./0040755000047000001600000000000011064041137007630 5ustar irafiraf./bin0120777000047000001600000000000011064041122012417 2bin.genericustar irafiraf./bin.cygwin0120777000047000001600000000000011064041137015435 2../irafbin/bin.cygwinustar irafiraf./bin.freebsd0120777000047000001600000000000011064041137015661 2../irafbin/bin.freebsdustar irafiraf./bin.generic/0040755000047000001600000000000010745164214012022 5ustar irafiraf./bin.linux0120777000047000001600000000000011064041137015133 2../irafbin/bin.linuxustar irafiraf./noao/0040755000047000001600000000000011063566640010576 5ustar irafiraf./noao/artdata/0040755000047000001600000000000011063566640012216 5ustar irafiraf./noao/artdata/artdata.cl0100644000047000001600000000042404771252377014162 0ustar irafiraf#{ ARTDATA - Artificial data package package artdata task gallist, mk1dspec, mk2dspec, mkechelle, mkheader, mknoise, mkobjects, mkpattern, starlist = "artdata$x_artdata.e" set mkexamples = "artdata$mkexamples/" task mkexamples = "mkexamples$mkexamples.cl" clbye() ./noao/artdata/artdata.hd0100644000047000001600000000131304771252472014151 0ustar irafiraf# Help directory for the ARTDATA package. $defdir = "noao$artdata/" $doc = "noao$artdata/doc/" $lists = "noao$artdata/lists/" $mkexamples = "noao$artdata/mkexamples/" gallist hlp=doc$gallist.hlp, src=lists$t_gallist.x mk1dspec hlp=doc$mk1dspec.hlp, src=t_mk1dspec.x mk2dspec hlp=doc$mk2dspec.hlp, src=t_mk2dspec.x mkechelle hlp=doc$mkechelle.hlp, src=t_mkechelle.x mkexamples hlp=doc$mkexamples.hlp, src=mkexamples$mkexamples.cl mkheader hlp=doc$mkheader.hlp, src=t_mkheader.x mknoise hlp=doc$mknoise.hlp, src=t_mknoise.x mkobjects hlp=doc$mkobjects.hlp, src=t_mkobjects.x mkpattern hlp=doc$mkpattern.hlp, src=t_mkpattern.x starlist hlp=doc$starlist.hlp, src=lists$t_starlist.x revisions sys=Revisions ./noao/artdata/artdata.men0100644000047000001600000000106304771252427014337 0ustar irafiraf gallist - Make an artificial galaxies list mk1dspec - Make/add artificial 1D spectra mk2dspec - Make/add artificial 2D spectra using 1D spectra templates mkechelle - Make artificial 1D and 2D echelle spectra mkexamples - Make artificial data examples mkheader - Append/replace header parameters mknoise - Make/add noise and cosmic rays to 1D/2D images mkobjects - Make/add artificial stars and galaxies to 2D images mkpattern - Make/add patterns to images starlist - Make an artificial star list ./noao/artdata/artdata.par0100644000047000001600000000103406273671237014343 0ustar irafiraf# ARTDATA - Artificial data package nxc,i,h,5,1,,Number of PSF centers per pixel in X nyc,i,h,5,1,,Number of PSF centers per pixel in Y nxsub,i,h,10,1,,Number of pixel subsamples in X nysub,i,h,10,1,,Number of pixel subsamples in Y nxgsub,i,h,5,1,,Number of galaxy pixel subsamples in X nygsub,i,h,5,1,,Number of galaxy pixel subsamples in Y dynrange,r,h,100000.,2.,,Profile intensity dynamic range psfrange,r,h,10.,2.,,PSF convolution dynamic range ranbuf,i,h,0,0,,"Random number buffer size " version,s,h,"V1.1: August 1990" mode,s,h,ql ./noao/artdata/doc/0040755000047000001600000000000006005523024012750 5ustar irafiraf./noao/artdata/doc/gallist.hlp0100644000047000001600000004506111015057124015117 0ustar irafiraf.help gallist Feb90 noao.artdata .ih TASK gallist -- make an artificial galaxies list .ih USAGE gallist gallist ngals .ih PARAMETERS .ls gallist The name of the output text file for the x and y coordinates, magnitudes, profile types, half-flux radii, axial ratios, and position angles of the artificial galaxies. Output will be appended to this file if it exists. .le .ls ngals = 100 The number of galaxies in the output galaxies list. .le .ls interactive = no Examine plots and change the parameters of the spatial, luminosity, and morphology distributions interactively. .le SPATIAL DISTRIBUTION .ls spatial = "uniform" Type of spatial distribution for the galaxies. The types are: .ls uniform The galaxies are uniformly distributed between \fIxmin\fR, \fIxmax\fR, \fIymin\fR, and \fIymax\fR. .le .ls hubble The galaxies are distributed around the center of symmetry \fIxcenter\fR and \fIycenter\fR according to a Hubble density law of core radius \fIcore_radius\fR and background density \fIbase\fR. .le .ls file The radial density function is contained in the text file \fIsfile\fR. .le .le .ls xmin = 1., xmax = 512., ymin = 1., ymax = 512. The range of the output coordinates in pixels. .le .ls xcenter = INDEF, ycenter = INDEF The coordinate of the center of symmetry for the "hubble" and "file" radial density functions. The default is the midpoint of the coordinate limits. .le .ls core_radius = 50 The core radius of the Hubble density distribution in pixels. .le .ls base = 0.0 The background density relative to the central density of the Hubble density distribution. .le .ls sseed = 2 The initial value supplied to the random number generator used to generate the output x and y coordinates. If a value of "INDEF" is given then the clock time (integer seconds since 1980) is used as the seed yielding different random numbers for each execution. .le MAGNITUDE DISTRIBUTION .ls luminosity = "powlaw" Type of luminosity distribution for the galaxies. The types are: .ls uniform The galaxies are uniformly distributed between \fIminmag\fR and \fImaxmag\fR. .le .ls powlaw The galaxies are distributed according to a power law with coefficient \fIpower\fR. .le .ls schecter The galaxies are distributed according to a Schecter luminosity function with characteristic magnitude \fImstar\fR and power law exponent \fIalpha\fR between \fIminmag\fR and \fImaxmag\fR. .le .ls file The luminosity function is contained in the text file \fIlfile\fR. .le .le .ls minmag = -7., maxmag = 0. The range of output relative magnitudes. .le .ls mzero = 15. Magnitude zero point for Schecter luminosity function. .le .ls power = 0.6 Coefficient for the power law magnitude distribution The default value of 0.6 is the Euclidean value. .le .ls alpha = -1.24 The power law exponent of the Schecter luminosity function. The default value is that determined by Schecter from nearby galaxies. .le .ls mstar = -21.41 The characteristic magnitude of the Schecter luminosity function. .le .ls lseed = 2 The initial value supplied to the random number generator used to generate the output magnitudes. If a value of "INDEF" is given then the clock time (integer seconds since 1980) is used as the seed yielding different random numbers for each execution. .le MORPHOLOGY DISTRIBUTION .ls egalmix = 0.4 The fraction of the galaxies that are "ellipticals" represented by a de Vaucouleurs surface brightness law as opposed to "spirals" represented by an exponential disk surface brightness law. .le .ls ar = 0.3 Minimum elliptical galaxy axial ratio (major/minor ratio). .le .ls eradius = 20.0 The maximum elliptical galaxy half-flux semi-major scale radius. This is the radius of an elliptical galaxy with magnitude \fIminmag\fR before a random factor is added. Spiral galaxies and fainter galaxies are scaled from this value. .le .ls sradius = 1.0 Ratio between half-flux scale radii of spiral and elliptical models at the same magnitude. For example an elliptical galaxy with magnitude \fIminmag\fR will have radius \fIeradius\fR while a spiral galaxy of the same magnitude with have radius \fIsradius\fR * \fIeradius\fR. .le .ls absorption = 1.2 Absorption correction for edge on spirals in magnitudes. .le .ls z = 0.05 Minimum redshift for power law distributed galaxies. This is the redshift assigned galaxies of magnitude \fIminmag\fR. The redshifts are assumed proportional to the square root of the apparent luminosity; i.e the luminosity distance proportional to redshift. The redshift is used for computing the mean apparent sizes of the galaxies according to (1+z)**2 / z. .le USER FUNCTIONS .ls sfile = "" The name of the input text file containing the sampled spatial radial density function, one sample point per line, with the radius and relative probability in columns one and two respectively. The sample points need not be uniformly spaced or normalized. .le .ls nssample = 100 The number of points at which the spatial density function is sampled. If the spatial density function is analytic or approximated analytically (the "hubble" option) the function is sampled directly. If the function is read from a file (the "file" option) an initial smoothing step is performed before sampling. .le .ls sorder = 10 The order of the spline fits used to evaluate the integrated spatial density function. .le .ls lfile = "" The name of the input text file containing the sampled luminosity function, one sample point per line, with the magnitude and relative probability in columns one and two respectively. The sample points need not be uniformly spaced or normalized. .le .ls nlsample = 100 The number of points at which the luminosity function is sampled. If the luminosity function is analytic or approximated analytically (the "uniform", "powlaw" and "schecter" options) the function is sampled directly. If it is read from a file (the "file" option) an initial smoothing step is performed before sampling. .le .ls lorder = 10 The order of the spline fits used to evaluate the integrated luminosity function. .le INTERACTIVE PARAMETERS .ls rbinsize = 10. The bin size in pixels of the plotted histogram of the radial density distribution. .le .ls mbinsize = 0.5 The bin size in magnitudes of the plotted histogram of the luminosity function. .le .ls dbinsize = 0.5 The bin size in pixels of the plotted histogram of the half-power semi-major axis distribution. .le .ls ebinsize = 0.1 The bin size of the plotted histogram of the axial ratio distribution. .le .ls pbinsize = 20. The bin size in degrees of the plotted histogram of the position angle distribution. .le .ls graphics = stdgraph The default graphics device. .le .ls cursor = "" The graphics cursor. .le .ih DESCRIPTION \fBGallist\fR generates a list of x and y coordinates, magnitudes, morphological types, half-power radii, axial ratios, and position angles for a sample of \fIngals\fR galaxies based on a user selected spatial density function \fIspatial\fR and luminosity function \fIluminosity\fR and writes (appends) the results to the text file \fIgallist\fR. If the \fIinteractive\fR parameter is "yes" the user can interactively examine plots of the spatial density function, the radial density function, the luminosity function, radii, axial ratios, and position angle distributions and alter the parameters of the task until a satisfactory artificial field is generated. The spatial density function generates x and y values around a center of symmetry defined by \fIxcenter\fR and \fIycenter\fR within the x and y limits \fIxmin\fR, \fIxmax\fR, \fIymin\fR and \fIymax\fR according to the spatial density function specified by \fIspatial\fR. The three supported spatial density functions are listed below where R is the radial distance in pixels, P is the relative spatial density, C is a constant, and f is the best fitting cubic spline function to the spatial density function R(user), P(user) supplied by the user in the text file \fIsfile\fR. .nf uniform: P = C hubble: P = 1.0 / (1 + R / core_radius) ** 2 + base file: P = f (R(user), P(user)) .fi The Hubble and user spatial density functions are sampled at \fInssample\fR equally spaced points, and integrated to give the spatial density probability function at each sampled point. The integrated probability function is normalized and approximated by a cubic spline of order \fIsorder\fR. The x and y coordinates are computed by randomly sampling the integrated probability function until \fIngals\fR galaxies which satisfy the x and y coordinate limits \fIxmin\fR, \fIxmax\fR, \fIymin\fR and \fIymax\fR are generated. The luminosity function generates relative magnitude values between \fIminmag\fR and \fImaxmag\fR (before absorption effects are added) according to the luminosity function specified by \fIluminosity\fR. The four supported luminosity functions are listed below where M is the magnitude, P is the relative luminosity function, C is a constant and f is the best fitting cubic spline function to the luminosity function M(user), P(user) supplied by the user in the text file \fIlfile\fR. .nf uniform: P = C powlaw: P = C * 10. ** (power * M) schecter: P = C * 10. ** (alpha * dM) * exp (-10. ** dM) file: P = f (M(user), P(user)) where dM = 0.4 * (mstar - M + mzero) .fi The uniform distribution is not very physical but may be useful for testing. The power law distribution is that expected for a homogeneous and isotropic distribution of galaxies. The default value of 0.6 is that which can be calculated simply from Euclidean geometry. Observations of faint galaxies generally show a smaller value. The Schecter function provides a good approximation to a galaxy cluster when used in conjunction with the Hubble spatial distribution (though there is no mass segregation applied). The "best fit" values for the parameters \fImstar\fR and \fIalpha\fR are taken from the paper by Schecter (Ap.J 203, 297, 1976). The \fImzero\fR parameter is used to convert to absolute magnitudes. Note that it is equivalent to set \fImzero\fR to zero and adjust the characteristic magnitude to the same relative magnitude scale or to use absolute magnitudes directly. The Schecter and user file distributions are sampled at \fInlsample\fR equally spaced points, and integrated to give the luminosity probability function at each sampled point. The probability function is normalized and approximated by a cubic spline of order \fIlorder\fR. The magnitudes are computed by randomly sampling the integrated probability function until \fIngals\fR objects which satisfy the magnitude limits \fIminmag\fR and \fImaxmag\fR are generated. The artificial galaxies have one of two morphological types, "ellipticals" with a de Vaucouleurs surface brightness law and "spirals" with an exponential surface brightness law. The fraction of elliptical galaxies is set by the parameter \fIegalmix\fR. The position angles of the major axis are distributed uniformly between 0.0 and 360.0 degrees. The axial ratio (major to minor) of the elliptical models is allowed to range uniformly between 1 and \fIar\fR (that is E0 - E7). The spiral models have inclinations, i, ranging uniformly between 0 and 90 degrees. The axial ratio is then given by a/b = sqrt (sin(i)**2 * .99 + .01) which is taken from Holmberg in Galaxies and the Universe (which references the work of Hubble). Note the axial ratio is limited to 0.1 by this formula. An internal absorption correction is then made based on the inclination using the relation dM = A * (min (10, cosecant (i)) - 1) / 9 where is the absorption of an edge on galaxy relative to face on and the cosecant is limited to 10. Note that this correction changes allows galaxies with magnitudes less than \fImaxmag\fR and alters the luminosity function somewhat. Or in other words, the luminosity function is based on absorption corrected magnitudes. The sizes of the galaxy images are scaled from the maximum half-flux radius of an elliptical galaxy given by the parameter \fIeradius\fR. This is the radius given to an elliptical galaxy of magnitude \fIminmag\fR (prior to adding a random factor described below). The ratio between the half-flux radii of the exponential disk and de Vaucouleurs models at a given total magnitude is set by the parameter \fIsradius\fR (note this is a fraction of \fIeradius\fR and not an actual radius). This allows adjusting the relative surface brightness of elliptical and spiral models. The distribution of sizes is based on the apparent magnitude of the galaxies. For the power law magnitude distribution the cosmological redshift factor for angular diameters is used. The redshift/magnitude relation is assumed to be such that the redshift is proportional to the luminosity distance (the square root of the apparent luminosity). Thus, .nf Z = z * 10. ** (0.2 * (M - minmag)) Zfactor = ((1+Z)**2 / Z) / ((1+z)**2 / z) ellipticals: r = eradisus * Zfactor spirals: r = sradius * eradius * Zfactor .fi where z is the reference redshift at the minimum magnitude, and Z is the redshift at magnitude M. For very small z the size varies as the luminosity distance but at larger z the images appear more extended with lower surface brightness. For very deep simulations a pure luminosity distance relation gives faint galaxies which are too small and compact compared to actual observations. For the other magnitude distributions, the Schecter cluster function in particular where all galaxies are at the same distance, the scale radius obeys the following relation. .nf ellipticals: r = eradius * 10. ** ((minmag - M) / 6) spirals: r = sradius * eradius * 10. ** ((minmag - M) / 6) .fi This relation gives the size decreasing slightly less rapidly than that giving a constant surface brightness. This relation is taken from Holmberg (Galaxies and the Universe). A uniform random factor of 50% is added to the sizes computed for the power law magnitude distribution and 20% for the other distributions. The interactive spatial plot shows the positions of the galaxies, the galaxy type (circles are de Vaucouleurs profiles and other types are diamonds), and rough size. .ih CURSORS The following interactive keystroke commands are available from within the GALLIST task. .nf Gallist Keystroke Commands ? Print options f Fit one or more of following Spatial density function (SDF) Luminosity function (LF) Distribution of morphological type Diameter distribution Roundness distribution Position angle distribution x Plot the x-y spatial density function r Plot the histogram of the radial density function m Plot the histogram of the luminosity function d Plot the histogram of the diameter values e Plot the histogram of the roundness values p Plot the histogram of the position angle values : Colon escape commands (see below) q Exit program .fi The following parameters can be shown or set from within the GALLIST task. .nf Gallist Colon Commands :show Show gallist parameters :ngal [value] Number of galaxies :spatial [string] Spatial density function (SDF) (uniform|hubble|file) :xmin [value] Minimum X value :xmax [value] Maximum X value :ymin [value] Minimum Y value :ymax [value] Maximum Y value :xcenter [value] X center for SDF :ycenter [value] Y center for SDF :core [value] Core radius for Hubble density function :base [value] Background density for Hubble density function :luminosity [string] Luminosity function (LF) (uniform|powlaw|schecter|file) :minmag [value] Minimum magnitude :maxmag [value] Maximum magnitude :mzero [value] Magnitude zero-point of schecter LF :power [value] Power law coefficient for powlaw LF :alpha [value] Schecter parameter :mstar [value] Characteristic mag for Schecter LF :egalmix [value] Elliptical/Spiral galaxy ratio :ar [value] Minimum elliptical galaxy axial ratio :eradius [value] Maximum elliptical half flux radius :sradius [value] Spiral/elliptical radius at same magnitude :z [value] Minimum redshift :absorption [value] Absorption correction for spirals :lfile [string] Name of the LF file :sfile [string] Name of the SDF file :nlsample [value] Number of LF sample points :lorder [value] Order of spline approximation to the integrated LF :nssample [value] Number of SDF sample points :sorder [value] Order of spline approximation to the integrated SDF :rbinsize [value] Resolution of radial SDF histogram in pixels :mbinsize [value] Resolution of magnitude histogram in magnitudes :dbinsize [value] Resolution of diameter histogram in pixels :ebinsize [value] Resolution of roundness histogram in pixels :pbinsize [value] Resolution of position angle histogram in degrees .fi .ih EXAMPLES 1. Create a galaxy cluster with a power law distribution of field galaxies and stars as background/foreground. .nf ar> gallist galaxies.dat 100 spatial=hubble lum=schecter egal=.8 ar> gallist galaxies.dat 500 ar> starlist galaxies.dat 100 ar> mkobjects galaxies obj=galaxies.dat gain=3 rdnoise=10 poisson+ .fi Note that the objects are appended to the same file. Actually making the image with \fBmkobjects\fR takes about 5 minutes (2.5 min cpu) on a SPARCstation 1. 2. Examine the distributions for a uniform spatial distribution and power law magnitude distribution using 1000 galaxies without creating a data file. .nf ar> gallist dev$null 1000 inter+ ... an x-y plot will appear on the screen ... type r to examine the radial density function ... type m to examine the luminosity function ... type d to examine the half-flux radii distribution ... type e to examine the axial ratio distribution ... type = to make a copy of any of the plots ... type q to quit .fi .ih REVISIONS .ls GALLIST V2.11+ The random number seeds can be set from the clock time by using the value "INDEF" to yield different random numbers for each execution. .le .ls GALLIST V2.11 The default value for the minimum elliptical galaxy axial ratio was change to 0.3 to cover the range E0-E7 uniformly. .le .ih BUGS This is a first version and is not intended to produce a full model of galaxy fields. Some of the relations used are empirical and simple minded with the aim being to produce reasonably realistic images. The spline approximation to the spatial density and luminosity probability functions can cause wiggles in the output spatial density and luminosity functions. Users can examine the results interactively and experiment with the spline order and number of sample points if they are not satisfied with the results of GALLIST. The default setup of 10 sample points per spline piece is generally satisfactory for the spatial density and luminosity functions supplied here. .ih SEE ALSO starlist mkobjects .endhelp ./noao/artdata/doc/mk1dspec.hlp0100644000047000001600000003272611015057657015206 0ustar irafiraf.help mk1dspec Jul95 noao.artdata .ih NAME mk1dspec -- Make/add artificial 1D spectra .ih USAGE mk1dspec input .ih PARAMETERS .ls input Spectra to create or modify. .le .ls output = "" Output spectra when modifying input spectra. If no output spectra are given then existing spectra in the input list are modified directly. If an output list is given then it must match in number the input list. .le .ls ap = 1 Image line to be created or modified in images of dimension greater than 1. .le .ls rv = 0. Radial velocity (km/s) or redshift, as selected by the parameter \fIz\fR, applied to line positions and continuum. Velocities are converted to redshift using the relativistic relation 1+z = sqrt ((1+rv/c)/(1-rv/c)). Note the shift is not a shift in the dispersion parameters but in the underlying artificial spectrum. .le .ls z = no Is the velocity parameter a radial velocity or a redshift? .le WHEN CREATING NEW SPECTRA .ls title = "" Image title to be given to the spectra. Maximum of 79 characters. .le .ls ncols = 512 Number of columns. .le .ls naps = 1 Number of lines or apertures. .le .ls header = "artdata$stdheader.dat" Image or header keyword data file. If an image is given then the image header is copied. If a file is given then the FITS format cards are copied. This only applies to new images. The data file consists of lines in FITS format with leading whitespace ignored. A FITS card must begin with an uppercase/numeric keyword. Lines not beginning with a FITS keyword such as comments or lower case are ignored. The user keyword output of \fBimheader\fR is an acceptable data file. See \fBmkheader\fR for further information. .le .ls wstart = 4000., wend = 8000. Starting and ending wavelengths in Angstroms. The dispersion is determined by these values and the number of columns. .le CONTINUUM PARAMETERS .ls continuum = 1000., slope = 0. Continuum of the starting wavelength at rest and the slope of the continuum. .le .ls temperature = 5700. Blackbody continuum temperature in Kelvin. A value of 0 is used if no blackbody continuum is desired. The intensity level is set by scaling to the continuum level of the starting wavelength at rest. .le .ls fnu = no Compute the continuum as flux per unit frequency (F-nu) if yes or flux per unit wavelength (F-lambda) if no. .le LINE PARAMETERS .ls lines = "" List of spectral line files. Spectral line files contain lines of rest wavelength, peak, profile type, and widths (see the the DESCRIPTION section). The latter parameters may be missing or INDEF in which case they default to the task \fIpeak\fR, \fIprofile\fR, \fIgfwhm\fR, and \fIlfwhm\fR parameters (note that the \fIpeak\fR parameter is not a constant but the random number scaling). If no file or a new (nonexistent) file is specified then a number of random lines given by the parameter \fInlines\fR is generated. If a new file name is specified then the lines generated are recorded in the file. If the list of spectral line files is shorter than the list of input spectra, the last spectral line list file is reused. .le .ls nlines = 0 If no spectral line file or a new file is specified then the task will generate this number of random spectral lines. The rest wavelengths are uniformly random within the limits of the spectrum, the peaks are uniformly random between zero and the value of the \fIpeak\fR parameter, the profile type is given by \fIprofile\fR, and the widths are fixed at the values of the \fIgfhwm\fR ad \fIlfwhm\fR parameters. If a redshift is applied the rest wavelengths are shifted and repeated periodically. .le .ls profile = "gaussian" (gaussian|lorentzian|voigt) The default profile type for random lines or when not specified in the spectral line file. The profile types are: .nf gaussian - Gaussian profile lorentzian - Lorentzian profile voigt - Voigt profile .fi .le .ls peak = -0.5 The maximum spectral line peak value when generating random lines or when the peak is missing from the spectral line file. This value is relative to the continuum unless the continuum is zero. Negative values are absorption lines and positive values are emission lines. .le .ls gfwhm = 20., lfwhm = 20. The default gaussian and lorentzian full widths at half maximum (FWHM), in Angstroms, used when generating random lines or when the widths are missing from the spectral line file. .le .ls seed = 1 Random number seed. If a value of "INDEF" is given then the clock time (integer seconds since 1980) is used as the seed yielding different random numbers for each execution. .le .ls comments = yes Include comments recording task parameters in the image header? .le PACKAGE PARAMETERS .ls nxsub = 10 Number of pixel subsamples used in computing the gaussian spectral line profiles. .le .ls dynrange = 100000. The gaussian line profiles extend to infinity so a dynamic range, the ratio of the peak intensity to the cutoff intensity, is imposed to cutoff the profiles. .le .ih DESCRIPTION This task creates or modifies one dimensional spectra. with a combination of blackbody and linear sloped continuum and emission and absorption spectral lines. The spectral lines may be gaussian, lorentzian, or voigt profiles. A velocity shift may be applied to the underlying artificial spectrum which is shifted into the specified observed wavelength region. No noise is included but may be added with the task \fBmknoise\fR. New spectra are created with the specified number of pixels, wavelength range, and real datatype. When \fInlines\fR is greater than 1 then an image with the specified number of lines is created though only the line given by the \fIap\fR is will have a spectrum. Existing spectra may be modified in place or new spectra output. Spectra are modified by adding the continuum and lines defined by the parameters. For new images a set of header keywords may be added by specifying an image or data file with the \fIheader\fR parameter (see also \fBmkheader\fR). If a data file is specified lines beginning with FITS keywords are entered in the image header. Leading whitespace is ignored and any lines beginning with words having lowercase and nonvalid FITS keyword characters are ignored. In addition to this optional header, parameters for the wavelength coordinates are defined. Finally, comments may be added to the image header recording the task parameters and any information from the line file which are not line definitions. Initially all spectra are created without a dispersion function; i.e. pixel coordinates. For multiple spectra in an image this task must be executed for each image line to set the dispersion function and add data. When an image line is selected if it has a defined dispersion function that is used otherwise the task wavelength parameters are used. A continuum is defined by the value at the starting wavelength at rest, a slope, and a blackbody function of a given temperature. The blackbody function is scaled to have the specified continuum value at the starting wavelength at rest. The blackbody flux units are per unit wavelength (F-lambda). A zero continuum value or a zero temperature will not produce a blackbody continuum. Spectral lines are modeled by gaussian, lorentzian, or voigt profiles of specified wavelength, peak, and widths. The lines are defined in a spectral line file or generated randomly. A spectral line file consists of text lines giving rest wavelength, peak, profile type, gaussian full width at half maximum and/or lorentzian full width at half maximum. Only the wavelength is required and subsequent fields may be missing or given as INDEF. The following table shows the possible formats where wavelength, peak, gfwhm, and lfwhm are values of wavelength, peak, gaussian FWHM, and lorentzian FWHM. The profile types are as shown though they may be abbreviated to one character. .nf wavelength wavelength peak wavelength peak gaussian wavelength peak gaussian gfwhm wavelength peak gaussian gfwhm wavelength peak lorentzian wavelength peak lorentzian lfwhm wavelength peak lorentzian lfwhm wavelength peak voigt wavelength peak voigt gfwhm wavelength peak voigt gfwhm lfwhm wavelength peak voigt gfwhm lfwhm .fi When a field is missing or INDEF the values given by the parameters \fIpeak\fR, \fIprofile\fR, \fIgfwhm\fR, and \fIlfwhm\fR are used. If a peak value is missing, random values between zero and the \fIpeak\fR value are generated. Note that to get random line intensities with some specified profile type and widths the value INDEF would be used for the peak field. If no spectral line file is specified or a new (nonexistent) file is named then the number of random lines given by the parameter \fInlines\fR is generated. The rest wavelengths are uniformly random within the wavelength range of the spectrum and extend periodically outside this range in the case of an applied velocity shift, the peaks are uniformly random between zero and the \fIpeak\fR parameter, and the profile type and widths are given by the \fIprofile\fR, \fIgfwhm\fR, and \fIlfwhm\fR parameters. If a new file is named then the parameters of the generated lines will be output. The peak values are taken relative to a positive continuum. In other words the generated line profile is multiplied by the continuum (with a minimum of zero for fully saturated absorption lines). If the continuum is less than or equal to zero, as in the case of an artificial arc spectrum or pure emission line spectrum, then the peak values are absolute intensities. Positive peak values produce emission lines and negative values produce absorption lines. Odd results will occur if the continuum has both positive and zero or negative values. The underlying rest spectrum may be shifted. This is used primarily for testing radial velocity measuring algorithms and is not intended as a complete model of redshift effects. The starting and ending wavelengths are not changed by redshifting; these are the instrumental observed wavelengths. Input line wavelengths are specified at rest and then shifted into or out of the final spectrum. To be realistic the line list should include wavelengths over a great enough range to cover all desired redshifts. The peaks and widths are also appropriately modified by a redshift. As an example, if the redshift is 1 the lines will appear broader by a factor of 2 and the peaks will be down by a factor of 2 in order to maintain the same flux. The random line generation is difficult in that one wants to have the same set of lines (for a given seed) observed at different redshifts. What is done is that the specified number of random lines is generated within the observed wavelength interval taken at rest. This set is then repeated periodical over all wavelengths. A redshift will then shift these rest lines in to or out of the observed spectrum. If the lines are output, they are given at rest. \fBNote that this periodicity may be important in interpreting cross correlation redshift tests for large shifts between template and object spectra.\fR The definitions of the continuum are also affected by a redshift. The reference point for the continuum level, slope, and blackbody continuum is the starting wavelength taken at rest. Shifts will then modify the continuum level at the first pixel appropriately. In particular a large redshift will shift the blackbody in such a way that the flux is still given by the \fIcontinuum\fR parameter at the starting wavelength at rest. .ih EXAMPLES 1. Create a simple blackbody continuum between the default wavelengths. .nf cl> mk1dspec bb title=Blackbody .fi 2. Create a random absorption spectrum on a blackbody continuum without saving the line list. .nf cl> mk1dspec bbab title=Absorption nlines=100 .fi 3. Create a random absorption spectrum with noise and cosmic rays. .nf cl> mk1dspec bbab title=Absorption nlines=100 cl> mknoise bbab rdnoise=10 poisson+ ncos=5 energy=1000 .fi 4. Create a random emission spectrum on a blackbody continuum and save the line list. .nf cl> mk1dspec bbem title=Emission nl=30 peak=0.6 lines=bbem.dat .fi 5. Create an artificial random arc line spectrum. .nf cl> mk1dspec arc title="Arc lines" cont=0 peak=500 nl=30 .fi 6. Create a test spectrum with a line list. .nf cl> type linelist 4100 -.1 g 20 4200 -2. g 20 4300 -.3 g 20 5100 -.9 g 2 5200 -.9 g 4 5300 -.9 g 8 6700 .9 g 8 6800 .9 g 2 6900 .9 g 4 7700 .3 g 20 7800 .2 g 20 7900 .1 g 20 cl> mk1dspec testspec title=Test cont=500 temp=0 lines=linelist .fi 7. Add absorption lines to a spectrum. .nf cl> mk1dspec bb out=artspec cont=0 lines=STDIN 4300 -60 5000 -200 [EOF] .fi Normally the input spectrum would be a real spectrum. 8. Make two spectra taken from the same set of random lines but differing in redshift. .nf cl> mk1dspec restspec nl=30 cl> mk1dspec redspec rv=3000 nl=30 cl> mk1dspec bluespec rv=-.01 z+ nl=30 .fi 9. Make a multispec image with 5 apertures and a range of redshifts. .nf cl> mk1dspec spec.ms ap=1 nl=30 rv=0 naps=5 cl> mk1dspec spec.ms ap=2 nl=30 rv=1000 cl> mk1dspec spec.ms ap=3 nl=30 rv=2000 cl> mk1dspec spec.ms ap=4 nl=30 rv=3000 cl> mk1dspec spec.ms ap=5 nl=30 rv=4000 .fi .ih REVISIONS .ls MK1DSPEC V2.11+ The random number seed can be set from the clock time by using the value "INDEF" to yield different random numbers for each execution. .le .ls MK1DSPEC V2.11 Lorentzian and Voigt profiles were added and the parameters and input line list format were changed. The widths are now FWHM instead of gaussian sigmas. .le .ls MK1DSPEC V2.10.3 The format parameter was eliminated and the task updated to produce the current coordinate system format. .le .ih SEE ALSO mknoise, mk2dspec, mkheader, onedspec.sinterp .endhelp ./noao/artdata/doc/mk2dspec.hlp0100644000047000001600000001561411015060030015157 0ustar irafiraf.help mk2dspec Aug90 noao.artdata .ih NAME mk2dspec -- Make/add 2D spectra using 1D spectra templates .ih USAGE mk2dspec input .ih PARAMETERS .ls input Spectra to create or modify. .le .ls output = "" Output spectra when modifying input spectra. If no output spectra are given then existing spectra in the input list are modified directly. If an output list is given then it must match in number the input list. .le .ls models = "" List of model parameter files. If the list of model files is shorter than the list of input images then the last model file is reused. The model parameter files contain lines giving one dimensional spectrum template name, intensity scale, type of cross dispersion profile, profile width in the center line, change of width per line, profile position in the center line, and change of position per line (see the DESCRIPTION section). .le .ls comments = yes Include comments recording task parameters in the image header? .le WHEN CREATING NEW SPECTRA .ls title = "" Image title to be given to the spectra. Maximum of 79 characters. .le .ls ncols = 100, nlines = 512 Number of columns and lines. .le .ls header = "artdata$stdheader.dat" Image or header keyword data file. If an image is given then the image header is copied. If a file is given then the FITS format cards are copied. This only applies to new images. The data file consists of lines in FITS format with leading whitespace ignored. A FITS card must begin with an uppercase/numeric keyword. Lines not beginning with a FITS keyword such as comments or lower case are ignored. The user keyword output of \fBimheader\fR is an acceptable data file. See \fBmkheader\fR for further information. .le .ih DESCRIPTION This task creates or modifies two dimensional spectra by taking one dimensional spectra, convolving them with a spatial profile across the dispersion, and adding them into two dimensional images. The one dimensional spectra may be real data or artificial data created with the task \fBmk1dspec\fR. No noise is included but may be added with the task \fBmknoise\fR. The spatial profile is fully subsampled and may vary in width and position along the dispersion axis. The spatial axis is along the first dimension and the dispersion is along the second dimension. For new images a set of header keywords may be added by specifying an image or data file with the \fIheader\fR parameter (see also \fBmkheader\fR). If a data file is specified lines beginning with FITS keywords are entered in the image header. Leading whitespace is ignored and any lines beginning with words having lowercase and nonvalid FITS keyword characters are ignored. In addition, comments may be added to the image header recording the model file name and the contents of the model file. The spatial profile models are specified in one or more model parameter files. These files contain lines giving a one dimensional spectrum template name, intensity scale, type of cross dispersion profile, profile width in the center line, change of width per line, profile position in the center line, and change of position per line. More specifically: .ls