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: http://sn.sai.msu.ru/~sil/mpfshelp/
Дата изменения: Tue Aug 24 18:45:56 1999 Дата индексирования: Mon Oct 1 19:31:39 2012 Кодировка: Поисковые слова: asteroid |
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)