Iraf Parameters

Each flat and twilight was normalized using response.

noao.imred.specred.response

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = response calibrat= Flat_ub.fits Longslit calibration images normaliz= Flat_ub.fits Normalization spectrum images response= nFlat_ub.fits Response function images (interac= yes) Fit normalization spectrum interactively? (thresho= 100.) Response threshold (sample = 400:3700) 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

noao.imred.specred.response
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = response calibrat= Flat_ub.fits Longslit calibration images normaliz= Flat_ub.fits Normalization spectrum images response= nFlat_ub.fits Response function images (interac= yes) Fit normalization spectrum interactively? (thresho= 100.) Response threshold (sample = 400:3700) 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

Before the flatfielding could be completed, CCDSEC in each header had to be changed to match the size of the image after chopping. (everything before flatfielding was done by Dan before I got the data)

noao.imred.ccdred.ccdproc

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= object) 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= no) Apply overscan strip correction? (trim = no) Trim the image? (zerocor= no) Apply zero level correction? (darkcor= no) Apply dark count correction? (flatcor= yes) 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= column) 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 = ../../nFlat_bb.fits) 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= no) Fit overscan interactively? (functio= chebyshev) Fitting function (order = 2) 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 = 0.) Rejection growing radius

noao.imred.ccdred.ccdproc
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= object) 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= no) Apply overscan strip correction? (trim = no) Trim the image? (zerocor= no) Apply zero level correction? (darkcor= no) Apply dark count correction? (flatcor= yes) 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= column) 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 = ../../nFlat_bb.fits) 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= no) Fit overscan interactively? (functio= chebyshev) Fitting function (order = 2) 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 = 0.) Rejection growing radius

I used apall to extract the spectra. For the last night of observing, the aperture parameters 'upper' and 'lower' were changed to 4 and -4.

noao.imred.specred.apall

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = apall input = testbright4.fits 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 = no) 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 = -100) Number of dispersion lines to sum or median # DEFAULT APERTURE PARAMETERS (lower = -8.) Lower aperture limit relative to center (upper = 8.) 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= -50:-30,30:50) 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 = -8.) Lower aperture limit relative to center (ulimit = 8.) Upper aperture limit relative to center (ylevel = 0.1) Fraction of peak or intensity for automatic wid (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 bef (t_funct= legendre) Trace fitting function (t_order= 3) 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= INDEF) Saturation level (readnoi= 5) Read out noise sigma (photons) (gain = 1.16) Photon gain (photons/data number) (lsigma = 4.) Lower rejection threshold (usigma = 4.) Upper rejection threshold (nsubaps= 1) Number of subapertures per aperture

noao.imred.specred.apall
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = apall input = testbright4.fits 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 = no) 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 = -100) Number of dispersion lines to sum or median # DEFAULT APERTURE PARAMETERS (lower = -8.) Lower aperture limit relative to center (upper = 8.) 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= -50:-30,30:50) 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 = -8.) Lower aperture limit relative to center (ulimit = 8.) Upper aperture limit relative to center (ylevel = 0.1) Fraction of peak or intensity for automatic wid (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 bef (t_funct= legendre) Trace fitting function (t_order= 3) 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= INDEF) Saturation level (readnoi= 5) Read out noise sigma (photons) (gain = 1.16) Photon gain (photons/data number) (lsigma = 4.) Lower rejection threshold (usigma = 4.) Upper rejection threshold (nsubaps= 1) Number of subapertures per aperture

I used a combination of long arcs (made by Dr. Harding) longcuarne_01_blk to run identify, and then used reidentify on all the other arcs.

noao.imred.specred.identify

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = identify images = longcuarne_01_blk Images containing features to be identified (section= middle col) Section to apply to two dimensional images (databas= database) Database in which to record feature data (coordli= database/wht_cuarne_blue.dat) User coordinate list (units = ) Coordinate units (nsum = 10) Number of lines/columns/bands to sum in 2D image (match = -3.) Coordinate list matching limit (maxfeat= 100) Maximum number of features for automatic identif (zwidth = 100.) Zoom graph width in user units (ftype = emission) Feature type (fwidth = 4.) Feature width in pixels (cradius= 5.) Centering radius in pixels (thresho= 0.) Feature threshold for centering (minsep = 2.) Minimum pixel separation (functio= spline3) Coordinate function (order = 1) Order of coordinate function (sample = *) Coordinate sample regions (niterat= 0) Rejection iterations (low_rej= 2.5) Lower rejection sigma (high_re= 2.5) Upper rejection sigma (grow = 0.) Rejection growing radius (autowri= no) Automatically write to database (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input crval = Approximate coordinate (at reference pixel) cdelt = Approximate dispersion (aidpars= ) Automatic identification algorithm parameters

noao.imred.specred.identify
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = identify images = longcuarne_01_blk Images containing features to be identified (section= middle col) Section to apply to two dimensional images (databas= database) Database in which to record feature data (coordli= database/wht_cuarne_blue.dat) User coordinate list (units = ) Coordinate units (nsum = 10) Number of lines/columns/bands to sum in 2D image (match = -3.) Coordinate list matching limit (maxfeat= 100) Maximum number of features for automatic identif (zwidth = 100.) Zoom graph width in user units (ftype = emission) Feature type (fwidth = 4.) Feature width in pixels (cradius= 5.) Centering radius in pixels (thresho= 0.) Feature threshold for centering (minsep = 2.) Minimum pixel separation (functio= spline3) Coordinate function (order = 1) Order of coordinate function (sample = *) Coordinate sample regions (niterat= 0) Rejection iterations (low_rej= 2.5) Lower rejection sigma (high_re= 2.5) Upper rejection sigma (grow = 0.) Rejection growing radius (autowri= no) Automatically write to database (graphic= stdgraph) Graphics output device (cursor = ) Graphics cursor input crval = Approximate coordinate (at reference pixel) cdelt = Approximate dispersion (aidpars= ) Automatic identification algorithm parameters

noao.imred.specred.identify

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = reidentify referenc= longcuarne_01_blk Reference image images = testarc3.ms.fits Images to be reidentified (interac= yes) Interactive fitting? (section= middle col) Section to apply to two dimensional images (newaps = yes) Reidentify apertures in images not in reference? (overrid= yes) 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 = 0) 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= database/wht_cuarne_blue.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= no) 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

noao.imred.specred.identify
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = reidentify referenc= longcuarne_01_blk Reference image images = testarc3.ms.fits Images to be reidentified (interac= yes) Interactive fitting? (section= middle col) Section to apply to two dimensional images (newaps = yes) Reidentify apertures in images not in reference? (overrid= yes) 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 = 0) 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= database/wht_cuarne_blue.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= no) 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

I then ran refspectra using an @file to associate arcs with spectra.

noao.imred.specred.refspectra

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = refspectra input = r748413.ms.fits List of input spectra (referen= testarc3.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= yes) Override previous assignments? (confirm= no) Confirm reference spectrum assignments? (assign = yes) Assign the reference spectra to the input spectr (logfile= STDOUT,logfile) List of logfiles (verbose= yes) Verbose log output? answer = yes Accept assignment?

noao.imred.specred.refspectra
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = refspectra input = r748413.ms.fits List of input spectra (referen= testarc3.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= yes) Override previous assignments? (confirm= no) Confirm reference spectrum assignments? (assign = yes) Assign the reference spectra to the input spectr (logfile= STDOUT,logfile) List of logfiles (verbose= yes) Verbose log output? answer = yes Accept assignment?

I then ran dispcor to set the wavelength scale for the spectra.

noao.imred.specred.identify

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = dispcor input = @stars List of input spectra output = w//@stars List of output spectra (lineari= yes) Linearize (interpolate) spectra? (databas= database) Dispersion solution database (table = ) Wavelength table for apertures (w1 = 3660.) Starting wavelength (w2 = 5380.) Ending wavelength (dw = 0.438) Wavelength interval per pixel (nw = 4099) Number of output pixels (log = no) Logarithmic wavelength scale? (flux = yes) Conserve flux? (blank = 0.) Output value of points not in input (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

noao.imred.specred.identify
I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = dispcor input = @stars List of input spectra output = w//@stars List of output spectra (lineari= yes) Linearize (interpolate) spectra? (databas= database) Dispersion solution database (table = ) Wavelength table for apertures (w1 = 3660.) Starting wavelength (w2 = 5380.) Ending wavelength (dw = 0.438) Wavelength interval per pixel (nw = 4099) Number of output pixels (log = no) Logarithmic wavelength scale? (flux = yes) Conserve flux? (blank = 0.) Output value of points not in input (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

I used the following parameters for all my runs of fxcor.

noao.rv.fxcor

I R A F Image Reduction and Analysis Facility PACKAGE = rv TASK = fxcor objects = @stdsred List of object spectra template= BD+01_2916_template2.ms List of template spectra (apertur= *) Apertures to be used (cursor = ) Graphics input cursor (continu= object) Continuum subtract spectra? (filter = both) Fourier filter the spectra? (rebin = smallest) Rebin to which dispersion? (pixcorr= no) Do a pixel-only correlation? (osample= *) Object regions to be correlated ('*' => all) (rsample= *) Template regions to be correlated (apodize= 0.25) Apodize end percentage (functio= gaussian) Function to fit correlation (width = 9.) Width of fitting region in pixels (height = 0.) Starting height of fit (peak = no) Is height relative to ccf peak? (minwidt= 3.) Minimum width for fit (maxwidt= 21.) Maximum width for fit (weights= 1.) Power defining fitting weights (backgro= 0.) Background level for fit (window = INDEF) Size of window in the correlation plot (wincent= INDEF) Center of peak search window (output = rv) Root spool filename for output (verbose= txtonly) Verbose output to spool file? (imupdat= no) Update the image header? (graphic= stdgraph) Graphics output device (interac= no) Interactive graphics? (autowri= yes) Automatically record results? (autodra= yes) Automatically redraw fit results? (ccftype= image) Output type of ccf (observa= lapalma) Observation location database (continp= ) Continuum processing parameters (filtpar= ) Filter parameters pset (keywpar= ) Header keyword translation pset

noao.rv.fxcor
I R A F Image Reduction and Analysis Facility PACKAGE = rv TASK = fxcor objects = @stdsred List of object spectra template= BD+01_2916_template2.ms List of template spectra (apertur= ) Apertures to be used (cursor = ) Graphics input cursor (continu= object) Continuum subtract spectra? (filter = both) Fourier filter the spectra? (rebin = smallest) Rebin to which dispersion? (pixcorr= no) Do a pixel-only correlation? (osample= ) Object regions to be correlated ('' => all) (rsample= ) Template regions to be correlated (apodize= 0.25) Apodize end percentage (functio= gaussian) Function to fit correlation (width = 9.) Width of fitting region in pixels (height = 0.) Starting height of fit (peak = no) Is height relative to ccf peak? (minwidt= 3.) Minimum width for fit (maxwidt= 21.) Maximum width for fit (weights= 1.) Power defining fitting weights (backgro= 0.) Background level for fit (window = INDEF) Size of window in the correlation plot (wincent= INDEF) Center of peak search window (output = rv) Root spool filename for output (verbose= txtonly) Verbose output to spool file? (imupdat= no) Update the image header? (graphic= stdgraph) Graphics output device (interac= no) Interactive graphics? (autowri= yes) Automatically record results? (autodra= yes) Automatically redraw fit results? (ccftype= image) Output type of ccf (observa= lapalma) Observation location database (continp= ) Continuum processing parameters (filtpar= ) Filter parameters pset (keywpar= ) Header keyword translation pset

These are the parameters used for all runs of fxcor.

noao.rv.continpars

(c_inter= no) Fit continuum interactively? (c_sampl= *) Sample of points to use in fit (c_funct= spline3) Fitting function (spline3|legendre|chebyshev|spline1) (naverag= 1) Number of points in sample averaging (order = 19) Order of fitting function (replace= no) Replace rejected spectrum w/ fit? (low_rej= 2.) Low rejection in sigma of fit (high_re= 5.) High rejection in sigma of fit (niterat= 5) Number of rejection iterations (grow = 1.) Rejection growing radius

noao.rv.continpars
(c_inter= no) Fit continuum interactively? (c_sampl= *) Sample of points to use in fit (c_funct= spline3) Fitting function (spline3\|legendre\|chebyshev\|spline1) (naverag= 1) Number of points in sample averaging (order = 19) Order of fitting function (replace= no) Replace rejected spectrum w/ fit? (low_rej= 2.) Low rejection in sigma of fit (high_re= 5.) High rejection in sigma of fit (niterat= 5) Number of rejection iterations (grow = 1.) Rejection growing radius

noao.rv.filtpars

(f_type = ramp) Filter window type (cuton = 35) Cuton component for filter (cutoff = 1000) Cutoff component for filter (fullon = 50) Component at which (ramp) filter reaches full va (fulloff= 1200) Component at which (ramp) filter reaches zero

noao.rv.filtpars
(f_type = ramp) Filter window type (cuton = 35) Cuton component for filter (cutoff = 1000) Cutoff component for filter (fullon = 50) Component at which (ramp) filter reaches full va (fulloff= 1200) Component at which (ramp) filter reaches zero

noao.rv.keywpars

(ra = RA) Right Ascension keyword (dec = DEC) Declination keyword (ut = UT) UT of observation keyword (utmiddl= UTMIDDLE) UT of mid-point of observation keyword (exptime= EXPTIME) Exposure time keyword (epoch = EPOCH) Epoch of observation keyword (date_ob= DATE-OBS) Date of observation keyword (hjd = HJD) Heliocentric Julian date keyword (mjd_obs= MJD-OBS) Modified Julian Date of observation keyword (vobs = VOBS) Observed velocity keyword (vrel = VREL) Relative velocity keyword (vhelio = VHELIO) Heliocentric velocity keyword (vlsr = VLSR) LSR velocity keyword (vsun = VSUN) Epoch of solar motion keyword

noao.rv.keywpars
(ra = RA) Right Ascension keyword (dec = DEC) Declination keyword (ut = UT) UT of observation keyword (utmiddl= UTMIDDLE) UT of mid-point of observation keyword (exptime= EXPTIME) Exposure time keyword (epoch = EPOCH) Epoch of observation keyword (date_ob= DATE-OBS) Date of observation keyword (hjd = HJD) Heliocentric Julian date keyword (mjd_obs= MJD-OBS) Modified Julian Date of observation keyword (vobs = VOBS) Observed velocity keyword (vrel = VREL) Relative velocity keyword (vhelio = VHELIO) Heliocentric velocity keyword (vlsr = VLSR) LSR velocity keyword (vsun = VSUN) Epoch of solar motion keyword

I used scombine to combine all observations of each standard. I also used it, with the following parameters, to combine all observations of each program object. I used this cl file to run it.

noao.imred.specred.scombine

I R A F Image Reduction and Analysis Facility PACKAGE = specred TASK = scombine input = wr750489.ms.fits,wr750492.ms.fits List of input spectra output = M71_H30_sc.ms List of output spectra (noutput= ) List of output number combined spectra (logfile= STDOUT) Log file (apertur= ) Apertures to combine (group = apertures) Grouping option (combine= average) Type of combine operation (reject = ccdclip) Type of rejection (first = no) Use first spectrum for dispersion? (w1 = INDEF) Starting wavelength of output spectra (w2 = INDEF) Ending wavelength of output spectra (dw = INDEF) Wavelength increment of output spectra (nw = INDEF) Length of output spectra (log = no) Logarithmic increments? (scale = median) Image scaling (zero = none) Image zero point offset (weight = none) Image weights (sample = ) Wavelength sample regions for statistics (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= 15) ccdclip: CCD readout noise (electrons) (gain = 1.16) 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 1D neighbor rejection (blank = 0.) Value if there are no pixels (mode = ql)