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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: южная атлантическая аномалия |
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)