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Last modified: Sat Aug 21 09:32:58 1999.
NAME:
ADD_HEADER
PURPOSE:
addition information from FITS-headers MPFS-frames
DESCRIPTION:
The function computes the total exposure, mean value zenit distance
and modified FITS header
CALLING SEQUENCE:
Result =ADD_HEADER( headers )
CATEGORY:
reduction MPFS-data
INPUTS:
Headers = String array FITS-headers from the MPFS data
OUTPUTS:
Header = String array containing the header from the FITS file.
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Procedures: SXADDPAR,SXADDHIST
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\add_head.pro)
NAME:
CHECK_FITS
PURPOSE:
Given a FITS array IM, and a associated FITS or STSDAS header HDR, this
procedure will check that
(1) HDR is a string array, and IM is defined and numeric
(2) The NAXISi values in HDR are appropiate to the dimensions
of IM
(3) The BITPIX value in HDR is appropiate to the datatype of IM
If HDR contains a DATATYPE keyword (as in STSDAS files), then this is
also checked against the datatype of of IM
If the UPDATE keyword is present, then FITS header will be modified, if
necessary, to force agreement with the image array
CALLING SEQUENCE:
check_FITS, im, hdr, [ dimen, idltype, /UPDATE, /NOTYPE, /SDAS ]
INPUTS:
IM - FITS or STSDAS array, (e.g. as read by SXREAD or READFITS )
HDR - FITS or STSDAS header (string array) associated with IM
OPTIONAL OUTPUTS:
dimen - vector containing actual array dimensions
idltype- data type of the FITS array as specified in the IDL SIZE
function (1 for BYTE, 2 for INTEGER*2, 3 for INTEGER*4, etc.)
OPTIONAL KEYWORD INPUTS:
/NOTYPE - If this keyword is set, then only agreement of the array
dimensions with the FITS header are checked, and not the
data type.
/UPDATE - If this keyword is set then the BITPIX, NAXIS and DATATYPE
FITS keywords will be updated to agree with the array
/SDAS - If this keyword is set then the header is assumed to be from
an SDAS (.hhh) file. CHECK_FITS will then ensure that (1)
a DATATYPE keyword is included in the header and (2) BITPIX
is always written with positive values.
/FITS - If this keyword is present then CHECK_FITS assumes that it is
dealing with a FITS header and not an SDAS header, see notes
below.
SYSTEM VARIBLE:
If there is a fatal problem with the FITS array or header then !ERR is
set to -1. ( If the UPDATE keyword was supplied, and the header could
be fixed then !ERR = 0.)
PROCEDURE:
Program checks the NAXIS1 and NAXIS2 parameters in the header to
see if they match the image array dimensions.
NOTES:
An important distinction between an STSDAS header and a FITS header
is that the BITPIX value in an STSDAS is always positive, e.g. BITPIX=32
for REAL*4 data. Users should use either the /SDAS or the /FITS
keyword if it is important whether the STSDAS or FITS convention for
REAL*4 data is used. Otherwise, CHECK_FITS assumes that if a
DATATYPE keyword is present then it is dealing with an STSDAS header.
MODIFICATION HISTORY:
Written, December 1991 W. Landsman Hughes/STX to replace CHKIMHD
No error returned if NAXIS=0 and IM is a scalar W. Landsman Feb 93
Fixed bug for REAL*8 STSDAS data W. Landsman July 93
Make sure NAXIS agrees with NAXISi W. Landsman October 93
(See d:\rsi\idl40\mpfs.lib\CHECK_FI.PRO)
NAME:
CONV_VAX_UNIX
PURPOSE:
To convert VAX IDL data types to UNIX (Sun,MIPS,etc.) IDL data types.
The architecture is obtained from IDL sys.var. !VERSION.ARCH.
(Derived from the IUE procedure VAX2SUN)
CALLING SEQUENCE:
var_unix = conv_vax_unix( var_vax )
PARAMETERS:
variable (REQ) (IO) (BIFDC) (012)
The data variable to be converted. This may be a scalar
or an array. All IDL datatypes are valid (including structures).
The result of the conversion is returned by the function.
KEYWORD:
TARGET_ARCH = name (string) of desired target architecture
if using this function on a VAX.
otherwise !VERSION.ARCH is used to determine the conversion.
EXAMPLE:
Read a 100 by 100 matrix of floating point numbers from a data
file created on a VAX. Then convert the matrix values into Sun format.
IDL> openr,1,'vax_float.dat'
IDL> data = fltarr(100,100)
IDL> readu,1,data
IDL> data = conv_vax_unix( data )
MODIFICATION HISTORY:
Written F. Varosi August 1990
Modified P. Keegstra April 1992
Implemented MIPSEL architecture
(See d:\rsi\idl40\mpfs.lib\CONV_VAX.PRO)
NAME:
CORRSENT
PURPOSE:
correction spectral sensitivity
DESCRIPTION:
The function computes the absolute spectral distribution in reduced
2-dimensional array MPFS-spectra in erg/cm^2/sec/A.
Routine read vector spectral sensitivity
from disk in working directory with standard name 'sent.fts',
sky-substraction linearised spectra (filename='*-sky.fts', where
image_type='*') and modified FITS header
CALLING SEQUENCE:
CORRSENT, LOG,file_name,PLOT=plot
CATEGORY:
reduction MPFS-data
INPUTS:
LOG = String scalarfile name of FITS-header from the LOG observation MPFS data
image_type= string scalar ( value 'obj' or 'test'
OUTPUTS:
Saved in working directory in file '*_abs.fts'
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
PLOT - if present then plotted spectra central part lens array to display,
else save plot to POSTSCRIPT file in working directory with name '*.ps'
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function : DEF_WDIR,READ_FTS,SXPAR,OS_FAMILY
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\corrsent.pro)
NAME: COSIN_APOD PURPOSE: Apodize a 1-D data set with a cosine apodizing function. CALLING SEQUENCE: Result = COSIN_APOD(N,P) INPUTS: N = number of points of the data set. OPTIONAL INPUTS: P = dimension of the cosine function, in percentage of N. Default is 10 %. OUTPUT: Result = a cosine window function. KEYWORDS: None. COMMON BLOCKS: None. SIDE EFFECTS: None. RESTRICTIONS: None. PROCEDURE: The two edges of the output array are multiplied by a cosine function. MODIFICATION HISTORY: Written by Roberto Luis Molowny Horas, January 1994.
(See d:\rsi\idl40\mpfs.lib\cosin_ap.pro)
NAME:
COSMETIC
PURPOSE:
replace bad column in CCD-frame
DESCRIPTION:
CALLING SEQUENCE:
Result=COSMETIC(image_in,bad_column)
CATEGORY:
reduction MPFS-data
INPUTS:
image_in = 2-dimensional float array CCD-frame MPFS-data
bad_column = 1-dimensional integer array value bad column
OUTPUTS:
Result = 2-dimensional float array
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
no
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\cosmetic.pro)
NAME:
CREA_DISPER
PURPOSE:
Identefication comparison spectra & creation array coefficient dispersion curve
DESCRIPTION:
The routine compare position lines in 2D-array comparison MPFS-spectrum
(from file 'neon_s.fts') with tabulated wavelength from file 'LINES.TAB',
and create after 2-dimensional
polynomial approximation array dispersion coefficients
CALLING SEQUENCE:
CREA_DISPER,LOGFILE,FWHM,N_deg,PLOT=plot
CATEGORY:
reduction MPFS-data
INPUTS:
LOG = String scalar of file name FITS-header from the LOG observation
FWHM = width spectral lines in px
N_deg = degree of 2D-polynomial approximation dispersion curve
OUTPUTS:
2-dimensional ( N_deg+1) x N_spectra float array coefficient dispersion curve,
saved to the disk in working directory with standard name 'disper.fts' and
print in file 'disper.txt'.
Last value in every string is rms approximation i px
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
PLOT - if present 2-d errors of approximation plotted to display,
else save plot to POSTSCRIPT file in working directory with name 'err_line.ps'
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function : DEF_WDIR,DEF_RDIR,DEF_NAME,READ_FTS,INP_WAVE
Procedures: CRSPROD,GOODPOLY
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\crea_dis.pro)
NAME:
CREA_TRA
PURPOSE:
creation traectory for every spectra
DESCRIPTION:
Routine interpolated traectory etalon spectra from file 'eta_tra.fts'
in working directory in position every fiber. Routine used table
position etalon fiber from file 'ETALON.POS' and spectra fiber
(file 'FIBER.POS'). Result save in file 'fib_tra.fts'
CALLING SEQUENCE:
CREA_TRA, LOGFILE
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
saved in file 'fib_tra.fts'
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function : DEF_WDIR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\crea_tra.pro)
NAME:
CROSS_NORM
CLASS:
cross-correlation
CATEGORY:
PURPOSE:
To compute a cross correlation for two spectral segments
which are sampled on the same linear or log(lambda) scale,normalised at
dispersion
CALLING SEQUENCE:
result=CROSS_NORM(FFIR,FSEC,NSPR)
PARAMETERS:
FFIR (REQ) (I) (1) (F)
Required input vector giving the flux data for the first
spectrum.
FSEC (REQ) (I) (1) (F)
Required input vector giving the flux data for the second
spectrum.
NSPR (REQ) (I) (0) (F)
Required input parameter specifying the spectral range to
be considered in the cross-correlation function.
EXAMPLES:
To compute the cross-correlation function for two spectra, FIRST
and SECOND, using the recommended initial spectral range from CRSCOR,
result=CROSS_NORM(FIRST,SECOND)
SYSTEM VARIABLES USED:
INTERACTIVE INPUT:
SUBROUTINES CALLED:
PARCHECK
FILES USED:
SIDE EFFECTS:
RESTRICTIONS:
NOTES:
Assumes same number of elements in both spectra. (Both fluxes are
divided by the number of elements in the first spectrum.)
PROCEDURE:
CROSS is determined for (2*nspr + 1) tags or shifts going from -15
to +15 shifts from the starting locations.
After subtracting the average flux from each spectrum, the cross
correlation function is computed as follows for each point in
the spectra,
TEMP = (second spectrum) * SHIFT(first spectrum,ns)
CROSS(L) = TOTAL(TEMP(ls:us)/nele)
MODIFICATION HISTORY:
25 Jun 1991 PJL cleaned up; added PARCHECK and parameter eq 0
print; tested on SUN and VAX; updated prolog
(See d:\rsi\idl40\mpfs.lib\CROSS_N.PRO)
NAME:
CRSPROD
CLASS:
cross-correlation
CATEGORY:
PURPOSE:
To compute a normalized cross correlation for two spectral segments
which are sampled on the same linear or log(lambda) scale.
CALLING SEQUENCE:
CRSPROD,FFIR,FSEC,NSPR,CROSS,CRMIN,CRMAX
PARAMETERS:
FFIR (REQ) (I) (1) (F)
Required input vector giving the flux data for the first
spectrum.
FSEC (REQ) (I) (1) (F)
Required input vector giving the flux data for the second
spectrum.
NSPR (REQ) (I) (0) (F)
Required input parameter specifying the spectral range to
be considered in the cross-correlation function.
CROSS (REQ) (O) (1) (F)
Required output vector containing the cross-correlation
function.
CRMIN (REQ) (O) (0) (F)
Required output vector containing the minimum of the
cross-correlation function.
CRMAX (REQ) (O)
Required output vector containing the maximum of the
cross-correlation function.
EXAMPLES:
To compute the cross-correlation function for two spectra, FIRST
and SECOND, using the recommended initial spectral range from CRSCOR,
CRSPROD,FIRST,SECOND,15,CROSS,CRMIN,CRMAX
SYSTEM VARIABLES USED:
INTERACTIVE INPUT:
SUBROUTINES CALLED:
PARCHECK
FILES USED:
SIDE EFFECTS:
RESTRICTIONS:
NOTES:
Assumes same number of elements in both spectra. (Both fluxes are
divided by the number of elements in the first spectrum.)
PROCEDURE:
CROSS is determined for (2*nspr + 1) tags or shifts going from -15
to +15 shifts from the starting locations.
After subtracting the average flux from each spectrum, the cross
correlation function is computed as follows for each point in
the spectra,
TEMP = (second spectrum) * SHIFT(first spectrum,ns)
CROSS(L) = TOTAL(TEMP(ls:us)/nele)
MODIFICATION HISTORY:
25 Jun 1991 PJL cleaned up; added PARCHECK and parameter eq 0
print; tested on SUN and VAX; updated prolog
(See d:\rsi\idl40\mpfs.lib\crsprod.pro)
NAME:
CUBE_CLE
PURPOSE:
cleaning cosmic hits in data cube
DESCRIPTION:
CALLING SEQUENCE:
Result = CUBE_CLE( image, tresh )
CATEGORY:
reduction MPFS-data
INPUTS:
image - cube of data in 2D-view : array Nz x (Nx*Ny) elements for cleaning
tresh - level discrimination data in sigma (typical value 10)
OUTPUTS:
Result - cleaned cube
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\cube_cle.pro)
NAME:
DATATYPE
PURPOSE:
Datatype of variable as a string (3 char or spelled out).
CATEGORY:
CALLING SEQUENCE:
typ = datatype(var, [flag])
INPUTS:
var = variable to examine. in
flag = output format flag (def=0). in
KEYWORD PARAMETERS:
Keywords:
/DESCRIPTOR returns a descriptor for the given variable.
If the variable is a scalar the value is returned as
a string. If it is an array a description is return
just like the HELP command gives. Ex:
datatype(fltarr(2,3,5),/desc) gives
FLTARR(2,3,5) (flag always defaults to 3 for /DESC).
OUTPUTS:
typ = datatype string or number. out
flag=0 flag=1 flag=2 flag=3
UND Undefined 0 UND
BYT Byte 1 BYT
INT Integer 2 INT
LON Long 3 LON
FLO Float 4 FLT
DOU Double 5 DBL
COM Complex 6 COMPLEX
STR String 7 STR
STC Structure 8 STC
DCO DComplex 9 DCOMPLEX
COMMON BLOCKS:
NOTES:
MODIFICATION HISTORY:
Written by R. Sterner, 24 Oct, 1985.
RES 29 June, 1988 --- added spelled out TYPE.
R. Sterner, 13 Dec 1990 --- Added strings and structures.
R. Sterner, 19 Jun, 1991 --- Added format 3.
R. Sterner, 18 Mar, 1993 --- Added /DESCRIPTOR.
R. Sterner, 1995 Jul 24 --- Added DCOMPLEX for data type 9.
Johns Hopkins University Applied Physics Laboratory.
Copyright (C) 1985, 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.
(See d:\rsi\idl40\mpfs.lib\DATATYPE.PRO)
NAME:
DEF_NAME
PURPOSE:
definition filename of different type exposure MPFS-data
DESCRIPTION:
CALLING SEQUENCE:
Result=DEF_NAME(FILELOG,TYPE_EXP,N_EXP)
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
TYPE_EXP = string scalar type exposure (values: 'bias','obj','star','flat',
'eta','star','test')
OUTPUTS:
Result = string scalar filename for reading (without extention)
OPTIONAL OUTPUT:
N_exp - number exposures with every value TYPE_EXP
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\def_name.pro)
NAME:
DEF_RDIR
PURPOSE:
DEFINIRION DIRECTORY FOR READING DATA FROM LOG FILE
DESCRIPTION:
CALLING SEQUENCE:
Result=DEF_RDIR(FILELOG)
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
Result = string scalar name directory for reading
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\def_rdir.pro)
NAME:
DEF_SENT
PURPOSE:
definition spectral sensitivity
DESCRIPTION:
routine used linearised MPFS-spectra of standard star (filename in working
directory 'star_lin.fts'), information from FITS-header about total exposure,
gain CCD, mean value zenit distance for calculation observed flux. Observed
flux compare with absolute energy distribution star.
Routine used ASCII data files for the Oke (AJ,99, 1621, 1990) optical
spectrophotometric standard stars
CALLING SEQUENCE:
DEF_SENT, LOGFILE, PLOT=plot
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
in working directory saved 1-dimensional float array spectral sensitivity
in erg/cm^2/sec/A per ADU (standard filename 'sent.fts');
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
PLOT - if present the curve DQE plotted to display,
else save plot to POSTSCRIPT file in working directory with name 'DQE.ps'
RESTRICTIONS:
no
NOTES:
no;
PROCEDURES USED:
Function : DEF_WDIR,NAME_TAB,READ_FTS,INP_WAVE,OS_FAMILY
Procedures: SXPAR,SXADDPAR,MKHDR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\def_sent.pro)
NAME:
DEF_SHIFT
PURPOSE:
definition shift between two image in any direction
DESCRIPTION:
CALLING SEQUENCE:
Result = DEF_SHIFT ( image1, image2, coord, c, w)
CATEGORY:
reduction MPFS-data
INPUTS :
image1 and image2 - images to be shifted
coord - string scalar define shift direction (value 'x' or 'y')
c - magnification for calculation cross-correlation
w - width band integration in cross-shift direction
OUTPUTS:
Result = float scalar
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
CRSPROD
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\DEF_SHI.PRO)
NAME:
DEF_WDIR
PURPOSE:
DEFINIRION DIRECTORY FOR WRITING DATA
DESCRIPTION:
CALLING SEQUENCE:
Result=DEF_WDIR(FILELOG)
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
Result = string scalar name directory for writing
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\def_wdir.pro)
NAME:
EXTRACT
PURPOSE:
extraction spectra in frame MPFS-image
DESCRIPTION:
Routine extracted spectra in MFPS-frame in file with standard name '*_n.fts'
('*'=image_type) along traectory from file with standard name 'fib_tra.fts',
for obj-fibers, and along traectory etalon (from file 'eta_tra.fts' for sky
Routine modified FITS-header
CALLING SEQUENCE:
EXTRACT, LOGFILE, fwhm, image_type
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
fwhm = width band of spectra
image_type = string scalar type exposure (values: 'obj','star','eta',
'neon','test')
OUTPUTS:
Result - array float point spectra saved to disk in working directory
with standard name '*_s.fts'.
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
DEF_WDIR,SXADDPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\extract.pro)
NAME:
FDECOMP
PURPOSE:
Routine to decompose a file name for any operating system
CALLING SEQENCE:
FDECOMP, filename, disk, dir, name, qual, version, [OSFamily = ]
INPUT:
filename - string file name, scalar
OUTPUTS:
All the output parameters are scalar strings
disk - disk name, always '' on a Unix machine, scalar string
dir - directory name, scalar string
name - file name, scalar string
qual - qualifier, set equal to the characters beyond the last "."
version - version number, always '' on a non-VMS machine, scalar string
OPTIONAL INPUT KEYWORD:
OSFamily - one of the four scalar strings specifying the operating
system: 'vms','windows','MacOS' or 'unix'. If not supplied,
then OS_FAMILY() is used to determine the operating system.
EXAMPLES:
Consider the following file names
Unix: file = '/rsi/idl40/avg.pro'
VMS: file = '$1$dua5:[rsi.idl40]avg.pro;3
Mac: file = 'Macintosh HD:Programs:avg.pro'
Windows: file = 'd:\rsi\idl40\avg.pro'
then IDL> FDECOMP, file, disk, dir, name, qual, version
will return the following
Disk Dir Name Qual Version
Unix: '' '/rsi/idl40/' 'avg' 'pro' ''
VMS: '$1$dua5' '[RSI.IDL40]' 'avg' 'pro' '3'
Mac: 'Macintosh HD' ':Programs:' 'avg' 'pro' ''
Windows: 'd:' \rsi\idl40\ 'avg' 'pro' ''
NOTES:
(1) All tokens are removed between
1) name and qual (i.e period is removed)
2) qual and ver (i.e. VMS semicolon is removed)
(2) On VMS the filenames "MOTD" and "MOTD." are distinguished by the
fact that qual = '' for the former and qual = ' ' for the latter.
ROUTINES CALLED:
Function GETTOK(), OS_FAMILY()
Users with V4.0 or later can replace OS_FAMILY() with !VERSION.OS_FAMILY
HISTORY
version 1 D. Lindler Oct 1986
Include VMS DECNET machine name in disk W. Landsman HSTX Feb. 94
Converted to Mac IDL, I. Freedman HSTX March 1994
(See d:\rsi\idl40\mpfs.lib\FDECOMP.PRO)
NAME:
FIND_ETA
PURPOSE:
Find and creation traectory spectra etalon fibers
DESCRIPTION:
Routine find etalon spectra in MPFS-frame from file 'eta_n.fts' and
create after polynomial approximation traectory etalon fibers
CALLING SEQUENCE:
FIND_ETA, LOGFILE, GAUSS=gauss, PLOT=plot
CATEGORY:
reduction MPFS-data
INPUTS:
LOG = String scalar of file name FITS-header from the LOG observation
OUTPUTS:
Result saved to disk in working directory in files with standard names
'eta_tra.fts' - 2D float array traectory fibers
'eta_poly.txt' - table coefficient polynomyal approximation traectory
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
GAUSS - if present cross-dispersion profile fitted by gauss-function
PLOT - if present 2-d errors of approximation plotted to display,
else save plot to POSTSCRIPT file in working directory with name 'err_line.ps'
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function : DEF_WDIR,READ_FTS
Procedures: FI_PEAK
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\find_eta.pro)
NAME:
FI_PEAK
PURPOSE:
Find peaks in a lineout
CATEGORY:
reduction MPFS-data
CALLING SEQUENCE:
peak_find
INPUTS:
xpl: x array
ypl: y array
pkcut: cutoff value for determining peak
KEYWORD PARAMETERS:
no
OUTPUTS:
ipix: pixel location of peaks, array
xpk: x location of peaks, array
ypk: y location of peaks, array
bkpk: background at peak locations, array
COMMON BLOCKS:
None
SIDE EFFECTS:
None.
RESTRICTIONS:
None.
PROCEDURE:
no
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\fi_peak.pro)
NAME:
FLAT_REDUCTION
PURPOSE:
reduction MPFS-image at flat field
DESCRIPTION:
Routine read in working directory flat-field frame from file 'flat_i.fts'
In flat-field frame extracted scattering ligth, end frame normalised
Image with type '*' read from file '*_i.fts', and divided after
scattering ligth by flat. Routine use for calculation scattering ligth
file 'eta_tra.fts'
CALLING SEQUENCE:
FLAT_REDUCTION, LOGFILE, image_type
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
image_type = string scalar type exposure (values: 'obj','star','flat',
'eta','star','test');
OUTPUTS:
Result saved to disk i working directory in file '*_n.fts'
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function DEF_WDIR,READ_FTS, SCATTER
Procedure SXADDPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\flat_red.pro)
NAME: GETTOK PURPOSE: Function to retrieve the first part of the string until the character char is encountered. CALLING SEQUENCE: token = gettok( st, char ) INPUT: char - character separating tokens, scalar string INPUT-OUTPUT: st - (scalar) string to get token from (on output token is removed) OUTPUT: token - scalar string value is returned EXAMPLE: If ST is 'abc=999' then gettok(ST,'=') would return 'abc' and ST would be left as '999' HISTORY version 1 by D. Lindler APR,86 Remove leading blanks W. Landsman (from JKF) Aug. 1991
(See d:\rsi\idl40\mpfs.lib\GETTOK.PRO)
NAME:
GET_DATE
PURPOSE:
Return the current date in DD/MM/YY format. This is the format
required by the DATE and DATE-OBS keywords in a FITS header
CALLING SEQUENCE:
GET_DATE, dte
INPUTS:
None
OUTPUTS:
dte = An eight character scalar string specifying the current day
(0-31), current month (1-12), and last two digits of the
current year
EXAMPLE:
Add the current date to the DATE keyword in a FITS header,h
IDL> GET_DATE,dte
IDL> sxaddpar, h, 'DATE', dte
REVISION HISTORY:
Written W. Landsman March 1991
(See d:\rsi\idl40\mpfs.lib\GET_DATE.PRO)
NAME: goodpoly PURPOSE: (one line) Robust fitting of a polynomial to data. DESCRIPTION: This is a multi-pass fitting routine that fits a fixed order polynomial to the input data. After each pass, the scatter of the fit relative to the fitted line is computed. Each point is examined to see if it falls beyond THRESH sigma from the line. If is does, it is removed from the data and the fit is tried again. This will make two attempts to remove bad data. CATEGORY: CALLING SEQUENCE: coeff = goodpoly(x,y,order,thresh,yfit,newx,newy) INPUTS: x - Input dataset, independant values. y - Input dataset, dependant values. order - Order of the polynomial fit (linear = 1). thresh - Sigma threshold for removing outliers. OPTIONAL INPUT PARAMETERS: KEYWORD PARAMETERS: OUTPUTS: yfit - Fitted values for y that match the input vector. newx - X values from input that were considered good. newy - Y values from input that were considered good. Return value is the set of polynomial coefficients. COMMON BLOCKS: SIDE EFFECTS: RESTRICTIONS: PROCEDURE: MODIFICATION HISTORY: Written 1991 Feb., Marc W. Buie, Lowell Observatory 93/11/12, MWB, Program fixed to return a computed y for all input x.
(See d:\rsi\idl40\mpfs.lib\goodpoly.pro)
NAME: HOST_TO_IEEE PURPOSE: To translate an IDL variable from the host machine representation into IEEE-754 representation (as used, for example, in FITS data ). CALLING SEQUENCE: HOST_TO_IEEE, data, [ IDLTYPE = , ] INPUT-OUTPUT PARAMETERS: data - any IDL variable, scalar or vector. It will be modified by HOST_TO_IEEE to convert from host to IEEE representation. Byte and string variables are returned by HOST_TO_IEEE unchanged OPTIONAL KEYWORD INPUTS: IDLTYPE - scalar integer (1-7) specifying the IDL datatype according to the code given by the SIZE function. This keyword will usually be used when suppying a byte array that needs to be interpreted as another data type (e.g. FLOAT). EXAMPLE: Suppose FITARR is a 2880 element byte array to be converted to a FITS record and interpreted a FLOAT data. IDL> host_to_ieee, FITARR, IDLTYPE = 4 METHOD: The BYTEORDER procedure is called with the appropriate keywords RESTRICTION: Assumes the IDL version is since 2.2.2 when the /XDRTOF keyword became available to BYTEORDER. There were two bad implementations in BYTEORDER for double precision: (1) in IDL V3.* for DecStations (!VERSION.ARCH = 'mipsel') and (2) on Dec Alpha OSF machines. IEEE_TO_HOST works around these cases by swapping the byte order directly. MODIFICATION HISTORY: Adapted from CONV_UNIX_VAX, W. Landsman Hughes/STX January, 1992 Fixed Case statement for Float and Double September, 1992 Workaround for /DTOXDR on DecStations January, 1993 Workaround for /DTOXDR on Alpha OSF July 1994 Assume since Version 2.2.2, Ultrix problems persist November 1994 Add support for double complex July, 1995 Workaround for VAX VMS bug in BYTEORDER,/FTOXDR in V4.0 August 1995 Workaround for VMS bug in BYTEORDER,/FTOXDR and /DTOXDR in V4.0.1 (sigh...) W. Landsman August 1995 Workaround for /FTOXDR bug in OSF V4.0.1 September 1995
(See d:\rsi\idl40\mpfs.lib\HOST_TO_.PRO)
NAME: IEEE_TO_HOST PURPOSE: To translate an IDL variable in IEEE-754 representation (as used, for example, in FITS data ), into the host machine architecture. CALLING SEQUENCE: IEEE_TO_HOST, data, [ IDLTYPE = , ] INPUT-OUTPUT PARAMETERS: data - any IDL variable, scalar or vector. It will be modified by IEEE_TO_HOST to convert from IEEE to host representation. Byte and string variables are returned by IEEE_TO_HOST unchanged OPTIONAL KEYWORD INPUTS: IDLTYPE - scalar integer (1-7) specifying the IDL datatype according to the code given by the SIZE function. This keyword is usually when DATA is a byte array to be interpreted as another datatype (e.g. FLOAT). EXAMPLE: A 2880 byte array (named FITARR) from a FITS record is to be interpreted as floating and converted to the host representaton: IDL> IEEE_TO_HOST, fitarr, IDLTYPE = 4 METHOD: The BYTEORDER procedure is called with the appropriate keyword RESTRICTION: Assumes the IDL version is since 2.2.2 when the /XDRTOF keyword became available to BYTEORDER. There were two bad implementations in BYTEORDER for double precision: (1) in IDL V3.* for DecStations (!VERSION.ARCH = 'mipsel') and (2) on Dec Alpha OSF machines. IEEE_TO_HOST works around these cases by swapping bytes directly MODIFICATION HISTORY: Written, W. Landsman Hughes/STX May, 1992 Fixed error Case statement for float and double September 1992 Workaround to /XDRTOD problem on DecStations January 1993 Assume since Version 2.2, correct double precision problems in Alpha/OSF, implement Ultrix corrections from Tom McGlynn November 1994 Added support for double precision complex July 1995 Workaround for BYTEORDER, /FTOXDR bug in VAX VMS V4.0 August 1995
(See d:\rsi\idl40\mpfs.lib\IEEE_TO_.PRO)
NAME:
INP_WAVE
PURPOSE:
DEFINIRION CENTRAL WAVELENGTH AND DISPERSION FROM LOG FILE
DESCRIPTION:
CALLING SEQUENCE:
Result = INP_WAVE ( FILELOG )
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
Result = 2 element vector, were first element - central wavelength in A
second - dprevius value dispersion in A/px
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\inp_wave.pro)
NAME:
IS_IEEE_BIG
PURPOSE:
Determine if the current machine is use IEEE, big-endian numbers.
(This implies that byteorder conversions are no-ops).
CALLING SEQUENCE:
flag = is_ieee_big()
INPUT PARAMETERS:
None
RETURNS:
1 if the machine appears to be IEEE-compliant, 0 if not.
COMMON BLOCKS:
None.
SIDE EFFECTS:
None
RESTRICTIONS:
PROCEDURE:
A sample int, long, float and double are converted using
byteorder and compared with the original. If there is no
change, the machine is assumed to be IEEE compliant and
big-endian.
MODIFICATION HISTORY:
Written 15-April-1996 by T. McGlynn for use in MRDFITS.
(See d:\rsi\idl40\mpfs.lib\IS_IEEE_.PRO)
NAME:
LINEAR
PURPOSE:
linearisation spectra
DESCRIPTION:
CALLING SEQUENCE:
Result = LINEAR ( spectr, disper_par, N_lin, lambda_0, d_lambda)
CATEGORY:
reduction MPFS-data
INPUTS:
spectr = 2D array MPFS extracted spectra
disper_par = 2D array polynomial coefficits dispersion curve for every fiber
N_lin = numper ponts in linearised spectra
lambda_0 = beginning wavelength in A linearised spectra
d_lambda = dispersion in A/px linearised spectra
OUTPUTS:
Result = 2D array spectra
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
no
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\linear.pro)
NAME:
LINERISATION
PURPOSE:
linearisation spectra
DESCRIPTION:
Routine read extracted MPFS-spectra with type '*' from file '*_s.fts'
in working directory and lineriarised. If parameter 'OUT_WAVE' in LOG
observation is non-zero, routine use parameters linearisation from LOG,
else use mean parameter linearisation (beginning wavelength and dispersion)
calculated by file 'disper_par.fts'. Routine modified FITS-header of result
CALLING SEQUENCE:
LINERISATION, logfile, image_name
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
image_type = string scalar type exposure (values: 'obj','star','neon',,'test')
OUTPUTS:
Result saved to disk i working directory in file '*_lin.fts'
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function DEF_WDIR,READ_FTS, OUT_WAVE
Procedure SXADDPAR,SXADDHIST
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\lineris.pro)
NAME:
MKHDR
PURPOSE:
Make a minimal primary FITS image header or a minimal FITS IMAGE
extension header. If an array is supplied then the
created FITS header will be appropiate to the supplied array.
Otherwise, the user can specify the dimensions and datatype.
CALLING SEQUENCE:
MKHDR, header ;Prompt for image size and type
or
MKHDR, header, im, [ /IMAGE, /EXTEND ]
or
MKHDR, header, type, naxisx, [/IMAGE, /EXTEND ]
OPTIONAL INPUTS:
IM - If IM is a vector or array then the header will be made
appropiate to the size and type of IM. IM does not have
to be the actual data; it can be a dummy array of the same
type and size as the data. Set IM = '' to create a dummy
header with NAXIS = 0.
TYPE - If more than 2 parameters are supplied, then the second parameter
is intepreted as an integer giving the IDL datatype e.g.
1 - LOGICAL*1, 2 - INTEGER*2, 4 - REAL*4, 3 - INTEGER*4
NAXISX - Vector giving the size of each dimension (NAXIS1, NAXIS2,
etc.).
OUTPUT:
HDR - image header, (string array) with required keywords
BITPIX, NAXIS, NAXIS1, ... Further keywords can be added
to the header with SXADDPAR.
OPTIONAL INPUT KEYWORDS:
IMAGE = If set, then a minimal header for a FITS IMAGE extension
is created. An IMAGE extension header is identical to
a primary FITS header except the first keyword is
'XTENSION' = 'IMAGE' instead of 'SIMPLE ' = 'T'
EXTEND = If set, then the keyword EXTEND is inserted into the file,
with the value of "T" (true).
RESTRICTIONS:
(1) MKHDR should not be used to make an STSDAS header or a FITS
ASCII or Binary Table header. Instead use
SXHMAKE - to create a minimal STSDAS header
FXHMAKE - to create a minimal FITS binary table header
FTCREATE - to create a minimal FITS ASCII table header
(2) Any data already in the header before calling MKHDR
will be destroyed.
EXAMPLE:
Create a minimal FITS header, HDR, for a 30 x 40 x 50 INTEGER*2 array
IDL> MKHDR, HDR, 2, [30,40,50]
Alternatively, if the array already exists as an IDL variable, ARRAY,
IDL> MKHDR, HDR, ARRAY
PROCEDURES CALLED:
SXADDPAR, GET_DATE
REVISION HISTORY:
Written November, 1988 W. Landsman
May, 1990, Adapted for IDL Version 2.0, J. Isensee
(See d:\rsi\idl40\mpfs.lib\MKHDR.PRO)
NAME: moment PURPOSE: (one line) Compute various statistical moments of the data. DESCRIPTION: This routine computes the average, average deviation, standard deviation, variance, skew and kurtosis of the input data. The various output quantities are always returned as floating point scalars. The statistics are compute with no regard for the dimensionality of the input data. CATEGORY: statistics CALLING SEQUENCE: moment_r,data,avg,avgdev,stddev,var,skew,kurt INPUTS: data - Input data to be analyzed. OPTIONAL INPUT PARAMETERS: None. KEYWORD PARAMETERS: None. OUTPUTS: avg - Sample mean. avgdev - Average deviation of the data from the mean. stddev - Standard deviation of the data from the mean. var - Variance of the data from the mean. skew - Skewness, third statistical moment. kurt - Kurtosis, fourth statistical moment. COMMON BLOCKS: None. SIDE EFFECTS: None. RESTRICTIONS: None. PROCEDURE: Standard techniques, see section 13.1 in Numerical Recipies. MODIFICATION HISTORY: Written by Marc W. Buie, Lowell Observatory, 1992 Jan 20
(See d:\rsi\idl40\mpfs.lib\moment_r.pro)
NAME:
NAME_TAB
PURPOSE:
DEFINIRION NAME OF TABLE WITH ABSOLUTE ENERGY DISTRIBUTION OF STAR
DESCRIPTION:
CALLING SEQUENCE:
Result=NAME_TAB(FILELOG)
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
Result = string scalar name file
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\name_tab.pro)
NAME: OS_FAMILY PURPOSE: Return the current operating system as in !VERSION.OS_FAMILY CALLING SEQUENCE result = OS_FAMILY() INPUTS: None OUTPUTS: result - scalar string containing one of the four values 'Windows','MacOS','vms' or 'unix' NOTES: OS_FAMILY is assumed to be 'unix' if !VERSION.OS is not 'windows', 'MacOS' or 'vms' To make procedures from IDL V4.0 and later compatibile with earlier versions of IDL, replace calls to !VERSION.OS_FAMILY with OS_FAMILY(). PROCEDURES CALLED function tag_exists REVISION HISTORY: Written, W. Landsman
(See d:\rsi\idl40\mpfs.lib\OS_FAMIL.PRO)
NAME:
OUT_WAVE
PURPOSE:
read parameter of linerisation from LOG observation
DESCRIPTION:
CALLING SEQUENCE:
Result=OUT_WAVE(FILELOG)
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
Result = 2 elements float point array contain beginning wavelength in A,
dispersion in A/px and number elements in linearised spectra
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\out_wave.pro)
NAME:
PAR_LINE
PURPOSE:
calculation parameter of line in nigth sky spectrum
DESCRIPTION:
CALLING SEQUENCE:
Result = PAR_LINE ( vector,param,FWHM,line)
CATEGORY:
reduction MPFS-data
INPUTS :
vector input vector spectra
param=[lambda_0,d_lambda] beginnig wavelength(A) end dispersion(A/px)
FWHM previus value width lines in px
line wavelength line in A
OUTPUTS:
Result =[flux,position(in px),FWHM(in px)]
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
ROBOMEAN
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\par_line.pro)
NAME:
READFILE
PURPOSE:
read files with MPFS-images. Will also read zip compressed FTS-files
DESCRIPTION:
CALLING SEQUENCE:
Result= READFILE ( rdir, filename, ext, head)
CATEGORY:
reduction MPFS-data
INPUTS:
rdir - string name input directory for reading
filename - string name file withot extention
ext - string name extention file for reading (value '.zip' or '.fts')
if extention e.q. '.zip' routine unzippiped files
OUTPUTS:
Result = 2D ploat point array MPFS-image
OPTIONAL OUTPUT:
head - string array contain FITS-header image
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
READ_FTS, SPAWN
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\readfile.pro)
NAME:
READFITS
PURPOSE:
Read a FITS file into IDL data and header variables. Will also
read gzip compressed FITS files on Unix machines.
CALLING SEQUENCE:
Result = READFITS( Filename,[ Header, /NOSCALE, EXTEN_NO = ,
/SILENT , NaNVALUE = , STARTROW = , NUMROW = ] )
INPUTS:
FILENAME = Scalar string containing the name of the FITS file
(including extension) to be read. If the filename has
a *.gz extension, it will be treated as a gzip compressed
file.
OUTPUTS:
Result = FITS data array constructed from designated record.
If the specified file was not found, then Result = -1
OPTIONAL OUTPUT:
Header = String array containing the header from the FITS file.
OPTIONAL INPUT KEYWORDS:
NOSCALE - If present and non-zero, then the ouput data will not be
scaled using the optional BSCALE and BZERO keywords in the
FITS header. Default is to scale.
SILENT - Normally, READFITS will display the size the array at the
terminal. The SILENT keyword will suppress this
NaNVALUE - This scalar is only needed on VMS architectures. It
specifies the value to translate any IEEE "not a number"
values in the FITS data array. It is needed because
the VMS does not recognize the "not a number" convention.
EXTEN_NO - scalar integer specify the FITS extension to read. For
example, specify EXTEN = 1 or /EXTEN to read the first
FITS extension. Extensions are read using recursive
calls to READFITS.
POINT_LUN - Position (in bytes) in the FITS file at which to start
reading. Useful if READFITS is called by another procedure
which needs to directly read a FITS extension. Should
always be a multiple of 2880.
STARTROW - This keyword only applies when reading a FITS extension
It specifies the row (scalar integer) of the extension table at
which to begin reading. Useful when one does not want to read
the entire table.
NUMROW - This keyword only applies when reading a FITS extension.
If specifies the number of rows (scalar integer) of the
extension table to read. Useful when one does not want to
read the entire table.
EXAMPLE:
Read a FITS file TEST.FITS into an IDL image array, IM and FITS
header array, H. Do not scale the data with BSCALE and BZERO.
IDL> im = READFITS( 'TEST.FITS', h, /NOSCALE)
If the file contain a FITS extension, it could be read with
IDL> tab = READFITS( 'TEST.FITS', htab, /EXTEN )
The function TBGET() can be used for further processing of a binary
table, and FTGET for an ASCII table.
To read only rows 100-149 of the FITS extension,
IDL> tab = READFITS( 'TEST.FITS', htab, /EXTEN,
STARTR=100, NUMR = 50 )
To read in a file that has been compressed:
IDL> tab = READFITS('test.fits.gz',h)
ERROR HANDLING:
If an error is encountered reading the FITS file, then
(1) the system variable !ERROR is set (via the MESSAGE facility)
(2) the error message is displayed (unless /SILENT is set),
and the message is also stored in !ERR_STRING
(3) READFITS returns with a value of -1
RESTRICTIONS:
(1) Cannot handle random group FITS
(2) Cannot read the heap area in a variable length binary table
NOTES:
The procedure FXREAD can be used as an alternative to READFITS.
FXREAD has the option of reading a subsection of the primary FITS data.
PROCEDURES USED:
Functions: SXPAR(), WHERENAN()
Procedures: IEEE_TO_HOST, SXADDPAR, FDECOMP
MODIFICATION HISTORY:
MODIFIED, Wayne Landsman October, 1991
Added call to TEMPORARY function to speed processing Feb-92
Added STARTROW and NUMROW keywords for FITS tables Jul-92
Work under "windows" R. Isaacman Jan-93
Check for SIMPLE keyword in first 8 characters Feb-93
Removed EOF function for DECNET access Aug-93
Work under "alpha" Sep-93
Null array processing fixed: quotes in a message
properly nested, return added. Affected case when
readfits called from another procedure. R.S.Hill Jul-94
Correct size of variable length binary tables W.Landsman Dec-94
To read in compressed files on Unix systems. J. Bloch Jan-95
Check that file is a multiple of 2880 bytes Aug-95
Added FINDFILE check for file existence K.Feggans Oct-95
Consistent Error Handling W. Landsman Nov-95
Handle gzip image extensions W. Landsman Apr-96
Fixed bug reading 1-d data introduced Apr-96 W. Landsman Jun-96
(See d:\rsi\idl40\mpfs.lib\READFITS.PRO)
NAME: READ_FTS PURPOSE: Read a FITS file into IDL data and header variables. Will also read gzip compressed FITS files on Unix machines. CALLING SEQUENCE: Result = READ_FTS( Filename,[ Header, /NOSCALE, EXTEN_NO = , /SILENT , NaNVALUE = , STARTROW = , NUMROW = ] ) INPUTS: FILENAME = Scalar string containing the name of the FITS file (including extension) to be read. If the filename has a *.gz extension, it will be treated as a gzip compressed file. OUTPUTS: Result = FITS data array constructed from designated record. If the specified file was not found, then Result = -1 OPTIONAL OUTPUT: Header = String array containing the header from the FITS file. OPTIONAL INPUT KEYWORDS: NOSCALE - If present and non-zero, then the ouput data will not be scaled using the optional BSCALE and BZERO keywords in the FITS header. Default is to scale. SILENT - Normally, READFITS will display the size the array at the terminal. The SILENT keyword will suppress this NaNVALUE - This scalar is only needed on VMS architectures. It specifies the value to translate any IEEE "not a number" values in the FITS data array. It is needed because the VMS does not recognize the "not a number" convention. EXTEN_NO - scalar integer specify the FITS extension to read. For example, specify EXTEN = 1 or /EXTEN to read the first FITS extension. Extensions are read using recursive calls to READFITS. POINT_LUN - Position (in bytes) in the FITS file at which to start reading. Useful if READFITS is called by another procedure which needs to directly read a FITS extension. Should always be a multiple of 2880. STARTROW - This keyword only applies when reading a