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Дата изменения: Tue Aug 24 18:45:56 1999 Дата индексирования: Mon Oct 1 19:31:39 2012 Кодировка: Поисковые слова: п п п п п п п п п п п п п п п |
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 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
MODIFIED for MPFS FITS-format by Victor Afanasiev Jul-99
(See d:\rsi\idl40\mpfs.lib\read_fts.pro)
NAME:
REDUCTION
PURPOSE:
bias substraction,replace bad pixels, remove cosmic hits and
correction flexibility in set MPFS-image with different type
DESCRIPTION:
Routine make bias substraction,replace bad pixels, remove cosmic hits and
correction flexibility in set MPFS-image with different type.
image shiftted at differnt way for different value image_type:
obj and neon-images shifted relatively 1-st image in both direction,
flat-images shifted relatively reduced obj-image only in cross-dispersion
direction, star,eta and test-images shifted relatively reduced flat-image
in cross-dispersion direction. Routine modified FITS-header saved FITS-files
CALLING SEQUENCE:
REDUCTION, LOGFILE, image_type, SHIFT=shift
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
image_type = string array type of exposure (values: 'bias','obj','star',
'flat','eta','neon','test')
OUTPUTS:
Result saved at working directory in file '*_i.fts',where '*'=image_type
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
SHIFT if keyword preset image to be shiftted
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function DEF_WDIR, DEF_RDIR, DEF_NAME, READFILE, READ_FTS,
COSMETIC, DEF_SHIFT, SHIFT_IMAGE
Procedure SXADDPAR, SXADDHIST, REM_HITS
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\reduct.pro)
NAME:
REM_HITS
PURPOSE:
remove cosmic hits on exposure frames
DESCRIPTION:
CALLING SEQUENCE:
Result = REM_HITS ( obj_spp, NOSMOOTH=nosmooth)
CATEGORY:
reduction MPFS-data
INPUTS :
obj_spp - set of analised images
OUTPUTS:
Result = total image cleaned at cosmic hits
OPTIONAL OUTPUT:
obj_spp - set of images cleaned at cosmic hits
OPTIONAL INPUT KEYWORDS:
NOSMOOTH if keyword present, data not smoothed along dispersion
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\rem_hits.pro)
NAME: RFIX PURPOSE: Round X to its nearest integer. CALLING SEQUENCE: Result = RFIX(X) INPUT: X = number, vector or array to be rounded. KEYWORDS: LONG = if set, it will round to a longword integer. OUTPUT: Result = nearest integer rounded version of X. SIDE EFFECTS: None. COMMON BLOCKS: None. RESTRICTIONS: None. PROCEDURE: Straightforward. Algorithm is faster than ASTROLIB NINT function. MODIFICATION HISTORY: Written by Roberto Luis Molowny Horas, November 1991.
(See d:\rsi\idl40\mpfs.lib\rfix.pro)
NAME:
robomean
PURPOSE: (one line)
Robust 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 computed with no regard for the dimensionality of
the input data.
The statistics are robust in that the data is searched for outliers
after the moments are computed. If outliers are found they are
removed and the statistics are computed again. This continues until
either no outliers are found or if the removal of outliers has an
insignificant effect on the statistics.
CATEGORY:
statistics
CALLING SEQUENCE:
robomean,data,thresh,eps,avg,avgdev,stddev,var,skew,kurt,nfinal
INPUTS:
data - Input data to be analyzed.
thresh - Deviation from the mean to signify an outlier.
eps - Smallest significant change in mean in units of std dev.
OPTIONAL INPUT PARAMETERS:
None.
INPUT KEYWORD PARAMETERS:
None.
OUTPUT KEYWORD PARAMETERS:
STDMEAN : Optional return of standard deviation of the mean.
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.
nfinal - Number of points used in the final result.
new - Vector of 'clean' pixels (optional).
COMMON BLOCKS:
None.
SIDE EFFECTS:
None.
RESTRICTIONS:
None.
PROCEDURE:
Standard techniques, see section 13.1 in Numerical Recipies. The
thresh and eps values are not tremendously important. Thresh=5.0
and eps=0.5 appear to work pretty well most of the time.
MODIFICATION HISTORY:
Written by Marc W. Buie, Lowell Observatory, 1992 Jan 20.
Fix - nfinal was not being returned to calling program.
Doug Loucks, Lowell Observatory, 1992 Oct 22.
Fix - Sense of test to determine additional refinement was
not correct for some cases. Changed logic to parallel
the C version, since the WHILE statement is now available
in IDL.
Mod - Added by Marc Buie: Argument 'new,' allowing the 'clean' pixels
to be returned to the caller.
Mod - 2/11/94, DWL, Added keyword STDMEAN to permit return of this
value to the caller.
Modified for MPFS-data by Victor Afanasiev, Jul 1999
(See d:\rsi\idl40\mpfs.lib\robomean.pro)
NAME:
SCATTER
PURPOSE:
substraction scattering ligth
DESCRIPTION:
Routine estimate level scattering light outside of first and
last traectory etalon spectra and substracted scattering light
CALLING SEQUENCE:
Result=SCATTER ( image, traectory_eta)
CATEGORY:
reduction MPFS-data
INPUTS:
image - input MPFS image
traectory_tra - 2D array traectories etalon spectra
OUTPUTS:
Result = scattering ligth substracted image
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
no
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
GOODPOLY
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\scatter.pro)
NAME:
SHIFT_IMAGE
PURPOSE: Remap image by linear interpolation
CATEGORY:
CALLING SEQUENCE:
In = shift_image(im,dx,dy)
INPUTS:
Im = Image to be shifted
Dx = Shift in X-direction
Dy = Shift in Y-direction
KEYWORD PARAMETERS:
OUTPUTS:
In
COMMON BLOCKS:
None.
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
MODIFICATION HISTORY:
Z. Yi, UiO, June, 1992.
modified for MPFS-data by Victor Afanasiev, Jul 1999
(See d:\rsi\idl40\mpfs.lib\shift_im.pro)
NAME:
SHIFT_S
PURPOSE: Remap spectrum by linear interpolation
CATEGORY:
CALLING SEQUENCE:
In = shift_s ( Vector , dx )
INPUTS:
Vector = Image to be shifted
Dx = Shift in X-direction
KEYWORD PARAMETERS:
OUTPUTS:
In
COMMON BLOCKS:
None.
SIDE EFFECTS:
RESTRICTIONS:
PROCEDURE:
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophisical observatory, July, 1999.
(See d:\rsi\idl40\mpfs.lib\shift_s.pro)
NAME:
SHOW_3
PURPOSE:
visualisation 3 images : obj_s.fts, obj_lin.fts, obj-sky.fts
DESCRIPTION:
CALLING SEQUENCE:
SHOW_3, LOGFILE, PS=ps
CATEGORY:
reduction MPFS-data
INPUTS:
LOGFILE = file name of LOG observation (in format FITS-header)
OUTPUTS:
no
OPTIONAL OUTPUT:
no
OPTIONAL INPUT KEYWORDS:
PS - if keyword preset plot image print in POSTSCRIPT file
in working directory (standard name image_3.ps)
RESTRICTIONS:
no
NOTES:
no
PROCEDURES USED:
Function - DEF_NAME,
Procedure - SXPAR
MODIFICATION HISTORY:
Written by Victor Afanasiev, Special Astrophysical Observatory RAS, Jul 1999
(See d:\rsi\idl40\mpfs.lib\show_3.pro)
NAME:
SPEXTR
PURPOSE:
extraction spectra in MPFS-image
DESCRIPTION:
CALLING SEQUENCE:
Result = SPEXTR ( image , traectory , fwhm )
CATEGORY:
reduction MPFS-data
INPUTS:
image - input image (2D float point array)
traectory - 2D array traectory spectra
fwhm - width of the strobe
OUTPUTS:
Result =2D array spectra
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\spextr.pro)
NAME:
STRN
PURPOSE:
The main and original purpose of this procedure is to convert a number
to an unpadded string (i.e. with no blanks around it.) However, it
has been expanded to be a multi-purpose formatting tool. You may
specify a length for the output string; the returned string is either
set to that length or padded to be that length. You may specify
characters to be used in padding and which side to be padded. Finally,
you may also specify a format for the number. NOTE that the input
"number" need not be a number; it may be a string, or anything. It is
converted to string.
CALLING SEQEUNCE:
tmp = STRN( number, [ LENGTH=, PADTYPE=, PADCHAR=, FORMAT = ] )
INPUT:
NUMBER This is the input variable to be operated on. Traditionally,
it was a number, but it may be any scalar type.
OPTIONAL INPUT:
LENGTH This KEYWORD specifies the length of the returned string.
If the output would have been longer, it is truncated. If
the output would have been shorter, it is padded to the right
length.
PADTYPE This KEYWORD specifies the type of padding to be used, if any.
0=Padded at End, 1=Padded at front, 2=Centered (pad front/end)
IF not specified, PADTYPE=1
PADCHAR This KEYWORD specifies the character to be used when padding.
The default is a space (' ').
FORMAT This keyword allows the FORTRAN type formatting of the input
number (e.g. '(f6.2)')
OUTPUT:
tmp The formatted string
USEFUL EXAMPLES:
print,'Used ',strn(stars),' stars.' ==> 'Used 22 stars.'
print,'Attempted ',strn(ret,leng=6,padt=1,padch='0'),' retries.'
==> 'Attempted 000043 retries.'
print,strn('M81 Star List',length=80,padtype=2)
==> an 80 character line with 'M81 Star List' centered.
print,'Error: ',strn(err,format='(f15.2)')
==> 'Error: 3.24' or ==> 'Error: 323535.22'
HISTORY:
03-JUL-90 Version 1 written by Eric W. Deutsch
10-JUL-90 Trimming and padding options added (E. Deutsch)
29-JUL-91 Changed to keywords and header spiffed up (E. Deutsch)
Ma7 92 Work correctly for byte values (W. Landsman)
19-NOV-92 Added Patch to work around IDL 2.4.0 bug which caused an
error when STRN('(123)') was encountered. (E. Deutsch)
(See d:\rsi\idl40\mpfs.lib\STRN.PRO)
NAME:
STRNUMBER
PURPOSE:
Function to determine if a string is a valid numeric value.
CALLING SEQUENCE:
result = strnumber( st, [val] )
INPUTS:
st - any IDL scalar string
OUTPUTS:
1 is returned as the function value if the string st has a
valid numeric value, otherwise, 0 is returned.
OPTIONAL OUTPUT:
val - (optional) value of the string. real*8
WARNING:
(1) In V2.2.2 there was a bug in the IDL ON_IOERROR procedure that
will cause the following statement to hang up IDL
IDL> print,'' + string( strnumber('xxx') )
This bug was fixed in V2.3.0
(2) In V2.3.2, an IDL bug is seen in the following statements
IDL> st = 'E'
IDL> q = strnumber(st) & print,st
The variable 'st' gets modified to an empty string. This problem
is related to the ambiguity of whether 'E' is a number or not
(could be = 0.0E). This bug was fixed in V3.0.0
(3) STRNUMBER was modified in February 1993 to include a special
test for empty or null strings, which now returns a 0 (not a
number). Without this special test, it was found that a
empty string (' ') could corrupt the stack.
HISTORY:
version 1 By D. Lindler Aug. 1987
test for empty string, W. Landsman February, 1993
(See d:\rsi\idl40\mpfs.lib\STRNUMBE.PRO)
NAME: SUB_NSKY PURPOSE: substraction nigth sky spectrum in MPFS data CALLING SEQUENCE: Result = SUB_NSKY, LOGFILE, image_name, [LINE='line'] INPUTS: LOGFILE = file name of LOG observation (in format FITS-header) image_name = string scalar type of exposure values '*'= 'obj' or 'star' or 'test' routine read in working directory coefficients dispersion curves (file 'disper.fts'), extracted linearised spectra object (file '*_lin.fts') and nigth sky probe (file '*_ns.fts) OUTPUTS: saved in file '*-sky.fts' OPTIONAL OUTPUT: no OPTIONAL INPUT KEYWORDS: LINE - use separate nigth sky line for determination accuracy sky substraction PLOT - on control plotting ERROR HANDLING: no RESTRICTIONS: no NOTES: no PROCEDURES USED: Functions: SPEXTR, PAR_LINE, LINEAR,READ_FTS Pricedure: SXADDPAR MODIFICATION HISTORY: MODIFIED by Victor Afanasiev, Special Astrophysical Observatory July, 1999
(See d:\rsi\idl40\mpfs.lib\sub_nsky.pro)
NAME: SXADDHIST PURPOSE: Procedure to add history line(s) to a FITS or STSDAS header CALLING SEQUENCE sxaddhist, history, header, [ /PDU ] INPUTS: history - string or string array containing history line(s) to add to the header header - string array containing the FITS or STSDAS header KEYWORD INPUTS: /PDU - if specified, the history will be added to the primary data unit header, (before the line beginning BEGIN EXTENSION...) Otherwise, it will be added to the end of the header OUTPUTS: header - unpdated header EXAMPLES: sxaddhist, 'I DID THIS', header hist = strarr(3) hist(0) = 'history line number 1' hist(1) = 'the next history line' hist(2) = 'the last history line' sxaddhist, hist, header HISTORY: D. Lindler Feb. 87 April 90 Converted to new idl D. Lindler Put only a single space after HISTORY W. Landsman November 1992 Aug. 95 Added PDU keyword parameters
(See d:\rsi\idl40\mpfs.lib\SXADDHIS.PRO)
NAME: SXADDPAR PURPOSE: Add or modify a parameter in a FITS or STSDAS header array. CALLING SEQUENCE: sxaddpar, Header, Name, Value, [ Comment, Location, BEFORE =, AFTER = , FORMAT= , /PDU] INPUTS: Header = String array containing FITS or STSDAS header. The length of each element must be 80 characters. If not defined, then SXADDPAR will create an empty FITS header array. Name = Name of parameter. If Name is already in the header the value and possibly comment fields are modified. Otherwise a new record is added to the header. If name = 'HISTORY' then the value will be added to the record without replacement. In this case the comment parameter is ignored. Value = Value for parameter. The value expression must be of the correct type, e.g. integer, floating or string. String values of 'T' or 'F' are considered logical values. OPTIONAL INPUT PARAMETERS: Comment = String field. The '/' is added by this routine. Added starting in position 31. If not supplied, or set equal to '', then the previous comment field is retained (when found) Location = Keyword string name. The parameter will be placed before the location of this keyword. This parameter is identical to the BEFORE keyword and is kept only for consistency with earlier versions of SXADDPAR. OPTIONAL INPUT KEYWORD PARAMETERS: BEFORE = Keyword string name. The parameter will be placed before the location of this keyword. For example, if BEFORE='HISTORY' then the parameter will be placed before the first history location. This applies only when adding a new keyword; keywords already in the header are kept in the same position. AFTER = Same as BEFORE, but the parameter will be placed after the location of this keyword. This keyword takes precedence over BEFORE. FORMAT = Specifies FORTRAN-like format for parameter, e.g. "F7.3". A scalar string should be used. For complex numbers the format should be defined so that it can be applied separately to the real and imaginary parts. /PDU = specifies keyword is to be added to the primary data unit header. If it already exists, it's current value is updated in the current position and it is not moved. OUTPUTS: Header = updated FITS header array. RESTRICTIONS: Warning -- Parameters and names are not checked against valid FITS parameter names, values and types. MODIFICATION HISTORY: DMS, RSI, July, 1983. D. Lindler Oct. 86 Added longer string value capability Converted to NEWIDL D. Lindler April 90 Added Format keyword, J. Isensee, July, 1990 Added keywords BEFORE and AFTER. K. Venkatakrishna, May '92 Pad string values to at least 8 characters W. Landsman April 94 Aug 95: added /PDU option and changed routine to update last occurence of an existing keyword (the one SXPAR reads) instead of the first occurence.
(See d:\rsi\idl40\mpfs.lib\SXADDPAR.PRO)
NAME: SXDELPAR PURPOSE: Procedure to delete a keyword parameter(s) from a FITS or STSDAS header CALLING SEQUENCE: sxdelpar, h, parname INPUTS: h - FITS or STSDAS header, string array parname - string or string array of keyword name(s) to delete OUTPUTS: h - updated FITS or STSDAS header, If all lines are deleted from the header, then h is returned with a value of 0 EXAMPLE: Delete the astrometry keywords CDn_n from a FITS header, h IDL> sxdelpar, h, ['CD1_1','CD1_2','CD2_1','CD2_2'] NOTES: (1) No message is returned if the keyword to be deleted is not found (2) All appearances of a keyword in the header will be deleted HISTORY: version 1 D. Lindler Feb. 1987 Converted to new IDL April 1990 by D. Lindler Test for case where all keywords are deleted W. Landsman Aug 1995
(See d:\rsi\idl40\mpfs.lib\SXDELPAR.PRO)
NAME:
SXPAR
PURPOSE:
Obtain the value of a parameter in a FITS or STSDAS header
CALLING SEQUENCE:
result = SXPAR( Hdr, Name, [ Abort, COUNT=, COMMENT = ])
INPUTS:
Hdr = FITS or STSDAS header array, (e.g. as returned by READFITS or
SXOPEN) string array, each element should have a length of 80
characters
Name = String name of the parameter to return. If Name is of
the form 'keyword*' then an array is returned containing
values of keywordN where N is an integer. The value
of keywordN will be placed in RESULT(N-1). The data type
of RESULT will be the type of the first valid match of keywordN
found.
OPTIONAL INPUTS:
ABORT - string specifying that SXPAR should do a RETALL
if a parameter is not found. ABORT should contain
a string to be printed if the keyword parameter is not found.
If not supplied SXPAR will return with a negative
!err if a keyword is not found.
OPTIONAL OUTPUT KEYWORDS:
COUNT - Optional keyword to return a value equal to the number of
parameters found by sxpar, integer scalar
COMMENT - Array of comments associated with the returned values
OUTPUTS:
Function value = value of parameter in header.
If parameter is double precision, floating, long or string,
the result is of that type. Apostrophes are stripped
from strings. If the parameter is logical, 1 is
returned for T, and 0 is returned for F.
If Name was of form 'keyword*' then a vector of values
are returned.
SIDE EFFECTS:
!ERR is set to -1 if parameter not found, 0 for a scalar
value returned. If a vector is returned it is set to the
number of keyword matches found.
If a keyword occurs more than once in a header, a warning is given,
and the first occurence is used.
EXAMPLES:
Given a FITS header, h, return the values of all the NAXISi values
into a vector. Then place the history records into a string vector.
IDL> naxisi = sxpar( h ,'NAXIS*') ; Extract NAXISi value
IDL> history = sxpar( h, 'HISTORY' ) ; Extract HISTORY records
PROCEDURE:
The first 8 chacters of each element of Hdr are searched for a
match to Name. The value from the last 20 characters is returned.
An error occurs if there is no parameter with the given name.
If a numeric value has no decimal point it is returned as type
LONG. If it contains more than 8 numerals, or contains the
character 'D', then it is returned as type DOUBLE. Otherwise
it is returned as type FLOAT
MODIFICATION HISTORY:
DMS, May, 1983, STPAR Written.
D. Lindler Jan 90 added ABORT input parameter
J. Isensee Jul,90 added COUNT keyword
W. Thompson, Feb. 1992, added support for FITS complex values.
W. Thompson, May 1992, corrected problem with HISTORY/COMMENT/blank
keywords, and complex value error correction.
W. Landsman, November 1994, fix case where NAME is an empty string
W. Landsman, March 1995, Added COMMENT keyword, ability to read
values longer than 20 character
W. Landsman, July 1995, Removed /NOZERO from MAKE_ARRAY call
(See d:\rsi\idl40\mpfs.lib\SXPAR.PRO)
NAME:
WRITEFITS
PURPOSE:
Write an an IDL array into a disk FITS file. Works with all types
of FITS files except random groups
CALLING SEQUENCE:
WRITEFITS, filename, data [, header, NaNvalue = , /APPEND]
INPUTS:
FILENAME = String containing the name of the file to be written.
DATA = Image array to be written to FITS file. If DATA is
undefined or a scalar, then only the FITS header (which
must have NAXIS = 0) will be written to disk
OPTIONAL INPUT:
HEADER = String array containing the header for the FITS file.
If variable HEADER is not given, the program will generate
a minimal FITS header.
OPTIONAL INPUT KEYWORD:
NaNvalue - Value in the data array to be set to the IEEE NaN
condition. This is the FITS representation of undefined
values
APPEND - If this keyword is set then the supplied header and data
array are assumed to be an extension and are appended onto
the end of an existing FITS file. Note that the primary
header in the existing file must already have an EXTEND
keyword to indicate the presence of an FITS extension.
OUTPUTS:
None
RESTRICTIONS:
(1) It recommended that BSCALE and BZERO not be used (or set equal
to 1. and 0) with REAL*4 or REAL*8 data.
(2) WRITEFITS will remove any group parameters from the FITS header
EXAMPLE:
Write a randomn 50 x 50 array as a FITS file creating a minimal header.
IDL> im = randomn(seed, 50, 50) ;Create array
IDL> writefits, 'test', im ;Write to a FITS file "test"
PROCEDURES USED:
CHECK_FITS, HOST_TO_IEEE, IS_IEEE_BIG(), SXDELPAR, SXADDPAR, SXPAR()
MODIFICATION HISTORY:
WRITTEN, Jim Wofford, January, 29 1989
MODIFIED, Wayne Landsman, added BITPIX = -32,-64 support for UNIX
Use new BYTEODER keywords 22-Feb-92
Modify OPENW for V3.0.0 W. Landsman Dec 92
Work for "windows" R. Isaacman Jan 93
More checks for null data Mar 94
Work for Linux W. Landsman Sep 95
Added call to IS_IEEE_BIG() W. Landsman Apr 96
(See d:\rsi\idl40\mpfs.lib\WRITEFIT.PRO)