# # Used 3 poly terms when fitting flat. # # Data file specifying data dependent parameters for reduce.pl script. # Typically one should one such file for each night, arm of spectrograph # etc. # # Note # is the comment flag, = defines the start of a data item, # a space defines its end. (i.e. no space in data items are possible). # # reduce.pl will look for exact matches to the words before the = # sign so don't be tempted to shorten them. It does not mind about changing # the number of spaces. # # ND 'reduce.pl' applies pattern matching rules to recognise the data items # and if your value fails you will get a message of the form # 'xstart undefined' # # If this happens look at the relevant entry in the data file. # # Examples of recognized integers: +34, 4, -6 # although note that some variables expect only positive integers and # negative values will fail. # Version version = 12/12/2005 # Must match the version in "reduce.pl" # NDF files always needed for reduction balance = balance # Balance frame name zero = zero # name of null frame unit = unit # name of unit frame master sky = SRMAST # name of master sky region file for skymov # Script and log files (output and useful for checking on reduction) data types = zzz_datatypes # file of data types reduce script = zzz_reduction # reduction script used reduce log = zzz_reduction.log # log of running reduction script. files = # Any extra files or file lists in adition to those on the command line. # Arc selection arc_pos_tolerance = 2 # Tolerance on sky position (deg) for arc/object arc_pa_tolerance = 2. # Tolerance on PA of slit (deg) for arc/object arc_time_tolerance = 80. # Tolerance on time (minutes) for arc/object # valid region of frame (i.e. avoiding all dodgy areas) xstart = 10 # start of useful region in X xend = 100 # end of useful region in X ystart = 801 # start of useful region in Y yend = 3800 # end of useful region in Y # noise model readout = 2.9 # Readout noise, RMS ADU. bias_region = debias.reg # If defined, readout noise will be measured for each frame from this region photon = 1.05 # electrons/ADU # Object identifier - use to distinguish spectra if extracting more than one object/frame. identifier = # String that gets tacked onto files names. # idtype parameters idtype_track = TRMAST # name of trace file (same one used for all files). Leave blank if you don't want one. idtype_nxwidth = 11 # median filter width in X idtype_nywidth = 15 # median filter width in Y idtype_tobjm = 1.2 # multiplicative object threshold (only just > 1 if sky strong) idtype_tobja = 40.0 # additive object threshold idtype_tlinm = 50. # multiplicative line threshold idtype_tlina = 5000. # additive line threshold idtype_flim = 10000. # junk/flat discrimination # Tracing of curved spectra track_npoly = 4 # Order of tracing polynomial, 0 ==> no tracing track_xstart = 20 # start of region to search for objects track_xend = 90 # end of region to search for objects track_template = # template trace dealing with high order coefficients. Blank to ignore track_tweak = false # 'true' or 'false' to tweak or not to find initial position (only relevant if track_template file specified) track_offset = 1 # Offset to add when tweak (if track_tweak) track_fchange = 2 # Reject if position changes by more than this after first position refine (if track_tweak) track_nobj = 1 # Number of objects in the frame (if not !track_tweak) track_iobj = 1 # Spectrum to extract counting from the left (if not !track_tweak) track_iblock = 500 # No. of rows to average in finding objects (if not !track_tweak) track_ypos = 2000 # Initial y position. track_width = 25 # width of the window track_esig = 4. # FWHM of gaussian for cross correlation. track_fwhm = 3. # Estimated true FWHM of profile track_clip = 3. # Rejection criterion for poly fitting track_nblock = 1 # No. of rows to average in tracing objects track_psig = 4 # Rejection criterion for blocking track_tcycle = 10 # Number of rejection cycles for poly fitting track_change = 1 # Reject if position changes by more than this after reject # Flats # # Fits to spectrum use ARD mask file to remove bad parts. # Example: # # DIMENSION(1) # LINE(0,54) .OR. LINE(1075,2100) # # This masks pixels at the start and end of the spectrum. nearflat = false # true/false to to create individual flats for object frames, in which case you need: twilight = unit # name of twilight frame (set = unit for no effect) maskfile = ardfile # ARD mask file for masking fit to mean flat spectrum flat_pos_tolerance = 2 # Tolerance on sky position (deg) for flat/object association flat_pa_tolerance = 10. # Tolerance on PA of slit (deg) for flat/object flat_time_tolerance = 160. # Tolerance on time (minutes) for flat/object flat_npoly = 2 # No. of poly coeffs for fitting spectral variation of flats. flat_thrlo = -3 # Lower reject threshold flat_thrhi = 3 # Upper reject threshold flat_ncycle = 10 # Number of rejection cycles. # Dichroic ripple # --------------- # On WHT ISIS blue arm spectra, the dichroic "ripple" moves around, but there # is not enough signal in a typical flat at the extreme blue end, so using # "nearflat" directly can more than double the noise. To cope with this, we # form a balance frame by extracting a spectral response from the balance # frame created by "nearflat" between dichroic_ylo and dichroic_yhi and # multiply it row-wise through a dichroic_balance - a balance frame for which the # spectral response has been comletely divided out. (or for which the dichroic was # taken out, or a unit frame). # Note that these are figaro-style values i.e., pixel no. - 0.5 # To disable this feature, set dichroic_ylo=0 (or nearflat = 0). # (PFLM 1 May 2001) dichroic_ylo = 0.0 # Lower limit to extract dichroic response. dichroic_yhi = 134.5 # Upper limit to extract dichroic response. dichroic_balance = dichroic_balance # Flat with pixel-to-pixel noise only. # skymov parameters skymov_slo = 20 # start of search region skymov_shi = 80 # end of search region skymov_fwhm = 4.0 # FWHM skymov_xpos = 52.193 # object reference position skymov_npoly = 3 # number of poly coeffs skymov_tlo = -3.5 # lower reject threshold skymov_thi = +3.2 # upper reject threshold skymov_nmin = 3 # minimum block of bad pixels skymov_nwidth = 15 # median filter width # Next is optional 'ardmask' file to mask bad pixels which # are fixed relative to the CCD sky_mask = skymask.ard # name of 1-D ardmask file to mask bad pixels # skyfit parameters skyfit_npoly = 3 # number of poly coeffs skyfit_thresh = 3. # reject threshold # extopt parameters (if tracing not being used) extopt_npoly = 6 # number of poly coeffs extopt_thresh = 5. # reject threshold extopt_nblock = 3 # rows/block extopt_nmed = 5 # median filter width extopt_ratlim = 4. # cosmic ray rejection extopt_eps = 0.01 # prevent spurious rejection at high S/N # Profile fitting (if tracing being used) profit_npoly = 3 # Order of profile fitting polynomial profit_sizex = 0.5 # The separation in pixels between the polynomials. profit_thresh = 3.0 # Sigma threshold for poly fits. profit_nblock = 1 # Data will be taken in groups of NBLOCK rows profit_nmed = 5 # median filter width profit_badval = 50000 # Bad pixel value for profit. Set large to ignore profit_nslow = 30 # Number of pixels to reject slowly # optext parameters (if tracing is being used) optext_ratlim = 3.8 # cosmic ray rejection optext_eps = 0.025 # prevent spurious rejection at high S/N optext_iave = 1 # Number of sky pixels to average over.