Processing of data from JAN00 PFU+MITLL3 run. ===================================================================== processing summary ........ All data was taken in SPEED normal with the MITLL3 CCD (15um pixels) and the AAT triplet corrector. This gives an image scale of 0.228"/pixel of 15.56' x 7.78' field of view. It will have a small amount of pincushion distortion (it should reach about 1.4% at 30' radius, so be considerably smaller in the single MITLL3 FOV.) Gain = 1.1e/adu and read noise = 2e-. Images were taken in a variety of windows, but the only ones of note are MITLL_FULL (2kx4K) and MITLL_SQUARE (2Kx2K in the centre of the CCD). Orientation of the images on the sky is N to the right, E to the top. Filters used were the 165x165mm square Schott glass filters constructed for PFU use (numbers 48-52 from the AAo Filter catalogue http://www.aao.gov.au/local/www/cgt/ccdimguide/filtercat.html) and one of the TTF red blocking filters R8 (#86 from the catalogue). The PFU filters had not been AR coated, and the I filter had not had its long-wavelength cut-off applied, so it was really a combined IZ filter with response determined by the cut-on of RG9 and the cut-off of the MITLL3). Data was taken in U only to examine instrument throughput. Not flats were obtained and the U data has not been reduced. Landolt Standards were observed on at least one night, and these should be reduced to determine colour terms for these filters. The night of 28 jan 2000 is believed to have been photometric based on quick looks at the data at the telescope. You can find scanned pages from my handwritten log in the directory logsheets/log*.jpg. You can create your own versions of the log from the AAT archive for each night at http://site.aao.gov.au/AATdatabase/aat/log_book.html You can read the reports on the observing run created as I was going at http://www.aao.gov.au/local/www/cgt/wfi/commission1.html. This page also contains links to the handwritten logs. *** All data was bias subtracted taking into account a small amount of structure seen in the vertical direction in the overscans. The vertical structure in the overscan of each image was extracted and a polynomial fit to it. This was then subtracted from each image. Bias subtraction should be good to << 1e over large regions of each image. Files renamed => b{28,29,30,31}jan????.sdf *** There are numerous bad columns and hot pixels. These are not well corrected by subtracting biases, so they are still present in the processed data. Sample biases are in reduction_files/bias_30jan.sdf reduction_files/bias_31jan.sdf These are provided for information ... I didn't actually subtract them as part of the processing. *** The shutter used on this run leaked light - both around the shutter during exposures at ~1% level and around/through the shutter during read out. This means that we could NOT use twilight sky frames to make flat fields. We could however use dome flats, since we could turn the dome lamps OFF during read-out to reduce contamination. Several tests were made of various flat recipes, the final flats adopted are -rw-r--r-- 1 cgt 33561600 Apr 13 15:57 reduction_files/bflat.sdf -rw-r--r-- 1 cgt 33561088 Apr 13 16:17 reduction_files/vflat.sdf -rw-r--r-- 1 cgt 33561088 Apr 26 16:16 reduction_files/r8flat.sdf -rw-r--r-- 1 cgt 33561088 Apr 26 15:40 reduction_files/rflat.sdf -rw-r--r-- 1 cgt 33561088 Apr 26 16:04 reduction_files/iflat.sdf Files renamed => db{28,29,30,31}jan????.sdf *** The files were renamed to put a filter identification flag into the file names. Files renamed => db{28,29,30,31}jan????{b,v,r,i,r8}.sdf *** The files were modified to put the correct exposure times in their headers. because this was an interim system, we controlled CCD readout and shutter timing seperately. In the modified files the FITS Keyword EXPOSED is the shutter open time, and the keywords ELAPSED is the CCD exposure time. Use EXPOSED as the exposure time of these images. *** I-band files were then fringe corrected. This took some playing around. An acceptable fringe frame was obtained by taking all the I-band frames NOT taken at similar positions and (1) subtracting off the sky level in a region free of bright stars in all these frames, (2) normalising the result by their exposure times, and (3) medianning. (Ideally a second pass would have normalised to this first guess by the data itself, not the exposure times, however this did not prove necessary). Then each image to be fringe corrected had its sky level in the same sample region subtracted, the fringe frame was divided out, and the normalisation factor in the sample region derived. This factor was then multiplied by the fringe frame, and this subtracted of the flattened image. The resulting fringe subtracted images show no systemtic fringing when visually examined, so fringing should be removed to well below the photon counting noise. Files renamed => fdb{28,29,30,31}jan????i.sdf Chris Tinney 9/5/00 cgt@aaoepp.aao.gov.au PS: apologies for the delay. Since this is a 'lash up' version of a new observing configuration, I wanted to work out how to reduce this data myself, before distributing it. ===================================================================== processing notes ........ Data is on DAT tape, in four tar files, and takes up 4.6Gb. 1240930 000129 1104595 000130 1048939 000131 1223764 000128 rawtape.lis is a listing of the rawdata filenames. Processing steps (1) Convert all files to Floats, which has to be done in steps. rm -r 0001*/cursor.dat chmod -x 0*/*.sdf cd mir5 mkdir PFUJAN00 cd mir4 mkdir PFUJAN00 mkdir float cd float mkdir 000129 mkdir 000130 ln -s ~/mir5/PFUJAN00 000128 ln -s ~/mir4/PFUJAN00 000131 foreach i ( 000128/*.sdf 000131/*.sdf ) retype $i:r float float/$i:r end Once this completes successfully, we can delete the USHORT versions on mir2, which should leave enough space to convert the rest of the data rm 000128/*.sdf 000131/*.sdf foreach i ( 000129/*.sdf) retype $i:r float float/$i:r end rm 000129/*.sdf foreach i ( 000130/*.sdf) retype $i:r float float/$i:r end rm 000130/*.sdf rm -r 0001* *** Windows ... the following windows were used foreach i ( float/*/*.sdf ) fitskeys $i:r WINDOW | head -1 | awk '{print $2}' end rm windows.lis foreach i ( float/*/*.sdf ) echo $i:r `fitskeys $i:r | grep WINDOW | head -1 | awk '{print $2}'` >> windows.lis end copies of which can be found at awk '{print $2}' windows.lis | sort | uniq MITLL_ACQ X:701-1348 Y:1729-2373 + overscan Used on a couple of nights. Can be deleted except for float/000128/28jan0015 'first light'. MITLL_CENTRE X:514-1537 Y:1537-2560 + overscan Only used for set-up on the first night. Moved to 'first light' MITLL_FULL X:1-2048 Y:1-4096 + overscan Used for data. MITLL_KPNO X:551-1550 Y:1551-2550 + overscan Used for flexure tests on 31 Jan. Moved to 'flexure tests' MITLL_SQUARE X:1-2048 Y:1025-3072 + overscan. Used for standards & data. So after re-arranging this data we have only files in the MITLL_FULL and MITLL_SQUARE windows. ============================================================== Bias subtract.... bias.csh will bias process the files.... but before using it, we need to check to make sure the biases are OK. Seems to perform OK. We have between 2 and 13 adu/pixel contamination by scattered light in a 10s exposure plus read when the shutter is never opened at night. The contamination ramps up in the readout direction, as expected if light continues to leak in as the chip is read out. By 30jan with dome lights off, this is only a few adu. However, interestingly I see that the overscan regions are not flat in the Y direction, with slopes, curves etc of about 1-3 adu p-p. So unusually for AAO CCD/Controllers, we need to subtract the overscan with structure. The bias.csh has been modified to do this. It subtracts a polynomial fit to the overscan. ============================================================== 12 April 2000 Backed up real images to DDS3 tape CGTAR400 file (1) Then leave bias subtraction job to run later tonight sleep 14400 ; ./bias.csh -k float/0001*/??jan*.sdf ============================================================== 13 April 2000 Check the bias subtracted files. Then make flat fields. Made biases from 30jan and 31jan data (see bias_30jan.lis and bias_31jan.lis) Medianned these seperately into bias_30jan.sdf and bias_30jan.sdf The 'defects' on the CCD are 1) about 6 bright (saturated or very bright => useless) columns near X=114 2) two bright columns (200 above bias) trailing from a defect (1214,437) 3) two bright columns (1000-200 above bias) trailing from a defect (1295, 209) 4) two bright columns (500 above bias) trailing from a defect (1317, 155) 5) faint column (10-20 above bias) trailing from a defect (1157, 1233) 6) bright fading column (50-0 above bias) trailing from a defect (733, 932) Plus nmerous much weaker defects producing trailing - these ar listed on the report on comsteics on the MITLL3 WWW page. In data with even only a few hundred counts, the weak defects don't appear to be visible. Though charge transfer may be poor along these columns. The weaker features do bias subtract from each other, though the defect pixels are usually left behind. I have not subtracted these bias frames. However they should be useful for creating bad pixel masks for the images. ============================================================== 13 April 2000 Back up biassed images to DDS3 tape CGTAR400 file (2) Start making flat fields. Flat fielding will be non-trivial, because the camera and shutter were so leaky. The best flats I obtained were almost certainly the dome flats, where I could turn the dome lights on, ONLY during an exposure. Useful flats taken in this mode are 30jan0058-60 B 30jan0061-63 I 30jan0064-66 R8 31jan0008,10,11 B 31jan0009 B But through lights turned on, shutter not opened, so this tells us how much light is leaking AROUND shutter instead of going through front of camera. This is about 50-230 adu for a 50s light-on period, compared to the 50s light-on shutter-open counts of 39000adu. 31jan0012,14,15 V 31jan0013 B But through lights turned on, shutter not opened, so this tells us how much light is leaking AROUND shutter instead of going through front of camera. This is about 50-230 adu for a 50s light-on period, 31jan0016-18 R 31jan0019 R But through lights turned on, shutter not opened, so this tells us how much light is leaking AROUND shutter instead of going through front of camera. This is about 3-14 adu for a 50s light-on period, *** B average noflist nf=3 out=bflat1 Enter frame 1 file name - float/000131/b31jan0008 Enter frame 2 file name - float/000131/b31jan0010 Enter frame 3 file name - float/000131/b31jan0011 isub bflat1 float/000131/b31jan0009 bflat2 istat bflat1 xs=280 xe=500 ys=1070 ye=1370 median icdiv bflat1 stat_mean bflat1 istat bflat2 xs=280 xe=500 ys=1070 ye=1370 median icdiv bflat2 stat_mean bflat2 We also have sky flats (94-96) taken in twilight on 28jan. 96 has too much of a light leak, and its exposure is too short compared to the readout time. average noflist nf=2 foreach i ( float/000128/b28jan009[456].sdf) set j = $i:t istat $i:r xs=280 xe=500 ys=1070 ye=1370 median icdiv $i:r stat_median n$j:r end ls nb*.sdf > bskys.lis medsky file=bskys.lis noscale out=bflat3 Now test both of these on some data ... 31jan idiv float/000131/b31jan0026 bflat1 test1 idiv float/000131/b31jan0026 bflat2 test2 idiv float/000131/b31jan0026 bflat3 test3 bflat1 and bflat2 remove brickwall pattern to a level of 1%. Though its still weakly there and still noticeable. The 'edge effects' produced by the leakage around the shutter seem to be negligible, so bflat1 can be used. bflat3 leaves no brickwall, but a 1% left hand edge effect. 30jan idiv float/000130/b30jan0043 bflat1 test1 idiv float/000130/b30jan0043 bflat2 test2 idiv float/000130/b30jan0043 bflat3 test3 brickwall pattern here is 2% p-p. there is no differenmce in the correction for the 'edge' effect on the left hand side, which is more visible in this data, between bflat1 and bflat2. bflat3 looks great. 28jan idiv float/000128/b28jan0073 bflat1 test1 idiv float/000128/b28jan0073 bflat2 test2 idiv float/000128/b28jan0073 bflat3 test3 brickwall pattern here is 1.5% p-p. Once again bflat2 does not correct left hand edge problem. bflat3 looks great. I will use bflat3 as the 'prefered' B band flat. *** V average noflist nf=3 out=vflat1 Enter frame 1 file name - float/000131/b31jan0012 Enter frame 2 file name - float/000131/b31jan0014 Enter frame 3 file name - float/000131/b31jan0015 isub vflat1 float/000131/b31jan0013 vflat2 istat vflat1 xs=280 xe=500 ys=1070 ye=1370 median icdiv vflat1 stat_mean vflat1 istat vflat2 xs=280 xe=500 ys=1070 ye=1370 median icdiv vflat2 stat_mean vflat2 31jan idiv float/000131/b31jan0023 vflat1 test1 idiv float/000131/b31jan0023 vflat2 test2 Both look good - marginally prefer bflat2 28jan idiv float/000129/b29jan0023 vflat1 test1 idiv float/000129/b29jan0023 vflat2 test2 Seems OK. Adopt vflat2.sdf *** R 31jan0016-18 R 31jan0019 R But through lights turned on, shutter not opened, so this tells us how much light is leaking AROUND shutter instead of going through front of camera. This is about 3-14 adu for a 50s light-on period, average noflist nf=3 out=rflat1 Enter frame 1 file name - float/000131/b31jan0016 Enter frame 2 file name - float/000131/b31jan0017 Enter frame 3 file name - float/000131/b31jan0018 isub rflat1 float/000131/b31jan0019 rflat2 istat rflat1 xs=280 xe=500 ys=1070 ye=1370 median icdiv rflat1 stat_mean rflat1 istat rflat2 xs=280 xe=500 ys=1070 ye=1370 median icdiv rflat2 stat_mean rflat2 Test these out. 28jan idiv float/000128/b28jan0059 rflat1 test1 idiv float/000128/b28jan0059 rflat2 test2 29jan idiv float/000129/b29jan0019 rflat1 test1 idiv float/000129/b29jan0019 rflat2 test2 31jan idiv float/000131/b31jan0032 rflat1 test1 idiv float/000131/b31jan0032 rflat2 test2 Both test1 and test2 look OK. Since leak at R seems small prefer rflat1 *** I 30jan0061-63 I average noflist nf=3 out=iflat Enter frame 1 file name - float/000130/b30jan0061 Enter frame 2 file name - float/000130/b30jan0062 Enter frame 3 file name - float/000130/b30jan0063 istat iflat xs=280 xe=500 ys=1070 ye=1370 median icdiv iflat stat_mean iflat idiv float/000128/b28jan0076 iflat test1 idiv float/000129/b29jan0032 iflat test2 idiv float/000130/b30jan0028 iflat test1 idiv float/000130/b30jan0040 iflat test2 The resulting frames have considerable fringing (2% level). *** R8 30jan0064-66 R8 average noflist nf=3 out=r8flat Enter frame 1 file name - float/000130/b30jan0064 Enter frame 2 file name - float/000130/b30jan0065 Enter frame 3 file name - float/000130/b30jan0066 istat r8flat xs=280 xe=500 ys=1070 ye=1370 median icdiv r8flat stat_mean r8flat idiv float/000130/b30jan0033 r8flat test1 The resulting frames have considerable fringing (5% level). **** Now to apply these flats we not only need to know which flat goes with which file, but also whether a subsetted flat is needed. That is if we have window MITLL_SQUARE or MITLL_FULL. o flats we have are for MITLL_FULL. o make {b,v,r,i,r8}flat_square.sdf also. foreach i ( reduction_files/{b,v,r,i,r8}flat.sdf ) isubset $i:r xs=1 xe=2048 ys=1025 ye=3072 out=${i:r}_square end Then create reduction_files/flatten.csh to do the flattening, which will rely on a list of files and filters in flatten.dat Then do the flattening .... *** Check flattening has worked well. All files visuall inspected and OK. Though 29jan35-39 have significant scattered light problems, due to moon being less than 10 degrees away. *** Rename files to put filter names in filenames. cd flattened /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/rename.csh *** Insert correct exposure time information in all the files. /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/settimes.csh *** Now need to play with fringe frame correction. 28JAN00 Get a list of useful fringe frame files in fringe1.lis No fringing in 70-72. Fringing in 75-80 average (FLIST) Input file names are in a file ? [NO] - y (FILE) File containing list of images or spectra [bskys.lis] - fringe1.lis Averaging 6 frames. (OUTput) The file containing the average of the inputs [test3] - test1 Examine and identify a clean region rm makesky.lis foreach i (`cat fringe1.lis`) istat $i:r ys=1238 ye=1452 xs=1334 xe=1656 median icsub $i:r stat_median s$i:r myclip s$i:r lowclip=-1000 highclip=1000 lowbad highbad out=s$i:r echo s$i:r >> makesky.lis end medsky file=makesky.lis nosc out=fringe_guess1 This produces a reasonably clean fringemap. Next try this to make maps for the other two nights, then see if their maps can correct each other (ie is a 'global' map useful). rm makesky.lis foreach i (`cat fringe2.lis`) istat $i:r ys=1238 ye=1452 xs=1334 xe=1656 median icsub $i:r stat_median s$i:r myclip s$i:r lowclip=-1000 highclip=1000 lowbad highbad out=s$i:r echo s$i:r >> makesky.lis end medsky file=makesky.lis nosc out=fringe_guess2 rm makesky.lis foreach i (`cat fringe3.lis`) istat $i:r ys=1238 ye=1452 xs=1334 xe=1656 median icsub $i:r stat_median s$i:r myclip s$i:r lowclip=-1000 highclip=1000 lowbad highbad out=s$i:r echo s$i:r >> makesky.lis end medsky file=makesky.lis nosc out=fringe_guess3 Results : fringe_guess[123] seem to do a reasonable job of subtracting each other. The noticeable residuals between the frames are actually the residuals of bright stars left over from the medianning process. A quick check with all the data shows that medianning all the files actually does a pretty bood job of subtracting the fringes off. However, I have neglected to normalise the fringe frames for their exposure times, or to normalise what I subtract off to the exposure time of the science frame. Though the 'brute force' technique above does an acceptable job, I should try to do it properly. rm makesky.lis cat fringe[123].lis > fringe.lis foreach i (`cat fringe.lis`) set exposed = `fitskeys $i:r | grep EXPOSED | awk '{print $2}'` icdiv s$i:r $exposed s$i:r echo s$i:r >> makesky.lis end medsky file=makesky.lis nosc out=fringe_norm However, when it comes to applying this fringe frame, you can't just normalise by exposure time ... it doesn't work. However, try normalising by the level of the fringes themselves. This works ... even on frames with no fringing noticeable, we get a negligible fringe frame correction. list the files to be corrected in fringe_correct.lis foreach i ( `cat /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/fringe_correct.lis` ) echo istat $i:r ys=1238 ye=1452 xs=1334 xe=1656 median istat $i:r ys=1238 ye=1452 xs=1334 xe=1656 median echo icsub $i:r stat_median test icsub $i:r stat_median test echo idiv test /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/fringe_norm test1 idiv test /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/fringe_norm test1 echo istat test1 ys=1238 ye=1452 xs=1334 xe=1656 median istat test1 ys=1238 ye=1452 xs=1334 xe=1656 median echo icmult /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/fringe_norm stat_median tmp icmult /mir2/cgt/PFU_MITLL3_JAN00/reduction_files/fringe_norm stat_median tmp echo isub $i:r tmp f$i:r isub $i:r tmp f$i:r end rm tmp.sdf test.sdf test1.sdf Tmp*.sdf NB: we don't bother applying fringe frame corrections to the standard star frames, since they have negligible amounts of fringing. *** Then split data up for the various service observers. Each observer gets README reduction_files ok standards (raw and flattened) flattened ok calibrations (raw) (flatfields, darks etc) fringe_data (raw) data (raw and flattened and fringe corrected) Observers are C259 flattened/fringed ok C256 flattened/fringed ok C255 flattened/fringed ok C258 flattened/fringed ok dfm_sl raw not needed flattened/fringed ok cgt raw not needed flattened/fringed ok All raw data converted to BITPIX=16 FITS files and compressed. *** Backup final data structure to TAPE. *** Convert to FITS and distribute. ============================================================== #!/bin/csh # bias.csh # if ( $1 == '-k' ) then shift set del = "y" else set del = "n" endif foreach i ( $* ) set root = $i:r set head = $root:h set tail = $root:t set ifile = $i:r set ofile = $head/b$tail fitskeys $i | grep WIN > /tmp/cgt_bias.dat set win = `grep WINDOW /tmp/cgt_bias.dat | awk '{print $2}'` echo "Bias subtracting $i:r - WINDOW=$win" set xs = `grep WINDOXS1 /tmp/cgt_bias.dat | awk '{print $2}'` set xe = `grep WINDOXE1 /tmp/cgt_bias.dat | awk '{print $2}'` set ys = `grep WINDOYS1 /tmp/cgt_bias.dat | awk '{print $2}'` set ye = `grep WINDOYE1 /tmp/cgt_bias.dat | awk '{print $2}'` set oxs = `grep WINDOXS2 /tmp/cgt_bias.dat | awk '{print $2}'` set oxe = `grep WINDOXE2 /tmp/cgt_bias.dat | awk '{print $2}'` echo " X:$xs - $xe Y:$ys - $ye OX:$oxs - $oxe" if ( $win == 'MITLL_SQUARE' ) then set osxs = 2055 set osxe = 2068 set osys = 100 set osye = 1900 set xs=1 set xe=2048 set ys=1 set ye=2048 ~/bin_solaris/istat $ifile xs=$osxs xe=$osxe ys=$osys ye=$osye set num = `echo $osxs $osxe | awk '{print $2-$1+1}'` ystract $ifile xs=$osxs xe=$osxe sp=tmp1 echo ystract $ifile $osxs xe=$osxe tmp1 icdiv tmp1 $num tmp1 sfit tmp1 or=2 nologs out=tmp2 splot tmp1 au wh er col=y \\ splot tmp2 noau nowh noax noer col=r \\ isysub $ifile tmp2 $ofile echo isubset $ofile xs=$xs xe=$xe ys=$xs ye=$ye out=$ofile echo trimfile $ofile isubset $ofile xs=$xs xe=$xe ys=$xs ye=$ye out=$ofile trimfile $ofile echo " " if ( $del == "y" && -e $ofile.sdf ) then echo rm $i rm $i endif echo " " else if ( $win == 'MITLL_FULL' ) then set osxs = 2070 set osxe = 2110 set osys = 100 set osye = 4000 set xs=1 set xe=2048 set ys=1 set ye=4096 ~/bin_solaris/istat $ifile xs=$osxs xe=$osxe ys=$osys ye=$osye set num = `echo $osxs $osxe | awk '{print $2-$1+1}'` ystract $ifile xs=$osxs xe=$osxe sp=tmp1 echo ystract $ifile xs=$osxs xe=$osxe out=tmp1 icdiv tmp1 $num tmp1 sfit tmp1 or=2 nologs out=tmp2 splot tmp1 au wh er col=y \\ splot tmp2 noau nowh noax noer col=r \\ isysub $ifile tmp2 $ofile echo isubset $ofile xs=$xs xe=$xe ys=$xs ye=$ye out=$ofile echo trimfile $ofile isubset $ofile xs=$xs xe=$xe ys=$xs ye=$ye out=$ofile trimfile $ofile echo " " if ( $del == "y" && -e $ofile.sdf ) then echo rm $i rm $i endif else echo "*****************************************" echo "$i:r CANNOT BE BIAS SUBTRACTED OR TRIMMED" echo "*****************************************" echo " " endif end ============================================================== #!/bin/csh #flatten.csh if ( $1 == '-k' ) then shift set del = "y" else set del = "n" endif foreach i ( $* ) set root = $i:r set head = $root:h set tail = $root:t set ifile = $i:r # # Note results are written to flattened/*! # set ofile = flattened/d$tail if { grep -s $ifile reduction_files/flatten.dat >>& /dev/null } then set filt = `grep $ifile reduction_files/flatten.dat | head -1 | awk '{print $2}'` fitskeys $i | grep WIN > /tmp/cgt_bias.dat set win = `grep WINDOW /tmp/cgt_bias.dat | awk '{print $2}'` echo "Flattening $ifile - WINDOW=$win" if ( $win == 'MITLL_SQUARE' ) then echo idiv $ifile reduction_files/${filt}flat_square $ofile idiv $ifile reduction_files/${filt}flat_square $ofile if ( $del == "y" && -e $ofile.sdf ) then echo rm $i rm $i endif echo " " else if ( $win == 'MITLL_FULL' ) then echo idiv $ifile reduction_files/${filt}flat $ofile idiv $ifile reduction_files/${filt}flat $ofile if ( $del == "y" && -e $ofile.sdf ) then echo rm $i rm $i endif echo " " endif else echo "**************************************************" echo "Skipping $i:r - not found in flatten.dat" echo "**************************************************" endif end ============================================================== #!/bin/csh #rename.csh mv db28jan0016.sdf db28jan0016i.sdf mv db28jan0017.sdf db28jan0017r.sdf mv db28jan0018.sdf db28jan0018v.sdf mv db28jan0019.sdf db28jan0019b.sdf mv db28jan0023.sdf db28jan0023b.sdf mv db28jan0024.sdf db28jan0024b.sdf mv db28jan0027.sdf db28jan0027v.sdf mv db28jan0028.sdf db28jan0028v.sdf mv db28jan0029.sdf db28jan0029v.sdf mv db28jan0030.sdf db28jan0030v.sdf mv db28jan0031.sdf db28jan0031r.sdf mv db28jan0032.sdf db28jan0032r.sdf mv db28jan0033.sdf db28jan0033i.sdf mv db28jan0034.sdf db28jan0034i.sdf mv db28jan0041.sdf db28jan0041i.sdf mv db28jan0042.sdf db28jan0042r.sdf mv db28jan0043.sdf db28jan0043v.sdf mv db28jan0044.sdf db28jan0044b.sdf mv db28jan0046.sdf db28jan0046v.sdf mv db28jan0047.sdf db28jan0047v.sdf mv db28jan0048.sdf db28jan0048v.sdf mv db28jan0049.sdf db28jan0049v.sdf mv db28jan0050.sdf db28jan0050v.sdf mv db28jan0051.sdf db28jan0051v.sdf mv db28jan0052.sdf db28jan0052b.sdf mv db28jan0053.sdf db28jan0053b.sdf mv db28jan0054.sdf db28jan0054b.sdf mv db28jan0055.sdf db28jan0055v.sdf mv db28jan0056.sdf db28jan0056v.sdf mv db28jan0057.sdf db28jan0057v.sdf mv db28jan0058.sdf db28jan0058r.sdf mv db28jan0059.sdf db28jan0059r.sdf mv db28jan0060.sdf db28jan0060r.sdf mv db28jan0062.sdf db28jan0062b.sdf mv db28jan0063.sdf db28jan0063b.sdf mv db28jan0064.sdf db28jan0064v.sdf mv db28jan0065.sdf db28jan0065v.sdf mv db28jan0066.sdf db28jan0066r.sdf mv db28jan0067.sdf db28jan0067i.sdf mv db28jan0069.sdf db28jan0069i.sdf mv db28jan0070.sdf db28jan0070i.sdf mv db28jan0071.sdf db28jan0071i.sdf mv db28jan0072.sdf db28jan0072i.sdf mv db28jan0073.sdf db28jan0073b.sdf mv db28jan0074.sdf db28jan0074b.sdf mv db28jan0075.sdf db28jan0075i.sdf mv db28jan0076.sdf db28jan0076i.sdf mv db28jan0077.sdf db28jan0077i.sdf mv db28jan0078.sdf db28jan0078i.sdf mv db28jan0079.sdf db28jan0079i.sdf mv db28jan0080.sdf db28jan0080i.sdf mv db28jan0081.sdf db28jan0081b.sdf mv db28jan0082.sdf db28jan0082b.sdf mv db28jan0083.sdf db28jan0083b.sdf mv db28jan0084.sdf db28jan0084v.sdf mv db28jan0085.sdf db28jan0085v.sdf mv db28jan0086.sdf db28jan0086r.sdf mv db28jan0087.sdf db28jan0087r.sdf mv db28jan0088.sdf db28jan0088i.sdf mv db28jan0089.sdf db28jan0089i.sdf mv db29jan0010.sdf db29jan0010b.sdf mv db29jan0011.sdf db29jan0011b.sdf mv db29jan0012.sdf db29jan0012b.sdf mv db29jan0013.sdf db29jan0013v.sdf mv db29jan0014.sdf db29jan0014v.sdf mv db29jan0015.sdf db29jan0015v.sdf mv db29jan0016.sdf db29jan0016r.sdf mv db29jan0017.sdf db29jan0017r.sdf mv db29jan0018.sdf db29jan0018r.sdf mv db29jan0019.sdf db29jan0019r.sdf mv db29jan0020.sdf db29jan0020r.sdf mv db29jan0021.sdf db29jan0021r.sdf mv db29jan0022.sdf db29jan0022r.sdf mv db29jan0023.sdf db29jan0023v.sdf mv db29jan0024.sdf db29jan0024v.sdf mv db29jan0025.sdf db29jan0025v.sdf mv db29jan0026.sdf db29jan0026b.sdf mv db29jan0027.sdf db29jan0027b.sdf mv db29jan0028.sdf db29jan0028b.sdf mv db29jan0029.sdf db29jan0029b.sdf mv db29jan0030.sdf db29jan0030i.sdf mv db29jan0031.sdf db29jan0031i.sdf mv db29jan0032.sdf db29jan0032i.sdf mv db29jan0033.sdf db29jan0033i.sdf mv db29jan0034.sdf db29jan0034i.sdf mv db29jan0035.sdf db29jan0035i.sdf mv db29jan0036.sdf db29jan0036i.sdf mv db29jan0037.sdf db29jan0037i.sdf mv db29jan0038.sdf db29jan0038i.sdf mv db29jan0039.sdf db29jan0039i.sdf mv db29jan0040.sdf db29jan0040b.sdf mv db29jan0041.sdf db29jan0041b.sdf mv db29jan0042.sdf db29jan0042b.sdf mv db29jan0043.sdf db29jan0043b.sdf mv db30jan0022.sdf db30jan0022b.sdf mv db30jan0023.sdf db30jan0023b.sdf mv db30jan0024.sdf db30jan0024b.sdf mv db30jan0025.sdf db30jan0025b.sdf mv db30jan0026.sdf db30jan0026b.sdf mv db30jan0027.sdf db30jan0027i.sdf mv db30jan0028.sdf db30jan0028i.sdf mv db30jan0029.sdf db30jan0029i.sdf mv db30jan0030.sdf db30jan0030r8.sdf mv db30jan0031.sdf db30jan0031i.sdf mv db30jan0032.sdf db30jan0032r8.sdf mv db30jan0033.sdf db30jan0033r8.sdf mv db30jan0034.sdf db30jan0034i.sdf mv db30jan0035.sdf db30jan0035i.sdf mv db30jan0036.sdf db30jan0036r8.sdf mv db30jan0037.sdf db30jan0037r8.sdf mv db30jan0038.sdf db30jan0038i.sdf mv db30jan0039.sdf db30jan0039i.sdf mv db30jan0040.sdf db30jan0040i.sdf mv db30jan0041.sdf db30jan0041i.sdf mv db30jan0042.sdf db30jan0042b.sdf mv db30jan0043.sdf db30jan0043b.sdf mv db30jan0044.sdf db30jan0044i.sdf mv db30jan0045.sdf db30jan0045i.sdf mv db30jan0046.sdf db30jan0046i.sdf mv db30jan0047.sdf db30jan0047i.sdf mv db30jan0048.sdf db30jan0048i.sdf mv db30jan0049.sdf db30jan0049i.sdf mv db30jan0050.sdf db30jan0050b.sdf mv db30jan0051.sdf db30jan0051b.sdf mv db30jan0052.sdf db30jan0052b.sdf mv db31jan0020.sdf db31jan0020b.sdf mv db31jan0021.sdf db31jan0021b.sdf mv db31jan0022.sdf db31jan0022v.sdf mv db31jan0023.sdf db31jan0023v.sdf mv db31jan0024.sdf db31jan0024v.sdf mv db31jan0025.sdf db31jan0025v.sdf mv db31jan0026.sdf db31jan0026b.sdf mv db31jan0027.sdf db31jan0027b.sdf mv db31jan0028.sdf db31jan0028v.sdf mv db31jan0029.sdf db31jan0029v.sdf mv db31jan0030.sdf db31jan0030v.sdf mv db31jan0031.sdf db31jan0031r.sdf mv db31jan0032.sdf db31jan0032r.sdf mv db31jan0033.sdf db31jan0033r.sdf mv db31jan0034.sdf db31jan0034r.sdf mv db31jan0035.sdf db31jan0035r.sdf mv db31jan0036.sdf db31jan0036r.sdf mv db31jan0037.sdf db31jan0037b.sdf mv db31jan0038.sdf db31jan0038b.sdf mv db31jan0039.sdf db31jan0039b.sdf mv db31jan0040.sdf db31jan0040v.sdf mv db31jan0041.sdf db31jan0041v.sdf mv db31jan0042.sdf db31jan0042v.sdf mv db31jan0043.sdf db31jan0043v.sdf mv db31jan0044.sdf db31jan0044v.sdf mv db31jan0045.sdf db31jan0045v.sdf mv db31jan0046.sdf db31jan0046b.sdf mv db31jan0047.sdf db31jan0047r.sdf mv db31jan0048.sdf db31jan0048r.sdf mv db31jan0049.sdf db31jan0049r.sdf mv db31jan0050.sdf db31jan0050r8.sdf mv db31jan0051.sdf db31jan0051r8.sdf mv db31jan0052.sdf db31jan0052r8.sdf mv db31jan0053.sdf db31jan0053r8.sdf mv db31jan0054.sdf db31jan0054r8.sdf mv db31jan0067.sdf db31jan0067b.sdf mv db31jan0068.sdf db31jan0068b.sdf ============================================================== #!/bin/csh #settimes.csh fitset db28jan0016i elapsed 224.0 \\ ; fitset db28jan0016i exposed 7.0 \\ fitset db28jan0017r elapsed 147.0 \\ ; fitset db28jan0017r exposed 7.0 \\ fitset db28jan0018v elapsed 153.0 \\ ; fitset db28jan0018v exposed 7.0 \\ fitset db28jan0019b elapsed 160.0 \\ ; fitset db28jan0019b exposed 10.0 \\ fitset db28jan0023b elapsed 15.0 \\ ; fitset db28jan0023b exposed 10 \\ fitset db28jan0024b elapsed 70.0 \\ ; fitset db28jan0024b exposed 60 \\ fitset db28jan0027v elapsed 70.0 \\ ; fitset db28jan0027v exposed 60 \\ fitset db28jan0028v elapsed 15.0 \\ ; fitset db28jan0028v exposed 10 \\ fitset db28jan0029v elapsed 15.0 \\ ; fitset db28jan0029v exposed 10 \\ fitset db28jan0030v elapsed 70.0 \\ ; fitset db28jan0030v exposed 60 \\ fitset db28jan0031r elapsed 70.0 \\ ; fitset db28jan0031r exposed 60 \\ fitset db28jan0032r elapsed 15.0 \\ ; fitset db28jan0032r exposed 10 \\ fitset db28jan0033i elapsed 15.0 \\ ; fitset db28jan0033i exposed 10 \\ fitset db28jan0034i elapsed 70.0 \\ ; fitset db28jan0034i exposed 60 \\ fitset db28jan0041i elapsed 15.0 \\ ; fitset db28jan0041i exposed 10 \\ fitset db28jan0042r elapsed 15.0 \\ ; fitset db28jan0042r exposed 10 \\ fitset db28jan0043v elapsed 15.0 \\ ; fitset db28jan0043v exposed 10 \\ fitset db28jan0044b elapsed 15.0 \\ ; fitset db28jan0044b exposed 10 \\ fitset db28jan0046v elapsed 315.0 \\ ; fitset db28jan0046v exposed 300 \\ fitset db28jan0047v elapsed 315.0 \\ ; fitset db28jan0047v exposed 300 \\ fitset db28jan0048v elapsed 315.0 \\ ; fitset db28jan0048v exposed 300 \\ fitset db28jan0049v elapsed 315.0 \\ ; fitset db28jan0049v exposed 300 \\ fitset db28jan0050v elapsed 315.0 \\ ; fitset db28jan0050v exposed 300 \\ fitset db28jan0051v elapsed 315.0 \\ ; fitset db28jan0051v exposed 300 \\ fitset db28jan0052b elapsed 310.0 \\ ; fitset db28jan0052b exposed 300 \\ fitset db28jan0053b elapsed 310.0 \\ ; fitset db28jan0053b exposed 300 \\ fitset db28jan0054b elapsed 310.0 \\ ; fitset db28jan0054b exposed 300 \\ fitset db28jan0055v elapsed 130.0 \\ ; fitset db28jan0055v exposed 120 \\ fitset db28jan0056v elapsed 130.0 \\ ; fitset db28jan0056v exposed 120 \\ fitset db28jan0057v elapsed 130.0 \\ ; fitset db28jan0057v exposed 120 \\ fitset db28jan0058r elapsed 110.0 \\ ; fitset db28jan0058r exposed 100 \\ fitset db28jan0059r elapsed 110.0 \\ ; fitset db28jan0059r exposed 100 \\ fitset db28jan0060r elapsed 110.0 \\ ; fitset db28jan0060r exposed 100 \\ fitset db28jan0062b elapsed 15.0 \\ ; fitset db28jan0062b exposed 10 \\ fitset db28jan0063b elapsed 15.0 \\ ; fitset db28jan0063b exposed 10 \\ fitset db28jan0064v elapsed 15.0 \\ ; fitset db28jan0064v exposed 10 \\ fitset db28jan0065v elapsed 15.0 \\ ; fitset db28jan0065v exposed 10 \\ fitset db28jan0066r elapsed 15.0 \\ ; fitset db28jan0066r exposed 10 \\ fitset db28jan0067i elapsed 15.0 \\ ; fitset db28jan0067i exposed 10 \\ fitset db28jan0069i elapsed 310.0 \\ ; fitset db28jan0069i exposed 300 \\ fitset db28jan0070i elapsed 460.0 \\ ; fitset db28jan0070i exposed 450 \\ fitset db28jan0071i elapsed 460.0 \\ ; fitset db28jan0071i exposed 450 \\ fitset db28jan0072i elapsed 460.0 \\ ; fitset db28jan0072i exposed 450 \\ fitset db28jan0073b elapsed 310.0 \\ ; fitset db28jan0073b exposed 300 \\ fitset db28jan0074b elapsed 310.0 \\ ; fitset db28jan0074b exposed 300 \\ fitset db28jan0075i elapsed 510.0 \\ ; fitset db28jan0075i exposed 500 \\ fitset db28jan0076i elapsed 510.0 \\ ; fitset db28jan0076i exposed 500 \\ fitset db28jan0077i elapsed 510.0 \\ ; fitset db28jan0077i exposed 500 \\ fitset db28jan0078i elapsed 510.0 \\ ; fitset db28jan0078i exposed 500 \\ fitset db28jan0079i elapsed 510.0 \\ ; fitset db28jan0079i exposed 500 \\ fitset db28jan0080i elapsed 510.0 \\ ; fitset db28jan0080i exposed 500 \\ fitset db28jan0081b elapsed 310.0 \\ ; fitset db28jan0081b exposed 300 \\ fitset db28jan0082b elapsed 15.0 \\ ; fitset db28jan0082b exposed 10 \\ fitset db28jan0083b elapsed 15.0 \\ ; fitset db28jan0083b exposed 10 \\ fitset db28jan0084v elapsed 15.0 \\ ; fitset db28jan0084v exposed 10 \\ fitset db28jan0085v elapsed 15.0 \\ ; fitset db28jan0085v exposed 10 \\ fitset db28jan0086r elapsed 15.0 \\ ; fitset db28jan0086r exposed 10 \\ fitset db28jan0087r elapsed 15.0 \\ ; fitset db28jan0087r exposed 10 \\ fitset db28jan0088i elapsed 15.0 \\ ; fitset db28jan0088i exposed 10 \\ fitset db28jan0089i elapsed 15.0 \\ ; fitset db28jan0089i exposed 10 \\ fitset db29jan0010b elapsed 310.0 \\ ; fitset db29jan0010b exposed 300 \\ fitset db29jan0011b elapsed 310.0 \\ ; fitset db29jan0011b exposed 300 \\ fitset db29jan0012b elapsed 310.0 \\ ; fitset db29jan0012b exposed 300 \\ fitset db29jan0013v elapsed 130.0 \\ ; fitset db29jan0013v exposed 120 \\ fitset db29jan0014v elapsed 130.0 \\ ; fitset db29jan0014v exposed 120 \\ fitset db29jan0015v elapsed 130.0 \\ ; fitset db29jan0015v exposed 120 \\ fitset db29jan0016r elapsed 110.0 \\ ; fitset db29jan0016r exposed 100 \\ fitset db29jan0017r elapsed 110.0 \\ ; fitset db29jan0017r exposed 100 \\ fitset db29jan0018r elapsed 110.0 \\ ; fitset db29jan0018r exposed 100 \\ fitset db29jan0019r elapsed 110.0 \\ ; fitset db29jan0019r exposed 100 \\ fitset db29jan0020r elapsed 210.0 \\ ; fitset db29jan0020r exposed 200 \\ fitset db29jan0021r elapsed 210.0 \\ ; fitset db29jan0021r exposed 200 \\ fitset db29jan0022r elapsed 210.0 \\ ; fitset db29jan0022r exposed 200 \\ fitset db29jan0023v elapsed 250.0 \\ ; fitset db29jan0023v exposed 240 \\ fitset db29jan0024v elapsed 250.0 \\ ; fitset db29jan0024v exposed 240 \\ fitset db29jan0025v elapsed 250.0 \\ ; fitset db29jan0025v exposed 240 \\ fitset db29jan0026b elapsed 610.0 \\ ; fitset db29jan0026b exposed 600 \\ fitset db29jan0027b elapsed 610.0 \\ ; fitset db29jan0027b exposed 600 \\ fitset db29jan0028b elapsed 610.0 \\ ; fitset db29jan0028b exposed 600 \\ fitset db29jan0029b elapsed 310.0 \\ ; fitset db29jan0029b exposed 300 \\ fitset db29jan0030i elapsed 510.0 \\ ; fitset db29jan0030i exposed 500 \\ fitset db29jan0031i elapsed 510.0 \\ ; fitset db29jan0031i exposed 500 \\ fitset db29jan0032i elapsed 510.0 \\ ; fitset db29jan0032i exposed 500 \\ fitset db29jan0033i elapsed 510.0 \\ ; fitset db29jan0033i exposed 500 \\ fitset db29jan0034i elapsed 510.0 \\ ; fitset db29jan0034i exposed 500 \\ fitset db29jan0035i elapsed 510.0 \\ ; fitset db29jan0035i exposed 500 \\ fitset db29jan0036i elapsed 510.0 \\ ; fitset db29jan0036i exposed 500 \\ fitset db29jan0037i elapsed 510.0 \\ ; fitset db29jan0037i exposed 500 \\ fitset db29jan0038i elapsed 510.0 \\ ; fitset db29jan0038i exposed 500 \\ fitset db29jan0039i elapsed 510.0 \\ ; fitset db29jan0039i exposed 500 \\ fitset db29jan0040b elapsed 510.0 \\ ; fitset db29jan0040b exposed 500 \\ fitset db29jan0041b elapsed 510.0 \\ ; fitset db29jan0041b exposed 500 \\ fitset db29jan0042b elapsed 510.0 \\ ; fitset db29jan0042b exposed 500 \\ fitset db29jan0043b elapsed 510.0 \\ ; fitset db29jan0043b exposed 500 \\ fitset db30jan0022b elapsed 455.0 \\ ; fitset db30jan0022b exposed 450 \\ fitset db30jan0023b elapsed 455.0 \\ ; fitset db30jan0023b exposed 450 \\ fitset db30jan0024b elapsed 455.0 \\ ; fitset db30jan0024b exposed 450 \\ fitset db30jan0025b elapsed 455.0 \\ ; fitset db30jan0025b exposed 450 \\ fitset db30jan0026b elapsed 455.0 \\ ; fitset db30jan0026b exposed 450 \\ fitset db30jan0027i elapsed 455.0 \\ ; fitset db30jan0027i exposed 450 \\ fitset db30jan0028i elapsed 455.0 \\ ; fitset db30jan0028i exposed 450 \\ fitset db30jan0029i elapsed 455.0 \\ ; fitset db30jan0029i exposed 450 \\ fitset db30jan0030r8 elapsed 128.0 \\ ; fitset db30jan0030r8 exposed 7 \\ fitset db30jan0031i elapsed 15.0 \\ ; fitset db30jan0031i exposed 10 \\ fitset db30jan0032r8 elapsed 305.0 \\ ; fitset db30jan0032r8 exposed 300 \\ fitset db30jan0033r8 elapsed 305.0 \\ ; fitset db30jan0033r8 exposed 300 \\ fitset db30jan0034i elapsed 305.0 \\ ; fitset db30jan0034i exposed 300 \\ fitset db30jan0035i elapsed 305.0 \\ ; fitset db30jan0035i exposed 300 \\ fitset db30jan0036r8 elapsed 305.0 \\ ; fitset db30jan0036r8 exposed 300 \\ fitset db30jan0037r8 elapsed 305.0 \\ ; fitset db30jan0037r8 exposed 300 \\ fitset db30jan0038i elapsed 305.0 \\ ; fitset db30jan0038i exposed 300 \\ fitset db30jan0039i elapsed 455.0 \\ ; fitset db30jan0039i exposed 450 \\ fitset db30jan0040i elapsed 455.0 \\ ; fitset db30jan0040i exposed 450 \\ fitset db30jan0041i elapsed 455.0 \\ ; fitset db30jan0041i exposed 450 \\ fitset db30jan0042b elapsed 455.0 \\ ; fitset db30jan0042b exposed 450 \\ fitset db30jan0043b elapsed 455.0 \\ ; fitset db30jan0043b exposed 450 \\ fitset db30jan0044i elapsed 455.0 \\ ; fitset db30jan0044i exposed 450 \\ fitset db30jan0045i elapsed 455.0 \\ ; fitset db30jan0045i exposed 450 \\ fitset db30jan0046i elapsed 455.0 \\ ; fitset db30jan0046i exposed 450 \\ fitset db30jan0047i elapsed 455.0 \\ ; fitset db30jan0047i exposed 450 \\ fitset db30jan0048i elapsed 455.0 \\ ; fitset db30jan0048i exposed 450 \\ fitset db30jan0049i elapsed 455.0 \\ ; fitset db30jan0049i exposed 450 \\ fitset db30jan0050b elapsed 455.0 \\ ; fitset db30jan0050b exposed 450 \\ fitset db30jan0051b elapsed 455.0 \\ ; fitset db30jan0051b exposed 450 \\ fitset db30jan0052b elapsed 455.0 \\ ; fitset db30jan0052b exposed 450 \\ fitset db31jan0020b elapsed 605.0 \\ ; fitset db31jan0020b exposed 600 \\ fitset db31jan0021b elapsed 605.0 \\ ; fitset db31jan0021b exposed 600 \\ fitset db31jan0022v elapsed 305.0 \\ ; fitset db31jan0022v exposed 300 \\ fitset db31jan0023v elapsed 305.0 \\ ; fitset db31jan0023v exposed 300 \\ fitset db31jan0024v elapsed 305.0 \\ ; fitset db31jan0024v exposed 300 \\ fitset db31jan0025v elapsed 305.0 \\ ; fitset db31jan0025v exposed 300 \\ fitset db31jan0026b elapsed 605.0 \\ ; fitset db31jan0026b exposed 600 \\ fitset db31jan0027b elapsed 605.0 \\ ; fitset db31jan0027b exposed 600 \\ fitset db31jan0028v elapsed 125.0 \\ ; fitset db31jan0028v exposed 120 \\ fitset db31jan0029v elapsed 125.0 \\ ; fitset db31jan0029v exposed 120 \\ fitset db31jan0030v elapsed 125.0 \\ ; fitset db31jan0030v exposed 120 \\ fitset db31jan0031r elapsed 105.0 \\ ; fitset db31jan0031r exposed 100 \\ fitset db31jan0032r elapsed 105.0 \\ ; fitset db31jan0032r exposed 100 \\ fitset db31jan0033r elapsed 105.0 \\ ; fitset db31jan0033r exposed 100 \\ fitset db31jan0034r elapsed 105.0 \\ ; fitset db31jan0034r exposed 100 \\ fitset db31jan0035r elapsed 105.0 \\ ; fitset db31jan0035r exposed 100 \\ fitset db31jan0036r elapsed 105.0 \\ ; fitset db31jan0036r exposed 100 \\ fitset db31jan0037b elapsed 305.0 \\ ; fitset db31jan0037b exposed 300 \\ fitset db31jan0038b elapsed 305.0 \\ ; fitset db31jan0038b exposed 300 \\ fitset db31jan0039b elapsed 305.0 \\ ; fitset db31jan0039b exposed 300 \\ fitset db31jan0040v elapsed 125.0 \\ ; fitset db31jan0040v exposed 120 \\ fitset db31jan0041v elapsed 125.0 \\ ; fitset db31jan0041v exposed 120 \\ fitset db31jan0042v elapsed 125.0 \\ ; fitset db31jan0042v exposed 120 \\ fitset db31jan0043v elapsed 125.0 \\ ; fitset db31jan0043v exposed 120 \\ fitset db31jan0044v elapsed 125.0 \\ ; fitset db31jan0044v exposed 120 \\ fitset db31jan0045v elapsed 125.0 \\ ; fitset db31jan0045v exposed 120 \\ fitset db31jan0046b elapsed 305.0 \\ ; fitset db31jan0046b exposed 300 \\ fitset db31jan0047r elapsed 105.0 \\ ; fitset db31jan0047r exposed 100 \\ fitset db31jan0048r elapsed 105.0 \\ ; fitset db31jan0048r exposed 100 \\ fitset db31jan0049r elapsed 305.0 \\ ; fitset db31jan0049r exposed 300 \\ fitset db31jan0050r8 elapsed 305.0 \\ ; fitset db31jan0050r8 exposed 300 \\ fitset db31jan0051r8 elapsed 305.0 \\ ; fitset db31jan0051r8 exposed 300 \\ fitset db31jan0052r8 elapsed 305.0 \\ ; fitset db31jan0052r8 exposed 300 \\ fitset db31jan0053r8 elapsed 305.0 \\ ; fitset db31jan0053r8 exposed 300 \\ fitset db31jan0054r8 elapsed 305.0 \\ ; fitset db31jan0054r8 exposed 300 \\ fitset db31jan0067b elapsed 455.0 \\ ; fitset db31jan0067b exposed 450 \\ fitset db31jan0068b elapsed 455.0 \\ ; fitset db31jan0068b exposed 450 \\