IRAF REDUCTION The steps involved in the IRAF reduction are to take the raw files specified by the extension _raw.fits and 1) Generate the raw.coo.1 files with DAOFIND. The parameters used are the following --In datapars (to reach type da>> epar datapars) -------------------------------------------------------------- PACKAGE = daophot TASK = datapars (scale = 1.) Image scale in units per pixel (fwhmpsf= 4.) FWHM of the PSF in scale units (emissio= yes) Features are positive ? (sigma = 10.) Standard deviation of background in counts (datamin= 1.) Minimum good data value (datamax= 10000.) Maximum good data value (noise = poisson) Noise model (ccdread= ) CCD readout noise image header keyword (gain = ) CCD gain image header keyword (readnoi= 0.) CCD readout noise in electrons (epadu = 1.) Gain in electrons per count (exposur= ) Exposure time image header keyword (airmass= ) Airmass image header keyword (filter = ) Filter image header keyword (obstime= ) Time of observation image header keyword (itime = 1.) Exposure time (xairmas= INDEF) Airmass (ifilter= INDEF) Filter (otime = INDEF) Time of observation (mode = ql) -------------------------------------------------------------------- --in centerpars (to reach type da>> epar centerpars) -------------------------------------------------------------- PACKAGE = daophot TASK = centerpars (calgori= centroid) Centering algorithm (cbox = 5.) Centering box width in scale units (cthresh= 0.) Centering threshold in sigma above background (minsnra= 1.) Minimum signal-to-noise ratio for centering algorithi (cmaxite= 10) Maximum iterations for centering algorithm (maxshif= 1.) Maximum center shift in scale units (clean = no) Symmetry clean before centering (rclean = 1.) Cleaning radius in scale units (rclip = 2.) Clipping radius in scale units (kclean = 3.) K-sigma rejection criterion in skysigma (mkcente= no) Mark the computed center (mode = ql) --------------------------------------------------------------------- --in fitskypars (to reach type da>>epar fitskypar) -------------------------------------------------------------------- PACKAGE = daophot TASK = fitskypars (salgori= mode) Sky fitting algorithm (annulus= 10.) Inner radius of sky annulus in scale units (dannulu= 5.) Width of sky annulus in scale units (skyvalu= 0.) User sky value (smaxite= 10) Maximum number of sky fitting iterations (sloclip= 0.) Lower clipping factor in percent (shiclip= 0.) Upper clipping factor in percent (snrejec= 50) Maximum number of sky fitting rejection iterations (sloreje= 3.) Lower K-sigma rejection limit in sky sigma (shireje= 3.) Upper K-sigma rejection limit in sky sigma (khist = 3.) Half width of histogram in sky sigma (binsize= 0.1) Binsize of histogram in sky sigma (smooth = no) Boxcar smooth the histogram (rgrow = 0.) Region growing radius in scale units (mksky = no) Mark sky annuli on the display (mode = ql) --------------------------------------------------------------------- and in daofind itself, the parameters are (the file all_fits_files.txt contains the name of all the fits files in the ../raw directory) PACKAGE = daophot TASK = daofind image = @all_fits_files.txt Input image(s) output = ../mag_1_06/ Output coordinate file(s) (default: image.coo.?) (starmap= ) Output density enhancement image(s) (skymap = ) Output sky image(s) (datapar= ) Data dependent parameters (findpar= ) Object detection parameters (boundar= nearest) Boundary extension (constant|nearest|reflect|wrap) (constan= 0.) Constant for boundary extension (interac= no) Interactive mode ? (icomman= ) Image cursor: [x y wcs] key [cmd] (gcomman= ) Graphics cursor: [x y wcs] key [cmd] (wcsout = )_.wcsout) The output coordinate system (logical,tv,physical) (cache = )_.cache) Cache the image pixels ? (verify = )_.verify) Verify critical daofind parameters ? (update = )_.update) Update critical daofind parameters ? (verbose= )_.verbose) Print daofind messages ? (graphic= )_.graphics) Graphics device (display= )_.display) Display device (mode = ql) -------------------------------------------------------------------- This will generate the .coo files that contain information about the extracted objects. The next step is 2) Produce the .mag files with DAOPHOT. The paramters used are ------------------------------------------------------------------- PACKAGE = daophot TASK = phot image = @all_fits_files.txt Input image(s) coords = ../mag_1_06/ Input coordinate list(s) (default: image.coo.?) output = ../mag_1_06/ Output photometry file(s) (default: image.mag.?) skyfile = Input sky value file(s) (plotfil= ) Output plot metacode file (datapar= ) Data dependent parameters (centerp= ) Centering parameters (fitskyp= ) Sky fitting parameters (photpar= ) Photometry parameters (interac= no) Interactive mode ? (radplot= no) Plot the radial profiles? (icomman= ) Image cursor: [x y wcs] key [cmd] (gcomman= ) Graphics cursor: [x y wcs] key [cmd] (wcsin = )_.wcsin) The input coordinate system (logical,tv,physical,worl (wcsout = )_.wcsout) The output coordinate system (logical,tv,physical) (cache = )_.cache) Cache the input image pixels in memory ? (verify = )_.verify) Verify critical phot parameters ? (update = )_.update) Update critical phot parameters ? (verbose= )_.verbose) Print phot messages ? (graphic= )_.graphics) Graphics device (display= )_.display) Display device (mode = ql) ------------------------------------------------------------------------ The .mag files are not in an appropriate format for IDL, so to produce an appropriate form, the txdump utility is used. It is placed in a .cl script called testscript.cl that contains the following lines list="all_mag_files.txt" print(list) while ( fscan (list, s1) != EOF) { txdump (s1, "xcenter,ycenter,xerr,yerr,mag", yes, >> s1//".txt") This will dump the parameters into a .mag.1.txt file. ------------------------------------------------------------------------ IDL ANALYSIS The IDL analysis uses the .coo and .mag.1.txt files. The script that is used first is SCRIPT 1) routine_coo_mag_to_stats.pro This script will go through each one of the .coo and .mag.1.txt files (for a particular image) and compute a center of the available coordinates, as well as the difference between the centroid and the ideal grid position. IDL SCRIPTS ------------------------- The steps to analyse the data in IRAF are the following 1) Run the script routine_coo_mag_to_stats.pro This script will extract the relevant quantities from the IRAF .coo and .mag files and move them to a file with the extension _stats.txt in the chosen stats/ directory. (This is set as a keyword in the script). It will also fit a center to each frame (i.e. a center coordinate for the ShackHartman grid in each picture). Once these quantities have been extracted, the centers are piecemeal fit with 2) routine_center_drift.pro This will perfrom a linear fit to the center of the grid vs. time. The large jumps, assumed to be slews in the telescope are indicated as a file_number in the script. Once the new centers are calculated, the offsets of the centroids relative to the newly centered grids are obtained and put in the files offsets.txt.This is accomplished by running 3) routine_xy_offsets.pro There will be several output files. The first set of output files will have the extension _offsets.txt. They contain the value of the x offset, y offset, magnitude of the vector, angle of the vector, the bolometric magnitude and so on. The second set will have the extension sub_offsets.txt. These files have the average offset subtracted from each grid point to account for the distorted grid. Finally, the file Average_Offsets.txt will be output. This file contains the distortions of the grid from an ideal rectangle. The next step is to run 4) routine_cn_log_depth.pro This will generate the covariance plots.