noao.imred.ccdred.zerocombine

I R A F Image Reduction and Analysis Facility PACKAGE = ccdred TASK = zerocombine input = @zeros.list List of zero level images to combine (output = Zero) Output zero level name (combine= average) Type of combine operation (reject = minmax) Type of rejection (ccdtype= zero) CCD image type to combine (process= no) Process images before combining? (delete = no) Delete input images after combining? (clobber= no) Clobber existing output image? (scale = none) Image scaling (statsec= ) Image section for computing statistics (nlow = 0) minmax: Number of low pixels to reject (nhigh = 1) minmax: Number of high pixels to reject (nkeep = 1) Minimum to keep (pos) or maximum to reject (neg) (mclip = yes) Use median in sigma clipping algorithms? (lsigma = 3.) Lower sigma clipping factor (hsigma = 3.) Upper sigma clipping factor (rdnoise= 0.) ccdclip: CCD readout noise (electrons) (gain = 1.) ccdclip: CCD gain (electrons/DN) (snoise = 0.) ccdclip: Sensitivity noise (fraction) (pclip = -0.5) pclip: Percentile clipping parameter (blank = 0.) Value if there are no pixels

I used hedit to set biassec in images hedit *.????.fits BIASSEC [2696:2708,1:256]

I used ccdproc to zero correct all the images.

noao.imred.ccdred.zerocombine

I R A F Image Reduction and Analysis Facility PACKAGE = ccdred TASK = ccdproc images = *.fits List of CCD images to correct (output = ) List of output CCD images (ccdtype= ) CCD image type to correct (max_cac= 0) Maximum image caching memory (in Mbytes) (noproc = no) List processing steps only? (fixpix = no) Fix bad CCD lines and columns? (oversca= yes) Apply overscan strip correction? (trim = yes) Trim the image? (zerocor= yes) Apply zero level correction? (darkcor= no) Apply dark count correction? (flatcor= no) Apply flat field correction? (illumco= no) Apply illumination correction? (fringec= no) Apply fringe correction? (readcor= no) Convert zero level image to readout correction? (scancor= no) Convert flat field image to scan correction? (readaxi= line) Read out axis (column|line) (fixfile= ) File describing the bad lines and columns (biassec= image) Overscan strip image section (trimsec= ) Trim data section (zero = Zero) Zero level calibration image (dark = ) Dark count calibration image (flat = ) Flat field images (illum = ) Illumination correction images (fringe = ) Fringe correction images (minrepl= 1.) Minimum flat field value (scantyp= shortscan) Scan type (shortscan|longscan) (nscan = 1) Number of short scan lines (interac= yes) Fit overscan interactively? (functio= chebyshev) Fitting function (order = 3) Number of polynomial terms or spline pieces (sample = *) Sample points to fit (naverag= 1) Number of sample points to combine (niterat= 1) Number of rejection iterations (low_rej= 3.) Low sigma rejection factor (high_re= 3.) High sigma rejection factor (grow = 1.) Rejection growing radius

I combined the flats from Nov. 30 into Flat.fits, and created two flats for Dec. 1, one with the filter (sFlat.fits) and one without the filter (qFlat.fits).

noao.imred.ccdred.zerocombine

I R A F Image Reduction and Analysis Facility PACKAGE = ccdred TASK = flatcombine input = @sflats.list List of flat field images to combine (output = sFlat) Output flat field root name (combine= average) Type of combine operation (reject = ccdclip) Type of rejection (ccdtype= flat) CCD image type to combine (process= yes) Process images before combining? (subsets= yes) Combine images by subset parameter? (delete = no) Delete input images after combining? (clobber= no) Clobber existing output image? (scale = mode) Image scaling (statsec= ) Image section for computing statistics (nlow = 1) minmax: Number of low pixels to reject (nhigh = 1) minmax: Number of high pixels to reject (nkeep = 1) Minimum to keep (pos) or maximum to reject (neg) (mclip = yes) Use median in sigma clipping algorithms? (lsigma = 3.) Lower sigma clipping factor (hsigma = 3.) Upper sigma clipping factor (rdnoise= RDNOISE) ccdclip: CCD readout noise (electrons) (gain = GAIN) ccdclip: CCD gain (electrons/DN) (snoise = 0.) ccdclip: Sensitivity noise (fraction) (pclip = -0.5) pclip: Percentile clipping parameter (blank = 1.) Value if there are no pixels

I used imarith to divide the quartz flats from each night; the std dev for any given point was around or less than 1%, so I used imcombine to create a combined flat (cFlat.fits) using the mean of the two.

I then used response to normalize this flat, creating nFlat.fits.

noao.twodspec.longslit.response

I R A F Image Reduction and Analysis Facility PACKAGE = longslit TASK = response calibrat= cFlat Longslit calibration images normaliz= cFlat Normalization spectrum images response= nFlat Response function images (interac= yes) Fit normalization spectrum interactively? (thresho= INDEF) Response threshold (sample = *) Sample of points to use in fit (naverag= 1) Number of points in sample averaging (functio= spline3) Fitting function (order = 13) Order of fitting function (low_rej= 3.) Low rejection in sigma of fit (high_re= 3.) High rejection in sigma of fit (niterat= 1) Number of rejection iterations (grow = 0.) Rejection growing radius (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input

I ran ccdproc again, changing:
(flatcor= yes) Apply flat field correction?
(flat = Flat) Flat field images
(interac= no) Fit overscan interactively?
(order = 4) Number of polynomial terms or spline pieces
(grow = 0.) Rejection growing radius

I combined the twilight images from each night using imcombine, then used response to normalize the image, and illumination to normalize in the other direction.

images.immatch.imcombine

I R A F Image Reduction and Analysis Facility PACKAGE = immatch TASK = imcombine input = @twi.list List of images to combine output = Sky List of output images (headers= ) List of header files (optional) (bpmasks= ) List of bad pixel masks (optional) (rejmask= ) List of rejection masks (optional) (nrejmas= ) List of number rejected masks (optional) (expmask= ) List of exposure masks (optional) (sigmas = ) List of sigma images (optional) (logfile= STDOUT) Log file (combine= average) Type of combine operation (reject = none) Type of rejection (project= no) Project highest dimension of input images? (outtype= real) Output image pixel datatype (outlimi= ) Output limits (x1 x2 y1 y2 ...) (offsets= none) Input image offsets (masktyp= none) Mask type (maskval= 0.) Mask value (blank = 0.) Value if there are no pixels (scale = mode) Image scaling (zero = none) Image zero point offset (weight = none) Image weights (statsec= ) Image section for computing statistics (expname= ) Image header exposure time keyword (lthresh= INDEF) Lower threshold (hthresh= INDEF) Upper threshold (nlow = 1) minmax: Number of low pixels to reject (nhigh = 1) minmax: Number of high pixels to reject (nkeep = 1) Minimum to keep (pos) or maximum to reject (neg) (mclip = yes) Use median in sigma clipping algorithms? (lsigma = 3.) Lower sigma clipping factor (hsigma = 3.) Upper sigma clipping factor (rdnoise= 0.) ccdclip: CCD readout noise (electrons) (gain = 1.) ccdclip: CCD gain (electrons/DN) (snoise = 0.) ccdclip: Sensitivity noise (fraction) (sigscal= 0.1) Tolerance for sigma clipping scaling corrections (pclip = -0.5) pclip: Percentile clipping parameter (grow = 0.) Radius (pixels) for neighbor rejection

noao.imred.specred.response

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = response calibrat= Sky.fits Longslit calibration images normaliz= Sky.fits Normalization spectrum images response= nSky.fits Response function images (interac= yes) Fit normalization spectrum interactively? (thresho= INDEF) Response threshold (sample = *) Sample of points to use in fit (naverag= 1) Number of points in sample averaging (functio= legendre) Fitting function (order = 8) Order of fitting function (low_rej= 2.) Low rejection in sigma of fit (high_re= 3.) High rejection in sigma of fit (niterat= 5) Number of rejection iterations (grow = 3.) Rejection growing radius (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input

The dispersion bins were deleted and re-selected, to avoid major lines.

noao.imred.specred.illumination

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = illumination images = nSky.fits Longslit calibration images illumina= iSky.fits Illumination function images (interac= yes) Interactive illumination fitting? (bins = ) Dispersion bins (nbins = 5) Number of dispersion bins when bins = "" (sample = *) Sample of points to use in fit (naverag= 1) Number of points in sample averaging (functio= spline3) Fitting function (order = 3) Order of fitting function (low_rej= 3.) Low rejection in sigma of fit (high_re= 2.) High rejection in sigma of fit (niterat= 1) Number of rejection iterations (grow = 2.) Rejection growing radius (interpo= poly3) Interpolation type (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input

I ran ccdproc, changing:
(illumco= yes) Apply illumination correction?
(illum = nSky) Illumination correction images

Using hselect, I created a list of stars and a list of arcs for each night. I used apall to extract the spectra.

noao.imred.specred.apall

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = apall input = @stars.list List of input images (output = ) List of output spectra (apertur= ) Apertures (format = multispec) Extracted spectra format (referen= ) List of aperture reference images (profile= ) List of aperture profile images (interac= yes) Run task interactively? (find = yes) Find apertures? (recente= yes) Recenter apertures? (resize = yes) Resize apertures? (edit = yes) Edit apertures? (trace = yes) Trace apertures? (fittrac= yes) Fit the traced points interactively? (extract= yes) Extract spectra? (extras = yes) Extract sky, sigma, etc.? (review = yes) Review extractions? (line = INDEF) Dispersion line (nsum = -500) Number of dispersion lines to sum or median # DEFAULT APERTURE PARAMETERS (lower = -5.) Lower aperture limit relative to center (upper = 5.) Upper aperture limit relative to center (apidtab= ) Aperture ID table (optional) # DEFAULT BACKGROUND PARAMETERS (b_funct= chebyshev) Background function (b_order= 2) Background function order (b_sampl= -40:-20,20:40) Background sample regions (b_naver= -21) Background average or median (b_niter= 0) Background rejection iterations (b_low_r= 3.) Background lower rejection sigma (b_high_= 3.) Background upper rejection sigma (b_grow = 0.) Background rejection growing radius # APERTURE CENTERING PARAMETERS (width = 11.) Profile centering width (radius = 10.) Profile centering radius (thresho= 0.) Detection threshold for profile centering # AUTOMATIC FINDING AND ORDERING PARAMETERS nfind = 1 Number of apertures to be found automatically (minsep = 5.) Minimum separation between spectra (maxsep = 1000.) Maximum separation between spectra (order = increasing) Order of apertures # RECENTERING PARAMETERS (aprecen= ) Apertures for recentering calculation (npeaks = INDEF) Select brightest peaks (shift = yes) Use average shift instead of recentering? # RESIZING PARAMETERS (llimit = -10.) Lower aperture limit relative to center (ulimit = 10.) Upper aperture limit relative to center (ylevel = 0.1) Fraction of peak or intensity for automatic widt (peak = yes) Is ylevel a fraction of the peak? (bkg = yes) Subtract background in automatic width? (r_grow = 0.) Grow limits by this factor (avglimi= no) Average limits over all apertures? # TRACING PARAMETERS (t_nsum = 100) Number of dispersion lines to sum (t_step = 50) Tracing step (t_nlost= 3) Number of consecutive times profile is lost befo (t_funct= legendre) Trace fitting function (t_order= 5) Trace fitting function order (t_sampl= *) Trace sample regions (t_naver= 1) Trace average or median (t_niter= 2) Trace rejection iterations (t_low_r= 3.) Trace lower rejection sigma (t_high_= 3.) Trace upper rejection sigma (t_grow = 0.) Trace rejection growing radius # EXTRACTION PARAMETERS (backgro= fit) Background to subtract (skybox = 1) Box car smoothing length for sky (weights= variance) Extraction weights (none|variance) (pfit = fit1d) Profile fitting type (fit1d|fit2d) (clean = yes) Detect and replace bad pixels? (saturat= 60000.) Saturation level (readnoi= 3) Read out noise sigma (photons) (gain = 1) Photon gain (photons/data number) (lsigma = 4.) Lower rejection threshold (usigma = 4.) Upper rejection threshold (nsubaps= 1) Number of subapertures per aperture

The aperture trace changes between 2-4 pixels from one end to the other.
30nov05.0130 had a bad trace (lots of bumps), it also had a double spike, check image.
In the log, for 30nov05.0162-164, it says 'funny things happen'; 162 appears to be blank. I ignored these.
1dec05.0213 has a note in the log saying the star is on three positions on the slit; I only see two. (?) 1dec05.0239 has a brighter star offset, and a fainter stars centered; I chose the centered one.
1dec05.0267 has four equally bright stars, I chose the one closest to the center.
1dec05.0269 has one bright star on the edge, and a fainter one in the center; I chose the center one.
1dec05.0288 has very low counts and a bad trace
1dec05.0302 had a bumpy trace
1dec05.0311 has four stars, I chose the brightest one.
1dec05.0321 and 1dec05.0322 have very low counts and bad traces

Using the log, I made a .cl (arcsref.cl) file of arcs and the images they refer to, which I used to run apall for each night, changing:
(interac= no) Run task interactively?
(recente= no) Recenter apertures?
(trace = no) Trace apertures?
(review = no) Review extractions?
(backgro= none) Background to subtract

The filenames I used for the extracted arcs are date.arc#.star#.ms
1dec05.0274 does not exist? this should be an arc.

To wavelength calibrate the spectra, I used the calibration from the previous MMT data. I copied the arc spectra which I had used as a reference for that data into the 30nov05 directory as test.ms, and ran reid, refspec and dispcor on an arc and a star from the new data. The fit was good, and the process did not generate any errors, so I used reid on all of the arcs.

noao.imred.specred.reidentify

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = reidentify referenc= test.ms.fits Reference image images = *.????.????.ms.fits Images to be reidentified (interac= yes) Interactive fitting? (section= middle line) Section to apply to two dimensional images (newaps = yes) Reidentify apertures in images not in reference? (overrid= no) Override previous solutions? (refit = yes) Refit coordinate function? (trace = no) Trace reference image? (step = 10) Step in lines/columns/bands for tracing an image (nsum = 10) Number of lines/columns/bands to sum (shift = 0.) Shift to add to reference features (INDEF to sea (search = 0.) Search radius (nlost = 4) Maximum number of features which may be lost (cradius= 5.) Centering radius (thresho= 0.) Feature threshold for centering (addfeat= no) Add features from a line list? (coordli= linelists$idhenear.dat) User coordinate list (match = -3.) Coordinate list matching limit (maxfeat= 50) Maximum number of features for automatic identif (minsep = 2.) Minimum pixel separation (databas= database) Database (logfile= logfile) List of log files (plotfil= ) Plot file for residuals (verbose= yes) Verbose output? (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input answer = yes Fit dispersion function interactively? crval = Approximate coordinate (at reference pixel) cdelt = Approximate dispersion (aidpars= ) Automatic identification algorithm parameters

1dec05.0330.0327.ms has an RMS of 1.27, as it is not an arc (image deleted). I keep getting errors when I try to extract an arc using this star as a reference, so I will continue to work on it.

I ran refspec using a .cl file, refspec.cl, for each day's data.

noao.imred.specred.refspectra

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = refspectra input = teststar.ms.fits List of input spectra (referen= testarc.ms.fits) List of reference spectra (apertur= ) Input aperture selection list (refaps = ) Reference aperture selection list (ignorea= no) Ignore input and reference apertures? (select = average) Selection method for reference spectra (sort = jd) Sort key (group = ljd) Group key (time = no) Is sort key a time? (timewra= 17.) Time wrap point for time sorting (overrid= no) Override previous assignments? (confirm= yes) Confirm reference spectrum assignments? (assign = yes) Assign the reference spectra to the input spectrum? (logfile= STDOUT,logfile) List of logfiles (verbose= no) Verbose log output? answer = YES Accept assignment?

I ran dispcor on all the stars.

noao.imred.specred.dispcor

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = dispcor input = @starsms.list List of input spectra output = w//@starsms.list List of output spectra (lineari= yes) Linearize (interpolate) spectra? (databas= database) Dispersion solution database (table = ) Wavelength table for apertures (w1 = 3513.) Starting wavelength (w2 = 5520.) Ending wavelength (dw = 0.75) Wavelength interval per pixel (nw = 2685) Number of output pixels (log = no) Logarithmic wavelength scale? (flux = yes) Conserve flux? (samedis= no) Same dispersion in all apertures? (global = no) Apply global defaults? (ignorea= no) Ignore apertures? (confirm= no) Confirm dispersion coordinates? (listonl= no) List the dispersion coordinates only? (verbose= yes) Print linear dispersion assignments? (logfile= ) Log file

Using the log, I double-checked the headers, and corrected the few which were incorrectly labeled.