rr[1,*] is ecliptic latitude of los
(i.e. a helioecliptic coordinate system is assumed)
if /ecliptic is SET:
rr[0,*] is ecliptic longitude of los
rr[1,*] is ecliptic latitude of los
if /equatorial is SET:
rr[0,*] is right ascension of los
rr[1,*] is declination of los
The units of the angles are set by keyword /degrees
NOTE: it is allowed to specify rr as an array[3,*] with the
3rd element in the first dimension the line of sight distance
(only the angles are used)
OPTIONAL INPUT PARAMETERS:
ndim=ndim array[2]; type: integer; default: none
if present, a full-sky map is set up in the coordinate system
implied by setting of /ecliptic and /equatorial
The lines of sight used are returned in rr
range=range array[2,2]; type: float; default: none
range of grid in longitude and latitude.
Used in conjunction with keyword 'ndim'.
range[0:1,0]; start and end longitude
range[0:1,0]; start and end latitude
These are the outer bin edges, NOT the bin centers.
/degrees if SET the angles in argument 'rr' and 'range'
are in degrees; default is radians
/equatorial if SET then 'rr' is specified in equatorial coordinates
/ecliptic if SET then 'rr' is specified in ecliptic coordinates
if neither /equatorial nor /ecliptic is set then 'rr' is
assumed to be in helioecliptic coordinates
/get_version makes the zodial light model version number the
function return value
Each of the following keywords selects a different zld model. If none is set then
/model_4 is used (this is the default model; the other ones are pretty much obsolete).
The providence of the first three models is hazy at best.
/model_1
/model_2
/model_3
/model_4 this is the official, published model
use_zld_version=use_zld_version
scalar; type: integer (1,2,3,4)
alternative to setting one of the /model_* keywords
Overrides /model_* keywords only if one of the valid
integer values is passed
The following four keywords are only applied for the default model (model_4)
zld_component=zld_component
array; type: integer; default: none
For the time being the default for model 4 only includes
the first three components.
By default, all zld components are included. Individual
components can be controlled by adding them to the zld_component,
an array of integers (defined in include file smei_zld_parts.pro)
indicating which components of the zld model will be included:
ZLD_MDL__BACKGROUND main background model
ZLD_MDL__GEGENSCHEIN Gegenschein
ZLD_MDL__SLAB slab along ecliptic
ZLD_MDL__FNC_DUMBBELL analytic dumbbell-shape component
ZLD_MDL__RES_DUMBBELL static residue map
ZLD_MDL__FNC_WEEKLY analytic time-dependent component
ZLD_MDL__RES_WEEKLY weekly residue map
The last two are NEVER applied to camera 3.
OUTPUTS:
result if /get_version NOT set:
array[*]; type: double
the model brightness of the zodiacal dust cloud
if /get_version SET:
version number of the zodiacal light model
rr array[2,n,m]; type: double
(only if keyword ndim is used)
The lines of sight used to create a full-sky map
OPTIONAL OUTPUTS:
version=version scalar; type: float
returns the version number of the zodiacal light model
(as specified by the /model_* keywords)
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_zld_parts.pro
CALLS: ***
AngleRange, AngleUnits, BadValue, CvSky, InitVar, IsType, ToRadians, WhatIs, big_eph
destroyvar, gridgen, jpl_body, smei_zld_dumbbell, smei_zld_weekly
CALLED BY:
smei_sky_read, smei_star_remove, smei_zld_remove [1], smei_zld_remove [2]
smei_zldsky
EXAMPLE:
To get the zodiacal dust cloud brightness on an equatorial grid with a resolution
of one degree at the current time:
tt = TimeSystem()
rr = gridgen([360,180],/open,range=[[0,360],[-90,90]],/multid)
zz = smei_zld_model(tt,rr,/degrees,/equatorial)
returns an double precision array zz[360,180].
PROCEDURE:
Purely empirical fit
The brightness scale corresponds to camera 2 at nominal gain 1.
To subtract this model from a skymap the map needs to multiplied by the
time- and camera-dependent gain factor returned by smei_camera_gain.
MODIFICATION HISTORY:
AUG-2006, Jordan Vaughan (jtvaugha@ucsd.edu), Paul Hick (UCSD/CASS)
Based on Andys zodiac_model.for, but substantially rewritten.
DEC-2007, Paul Hick (UCSD/CASS)
Added second zodiacal light model (keyword /model_2),
based on the model first used for the comet movies.
The old model is available with keyword /model_1.
APR-2008, Paul Hick (UCSD/CASS)
Next iteration on zld model added as /model_3.
(/model_2 remains the default).
Added keyword "version"
NOV-2008, Paul Hick (UCSD/CASS)
Next iteration on zld model added as /model_4.
DEC-2008, Paul Hick (UCSD/CASS)
Model 4 is now the default model (was model 2)
Bug fix in new model (V4.01)
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu), V4.02
Added static dumbbell and time-dependent (weekly)
corrections. Added keyword zld_component to control
which components are include in the returned zld model.
Increased version number from V4.01 to V4.02 to cover
a bugfix in smei_zld_remove (lores skymaps in
ext 5 and 6 did not have NaNs replaced by BAD_DATA
value in Fits header).
MAY-2010, John Clover (UCSD/CASS), V4.03
Implements the full ZLD model with all functional
and residual adjustments.
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NAME:
smei_zld_parts
PURPOSE:
Defines IDs for various parts of the zodiacal light model
CATEGORY:
camera/idl/zld
CALLING SEQUENCE:
@smei_zld_parts.pro
PROCEDURE:
Include where needed
MODIFICATION HISTORY:
JUN-2010, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added documentation
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NAME:
smei_zld_remove
PURPOSE:
Removes zodiacal light distribution from SMEI orbital sky maps
CATEGORY:
ucsd/camera/idl/zld
CALLING SEQUENCE:
PRO smei_zld_remove, wanted_map , $
destination = destination , $
to_smeidb = to_smeidb , $
checkversion= checkversion , $
overwrite = overwrite , $
force = force , $
silent = silent , $
width = width , $
reverse_loop= reverse_loop , $
_extra = _extra , $
new_style_ecl = new_style_ecl
INPUTS:
wanted_map array[n]; type: see smei_getfile
Selects skymap files to be processed
in combination with other keywords passed
using _extra.
OPTIONAL INPUT PARAMETERS:
/to_smeidb if set, write to directory structure as used
for SMEI data base (separate subdirs for mode
and camera) with 'destination' as the base dir.
destination=destination
scalar; type: string
destination directory for skymaps
if /to_smeidb NOT set then maps are written
directly to 'destination'.
The default in this case is $TUB
if /to_smeidb SET then files are written to
a directory structure as used for the
SMEI data base with 'destination' as the
base directory.
The default in this case is 'SMEIDB?' (the
SMEI database).
If destination starts with a "user@host:" identifier then
the output is first created locally in $TUB
and is then transferred to the remote host using scp;
the local files will be deleted after the transfer;
note that this will only work if the remote host has
been configured for ssh using private/public keys
allowing login without passwords.
/silent if set, suppresses informational messages
/checkversion overwrite existing skymaps only if the version
number has increased.
/overwrite overwrite existing skymaps
/new_style_ecl forces creation of new-style ecl files (see PROCEDURE)
When ready for the change to the new-style maps this
keyword should be changed to /old_style_ecl to switch
default operation to the new-style. At some point
the /old_style_ecl probably should be removed altogether.
_extra=_extra keywords passed to smei_getfile
OUTPUTS:
Files in destination directory
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
ArrayLocation, BadValue, CheckDir, CvSky, FILEPATH, FXADDPAR, FXPAR, GetFileSpec
HEADFITS, InitVar, IsType, MKHDR, READFITS, TimeGet, TimeOp, TimeSet, TimeSystem, TimeUnit
WRITEFITS, big_eph, cvsmei, cvsmei_init, do_file, gridgen, gzip_file, hide_env, jpl_body
smei_camera_gain, smei_filename, smei_filepath, smei_getfile, smei_sky
smei_zld_model
PROCEDURE:
All maps in the ecl files are low-res maps (720 x 360, i.e. 0.5 degree resolution)
Extension 0, 1, 5 and 6 are different in old-style and new-style maps
Old-style ecl file:
Extension 0, Helioecliptic map HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map based on star-subtracted "bumpy" maps with zld removed
Extension 1, Helioecliptic map HLNG=[-180,180],HLAT=[-90,+90] (flat)
Helio-ecliptic map based on star-subtracted "flat" maps with zld removed
Extension 2, Time (fraction of orbit) HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of time in orbit as fraction of orbit
Extension 3, Time (sec since TORIGIN) HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of time in orbit as seconds since TORIGIN
Extension 4, Contributing pixel count HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of contributing pixel count
Extension 5, Equatorial map RA=[0,360],DEC=[-90,+90]
Equatorial map based on star-subtracted "bumpy" maps with zld removed
Extension 6, Equatorial map RA=[0,360],DEC=[-90,+90] (flat)
Equatorial map based on star-subtracted "flat" maps with zld removed
Extension 7, Time (fraction of orbit) RA=[0,360],DEC=[-90,+90]
Equatorial map of time in orbit as fraction of orbit
Extension 8, Time (sec since TORIGIN) RA=[0,360],DEC=[-90,+90]
Equatorial map of time in orbit as seconds since TORIGIN
Extension 9, Contributing pixel count RA=[0,360],DEC=[-90,+90]
Equatorial map of contributing pixel count
New-style ecl file:
Extension 0, Helioecliptic map HLNG=[-180,180],HLAT=[-90,+90] (no zld)
Helio-ecliptic map based on star-subtracted "flat" maps with zld removed
(this is extension 1 from the old-style ecl file)
Extension 1, Helioecliptic map HLNG=[-180,180],HLAT=[-90,+90] (with zld)
Helio-ecliptic map based on star-subtracted "flat" maps with zld NOT removed
Extension 2, Time (fraction of orbit) HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of time in orbit as fraction of orbit
Extension 3, Time (sec since TORIGIN) HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of time in orbit as seconds since TORIGIN
Extension 4, Contributing pixel count HLNG=[-180,180],HLAT=[-90,+90]
Helio-ecliptic map of contributing pixel count
Extension 5, Equatorial map RA=[0,360],DEC=[-90,+90] (no zld)
Equatorial map based on star-subtracted "flat" maps with zld removed
(this is extension 6 from the old-style ecl file)
Extension 6, Equatorial map RA=[0,360],DEC=[-90,+90] (with zld)
Equatorial map based on star-subtracted "flat" maps with zld NOT removed
Extension 7, Time (fraction of orbit) RA=[0,360],DEC=[-90,+90]
Equatorial map of time in orbit as fraction of orbit
Extension 8, Time (sec since TORIGIN) RA=[0,360],DEC=[-90,+90]
Equatorial map of time in orbit as seconds since TORIGIN
Extension 9, Contributing pixel count RA=[0,360],DEC=[-90,+90]
MODIFICATION HISTORY:
SEP-2005, Paul Hick (UCSD/CASS), V1.0
Started, but never finished
DEC-2007, Paul Hick (UCSD/CASS), v2.0
First working version. Now uses /model_2 in smei_zld_model
FEB-2008, Paul Hick (UCSD/CASS)
Location of files now done using smei_getfile.
APR-2008, Paul Hick (UCSD/CASS)
Rewrite. Not using smoothsphere to reduce resolution
(too slow). Instead the raw maps (equatorial, polar)
are now smoothed using the IDL smooth function. Then
The sun-centered ecliptic map is obtained using
bi-linear interpolation on the smoothed raw maps.
Version number will be increased once the next
(final?) zld model becomes available.
SEP-2008, Paul Hick (UCDS/CASS)
Added code to check star subtraction version and
sidereal background version when /checkversion is
set.
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added code to prepare for switch to new-style ecl file (see
PROCEDURE). For now the procedure works as before (producing
old-style ecl files) if the input equ file was made with
star-subtraction version < 7.0, unless the keyword /new_style_ecl
is set. For star subtraction version >= 7.0 only new-style
ecl files can be made.
Bug fix. For the equatorial skymaps (extensions 5 and 6) NaN values
were not replaced by the BAD_DATA value in the header.
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NAME:
smei_zld_remove
PURPOSE:
Removes zodiacal light distribution from SMEI orbital sky maps
CATEGORY:
ucsd/camera/idl/zld
CALLING SEQUENCE:
PRO smei_zld_remove, wanted_map , $
destination = destination , $
to_smeidb = to_smeidb , $
checkversion= checkversion , $
overwrite = overwrite , $
force = force , $
silent = silent , $
width = width , $
reverse_loop= reverse_loop , $
_extra = _extra , $
keep_gegenschein = keep_gegenschein
INPUTS:
wanted_map array[n]; type: see smei_getfile
Selects skymap files to be processed
in combination with other keywords passed
using _extra.
OPTIONAL INPUT PARAMETERS:
/to_smeidb if set, write to directory structure as used
for SMEI data base (separate subdirs for mode
and camera) with 'destination' as the base dir.
destination=destination
scalar; type: string
destination directory for skymaps
if /to_smeidb NOT set then maps are written
directly to 'destination'.
The default in this case is $TUB
if /to_smeidb SET then files are written to
a directory structure as used for the
SMEI data base with 'destination' as the
base directory.
The default in this case is 'SMEIDB?' (the
SMEI database).
If destination starts with a "user@host:" identifier then
the output is first created locally in $TUB
and is then transferred to the remote host using scp;
the local files will be deleted after the transfer;
note that this will only work if the remote host has
been configured for ssh using private/public keys
allowing login without passwords.
/silent if set, suppresses informational messages
/checkversion overwrite existing skymaps only if the version
number has increased.
/overwrite overwrite existing skymaps
_extra=_extra keywords passed to smei_getfile
OUTPUTS:
Files in destination directory
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS:
ArrayLocation, BadValue, CheckDir, CvSky, GetFileSpec, InitVar, IsType, TimeGet, TimeOp
TimeSet, TimeSystem, TimeUnit, big_eph, gridgen, gzip_file, hide_env, jpl_body
smei_camera_gain, smei_filename, smei_sky, smei_zld_model
PROCEDURE:
MODIFICATION HISTORY:
SEP-2005, Paul Hick (UCSD/CASS), V1.0
Started, but never finished
DEC-2007, Paul Hick (UCSD/CASS), v2.0
First working version. Now uses /model_2 in smei_zld_model
FEB-2008, Paul Hick (UCSD/CASS)
Location of files now done using smei_getfile.
APR-2008, Paul Hick (UCSD/CASS; ppick@ucsd.edu)
Rewrite. Not using smoothsphere to reduce resolution
(too slow). Instead the raw maps (equatorial, polar)
are now smoothed using the IDL smooth function. Then
The sun-centered ecliptic map is obtained using
bi-linear interpolation on the smoothed raw maps.
Version number will be increased once the next
(final?) zld model becomes available.
SEP-2008, Paul Hick (UCDS/CASS; pphick@ucsd.edu)
Added code to check star subtraction version and
sidereal background version when /checkversion is
set.
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NAME:
smei_zld_weekly
PURPOSE:
CATEGORY:
camera/idl/zld
CALLING SEQUENCE:
FUNCTION smei_zld_weekly, t, r , $
elo_angle = elo_angle , $
pa_angle = pa_angle , $
degrees = degrees , $
silent = silent , $
zld_component = zld_component
INPUTS:
t array[1]; type: time structure
r array[2,n]; type: float
Sun-centered ecliptic longitude and latitude
OPTIONAL INPUT PARAMETERS:
elo_angle=elo_angle
array[n]; type: float
solar elongation of locations r
(calculated from r if not specified)
pa_angle=pa_angle
array[n]; type: float
position angle of locations r: angle from
ecliptic north measured counter-clockwise
(calculated from r if not specified)
/degrees if set then angles are in degrees (default: radians)
zld_component = zld_component
array; type: integer; default: none
By default, both components (analytic and residue
map) are returned.
The values ZLD_MDL__FNC_WEEKLY and ZLD_MDL__RES_WEEKLY
can be used in zld_component to extract either one
of both components. The constants are defined in
include file smei_zld_parts.pro
OUTPUTS:
R array; type: double
zodiacal brightness at locations r
INCLUDE:
@compile_opt.pro ; On error, return to caller
@smei_zld_parts.pro
CALLS: ***
AngleRange, FILEPATH, InitVar, IsTime, IsType, READFITS, SyncDims, TimeGet, TimeOp
TimeSet, TimeUnit, ToDegrees, WhatIs, big_eph, cvsmei, sgp4_orbit_axis
sphere_distance
CALLED BY:
smei_zld_model
PROCEDURE:
Correction consists of an analytic part, plus
a residual map based on a sequence of 52 weekly residues.
The analytic correction consists of a strictly time-depenent
part that matches cameras 2 and 3, and corrects for discontinuities
in camera 3 introduced by different "bad-pixel" masks, and a second
part that depends on the orientation of the Coriolis orbital plane
relative to the Sun.
The residue maps are stored in $SMEIDB/c3zldresidue.fts.gz. The
residual correction is calculated by lineary interpolation between
two neigbouring weekly maps.
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS)
DEC-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Removed /add_residue, and instead added keyword zld_component.
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NAME:
smei_zldsky
PURPOSE:
Quick and dirty way for plotting the zodiacal light models
in smei_zld_model
CATEGORY:
camera/idl/zld
CALLING SEQUENCE:
PRO smei_zldsky, tt, $
nra = nra , $
ndec = ndec , $
equatorial = equatorial , $
degrees = degrees , $
zero_shift = zero_shift , $
_extra = _extra
INPUTS:
tt array[1]; type: time structure
OPTIONAL INPUT PARAMETERS:
nra=nra scalar; type: integer
nr of elements for right ascension
ndec=ndec scalar; type: integer
nr of elemens for declination
/equatorial
/degrees
zero_shift=zero_shift
_extra=_extra
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, InitVar, PlotEarthSkymap [1], PlotEarthSkymap [2]
PlotEarthSkymap [3], PlotEarthSkymap [4], TimeSystem, ToDegrees, ToRadians, WhatIs
get_page, gridgen, set_page, smei_zld_model
PROCEDURE:
MODIFICATION HISTORY:
APR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smeidb_mounted
PURPOSE:
Check whether SMEI data base is accessible
CATEGORY:
camera/idl/misc
CALLING SEQUENCE:
FUNCTION smeidb_mounted, tf, drive=drive
INPUTS:
tf scalar, or array[1]
either a time (in the form of a standard
time structure), or the name of a SMEI frame
(e.g. 'c2frm_2003_123_456789')
OPTIONAL INPUT PARAMETERS:
The SMEI frames are stored in directories of the form
$SMEIDB#/yyyy_doy/c#.
OUTPUTS:
sts scalar; type: string
directory where frame(s) for specified time are located
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
smei_orbit_stats
COMMON BLOCKS:
common smei_filepath_save, checkdrives, sdat
CALLS: ***
CheckDir, FILEPATH, InitVar, IsTime, IsType, TimeGet, TimeSet, destroyvar, flt_read
flt_string, smei_filepath, timeposn, who_am_i
PROCEDURE:
MODIFICATION HISTORY:
JUL-2004, Paul Hick (UCSD/CASS)
MAR-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Introduced timeposn call to extract time from frame
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NAME:
smeifig
CALLING SEQUENCE:
PRO smeifig, figure, xysize=xysize,_extra=_extra
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, LOADCT, arrow3d, get_page, plot3darc, plot3dline, plot3dtext, set_page, setup3d
twin, vectorproduct
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NAME:
SMEIremoteDisplay__define
PURPOSE:
Defines SMEIremoteDisplay class structure
CATEGORY:
SMEIremote
CALLING SEQUENCE:
display = obj_new('SMEIremoteDisplay')
INPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
PROCEDURE:
MODIFICATION HISTORY:
AUG-2002, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SMEIremoteFOV__define
PURPOSE:
Defines SMEIremoteFOV class structure
CATEGORY:
SMEIremote
CALLING SEQUENCE:
fov = obj_new('SMEIremoteFOV')
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS:
SEE ALSO:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
AUG-2002, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SMEIremoteMatrix__define
PURPOSE:
Defines SMEIremoteMatrix class structure
CATEGORY:
SMEIremote
CALLING SEQUENCE:
fov = obj_new('SMEIremoteMatrix')
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS:
SEE ALSO:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
AUG-2002, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SMEIremoteView__define
PURPOSE:
Defines SMEIremoteView class structure
CATEGORY:
SMEIremote
CALLING SEQUENCE:
fov = obj_new('SMEIremoteView')
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
EXTERNAL:
CALLS:
SEE ALSO:
SIDE EFFECTS:
RESTRICTIONS:
EXAMPLE:
PROCEDURE:
MODIFICATION HISTORY:
AUG-2002, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
smooc
PURPOSE:
This function smooths an image file within the boundaries of the
windowed area so that point glitches, cosmic rays, especially
are removed from the images.
CALLING SEQUENCE:
function smooc,ar,nh,nv,xsize,ysize,minx,maxx,miny,maxy,difmax,i2
CALLS: ***
C1_WSMDIF, COSRMV, WRITEFITS
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NAME:
sphere_distance
PURPOSE:
Get angle between two vectors
CATEGORY:
sat/idl/toolbox/math
CALLING SEQUENCE:
FUNCTION sphere_distance, Los1, Los2, Los3, Los4, Los5, Los6, $
degrees = degrees , $
rectangular = rectangular , $
eps = eps
INPUTS:
Los1, Los2 any arrays with 1st dimension of 2 or 3 elements
containing vector coordinates in spherical
(longitude, latitude, distance) or rectangular (x,y,z)
coordinates.
OPTIONAL INPUT PARAMETERS:
/degrees if set, all angles are in degrees (default: radians)
/rectangular if set, Los1 and Los2 are in rectangular (x,y,z) coordinates
OUTPUTS:
E distances in range [0,180] degrees.
The array size is the same as for the input array with
the 1st dimension removed.
OPTIONAL OUTPUT PARAMETERS:
eps=eps position angle of Los2 relative to north at Los2
(only works if /rectangular is NOT set)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, SubArray, SuperArray, SyncArgs, SyncDims, ToRadians
CALLED BY:
PlotCoronagraph, PlotEarthSkymap [1], PlotEloTimeMap, RemoteView_FOV_Cube
RemoteView_Init_FOV, ThomsonLOSRomb, ThomsonLOSStep, big_elongation
coriolis_map, cv, eclipsed_area, maygeometry, qnagoya_plot, smei_findpnt
smei_frm_summary, smei_hdr_plot, smei_sgp4_orbits, smei_star_fit, smei_star_test
smei_zld_weekly, sphere_great_arc, sphere_smooth, stardistance, vu_point_source
EXAMPLE:
Specify vectors in spherical coordinates (all in the equatorial plane).
Every vector in los2 is combined with the vector in los1. All angles are in degrees.
los1 = [0,0,1]
los2 = [[0,0,1], [45,0,1], [90,0,1], [135,0,1], [180,0,1]]
e = sphere_distance(los1, los2, /degrees)
print, e
0.000000 45.0000 90.0000 135.000 180.000
help, los1, los2, e
LOS1 INT = Array[3]
LOS2 INT = Array[3, 5]
E FLOAT = Array[5]
PROCEDURE:
Apply the following to the longitude and latitude angles:
L = acos( sin(lat1)*sin(lat2)+cos(lat1)*cos(lat2)*cos(lng1-lng2) )
MODIFICATION HISTORY:
AUG-2000, Paul Hick (UCSD/CASS)
DEC-2000, Paul Hick (UCSD/CASS)
Modified to accept vector arrays of any number of dimensions
JUL-2006, Paul Hick (UCSD/CASS)
Added option to provide components of vectors seperately
(using 4 or 6 arguments).
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword 'eps'. Renamed from 'elongation' to
'sphere_distance'
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NAME:
sphere_great_arc
PURPOSE:
Returns array of points along great circle
connecting two points on sphere
CATEGORY:
sat/widget/qimage_cw
CALLING SEQUENCE:
FUNCTION sphere_great_arc, los1, los2, $
npoints = npoints , $
degrees = degrees
INPUTS:
los1
los2
OPTIONAL INPUT PARAMETERS:
npoints = npoints
/degrees
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, SyncArgs, ToRadians, gridgen, sphere_distance
PROCEDURE:
MODIFICATION HISTORY:
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
sphere_smooth
PURPOSE:
Smooths data on a sphere
CATEGORY:
sat/idl/toolbox/math
CALLING SEQUENCE:
FUNCTION sphere_smooth, FF , $
irange = irange , $
igrid = igrid , $ ; Input grid
odim = odim_ , $ ; Output grid
orange = orange , $
ogrid = ogrid , $
width = width , $
gauss = gauss , $
degrees = degrees , $
weightfnc = weightfnc , $
fillall = fillall , $
fillbad = fillbad , $
fillgood = fillgood , $
min_weight = min_weight
INPUTS:
FF array[N,M,L]; type: any numerical type
N: longitudinal dimension
M: latitudinal dimension
L: number of arrays to be smoothed
OPTIONAL INPUT PARAMETERS:
irange=irange array[2,2]; type: float; default: [[0,360],[-90,90]]
Specifies the range of the input grid on which
F is defined
irange[*,0]: longitude range
irange[*,1]: latitude range
The grid specifies a skymap in
equirectangular projection
igrid=igrid array[2,N,M]; type: float
Instead of giving irange, the grid can be specified
explicitly:
igrid[0,*,*]: longitudes
igrid[1,*,*]; latitudes
Note that the grid must still be equirectangular
odim=odim array[2]; type: integer; default: [N,M]
dimensions of smoothed output skymap
The dimensions must be smaller then/equal to
the input dimensions and must be a factor of
the input dimensions.
orange=orange array[2,2]; type: float; default: irange
Specifies the range of the output grid on which
R is defined.
orange[*,0]; longitude range
orange[*,1]: latitude range
Again, this is a equirectangular grid.
ogrid=ogrid array[2,n,m]; type: float
Instead of giving odim and orange, the output
grid can be specified explicitly:
grid[0,*,*]: longitudes
grid[1,*,*]; latitudes
width=width scalare; type: float; default: 1 degree
width used to select points near each grid point
to be used for a weighted mean.
/gauss forces use of a Gaussian weighting function
with width specified in keyword 'width'.
/degrees if set, all angles are in degrees; default: radians
weight_fnc=weight_fnc
name of user-defined function to be used to calculate
weight (see PROCEDURE).
min_weight threshold for the weights. Smoothed values are ignored
if the total weight of the contributing input bins
is less then min_weight
/fillbad only fill-in 'bad' values (NaN in input array FF)
with smoothed values. This is only allowed if the
input dimension (N,M) are the same as the output
dimension odim.
/fillgood only replace good values with smoothed values
/fillall fill all values (both good and bad) by smoothed
values, i.e., same as setting both /fillbad, /fillgood.
This is also the default if neither /fillbad nor
/fillgood is set.
OUTPUTS:
R array[n,m]; type: same as FF
smoothed output skymap
OPTIONAL OUTPUT PARAMETERS:
igrid=igrid if not defined on input, they are returned as calculated
ogrid=ogrid .. from the *dim and *range keywords.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
AngleRange, ArrayLocation, BadValue, InitVar, IsType, SubArray, SuperArray, ToDegrees
ToRadians, gridgen, sphere_distance
PROCEDURE:
> If neither /gauss, nor weight_fnc is set than all points within
'width' (angular separation) of a grid point will be averaged with
the same weight.
> If /gauss is set a Gaussian weight is used in the calculation
of the average (with weight exp(-(elo/width)^2). Contributing points
will extend to about 3*width away in angular separation.
> A user-defined function weight_fnc can be used to calculate the weight.
The function should have the form
W = weight_fnc(elo, width=width, degrees=degrees)
with 'elo' (in units indicated by keyword 'degrees') the elongation,
and 'width' the input argument 'width' to this function.
MODIFICATION HISTORY:
JAN-2008, Paul Hick (UCSD/CASS)
APR-2008, Paul Hick (UCSD/CASS)
Bugfix. Weighting was done wrong.
APR-2012, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Fixed problem with /fillbad keyword. Procedure will now abort
if /fillbad is set and (some) of the points from the output grid
are not present in the input grid (this is necessary to be able
to retain good values from input array in the output array.
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NAME:
spokes
CALLING SEQUENCE:
PRO spokes
INCLUDE:
@compile_opt.pro
CALLS: ***
READFITS, WRITEFITS, WhatIs, gridgen
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NAME:
square_on_sky
CALLING SEQUENCE:
PRO square_on_sky
INCLUDE:
@compile_opt.pro
CALLS: ***
twin
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NAME:
ss_map
CALLING SEQUENCE:
pro ss_map, axyz=axyz
INCLUDE:
@compile_opt.pro
COMMON:
common defcolor
pforeground
pbackground
common ss_br_map
v_br
p_br
CALLS: ***
AngleRange, CARRINGTONT, CV_COORD, CvSky, FLT3DGEN, PLOT3DAXIS, READ_TOMOGRAPHY_B3D
gridfill, plot3darc, setup3d, twin
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NAME:
stardistance
PURPOSE:
CALLING SEQUENCE:
PRO stardistance, arcmax=arcmax, mkelo=mkelo, tmo=tmo
INCLUDE:
@compile_opt.pro
CALLING SEQUENCE:
CALLS: ***
AngleUnits, BadValue, CV_COORD, EulerRotate, FILEPATH, FindAllFiles, GeographicInfo
InitVar, Inside_Wedge, IsType, LINEARLSQFIT, MagnifyArray, REVERSE, SuperArray
TimeGet, TimeOp, TimeSet, bin_read, cvsmei, destroyvar, flat_centerofmass, gridgen
jpl_body, jpl_eph, lsqLinearFit, smei_camera, smei_frm_read, smei_frm_where
smei_pick_stars, smei_property, smei_star_info, smei_star_list, sphere_distance
view, wedge_bounding_box, wedge_content
MODIFICATION HISTORY:
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NAME:
statpos
PURPOSE:
Calculate position of average, median and maximum of array
CATEGORY:
Statistics
CALLING SEQUENCE:
FUNCTION statpos, Y , $
min = min , $
max = max , $
binsize = binsize , $
hist = hist , $
fraction= fraction
INPUTS: (read-only)
A array array for which median value is requested
A should already represent a histogram
If it isn't use one of the histogram
keywords
OPTIONAL INPUT PARAMETERS:
min=min
max=max
binsize=binsize
if any one of these keywords is set then
array Y is fed to the IDL histogram function
with these keywords.
fraction=fraction
scalar; type: float; default: 0.5
sets the fraction used for the median
calculation, i.e. finds the position
where 'fraction' are lower and 1-fraction
are higher.
OUTPUTS:
STATPOS 3 element float array
StatPos[0] position of average ('center of mass')
StatPos[1] position of median
StatPos[2] position of maximum
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType
CALLED BY:
bargraph
PROCEDURE:
The values returned by StatPos are based on the array index, i.e.
0 <= StatPos[i] <= n_elements(A)-1 (i=0,1,2)
Note that the average calculated here from the histogram depends
on the bin size. Use the mean function if that's a problem.
MODIFICATION HISTORY:
MAY-1993, Paul Hick (UCSD/CASS)
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Added keyword 'fraction'
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NAME:
StereoAOrbit
PURPOSE:
Calculate position of Stereo A (Ahead)
CATEGORY:
smei/gen/idl/ephem
CALLING SEQUENCE:
FUNCTION StereoAOrbit, T, degrees=degrees
INPUTS:
T array[n]; type: time structure
times at which s/c positions are needed
OPTIONAL INPUT PARAMETERS:
/degrees if set then angles are output in degrees
(default: radians)
OUTPUTS:
Result array[3,*]; type: float
J2000 ecliptic longitude (deg/rad), latitude
(deg/rad) and distance (AU).
The angular units depend on the setting of /degrees
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, KeplerOrbit, TimeGet, TimeSet, ToDegrees
CALLED BY:
big_eph
RESTRICTIONS:
The precision is probably about 0.1 degrees in ecliptic longitude,
provided orbital elements are added as needed (once or twice year?)
PROCECURE:
From http://ssd.jpl.nasa.gov/horizons.cgi
(J2000.0 Orbital Elements)
Elements cover four periods between 2007/01/01 and 2007/09/30:
2007/01/01 -> 2007/01/31
2454115.500000000 = A.D. 2007-Jan-15 00:00:00.0000 (CT)
EC= 9.509555173766652E-03 QR= 9.620747268989945E-01 IN= 1.306235954146905E-01
OM= 2.380953113698972E+02 W = 3.355229542907300E+02 Tp= 2454210.608155566733
N = 1.029594704279364E+00 MA= 2.620771466946642E+02 TA= 2.609996629128498E+02
A = 9.713114668842425E-01 AD= 9.805482068694904E-01 PR= 3.496521480770163E+02
2007/02/01 -> 2007/02/28
2454147.500000000 = A.D. 2007-Feb-16 00:00:00.0000 (CT)
EC= 6.279052167650651E-03 QR= 9.596197332195503E-01 IN= 1.213139724936570E-01
OM= 2.169765459780858E+02 W = 5.374894575771112E+01 Tp= 2454265.510775187053
N = 1.038608771871410E+00 MA= 2.374329737152352E+02 TA= 2.368291467561132E+02
A = 9.656833090947861E-01 AD= 9.717468849700218E-01 PR= 3.466175231231067E+02
2007/03/01 -> 2007/03/31
2454175.500000000 = A.D. 2007-Mar-16 00:00:00.0000 (CT)
EC= 6.226246274394636E-03 QR= 9.577018334129234E-01 IN= 1.234975641202794E-01
OM= 2.149185709343068E+02 W = 7.828787777683904E+01 Tp= 2454286.911843170412
N = 1.041813256894421E+00 MA= 2.439296648101152E+02 TA= 2.432909800026552E+02
A = 9.637020798975118E-01 AD= 9.697023263821002E-01 PR= 3.455513717238894E+02
2007/04/01 -> 2007/10/01
2454253.500000000 = A.D. 2007-Jun-02 00:00:00.0000 (CT)
EC= 5.917966070544746E-03 QR= 9.565996862733112E-01 IN= 1.251469150146348E-01
OM= 2.143572837656983E+02 W = 9.239562034525594E+01 Tp= 2454299.754766134545
N = 1.044099914070154E+00 MA= 3.117054026536591E+02 TA= 3.111966164343318E+02
A = 9.622945125484443E-01 AD= 9.679893388235775E-01 PR= 3.447945882847869E+02
2007/10/01 -> now
2454466.500000000 = A.D. 2008-Jan-01 00:00:00.0000 (CT)
EC= 5.655394382946006E-03 QR= 9.564978161375505E-01 IN= 1.253836830038676E-01
OM= 2.142571411361414E+02 W = 9.225614784090398E+01 Tp= 2454299.536585085094
N = 1.044680486714094E+00 MA= 1.744234215566499E+02 TA= 1.744859573944121E+02
A = 9.619379546429810E-01 AD= 9.673780931484115E-01 PR= 3.446029715098184E+02
2011/01/21 -> 2012/01/21
2455583.500000000 = A.D. 2011-Jan-22 00:00:00.0000 (CT)
EC= 5.649610774525156E-03 QR= 9.563712745374616E-01 IN= 1.256261457055498E-01
OM= 2.140504362161804E+02 W = 9.348075068567380E+01 Tp= 2455678.680902264081
N = 1.044896949233696E+00 MA= 2.605457655988884E+02 TA= 2.599079145507906E+02
A = 9.618050989876956E-01 AD= 9.672389234379295E-01 PR= 3.445315830082727E+02
2012/01/21 -> now
2455948.500000000 = A.D. 2012-Jan-22 00:00:00.0000 (CT)
EC= 5.705938568515530E-03 QR= 9.563266675804051E-01 IN= 1.257640058659871E-01
OM= 2.139833070619798E+02 W = 9.406913424182217E+01 Tp= 2456023.716625969391
N = 1.044881265762684E+00 MA= 2.814075566505216E+02 TA= 2.807657290779928E+02
A = 9.618147233058820E-01 AD= 9.673027790313589E-01 PR= 3.445367543624463E+02
JDCT Epoch Julian Date, Coordinate Time
EC Eccentricity, e
QR Periapsis distance, q (AU)
IN Inclination w.r.t xy-plane, i (degrees)
OM Longitude of Ascending Node, OMEGA, (degrees)
W Argument of Perifocus, w (degrees)
Tp Time of periapsis (Julian day number)
N Mean motion, n (degrees/day)
MA Mean anomaly, M (degrees)
TA True anomaly, nu (degrees)
A Semi-major axis, a (AU)
AD Apoapsis distance (AU)
PR Orbital period (day)
MODIFICATION HISTORY:
AUG-2007, George Megally (UCSD/CASS; gmegally@ucsd.edu)
AUG-2007, John Clover (UCSD/CASS; jclover@ucsd.edu)
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Split up into seperate routines for A and B.
Updated orbital elements from Horizon (almost, but not quite the
same as the original ones).
JUN-2009, John Clover (UCSD/CASS; jclover@ucsd.edu)
Fixed time structure to cover the whole of the end of the day between
elements.
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NAME:
StereoBOrbit
PURPOSE:
Calculate position of Stereo B (Behind)
CATEGORY:
smei/gen/idl/ephem
CALLING SEQUENCE:
FUNCTION StereoBOrbit, T, degrees=degrees
INPUTS:
T array[n]; type: time structure
times at which s/c positions are needed
OPTIONAL INPUT PARAMETERS:
/degrees if set then angles are output in degrees (default: radians)
OUTPUTS:
Result array[3,*]; type: float
J2000 ecliptic longitude (deg/rad), latitude
(deg/rad) and distance (AU).
The angular units depend on the setting of /degrees
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, KeplerOrbit, TimeGet, TimeSet, ToDegrees
CALLED BY:
big_eph
RESTRICTIONS:
The precision is probably about 0.1 degrees in ecliptic longitude,
provided orbital elements are added as needed (once or twice year?)
PROCECURE:
From http://ssd.jpl.nasa.gov/horizons.cgi
(J2000.0 Orbital Elements)
Elements cover four periods between 2007/01/01 and 2007/09/30:
2007/01/01 -> 2007/01/31
2454115.500000000 = A.D. 2007-Jan-15 00:00:00.0000 (CT)
EC= 2.717512429419864E-02 QR= 9.315766343405397E-01 IN= 2.062856692554812E-01
OM= 1.265504225590081E+02 W = 2.009817559818071E+02 Tp= 2453977.546381154098
N = 1.051787957703235E+00 MA= 1.450979550234674E+02 TA= 1.468311244708070E+02
A = 9.575995203295605E-01 AD= 9.836224063185813E-01 PR= 3.422743123871886E+02
2007/02/01 -> 2007/02/28
2454147.500000000 = A.D. 2007-Feb-16 00:00:00.0000 (CT)
EC= 4.699285093170608E-02 QR= 9.871128055468245E-01 IN= 2.992287472926523E-01
OM= 3.392409078493881E+02 W = 1.283202740400959E+02 Tp= 2454109.145052516367
N = 9.349709833378660E-01 MA= 3.586076296454760E+01 TA= 3.917087846701419E+01
A = 1.035787408847744E+00 AD= 1.084462012148664E+00 PR= 3.850386872058772E+02
2007/03/01 -> 2007/03/31
2454175.500000000 = A.D. 2007-Mar-16 00:00:00.0000 (CT)
EC= 4.372120282913373E-02 QR= 9.936734937715849E-01 IN= 3.079140638493386E-01
OM= 3.385303364716559E+02 W = 1.396338867376834E+02 Tp= 2454119.296489763539
N = 9.304977044270033E-01 MA= 5.229723725577440E+01 TA= 5.639454403113316E+01
A = 1.039104387456201E+00 AD= 1.084535281140816E+00 PR= 3.868897239479882E+02
2007/04/01 -> 2007/10/01
2454253.500000000 = A.D. 2007-Jun-02 00:00:00.0000 (CT)
EC= 4.182627806223717E-02 QR= 9.986984397920566E-01 IN= 2.942094890131228E-01
OM= 3.365510702179411E+02 W = 1.467482264878249E+02 Tp= 2454124.112501636613
N = 9.262301226788787E-01 MA= 1.198425984820785E+02 TA= 1.238910903027097E+02
A = 1.042293706168792E+00 AD= 1.085888972545528E+00 PR= 3.886723085174492E+02
2007/10/01 -> now
2454466.500000000 = A.D. 2008-Jan-01 00:00:00.0000 (CT)
EC= 4.143096626093998E-02 QR= 9.996061655975762E-01 IN= 2.943195765731059E-01
OM= 3.364601578200525E+02 W = 1.467863556683245E+02 Tp= 2454512.857852065004
N = 9.255412455738544E-01 MA= 3.170938958574695E+02 TA= 3.137364080607738E+02
A = 1.042810825735152E+00 AD= 1.086015485872728E+00 PR= 3.889615959543680E+02
JDCT Epoch Julian Date, Coordinate Time
EC Eccentricity, e
QR Periapsis distance, q (AU)
IN Inclination w.r.t xy-plane, i (degrees)
OM Longitude of Ascending Node, OMEGA, (degrees)
W Argument of Perifocus, w (degrees)
Tp Time of periapsis (Julian day number)
N Mean motion, n (degrees/day)
MA Mean anomaly, M (degrees)
TA True anomaly, nu (degrees)
A Semi-major axis, a (AU)
AD Apoapsis distance (AU)
PR Orbital period (day)
MODIFICATION HISTORY:
AUG-2007, George Megally (UCSD/CASS; gmegally@ucsd.edu)
AUG-2007, John Clover (UCSD/CASS; jclover@ucsd.edu)
JUL-2008, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Split up into seperate routines for A and B.
Updated orbital elements from Horizon (almost, but not quite the
same as the original ones).
JUN-2009, John Clover (UCSD/CASS; jclover@ucsd.edu)
Fixed time structure to cover the whole of the end of the day between
elements.
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NAME:
stopwatch
PURPOSE:
CATEGORY:
Totally unnecessary
CALLING SEQUENCE:
PRO stopwatch, set=set, start=start, stop=stop
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType, TimeGet, TimeOp, TimeSystem, TimeUnit
CALLED BY:
flt_read
MODIFICATION HISTORY:
JUL-2003, Paul Hick (UCSD/CASS)
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NAME:
strbreak
PURPOSE:
Split string in pieces at white space
CALLING SEQUENCE:
FUNCTION strbreak, label, tokens=tokens
COMMON:
@compile_opt.pro
CALLS: ***
boost, destroyvar
CALLED BY:
txt_block_read
PROCEDURE:
Substrings enclosed by double quotes are left intact,
i.e. are treated as a single piece without whitespace.
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NAME:
STRETCH
PURPOSE:
Stretch the image display color tables so the full range
runs from one color index to another.
CATEGORY:
Image processing, point operations.
CALLING SEQUENCE:
STRETCH, Low, High [, /CHOP]
INPUTS:
Low: The lowest pixel value to use. If this parameter is omitted,
0 is assumed. Appropriate values range from 0 to the number
of available colors-1.
High: The highest pixel value to use. If this parameter is omitted,
the number of colors-1 is assumed. Appropriate values range
from 0 to the number of available colors-1.
OPTIONAL INPUTS:
Gamma: Gamma correction factor. If this value is omitted, 1.0 is
assumed. Gamma correction works by raising the color indices
to the Gamma power, assuming they are scaled into the range
0 to 1.
KEYWORD PARAMETERS:
CHOP: If this keyword is set, color values above the upper threshold
are set to color index 0. Normally, values above the upper
threshold are set to the maximum color index.
OUTPUTS:
No explicit outputs.
CALLED BY:
GetColors [2], GetColors [3], PlotEarthSkymap [2], PlotEarthSkymap [3]
PlotEarthSkymap [4], Stretch_Colors, allsky [1], allsky [2], allsky [3], allsky_f
flip_colors, ipsv [1], ipsv [2], ipsv [3], nagoya_glevel, vu_get_page
vu_thomson_antifish, vu_thomson_hammer
COMMON BLOCKS:
COLORS: The common block that contains R, G, and B color
tables loaded by LOADCT, HSV, HLS and others.
SIDE EFFECTS:
Image display color tables are loaded.
RESTRICTIONS:
Common block COLORS must be loaded before calling STRETCH.
PROCEDURE:
New R, G, and B vectors are created by linearly interpolating
the vectors in the common block from Low to High. Vectors in the
common block are not changed.
If NO parameters are supplied, the original color tables are
restored.
EXAMPLE:
Load the STD GAMMA-II color table by entering:
LOADCT, 5
Create and display and image by entering:
TVSCL, DIST(300)
Now adjust the color table with STRETCH. Make the entire color table
fit in the range 0 to 70 by entering:
STRETCH, 0, 70
Notice that pixel values above 70 are now colored white. Restore the
original color table by entering:
STRETCH
MODIFICATION HISTORY:
DMS, RSI, Dec, 1983.
DMS, April, 1987. Changed common.
DMS, October, 1987. For unix.
DMS, RSI, Nov., 1990. Added GAMMA parameter.
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NAME:
Stretch_Colors
PURPOSE:
Reverse color table
CATEGORY:
Annoying
CALLING SEQUENCE:
PRO Stretch_Colors, reverse=reverse, silent=silent
INPUTS:
(none)
OPTIONAL INPUT PARAMETERS:
/reverse if set then reverse the color table
OUTPUTS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, STRETCH
PROCEDURE:
MODIFICATION HISTORY:
MAR-2009, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
strposn
PURPOSE:
Locates a substring in an array of strings and returns
string arrays for preceding and trailing parts. By default, the
substring is removed, but can be retained using keywords
TrailingFront or LeadingBack
CATEGORY:
string manipulation
CALLING SEQUENCE:
FUNCTION strposn, Strings, SubStr, Front, Back, $
Last = Last , $
frontdefault = FrontDefault , $
trailingfront = TrailingFront , $
leadingback = LeadingBack
INPUTS:
Strings string array or scalar (read-only)
Substr string scalar or array (read-only)
If not specified the scalar Substr=',' (comma) is used
Substring(s) to be searched for. If more than one
substring is specified to position of the string with
the lowest (highers if /last is set) index is returned.
OPTIONAL INPUT PARAMETERS:
/last if set, search is for the last occurence of Substr
(similar to rstrpos; default is to search for the
first occurence, similar to strpos)
/frontdefault if set, strings which do not contain Substr
are returned in the Front array
(by default these strings will be returned in Back)
/trailingfront if set, and Substr is found it will be attached to
the end of the Front array (i.e. SubStr is used as a
terminator).
/leadingback if set, and Substr is found it will be attached to the
front of the Back array (i.e. Substr is used as a prefix)
OUTPUTS:
Index long integer array of same structure as Strings
Contains the starting positions of SubStr (set to -1
for strings not containing SubStr) i.e. same as for
strpos and rstrpos
Front string variable of same structure as Strings.
Contains the sections of the strings preceding SubStr
- includes Substr if Trailingfront is set
- includes strings not containing SubStr if
Frontdefault is set
Back string variable of same structure as Strings.
Contains the sections of the strings following SubStr
- includes Substr if Leadingback is set
- includes strings not containing SubStr unless
Frontdefault is set
OPTIONAL OUTPUT PARAMETERS:
(None)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, REVERSE, SyncDims, UNIQ
CALLED BY:
GetFileSpec, PutFileSpec, SetFileSpec, timeposn, txt_block_read, vox_update
www_help_crosslinks, www_help_make, www_help_names, www_help_tree
SIDE EFFECTS:
TrailingFront and LeadingBack are mutually exclusive. If both are
present TrailingFront takes precedence.
RESTRICTIONS:
None
PROCEDURE:
MODIFICATION HISTORY:
DEC-1997, Paul Hick (UCSD/CASS)
MAR-2003, Paul Hick (UCSD/CASS)
Improved efficiency. Removed one of the two remaining explicit DO-loops,
made the second more compact.
DEC-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Argument Substr can now be an array (used to be scalar only)
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NAME:
strreverse
PURPOSE:
Reverse order of chars in string
CATEGORY:
gen/idl/toolbox
CALLING SEQUENCE:
FUNCTION strreverse, str
INPUTS:
str scalar or array; type: string
OUTPUTS:
result same as input with order of chars
in all strings reversed
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
REVERSE
CALLED BY:
TimePosn_test, qsmei_sky_pick, smei_filename
MODIFICATION HISTORY:
DEC-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SubArray
PURPOSE:
Extract/add/multiply subarrays in a multi-dimensional array
CATEGORY:
Array strangling
CALLING SEQUENCE:
FUNCTION SubArray, L, $
element = Element , $
dimension = Dimension , $
lastelement = LastElement , $
lastdimension = LastDimension , $
add = add , $
multiply = multiply , $
divide = divide , $
replace = replace , $
clear = clear , $
type = type , $
value = value
R = SubArray(L) Extract subarray with dimension=0, element=0
R = SubArray(L,add=1) Add 1 to subarray with dimension=0, element=0
INPUTS:
L any multi-dimensional array
OPTIONAL INPUT PARAMETERS:
dimension=dimension scalar; type: integer
identifies one of the dimensions, 0,..,(size(L))[0]-1
/lastdimension selects the trailing dimension of L, i.e.
equivalent to dimension=(size(L))[0]-1
(/lastdimension takes precedence over the dimension keyword)
If neither 'dimension' nor 'lastdimension' are used, then dimension=0 is assumed
element=element scalar; type: integer
identifies one of the elements in the selected dimension,
0,..,(size(L))[Dimension+1]-1
/lastelement selects the last element of the selected dimension, i.e.
equivalent to element=(size(L))[Dimension+1]-1.
If neither 'element' nor 'lastelement' are used, then element=0 is assumed
add=add scalar or array with same # elements as the subarray identified
by (dimension, element). 'Add' will be added to the subarray.
multiply=multiply scalar or array with same # elements as the subarray identified
by (dimension, element). 'multiply' will be multiplied to
the subarray.'multiply' is executed prior to 'add'
replace=Replace replaces elements
Takes precedence over 'add' and 'multiply'
/clear sets elements to zero (numerical input) or null-string (string input)
Take precedence over 'multiply'
type=type makes a subarray of the appropriate type (filled with zeroes)
If neither of 'type','add','multiply','replace' and 'clear' is used, then
the selected subarray will be extracted.
OUTPUTS:
If 'add' or 'multipy' or 'replace', or 'clear' are used:
Input array with the selected subarray modified.
If 'type is set then a subarray of the selected type is returned
Otherwise:
Array with one dimension less than the input array, corresponding
to the selected subarray.
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, IsType
CALLED BY:
AngleUnits, Carrington, CenterOfMass, CvPointOnLos, CvSky_Equatorial, CvSky_GSE
CvSky_GSEQ, CvSky_GSM, CvSky_Geographic, CvSky_HEEQ, CvSky_Heliographic, CvSky_IHG
CvSky_Precess, CvSky_RTN, CvSky_Solar_EloPa, Distance2Line, EulerRotate
GeographicInfo, IPS_hlevel_w, Inside_Wedge, RotationMeasure, TMO_skymotion
ThomsonBrightness, TimeArray, TimeGet, cvsmei, haystack_2006, img_read, jpl_parallax
jpl_phase, jpl_sizeofsun, lospos, lsqCircleFit, lsqQuadraticFit, put_logo
qImage_cw_BoxCosine, smei_ccd2sky, smei_radial2theta, smei_theta2radial
sphere_distance, sphere_smooth, thomsonfig, vu_atlocation, vu_cvgrid, vu_fnc
vu_lineofsight, vu_type_insitu
PROCEDURE:
Trivial
MODIFICATION HISTORY:
MAR-1998, Paul Hick (UCSD/CASS)
OCT-2004, Paul Hick (UCSD/CASS)
Modifications to allow string input for /clear and /replace
MAR-200r, Paul Hick (UCSD/CASS, pphick@ucsd.edu)
Added type=type keyword.
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NAME:
SuperArray
PURPOSE:
Add a dimension to an array
CATEGORY:
Array strangling
CALLING SEQUENCE:
FUNCTION SuperArray, L, N, lead=Lead, trail=Trail, after=After, before=Before
INPUTS:
L numerical scalar or array
N int scalar
# elements in the extra dimension
OPTIONAL INPUT PARAMETERS:
!!! dimensions are counted 1,..,size(L)
/lead new dimension is first dimension
/trail new dimension is last dimension
after=After
insert new dimension after dimension After
before=Before
insert new dimension before dimension Before
OUTPUTS:
Array with one dimension of N elements more than input variable
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
IsType
CALLED BY:
AngleUnits, ColorEloTimeBox, ColorPolarBox, ColorSkybox, CvSky, CvSky_Equatorial
CvSky_GSEQ, CvSky_GSM, CvSky_Geographic, CvSky_HEEQ, CvSky_Heliographic, CvSky_IHG
CvSky_Precess, Distance2Line, Distance2Sun, EarthSky3DLoc, EarthTransit3DLoc
EulerRotate, FrameMoments, GetStarShape, HOSOrbit, IPS_hlevel_w, MagnifyArray
PRO bold, PlotCoronagraph, PlotEarthSkymap [1], PlotEarthSkymap [2]
PlotEloTimeMap, RGBO_DepthCue, RGBO_Project, RemoteView, RemoteView_Display2D
RemoteView_Display3D, RemoteView_FOV, RemoteView_Init_Matrix
RemoteView_Init_View, RemoteView_StereoStates, SMEI_cr_removal, SyncArgsSub
TMO_skymotion, TMO_tracksky, ThomsonLOSDensity, ThomsonLOSStep, TimeArray, TimeGet
allsky [1], allsky [2], allsky [3], allsky_f, badpix, big_eph, even_light
even_light_corrections, even_light_info, get_page, gridgen, haystack_2006
img_read, jpl_mag, jpl_phase, lospos, lsqLinearFit, mpc_eph, mpc_orbit_eph, plot3darc
plot_ipv6_fraction, plot_traffic, put_logo, qImage_cw_BoxCosine
qImage_cw_ZEllipse, qView_FileFilter, qView_ModifyData, qView_PickFiles
qView_PlotSeries, qView_SubtractBase, sgp4_eph, sgp4_tle, show_wso, smei_findpnt
smei_frm_flatfield, smei_frm_where, smei_radial2theta, smei_sky, smei_sky_track
sphere_distance, sphere_smooth, stardistance, testsmei, thomsonfig, trypleiades
unitvectors, vu_atlocation, vu_check, vu_coronagraph, vu_earthskymap, vu_elotime
vu_extract, vu_lineofsight, vu_mean, vu_radialcut, vu_read, vu_syncgrid
vu_synopticmap, vu_timeseries, wedge_content
EXAMPLE:
R = SuperArray( indgen(3,4,5), 10, after=2)
creates an array R[3,4,10,5)
PROCEDURE:
The basic building block is the expression replicate(1,N)#L
Reform and transpose are used to control the array structure.
MODIFICATION HISTORY:
MAR-1998, Paul Hick (UCSD/CASS)
FEB-2000, Paul Hick (UCSD/CASS)
added handling of string arrays.
JUN-2003, Paul Hick (UCSD/CASS, pphick@ucsd.edu)
Fixed bug adding to array with trailing dummy dimension.
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NAME:
surfertable
CALLING SEQUENCE:
PRO surfertable
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MODIFYCT, gridgen, surfertable_update [1], surfertable_update [2]
CALLED BY:
surfertable_update [1], surfertable_update [2]
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NAME:
surfertable
CALLING SEQUENCE:
PRO surfertable
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MODIFYCT, gridgen, surfertable_update [1], surfertable_update [2]
CALLED BY:
surfertable_update [1], surfertable_update [2]
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NAME:
surfertable
CALLING SEQUENCE:
PRO surfertable
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MODIFYCT, gridgen, surfertable_update [1], surfertable_update [2]
CALLED BY:
surfertable_update [1], surfertable_update [2]
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NAME:
surfertable_update
CALLING SEQUENCE:
PRO surfertable_update, itable, name, p,r,g,b, bw=bw
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MODIFYCT, gridgen, surfertable [1], surfertable [2], surfertable [3]
CALLED BY:
surfertable [1], surfertable [2], surfertable [3]
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NAME:
surfertable_update
CALLING SEQUENCE:
PRO surfertable_update, itable, name, p,r,g,b, bw=bw
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MODIFYCT, gridgen, surfertable [1], surfertable [2], surfertable [3]
CALLED BY:
surfertable [1], surfertable [2], surfertable [3]
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NAME:
SyncArgs
PURPOSE:
Change a list of arguments (usually a combination of scalars and
arrays) to a list of arrays of equal size.
CALLING SEQUENCE:
PRO SyncArgs, A0,A1,A2,A3,A4,A5,A6,A7,A8,A9
INPUTS:
A0,...,A9 any type of argument
OUTPUTS:
A0,...,A9 arguments of same size
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
who_am_i
CALLED BY:
CombineRotations, EarthSky3DLoc, GeographicInfo, HOSOrbit, ThomsonLOSFar
ThomsonLOSRomb, ThomsonMidpointFar, ThomsonPDistance, ThomsonPDistanceFar
TimeMonth, TimeSet, TimeYDate, eclipsed_area, lsqCircleFit, lsqQuadraticFit
nrZBrent, nrZbrac, scalarproduct, sgp4_orbit_period, smei_filename, smei_frm_mask
smei_sky_field, sphere_distance, sphere_great_arc, timeposn, vectorproduct
RESTRICTIONS:
A maximum of 10 arguments is permitted
PROCEDURE:
> Arguments that don't exist on input, will be created as type byte
(unless none of the arguments exist)
> If no arrays are present a list of scalars is returned
> Arguments are changed to arrays with the same structure as the largest
array in the list of arguments.
> If there is more than one such array, the first one in the list used
as target. The others are reformed to match the target type
> Scalars and arrays with one element will always be changed to match
the largest array.
> Arrays with size smaller than the target array are boosted to match
the target array only if the dimensions are the same as the leading
dimensions are the same as for the target array.
MODIFICATION HISTORY:
MAR-1995, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SyncArgsSub
PURPOSE:
Intenal use by SyncArgs only
CALLING SEQUENCE:
PRO SyncArgsSub, A0, N, s
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
SuperArray
MODIFICATION HISTORY:
MAR-1995, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
SyncDims
PURPOSE:
Reforms A to have the same size (scalar or array) as specified in Size
CATEGORY:
Toolbox
CALLING SEQUENCE:
SyncDims, A, sizeinfo = size(SomeVariable)
SyncDims, A, extendinfo = size(SomeVariable)
SyncDims, A, replicateinfo = [size(Array1), size(Array2),...]
INPUTS:
A scalar or array of any type
OPTIONAL INPUTS:
sizeinfo 'size and type' vector as returned by the IDL
'size' function (only the size information is used)
OUTPUTS:
sizeinfo:
A input array with structure modified to match SizeInfo
(note: array content is not tampered with)
extendinfo:
A
replicateinfo:
A 'size and type' vector, obtained by concatenating the
information from the input 'size and type' vectors.
CALLED BY:
AngleUnits, BZero, CenterOfMass, CvPointOnLos, Distance2Line, EulerRotate, FishEye
GetFileSpec, HammerAitoff, MercatorProj, NewcombSun, RemoteView_FOV_loc
SetFileSpec, TMO_skymotion, ThomsonLOSRomb, TimeInterpol, TimeSplit, TimeString
coord3to2, cvsmei, nrZbrak, qImage_cw_Transform, scalarproduct, smei_ccd2sky
smei_sky2cam, smei_sky2ccd, smei_sky_field, smei_zld_dumbbell, smei_zld_weekly
sphere_distance, strposn, vectorproduct, vu_atlocation
RESTRICTIONS:
No check is made that Size actually represents a valid size vector.
PROCEDURE:
Used usually before exiting a procedure to make sure that
input and output array have exactly the same structure.
MODIFICATION HISTORY:
DEC-1997, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
