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NAME:
Radio Astronomy Group Fits Read
PURPOSE:
Reads RAG spectrograms from FITS files
including non-regular axes.
The procedure reads also with gzip compressed files
if they end with the extention ".gz"
CALLING SEQUENCE:
RAGFitsRead, filename[ , image, xAxis, yAxis ]
INPUT:
filename: string containing name of the file with extension
OUTPUTS:
image: 2D array containing the array read.
xAxis, yAxis: 1D arrays containing the axes.
KEYWORDS:
used for getting header informations. See "RAGFitsWrite"
for default information written.
ORIGIN, TELESCOPE, INSTRUMENT,
OBJECT: name of observed object
DATEOBS: observation date in form dd/mm/yy
TIMEOBS: start time of observation ( hh:mm:ss.ddd )
or "No Time"
DATEEND, TIMEEND: as DATEOBS and TIMEOBS,
but for the end of the observation.
BZERO, BSCALE: If they are not 0 and 1, respectively,
the data is reconstructed with the formula
with image = BZERO + BSCALE*data
BUNIT: string containing the units of the image pixels.
CTYPE1, CTYPE2: string containing the FITS type of
physical coordinates.
COMMENT, HISTORY: strings for description
of the image
NOSCALE: if set, the reconstruction with BZERO and
BSCALE is not done.
SILENT: if set, the FITS header is not printed on screen
DATAMIN, DATAMAX: Max and min of the data.
RELATIVETIME: If set, the decimal value of TIMEOBS
is NOT added to the axis values.
SIDE EFFECT:
A fits file is opened.
MODIFICATION HISTORY
Created: A. Csillaghy, ETHZ, October 1992
For IDL Sun in May 1993, A.Cs.
SILENT in june, 93, A.Cs
DATAMIN, DATAMAX; When only filename provided, the header
is read but not the array. Oct. 93, A.Cs
RELATIVETIME in august 1995, ACs
Read also compressed file in November 95, ACs
Adaptation for IDL5/SSW/Ragview in March 98 -- ACs
CALLS:
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NAME:
Radio Astronomy Group Fits Write
PURPOSE:
Writes RAG spectrograms in FITS files
including non-regular axes.
CALLING SEQUENCE:
RAGFitsWrite, image [, xAxis, yAxis ]
INPUTS:
image: 2D or 3D array of any type except string and complex.
xAxis, yAxis: 1D arrays of any type but string and complex.
They must have the same dimensions as their
corresponding dimension in "image".
The third dimension of the image must have 2 elements:
(0) the flux and (1) the polarization
KEYWORDS:
FILENAME: string containing name of the file with
extension
CONTENT: default: 'SPECTROGRAM'
ORIGIN: default; 'RAG / ETH Zurich'
TELESCOPE: default: 'Bleien Radio'
INSTRUMENT: default: 'PHOENIX'
OBJECT: default: 'SUN'
DATEOBS:observation date in form dd/mm/yy,
default: empty string.
TIMEOBS:start time of observation ( hh:mm:ss.ddd )
default: the first element of the x-axis
This keyword should generally not be used,
since the time start is generally contained in
first element of the x-axis. If timeobs is used,
its quantity will be added to the x(0)-element
when the file is read by RagFitsRead.
DATEEND, TIMEEND: as DATEOBS and TIMEOBS,
but for the end of the observation.
default: TIMEEND = TIMEOBS;
TIMEEND = empty string.
BZERO, BSCALE: to set if the data has to be reconstructed
with data = BZERO + BSCALE*image
Default: BZERO = 0; BSCALE = 1 (see
the keyword SCALING.
XZERO, YZERO: as BZERO but for x, resp, y axes.
YSCALE, YSCALE: as BSCALE but for x, resp. y axes.
These 4 keywords are only used in case of non-
regular axes.
SCALING: If present, the procedure scales automatically
the data and writes in the fits header
the computed BSCALE AND BZERO values.
If not present, the current type of the array is
stored.
"Byte": the data is written in 8-bit format.
"Integer": the data is written in 16-bit format.
"LongInt": the data is written in 32-bit format.
BUNIT: string containing the units of the image pixels.
default: '45*LOG(SFU+10)'
CTYPE1, CTYPE2: string containing the FITS type of
physical coordinates. Defaults:
CTYPE1 = 'TIME' and CTYPE2 = 'FREQ'
COMMENT, HISTORY: strings for description
of the image
INTERACTIVE: if set, the filename is asked interactively
BYTE: If SCALED is not used, BYTE allows to write
real data in byte format (symply transforming
the data without byte scaling )
NOROUND : if set, the axis is NOT rounded to two significant
digits, (default for RAG fits )
SIDE EFFECT:
A fits file is created.
MODIFICATION HISTORY
Created: A. Csillaghy, ETHZ, October 1992
BYTE keyword added in May 93, A.Cs.
NOROUND in Nov 93, A.Cs
CALLS:
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PROGECT:
Phoenix 2 solar radio spectrometer
NAME:
Radio Astronomy Group View (RAG View)
PURPOSE:
Ragview is the top level menu interface to the data
analysis software package of the Radio and Plasma Astrophysics
Group at ETH in Zurich. It is designed for, but not limited to,
the analysis of solar radio spectrograms.
More information is available at
http://www.astro.phys.ethz.ch/rag/software/ragview-manual.ps
CATEGORY
Radio (/ssw/radio)
CALLING SEQUENCE:
RagView
KEYWORDS:
FILENAME: the name of the file to read in. Allows to avoid the
file menu interface when the filename is known.
CALLS: ***
BREAK_FILE [1], BREAK_FILE [2], BREAK_FILE [3], Custom_2D, DISPLAY_2D
Files_Handling [1], Files_Handling [2], GETHMS, GETWNR, GET_DFONT [1]
GET_DFONT [2], INIT_SELECTION, Image_Info, Init_Display, LOADCT, MDisp, MODIFY, PUTHMS
PUT_SELECTION, RAGVIEW, RESPOND_WIDG, Ragview_MDisp_Int, SEL_DEL, SHOW_IMAGE
Settings, WINDOW_MANAGEMENT, break_file [4], ethz_XCHOICE
COMMON BLOCKS:
ImageReal, image, xAxis, yAxis, fName:
image: contains the 2D image array in byte, int or
real types
x-axis, y-axis: contain 1D arrays determining the
time (x) and frequency (y) values of
the image pixels.
filename: a string with the file name of the current image
Boundaries, xMin, xMax, yMin, yMax: these four
parameters are used to determine which part of the
image is actually displayed.
These common blocks are only used in the top-level user interface..
The procedures called by RagView do not use them. They are
used to access RagView data outside of the RagView program
SIDE EFFECTS:
RagView opens a lot of windows and creates files, dependent
of the user's choices.
RESTRICTIONS:
THIS SOFTWARE WORKS ONLY IN THE SSW ENVIRONMENT.
You must install it using instructions related to the ssw.
See the documntation in http://www.lmsal.com/solarsoft/
RagView requires IDL version 5.1
Works only in interactive mode.
Works only on X-Windows systems
Currently only tested on Unix systems
MODIFICATION HISTORY:
Created: (4/91) (under the name of enrad) A.Csillaghy
Institute for Astronomy, ETH Zurich
Window+Selection Management added in August 1991, Cs.
NOERASE keyword in June, 93
titles kept even outside the session, Nov 93, A.cs
IDL transformations Jan 95 ACs
SSW adaptation, renamed from enrad to ragview,
IDL 5 version March 1998 ACs
IDL 5.1 version in October 1998, csillag@ssl.berkeley.edu
The procedure General_Menu was replaced by XChoice
since WMenu (used in general_menu) crashes on
solaris/idl 5.1
xchoice changed to ethz_xchoice 12/9/98 ACs
Parameters in call to FILE_BREAK adapted to avoid setting
fName to an empty string. Oliver Trachsel,
oliver.trachsel@email.ch, 2002/01/30
2004-08-25- csillag@fh-aargau.ch, changed default color table
from 39 to 5
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PROGECT:
Phoenix 2 solar radio spectrometer
NAME:
Radio Astronomy Group View (RAG View)
PURPOSE:
Ragview is the top level menu interface to the data
analysis software package of the Radio and Plasma Astrophysics
Group at ETH in Zurich. It is designed for, but not limited to,
the analysis of solar radio spectrograms.
More information is available at
http://www.astro.phys.ethz.ch/rag/software/ragview-manual.ps
CATEGORY
Radio (/ssw/radio)
CALLING SEQUENCE:
RagView
KEYWORDS:
FILENAME: the name of the file to read in. Allows to avoid the
file menu interface when the filename is known.
CALLS: ***
BREAK_FILE [1], BREAK_FILE [2], BREAK_FILE [3], Custom_2D, DISPLAY_2D
Files_Handling [1], Files_Handling [2], GETHMS, GETWNR, GET_DFONT [1]
GET_DFONT [2], INIT_SELECTION, Image_Info, Init_Display, LOADCT, MDisp, MODIFY, PUTHMS
PUT_SELECTION, RAGVIEW, RESPOND_WIDG, Ragview_MDisp_Int, SEL_DEL, SHOW_IMAGE
Settings, WINDOW_MANAGEMENT, break_file [4], ethz_XCHOICE
COMMON BLOCKS:
ImageReal, image, xAxis, yAxis, fName:
image: contains the 2D image array in byte, int or
real types
x-axis, y-axis: contain 1D arrays determining the
time (x) and frequency (y) values of
the image pixels.
filename: a string with the file name of the current image
Boundaries, xMin, xMax, yMin, yMax: these four
parameters are used to determine which part of the
image is actually displayed.
These common blocks are only used in the top-level user interface..
The procedures called by RagView do not use them. They are
used to access RagView data outside of the RagView program
SIDE EFFECTS:
RagView opens a lot of windows and creates files, dependent
of the user's choices.
RESTRICTIONS:
THIS SOFTWARE WORKS ONLY IN THE SSW ENVIRONMENT.
You must install it using instructions related to the ssw.
See the documntation in http://www.lmsal.com/solarsoft/
RagView requires IDL version 5.1
Works only in interactive mode.
Works only on X-Windows systems
Currently only tested on Unix systems
MODIFICATION HISTORY:
Created: (4/91) (under the name of enrad) A.Csillaghy
Institute for Astronomy, ETH Zurich
Window+Selection Management added in August 1991, Cs.
NOERASE keyword in June, 93
titles kept even outside the session, Nov 93, A.cs
IDL transformations Jan 95 ACs
SSW adaptation, renamed from enrad to ragview,
IDL 5 version March 1998 ACs
IDL 5.1 version in October 1998, csillag@ssl.berkeley.edu
The procedure General_Menu was replaced by XChoice
since WMenu (used in general_menu) crashes on
solaris/idl 5.1
xchoice changed to ethz_xchoice 12/9/98 ACs
Parameters in call to FILE_BREAK adapted to avoid setting
fName to an empty string. Oliver Trachsel,
oliver.trachsel@email.ch, 2002/01/30
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NAME:
Radio Spectrogram FITS File reader
PURPOSE:
Reads (solar) radio spectrograms from FITS files,
including non-regular axes. Tested for ETHZ data as well as
for Potsdam data
CALLING SEQUENCE:
Radio_Spectro_FITS_Read, filename, spectrogram [, time_axis,
frequency_axis ]
INPUT:
filename: string containing the name of the file with extension
OUTPUTS:
image: 2D array containing the spectrogram.
frequency_axis: 1D array containing the frequency axis, in MHz
time_axis: 1D array containing the time in seconds from 1 Jan
1979 (can be converted in any other time formats
with Anytim). Can be set relative with the
RELATIVE_TIME keyword. Uses DATE_OBS to set the
correct time.
KEYWORDS:
AXIS_HEADER: returns a structure containing the axis binary
table header information
MAIN_HEADER: returns a structure containing the main header
information
NO_FSCALE: if set, the primary data are returned in bytes, i.e. the
scaling is not applied (note: the axes are always scaled)
STRUCTURE: if set, the reader returns a spectrogram structure:
{spectrogram: fltarr(nx,ny), x:fltarr(nx), y:fltarr(ny)}
VERBOSE: tells what it's doing while proceeding
MODIFICATION HISTORY
2004-04-15: protection against date_d$end missing from file
2003-10-29: added scaling of the result + no_fscale keyword
2003-04: stuff with loc_file added for idl < 5.6 on 5.6 we
will use file_search acs
2003-02: csillag@ssl.berkeley.edu Now reading the binary table
containing the axes with mrdfits instead of fxbread,
which does work right when the files are compressed
2000-03: Light version for Unix and PC in Jan/March 2000,
csillag@ssl.berkeley.edu
1999-11: Changed name from ragfitsread to radio_spectro_fits_read,
adapted for ssw Nov 1999, csillag@ssl.berkeley.edu
1998-12: Extended to read "transposed" fits data and extensions with
only time or frequency axis; Dec. 98, P.Hackenberg,
AIP Potsdam
1998-12: Adaptation for DATE-OBS keyword with time; Dec. 98, P.Hackenberg
1998-03: Adaptation for IDL5/SSW/Ragview in March 98 -- ACs
1995-11 Read also compressed file in November 95, ACs
1995-08 RELATIVETIME in august 1995, ACs
1993-10 DATAMIN, DATAMAX; When only filename provided, the header
is read but not the array. Oct. 93, A.Cs
1993-06 SILENT in june, 93, A.Cs
1993-05 For IDL Sun in May 1993,
A.Cs. (originally it was a pv-wave program)
1992-10: Created: A. Csillaghy, ETHZ, October 1992
CALLS:
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NAME:
RADIOFLUX
PURPOSE:
Appends the latest complete radio flux file PREVFLUX.NOA to the
long term database file RADIOFLUX.NOA.
CATEGORY:
OVRO APC CALIBRATION
CALLING SEQUENCE:
radioflux
INPUTS:
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
COMMENTS:
CALLS: ***
DAYOFYR [1], dayofyr [2]
SIDE EFFECTS:
The !DEFAULTS.EPHEMDIR+'RADIOFLUX.NOA' file is extended.
RESTRICTIONS:
MODIFICATION HISTORY:
Written 04-Jan-2001 by Dale E. Gary
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NAME:
Radiospectrogram FITS File reader
PURPOSE:
Reads (solar) radio spectrograms from RAG-FITS files,
including non-regular axes. Tested for ETHZ data as well as
for Potsdam data
CALLING SEQUENCE:
Radio_Spectro_FITS_Read, filename, spectrogram [, time_axis,
frequency_axis ]
INPUT:
filename: string containing the name of the file with extension
OUTPUTS:
image: 2D array containing the spectrogram.
frequency_axis: 1D array containing the frequency axis, in MHz
time_axis: 1D array containing the time in seconds from 1 Jan
1979 (can be converted in any other time formats
with Anytim). Can be set relative with the
RELATIVE_TIME keyword. Uses DATE_OBS to set the
correct time.
KEYWORDS:
AXIS_HEADER: returns a structure containing the axis binary
table header information
MAIN_HEADER: returns a structure containing the main header
information
RELATIVE_TIME: If set, the time axis starts with zero instead
of starting with the value of DATE_OBS
STRUCTURE: returns a tplot-like structure with the data
instead of three variables (note: with anytim time values)
VERBOSE: tells what it's doing while proceeding
NO_FSCALE: if set, the primary data are returned in bytes, i.e. the
scaling is not applied (note: the axes are always scaled)
STRUCTURE: if set, the reader returns a spectrogram structure:
{spectrogram: fltarr(nx,ny), x:fltarr(nx), y:fltarr(ny)}
MODIFICATION HISTORY
2003-10-29: added scaling of the result + no_fscale keyword
2003-04: stuff with loc_file added for idl < 5.6 on 5.6 we
will use file_search acs
2003-02: csillag@ssl.berkeley.edu Now reading the binary table
containing the axes with mrdfits instead of fxbread,
which does nork right when the files are compressed
Light version for Unix and PC in Jan/March 2000, csillag@ssl.berkeley.edu
Changed name from ragfitsread to radio_spectro_fits_read,
adapted for ssw Nov 1999, csillag@ssl.berkeley.edu
Extended to read "transposed" fits data and extensions with
only time or frequency axis; Dec. 98, P.Hackenberg,
AIP Potsdam
Adaptation for DATE-OBS keyword with time; Dec. 98, P.Hackenberg
Adaptation for IDL5/SSW/Ragview in March 98 -- ACs
Read also compressed file in November 95, ACs
RELATIVETIME in august 1995, ACs
DATAMIN, DATAMAX; When only filename provided, the header
is read but not the array. Oct. 93, A.Cs
SILENT in june, 93, A.Cs
For IDL Sun in May 1993, A.Cs. (originally it was a pv-wave program)
Created: A. Csillaghy, ETHZ, October 1992
CALLS:
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NAME:
RAG Exponentiation
PURPOSE:
exponentiates the image with parameters asked
interactively. If no values are entered, the defaults
values for SFU decompression are used.
CALLING SEQUENCE:
result = RAGExp( array )
INPUT:
array: any parameter but a string ( normally 2D image )
RESULT:
result = a exp( b * input + c + d )
RESTRICTION
works only after compilation of modify.pro
CALLS:
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NAME:
RAG Log
PURPOSE:
compacts the image with parameters asked
interactively. If no values are entered, the defaults
values for SFU compression are used. Negative values
are replaced by a constant ( 1e-7).
CALLING SEQUENCE:
result = RAGLog( array )
INPUT:
array: any parameter but a string ( normally 2D image )
RESULT:
result = a log( b * input + c + d ) (log basis e)
RESTRICTION:
works only after compilation of modify.pro
CALLS:
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PROJECT:
Phoenix II
NAME:
RAG_ADJCT
PURPOSE:
Interactively adjusts color tables using mouse input.
CATEGORY:
Image display.
CALLING SEQUENCE:
RAG_ADJCT
INPUTS:
No explicit inputs.
OUTPUTS:
No explicit outputs.
CALLS: ***
FINDINDEX, MENUS
CALLED BY:
CT_Handling, Display 2D Image
COMMON BLOCKS:
Colors - color table common block.
SIDE EFFECTS:
Color tables are modified.
RESTRICTIONS:
None.
PROCEDURE:
A new window is created and a graph of the color output value
versus pixel value is created. The user can adjust this function
a number of ways using the mouse.
MODIFICATION HISTORY:
DMS, March, 1988, written.
DMS, April, 1989, modified cursor handling to use less CPU
A.Csillaghy, Inst. of Astronomy, ETH Zurich, August 1991
Modified for IDL5/SSW/Ragview (renamed to rag_adjct)
in March 1998 -- ACs
New position of window, Dec 98 csillag@ssl.berkeley.edu
PSH 2003/02/26: removed call to set_xy.pro, which later made
utplot freak out and the time array to be lost.
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NAME:
Ragview_MDisp_Int
PURPOSE:
Interface used to transfer data from the two dimensional
image analysis software RagView to its one-dimensional
subsystem mdisp. The vectors of the transfered image will be \
stored in a plot table.
CATEGORY:
Data Management
CALLING SEQUENCE:
RagView_MDisp_Int, image [, xAxis, yAxis ]
INPUTS
image: the array to transfer.
xAxis, yAxis: the x and y axes of the image
KEYWORDS:
/YDIR: if present, the image is decomposed in y-plots
if not present x-plots are created.
/RESET: if present, the former plot table will be erased.
TITLE: The name of the plot. Deafult: "!p.title".
CALLS: ***
GETHMS, HMSCONVERT, INSERTPLOT, INSERTSEL, Init_Data, PUTTITLES, error
CALLED BY:
Radio Astronomy Group View RAG View [1]
Radio Astronomy Group View RAG View [2]
MODIFICATION HISTORY:
Created in June 1991 by A.Csillaghy
Few modifications for Ragview/ssw/IDL5 in March 1998, ACs.
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NAME:
ramaty_gysy
PURPOSE:
Derive gyrosyncrotron radiation from power-law electrons.
(c.f. Ramaty 1969, ApJ, 158, 753)
CALLING SEQUENCE:
ramaty_gysy,delta,bb,theta,nv,freq,fi,rc
ramaty_gysy,delta,bb,theta,nv,freq,fi,rc,omega,tau
INPUTS:
delta : power-law index of non-thermal e- distribution
bb : magnetic field strength [G]
theta : angle [degree] between Line-of-sight and magnetic vector
nv : [particles] total number (E>10keV) of non-thermal e-
omega : source size in surface angle [steradian]
OUTPUTS:
freq ; [GHz] frequency
fi ; [SFU] flux density (need 'nv' input)
rc : polarization degree
tau ; optical thickness
OPTIONAL OUTPUTS:
errflag ;
the number of omitted Bessel functions which should
be added to the results. The larger, the greater the error is.
CALLS: ***
RAMATY_GYSY_CORE
HISTORY:
Writtern 2000-05-03 T. Yokoyama
Revised 2000-10-18 T. Yokoyama nv,omega,tau
Revised 2001-08-28 T. Yokoyama
Option 'errflag' is added since new versions of IDL
does NOT support the Bessel function which has
an order higher than 20. Array 'errflag' returns
the number of omitted Bessel functions which should
be added to the results.
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NAME:
RAMATY_GYSY_CORE
PURPOSE:
This procedure calculates Gyrosynchrotoron Microwave Radiation
"Ramaty's code"
CALLING SEQUENCE:
ramaty_gysy_core,ex,anor,bmag,cs,theta,j1,j2,kf $
,ffbd,phi1,phi2,e1d,e2d,a1d,a2d,rccd,rcd $
INPUTS:
ex, anor: electron spectrum N(E) = anor * E^(-ex) (MeV^-1)
bmag: the magnetic field in Gauss assumed uniform
cs: the cosine of the angle between B and the line of sight (0<cs<1)
it appears that the routine works well for 0.1<cs<0.95.
theta: angular size of source in arc sec; source assumed spherical
OUTPUTS:
ffbd: frequency over gyrofrequency
phi1,phi2: ord/xord mode flux densities at Earth in
erg s^-1 Hz^-1 cm^-2 normalized to the total electron number
N(E) = anor E^(-ex) (MeV^-1)
OPTIONAL INPUTS:
j1, j2: determine the range of electron energies
used in the integration
10^(0.1*j1-2) MeV - 10^(0.1*j2-2) MeV.
For example
j1=1 and j2=40 corresponds to 0.01 - 100 MeV
j1=1 and j2=30 corresponds to 0.01 - 10 MeV
kf: determin the highest frequency fmax (in units of gyrofrequency)
if (kf < 100) then fmax = 10^(0.01*kf)
if (kf >= 100) then fmax = 10^(0.1*(kf-91))
For example,
kf=101 corresponds to ffb=10
kf=111 corresponds to ffb=100
kf=121 corresponds to ffb=1000
etr: is an assumed transition energy (in MeV).
Below etr the full gyrosynchrotron formalism is used; above etr
the program uses the ultrarelativistic (Ginzburg and Syrovatskii)
formula; to calculate the total emissions it is sufficient
to take etr about 3 MeV, except for cs close to 1 when etr should
be larger
alpha: Razin parameter
= 1.5 * (gyro frequency)/(plasma frequency)
OPTIONAL OUTPUTS:
e1d, e2d ord/xord mode emissivities in erg s^-1 sr^-1 Hz^-1 cm^-3
a1d, a2d:ord/xord mode absorption coefficients in cm^-1
both the emissivities and absorption coefficients are
normalized to an electron number density, E^(-ex) (MeV^-1 cm^-3).
rccd : degrees of polarization calculated from the emissivities
rcd: degrees of polarization calculated from the flux densities
CALLS: ***
BESPR, GSY, REFR, SEAR, SSY
CALLED BY:
ramaty_gysy
HISTORY:
Written 199? by Ramaty as a Fortran Code
Ported 1998-09-04 TY
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NAME:
RANGE_DETECTOR
PURPOSE:
Routine meant to automatically inspect spectrum data and divide
the frequency range in subranges obeying the same trend.
The algorithm computes an intrinsic fluctuation level and cut the data range in
subranges in wich data points change below the fluctuation level
CATEGORY:
OVSA APC CALIBRATION ANALYSIS
CALLING SEQUENCE:
range_detector,freq,flux [,lf=lf,uf=uf,pf=pf,pd=pd,$
width=width,range=range,i_lf=i_lf,i_max=i_max,i_uf=i_uf,nosmooth=nosmooth,$
goright=goright,goleft=goleft,first=first]
INPUTS:freq, flux
OUTPUTS: lf:low frequency array
uf:high frequency array
pf:peak frequency array
pd: peak flux array
each index correspond to a data subrange
OPTIONAL (KEYWORD) INPUT PARAMETERS:
width: minimum number of points in a data subrange
the rest of the parameters are meant to be used internally
ROUTINES CALLED:
OUTPUTS:
COMMENTS:
CALLED BY:
TP_FIT
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 14-Aug-2002 by Gelu M. Nita (gn2@njit.edu)
04-Jun-2006 DG
IUF was always one less than maximum range due to FOR loop
only going to IEND-1. Changed to go to IEND.
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NAME:
rapp_get_spectrogram.pro
PROJECT:
ETHZ Radio Astronomy
CATEGORY:
Utility
PURPOSE:
This routine, given a time interval (anytim format) and a frequency interval (optional),
returns the associated Phoenix data array, or a string if a problem occured (such as
no data available). The intensity data is returned as SFU values, unless
the /POL keyword is used, in which case the values are in % polarization
(negative=left).
CALLING SEQUENCE:
rapp_get_spectrogram,time_interval,freq_interval,ELIM=ELIM,BACK=BACK,POL=POL, $
xaxis=xaxis,yaxis=yaxis,avgback=avgback
INPUT:
time_interval : a 2-element array,in a format accepted by ANYTIM
OPTIONAL INPUT:
freq_interval : a 2-element int array (MHz). If not specified, the whole
frequency range is returned.
KEYWORD INPUT:
/NODECOMPRESS: if set, will NOT linearize the data. Normally, no point in using that keyword simultaneously with /LOG...
Also, when this keyword is used, the data type ("bunit") is not checked.
/LOG : if set, will output 45*alog( (data > (-9.)) +10.) . Normally, no point in using that keyword simultaneously with /NODECOMPRESS...
/ELIM: if set, will automatically remove bad channels
/POL : if set, will look for polarization data instead of intensity/L1/L2
/DESPIKE : if set, will use tracedespike.pro (from the TRACE part of the SSW) on the spectrogram. CAUTION: radio 'spikes' would surely be removed...
/FAST: if set, will not check each file for time interval (and assumes they are all 15 min. long -- works 99% of the time...)
BACK: if set, will automatically remove background
if set to 1 (/BACK): will take the least 3% of the data as background
if set to a single number (ex: 0.05): is the least fraction of the data to be considered as background (/BACK or BACK=0.03 does the same)
if set to a 2-element array, assumes those are ANYTIM time intervals to be taken as background
/ANYTIME: if set, xaxis will return times in anytim format, instead of seconds since midnight...
REMOVED!!!: /CALLISTO: if set, will look for data in /ftp/pub/rag/callisto/observations/
valid_file_identifiers:
archivedir: ex: /ftp/pub/rag/callisto/observations/
OUTPUT:
a Phoenix-2 spectrogram image, in LINEAR SFU scale (for intensities) or % circular polarization (negative = left)
KEYWORD OUTPUT:
xaxis : returns the xaxis, as per RagFitsRead.pro
yaxis : returns the yaxis, as per RagFitsRead.pro
avgback: array of averaged background values for each frequencies. Useful only if the BACK keyword has also been used!
CALLS
has_overlap.pro
int2str.pro
eventually (keyword /DESPIKE): phoenix_despike.pro
CALLS: ***
AVG [1], AVG [2], Congrid1d, DATATYPE [1], DATATYPE [2], DATATYPE [3]
ELIMWRONGCHANNELS, EXIST, RAGFITSREAD, RAPP_ELIMWRONG, RAPP_GET_FILE_LIST
RAPP_MERGE, RAPP_RETURN_FILE_INTERVAL, anytim [1], anytim [2], anytim [3]
anytim [4], anytim [5], constbacksub_v21, get_logenv [1], get_logenv [2]
has_overlap [1], has_overlap [2], int2str, phoenix_despike
CALLED BY:
Automatic polarization determination with background subtraction
RESTRICTIONS:
For now, only works inside ETH (because of file locations)
EXAMPLES:
time_intv='2001/09/01 '+['11:50:00','11:55:00']
data=rapp_get_spectrogram(time_intv,xaxis=xaxis,yaxis=yaxis,/ELIM,/BACK)
data=rapp_get_spectrogram(time_intv,xaxis=xaxis,yaxis=yaxis,/ELIM,BACK=0.05)
data=rapp_get_spectrogram(time_intv,xaxis=xaxis,yaxis=yaxis,/ELIM,BACK='2001/09/01 '+['11:45:00','11:46:00'])
time_intv='2001/09/20 '+['11:35:00','11:36:00']
data=rapp_get_spectrogram(time_intv,xaxis=xaxis,yaxis=yaxis,/POL)
HISTORY:
Pascal Saint-Hilaire, 2001/11/16 created
shilaire@astro.phys.ethz.ch
PSH 2002/01/21: corrected a bug where a break error occured if no data files were found.
Now, simply returns -1 if a problem occured
PSH 2002/01/28: returns a STRING if something went wrong, instead of -1. This string
usually contains an error message.
PSH 2002/01/28: major changes, renamed from rapp_get_array to rapp_get_spectrogram
and included most of the called subroutines (some of them heavily inspired by
previous work from A. Csillaghy and/or P. Messmer)
PSH 2002/05/03: Phoenix file duration is no longer always assumed to be 15 min...
PSH 2002/05/04: Added /DESPIKE keyword
Added /LOG keyword
PSH 2002/05/29: modified background subtraction (accepts a number, or an anytim time array)
PSH 2002/07/23: added an environmental variable: RAG_ARCHIVE
PSH 2002/07/24: replaced .gz by * for valid_file_identifiers (as some of the files aren't gzipped, for some reason...)
PSH 2002/08/05: added the /FAST keyword
PSH 2002/09/05: added the avgback keyword output
PSH 2002/10/09: corrected a bug where a freq_intv bigger than physical limits would crash the routine.
PSH 2002/11/18: corrected a bug where a low limit for the freq interval did not function properly.
PSH 2003/10/06: added keyword /ANYTIME
PSH 2004/04/26: added keyword /CALLISTO
PSH 2004/05/13: -further mods, so that the use of the keyword /CALLISTO also works for background-subtraction.
-added KEYWORD /NODECOMPRESS
PSH 2004/09/17: added keyword 'valid_file_identifiers' and 'archivedir', for greater flexibility.
Removed keyword /CALLISTO.
Uses phoenix_despike instead of tracedespike
PSH 2006/08/10: added recognition of the "quasi % " format.
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NAME:
RD_FICPOINT
PURPOSE:
Cette procedure lit le contenu d'un fichier de points de mesure
CATEGORY:
Fichier de points.
CALLING SEQUENCE:
RD_FICPOINT, FILE, TAB
INPUTS:
FILE Nom du fichier contenant les poins de mesure
KEYWORD PARAMETERS:
Non
OUTPUTS:
TAB Tableau de chaine resultant de la lecture du fichier
CALLS: ***
DCD_FICPOINT, SEL_FICPOINT, SEL_FICPOINT_EVENT, XMANAGER
CALLED BY:
DCD_FICPOINT, SEL_FICPOINT, SUN_IMAGE
COMMON BLOCKS:
Non
PROCEDURE:
Cette procedure transfere le contenu du fichier dans un tableau
de chaines
EXAMPLE:
Please provide a simple example here
MODIFICATION HISTORY:
Ecrit par: J Bonmartin ( obspm.fr) le 04/09/98
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NAME:
RD_NRH2I
PURPOSE:
Lecture d'une image dans un fichier NRH2, l'image est selectionnee
par l'heure
CATEGORY:
Fichiers
CALLING SEQUENCE:
RD_NRH2I, FILE, HEURE, STRINF, DATA, STR
INPUTS:
FILE nom du fichier
HEURE Chaine ASCII: hh:mn:ss:xxx, l'heure est prise en compte si
le keyword INDIC n'est pas present
STRINF Structure resultant de NRH_FOPEN
KEYWORD PARAMETERS:
STOKES Image STOKESV si = 1, STOKESI si = 0 ou abscent
INDIC Indice de l'image dans le fichier
OUTPUTS:
DATA Tableau d'image
STR Structure decrivant l'image (NRH_STR_IMAGE)
CALLS: ***
FXBCOLNUM [1], FXBCOLNUM [2], FXBREAD [1], FXBREAD [2], FXBREAD [3], MSH
TIME_IND_NRH
CALLED BY:
CPT_FLUX_NRH2, NRH2_PROJECT2D, READ_NRHIM
EXAMPLE:
Please provide a simple example here
MODIFICATION HISTORY:
Ecrit par: J Bonmartin (obspm.fr) le 29/05/98
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NAME:
RD_NRHGIF
PURPOSE:
Lecture des donnees SOHO EIT au format FITS
CATEGORY:
Input, Output
CALLING SEQUENCE:
RD_NRHGIF, File, Str_fic, Image, Str_im
INPUTS:
File chemin et nom du fichier a lire
Str_fic Structure d'information de fichiers (NRH_STR_INFIC)
KEYWORD PARAMETERS:
OUTPUTS:
Image tableau d'image
Str_im Structure d'image (NRH_STR_IMAGE)
CALLED BY:
READ_NRHIM
PROCEDURE:
Cette procedure lit l'image contenue dans un fichier GIF,
cree et remplit la structure STR_IM
La structure STR_FIC doit avoit ete correctement remplie par un appel
a FOPEN_GIF
CALLS: ***
READ_GIF
EXAMPLE:
MODIFICATION HISTORY:
Ecrit par: J Bonmartin (obspm.fr)le 09/09/98
Chargement des tables de couleurs GIF (JB Le 15/05/00)
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NAME:
RD_NRHPNG
PURPOSE:
Lecture des donnees SOHO EIT au format FITS
CATEGORY:
Input, Output
CALLING SEQUENCE:
RD_NRHPNG, File, Str_fic, Image, Str_im
INPUTS:
File chemin et nom du fichier a lire
Str_fic Structure d'information de fichiers (NRH_STR_INFIC)
KEYWORD PARAMETERS:
OUTPUTS:
Image tableau d'image
Str_im Structure d'image (NRH_STR_IMAGE)
CALLED BY:
READ_NRHIM
PROCEDURE:
Cette procedure lit l'image contenue dans un fichier PNG,
cree et remplit la structure STR_IM
La structure STR_FIC doit avoit ete correctement remplie par un appel
a FOPEN_PNG
CALLS: ***
LOADCT, READ_PNG
EXAMPLE:
MODIFICATION HISTORY:
Ecrit par: J Bonmartin (obspm.fr)le 09/09/98
Chargement des tables de couleurs PNG (JB Le 15/05/00)
24/03/2005 : traitement des images .png en 24 bits
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NAME:
RD_STDFITS
PURPOSE:
Lecture d'image au format FITS dans unfichier contenant une image
CATEGORY:
Fichiers NRH
CALLING SEQUENCE:
RD_STDFITS, File, Str_fic, Image, Str_im
INPUTS:
File chemin et nom du fichier a lire
Str_fic Structure d'information de fichiers (NRH_STR_INFIC)
KEYWORD PARAMETERS:
OUTPUTS:
Image tableau d'image
Str_im Structure d'image (NRH_STR_IMAGE)
CALLED BY:
READ_NRHIM
PROCEDURE:
Cette procedure lit l'image contenue dans un fichier FITS ,
cree et remplit la structure STR_IM
La structure STR_FIC doit avoit ete correctement remplie par un appel
a NRH_FOPEN correspondant a l'instrument choisi
CALLS: ***
MRDFITS [1], MRDFITS [2]
EXAMPLE:
MODIFICATION HISTORY:
Ecrit par: J Bonmartin le 14/09/98 (bonmartin@obspm.fr)
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NAME:
RDFILEPOS
PURPOSE:
lit une colonne d'un fichier de positions
RH_2D
CATEGORY:
RH_2D, recherche de positions
CALLING SEQUENCE:
Tab = RDFILEPOS(Fich, Col, Exte)
INPUTS:
Fich: Nom du fichier rh2d de positions
Col: Colonne a lire (numero ou intule)
Exte: Numero de l'extension
OUTPUTS:
Tab: Colonne lue
CALLS: ***
FXBCLOSE [1], FXBCLOSE [2], FXBOPEN [1], FXBOPEN [2], FXBOPEN [3], FXBREAD [1]
FXBREAD [2], FXBREAD [3]
CALLED BY:
MKFILEPOS, MK_RESUME, PLOT_MAXPOS, PLOT_SOURCES, RDLINE_FPOS, READ_NRHPOS
EXAMPLE:
time = RDFILEPOS('position.fts', 'TIME', 1)
MODIFICATION HISTORY:
Written by: C. Renié, 09/1998
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NAME:
RDLINE_FPOS
PURPOSE:
Cette procedure lit une source d'une position et la renvoie sous forme
d'une structure de type GAUSS (max, xamx, ymax, gra, grb, tet)
CATEGORY:
RH_2D, recherche de positions
CALLING SEQUENCE:
RDLINE_FPOS, Fichpos, NumPos, NumLigne, Gauss
INPUTS:
Fichpos: Fichier fits contenant les positions
NumPos: Numero de la position
NumLigne: Numero de la ligne
OUTPUTS:
Gauss: structure de type gauss
CALLS: ***
RDFILEPOS
CALLED BY:
PLOT_MAXPOS
MODIFICATION HISTORY:
Ecrit par: C Renie aout 1998
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NAME:
Read Data Byte
PURPOSE:
Reads a data byte in VMS format
CALLING SEQUENCE:
Read_Data_Byte, unit, data
INPUT PARAMETERS:
unit: The logical number of the opened file
OUTPUT PARAMETERS:
data: the byte array read.
CALLS:
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NAME:
Read VMS Record
PURPOSE:
Reads a VMS-format variable-length
record on the Unix system.
CALLING SEQUENCE:
ReadVMSRec, unit, record
INPUT PARAMETERS:
unit: The logical unit number of the (already opened)
VMS-format file
OUTPUT PARAMETERS:
record: The record read, an array of bytes.
RESTRICTIONS
This procedure cannot be used for Unix files.
CALLS: ***
ODD, READVMSREC
MODIFICATION HISTORY:
Created by A.Csillaghy in September 1991
Inst. of Astronomy, ETH Zurich
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NAME:
READ_ARRAY
PURPOSE:
Reads a file into an array variable. The file is assumed to
consist of lines of numbers, separated by tabs or spaces,
with the same number of values on each line. The file length
is arbitrary.
CATEGORY:
PROG
CALLING SEQUENCE:
READ_ARRAY, filename, array
INPUTS:
filename: The name of the file to be read.
array: The variable to hold the data.
KEYWORD PARAMETERS:
SKIP: The number of lines of "header" information in the
file to skip.
INTEGER: If the data in the file is integer. The default is
floating point.
ROWS: Returns the number of rows
COLUMNS: Returns the number of columns
SILENT: If set, do not output to the screen
OUTPUTS:
Returns a two-dimensional array whose first index is the
number of elements per line, and second index is the number of
lines in the file. Also outputs these numbers to the screen.
CALLED BY:
MDisp Read
RESTRICTIONS:
Not tested all that much. Does not read double precision data.
EXAMPLE:
READ_ARRAY, 'spectra.dat', spectrum, SKIP=3, /SILENT
Reads the file spectra.dat, skipping the first 3 lines, creating
the array variable spectrum. Don't print out anything.
MODIFICATION HISTORY:
Written by: Randall Smith, 6/19/95
Modified : RKS, 11/2/95
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NAME:
READ_CENTER_POINT
PURPOSE:
Cette procedure lit les valeurs associee a une source d'un fichier
de CENTRES ACTIFS (Sources)
CATEGORY:
Cfile
CALLING SEQUENCE:
NRH_READ_CENTER, File, Extd, Str
INPUTS:
FILE Nom du fichier
EXTD Numero de l'extension dans le fichier CENTRES
KEYWORD PARAMETERS:
HBEG Heure de debut selectionnee (HH:MN:SS:MMM)
HEND Heure de fin selectionnee
OUTPUTS:
STR structure contenant les valeurs associee a la source
Cette structure est cree dans la procedure
STR.Time Heure
STR.Flux Flux
STR.EWPOS Position est-ouest
STR.NSPOS Position nord_sud
CALLS: ***
FXBCLOSE [1], FXBCLOSE [2], FXBOPEN [1], FXBOPEN [2], FXBOPEN [3], FXBREAD [1]
FXBREAD [2], FXBREAD [3], FXPAR [1], FXPAR [2], HMS, IND_RS, NRH_READ_CENTER, TIME_IND
CALLED BY:
SUN_IMAGE
COMMON BLOCKS:
Non
RESTRICTIONS:
Seuls les fichiers CENTRE ACTIF calcules dans NRH peuvent etre traites
PROCEDURE:
Le numero de l'extension du fichier FITS peut etre determinee en
appelant CW_XTD_NRHF
EXAMPLE:
Please provide a simple example here
MODIFICATION HISTORY:
Ecrit par:J Bonmartin (bonmartin@obspm.fr) le 12/10/98
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NAME:
READ_CENTER_POINT
PURPOSE:
Cette procedure lit les valeurs associee a un point d'un fichier
de CENTRES ACTIFS
CATEGORY:
Cfile
CALLING SEQUENCE:
READ_CENTER_POINT, File, Extd, Heure, Str
INPUTS:
FILE Nom du fichier
EXTD Numero de l'extension dans le fichier CENTRES
HEURE Heure selectionnee (HH:MN:SS:MMM)
KEYWORD PARAMETERS:
Non
OUTPUTS:
STR structure contenant les valeurs associee au point
type (NRH_STR_COORD)
Cette structure est cree dans laprocedure
CALLS: ***
FXBCLOSE [1], FXBCLOSE [2], FXBOPEN [1], FXBOPEN [2], FXBOPEN [3], FXBREAD [1]
FXBREAD [2], FXBREAD [3], FXPAR [1], FXPAR [2], HMS, IND_RS, MSH, TIME_IND
CALLED BY:
SUN_IMAGE
COMMON BLOCKS:
Non
RESTRICTIONS:
Seuls les fichiers CENTRE ACTIF calcules dans NRH peuvent etre traites
PROCEDURE:
Le numero de l'extension du fichier FITS peut etre determinee en
appelant CW_XTD_NRHF
EXAMPLE:
Please provide a simple example here
MODIFICATION HISTORY:
Ecrit par:J Bonmartin (bonmartin@obspm.fr) le 12/10/98
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NAME:
Read_DriftData
PURPOSE:
CATEGORY:
CALLING SEQUENCE:
INPUTS:
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
openarc,newscan,getcycle,gaincor
OUTPUTS:
COMMENTS:
CALLS: ***
FREESCAN, GAINCOR, GET_CYCLE, JULDAY, MSEC2STR, NEWSCAN, OPENARC, OVSA_LST
CALLED BY:
READ_DRIFTSCAN
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
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NAME:
READ_DRIFTSCAN
PURPOSE:
Reads DRIFTSCAN observation data, for the two 27 m antennas, to
determine relative pointing shifts.
CATEGORY:
OVRO APC DATA CALIBRATION
CALLING SEQUENCE:
read_driftscan
INPUTS:
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
COMMENTS:
Use PLOT_DRIFTSCAN to read from the save file, DRIFTSCAN.SAV
and plot the results.
CALLS: ***
OPENARC, OVSA_GET_INDEX, Read_DriftData
SIDE EFFECTS:
A SAVE file is created for plotting with PLOT_DRIFTSCAN
RESTRICTIONS:
MODIFICATION HISTORY:
Written 08-Apr-2002 by Dale E. Gary
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NAME:
READ_FCHIST
PURPOSE:
Reads history files of frequency calibration parameters
determined during analysis of FCAL segments
CATEGORY:
OVRO APC ANALYSIS FCAL
CALLING SEQUENCE:
result = read_fchist(ant,timstr,fc,tc,tim)
INPUTS:
ant the antenna number, e.g. 1,2,4, etc., for which info
is desired
timstr the TIMSTR structure element from the current TLS
structure, for which to find the closest entry in time
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
result gives an indication of the success of the attempt to
write the updates to the file. If -1, the attempt
failed, 0 otherwise.
fc the table of frequencies, of size FC(9), three for each
oscillator.
tc the corresponding table of tuning currents.
tim the day and time of the actual entry selected, as DDDHHMM.
COMMENTS:
CALLS: ***
CVDOY
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 28-Nov-2000 by Dale E. Gary
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NAME:
READ_FLUX
PURPOSE:
Cette procedure traite les fichiers de FLUX ou assimiles du NRH
Elle permet de selecter un fichier de flux et dans le fichier
une ligne de FLUX.
CATEGORY:
Fichiers NRH
CALLING SEQUENCE:
READ_FLUX, Flux, Time, [Header]
INPUTS:
Non
KEYWORD PARAMETERS:
Non
OUTPUTS:
FLUX Tableau du flux lu
TIME Tableau de temps correspondant en ms
OPTIONAL OUTPUTS:
HEADER Header correspondant au flux lu
COMMON BLOCKS;
Non
PROCEDURE:
Cette procedure utilise DIALOG_PICKFILE pour selectionner le fichier
et CW_XTD_NRH pour selectionner la ligne
CALLS: ***
CW_XTD_NRHF, MRDFITS [1], MRDFITS [2]
EXAMPLE:
READ_FLUX, Flux,Time
MODIFICATION HISTORY:
Ecrit par: J Bonmartin (obspm.fr) le 11/09/98
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NAME:
READ_MAP_GIF
PURPOSE:
This procedure read a gif file to plot the image with the MAPPING
software (D Zarro)
It is necessary to be able to define the optical sun by 3 points
or by the center coodinates and the radius in pixels
CATEGORY:
NRH2D gen
CALLING SEQUENCE:
READ_MAP_GIF, File, Index, Data, [R], [G], [B]
INPUTS:
FILE GIF file
KEYWORD PARAMETERS:
DIR GIF file Directory (default current directory)
OUTPUTS:
INDEX Index to map
DATA Data to map
R,B,B Color table
CALLS: ***
OPTIC_CIRC, READ_GIF
COMMON BLOCKS:
No
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
The procedure generate a widget window to define the optical sun
EXAMPLE:
READ_MAP_GIF, 'image.gif', Index, Data, r, g, b
INDEX2MAP, Index, Data, Image
TVLCT,r,g,b
TVLCT,r,g,b,/get
nc = N_ELEMENTS(r)
PLOT_MAP, Image, NCOLORS=Nc
MODIFICATION HISTORY:
Ecrit par: Jen Bonmartin (jean;bonmartin@obspm.fr) le 25/04/01
18/05/01 Add colors table (JB)
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NAME:
READ_MAP_PNG
PURPOSE:
This procedure read a gif file to plot the image with the MAPPING
software (D Zarro)
It is necessary to be able to define the optical sun by 3 points
or by the center coodinates and the radius in pixels
CATEGORY:
NRH2D gen
CALLING SEQUENCE:
READ_MAP_PNG, File, Index, Data, [R], [G], [B]
INPUTS:
FILE PNG file
KEYWORD PARAMETERS:
DIR PNG file Directory (default current directory)
OUTPUTS:
INDEX Index to map
DATA Data to map
R,B,B Color table
CALLS: ***
OPTIC_CIRC, READ_PNG
COMMON BLOCKS:
No
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
The procedure generate a widget window to define the optical sun
EXAMPLE:
READ_MAP_PNG, 'image.png', Index, Data, r, g, b
INDEX2MAP, Index, Data, Image
TVLCT,r,g,b
TVLCT,r,g,b,/get
nc = N_ELEMENTS(r)
PLOT_MAP, Image, NCOLORS=Nc
MODIFICATION HISTORY:
Ecrit par: Jen Bonmartin (jean;bonmartin@obspm.fr) le 25/04/01
18/05/01 Add colors table (JB)
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NAME:
READ_MONITOR_SEG
PURPOSE:
Reads frequency calibration parameters from a monitor segment
CATEGORY:
OVRO APC ANALYSIS FCAL
CALLING SEQUENCE:
result = read_monitor_seg(srec,ant,tc_coef,time)
INPUTS:
srec the record number of the segment to read
ant the antenna index, e.g. 0,1,2, etc., for which info
is desired
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
result gives an indication of the success of the attempt to
write the updates to the file. If -1, the attempt
failed, 0 otherwise.
tc_coef the table (5,3) of tuning current coefficients for the 3 osc.
time the day and time of the actual entry selected, as DDDHHMM.
COMMENTS:
CALLS: ***
TL_DECODE, W2L
CALLED BY:
WFSURVEY
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 15-Feb-2002 by Dale E. Gary
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NAME:
READ_NRH
PURPOSE:
This procedure read 2 dimensions images array from
NRH files, (result of VISIBILITY to IMAGE conversion NRH widget)
or
VISIBILITY files from BASS2000 data base (http://mesola.obspm.fr )
and interface it with the D Zarro MAPPING SOFTWARE
CATEGORY:
NRH Gen
CALLING SEQUENCE:
READ_NRH, File, Index, Data
INPUTS:
FILE NRH file name (NRH file or VISIBILITY file
KEYWORD PARAMETERS:
HBEG Time (hh:mm:ss:cc) of the first image to read,
Default: begin of the file
HEND Time of the last image to read
Default same value than HBEG
STOKES Stokes V parameter instead of I parameter
FREQ Frequency number for VISIBILITY files [0 to 4]
DIR Directory from where to read data
OUTPUTS:
INDEX Structure to map
DATA Data array
CALLS: ***
ADD_TAG [1], ADD_TAG [2], FXPAR [1], FXPAR [2], MRDFITS [1], MRDFITS [2], MSH
NRH_CTRLREP, NRH_PIXARCSEC, RH_RDIMCUBE, TIME_IND_NRH, fits_interp
COMMON BLOCKS:
No
EXAMPLE:
READ_NRH, File name, Index, Data
Read the first imade of the file
Idex2map, Index, Data, Map
Map the image
READ_NRH, File name, Index, Data, HBEG='10:00', HEND='10:10:30'
Read images cube
MODIFICATION HISTORY:
Ecrit par: Jean Bonmartin (bonmartin@obspm.fr) 14/09/00
-ISHORT dans l'appel a FITS_INTERP pour avoir NAXISn en INT
plutot qu'en BYTE le 18/12/00 (JB)
le 04/04/01 Adapte pour les visibilites (JB)
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NAME:
READ_NRHIM
PURPOSE:
Cette procedure lit une image dans un fichier FITS
CATEGORY:
Fichier
CALLING SEQUENCE:
READ_NRHIM, File, Heure, Str_inf, Donnee, Str_im
INPUTS:
FILE Nom du fichier
HEURE Chaine contenant l'heure (hh:mn:ss:ccc), l'heure est prise
en compte si le keyword INDIC n'est pas present et si le
fichier contient plusieurs images
STR_INF Structure d'information du fichier resultant NRH_FOPEN
KEYWORD PARAMETERS:
STOKES Parametre de Stokes pour NRH: STOKESV si =1, sinon
STOKESI
INDIC Indice de l'image dans le fichier
OUTPUTS:
DATA Tableau contenant l'image
STR_IM Structure d'information liee a l'image (NRH_STR_IMAGE)
CALLS: ***
RD_NRH2I, RD_NRHGIF, RD_NRHPNG, RD_STDFITS
CALLED BY:
CW_POS, CW_SCANSOURCE, FLUX_NRH2, GR_IMAGES, NRH2_PROJECTION, NRH_ANIM, NRH_VISU_2D
PLOT_MAXPOS, SUN_IMAGE
COMMON BLOCKS:
Non.
PROCEDURE:
Cette procedure utile STR_INF.INSTRUME pour selectionner
la procedure de lecture associee a l'instrument
Instuments reconnus:
NRH
EIT SOHO
YOHKOH
PNG
EXAMPLE:
Please provide a simple example here
MODIFICATION HISTORY:
Ecrit par:J Bonmartin (obspm.fr) le 24/08/98
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NAME:
READ_NRHPOS
PURPOSE:
Cette procedure lit une position dans un fichier de positions NRH
CATEGORY:
RH_2D, recherche de positions
CALLING SEQUENCE:
READ_NRHPOS, Fichpos, NumPos, Strpos, Hext
INPUTS:
Fichpos: Fichier fits contenant les positions
NumPos: Numero de la position
OUTPUTS:
Strpos: structure de 8 tableaux
Hext: header de l'extension
CALLS: ***
FXPAR [1], FXPAR [2], HEADFITS [1], HEADFITS [2], HEADFITS [3], RDFILEPOS
CALLED BY:
CENTER_NRH2
MODIFICATION HISTORY:
Ecrit par: C Renie octobre 1998
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Project : ovsa
Name : read_ovsa_fits
Purpose : read an ovsa quicklook data file and write header and
data to a structure.
Category : OVSA quicklook analysis
Explanation :
Syntax : read_ovsa_fits, filename, data
CALLS: ***
FXBCLOSE [1], FXBCLOSE [2], FXBOPEN [1], FXBOPEN [2], FXBOPEN [3], FXBREAD [1]
FXBREAD [2], FXBREAD [3], HEADFITS [1], HEADFITS [2], HEADFITS [3]
CALLED BY:
MAKE_TPOVIEW, OVSA__DEFINE
Examples :
Inputs : filename = ovsa ql fits file
Outputs : data = Structure containing the data and header
Keywords : None
History : Written 09 December 1999, P. T. Gallagher, NJIT
Contact : ptg@penumbra.njit.edu
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NAME:
READ_RSTN_FLUX
PURPOSE:
Reads the daily NOAA solar flux values (primarily from RSTN and
Penticton), for comparison with the daily CTRCAL calibration.
CATEGORY:
OVRO APC CALIBRATION
CALLING SEQUENCE:
read_rstn_flux,f,s,tls
INPUTS:
tls the TIME/LABEL structure of the CTRCAL scan header
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
f the frequencies [GHz] for which fluxes are available in the
daily NOAA file. A value of -1 is returned if the
routine fails.
S the corresponding fluxes, in SFU. These are a simple
average of the data in the file. A value of -1 is
returned if the routine fails.
COMMENTS:
CALLS: ***
DAYOFYR [1], dayofyr [2]
CALLED BY:
WTPCAL
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 11-Nov-2000 by Dale E. Gary
04-Jan-2001 DG
Fixed to work with new RADIOFLUX archive file. This routine
is actually useful now, since it works for older data as well
as current data.
15-May-2002 GN
added keyword auto to generate an error message ctrlcalcheck is
called with this keyword set
09-Mar-2004 DG
Error messages were printed as READ_DAILY_FLUX, now changed to
the correct READ_RSTN_FLUX.
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NAME:
READ_SRBL
PURPOSE:
Read a SRBL lightcurve file and return the frequency, time, and
dynamic spectrum data for a given time range
CATEGORY:
OVRO APC DATA CALIBRATION
CALLING SEQUENCE:
read_srbl,filename,tstart,tend,freq,time,data
INPUTS:
filename the name of the SRBL plot file
tstart the start time of the desired data, in seconds since 0 UT
tend the end time of the desired data, in seconds since 0 UT
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
freq an array of frequencies, in GHz, of size NF
time an array of times, in seconds, of size NTIMES
data the array of data, of size (NF,NTIMES), in SFU. Note that
the OVRO SRBL takes only RCP data.
COMMENTS:
CALLED BY:
SRBL_2M_CAL
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 22-Aug-1999 by Dale Gary
07-Nov-2000 DG
Added FILENAME argument to make routine more general.
29-Apr-2001 DG
Added code to allow reading of original (BST) and new versions (PTLF)
of SRBL data.
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NAME:
Read_Test
PURPOSE:
Reads a value on the terminal and sets a default
if the return key has been pressed directly.
CATEGORY:
I/O
CALLING SEQUENCE:
Read_Test, text, default, value
INPUTS:
text: a message to print before the reading action
default: the value to set to the variable if it has not
been entered
OUTPUT:
value: the variable where the number read is stored.
KEYWORDS:
MINIMUM: the minimum set if the number is too low
MAXIMUM: the maximum set if the number is too high
HMS: The in/output format is of type hh:mm:ss.sss
RESTRICTION:
The type of the variable is REAL
CALLS: ***
HMSCONVERT, decconvert
CALLED BY:
ASCII_Read, Change_Selection, Columns_Read, Cont_Surf, Customize_1D
Determine Drift Rate, ETHZ_Background, Fitting, Histogram Facility
Initialize Selection [2], Integrate_2D, Integration, Modif_Axis
Modification of 1D Plots, Modify Image Pixels, Modify Titles, Overplot Texts
RAG Exponentiation, RAG Log, Selection delete, Texts_2D, Tv_Zoom, Zoom_1D, edit [1]
edit [2], put selection
MODIFICATION HISTORY:
Creadted by A.Csillaghy in June 1991
Max and min added in November 91
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NAME:
READ_TPFAC
PURPOSE:
Reads a total power calibration file (requests selection by the user)
and returns the total power factors (units/SFU) corresponding to the
frequencies specified on input.
CATEGORY:
OVRO APC DATA CALIBRATION
CALLING SEQUENCE:
tpfac = read_tpfac(frqlist)
INPUTS:
frqlist an array of frequencies [GHz] for which to return the
factors
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
tpfac an array of size FLTARR(4,n_elements(frqlist)) containing
the factors, one each for the four 27-m feeds. The
order of feeds is I1, L1, R2, I2
COMMENTS:
CALLS: ***
PICKFILE
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 07-Feb-1999 by Dale E. Gary
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NAME:
Read_Values
PURPOSE:
Reads interactively a point on the screen
CATEGORY:
User Interface
CALLING SEQUENCE:
Read_Values [,x, y]
OUTPUTS:
x,y: scalars, contains the x- and y-coordinate in data
units where the user clicked.
KEYWORD:
/NODISPLAY: if present, the result is not shown on
the screen, but stored in the x,y variables.
SIDE EFFECT:
On X terminals, uses windows.
CALLS: ***
CURSORVT, GETHMS, HMSCONVERT, PTO, WMESG
CALLED BY:
Display_1D
MODIFICATION HISTORY:
Created in June 1991 by A.Csillaghy
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Modification History
11-Jan-2003 DG
Slight change to read non-zero phi_ab from 12rli files.
CALLED BY
APCAL_ADD_27MANT [1], APCAL_ADD_2MANT, APCAL_ADD_2M_RL, CHECK_12AP, FLUX_3C84
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NAME:
REFINE_OFF
PURPOSE:
Routine containing much of the code of GCFIT, to refine the
channel offset values for a given model of nonlinearity.
CATEGORY:
OVRO APC DATA ANALYSIS
CALLING SEQUENCE:
newoff = refine_off(gcdata,gcflag,nlparm,oldoff)
INPUTS:
gcdata the GCAL data array, of size (2,7,5,86), where
the first index is ND off/on, second index is the
attenuation state (0,5,10,15,20,35,20*DB), the
third index is the total power channel, and the
last index is the frequency
gcflag a corresponding array containing 0 where the data are
bad and 1 where the data are good.
nlparm a 5-element array of nonlinearity parameters, one for
each data channel.
oldoff a 5-element array of offsets, one for each channel
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
OUTPUTS:
gcparm a 5-element array of revised offsets
COMMENTS:
CALLS: ***
FLAGPAIR
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 23-Jan-1998 by Dale E. Gary
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Just a quick (1-time) program to reformat the RSTN and Penticton fluxes
from the format they have on the NGDC on-line archive to the format used
by the daily announcements of fluxes. This goes from 01/01/1999 to
11/30/2000. The daily flux files will handle newer data. This routine
should be kept around, since we may want to go back further into the past
at some point.
MODIFICATION HISTORY
Written 04-Jan-2001 by Dale E. Gary
CALLS:
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NAME:
REGION_EVENT
PURPOSE:
Gestion des evenements de CW_REGION
CATEGORY:
WIDGET
CALLING SEQUENCE:
Result = REION_EVENT, event
OUTPUTS:
Au retour la fonction fournit la structure
result:{id:parent, Top:event.top, Handler:0L,$
XD:xd, XF:xf, YD:yd, YF:yf}
X, Y coordonnees de la region selectionnee
UVALUE = 'REGION'
CALLS: ***
BOX_CURSOR2, CW_FIELD, CW_REGION, IND_RS, RS_IND, STR_SEP, UVALUE_REGION
CALLED BY:
CW_REGION, UVALUE_REGION
COMMON BLOCKS:
IDENT_REG:
cursor identification du widget 'CURSOR'
reset identification du widget 'RESET'
textx identification du widget X:...
texty identification du widget Y:
state structure
MODIFICATION HISTORY:
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NAME:
RELPHZ
PURPOSE:
Given a time index during a scan, uses the phases at that time
as the phase calibration and applies those phases to all other
times. This has the effect of making the image at the given time
a point source at the map center, while images at other times show
the source structure and position relative to that at the
fiducial time.
CATEGORY:
OVSA APC Calibration
CALLING SEQUENCE:
out2 = relphz(out,calindex)
INPUTS:
out An array containing calibrated data (the result of acting
on AVG array with APPLY_CAL_ALL() routine).
calindex An integer value representing the time index into the OUT
array to use as the fiducial time (phases at that time
will become the phase calibration.
OPTIONAL (KEYWORD) INPUT PARAMETERS:
None
ROUTINES CALLED:
OUTPUTS:
out2 A array of the same data as in OUT, except that the
phases are modified by using the time indicated by
CALINDEX as the phase calibration.
COMMENTS:
This routine can be handy when the data for an event are not well
calibrated by standard techniques and data exist at another time
for which there is some reason to think that the source structure
is simple. The result can be used only as an indication of change
in source position and/or structure. If the fiducial time chosen
is not simple, the results will be garbage.
SIDE EFFECTS: -
RESTRICTIONS:
MODIFICATION HISTORY:
Written 31-Jan-2004 by Dale E. Gary
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NAME:
RELVIS
PURPOSE:
Determines relative visibility, V(S)/V(0), where V(s) is the visibility
as a function of fringe spacing s, and V(0) is the visibility at zero
fringe spacing, i.e. total power. The relative visibility is independent
of calibration, and will be unity for a point (unresolved) source but
will decrease with increasing s for a resolved one.
CATEGORY:
OVRO APC ANALYSIS
CALLING SEQUENCE:
rv = relvis(filename[,tp][,tpmin=tpmin])
INPUTS:
filename the name of the file containing output data from ANALYZE
*after* preflare subtraction. If preflare subtraction
has not been done, the results will be invalid.
OPTIONAL (KEYWORD) INPUT PARAMETERS:
tpmin if set, gives the minimum total power value for which to
determine the relative visibility. If omitted, 5 sfu is
the minimum value.
ROUTINES CALLED:
OUTPUTS:
rv the relative visibility of size (NBL,NF,NTIMES) for each
baseline. It will contain NaN where the total power is
less than TPMIN.
tp optional output containing the calibrated total power
used in determining RV, of size (NANT,NF,NTIMES).
COMMENTS:
Because of the strange way that OVSA measures polarization, the
strict relative visibility for circular polarization involves a
fudge factor ranging from 0 to 1, depending on the polarization
of the source. Write polarization measurements on baselines as Rij
and Lij, and linear polarization measurements as Iij, where ij are
antenna numbers. Write measurements in total power as Ai, where Ai
are in general (Ri + Li), but for some antennas R and/or L are not
measured at all. Thus, what is actually measured in total power is:
Antenna RCP position LCP position
A1 I1 = (R1 + L1) L1
A2 R2 I2 = (R2 + L2)
An>2 In = (Rn + Ln) In = (Rn + Ln)
The corresponding baseline correlated amplitudes are
Baseline RCP position LCP position
A12 sqrt(R1*R2) sqrt(L1*L2)
A1n sqrt(I1*In) sqrt(L1*Ln)
A2n sqrt(R2*Rn) sqrt(I2*In)
others sqrt(Im*In) sqrt(Im*In)
The fudge factors for the relative visibilities will then be
(from, e.g. RV = Aij/sqrt(Ai*Aj))
Baseline RCP position LCP position
A12 1/sqrt(1+L1/R1) 1/sqrt(R2/L2+1)
A1n 1 1/sqrt(Rn/Ln+1)
A2n 1/sqrt(1+Ln/Rn) 1
others 1 1
These fudge factors range from 0 to 1, depending on the polarization
of the source, as follows:
__Unpol'd__ _100% RCP_ _100% LCP_
BL RCP LCP RCP LCP RCP LCP
A12 0.707 0.707 1 0 0 1
A1n 1 0.707 1 0 1 1
A2n 0.707 1 1 1 0 1
oth 1 1 1 1 1 1
The relative visibility of a point source would then have these values,
and in order to convert this to unity, as required for a point source,
the RV will be divided by these values. Note that RV is only useful for
simple sources, so we will make the approximation that the total power
polarization is the true source polarization.
CALLS: ***
APPLY_CAL_ALL
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 04-Aug-2001 by Dale E. Gary
21-Nov-2001 DG
Fixed a couple of errors.
27-Dec-2001 DG
Removed subtraction of preflare, since it can be done much better
in OVSA_PRESUB.
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NAME: Remove from the Selection
PURPOSE: Removes a plot from the selection list.
CALLING SEQUENCE:
RemoveSel, name
CALLS:
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NAME:
Remove_Sel
PURPOSE:
Remove a plot from the selection
CATEGORY:
Data Management
CALLING SEQUENCE:
Remove_Sel, name
INPUT:
name: the name of the plot to be removed
COMMON BLOCK:
SelectionRetrieval, opaque, where the selection list is
stored.
SIDE EFFECT:
The selection list is changed
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NAME:
REPCHR
PURPOSE:
Replace all occurrences of one character with another in a text string.
CATEGORY:
CALLING SEQUENCE:
new = repchr(old, c1, [c2])
INPUTS:
old = original text string. in
c1 = character to replace. in
c2 = character to replace it with. in
default is space.
KEYWORD PARAMETERS:
OUTPUTS:
new = edited string. out
CALLED BY:
ADXY, CREATE_STRUCT [1], CREATE_STRUCT [2], CURVAL, Change_Selection
DT_TM_MAK [1], DT_TM_MAK [2], DT_TM_MAK [3], HESSI SOHDATA CLASS DEFINITION
Initialize Selection [2], NORH_CREATE_STRUCT [1], NORH_CREATE_STRUCT [2]
NORH_FITS_INTERP [1], NORH_FITS_INTERP [2], READCOL [3], Selection delete
fits_interp, put selection
COMMON BLOCKS:
NOTES:
MODIFICATION HISTORY:
R. Sterner. 28 Oct, 1986.
Johns Hopkins Applied Physics Lab.
RES 1 Sep, 1989 --- converted to SUN.
Copyright (C) 1986, Johns Hopkins University/Applied Physics Laboratory
This software may be used, copied, or redistributed as long as it is not
sold and this copyright notice is reproduced on each copy made. This
routine is provided as is without any express or implied warranties
whatsoever. Other limitations apply as described in the file disclaimer.txt.
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NAME:
Replace by Linear Interpolation
PURPOSE:
Replaces the values between the first and the last element
of "array" by the linear interpolation of
the values in array(minimum) and array(maximum).
CALLING SEQUENCE:
result = ArrayInterp( array )
INPUT:
array: 1D vector to change
RESULT:
the interpolated array.
CALLS: ***
REPLLININT, error
PROCEDURE:
1. computes slope and least value
2. replaces values in "array" by slope*i + leastValue
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NAME:
RH_CALCPOS
PURPOSE: equivalent de CALCPOS (a effacer)
CATEGORY:
NRH general
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NAME:
RH_CLOSE_HEADER
PURPOSE:
Cette procedure ferme les fichiers FITS d'images 2D
et met a jour les headers.
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_CLOSE_HEADER,iunit, dirdsmf, nbfreq, ch, $
itd, itf, numrec, npew, $
date, imstd, imstf, mmin, mmax
INPUTS:
nbfreq : nb de frequences
date : date
Npew : nb de points en EW et en NS
Imstd : heure de debut (ms)
Imstf : heure de fin (ms)
CH : pour la selection des frequences
= ch(10) 'Y' ou 'N'
OUTPUTS:
IUNIT : tableau des numeros d'unite d'ecriture
DIRDSMF : tableau des noms precedes du chemin des fichiers FITS
CALLS: ***
FXBFINISH [1], FXBFINISH [2], RH_MOD_HEADER
MODIFICATION HISTORY:
Ecrit par A. Bouteille
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Cette fonction renvoie les noms du couple d'antennes correspondant a
une correlation donnee;
A Bouteille 21 oct 2003
EX : print,rh_couple_correl(549)
ns08 ns09
CALLS:
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NAME:
RH_CR_HEADER_BT
PURPOSE:
Cette procedure cree un HEADER FITS PRIMAIRE MODELE pour les fichiers
2D FITS type BINARY TABLE
fichier contenant des IMAGES 2D Nancay .
Ce header modele est mis a jour par le programme DPATCHFITS
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_CR_HEADER_BT, header
OUTPUTS:
Header: header
CALLED BY:
RH_GET_HEADER
MODIFICATION HISTORY:
Ecrit par: A. Bouteille
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NAME:
RH_CR_HEADER_PR
PURPOSE:
Cette procedure cree un header fits primaire modele pour les fichiers
2D FITS type binary table, fichier de lignes contenant des images
ou des harmoniques des donnees 2D Nancay .
Ce header modele est ensuite mis a jour par les programmes dpatchfits
et de conversion harmoniques-images
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_CR_HEADER_PR, header
OUTPUTS:
Header: header
CALLED BY:
RH_GET_HEADER
MODIFICATION HISTORY:
Ecrit par: A. Bouteille
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NAME:
RH_CW_TIME
PURPOSE:
Permet de selectionner rapidemment une heure a l'aide d'un
slider ou plus precisement manuellement.
CALLING SEQUENCE:
widget = RH_CW_TIME(Parent)
INPUTS:
Parent: ID du widget pere.
KEYWORD PARAMETERS:
TITLE: titre du widget, pas de titre par defaut.
FRAME: bordure autour du widget, pas de bordure par defaut.
MINIMUM: valeur minimum du slider, [0,0,0,0] par defaut.
MAXIMUM: valeur maximum du slider, [23,59,59,99] par defaut.
XOFFSET offset en x, 0 par defaut.
YOFFSET: offset en y, 0 par defaut.
VALUE: valeur initiale du slider.
UVALUE: user value du widget.
OUTPUTS:
ID du widget cree.
CALLS: ***
RH_FTIME_GET_VALUE, RH_FTIME_SET_VALUE, RH_FTSLIDE_EVENT, RH_REALTOTIME
RH_STRTOTIME, RH_TIMETOREAL
PROCEDURE:
Pour changer la valeur courante
WIDGET_CONTROL, id, SET_VALUE=value
Pour obtenir la valeur courante.
WIDGET_CONTROL, id, GET_VALUE=var
MODIFICATION HISTORY:
28 Fevrier 1995 value represente une heure
tvalue est un tableau de 4 entiers
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RH_DATE100
Return a "mod 100" year in the range 50 to 150
Usage:
y100 = rh_date100(year[, /print])
Return:
y100 <input> The fixed year value
Argument:
year any input The year to be normalized
Keywords:
print ??? input If set, then return a true mod 100
value suitable for printing.
Full ??? input If set, then convert to a full year
with century
CALLED BY:
CALCPOS, I2CDATE, INIT_MALAX, RH_HDR_TIME, RH_IMCUBE, RH_NAME_FITS
History:
Original: 1/12/95; SJT
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RH_DATE100
Return a "mod 100" year in the range 50 to 150
Usage:
y100 = rh_date100(year[, /print])
Return:
y100 <input> The fixed year value
Argument:
year any input The year to be normalized
Keywords:
print ??? input If set, then return a true mod 100
value suitable for printing.
Full ??? input If set, then convert to a full year
with century
CALLED BY:
CALCPOS, I2CDATE, INIT_MALAX, RH_HDR_TIME, RH_IMCUBE, RH_NAME_FITS
History:
Original: 1/12/95; SJT
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Aide en ligne du logiciel DPATCH
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NAME:
RH_DP_INFO
PURPOSE:
Cette procedure rassemble les informations pour le calcul des fichiers
FITS Nrh 2D de sortie :
- nom des fichiers, - nombre d'images attendu dans chaque frequence
entre les heures hd et hf,
- taille em megaoctets.
CATEGORY:
Traitement de fichiers RH
CALLING SEQUENCE:
RH_DP_INFO, nomfich, ch, hd, hf, ipol, npew, $
dsmf, numcnt, taille_mega
INPUTS:
nomfich : nom du fichier RH d'entree
ch :
hd,hf : heures de debut et de fin
ipol : =0 NP seul , =1 NP+P
npew : nb de points de l'image en EW et NS
OUTPUTS:
dsmf(entfi.nf) : nom des fichiers FITS
numcnt(entfi.nf): nb d'images entre hd et hf
taille_mega(entfi.nf) : taille de chaque fichier FITS
CALLS: ***
RH_FRQCNT, RH_NAME_FITS, RH_OPEN, RH_READCH, rh_fich_ctr, rh_lecdeb
CALLED BY:
RH_RDCMP, RH_RDCUBE, RH_RDINT
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
MODIFICATION HISTORY:
Ecrit par A. Bouteille
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NAME:
RH_ECRHEAD_FITS
PURPOSE:
ecriture du header FITS donnees 2D RH
Les enregistrements sont de longueur 2880 octets
un mot-cle fits occupe une ligne de 80 octets
dans un record de 2880 octets on met 36 lignes de 80 octets
CALLING SEQUENCE:
ecrhead_fits,uic,tab
INPUTS:
uic : numero d'unite pour ecrire INT
tab : header STRARR(*)
nrec : nb de records du header
OUTPUTS:
CALLS:
MODIFICATION HISTORY:
ecrit par A.Bouteille (mars 1997)
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NAME:
RH_ELLIPSE_MAILLE()
PURPOSE:
Cette fonction calcule les parametres de l'ellipse qui approche la
section du lobe a mi-puissance. Pour determiner cette ellipse on
utilise la maille elementaire calculee dans RH_MAILLE_3.
La maille elementaire est calculee dans cette fonction
ou bien est fournie en entree par le KEYWORD MAILLE.(dans le cas
ou elle est calculee en amont dans le programme appelant)
Attention il faut d'abord avoir appele INIT_MALAX qui initialise
le common malax.
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
OUTPUTS:
ELLIPSE tableau contenant :
major axis, minor axis (in solar_radii), and angle in
degrees of the major axis with Ox axis.
OPTIONAL INPUTS:
(si non founis, le keyword MAILLE doit etre present.)
FREQ frequence (MHz)
HMSC heure (heures, minutes, secondes, centiemes)
CALLS: ***
RH_MAILLE_3
OPTIONAL KEYWORD INPUT:
MAILLE tableau contenant la maille elementaire quand il a ete
calcule en amont dans le programme appelant.
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
EXAMPLE:
MODIFICATION HISTORY:
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Type de fichier
--------------------------------------------------------------------
rh_fich_ctr, fich, path, typ1, typ2
fich: nom du fichier
path: directory du fichier
typ1: ier caractere du nom du fichier
typ2: 2eme caractere du nom du fichier
CALLS:
CALLED BY
RH_DP_INFO, RH_INIT_HEADER, rh_sel_fich
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NAME:
RH_FRQCNT
PURPOSE:
Cette procedure compte le nombre d'acq par frequence entre kdeb et
kfin
il faut 8 minutes pour parcourir 5 * 10 000 acq ( un fichier
comprime d'une journee a 2i/sec). Donc environ 10 sec pour 1000 images
CATEGORY:
Traitement de fichiers RH
INPUTS:
kdeb : n0 d'acq de depart
kfin : n0 d'acq de fin
OUTPUTS
numcnt : nb d'acq a chq frequence LONARR(entfi.nf)
: (NP + P) compte pour une seule acq
CALLS: ***
RH_READF
CALLED BY:
RH_DP_INFO, RH_INIT_HEADER
MODIFICATION HISTORY:
Ecrit par A. Bouteille
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NAME:
RH_GET_HEADER
PURPOSE:
Cette procedure remplit les header fits primaire et d'extension.
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_GET_HEADER, $
entree
num_freq, dsmf, ipolar, npew, npns, $
imstd, imstf, $
champ_Rs, tb, nbre_enrgt, $
mmax, mmin, $
sortie
hdr0, hdr1, $
entree optionnelle $
str_dp, temps_integ = temps_integ
INPUTS :
num_freq numero de la frequence ( de 0 a entfi.nf -1 )
dsmf tableau nom du fichier a ecrire
ipolar 0 sans polar,=1 avec polar
npew, npns nb de points de l'image 2D en EW et NS
imstd, imstf heure de debut et de fin (msec)
champ_Rs largeur du champ de l'image (Rs)
tb 1 unites des images temperature de brillance
nbre_enrgt nbre d'enregistrements, ie d'images dans le fichier
fits de sortie.
mmax,mmin max et min des fichiers.
OUTPUTS :
hdr0 tableau du header primaire
hdr1 tableau du header d'extension
KEYWORDS :
temps_integ reserve au traitement des images composites RH + GMRT
pour les parametres "exptime", "timestep"
et tdelt1. Ecrase entfi.itg .
OPTIONNEL INPUT :
str_dp : structure des parametres de calcul de l'image
figurant dans le header fits ( parametre
pouvant etre absent dans les versions anciennes.)
CALLS: ***
BIN_DATE, MSH, RH_CR_HEADER_BT, RH_CR_HEADER_PR, RH_HDR_TIME, SXADDPAR [1]
SXADDPAR [2], SXADDPAR [3], SXDELPAR [1], SXDELPAR [2], SXDELPAR [3]
CALLED BY:
RH_INIT_HEADER, RH_RDIMCUBE
COMMON BLOCKS :
RH : communique avec les routines de lecture des donnees
brutes RH
MODIFICATION HISTORY :
01 mar creation par A. Bouteille a partir de D2D_FITS.PRO . Ne traite
qu'une frequence a la fois. Renvoie les header en sortie
04 jun 30 ajout du mot-cle temps_integ pour pouvoir produire des
headers de fichiers fits d'images composite RH + GMRT.
Dans ce cas les donnees RH a haute cadence sont integrees
sur le temps d'integration du GMRT (~2 sec), et la cadence
de sortie (variables "exptime" et "timestep") est evidemment
celle du GMRT et ne peut etre deduite des headers du fichier
de donnees RH.
amelioration presentation.
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convertit l'heure [h,m,s,s/100] en centièmes de seconde
Le total est fait en LONG, donc pas de pb de precision.(juin 2002)
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NAME:
RH_HDR_TIME
PURPOSE:
Cette fonction effectue le codage date [et heure si le parametre ihms
est present] pour les mots-cles
DATE_OBS, DATE_END , DATE et DATE-OBS du header FITS
format standard : CCYY-MM-DDThh:mm:ss[.sss...]Z
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
chtime = HDR_TIME(idat,ihms)
INPUTS:
date : jour,mois,an
OPTIONAL INPUTS:
ihms : heure en millisec
OUTPUTS:
Chtime : heure au format standard FITS
CALLS: ***
MSH, rh_date100 [1], rh_date100 [2]
CALLED BY:
RH_GET_HEADER, RH_MOD_HEADER
MODIFICATION HISTORY:
Ecrit par: A. Bouteille
modif mai 98 : appel a la routine rh_date100 pour avoir une date
avec siecle quelque soit la date rentree sous forme j,m,a
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NAME:
RH_IMCUBE
PURPOSE:
Cette fonction calcule un cube d'images 2D
a partir d'un cube d'harmoniques 2D
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_IMCUBE, Tab_Harm, Tab_Image, SIZE= size, N_SOLAR_RADIUS= n_sol_rd
INPUTS:
tab_harm structure, cube d'harmoniques
(structure remplie par RH_RDCUBE)
OUTPUTS:
tab_image structure, cube d'images
(structure definie ici)
KEYWORDS:
SIZE : taille en X et en Y de l'image (128, 256 ou 512)
par defaut 128
N_SOLAR_RADIUS : largeur du soleil en rayons solaires ( 4 ou 6)
par defaut 4
TB : tb=0 amplitude en sfu
tb=1 amplitude temperature de brillance
NO_ROND : =1 image calculee en coord. interferometriques
=0 image calculee en coord heliographiques
par defaut image "ronde" donc en coord. heliographiques
CALLS: ***
INIT_MALAX, JULDAY, RH_BR_MALC_IM_2D, RH_COREC_PHASE, RH_MALCROND_IM_2D
RH_TAB_CORREL, rh_date100 [1], rh_date100 [2]
CALLED BY:
RH_RDIMCUBE
EXAMPLE:
IDL> rh_imcube,tab_harm,tab_image
IDL> help,tab_image
TAB_IMAGE STRUCT = -> IMAGNP Array[11]
IDL> help,tab_image,/struc
** Structure IMAGNP, 4 tags, length=65548:
TIME LONG 31293050
NSCAN LONG 0
FREQ FLOAT 236.600
STOKESI FLOAT Array[128, 128]
MODIFICATION HISTORY:
-Ecrit par: A. Bouteille (aout 2000)
04 juin 18 : ajout des antennes anti_alias : calcul des images
en utilisant le tableau des correlations calcule
par RH_TAB_CORREL
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NAME :
RH_INIT_HEADER
PURPOSE:
Cette procedure cree les fichiers FITS d'images 2D avec leurs
headers sur le repertoire dpatch_dir
Utilise par le soft RH seul. N'est plus utilise par le soft des images
composites RH + GMRT.
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_INIT_HEADER, nomfich, nbfreq, freq10, date, hdeb, $
kdeb, kfin, fac_integ, ch, ipolar, npew , npew, $
imstd, imstf, larg, tb, mmax, mmin, $
dpatch_dir, $
; Sortie
dsmf, numcnt, iunit, dirdsmf, errmsg
INPUTS:
Nomfich : nom du fichier a traiter
nbfreq, freq10 : nb de frequences et valeurs*10
date,hdeb : date et heure de debut
kdeb kfin : numeros de debut et de fin des images lues dans le
fichier de donnees (fichier qui peut etre comprime
ou non). temps_integ = temps_integ
fac_integ : facteur d'integration des donnees RH pour en reduire
la cadence
ipolar : 1 fichiers Helio avec polar
0 sans polar
npew : nb de points en EW et en NS
larg : largeur de l'image en rayons solaires 4 (ou 6)
imstd : heure de debut (ms)
imstf : heure de fin (ms)
dpatch_dir : repertoire d'ecriture des fichiers FITS 2D
ch : str_array(10) donnant la selection des frequences 'Y' ou 'N'
tb : si tb=1 images donnees en unites de temperature de brillance
sinon en unites de brillance
par defaut unites de brillance
OUTPUTS:
dsmf : nom de fichier de sortie
iunit : tableau des numeros d'unite d'ecriture
dirdsmf : tableau des noms precedes du chemin des fichiers FITS
errmsg : message d'erreur si dpatch_dir n'existe pas
CALLS: ***
FXBCREATE [1], FXBCREATE [2], FXWRITE [1], FXWRITE [2], RH_FRQCNT, RH_GET_HEADER
RH_NAME_FITS, RH_SEPARATOR, rh_fich_ctr
MODIFICATION HISTORY:
Ecrit par A. Bouteille
05 feb 2 : ajout de fac_integ a la liste d'entree. Cela sert a ne pas defi-
nir des fichiers de sortie inutilement trop gros d'un facteur
fac_integ.
reorganisation de la liste d'arguments.
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NAME:
RH_INTEGRE
PURPOSE:
Cette procedure integre les donnees sur un delta T donne.
Elle tourne sur des fichiers Nancay natifs et cree en sortie des
fichiers Nancay natifs.
CALLING SEQUENCE:
RH_INTEGRE, ['/data/extraits/vilmer/2d020220.01B'],'./2i020220.01B',
4.,[11,13,59,87],[11,17,47,50]
INPUTS:
tb_fich : Liste des fichiers a integrer
fichier_itg: nom du fichier integre
integ: temps d'integration en secondes
hdd: debut d'integration demande(h,mn,sec,ct)
hfd: fin d'integration demande "
KEYWORD:
TOUT: integration de tout le fichier
MODIFICATIONS:
juin 1999 : Passage aux fichiers 8 images/sec
lecture acq par acq
nov 1999 : Demarrage a la freq zero
jan 2006 : bug recherche heure de debut corrige
accepte nint=1 : fait alors une extraction simple
CALLS:
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msd : heure de debut demandee en millisec
msf : heure de fin demandee en millisec
kdeb : numero de la 1ere image a lire
kfin : numero de la derniere image a lire
22-07-1998 : nouvelles routines rh_read pour extension NS24
CALLS:
CALLED BY
RH_DP_INFO, RH_RDCMP, RH_RDCUBE, RH_RDINT
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NAME: RH_LISTFREQ
PURPOSE:
Cette procedure liste les frequences des manip RH du mois
Elle cree un fichier de nom freqyymm.lis
CATEGORY:
Traitement de fichiers NRH.
INPUTS:
STR_YYMM : chaine de carac. contenant yymm definissant le mois
KEYWORDS:
REPENT : repertoire des fichiers RH lus
par defaut /data/nancay
REPSOR : repertoire
par defaut repertoire courant
CALLS: ***
RH_CLOSE, RH_OPEN
MODIFICATION HISTORY:
A. Bouteille janvier 2003
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NAME:
RH_MOD_HEADER
PURPOSE:
Cette procedure met a jour les headers FITS primaire et d'extension
apres ecriture des lignes.
CATEGORY:
Traitement de fichiers NRH
INPUTS:
dsmf : nom du fichier
date : date
imstd : heure de debut
imstf : heure de fin
mmin : minimum des points
mmax : maximum des points
KEYWORD:
NBRE_ENRGT : pour reajuster NAXIS2 nb effectif de lignes remplies
CALLS: ***
FXHMODIFY [1], FXHMODIFY [2], MSH, RH_HDR_TIME
CALLED BY:
RH_CLOSE_HEADER
MODIFICATION HISTORY:
Ecrit par A. Bouteille
06-10-2004 : mot cle NBRE_ENRGT
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NAME:
RH_NAME_FITS
PURPOSE:
Cette fonction cree le nom d'un fichier fits RH:
nrhr_ffff_hpg_yyyymmjj_hhmnss:cc_c.fts
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_NAME_FITS, Res, Freq, Type, Npew, Integ, $
Date, Heure, Compr
INPUTS:
Res -> r reseau ew(e) ns(n) 1d(1) ou 2d(2) string
Freq -> ffff frequence en centaines de khz integer
Type i ou h ou p ou f string
i = coordonnees instrumentales
h = coordonnees heliographiques
a = harmoniques
p = fichier de type positions
f = fichier de type flux
Npew-> npew=2**p
p niveau d'interpolation de 0 a 9 integer
Integ-> g niveau d'integration de 0 a 9 integer
Date date (jour, mois, an). intarr(3)
Heure(4)-> heure de debut (h,m,s,c) intarr(3)
Compr-> c ou d ou b string
fichier comprime(c) ou decomprime(d) ou brut(b)
OUTPUTS:
nomfich = nom du fichier
CALLS: ***
rh_date100 [1], rh_date100 [2]
CALLED BY:
RH_DP_INFO, RH_INIT_HEADER
EXAMPLE:
nomfich = RH_NAME_FITS('2', 1640, 'h', npew, 0, $
[1996,10,21], [9,0,0,0], 'c')
MODIFICATIONS:
Le 27/09/00 'c' en tant que separateur de centiemmes de secondes
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Cette fonction renvoie le numero de la correlation (de 0 a entfi.nbcorel-1)
correspondant a un couple d'antennes.
A Bouteille 21 oct 2003
print, rh_num_correl(['ewE1','ew04'])
509
CALLS:
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NAME:
RH_PERIODISE
PURPOSE:
Cette procedure calcule l'image periodis'ee sur n_period periodes.
On prevoit que n_period puisse etre 1.5, 2 ou 4, a l'exclusion
d'aures valeurs.
CATEGORY:
CALLING SEQUENCE:
RH_PERIODISE, $
INPUTS:
PERIOD nombre de periodes a reproduire.
NPI dimension en x et en y de l'image (en pratique toujours l'image
interferometrique.
IMAGE image a periodiser.
OUTPUTS:
IMAGE_LARG : image elargie
KEYWORD PARAMETERS:
CALLS: ***
CONGRID [1], CONGRID [2], CONGRID [3]
EXAMPLE:
MODIFICATION HISTORY:
01 jul 17 clarification des commentaires, adoption de la notation npi
puisque PERIODISE n'est utilise que pour l'image interfero-
metrique.
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NAME:
RH_RDCMP.PRO
PURPOSE:
-sous programme de RH_RDCUBE
-lecture d'un cube de donnees RH comprimees
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE
rh_rdcmp,fich, hd, hf, nof, ipol, tab_harm
routines utilisees pour la lecture: RH_OPEN(..,/MONO) et RH_READCH
routine utilisee pour la recherche d'heure RH_LECDEB
INPUTS:
Fich : nom du fichier a traiter
hd : heure de debut (h,m,s)
hf : heure de fin (h,m,s)
Ipol : =0 sans polar
=1 avec polar
OUTPUTS:
tab_harm : tableau de structures contenant le cube de donnees lues
time,numim,stokesi(2,nb_harm)
avec ipol=1 time,numim,stokesi(2,nb_harm),stokesv(2,nb_harm)
CALLS: ***
HMS, RH_CLOSE, RH_DP_INFO, RH_HDEB, RH_HFIN, RH_OPEN, RH_RDCUBE, RH_RDINT, RH_READCH
RH_READSEL, rh_lecdeb
CALLED BY:
RH_RDCUBE, RH_RDINT
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
MODIFICATION HISTORY:
Ecrit par A. Bouteille ( 24 Aout 2000)
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NAME:
RH_RDCUBE.PRO
PURPOSE:
-lecture d'un cube de donnees RH
Pour les donnees non comprimees ( fichiers 2d ou 2q, 2i ) appel a RH_RDINT
Pour les donnees haute resolution comprimees ( fichiers 2c) appel a RH_RDCMP
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE
rh_rdcube, fich, tabharm, $
freq=ifreq, hdeb=ihdeb, hfin=ihfin, polar= ipolar
INPUTS:
Fich : nom du fichier a traiter
KEYWORDS:
HDEB : heure de debut 'HH:MM:SS:MMM'
par defaut heure de debut du fichier
HFIN : heure de fin 'HH:MM:SS:MMM'
par defaut = HDEB ( une seule image calculee)
POLAR : =0 sans polar ( STOKESI seul)
=1 avec polar ( STOKESI + STOKESV)
par defaut POLAR = 0
OUTPUTS:
tab_harm : tableau de structures contenant le cube de donnees lues
time,numim,stokesi(2,nb_harm)
avec ipolar=1 time,numim,stokesi(2,nb_harm),stokesv(2,nb_harm)
CALLS: ***
HMS, RH_CLOSE, RH_DP_INFO, RH_HDEB, RH_HFIN, RH_OPEN, RH_RDCMP, RH_RDINT, RH_READCH
RH_READSEL, rh_lecdeb
CALLED BY:
RH_RDCMP, RH_RDIMCUBE, RH_RDINT
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
EXAMPLE:
IDL> rh_rdcube,'/juke/128sec/2Q2000_3/2q000807.01',tabharm, $
freq=1,hdeb='8:43',hfin='9:0'
IDL> help,tab_harm
TAB_HARM STRUCT = -> HARMNP Array[11]
IDL> help,tab_harm,/struct
** Structure HARMNP, 4 tags, length=5204:
DATE INTARR(3)
TIME LONG 31293050
NSCAN LONG 0
FREQ FLOAT 236.600
STOKESI FLOAT Array[2, nb_harm]
MODIFICATION HISTORY:
Ecrit par A. Bouteille ( 24 Aout 2000)
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NAME:
RH_RDIMCUBE.PRO
PURPOSE:
-lecture et calcul d'un cube de donnees RH
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE
rh_rdimcube, fich, tab_image, hdr0, hdr1, $
FREQ=ifreq, HDEB=ihdeb, HFIN=ihfin, POLAR= ipolar, $
SIZE= size, N_SOLAR_RADIUS= n_sol_rd, TB= tb
INPUTS:
Fich : nom du fichier a traiter
KEYWORDS:
HDEB : heure de debut 'HH:MM:SS:MMM'
par defaut heure de debut du fichier
HFIN : heure de fin 'HH:MM:SS:MMM'
par defaut = HDEB ( une seule image calculee)
POLAR : =0 sans polar ( STOKESI seul)
=1 avec polar ( STOKESI + STOKESV)
par defaut POLAR = 0
SIZE : taille en X et en Y de l'image (128, 256 ou 512)
par defaut 128
N_SOLAR_RADIUS : largeur du soleil en rayons solaires ( 4 ou 6)
par defaut 4
TB : tb=0 amplitude en sfu
tb=1 amplitude en temperature de brillance
par defaut 1
OUTPUTS:
TAB_IMAGE : tableau de structures contenant le cube d'images
si ipolar=0 time,numim,stokesi(128,128)
si ipolar=1 time,numim,stokesi(128,128),stokesv(128,128)
HDR0 : header fits primaire
HDR1 : header d'extension #1
CALLS: ***
RH_CLOSE, RH_GET_HEADER, RH_IMCUBE, RH_OPEN, RH_RDCUBE, SXADDPAR [1], SXADDPAR [2]
SXADDPAR [3]
CALLED BY:
READ_NRH
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
EXAMPLE:
IDL> rh_rdimcube,'/data/nancay/2q000807.01',tab_image, hdr0,hdr1, $
freq=1,hdeb='08:43:00',hfin='09:30:00'
IDL> help,tab_image
IDL> TAB_IMAGE STRUCT = -> IMAGNP Array[11]
IDL> help,tab_image,/struc
** Structure IMAGNP, 4 tags, length=65548:
TIME LONG 31293050
NSCAN LONG 0
FREQ FLOAT 236.600
STOKESI FLOAT Array[128, 128]
Utilisation :
read_nrh,'2q040412.01',index,tab_image
index2map, index,tab_image,map
plot_map,map
MODIFICATION HISTORY:
Ecrit par A. Bouteille ( 24 Aout 2000)
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NAME:
RH_RDINT.PRO
PURPOSE:
-sous programme de RH_RDCUBE
-lecture d'un cube de donnees RH non comprimees
routines utilisees : RH_OPEN(..,/SEL) et RH_READSEL
routines utilisees pour la recherche d'heure RH_HDEB et RH_HFIN
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE
rh_rdint, fich, hd, hf, nof, ipol, tab_harm
INPUTS:
Fich : nom du fichier a traiter
hd : heure de debut (h,m,s)
hf : heure de fin (h,m,s)
Ipol : =0 sans polar
=1 avec polar
OUTPUTS:
tab_harm : tableau de structures contenant le cube de donnees lues
time,numim,stokesi(2,nb_harm) si ipol=0
time,numim,stokesi(2,nb_harm),stokesv(2,nb_harm) si ipol=1
CALLS: ***
HMS, RH_CLOSE, RH_DP_INFO, RH_HDEB, RH_HFIN, RH_OPEN, RH_RDCMP, RH_RDCUBE, RH_READCH
RH_READSEL, rh_lecdeb
CALLED BY:
RH_RDCMP, RH_RDCUBE
COMMON BLOCKS:
RH : communique avec les routines de lecture des donnees
brutes RH
MODIFICATION HISTORY:
Ecrit par A. Bouteille ( 24 Aout 2000)
Ajout antennes Anti Alias nb_harm : 576--> 648 harmoniques
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NAME:
RH_RONDCUBE
PURPOSE:
Cette procedure calcule l'image heliographique finale (soleil rond)
par interpolation de l'image interferometrique,
CATEGORY:
Traitement de fichiers NRH
CALLING SEQUENCE:
RH_RONDCUBE, Tab_Image, tab_image_helio, SIZE= size,
(structure remplie par RH_RDCUBE)
INPUTS:
tab_image : structure, cube d'images interfero.
OUTPUTS:
tab_image_helio : structure, cube d'images heliog.
(structure definie ici);
KEYWORDS:
SIZE : taille en X et en Y de l'image (128, 256 ou 512)
par defaut 128
N_SOLAR_RADIUS : largeur de l'image en rayons solaires ( 4 6 8 or 10)
par defaut 4
TB : tb=0 amplitude en sfu
tb=1 amplitude temperature de brillance
par defaut tb=1
CALLS: ***
INIT_MALAX, RH_GRILLE, RH_MAILLE_3, RH_NORM_IM
EXAMPLE:
IDL> rh_rondcube,tab_image, tab_image_helio, SIZE = 256, $
N_SOLAR_RADIUS = 6, TB = 1
IDL> help,tab_image
TAB_IMAGE STRUCT = -> IMAGNP Array[11]
IDL> help,tab_image,/struc
** Structure IMAGNP, 4 tags, length=65548:
TIME LONG 31293050
NSCAN LONG 0
FREQ FLOAT 236.600
STOKESI FLOAT Array[128, 128]
MODIFICATION HISTORY:
2004 juillet -Ecrit par: A. Bouteille
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Selection d'un fichier
--------------------------------------------------------------------
rh_sel_fich, fpath, , filter, fich, typ1, typ2
fpath : directory par defaut
separator : separateur
filter: filtre
fich nom du fichier
='' si pas de fichier selectionne
typ1 ier caractere du nom du fichier
typ2 2eme caractere du nom du fichier
CALLS:
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NAME: RH_SEL_FREQ
PURPOSE:
calcule les indices des frequences a traiter
CATEGORY:
Traitement de fichiers NRH.
INPUTS:
NOMFICH : nom du fichier
FREQ : tableau des frequences a traiter
OUTPUTS:
IND_FRQ : intarr() indices des frequences
ind_frq(k) = -1 quand la frequence n'existe pas
CALLS: ***
RH_CLOSE, RH_OPEN
MODIFICATION HISTORY:
version janvier 2003 : choix des frequences
calcule les indices des frequences a traiter
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NAME:
RS_IND
PURPOSE:
Cette fonction donne l'indice d'un pixel dans untableau
a partir de la position en rayon solaire, l'indice du centre le l'image,
la dimension du rayon solaire en pixels
CATEGORY:
RADIO
CALLING SEQUENCE:
IND=IND_RS(RS, pcentre, rayon)
INPUTS:
RS Position du pixel en rayon solaire
Pcentre Indice du centre de l'image
Rayon Nombre de pixels representant le rayon solaire
OUTPUTS:
IND Coordonnee en pixel
CALLED BY:
CW_REGION, NRH2_PROJECTION, NRH_COORDPIX, REGION_EVENT, SUN_IMAGE, UVALUE_REGION
EXAMPLE:
IND = RS_IND(-1, 32, 16)
IND indice du pixel situe a -1 rayon solaire
MODIFICATION HISTORY:
Ecrit par: J Bonmartin le 21/10/97 (bonmartin@obspm.fr)
Le 29/03/99 FIX remplace par ROUND
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NAME:
RSTN2ANT
PURPOSE:
Returns the flux spectrum expected to be measured by 27m or 2m
antennas, based on a quadratic fit to the flux spectrum reported
by RSTN/Penticton and modified by the primary beam size.
CATEGORY:
OVRO APC SUPPORT
CALLING SEQUENCE:
s = rstn2ant,f,s_in,frq[,/twometer]
INPUTS:
f the frequencies [GHz] measured by the RSTN network. If
F[0] = -1, which is the error return from READ_RSTN_FLUX
routine, then this routine returns 0.
s_in the corresponding fluxes, in SFU.
frq the frequencies at which to evaluate a quadratic fit to
f and s_in.
OPTIONAL (KEYWORD) INPUT PARAMETERS:
twometer A switch that indicates that a result for the 2m dishes
should be returned. The default is to return a result
valid for the 27m dishes.
ROUTINES CALLED:
OUTPUTS:
S The expected flux spectrum, in SFU, as measured by either
the 27m antennas (default) or 2m (if /TWOMETER switch is
set). The fluxes are evaluated at the frequencies given
in the FRQ input array. A value of 0 is returned if the
routine fails.
COMMENTS:
CALLS: ***
PANDB, POLY_FIT
CALLED BY:
WTPCAL
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 11-Nov-2000 by Dale E. Gary
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NAME:
RUNMN_RH
PURPOSE:
This procedure computes a running mean of a 1D RH-scan
At the border of the field of view use is made of the periodicity
of the scans.
CATEGORY:
NRH1 Positions
CALLING SEQUENCE:
RUNMN_RH, scan, width, mscan, sdev
INPUTS:
SCAN original 1D scan
WIDTH number of points used for the computation of the mean
KEYWORD PARAMETERS:
Non
OUTPUTS:
MSCAN array of running mean values (output)
SDEV standard deviation of the fit (output)
CALLED BY:
SIGRMN
COMMON BLOCKS:
Non
MODIFICATION HISTORY: (bonmartin@obspm.fr)
17/11/98 adapte du logiciel XHELIO
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NAME:
RVAV
PURPOSE:
Determines the best estimates of phase drift (PDOT) and amplitude
and phase at the reference time supplied. (For use by AMPHIT)
CATEGORY:
OVRO APC DATA CALIBRATION
CALLING SEQUENCE:
errflg = rvav(x,y,t,tref,aref,pref,pdot,siga,sigp)
INPUTS:
x Array of cosine channel values, of size X(NTIMES)
y Corresponding array of sine channel values
t Array of times corresponding to the data (times in min)
tref The reference time [min] at which PDOT, AREF and PREF should
be given.
OPTIONAL (KEYWORD) INPUT PARAMETERS:
ROUTINES CALLED:
ovsa_lfit
OUTPUTS:
aref The amplitude estimate at time TREF.
pref The phase estimate (degrees) at time TREF.
pdot The phase drift (degrees/hr) over the entire range of data.
siga The standard deviation of amplitudes about the mean.
sigp The standard deviation of the phases about the mean.
COMMENTS:
For now, this routine works only on a single frequency at a time.
It can (should?) be expanded to work with all frequencies at once.
CALLS: ***
OVSA_LFIT
CALLED BY:
AMPHIT
SIDE EFFECTS:
RESTRICTIONS:
MODIFICATION HISTORY:
Written 02-Dec-1998 by Dale E. Gary
04-Dec-1998 DG
Earlier version tried to use IDL LINFIT routine, but this one
implements the original LINFIT (now called LFIT to distinguish
from IDL routine) from AMPHIT.
23-Jul-2003 DG
Changed generic LFIT to OVSA_LFIT to distinguish from McTiernan
routine of the same name.