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NAME:
e9hos
CALLING SEQUENCE:
function e9hos, filename
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CONV_VAX_UNIX, E9REV, FRECL, InitVar
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NAME:
EarthSky3DLoc
PURPOSE:
Returns the 3D positions for all segments along a collection of lines
of sight. The lines of sight either form a grid for a 2D sky map, or
are explicitly input.
CATEGORY:
sat/idl/util
CALLING SEQUENCE:
FUNCTION EarthSky3DLoc, UT , $
cv2carrington=cv2carrington, $
nra = nra , $
nde = nde , $
nrr = nrr , $
drr = drr , $
equator = equator , $
degrees = degrees , $
ra = ra , $
dec = dec , $
zero_point = zero_point, $
zero_phase = zero_phase, $
zero_shift = zero_shift, $
rr_earth = rr_earth , $
ut_earth = tt , $
pa_earth = pa_earth , $
elo_earth = elo_earth , $
elo_sun = elo_sun , $
center = center , $
rr_los = rr_los , $`
_extra = _extra
INPUTS:
UT scalar; type: standard time structure
time when skymap is required
OPTIONAL INPUT PARAMETERS:
/degrees if set then all in- and ouput angles are in degrees
(default: radians)
/equator by default the lines of sight are specified in ecliptic coordinates
(i.e. in a skymap the horizontal plane is the ecliptic).
If /equator is set then equatorial coordinates are assumed (i.e.
in a skymap the horizontal plane is Earth's equator)
/cv2carrington
NOTE: this only makes sense if keyword /to_heliographic is set !!
By default, the longitudinal (first) dimension in the output
R and rr_earth is a phase angle (longitude).
If heliographic coordinates are used then instead of an angle
a Carrington variable within 0.5 of the Carrington variable
corresponding to input time UT is returned.
zero_shift=zero_shift
scalar; type: float; default: 0.0
shifts the center of the sky grid. Instead of centering on the
Sun the grid is shifted to increasing RA or ecliptic longitude
by 'zero_shift'.
The units must be consistent with the setting of /degrees.
nrr scalar; type: int; default: 20
number of steps along lines of sight at each point in the sky
drr scalar; type: float; default: 0.1
step size along line of sight (AU)
Lines of sight are specified as sidereal location in the sky (either
RA/dec (/equator SET) or ecliptic longitude/latitude (/equator NOT set).
If nRA and nDE are set to non-zero values then a grid of lines of sight
covering the entire sky is created (see PROCEDURE):
nra scalar; type: int; default: 72
nr of points in skymap in longitudinal direction (either right
ascensions of ecliptic longitude)
If nra or nde is set to zero then ra and dec are used as input.
nde scalar; type: int; default: 36
nr of points in skymap in latitudinal direction (either declination
or ecliptic latitude)
Alternatively, set the product nra*nde=0 and specify lines of sight explicitly
through keywords ra,dec:
ra[nLOS]
scalar or array; right ascensions (/equator SET) or
ecliptic longitudes (/equator NOT set)
dec[nLOS]
scalar or array; declinations (/equator SET) or
ecliptic latitudes (/equator NOT set).
OUTPUTS:
Result array[3,nra,nde,nrr]; type: double
array[3,nlos,nrr]; type: float (if nra or nde is zero)
3D locations for all segments along all lines of sight. This is where
values need to obtained by interpolation on the 3D arrays.
The result is in spherical coordinates in the coordinates specified
as one of the /to_* keywords to CvSky.
R[0,*,*,*]: longitudes
If /to_heliographic and /cv2carrington are SET then
these are Carrington variables within 0.5 of Carrington(UT)
R[1,*,*,*]; latitudes
R[2,*,*,*]: heliocentric distances (AU)
OPTIONAL OUTPUT PARAMETERS:
Only if nra*nde not equal 0 on input:
ra array[nra]; type: float
right ascensions or ecliptic longitudes across sky
(with ra/longitude of Sun in center of array)
i.e. ra = (ra Sun at time UT) -pi+2*pi/nra*[0.5,1.5,...,nra-0.5]
dec array[nDE]; type: float
declination or ecliptic latitude across sky
(with decl/lat zero in center of array)
DE = -pi/2+pi/nDE*[0.5,1.5,...,nDE-0.5]
Depending on setting of /equator, RA and DEC define a regular grid in
equatorial or ecliptic sky coordinates for the centers of the boxes for the
lines of sight used to build the skymap with the position of the Sun
centered in the RA/longitudinal direction.
zero_phase=zero_phase
scalar; type: float
right ascension or ecliptic longitude of Sun (plus zero_shift)
if specified) at time UT, i.e. this is the value on which ra is centered
zero_point=zero_point
scalar; type: float
right ascension or ecliptic longitude of Sun (plus zero_shift)
at time UT (i.e. same as 'zero_phase'; should stay to ensure
that the values are consistent when fed e.g. to PlotEarthSkymap)
rr_earth
array[3]; type: float
heliocentric location Earth in heliographic coordinates
rr_earth[0]: longitude
If /to_heliographic and /cv2carrington are SET then
these is a Carrington variable within 0.5 of Carrington(UT)
rr_earth[1]; latitude
rr_earth[2]: heliocentric distance (AU)
pa_earth=pa_earth
array[nra,nde,nrr]; type: float
line of sight position angle measured counterclockwise
from ecliptic north
elo_earth=elo_earth
array[nra,nde,nrr]; type: float
line of sight elongations: angle (Sun-Earth-los segment)
elo_sun=elo_sun
array[nra,nde,nrr]; type: float
angle Earth-Sun-los segment
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
GetColors [2], GetColors [3], PlotEarthSkymap [3], PlotEarthSkymap [4]
haystack_2006, vu_coronagraph, vu_earthskymap, vu_elotime, vu_lineofsight
vu_thomson_antifish, vu_thomson_hammer
SEE ALSO:
EarthTransit3DLoc, PlotEarthSkymap [1], PlotEarthSkymap [2]
PlotEarthSkymap [3], PlotEarthSkymap [4]
CALLS: ***
AngleRange, Carrington, CvPointOnLos, CvSky, InitVar, SuperArray, SyncArgs, ToRadians
big_eph, gridgen, jpl_body
PROCEDURE:
> The sky map is build from nRA*nDE line of sight integrations through the
F3D array. The locations in the sky of the lines of sight are
ra/Lng = (ra/Lng Sun) -180 + (360./nra)*[0.5, 1.5, .. , nra-0.5 ]
Decl./Lat = - 90 + (180./nde)*[0.5, 1.5, .. , nde-0.5 ]
Dist along los = drr*[0.5,1.5,...,nrr-1]
Note that each line of sight is centered on a 'box' of 360/nra by 180/nde
degrees, and that all lines of sight together cover the entire sky.
MODIFICATION HISTORY:
AUG-1999, Paul Hick (UCSD/CASS)
OCT-2004, Paul Hick (UCSD/CASS)
Added zero_shift keyword.
APR-2006, Paul Hick (UCSD/CASS)
Added keyword /longitudes (the previous version always returned
heliographic longitudes). Add option to explictly specify lines of sight
in RA,DEC after setting nRA*nDE=0.
FEB-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Replaced keyword /longitudes by keyword /cv2carrington
Added _extra keyword to be able to pass one of the /to_* keywords
to CvSky. This allows the return value to be in any one of the
coordinates supported by CvSky (instead of just heliographic coordinates)
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NAME:
EarthTransit3DLoc
PURPOSE:
Provides 3D heliographic coordinates for all lines of sight used for a 'transit sweep' across the sky
CATEGORY:
WWW: skymap
CALLING SEQUENCE:
FUNCTION EarthTransit3DLoc, UT, $
cv2carrington=cv2carrington, $
nra = nra , $
nde = nde , $
nrr = nrr , $
drr = drr , $
equator = equator , $
degrees = degrees , $
band = band , $
solar = solar , $
geolng = geolng , $
ra = ra , $
dec = dec , $
zero_phase = zero_phase, $
zero_point = zero_point, $
rr_earth = rr_earth , $
ut_earth = ut_earth , $
pa_earth = pa_earth , $
elo_earth = elo_earth , $
elo_sun = elo_sun , $
_extra = _extra
INPUTS:
UT scalar; type: time structure
universal time, UT
(usually UT corresponding to local noon at geographic longitude 'geolng')
OPTIONAL INPUT PARAMETERS:
/degrees if set then all in- and ouput angles are in degrees (default: radians)
Four parameters define the grid used to calculate the sky map (see PROCEDURE)
nra scalar; type: int; default: 36
# points in skymap in longitudinal direction (either right ascensions
of ecliptic longitude). Note that nRA may be modified if keyword
band is used.
nde scalar; type: int; default: 18
# points in skymap in latitudinal direction(either declination or
ecliptic latitude)
nrr scalar; type: int; default: 20
# steps along lines of sight at each point in the sky
drr scalar; type: float; default: 0.1
step size along line of sight (AU)
geolng=geolng
scalar; type: any; default: 0
geographic longitude of observing location
/equator
by default the local meridian is set up as a strip of sky centered on the
intersection with the ecliptic. This results in a sweep with the Sun
centered, and the ecliptic along the horizontal axis (but see RESTRICTIONS).
If /equator is set then the strip of sky is centered on the equator, i.e.
the strip covers the local meridian from equatorial north to equatorial south.\
This is a more strict interpretation of the concept of a 'transit sweep', but
has the disadvantage that the Sun is not at the center of the sky map.
band scalar; type: float
Width of strip to be processed (in hours)
If band is not set then meridian strips covering 24 hours centered
around UT are selected. Use this keyword to extract only a partial strip
of sky covering less than 24 hour.
/solar by default the meridian strips are centered around the meridian strip at time UT.
Setting /solar rearranges the strips, putting the meridian strip at noon in
the center (see PROCEDURE)
/cv2carrington
OUTPUTS:
R array[3,nra,nde,nrr]; type: float
3D locations (in heliographic coordinates) where values need to obtained
by interpolation on the 3D arrays.
nra scalar; type: integer
if keyword band is set then nra is set to the number of meridians
inside the RA range of width 'band'.
OPTIONAL OUTPUT PARAMETERS:
ra array[nra]; type: float
Right ascension for nra UT times covering 24 hours centered on UT
dec array[nde]; type: float
dec = -pi/2+pi/nde*[0.5,1.5,...,nde-0.5]
ra and dec define a regular grid in sky coordinates for the centers of
the boxes for the lines of sight used to sweep of the sky
zero_point=zero_point
scalar; type: float
/solar NOT set: RA angle for local meridian at 'geoloc' on time UT
/solar set : RA angle of Sun at time UT
zero_phase=zero_phase
/solar NOT set:
scalar, type: float
RA angle for local meridian at 'geoloc' on time UT
(i.e. same as zero_point)
/solar set :
array[nra]; type: float
RA angles of Sun for nRA UT times covering 24 hours centered
on UT (same times as used for output array RA).
(i.e. 'zero_point' is approximately centered in 'zero_phase')
pa_earth=pa_earth
array[nra,nde,nrr]; type: float
line of sight position angle measured counterclockwise
from ecliptic north
elo_earth=elo_earth
array[nra,nde,nrr]; type: float
line of sight elongations: angle (Sun-Earth-los segment)
elo_sun=elo_sun array[nra,nde,nrr]; type: float
angle (Earth-Sun-los segment)
rr_earth=rr_earth
array[3,nra]; type: float
heliocentric locations Earth in heliographic coordinates
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
Carrington, CvPointOnLos, CvSky, InitVar, IsType, SuperArray, TimeGST, TimeOp, TimeSet
TimeUnit, ToRadians, big_eph, gridgen, jpl_body
CALLED BY:
GetColors [2], GetColors [3], PlotEarthSkymap [3], PlotEarthSkymap [4]
vu_earthskymap, vu_thomson_antifish, vu_thomson_hammer
RESTRICTIONS:
If /equator is NOT set then the ecliptic is put on the horizontal axis. This is
done using a kludge. Each meridian strip (-90 to +90 degrees in declination with
the equator in the center, is shifted vertically to put the ecliptic in the center.
The sweep across the sky covers 24 hours in UT. Since UT is a solar time, the sweep covers
a little more than 360 degree of sky. However, the RA array still covers exactly 360
degrees (RA is passed to PlotEarthSkyMap to make a Hammer-Aitoff or fish-eye map).
PROCEDURE:
> UT is used to set up an array of nRA equally spaced times covering UT-12h to UT+12h
TT = UT+((0.5+findgen(nra))/nra-0.5)*(24)
(if 'band' is specified then only UT +/- band/2 is used).
> The geographic longitude, together with GST, is used to calculate the RA
of the local meridian (hour angle zero) at times TT
> At each ra(TT) value nde equally spaced declinations are taken
dec = ((0.5+findgen(nde))/nde-0.5)*90
> The resulting strips along the local meridian patched together give
a (partial) sweep of the sky. The return array RA is a monotonic increasing
array inside [-180,+180].
> If /solar is NOT set then the return array zero_phase contains the right ascension
of the local meridian at time UT.
If /solar is set then the return array zero_phase contains the right ascension of
the sun at the times centered on UT used also to calculate RA.
The scalar 'zero_point' and array 'zero_phase' are used to center the proper
RA in a skymap by subtracting it from RA.
> The output array rr_earth gives the location of Earth at times TT
MODIFICATION HISTORY:
SEP-1999, Paul Hick (UCSD/CASS)
FEB-2007, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
Replaced keyword /longitudes by keyword /cv2carrington
Added _extra keyword to be able to pass one of the /to_* keywords
to CvSky. This allows the return value to be in any one of the
coordinates supported by CvSky (instead of just heliographic coordinates)
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NAME:
eclipsed_area
PURPOSE:
Calculates fraction of solar disk eclipsed by Moon or Earth
CATEGORY:
gen/idl/toolbox
CALLING SEQUENCE:
FUNCTION eclipsed_area, loc_sun, loc_em, $
degrees = degrees , $
elo = elo , $
ut = ut , $
plotc = plotc , $
earth = earth , $
radius = radius , $
silent = silent , $
_extra = _extra
INPUTS:
loc_sun array[3,n] or array[3,2,n]; type: float
if array[3,n]; location of Sun in spherical coordinates
(RA,dec,distance, or long, lat, distance)
if array[3,2,n] then array[3,0,*] specifies the location
of the Sun and array[3,1,*] specifies the location
of the Moon or Earth. In this case loc_em is ignored.
loc_em array[3,n]; type: float
location of Earth or Moon in same coordinates as for the Sun.
OPTIONAL INPUT PARAMETERS:
/degrees if set, all angles are in degrees (default: radians)
/plotc if set, then results are plotted
(angular separation of Sun and Moon or Earth, and fraction of
disk eclipsed).
ut=ut array[*]; type: structure
time structure used to plot a time axis (only used
if /plotc is set).
OUTPUTS:
area array[n]; type: float
fraction of solar disk eclipsed by Moon or Earth.
OPTIONAL OUTPUT PARAMETERS:
elo array[*]; type: float
angular distance between Sun and Moon or Earth
INCLUDE:
@compile_opt.pro
CALLS: ***
BadValue, InitVar, IsTime, IsType, PlotCurve, SyncArgs, ToDegrees, ToRadians
sphere_distance
CALLED BY:
smei_frm_cvhdr, smei_frm_eclipse
PROCEDURE:
MODIFICATION HISTORY:
OCT-2004, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
edit_smei
PURPOSE:
Edits SMEI time series from ascii files
CATEGORY:
CALLING SEQUENCE:
INPUTS:
infile scalar; type: string; default: $TUB/03_148_02000_003.sm
name of input file
outfile scalar; type: string; default: <infile>.new
name of output file
OPTIONAL INPUT PARAMETERS:
first scalar; type: integer
index of first sky bin to be displayed
last scalar; type: integer
index of last sky bin to be displayed
OUTPUTS:
(written to output file)
CALLS: ***
BadValue, FILEPATH, InitVar, PlotCurve, flt_read, pcursor
PROCEDURE:
All displayed time series can be edited
Left-click selects a points; its data value is flagged as bad
Right-click terminates the selection of points, and writes the modified
data to the output file.
MODIFICATION HISTORY:
NOV-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
editsmei
PURPOSE:
Edits SMEI time series from ascii files
CATEGORY:
CALLING SEQUENCE:
INPUTS:
infile scalar; type: string; default: $TUB/03_148_02000_003.sm
name of input file
outfile scalar; type: string; default: <infile>.new
name of output file
OPTIONAL INPUT PARAMETERS:
first scalar; type: integer
index of first sky bin to be displayed
last scalar; type: integer
index of last sky bin to be displayed
OUTPUTS:
(written to output file)
CALLS: ***
BadValue, FILEPATH, InitVar, PlotCurve, flt_read, pcursor
PROCEDURE:
All displayed time series can be edited
Left-click selects a points; its data value is flagged as bad
Right-click terminates the selection of points, and writes the modified
data to the output file.
MODIFICATION HISTORY:
NOV-2003, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
env_slashes
PURPOSE:
Fixes environment variables on Windows
CATEGORY:
gen/idl/environment
CALLING SEQUENCE:
PRO env_slashes
INPUTS:
(from Windows by retrieving results of spawning
the DOS 'set' command).
OUTPUTS:
(modified env variables)
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
FILEPATH, txt_read
PROCEDURE:
On Windows SSW sets up environment variables with a mix
of back- and forward slashes. This causes problems for e.g.
the IDL dialog_pickfile procedure.
This procedure runs through all env variables and changes
forward slashes to backward slashes. Only env variables of
the form SSW_*_INSTR are not modified.
MODIFICATION HISTORY:
FEB-2002, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
EqKepler
PURPOSE:
Kepler's equation is used in the determination of orbital positions.
It gives the relation between mean and eccentric anomaly (for given
orbit eccentricity).
CATEGORY:
smei/gen/idl/ephem
CALLING SEQUENCE:
F = EqKepler(E,arg)
INPUTS:
E scalar; type: float
eccentric anomaly (radians)
arg array[2], type: float
arg[0] mean anomaly (radians)
arg[1] orbit ellipticity (eccentricity)
OUTPUTS:
EqKepler fnc value
EXTERNAL BY:
KeplerOrbit
PROCEDURE:
The eccentric anomaly is the root of Kepler's equation:
EqKepler = X-arg[1]*sin(X)-arg[0] = 0
See O. Montenbruck, "Practical Ephemeris Calculations", Springer
(1989), par. 3.1.1.4, p. 44
MODIFICATION HISTORY:
1990, Paul Hick (UCSD)
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NAME:
EulerRotate
PURPOSE:
Calculate spherical angles in rotated coordinate system
CATEGORY:
gen/idl/toolbox/math
CALLING SEQUENCE:
FUNCTION EulerRotate, ABG, In, In1, In2, degrees=Degrees, rectangular=Rectangular
INPUTS:
ABG array[3] or multi-dimensional array[3,..] with first dimension of 3
elements. If multi-dimensional, then:
1. either the array structure, except for the 1st dimension, is the same
as for In. Each position in In is rotated using the matching ABG set.
2. or In is only 1-dimensional i.e. contains only one position. Then
each ABG combination is applied to this one position.
Euler angles [A, B, G]
A phase angle of the pole Z(new) in old coordinate system
B polar angle of the pole Z(new) in old coordinate system
G phase angle of X(new) in coordinate system (2)
/rectangular NOT SET:
In any multi-dimensional array with first dimension of 2 or 3 elements.
array[0,..] is the longitude and array[1,..] the latitude;
array[3,..] (usually the radial distance) is not modified.
/rectangular SET:
In array[3,..], any multi-dimensional array with array[i,..] (i=0,2)
the x,y and z-components
OPTIONAL INPUTS:
/rectangular if set, the input array In is interpreted as vectors in rectangular
coordinates.
if not set, the input array In is assumed to be in spherical coordinates
(longitude, latitude, radial distance).
/degrees if set, input and output is in degrees
OUTPUTS:
/rectangular NOT SET:
double array with same structure as input array In
array[0:1,..] are longitude and latitude in new coordinate system
(0<=Lng<360, -90<=Lat<=90)
/rectangular SET:
array[3,..] with same structure as input array In
x,y,z coordinates in new coordinate system
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CvT3d, SubArray, SuperArray, SyncDims, ToRadians
CALLED BY:
CvPrecess, CvSky, FishEye, FitKeplerOrbit, GetColors [2], GetColors [3]
HammerAitoff, KeplerOrbit, MercatorProj, PlotCoronagraph, PlotEarthSkymap [1]
PlotEarthSkymap [2], PlotEarthSkymap [3], PlotEarthSkymap [4], PlotPlanarCut
RemoteView_CMEDensity, RemoteView_Init_FOV, RemoteView_StereoStates
RotationMeasure, ThomsonLOSDensity, qvu_draw, smei_star_stdmaps
smei_zld_dumbbell, stardistance, vu_coronagraph, vu_elotime, vu_linecut
vu_planarcut, vu_spherecut, vu_thomson_antifish, vu_thomson_hammer
PROCEDURE:
> /rectangular NOT SET:
Given longitude (phase angle) and latitude (90-polar angle) of a point
in some coordinate system [axes: X(old),Y(old),Z(old)], angles are
calculated in the new coordinate system [axes: X(new),Y(new),Z(new)]
rotated with respect to the original one over the Euler angles Alfa,
Beta, Gamma.
The rotation from old to new system is realized by
(1) rotation around Z(old) over Alfa ---> X(1),Y(1),Z(1)=Z(old)
(2) rotation around Y(1) over Beta ---> X(2),Y(2)=Y(1),Z(2)=Z(new)
(3) rotation around Z(new) over Gamma ---> X(new),Y(new),Z(new).
> /rectangular SET:
The 3D rotation !p.t is used do do the transformation.
MODIFICATION HISTORY:
1989, Paul Hick (MPAE,UCSD)
FEB-1998, Paul Hick (UCSD/CASS), added call to cvt3d to handle conversion
of rectangular coordinates
JUN-2000, Paul Hick (UCSD/CASS), added option to rotate
single position using multiple Euler angle combinations.
SEP-2001, Paul Hick (UCSD/CASS),
removed a restriction on ABG for a transformation of rectangular
coordinates. Only one set of Euler angles was allowed. Now separate
Euler angles can be specified for each vector in 'In'; these are
processed using an explicit do-loop).
AUG-2004, Paul Hick (UCSD/CASS)
For rotations of spherical coordinates (/Rectangular NOT set) a safety
check cos(angle) > (-1) made bad coordinate values disappear
(!values.f_nan > 1 returns 1, while !values.f_nan < 1 returns !values.f_nan).
The safety check now explicitly checks for bad values, so they don't
get lost.
DEC-2005, Paul Hick (UCSD/CASS, pphick@ucsd.edu)
Bug fix. When 1-element arrays are input at In and In1, the output would
be a scalar. The output should always have the same structure as the input.
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NAME:
even_light
PURPOSE:
Program used for the certification of the SMEI cameras using
the light box data take in the 3th floor clean room.
CATEGORY:
stuff
CALLING SEQUENCE:
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
CALLS: ***
ArrayLocation, BadValue, CV_COORD, CenterOfMass, EVEN_LIGHT_BIN_PHI
EVEN_LIGHT_BIN_RAD, EVEN_LIGHT_CENTROID, EVEN_LIGHT_FIRSTGUESS
EVEN_LIGHT_GEOMETRIC_FIX, EVEN_LIGHT_PRORATE, EVEN_LIGHT_SHIFT
EVEN_LIGHT_VIEW, FILEPATH, InitVar, Inside_Wedge, MEAN, REVERSE, SuperArray, TimeOp
TimeSystem, TimeUnit, WhatIs, bin_read, bin_write, destroyvar, even_light_background
even_light_corrections, even_light_pedestal, even_light_photometry
even_light_registration, flat_centerofmass, gridgen, img_read, lsqCircleFit
lsqQuadraticFit, twin, view, wedge_bounding_box
PROCEDURE:
MODIFICATION HISTORY:
???-200?, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_background
PURPOSE:
INPUTS:
adus
gain
P1
P2
OUTPUTS:
Background corrected adus
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLED BY:
even_light, even_light_info
PROCEDURE:
Calculate (adus-P1)/gain-P2
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_corrections
PURPOSE:
CATEGORY:
INPUTS:
hhvv identifies frame sequence
spot_centroid x-y coordinates of spot centroids (relative to center0)
good_spot list of spot indices to be used for obtaining corrections
bins_axis
bins_step
img_nr
center0 center of fov arc (pix)
OUTPUTS:
center0
dcenter
optaxis0
doptaxis
binwidth
dbinwidth
y_run
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
CV_COORD, FILEPATH, InitVar, IsDisplay, MEAN, SuperArray, get_page, lsqCircleFit
lsqQuadraticFit, qset_page, set_page, twin
CALLED BY:
even_light, even_light_info
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_figures
PURPOSE:
Draw stuff
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS
InitVar
CALLS: ***
InitVar, MEAN, QBARGRAPH, STDDEV, flt_read, gridgen, plot3darc, plot3dline, plot3dtext
setup3d, twin
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_info
PURPOSE:
CATEGORY:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, CORRELATE, FILEPATH, InitVar, IsType, MEAN, QPLOT, STDDEV, SuperArray, bargraph
bin_read, destroyvar, even_light_background, even_light_corrections
even_light_pedestal, even_light_photometry, even_light_plot
even_light_registration, lsqNormalFit, twin
PROCEDURE:
0: prints table of geometric constants to screen
/widget calls qplot widget
1: scatter plot: X0 vs. Y0
2: scatter plot: phi0 vs. R0
3: scatter plot: dX0 vs. dY0
4: scatter plot: VP vs. VR
5: scatter plot: bin widths vs. change in binwidth
6: scatter plot: P1+P2 vs. P2
7: widget with P1+P2, P1, P2 (including errors)
8: prints table of pedestal determination
/redo: uses adu_per_bin to recalculate pedestals before printing
if run_id is specified (single run) then a scatter plot of gain
vs. residual background for all images in the run is displayed.
if keyword /raw is set then gain vs. raw background is displayed
/excl_img: list of images to be excluded from recalculation of
pedestals and scatter plots.
9: photometric certification summary
displays summary plot of photometry: histgram of relative
photometric errors for all spots; gain, blank readout, dark reference
readout, raw background and residual background as a function of image
number.
if keyword /spots is set, all residual time series are plotted before
displaying the summary plot
if run_id is not specified (all_runs) then the qplot widget is shown
with the median photometic error for all runs.
if keyword /redo is set than the gains are recalculated using
the adu_per_bin array. Keyword excl_img can be used to exclude images
from the recalculation.
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_pedestal
PURPOSE:
CATEGORY:
camera/idl/cert
CALLING SEQUENCE:
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, LINFIT, LocalExtrema, MEAN, gridgen
CALLED BY:
even_light, even_light_info
PROCEDURE:
MODIFICATION HISTORY:
???-200?, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_photometry
PURPOSE:
CATEGORY:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, FILEPATH, InitVar, IsDisplay, IsType, MEAN, STDDEV, bargraph, destroyvar
get_page, qset_page, set_page, twin
CALLED BY:
even_light, even_light_info
PROCEDURE:
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_platescale
PURPOSE:
INCLUDE:
@compile_opt.pro ; Return to caller
CALLS: ***
MEAN, STDDEV, gridgen
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_plot
PURPOSE:
CATEGORY:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
InitVar, MEAN, STDDEV, twin
CALLED BY:
even_light_info
PROCEDURE:
MODIFICATION HISTORY:
???-????, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
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NAME:
even_light_registration
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
INPUTS:
OPTIONAL INPUT PARAMETERS:
OUTPUTS:
OPTIONAL OUTPUT PARAMETERS:
INCLUDE:
@compile_opt.pro ; On error, return to caller
CALLS: ***
BadValue, CV_COORD, FILEPATH, InitVar, IsDisplay, LINFIT, PlotCurve, STDDEV, bargraph
get_page, qset_page, set_page, twin
CALLED BY:
even_light, even_light_info
PROCEDURE:
MODIFICATION HISTORY:
???-200?, Paul Hick (UCSD/CASS; pphick@ucsd.edu)
