PACKAGE = images.immatchTASK = imcombine

input = bi*.fit List of images to combineoutput = zero.fit List of output images(rejmask= ) List of rejection masks (optional)(plfile = ) List of pixel list files (optional)(sigma = ) List of sigma images (optional)(logfile= STDOUT) Log file

(combine= median) 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 = median) Image scaling(zero = none) Image zero point offset(weight = none) Image weights(statsec= ) Image section for computing statistics(expname= ) Image header exposure time keyword

Combine Bias

(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(mode = ql)

Combined bias (zero.fits)

files *.fits > listaRemove bi*.fits from lista

PACKAGE = images.imutilTASK = imarith

operand1= @lista Operand image or numerical constantop = - Operatoroperand2= zero.fits Operand image or numerical constantresult = @lista Resultant image(title = ) Title for resultant image(divzero= 0.) Replacement value for division by zero(hparams= ) List of header parameters(pixtype= ) Pixel type for resultant image(calctyp= ) Calculation data type(verbose= yes) Print operations?(noact = no) Print operations without performing them?(mode = ql)

Images should have (close to) zero counts

Bias remotion

PACKAGE = immatchTASK = imcombine

input = ff*.fits List of images to combineoutput = flat.fits List of output images(rejmask= ) List of rejection masks (optional)(plfile = ) List of pixel list files (optional)(sigma = ) List of sigma images (optional)(logfile= STDOUT) Log file

(combine= median) Type of combine operation(reject = none) Type of rejection(project= no) Project highest dimension of input images?(outtype= real) Output image pixel datatype(offsets= none) Input image offsets(masktyp= none) Mask type(maskval= 0.) Mask value(blank = 0.) Value if there are no pixels

(scale = median) Image scaling(zero = none) Image zero point offset(weight = none) Image weights(statsec= ) Image section for computing statistics(expname= ) Image header exposure time keyword

Combine Flats

(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(mode = ql)

Combined Flat (flat.fits)

Make a good fit in response function changing the order of fitting function

PACKAGE = noao.twodspec.longslitTASK = response

calibrat= flat.fits Longslit calibration imagesnormaliz= flat.fits Normalization spectrum imagesresponse= flatfin.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= spline3) Fitting function(order = 20) Order of fitting function(low_rej= 0.) Low rejection in sigma of fit(high_re= 0.) 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(mode = ql)

Fit the normalization spectrum for flat.fits interactively (yes): yDispersion axis (1=along lines, 2=along columns, 3=along z) (1:3) (1): 1

Response function of Flats

Interactive fitting: try to make a good fit increasing the order with

o: # where # is the order of the functionf to fith x vs. y fitingl x vs. n (non linear part)j x vs. r (residuals)q quit once a good fit is made

Final flat field

Remove Flat field

Delete ff*.fits from lista

PACKAGE = imutilTASK = imarith

operand1= @lista Operand image or numerical constantop = / Operatoroperand2= flatfin.fits Operand image or numerical constantresult = @lista Resultant image(title = ) Title for resultant image(divzero= 0.) Replacement value for division by zero(hparams= ) List of header parameters(pixtype= ) Pixel type for resultant image(calctyp= ) Calculation data type(verbose= yes) Print operations?(noact = no) Print operations without performing them?(mode = ql)

PACKAGE = noao.imred.crutilTASK = cosmicrays

input = n4151.fits List of images in which to detect cosmic raysoutput = n4151nc.fits List of cosmic ray replaced output images (optio(badpix = ) List of bad pixel files (optional)(thresho= 20.) Detection threshold above mean(fluxrat= 10.) Flux ratio threshold (in percent)(npasses= 5) Number of detection passes(window = 5) Size of detection window(interac= no) Examine parameters interactively?answer = no) Examine parameters interactively?(train = no) Use training objects?(objects= ) Cursor list of training objects(savefil= ) File to save train objects(verbose= yes) Print log information to the standard output?(logfile= ) Text log file(plotfil= ) Log metacode plot file(graphic= stdgraph) Interactive graphics output device(cursor = ) Graphics cursor input(ccdtype= )(instrum= )(mode = ql)

Review parameters for a particular image? (no|yes|NO|YES) (yes): N

Repeat for standard star bd75325

Remove cosmic rays

Image with cosmic rays

Remove remnant cosmic rays

PACKAGE = images.tvTASK = imedit

input = n4151nc.fits Images to be editedoutput = n4151ncc.fits Output images(cursor = y) Cursor input(logfile= ) Logfile for record of cursor commands(display= yes) Display images?(autodis= yes) Automatic image display?(autosur= yes) Automatic surface plots?(apertur= circular) Aperture type(radius = 2.) Substitution radius(search = 2.) Search radius(buffer = 1.) Background buffer width(width = 2.) Background width(xorder = 2) Background x order(yorder = 2) Background y order(value = 0.) Constant value substitution(sigma = INDEF) Added noise sigma(angh = -33.) Horizontal viewing angle (degrees)(angv = 25.) Vertical viewing angle (degrees)(command= display $image 1 erase=$erase fill=yes order=0 >& dev$null) Display co(graphic= stdgraph) Graphics device(default= b) Default option for x-y input(fixpix = no) Fixpix style input?(mode = ql)

Interactive remotion keystrokes:b background replacement (aperture)+ increase radius- decrease radius

Q quit without saveq quit and save

Repeat for standard star

Removing cosmic rays

Image without cosmic rays

Sky lines

Calibration HeAr lamp

PACKAGE = noao.twodspec.longslitTASK = identify

images = lamp.fits Images containing features to be identified(section= middle line) Section to apply to two dimensional images(databas= database) Database in which to record feature data(coordli= linelists$idhear_br.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= 50) 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= 3.) Lower rejection sigma(high_re= 3.) Upper rejection sigma(grow = 0.) Rejection growing radius(autowri= no) Automatically write to database(graphic= stdgraph) Graphics output device

Write feature data to the database (yes)? y

Identify lamp lines

keystrokes:m mark a line and identify itf make a fitq quit

Mark and identify some lines

Make a good fit

PACKAGE = longslitTASK = reidentify

referenc= lamp Reference imageimages = lamp Images to be reidentified(interac= no) 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 = yes) Trace reference image?(step = 5) 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= linelists$idhear_br.dat) User coordinate list(match = -3.) Coordinate list matching limit(maxfeat= 50) Maximum number of features for automaticidentif(minsep = 2.) Minimum pixel separation

Reidentify lamp lines

Put header

PACKAGE = images.imutilTASK = hedit

images = n4151ncc.fits,bd75325ncc.fits images to be editedfields = REFSPEC1 fields to be editedvalue = lamp value expression(add = yes) add rather than edit fields(delete = no) delete rather than edit fields(verify = yes) verify each edit operation(show = yes) print record of each edit operation(update = yes) enable updating of the image header(mode = )

add n4151ncc.fits,REFSPEC1 = lampupdate n4151ncc.fits ? (yes): yadd bd75325ncc.fits,REFSPEC1 = lampupdate bd75325ncc.fits ? (yes): bd75325ncc.fits updated

PACKAGE = longslitTASK = fitcoords

images = lamp Images whose coordinates are to be fit(fitname= lamp) Name for coordinate fit in the database(interac= yes) Fit coordinates interactively?(combine= no) Combine input coordinates for a single fit?(databas= database) Database(deletio= deletions.db) Deletion list file (not used if null)(functio= chebyshev) Type of fitting function(xorder = 4) X order of fitting function(yorder = 1) Y order of fitting function(logfile= STDOUT,logfile) Log files(plotfil= plotfile) Plot log file(graphic= stdgraph) Graphics output device(cursor = ) Graphics cursor input(mode = ql)

Fit lamp interactively (yes): y

Fit coordinates

Fit coordinateskeystrokes:xo,yo change x,y orders of fittingd p delete points f fitq quit

PACKAGE = longslitTASK = transform

input = n4151ncc.fits,bd75325ncc.fits Input imagesoutput = n4151t.fits,bd75325t.fits Output imagesfitnames= lamplamp Names of coordinate fits in the database(databas= database) Identify database(interpt= spline3) Interpolation type(x1 = INDEF) Output starting x coordinate(x2 = INDEF) Output ending x coordinate(dx = INDEF) Output X pixel interval(nx = INDEF) Number of output x pixels(xlog = no) Logarithmic x coordinate?(y1 = INDEF) Output starting y coordinate(y2 = INDEF) Output ending y coordinate(dy = INDEF) Output Y pixel interval(ny = INDEF) Number of output y pixels(ylog = no) Logarithmic y coordinate?(flux = yes) Conserve flux per pixel?(logfile= STDOUT,logfile) List of log files(mode = ql)

Dispersion axis (1=along lines, 2=along columns, 3=along z) (1:3) (1): 1

Transform pixels to wavelength

Object calibrated in wavelength

PACKAGE = longslitTASK = background

input = n4151t.fits Input images to be background subtractedoutput = n4151b.fits Output background subtracted images(axis = 2) Axis along which background is fit and subtracte(interac= yes) Set fitting parameters interactively?(sample = *) Sample of points to use in fit(naverag= 1) Number of points in sample averaging(functio= chebyshev) Fitting function(order = 3) Order of fitting function(low_rej= 0.) Low rejection in sigma of fit(high_re= 0.) 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(mode = ql)

Fit Column= 512

Repeat for standard

Remove background

Keystrokes:s to mark level to substractq quit

s s ss

Image without background should not have sky lines

PACKAGE = noao.twodspec.apextractTASK = apall

input = n4151b.fits List of input images(output = NGC4151.fits) List of output spectra(apertur= 1) 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 = 10) 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)

Extract spectrum

# DEFAULT BACKGROUND PARAMETERS

(b_funct= chebyshev) Background function(b_order= 1) Background function order(b_sampl= -10:-6,6:10) Background sample regions(b_naver= -3) 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 = 5.) 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?

Extract spectrum (cont…)# RECENTERING PARAMETERS

(aprecen= ) Apertures for recentering calculation(npeaks = INDEF) Select brightest peaks(shift = yes) Use average shift instead of recentering?

# RESIZING PARAMETERS

(llimit = INDEF) Lower aperture limit relative to center(ulimit = INDEF) 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 = 10) Number of dispersion lines to sum(t_step = 10) Tracing step(t_nlost= 3) Number of consecutive times profile is lost befo(t_funct= spline3) Trace fitting function(t_order= 2) Trace fitting function order(t_sampl= *) Trace sample regions(t_naver= 1) Trace average or median(t_niter= 0) 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= none) Background to subtract(skybox = 1) Box car smoothing length for sky(weights= none) Extraction weights (none|variance)(pfit = fit1d) Profile fitting type (fit1d|fit2d)(clean = no) Detect and replace bad pixels?(saturat= INDEF) Saturation level(readnoi= 0.) 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(mode = ql)

Find apertures for n4151b.fits ? (yes): yNumber of apertures to be found automatically (1): 1Resize apertures for n4151b.fits ? (yes): yEdit apertures for n4151b.fits ? (yes): y

Keystrokes:l lower limit of apertureu upper limitq quitd p delete a pointf fit

Resize apertures with keystrokes u & l

Spectrum aperture fitting

Delete departing points

Extracted spectrum

Verify with splot NGC4151.fitsshould be calibrated in wavelengthRepeat for Standard star

Resize standard apertures with keystrokes u & l

Standard spectrum aperture fitting

Standard Spectrum extracted

Standard Spectrum calibrated in wavelength

Extract one-dimensional spectrum of standard star

PACKAGE = noao.onedspecTASK = standard

input = BD+75325.fits Input image file root nameoutput = std Output flux file (used by SENSFUNC)(samesta= yes) Same star in all apertures?(beam_sw= no) Beam switch spectra?(apertur= ) Aperture selection list(bandwid= INDEF) Bandpass widths(bandsep= INDEF) Bandpass separation(fnuzero= 3.6800000000000E-20) Absolute flux zero point(extinct= onedstds$kpnoextinct.dat) Extinction file(caldir = onedstds$local/) Directory containing calibration(observa= oagh) Observatory for data(interac= yes) Graphic interaction to define new bandpasses(graphic= stdgraph) Graphics output device(cursor = ) Graphics cursor inputstar_nam= bd75d325 Star name in calibration listairmass = 1.4 Airmassexptime = 600 Exposure time (seconds)answer = y (no|yes|NO|YES|NO!|YES!)(mode = ql)

Edit absorption linesKeystrokes:d delete featuresshift x resolutionr redrawq quit

PACKAGE = onedspecTASK = sensfunc

standard= std Input standard star data file (from STANDARD)sensitiv= sens Output root sensitivity function imagename(apertur= ) Aperture selection list(ignorea= no) Ignore apertures and make one sensitivity functi(logfile= logfile) Output log for statistics information(extinct= onedstds$kpnoextinct.dat) Extinction file(newexti= extinct.dat) Output revised extinction file(observa= oagh) Observatory of data(functio= spline3) Fitting function(order = 6) Order of fit(interac= yes) Determine sensitivity function interactively?(graphs = sri) Graphs per frame(marks = plus cross box) Data mark types (marks deleted added)(colors = 2 1 3 4) Colors (lines marks deleted added)(cursor = sri) Graphics cursor input(device = stdgraph) Graphics output deviceanswer = yes (no|yes|NO|YES)(mode = ql)

No extinction correction appliedFit aperture 1 interactively? (no|yes|NO|YES): Y

Sensitivity function

Keystrokes:d p delete pointr redraw-fito change order of funct.

Sensitivity function fitting

Flux calibration of standardPACKAGE = onedspecTASK = calibrate

input = BD+75325.fits Input spectra to calibrateoutput = BD+75325C.fits Output calibrated spectra(extinct= yes) Apply extinction correction?(flux = yes) Apply flux calibration?(extinct= onedstds$kpnoextinct.dat) Extinction file(observa= oagh) Observatory of observation(ignorea= no) Ignore aperture numbers in flux calibration?(sensiti= sens) Image root name for sensitivity spectra(fnu = no) Create spectra having units of FNU?airmass = 1.4 Airmassexptime = 1800 Exposure time (seconds)(mode = ql)

BD+75325C.fits:Extinction correction appliedFlux calibration applied

Standard calibrated in flux

Flux calibration of object

PACKAGE = onedspecTASK = calibrate

input = NGC4151.fits Input spectra to calibrateoutput = NGC4151C.fits Output calibrated spectra(extinct= yes) Apply extinction correction?(flux = yes) Apply flux calibration?(extinct= onedstds$kpnoextinct.dat) Extinction file(observa= oagh) Observatory of observation(ignorea= no) Ignore aperture numbers in flux calibration?(sensiti= sens) Image root name for sensitivity spectra(fnu = no) Create spectra having units of FNU?airmass = 1.1 Airmassexptime = 1800 Exposure time (seconds)(mode = ql)

NGC4151C.fits:Extinction correction appliedFlux calibration applied

Object calibrated in flux