QUICK REDUCTION OF SOME MagIC CAMERA DATA FROM LCO 1 May 2001 The MagIC is the MIT fast read camera at the Baade telescope. The scale is 0.069"/pix. There is no manual yet. The raw read format is [2064,2062][ushort] Estimated gain: ll: <> sig med N 1.974 0.106 1.974 37 (e-/ADU) gain 15.225 1.300 15.221 37 (e-) ron lr: 2.019 0.109 2.021 32 13.066 1.357 12.753 32 ul: 2.065 0.121 2.067 34 12.476 1.271 12.490 34 ur: 1.890 0.125 1.881 31 12.562 1.305 12.822 31 So a value of 2.0 and 13.5 is fine. Saturation is about 45000. 2.36' |-------------| | | E| | | | | | |-------------| N CCD REDUCTIONS This is a quick guess at what to do. An implot shows the following structure: x: 1:4 bad 5:1026 good data 1027:1032 bias (exclude 1027 which is slightly high) 1033:1038 bias (exclude 1038 which is slightly high) 1039:2060 good data 2061:2064 bad y: 1 bad 2:1025 good 1026:1038 bias region (?) 1039:2061 good 2062 bad I am not sure where there is a "bias" here. I will assume it is in the "x" direction, but will have to check on this. Rename the images. IRAF does not like names with start with "01" like 010317.010.fits, because it will tranlate it into octal. You have to refer to the data as "010317.010.fits" within IRAF. I changed the names to q*.imh rename cpimh *.imh del+ hedit r*.imh observat "lco" up+ ver- setjd *.imh hjd="" I wrote a task which pulls apart the 4 quads, reduces them to [OT] and reassembles the image. To run it, do the following: 1. Set up a special uparm as: setup: set stdimage = imt2048 set uparm = /uw50/nick/uparm/magic/ noao ctio nickcl imred ccdred keep Now edit ccdr: ccdr: (pixeltype = "real real") Output and calculation pixel datatypes (verbose = yes) Print log information to the standard output? (logfile = "logfile") Text log file (plotfile = "") Log metacode plot file (backup = "") Backup directory or prefix (instrument = "myiraf$/magic.dat") CCD instrument file (ssfile = "myiraf$/magic.sub") Subset translation file (graphics = "stdgraph") Interactive graphics output device (cursor = "") Graphics cursor input (version = "2: October 1987") (mode = "ql") ccdpr: images = "" List of CCD images to correct (output = "") List of output CCD images (ccdtype = "") CCD image type to correct (max_cache = 0) Maximum image caching memory (in Mbytes) (noproc = no) List processing steps only?\n (fixpix = no) Fix bad CCD lines and columns? (overscan = no) Apply overscan strip correction? (trim = no) Trim the image? (zerocor = no) Apply zero level correction? (darkcor = no) Apply dark count correction? (flatcor = no) Apply flat field correction? (illumcor = no) Apply illumination correction? (fringecor = no) Apply fringe correction? (readcor = no) Convert zero level image to readout correction? (scancor = no) Convert flat field image to scan correction?\n (readaxis = "line") Read out axis (column|line) (fixfile = "") File describing the bad lines and columns (biassec = "") Overscan strip image section (trimsec = "") Trim data section (zero = "") Zero level calibration image (dark = "") Dark count calibration image (flat = "") Flat field images (illum = "") Illumination correction images (fringe = "") Fringe correction images (minreplace = 1.) Minimum flat field value (scantype = "shortscan") Scan type (shortscan|longscan) (nscan = 1) Number of short scan lines\n (interactive = no) Fit overscan interactively? (function = "leg") Fitting function (order = 1) Number of polynomial terms or spline pieces (sample = "*") Sample points to fit (naverage = 1) Number of sample points to combine (niterate = 1) Number of rejection iterations (low_reject = 3.) Low sigma rejection factor (high_reject = 3.) High sigma rejection factor (grow = 0.) Rejection growing radius (mode = "ql") magic.dat: subset filtert exptime exptime darktime darktime imagetyp imagetyp biassec biassec datasec datasec trimsec trimsec fixfile fixfile FOCUS object OBJECT object DARK dark FLAT flat BIAS zero # Old software magic.sub: 'MagIC_t0' opaque 'MagIC_B' B 'V_LC3014' V ccdmagic: images = "q*.imh" input images (bias1 = "[1028:1032,2:1025]") bias for ll amp (bias2 = "[1033:1037,2:1025]") bias for lr amp (bias3 = "[1028:1032,1039:2061]") bias for ul amp (bias4 = "[1033:1037,1039:2061]") bias for ur amp (trim1 = "[5:1026,2:1025]") trim for ll amp (trim2 = "[1039:2060,2:1025]") trim for lr amp (trim3 = "[5:1026,1039:2061]") trim for ul amp (trim4 = "[1039:2060,1039:2061]") trim for ur amp (prefix = "r") Prefix for reduced data (niter = 3) Number of iterations for bias (reject = 2.5) Low and high sigma rejection (imglist = "tmp$tmp15763ka") (mode = "ql") Combine the biases as: zerocomb @inbias out=Zero Combine the flats: flatcomb @inb flatcomb @inv Now process the data as: ccdpr r*.imh (note: I forgot to change the IMAGETYP on some of the "focus" frames that were labeled "FLAT" to "OBJECT". For some reason, the ccdmagic processing clipped the data at 0 with no negative values. I can't figure out why it did this, but make sure that IMAGETYP is set correctly before doing ccdmagic and ccdpr) EDIT IN THE AIRMASS hedit ra,dec,epoch into the header. To do this, you must enter the value twice (an IRAF bug) or use my script editcoord: editcoord @in10 "07:24:15" "-00:32:55" 2000. editcoord @in11 "11:01:36.4" "-06:06:32" 2000. editcoord @in12 "10:50:03" "-00:00:32" 2000. etc. Now calculate the ST. I will write an IRAF task to do this later. hsel d*.imh $I,date-obs,ut yes > junk trans junk "-" " " | trans STDIN '"' " " > junk1 filecalc junk1 "$2; $3; $4; $5-4" form="%3d%3d%3d\t%h13" > junk2 junk2 should have: yyyy mm dd LT where LT is local time (!). You had better check that this is correct! Then run asttimes files=junk2 observatory=lco This outputs a text file with the ST. Edit this file to input the ST into the header. hedit r*.imh $I,st yes (you have to run this twice to get the proper units) Calculate the airmass: setairmass @in1 observatory=lco Put in the hour angle. hedit @in1 ha '(st-ra)' add+ DAOPHOT (the following is pretty specific to my reduction programs) copy the *.opt files, *.lib, *.tfm Make the *.inf file hsel @in1 $I,filtert,ut,airmass,exptime,jd,title,ha yes > junk1.dat translit junk1.dat '"' ' ' > junk.dat !$myprog/prog3a junk.dat /uw50/nick/daophot/irafstuff/filters_magic.dat 2. Measure the FWHM as: del junk.dat yaloshift @in1 etc. Then run $myprog/prog39 junk.dat 3. For standards, run BFIND2,using thresh about 12 for the bright stars. 4. DAOGROW ls -1 *.ap > magic.lis Use 3 unknowns, 0.9 0 for the last two, and set the uncertainty to 0.02. 5. DAOMATCH, DAOMASTER Use DAOMATCH or run yalocen on the data followed by. $myprog/prog52a junk.dat head -1 temp.mch mv temp.mch xxx.mch or sed s/tot/als/ temp.mch > rxxx.mch For then input to DAOMASTER use: ty myiraf$/in4_yaloopt 7. Display each first image in the *.mch files. Run the iraf task "fetch" and then the fortran task "fetch" to make the *.fet files. 8. Enter the data into COLLECT. Use prog43 to speed things up. !$myprog/prog43 ccd12.mch COLOR TERMS The BV color solution for this night was based on 27 standards, of two fields (Ru149 and pg1047) taken at the same airmass but 4 hours apart. The night looked quite photometric. M1=I1+I2 M2=I1 I1=M2 I2=M1-M2 O1 = M1 + A0 + A1*I2 + A2*X + A3*T O2 = M2 + B0 + B1*I2 + B2*X + B3*T A2=0.24 A3=0. m:b,v, I:V,B-V B2=0.12 B3=0. A0 = -1.1355085 0.0061041 << A1 = -0.0297454 0.0108595 << B0 = -1.4578034 0.0057458 << B1 = 0.0581488 0.0096709 << S1 = 0.0177567 << S2 = 0.0197406 << So: b = B + -0.030*(B-V) + zp v = V + +0.058*(B-V) + zp The V term is a bit higher than usual. The range in color was (-0.11,1.12). The color terms were not very linear and the fits were not very good, even though the data are extremely photometric. That is why the residuals had an extra scatter (S1,S2) of 0.017 and 0.019mag. The color term may be quadradic. For a photometric night on smaller telescopes, these are 0. There may be a small photometric gradient in x of about 0.04mag. Without more standards, I can't say. mag at 1ADU/s B 26.17 V 26.42