; NAME: ; pro darkcurrent_reduce.pro (v2.16) ; ; PURPOSE: ; This program takes a images listed in filename and produces estimates of ; dark current from them. A per-pixel dark current frame is produced, and ; individual dark current slope plots can optionally be created. ; ; CALLING SEQUENCE: ; darkcurrent_reduce, testdir, [outdir [, infile [, valoutfile $ ; [, noref [, ma_refcor [, region [,imgoutfile] [, groupfactor]]]]]] ; ; INPUTS: ; testdir string containing directory name wherein input ; images and a list of the image file names ; can be found ; ; KEYWORD PARAMETERS: ; outdir directory where output will be written; defaults to ; testdir + '\SlopePlots' ; infile input file name. File must be in directory specified by ; testdir. Default name is 'dark.lst' ; valoutfile name for output file containing read-by-read mode values. ; Will be written to outdir. Default is ; 'slopevals.txt'. ; imgoutfile name for output file containing names of slope images. ; Will be written to outdir. Default is ; 'slopeimgs.txt'. ; region rectangular region of SCA to consider for ; analysis. Should be entered as 4-element ; 1-d integer array, i.e. [x1,x2,y1,y2] to ; consider pixels in rows x1 to x2 and ; columns y1 to y2. Default is specified as ; all non-reference pixels ; ma_refcor set for maximal averaging reference pixel correction ; noref set to disable reference pixel correction ; gdmask set equal to the name of a good pixel mask. ; 1=good & 0=bad ; groupfactor sets number of reads placed together in a group for ; processing; defaults to 1 (which means ; mode of each read is determined). ; ; NOTE: Default behavior is to do spatial average reference pixel correction. ; If both ma_refcor and noref are set, the noref keyword over-rides the ; ma_refcor keyword and no reference pixel correction will be done. ; ; EXAMPLE ; ; Reduce data from specified directory, using default file names, ; generating slope plots and using maximal averaging reference pixel ; correction, using default region. ; ; IDL> dkdir = '\\rabbit\rockwell3\H2RG-006-5.0mu\cold1\dktest.3Apr03' ; IDL> darkcurrent_reduce, dkdir, /ma_refcor ; ; REFERENCE: ; ; MODIFICATION HISTORY: ; Written by: ; Don Figer, IDTL, May 3, 2003 ; Modified by: ; Don Figer, IDTL, May 5, 2002 ; Added output switches ; Bernie Rauscher, IDTL, August 5, 2002 ; Added reference pixel ; correction, glow correction, and spiffy line-fit plots. ; Ernie Morse, IDTL, October 21, 2002 (v1.1) ; Modified code so that choosing bjrmods option does ONLY the bjrmods ; section, and not the rest of the procedure ; Added code to create output file for use by darkjumbo2.pro ; Added readtime and month2days functions for use in creating ; darkjumbo output file ; Increased min and max histogram bin limits--they were too small for ; higher-signal images ; Ernie Morse, IDTL, October 31, 2002 (v1.2) ; Modified bjrmods section so that PostScript output files are put in ; outdir, not the current directory. ; Ernie Morse, IDTL, Nov. 7, 2002 (v1.2.1) ; Now gets SCA type from header, instead of assuming H1RG ; Calls refsub with SCA type instead of refsub_h1rg directly ; Ernie Morse, IDTL, January 7, 2003 (v1.2.2) ; Changed BJRMODS histogram setup so that histogram bins are ; centered around median signal in data instead of around 0. ; In the previous method, the actual distribution curve tended to ; move off the edge of the histogram range as signal increased and ; there were a lot of empty bins with negative values. ; Ernie Morse, IDTL, February 10-12, 2003 (v1.3) ; Changed reading of FITS files to frame-at-a-time to allow for ; reading arbitrarily large files to prevent limitations imposed by ; the amount of RAM available. ; Added region keyword to allow specification of custom region. ; Removed hard-coded assumptions that array size is 1024 x 1024 ; (array size now taken from header keywords). ; Removed hard-coded assumptions of analysis region. ; Changed plot parameters (increased line & char size & thickness, ; only print det. temp. to 1 mK accuracy). ; Ernie Morse, IDTL, March 5, 2003 (v1.3) ; Added keywords to allow specification of type of reference pixel ; correction ; Added information about analysis region and reference pixel ; correction to plots. ; Ernie Morse, IDTL, March 13, 2003 (v1.3) ; Added name of file to bottom margin area of slopefit plots in ; bjrmods section. ; Ernie Morse, IDTL, April 4, 2003 (v2.0) ; Started all over from scratch. ; Ernie Morse, IDTL, April 8, 2003 (v2.1) ; Cast values read in from headers to int and float data types to ; insure that the slope array ; written out at the end will be a float array in order to decrease ; size of the resulting FITS file. ; B.J. Rauscher, IDTL, April 10, 2003 (v2.2) ; Added ability to use good pixel masks ; Ernie Morse, IDTL, April 11, 2003 (v2.3) ; Changed calls to refsub--must now pass SCA name instead of SCA ; type ; Ernie Morse, IDTL, April 14, 2003 (v2.4) ; Removed the bin representing 0 from the gaussfit to protect against ; spurious zeros caused by railed pixels. ; Ernie Morse, IDTL, April 16, 2003 (v2.5) ; Corrected bug found in implementation of zero-bin rejection. ; Ernie Morse, IDTL, April 30, 2003 (v2.6) ; Added the rd_time keyword and code to allow the processing of the ; Fowler glow images. ; Ernie Morse, IDTL, May 9, 2003 (v2.7) ; Eliminated sa_refcor keyword--spatial average reference pixel ; correction is now default ; Added noref keyword--can be set to explicitly disable reference ; pixel correction ; Made changes in code to reflect new default case (spatial averaging). ; Changed default output directory to testdir+'SlopePlots' ; Ernie Morse, IDTL, May 15, 2003 (v2.8) ; Added write of reference pixel correction version number and type ; to header of slope images ; Ernie Morse, IDTL, October 10, 2003 (v2.9) ; Added cosmic ray detection to creation of per-pixel images ; Ernie Morse, IDTL, October 17, 2003 (v2.10) ; Added groupfactor keyword and modifications to allow grouping ; of reads for processing. Split outfile keyword into valoutfile and ; imgoutfile. Made some changes to format of valoutfile (it now ; must include read times as they can not be calculated in the ; analysis script anymore due to the addition of grouping). ; Ernie Morse, IDTL, December 2, 2003 (v2.11) ; Corrected bugs associated with operation when groupfactor = 1. ; Added graceful exit for case when all pixels in input image are ; railed. ; Ernie Morse, IDTL, July 15, 2004(v2.12) ; Changed from using binsize = 1.0 to starting out with 128 bins with ; size determined by data distribution. ; Added code to catch math errors (from curvefit) ; Corrected problems that arose when first reads of input image are ; at bottom rail. ; Ernie Morse, IDTL, July 22, 2004 (v2.13) ; Added rowinc and colinc keywords. ; Ernie Morse, IDTL, September 29, 2004 (v2.14) ; Modified error handler so that math errors are distinguished from ; non-math errors. ; Ernie Morse, IDTL, October 8, 2004 (v2.15) ; Made changes to prevent blank lines being written to imgoutfile for ; input images that are railed in every read. Moved opening of ; imgoutfile to end of procedure, conditional on there being at least ; one non-railed image and trimmed imginfo array to only include ; entries with non-null file names. ; Ernie Morse, IDTL, September 2, 2005 (v2.16) ; Now uses djsiterstat to determine median and standard ; deviation, which is used to calculate min and max ; for histogram procedure. Number of bins has been altered so ; that bin size = 1.0 ADU. ; Pro darkcurrent_reduce2, testdir, outdir = outdir, infile = infile, $ valoutfile = valoutfile, imgoutfile = imgoutfile, $ ma_refcor = ma_refcor, noref=noref, region = region, $ gdmask = gdmask, groupfactor = groupfactor, $ rowinc = rowinc, colinc = colinc ; set directory path delimiter pathdelim=path_sep() ; set directory path delimiter & end-of-line character based on ; operating system in use (non-unix is assumed to be Windows). if (!version.os_family eq 'unix') then begin endofline = string(10b) endif else begin endofline = string(13b) + string(10b) endelse ; check to see if input directory name ends in path delimiter--if not, ; add it to the end If (strmid(testdir, strlen(testdir)-1, 1) ne pathdelim) then testdir = testdir + pathdelim ; set outdir to testdir + 'SlopePlots' if not set by user If (keyword_set(outdir) eq 0) then outdir = testdir + 'SlopePlots' + pathdelim ; check to see if outdirectory name ends in path delimiter--if not, add it to the end If (strmid(outdir, strlen(outdir)-1, 1) ne pathdelim) then outdir = outdir + pathdelim ; set defaults for keyword values not provided by the calling context If (not keyword_set(infile)) then infile = 'dark.lst' If (not keyword_set(valoutfile)) then valoutfile = 'slopevals.txt' If (not keyword_set(imgoutfile)) then imgoutfile = 'slopeimgs.txt' If (not keyword_set(groupfactor)) then groupfactor = 1 ; If reference pixel correction is to be done, query the refsub function for ; the version number, otherwise, just set a flag indicating it was not done if (not keyword_set(noref)) then begin ref_ver = ' ' refsub, 0, sca=' ', version = ref_ver if (not keyword_set(ma_refcor)) then begin ref_type = 'Spatial averaging' endif else begin ref_type = 'Maximal averaging' endelse endif else begin ref_ver = 'Not used' ref_type = 'N/A' endelse if (not keyword_set(rowinc)) then begin rowinc = 1 endif if (not keyword_set(colinc)) then begin colinc = 1 endif ; open input file and read all filenames into an array Readcol, Testdir + Infile, ImgFiles, format='(A)' ; make an array of structs to hold filename and detector temperature for ; output slope images ImgInfo = replicate({name:'', dettemp:''}, n_elements(imgfiles)) ; open output file for slope values file_mkdir,Outdir openw, Lun_Val, Outdir + Valoutfile, /get_lun ; start by reading just the header of the first image in the list to get ; some required information Fits_read, Testdir + Imgfiles[0], 0, FirstHdr, /header_only Xsize = fix(sxpar(FirstHdr, 'NAXIS1')) Ysize = fix(sxpar(FirstHdr, 'NAXIS2')) SCAName = sxpar(FirstHdr, 'DETNAME') ; define the number of pixels to read in for one group of sample reads NumPixRd = long(Xsize) * Ysize ; extract SCA type from SCA name SCAType = strmid(SCAName, 0, strpos(ScaName, '-')) if stregex(SCAName,'HRG-10-007', /boolean) or SCAName eq ' ' then $ SCAType = 'H4RG' ; if the user didn't set the region, define default regions based on the SCA type if (not keyword_set(Region)) then begin case SCAType OF 'H4RG' : begin Region = [4, 4091, 4, 4091] SCAName = 'H4RG-10-007' end 'H1RG' : begin Region = [4, 1019, 4, 1019] end 'H2RG' : begin Region = [4, 2043, 4, 2043] end 'SB304': begin Region = [4, 2051, 0, 2047] end ELSE : begin print, 'Detector type ' + scaType + $ ' not supported. Exiting procedure.' return end endcase endif ; construct a string representation of the region array Region_Str = strtrim(string(Region), 2) Region_Out = '[' + Region_Str[0] + ':' + Region_Str[1] + ':' $ + strtrim(string(ColInc), 2) + ', ' + Region_Str[2] + ':' $ + Region_Str[3] + ':' + strtrim(string(RowInc), 2) + ']' ; write values common to all the images to the header of the output file printf, Lun_val, Ref_Ver printf, Lun_val, Ref_Type printf, Lun_val, Region_Out ; construct arrays for cosmic ray detection Mask10Sig = intarr(Xsize, Ysize) CosmicRays = fltarr(Xsize, Ysize) ; read mask array if present, otherwise construct mask of all 1s. if (keyword_set(GDMask)) then begin Fits_Read, GDMask, GDMask_Data, GDMask_Header, /data_only endif else begin GDMask_Data = make_array(Xsize, Ysize, /integer, value=1) endelse ; Form a region mask where the reference pixels are not located Region_Mask = GDMask_Data[Region[0]:Region[1]:Colinc, $ Region[2]:Region[3]:Rowinc] ; loop through images listed in input file and process them one frame at ; a time For ImgCount = 0, n_elements(ImgFiles) - 1 do begin ; To keep it simple, the standard formula from Numerical ; Recipes will be used to calculate slope per pixel in an incremental ; fashion. ; ; slope = N * S[x_i * y_i] - S[x_i] * S[y_i] / ( N * S[x_i^2] - ; S[x_i]^2 ) ; First initialize all sums that we will need. To keep it ; simple, I'll keep some redundant sums (e.g., the ; information already is available to the program) ; declare these running-sum arrays for each file so they'll be zeroed ; at the start each time Sxy = dblarr(xsize, ysize) Sx = dblarr(xsize, ysize) Sy = dblarr(xsize, ysize) Sxx = dblarr(xsize, ysize) ; read the 1st frame Fits_Read, Testdir + ImgFiles[Imgcount], 0, ImgHdr, /header_only ; extract information from header If SCAType ne 'H4RG' then begin Exposuretime = double(sxpar(imghdr, 'exp_time')) Numreads = fix(sxpar(imghdr, 'numutr')) Samples_Per_Read = fix(sxpar(imghdr, 'numsamrd')) Dettemp = float(sxpar(imghdr, 'dettemp')) ; Evidently, the last few reads in the dark current experiment ; for H2RG-003-SIPIN are corrupted. This can be seen by ; displaying the corresponding images. In order to address ; this problem, I (Don) added the following lines of code ; that throw away the last 10 reads. if (SCAname eq 'H2RG-003-SIPIN' and NumReads gt 12) then $ numreads = numreads - 10 Endif Else Begin Numreads = Fix(sxpar(ImgHdr, 'NGROUPS')) Samples_Per_Read = Fix(sxpar(ImgHdr, 'NREADS')) Ndrops = Fix(sxpar(ImgHdr, 'NDROPS')) DetTemp = float(sxpar(ImgHdr, 'MOLYTABL')) ExposureTime = 4096.*4096./32.*10.e-6*$ (Ndrops*NumReads+Samples_Per_Read*Numreads) Endelse ; find out how many frame groups there are Numframes = Numreads * Samples_Per_Read Numgroups = ceil(float(NumFrames) / Groupfactor) GroupEnds = indgen(NumGroups) * GroupFactor + (GroupFactor - 1) GroupEnds[NumGroups - 1] = GroupEnds[NumGroups - 1] < (NumFrames - 1) Groupstart = 0 ; create an array containing the time for each group of reads ReadTimes = dindgen(Groupfactor, Numgroups) / $ (NumGroups) * ExposureTime ; if groupfactor > 1 and the last group isn't completely filled ; (i.e., the number of reads in the exposure is not evenly ; divisible by the groupfactor), the readtimes array will contain ; exposure times for reads that aren't present because it assumes that ; all groups contain the same number of reads. Mark these invalid ; exposure times as NaN so they can be ignored in processing. Overtimes = where(Readtimes gt ExposureTime) if (Overtimes[0] ne -1) then ReadTimes[OverTimes] = !values.f_nan ; make an array to hold the exposure times for each group. Each ; element is the mean value of the exposure times of the reads ; contained in the group. Grouptimes = fltarr(NumGroups) For GroupNum = 0, NumGroups - 1 do begin GroupTimes[GroupNum] = mean(ReadTimes[*, GroupNum], /nan) Endfor ; read the frame groups in until the 1st non-railed group is encountered Groupnum = -1 Repeat Begin Groupnum = Groupnum + 1 Fits_Read, Testdir + ImgFiles[ImgCount], FirstGroup, $ first = (GroupEnds[GroupNum]) * NumPixRd, $ last = (GroupEnds[GroupNum + 1]) * NumPixRd - 1 ; transform the first group of reads into an average Framecount = GroupEnds[GroupNum + 1] - GroupEnds[Groupnum] Firstgroup = reform(float(Firstgroup), Xsize, Ysize, Framecount) Firstgroup = total(Firstgroup, 3) / Framecount RegionPix = FirstGroup[Region[0]:Region[1]:$ Colinc,Region[2]:Region[3]:Rowinc] Lowrailpix = where(RegionPix lt -32760) Hirailpix = where(RegionPix gt 32760) LowFraction = n_elements(Lowrailpix) / float(n_elements(RegionPix)) HiFraction = n_elements(Hirailpix) / float(n_elements(RegionPix)) Hi_or_Low = Hifraction ge Lowfraction ? 32767.0 : -32768.0 print, GroupNum Endrep Until ((LowFraction le 0.5 and HiFraction le 0.5) $ OR (Groupnum eq (NumGroups - 2))) ; skip to next image if all reads are railed low If (Groupnum eq Numgroups - 2) then begin ; make an array to hold the output combination of group time and ; corresponding mode value and raw signal OutCombo = fltarr(3, NumGroups) OutCombo[0, *] = Grouptimes OutCombo[2, *] = Hi_or_Low ; write out time and signal values for each read to the file, ; darkcurrent_analyze can be called later to make slope plots. Printf, Lun_Val, Testdir+Imgfiles[ImgCount] + ' ' + $ strtrim(string(NumGroups), 2) + ' ' + $ strtrim(string(GroupFactor), 2) Printf, Lun_Val, OutCombo, format='(F14.3, F14.3, F14.3)' Printf, Lun_Val ; print blank space to separate data for ; different images Continue Endif ; the first group is the zero-level for the dark current, so adjust ; the grouptimes to be relative to the time of the first group FirstGroupNum = Groupnum StartTime = GroupTimes[FirstGroupNum] GroupTimes = GroupTimes - StartTime ; find out where the railed pixels are RailedPix = where(FirstGroup gt 32760 OR FirstGroup lt -32760) ; exit the procedure if every pixel in the read is railed If (n_elements(Railedpix) eq n_elements(Firstgroup)) then begin stop, 'Processing cannot continue because every pixel in input ' + $ 'image is railed at the top or bottom of the A-D range.' Endif ; declare array to hold median and mode values TheMode = (theMedian = fltarr(NumGroups)) ; declare array to hold raw median signal for each read group RawSig = fltarr(NumGroups) RawSig[FirstGroupNum] = median(Firstgroup[Region[0]:Region[1]:ColInc, $ Region[2]:Region[3]:RowInc]) if (FirstGroupNum ne 0) then RawSig[0:FirstGroupNum - 1] = -32768 ; set up array used to hold previous read for cosmic ray detection Previousgroup = fltarr(Xsize,Ysize) ;Zero the Cosmic Ray Arrays Mask10Sig[*] = 0 CosmicRays[*] = 0 ; loop through the reads of an individual input file for Groupcount = FirstGroupNum + 1, Numgroups - 1 do begin print,'Reading group number ',GroupCount ; read all the frames composing one sample group Fits_Read, Testdir + ImgFiles[ImgCount], SCAGroup, $ first = (GroupEnds[GroupCount - 1] + 1) * NumPixRd, $ last = (GroupEnds[GroupCount] + 1) * NumPixRd - 1 ; transform the group of reads into an average Framecount = GroupEnds[GroupCount] - GroupEnds[GroupCount - 1] SCAgroup = reform(float(SCAGroup), Xsize, Ysize, FrameCount) SCAgroup = total(SCAGroup, 3) / FrameCount ; record the median signal RawSig[GroupCount] = Median(SCAGroup[Region[0]:Region[1]:ColInc, $ Region[2]:Region[3]:RowInc]) ; subtract off the first group as bias correction SCAGroup = SCAGroup - FirstGroup ; if it was requested, perform reference pixel correction on all ; reads If (not keyword_set(NoRef)) then begin print, 'Applying reference pixel correction to ' + $ ImgFiles[ImgCount] + ', read # ' + strtrim(string(GroupCount),2) if (not keyword_set(Ma_RefCor)) then begin RefSub, SCAGroup, scaName=SCAName,/plot endif else begin RefSub, SCAGroup, scaName=SCAName, /simple endelse Endif Else Begin print, 'No ref. pixel correction for ' + $ ImgFiles[ImgCount] + ', read #' + strtrim(string(GroupCount),2) endelse ; do cosmic ray detection DiffFrame = SCAGroup - PreviousGroup CRSDev = stddev(DiffFrame[4:Xsize-5, 4:Ysize-5]) CRMed = median(DiffFrame[4:Xsize-5, 4:Ysize-5]) Outliers = where(DiffFrame gt (CRMed + CRSDev*10)) Fits_Write, OutDir+'TestDiff.fits', DiffFrame stop if (Outliers[0] ne -1) then begin Mask10Sig[Outliers] = Mask10sig[Outliers] + 1 CosmicRays[Outliers] = DiffFrame[Outliers] endif PreviousGroup = SCAGroup ; do the incremental slope calculation operations Sxy = Sxy + GroupTimes[GroupCount] * SCAGroup Sx = Sx + GroupTimes[GroupCount] Sy = Sy + SCAGroup Sxx = Sxx + GroupTimes[GroupCount] ^ 2 ; extract the region of interest from the frame and apply the mask ; (which has already been cut down to the size of the region) SCA_Roi = SCAGroup[Region[0]:Region[1]:Colinc, $ Region[2]:Region[3]:Rowinc] SCA_Mask = SCA_Roi[where(Region_Mask eq 1)] ; begin the process of finding signal values for individual reads ; begin by getting the median and stddev using iterative sigma ; clipping algorithm. DJS_Iterstat, SCA_Mask, sigrej=4.0, sigma=DJSig, median=DJMed TheMedian[GroupCount] = DJMed ; We want to find the mode. The easiest way to do this is to fit a ; gaussian to a histogram. ; set min and max histogram bins, centered around the median of the ; data _Min = floor(DJMed - (DJSig * 4)) + 0.5 _Max = floor(DJMed + (DJSig * 4)) - 0.5 _nbins = _max - _min ; set up error handler to catch and deal with any errors ; caused by gaussfit procedure. math_err_stat = check_math(mask = 208) math_errcount = 0 catch, errval if (errval ne 0) then begin ; if there is a math error which has been thrown manually ; by a call to the message procedure, reduce the number of bins ; and retry if (strpos(!error_state.msg, 'math error') ne -1) then begin _nbins = _nbins / 2 message, /reset math_errcount = math_errcount + 1 endif else begin ; if this is an unexpected non-math error, cancel the ; error handler and retry, allowing the error to be ; handled by the default IDL handler (which should exit the ; procedure). catch, /cancel endelse endif ; make a histogram from the masked data in the region of interest. theHist = histogram(sca_mask, nbins=_nbins, min=_min, max=_max, /nan, locations = theVals) ; adjust values to center of bins theVals = theVals + ((_max - _min) / float(_nbins - 1)) / 2.0 ; fit the histogram counts and values to a gaussian theResult = gaussfit(theVals, theHist, A) math_err_stat = check_math(mask = 208) if (math_err_stat ne 0 and math_errcount lt 5) then message, 'math error' ; we want the mode, which is element 1 of the A array returned from ; gaussfit print, math_errcount, a[1] TheMode[groupcount] = A[1] endfor ; make an array to hold the output combination of group time and ; corresponding mode value and raw signal OutCombo = fltarr(3, n_elements(TheMode)) OutCombo[0, *] = GroupTimes + StartTime OutCombo[1, *] = TheMode OutCombo[2, *] = RawSig ; write out time and signal values for each read, ; darkcurrent_analyze can be called later to make slope plots. printf, lun_val, testdir+imgfiles[imgcount] + ' ' + strtrim(string(numgroups), 2) + ' ' + strtrim(string(groupfactor), 2) printf, lun_val, outcombo, format='(F14.3, F14.3, F14.3)' printf, lun_val ; print blank space to separate data for different images ; calculate the final per-pixel slope values outarray = (numgroups * Sxy - Sx * Sy) / (numgroups * Sxx - Sx * Sx) ; change output array to float to make output FITS file smaller outarray = float(outarray) ; set the detected cosmic rays/hot pixels to NaN if (mask10sig[0] ne -1) then begin crpix = where(mask10sig ne 0) if (crpix[0] ne -1) then outarray[crpix] = !values.f_nan endif ; correct values in the original header to indicate 1 frame of float ; values sxaddpar, imghdr, 'naxis3', 1 sxaddpar, imghdr, 'bitpix', -32 sxaddpar, imghdr, 'refver', ref_ver sxaddpar, imghdr, 'reftype', ref_type ; write out slope array with filename equal to original filename ; with '_slope' inserted prior to '.fits' NameParts = strsplit(imgfiles[imgcount], '.', /extract) OutName = strjoin(nameparts[0:n_elements(nameparts)-2], '.') + '_slope.fits' CosName = strjoin(NameParts[0:n_elements(NameParts)-2], '.') + '_cosmics.fits' print,'Writing file ',OutDir+OutName Fits_Write, Outdir + Outname, OutArray, ImgHdr print,'Writing file ',Outdir+CosName Fits_Write, Outdir + Cosname, CosmicRays, ImgHdr ; enter the output name and detector temperature (rounded to nearest ; 0.1 K) into imginfo array ImgInfo[ImgCount].name = OutName ImgInfo[ImgCount].dettemp = string(DetTemp, format='(F5.1)') endfor ; get rid of null file names (representing images that are railed in every read) validnames = where(imginfo.name ne '', numvalid) if (numvalid gt 0) then begin imginfo = imginfo[validnames] ; open output file for names of slope images openw, lun_img, outdir + imgoutfile, /get_lun ; sort the imginfo struct array by the detector temperature field imginfo = imginfo[sort(imginfo.dettemp)] ; find the lengths of all the filenames and set the length of the field for ; all names to the maximum value + 5 characters (for output formatting) namelen = strlen(imginfo.name) fieldlen = max(namelen) + 5 for i=0, n_elements(imginfo) - 1 do begin imginfo[i].name = imginfo[i].name + string(make_array(fieldlen - strlen(imginfo[i].name), /byte, val=32b)) endfor ; add EOL character(s) to output dettemp so that output will not all be on ; the same line imginfo.dettemp = imginfo.dettemp + endofline ; write the imginfo struct array out to the image list file writeu, lun_img, imginfo.name + endofline free_lun, lun_img endif ; close the output files free_lun, lun_val End