Lowell Buie Library

The following is a listing of the entire contents of this library for IDL. Click on an individual procedure name to view its header and source code. This listing is a shortened form of the much longer entire library help file. This may be handy for text searchs, be beware that some of these are huge and may take a long time to load or even crash your browser.

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List of Routines

• ACRE Automatic Cosmic Ray Extraction This program will attempt to identify and remove Cosmic Ray strikes from an image. This program was developed and tested on HST PC data prior to the refurbishment mission. It may work for other types of data but it is as of now untested elsewhere. The simplest usage is the single pass mode where the same parameters are used for the entire image. First, the image is smoothed with a median filter using a box filter size given by width. This smoothed image is then subtracted from the original image. A robust mean of a portion of the image is calculated and subtracted from the image though this mean
• ADDSLASH Append a trailing / to string (if needed).
• ADDSTARS Manipulate the master star catalog (add/replace)
• AIRINDEX Compute the real part of the refractive index of air. This function is based on the formulas in Filippenko, PASP, v. 94, pp. 715-721 for the index of refraction of air. The conversion from relative humidity to vapor pressure is from the Handbook of Chemistry
• AIRMASS Compute airmass for one or more times. This is should be a pretty good function for computing the air mass factor. The default is to use the cosine based formula derived by David Tholen but the older secant based formula from Hardie is still available. The zenith angle is corrected for refraction before using either formula (see REFRAC). The defaults on the atmospheric conditions are STP. This function should be quite good up to 5 airmasses. This formula will work up to a zenith angle of 80 degrees after which the computation id not done.
• ALTOHA Convert an object altitude to its hour angle.
• ANGSEP Compute the angular distance between two spherical coordinates.
• ASTCOL Collect astrometry observations for multiple objects
• ASTEVAL Evaulate an astrometric polynomial function.
• ASTLINKS Scan for linkages among a collection of asteroid astrometric measurements
• ASTLIST Create a summary listing from a final astrometry file.
• ASTPRED Simple asteroid position predictor when no orbit is available.
• ASTPRMT Promote version of an astrometry fit coefficient file to highest version.
• ASTRD2SN Astrometry conversion from ($\alpha$,$\delta$) to ($\xi$,$\eta$) Standard coordinate conversion (see Smart, p283)
• ASTRD2XY Astrometry conversion from ($\alpha$,$\delta$) to image (x,y) This transformation is based on a simple linear transformation with rotation from the celestial sphere to linear CCD chip coordinates. This is only an approximate treatment and will not work for very large
• ASTREPRO Re-reduce existing astrometry originally measured with ASTROM This file attempts to rereduce astrometric measurements in the current directory. These measures are x,y positions that are found in the file, position.dat. The files fitcoeff.dat and centers.dat are scanned for the corresponding transformation relations between x,y and RA,DEC. Any object.ast files in this directory will be overwritten.
• ASTROM Astrometry from a digital image.
• ASTSN2RD Astrometry conversion from ($\xi$,$\eta$) to ($\alpha$,$\delta$) Standard coordinate conversion (see Smart, p283)
• ASTSOLVE Solve for astrometric transformation from image to sky coordinates.
• ASTTERMS Evaulate the independent vectors to match an astrometric polynomial function.
• ASTXY2RD Astrometry conversion from image (x,y) to ($\alpha$,$\delta$) This transformation is based on a simple linear transformation with rotation from the celestial sphere to linear CCD chip coordinates. This is only an approximate treatment and will not work for very large
• ATMOFIT Fit 1 or 2 gaussians to an astronomical image that is seeing limited.
• AVGCLIP Average over a 3-D array, clipping unusual deviants. Calculate the average value of an array, or calculate the average value over one dimension of an array as a function of all the other
• AVGER Temporal averaging of time-series data. This program was written to perform N point averaging of raw photometry data. It will work on any temporal data streams or data that has clumpy independent variable values. The data are grouped together into bin that are specified by the THRESH input. Thresh specifies the size of a gap that will cause the group to be broken. The value for thresh is taken to be a multiple of the 'normal' spacing between points. If THRESH=2, then any gap twice as long as the previous point spacing will cause a break. Any number equal to or less than 1 will prevent all averaging. To prevent too much binning for long uniform data runs, MAXBIN puts an
• AVGSPEC[1] Robust average of a set of 1-D spectra from FITS files.
• AVGSPEC[2] Robust average of a set of 1-D spectra.
• BACKSUB Background subtraction from an image. The background is determined from a robust fit of a line to each row or column in the image depending on the keywords. If neither keyword is set, then the robust mean is used. These lines or means are then subtracted from the input image.
• BADPAR Validate an input parameter against valid entries.
• BASPHOTE Circular aperture photometry extraction from images.
• BIDR Compute the bi-directional reflectance (old Hapke formula).
• BIDR2 Compute the bi-directional reflectance (newer Hapke formula). This is coded from equation 12.55 on page 346 in Hapke's book, "Theory of Reflectance and Emittance Spectroscopy".
• BILDMASK Stack a set of bad pixel mask images into one master mask.
• BOXM Find location of a maximum within a sub-array.
• CALDATM Find year, month, day, hour, minute, second from Julian Date.
• CALVAL Validate overscan, cropping region, and calibration file settings.
• CCDGAIN Extract and plot CCD gain transfer curve from flat field image data.
• CCDPHOT General purpose display and processing of CCD image files (FITS). A general purpose widget application which displays and processes CCD image files. This includes bias and flat field calibration and photometry reduction (itool). This procedure supports FITS files from the LCCD and LORAL instruments.
• CENTROD Compute center of mass of an object aperture.
• CGETRNG How to integrate over a circle. This procedure is called to determine how to iterate when integrating over a circle. The circle's center is at (xc,yc), and its radius is r. For pixels with x-coordinate x, those in the intervals [y0,y1) and [y2,y3) are on or near the circle. Those in the interval [y1,y2) are definitely inside; all others are definitely outside. Of course, the routine can be called to determine an interval for fixed y by calling it as cgetrng,yc,xc,r,y,x0,x1,x2,x3. The appropriate way to integrate over a circle is therefore as follows: cgetrng,xc,yc,r,Round(xc),y0,y1,y2,y3
• CLEAN Remove a PSF from an image via the ``clean'' algorithm.
• CLEANDAT Interactive program to eliminate and smooth over bad data points.
• CLNSPEC Interactive cleaning of bad pixels in an OSIRIS XD spectrum. Plots one order at a time and allows cleaning up bad pixels. The left mouse button is used to alternately mark bad pixels and then their new new value for visual interpolating. The middle button causes the nearest point to be replaced by the average of its two nearest neighbors. CLEANDAT is called on each order.
• CLSCAN Scan a group of raw OSIRIS XD frames and find rough spectral location.
• COLBIAS Determine and subtract column-wise overscan correction with cropping.
• COLORSOL Find the standard color of an unknown star.
• COORD Given a list of names and JD, return coordinates (RA and Dec).
• CPUTIME Return the accumulated user and system times since an arbitrary time. The overhead in using this procedure is about 3 milliseconds per call.
• CRMATCH Create a standard name --- non-standard name correspondence file. Creates, from a photometry log file (alternate format) and a standard name --- non-standard name correspondence file, a new standard name --- non-standard name correspondence file.
• CW_IPMGR Display and edit itool image parameters.
• CW_ITOOL General purpose image display.
• CW_OSIPL Display the various spectra generated by xdavg
• CW_PFILE Widget application for plots and profiles of an image.
• CW_PIXED This compound widget may be used to edit a grid of pixels in an array. Unless near the edge of the image, the grid is centered on (xpos, ypos). The left column and the bottom row display the y and x coordinates, respectively, for the grid. Xpos and ypos are enclosed in brackets, for identification.
• CW_PPMGR Display and edit itool photometry parameters.
• CW_TPLAT Create a photometry template widget. This compound widget is invoked on a Top Level Base (from The Template Manager) and represents an individual template. Each template managed by The Template Manager has its own TLB and appears as a separate widget. The template structure for each template is stored in the user-value of
• CW_TPMGR Photometry template manager for itool.
• DECPARSE Convert Declination string to radians.
• DECSTR Convert declination in radians to an ASCII string.
• DERIV Compute the step-wise derivative of a function of one variable. Calculates the step-wise derivative of a function by computing deltaf / deltax. This requires that f and x be vectors with at least
• DEWP Compute dew point temperature give temperature and relative humidity
• DIFREF Compute amount of atmospheric refraction relative to 5000 Angstroms. this function is based on the formulas in Filippenko, PASP, v. 94, pp. 715-721 for the index of refraction of air (routine REFRAC).
• DIGIT Digitize from a displayed gif file.
• DISPHASE Apply distance and phase angle correction to observed magnitudes. Apply IAU standard asteroidal-law corrections to observed magnitudes given the distance, phase angle, and the G coefficient. Magnitudes are corrected to 1 AU from Sun and Earth and to 0 degrees phase angle.
• DISPLAY IDL procedure for initializing the X window display for plotting.
• DMSTORAD Convert from degrees, minutes, and seconds to radians.
• EDGEFIT Fit an edge between two signal levels
• EPH4MOVE Generates ephemeris files for use by the MOVE computer.
• EPHCHECK Compare a set of astrometry observations against an ephemeris.
• EPHEM Ephemeris generator for solar system objects. This program pipes the input data to an external FORTRAN program written by Larry Wasserman. The external program looks up the orbital elements of each object and computes the positions requested by the output code. The output code options are:
• EXISTS Check for file (or directory) existence.
• FIELDOBS Real-time display of standard star locations in the sky
• FINDMAX Find the interpolated local maximum in a 2-D array.
• FINDOBJ Locate image changes with 3-plane color overlays
• FINDSRC Automatic source detection and photometry from a digital image.
• FLAGSPEC Interactive marking of bad pixels in an OSIRIS XD spectrum. Plots one order at a time and allows marking bad pixels. See MARKDATA for operation of the widget used to mark data. No attempt is made to repair the spectrum. MARKDATA is called on each order.
• FLX2MAG Convert from flux units to magnitudes with errors.
• FOURFIT Fit one or more fourier terms to discrete (periodic) data.
• FOURFUNC Compute a Fourier series function (called by fourfit) This is to be used in cases where you already know the fundamental period. The input independent variable is assumed to be reduced to phase of a fundamental period already. The integer part of the number is not to the function.
• FUTUREOB Plot geometric circumstances for a solar system object for some years.
• FXTM Fix bad time codes from Anderson Mesa CCD software. This is a special purpose routine for fixing bad times that are generated from using MGO with the Hendon CCD control software at Anderson Mesa. For a string of times, this is what it looks like: Frame Stored time Actual time n t(n+1) t(n) n+1 t(n+2) t(n+1) n+2 t(n+3) t(n+2) n+3 t(n+3) t(n+3) for a four frame sequence. The times for n to n+2 are actually the
• GARTH Visual inspector of moving target triplet detections.
• GAUSS2D Compute a two dimensional gaussian within an array.
• GETANNUL Extract an annulus from a 2-D array.
• GETCOLOR Given a list of names and JD, return B-V and V-R colors.
• GETPAIR Read two OSIRIS XD data files and return the difference strip image.
• GETSALB Solve for single scattering albedo given bi-directional reflectance
• GETSPEC Extract a point source spectrum from OSIRIS XD data.
• GETSTARS Retrieve coordinates from the master star catalog
• GETSTRIP Extract a 2-d rectangular strip image from a OSIRIS XD image.
• GOODPOLY Robust fitting of a polynomial to data. This is a multi-pass fitting routine that fits a fixed order polynomial to the input data. After each pass, the scatter of the fit relative to the fitted line is computed. Each point is examined to see if it falls beyond THRESH sigma from the line. If is does, it is removed from the data and the fit is tried again. This will make up to two attempts to remove bad data.
• GPSPROC Process and average a single day GPS record.
• GRIDWT Compute circle overlap weights in a circle within an array.
• GXPAR General purpose FITS file header keyword extraction. This procedure is a 'front-end' to SXPAR and may be used to extract the value of a keyword from a FITS file header. Because there is so much variation of the keywords found in FITS file headers, the idea is to have and use a set of 'standard' keywords in programs that load and display FITS files. To facilitate this, gxpar uses a correspondence list to associate a standard keyword with a keyword found in a given FITS file header (or with a value different from that which might be in the header). This correspondence list consists of three linear arrays of the same
• HANGLE Compute the local hour angle of an object.
• HARDIM Create a postscript image and/or print from an image.
• HATOJD Find the nearest Julian date for a given hour angle and date.
• HGP Compute a single parameter Henyey-Greenstein phase function.
• HMSTORAD Convert from hours, minutes, and seconds of Right Ascension to radians.
• HSTPSF Find or create a HST PSF file using Tiny Tim. See Tiny Tim User's Manual, Version 2.4, for details.
• IMQUAL Generate a ``grade'' for image quality of input image.
• INSLIT Compute flux passing through a slit assuming a gaussian image.
• INST2STD Apply photometric transformation from instrumental to standard mags. The formula for applying transformation to a photometric measurement follows the basic formalism (including signs) from Hardie. A time dependent term has been added. The formula looks like this:
• INTERP One dimensional interpolation onto a new x grid (both irregular)
• INTRSECT Find the intersection or its inverse between two arrays.
• ITOOL General purpose image display (front-end for cw\_itool).
• IT_INIT Itool initialization.
• IT_PPLOD Load itool photometry parameters from a file.
• IT_PPSAV Save itool photometry parameters to a file.
• JD2YEAR Convert Julian date to decimal year.
• JDSTR Convert Julian date into an ASCII string.
• JUPLOC Find and extract Jupiter in images and create PDS FITS headers on output.
• KBOPLAN KBO observing planning table generation
• LANDSCAP Procedure for initializing the PS device for plotting. Output plotting device is change to PS in landscape mode with a Helvetica font.
• LCFIT Fit a lightcurve function (Fourier series plus phase coefficient).
• LCFITSVD Fit a lightcurve function (Fourier series plus phase coefficient).
• LCFUN Compute a lightcurve function (Fourier series plus phase coefficient). This is to be used in cases where you already know the fundamental period. The input independent variable is assumed to be reduced to phase of a fundamental period already. The integer part of the number is not used by the function.
• LCFUNF Compute a lightcurve function (Fourier series plus phase coefficient). This is to be used in cases where you already know the fundamental period. The input independent variable is assumed to be reduced to phase of a fundamental period already. The integer part of the number is not used by the function.
• LCLXTREM Find local minima or maxima in a 1-d vector.
• LDCALIB Load calibration frames and information as instructed by calib file.
• LDCALIR Load calibration information for OSIRIS XD data from a calib file.
• LIMBCEN Find center of body from centroid of limb points (Designed for Jupiter).
• LINKOBJ Cross check three source lists from one field and identify moving objects.
• LOADKEYS Load FITS header keyword correspondence list from file.
• LOADSTAR Load the master star catalog file
• LOGMANIP Widget for editing and manipulating photometry log files.
• LOOKER Visual identification and measurement of moving objects in digital images.
• LOWESS Lowess smoothing of data.
• LPLASTCHK Scan for linkages among a collection of asteroid astrometric measurements
• LSIDTIM Compute local sidereal time at a given longitude and time. This routine is based on the algorithms from p. 39 of "Astronomical Formulae for Calculators" by J. Meeus.
• LTCRV Photometric lightcurve reductions against a single comparison star.
• LTCRV2 Photometric lightcurve reductions with known transformation.
• MAG2FLX Convert from magnitudes to flux units with errors.
• MAPSEQ Animate a seqence of PLUTOMEM maps.
• MARKDATA Widget for marking/unmarking bad data. Mouse click and drag will define a selection of points. Newly selected points will be marked in green. To mark these as bad, click the 'Bad' button. To mark these green points as good, click the 'Good' button. Bad points are plotted in red. The rest of the control buttons should be self-explanatory.
• MATCHOBJ Find matches for non-standard names in a correspondence list.
• MATCHUP Read a batch of FITS files and create a list of common object exposures.
• MAXLOC Find the column-wise, row-wise, or point location of the image maximum.
• MAXMIN Return vector [max,min] of input array or vector. Return a 2 element array giving the maximum and minimum of a vector or array. This is faster than doing a separate MAX and MIN.
• MEANERR Calculate the mean and estimated errors for a set of data points This routine is adapted from Program 5-1, XFIT, from "Data Reduction and Error Analysis for the Physical Sciences", p. 76, by Philip R. Bevington, McGraw Hill. This routine computes the weighted mean using Instrumental weights (w=1/sigma^2).
• MEDARR Combine arrays with a median average. This will combine a series of arrays into a single array by filling each pixel in the output array with the median of the corresponding pixels in the input arrays.
• MKBIAS Collect and combine CCD bias frames into a superbias frame
• MKCALIB Interactive program for creating CCD calibration files.
• MKDARK Collect and combine CCD dark frames into a superdark frame
• MKFLAT Collect and combine CCD flat frames into a superflat frame
• MOMENT4 Compute various statistical moments of the data. This routine computes the average, average deviation, standard deviation, variance, skew and kurtosis of the input data. The various output quantities are always returned as floating point scalars. The statistics are compute with no regard for the dimensionality of the input data.
• MYSVDFIT Perform a general least squares fit with optional error estimates. This version uses SVD. A user-supplied function or a built-in polynomial is fit to the data.
• NAIFNAME Convert an ephem standard name to a common name (NAIF name scheme)
• NEGATIVE Invert the current display lookup table. The current lookup table is fetched, rotated end-for-end, and put
• NOBNAME Replace all blanks in a string with an underscore character.
• OBJRATIO Ratio object spectra to one or more comp star spectra. Ratio object spectra to comp stars, combined appropriately to match object airmasses. For a single comp star, obviously you just get a simple ratio - no real airmass correction. For two or more comp stars, an extinction is derived, and used to correct each comp star spectrum to the object airmass, prior to averaging the comp stars and performing the ratio. If the /NOEXT keyword is set, no extinction correction is derived or applied.
• OBSPLAN Generate a graphical summary of object location(s) for a given night.
• OBSPROP Observing proposal planning table generation
• OBSWIND Compute possible observing window for a celestial object.
• OCCPLOT Plot small pieces of stellar occultation data. This procedure is intended to be used in plotting a very large 1-d vector as a function of time in which you are only interested in plotting a small subset of the data. The time calibration is specified through the tstart and dt input parameters and the time axis is assumed to be strictly linear. All time calculations are done in double precision to ensure the full precision of the time axis is saved. Single precision gives out at the few millisecond level.
• ONCHIP Extract and optionally plot differential on-chip photometry. This program will read an altlog photometry file as generated by basphote and extract one object from the file, compute differential photometry for the program object (Serial #0000) against the field
• OPLERR Overplot data points with accompanying x or y error bars.
• OPTSPEC Optimal extraction of a point source spectrum from OSIRIS XD data. This program is custom built to extract spectra from OSIRIS XD data. The spectral images contain usually 3 or 4 cross-dispersed orders. Because of the high and variable sky background signal, all images are reduced as image pairs to permit excluding most sky signal at the very first step.
• OSICLEAN Automatic cleaning of bad and low signal data from OSIRIS XD spectrum
• OSIDVFIT Find the linear fit coefficients for a spectrum for each order The spectrum and a reference to be divided by are input. The spectrum is divided by the reference and this divided spectrum is then filtered for noise and deviant points. A linear fit is then applied to each order of the filtered divided spectrum.
• OSISLOPE Correct an IR OSIRIS spectrum for the slope problem. Each order of an IR spectrum from OSIRIS is corrected for the "sloping" problem given the linear fit coefficients for each order of the spectrum. The origin of this linear fit for each order is column 128 of the CCD
• OSISMEAN Compute mean of a set of OSIRIS XD spectra. Given a set of spectra, this will perform a straight average of the provided spectra. First, the relative signal level (relsig) is computed between all members of the set. This relative level is normalized to 1.0 for the individual spectrum with the highest signal level. Then, only those spectra with relsig >= 0.8 will be used for the set mean. If there aren't 4 spectra in this clase, then the brightest 4 spectra will be used, unless there aren't 4 spectra. In this latter case, all spectra will be averaged.
• P6MODEL Generate synthetic PSF images for the HST Planetary Camera, Chip 6. A generated PSF is added to the output array. If the array is not defined, it is created with dimensions 800 by 800. Successive calls will add objects (PSF's) to the array.
• PARSEKEY Extract FITS header information by parsing supplied keys
• PDM Period search by phase dispersion minimization ($\theta$ based). This routine computes the Theta statistic for period searching in time-series data using the technique described by Stellingwerf, ApJ, 224, pp. 953-960 (1978).
• PDM2 Period search by phase dispersion minimization ($\chi^2$ based) This routine computes a Chi^2 statistic for period searching in time-series data loosely based on the technique described by Stellingwerf, ApJ, 224, pp. 953-960 (1978).
• PDM2DIS Phase disconnect shift search by phase dispersion minimization ($\theta$ based). This routine computes the Theta statistic to look for the optimum zero-point shift between two datasets for a given period. The theta statistic is the same as used for period searching in time-series data using the technique described by Stellingwerf, ApJ, 224, pp. 953-960 (1978). The shift reported is that which is added to the phase of x2 to register with respect to x1.
• PDM2SHIF Zero-point shift search by phase dispersion minimization ($\theta$ based). This routine computes the Theta statistic to look for the optimum zero-point shift between two datasets for a given period. The theta statistic is the same as used for period searching in time-series data using the technique described by Stellingwerf, ApJ, 224, pp. 953-960 (1978). The shift reported is that which is added to x2 to register with respect to x1.
• PDMSHIF Zero-point shift search by phase dispersion minimization ($\theta$ based). This routine computes the Theta statistic to look for the optimum zero-point shift between two datasets for a given period. The theta statistic is the same as used for period searching in time-series data using the technique described by Stellingwerf, ApJ, 224, pp. 953-960 (1978). The shift reported is that which is added to x2 to register with respect to x1.
• PERSER Automated asteroid period search tool.
• PHASEBIN Compute a phase binned average lightcurve This routine bins lightcurve data as a function of time into a binned composite lightcurve. Bins with no data are not returned.
• PHOTRED Reduction of non-variable point source absolute photometry.
• PICKER Widget for selecting a text item from a list. This widget provides a simple mechanism for selecting a single item from a list. The items are all strings and the return from this call is the string selected.
• PICKIM Interactive program to select best image from cube for SL9 data. This is a special purpose routine built for selecting one image from a set of nearly identical images. The SL9 data was taken as image cubes ~5 images in rapid succesion in the same filter. This program will display all images raw and after unsharp masking. Click on the best (either version) to save it (after processing) to disk.
• PIXWT Circle-rectangle overlap area computation. Compute the fraction of a unit pixel that is interior to a circle. The circle has a radius r and is centered at (xc, yc). The center of the unit pixel (length of sides = 1) is at (x, y).
• PLAST Support routine for calling ``PLAST'' to get asteroids on an image.
• PLASTEXT Batch mode extraction of PLAST asteroid lists.
• PLCHFIT Two gaussian fit to an image of the Pluto-Charon system. Fit the equation y=f(i) where:
• PLCH_FUN Two 2-d gaussian images, support routine for PLCHFIT. Evaluate the sum of two 2-d guassian and a 2-d 2nd order polynomial and optionally return the value of it's partial derivatives.
• PLOTPHOT Plot extinction fits from Tholen's ltcrv program. This program will automatically generate a summary plot from an extinction fit produced by David Tholen's ltcrv program. If the file does not exist or if there aren't enough points to generate a meaningful plot, then no plot is generated and the top summary portion of the output file is printed (if found).
• PLOTSN Analyze a vector and retrieve the signal-to-noise ratio. First, fit a polynomial to the data, subtract the polynomial and add the mean of the polynomial to flatten the data. Compute the mean and standard deviation in the flattened data.
• PLOTSPEC Plot OSIRIS XD spectral data with wavelength scale.
• PORTRAIT IDL procedure for initializing the PS device for portrait mode plotting. Output plotting device is changed to PS in portrait mode with a Helvetica font.
• PRIVAL Reduce an angle to its principal value (0 $\leq \Theta < 2\pi$). This routine uses [0 to 2*PI) as the principal value of an angle. If the angle is negative, 2*PI is added to the remainder of division by 2*PI. If positive, then the value is the remainder of division by 2*PI. Nothing is done to the input value if it is already in range.
• PSFSTACK Generate an average numerical psf by stacking observed images.
• QANNOUNC Scrollable text display widget with true and false response buttons.
• QINPUT Prompt user for input from a widget.
• RADP Extract point-wise radial ``profile'' from image data.
• RADTODMS Convert an angle from radians to degrees, minutes, and seconds.
• RADTOHMS Convert from radians to hours, minutes, and seconds of right ascension.
• RAPARSE Convert Right Ascension (RA) string to radians.
• RASTR Convert RA in radians to hours, minutes, and seconds (ASCII string).
• RCGFIT Fit a radial gaussian function to the input data (no linear term). Fit the equation y=f(r) where:
• RDAST Read final astrometry data file.
• RDAT1I Read and return a one dimensional 2-byte integer vector. The file should contain at least num points.
• RDAT1R Read and return a one dimensional single precision floating point vector. The file should contain at least num points.
• RDAT2I Read and return a two dimensional two byte integer vector. The file should contain at least nrows x ncols points.
• RDAT2R Read and return a two dimensional single precision floating point vector. The file should contain at least nrows x ncols points.
• RDAT2U Read and return a two dimensional two byte unsigned integer vector. The file should contain at least nrows x ncols points.
• RDBYT Read and return a two dimensional byte array from an animation file.
• RDCTIOPH Reads raw card image CTIO photometry data files.
• RDDAT Display the X and Y value of the cursor in a plot
• RDFLT Read and return a two dimensional byte array from an animation file.
• RDGRAB Read raw binary IRTF-grabber1 format data files.
• RDIMG Read and return the two images in an old style MaxEnt map.
• RDKEYLIS Read a correspondence list file into arrays.
• RDLAND Read the Landolt Standards data file. This program automates the process of reading the Landolt 1983 Standard file as provided on the CD-ROM from NSSDC. Selected Astronomical Catalogs, Volume 1. Also supported is the table for the 1992 catalog as supplied by Arlo Landolt at Louisiana State University.
• RDLAND2 Read the Combined Landolt Standard system photometry file.
• RDMATCH Read a standard name --- non-standard name correspondence file.
• RDOBLIST Read a triplet object list from a file.
• RDOBSCOD Read standard observatory code data file.
• RDOCCPHT Read a Occultation Photometer data file.
• RDPHALT Reads photometry from an alternate format basphot log file. All photometry is read from the file and returned to the caller.
• RDPHOCAT Read a photometry standard catalog from a file.
• RDPHOT Reads photometry from a basphotc log file. All photometry for the given object serial number is read from the file and returned to the caller.
• RDPHOT2 Reads the original BASPHOTC photometry log file.
• RDPHOT3 Reads photometry from a reduced photometry file (see WRPHOT)
• RDPRICAT Read data from a private star catalog.
• RDRAW Read and return a two dimensional byte array from a raw animation file.
• RDRAWAST Read raw astrometry data file.
• RDTBL Read the data from the table file from one night of OSIRIS observations The table file is read one line at a time and then disected into the various pieces of information in the form of arrays. These arrays are then saved in
• READTIL Read and return the two images in a MaxEnt tile map file.
• REDFITS Apply standard CCD processing steps to a raw CCD image.
• REDUCTOR Automated photometry reduction tool.
• REFEXT Batch mode extraction of REFNET star catalog fields in support of ASTROM
• REFNET Support routine for calling ``REFNET'' to get stars from USNO A1.0 catalog.
• REFRAC Apply atmospheric refraction to a ``true'' zenith angle This calculation is based on a few different sources. First, it is assumed that the index of refraction of air at the base of the atmosphere can be calculated (see AIRINDEX). From the index of refraction, the bending is computed from the formula on p.55 of the old Explanatory Supplment to the Nautical Almanac. This formula has been modified by removing the h/rho term. The explanatory supplement doesn't indicate that this is legitimate but I've validated this computation against a more emperical formalism from Eisele and Shannon (NRL memo 3058, May 1975). Eisele and Shannon don't indicate the wavelength of light used but if I use 0.56 microns
• RELPATH Prepend a path to the file name if file starts with {\tt +}
• RENDER Render a rectangular projection map to a sphere. The most confusing aspect of this program is by far the image orientation. I can't make the conventions natural for everyone (not even myself), but here's what this program does:
• REPCHAR Replace a target string with a new string in string or string array.
• REPHOT Reprocess photometry data set by re-extracting from images. This program will use a previously created photometry log file (new format as read and defined by RDPHALT.PRO) to reprocess the photometry allowing a change to the CCD gain, photometric aperture, and more. It also normally is used to reprocess photometry with new calibration information but this is not required.
• REPWRITE Update file by replacing or adding line of information
• RFGFIT Fit a radial gaussian to the input data (no linear term, width fixed). Fit the equation y=f(r) where:
• RGFIT Fit a radial gaussian function and 2nd order polynominal to the input data. Fit the equation y=f(r) where:
• RINGPROF Compute a surface brightness profile.
• ROBOMEAN Robust statistical moments of the data. This routine computes the average, average deviation, standard deviation, variance, skew and kurtosis of the input data. The various output quantities are always returned as floating point scalars. The statistics are computed with no regard for the dimensionality of the input data.
• ROTPOINT Rotate x,y,z point(s) about arbitrary axis.
• ROUND round a floating point number. rounds a floating point number to the nearest whole number.
• RQGFIT Fit a radial gaussian function to the input data (no linear term). Fit the equation y=f(r) where:
• SALB Compute single particle scattering albedo.
• SAVESTAR Save the master star catalog file
• SEERAD Display a radial profile at X and Y value of the cursor
• SETUSYM Set the user defined symbol to be a filled circle (@ script).
• SETWIN Set current draw window, create if needed. This is intended to be a more general call for controlling the use of multiple plot windows especially in scripts or programs. In particular, this routine becomes a no-op if the current display device can't handle windows (like the PS device for printing). In its simplest form, just type setwin,number to make window number the current window. If the window does not exist it will be created. The other optional inputs work as described in the IDL documentation for WDEL, WSHOW, WINDOW, WSET. If the size and location of the window does not change, then the window is not recreated and its status on the screen is unchanged. Note that
• SIGRATIO Compute the relative signal level between a set of spectra (1-d vectors).
• SINCFLTR Pass 1-d data through a low-pass filter (damped sinc). This procedure will filter an array of data with a low pass filter. The input value, smofac, determines the high-frequency cut-off in the output data. The new cutoff will be 1/smofac times the old cutoff frequency which is defined to be 1/2 the sampling interval in the original data.
• SINT Sinc interpolation of a 1-D vector of data.
• SINT2D Sinc interpolation of a 2-D array of data.
• SINTERP4 Four-fold sinc interpolation of a vector of data. This function will do a 4-fold sinc interpolation of the data array that is passed.
• SKYSCLIM Compute stretch range for a hard stretch on the background in an image.
• SL9PROC Interactive program to process and crop image for SL9 data. This is a special purpose routine built for processing SL9 data image and selecting region of interest to crop. There is also special code to detect missing exposure times and allow user to enter a new value. (either version) to save it (after processing) to disk.
• SLIDEFIL Sliding spatial filter on time series data. This program scan a data stream looking for short duration, non-random excursions. Primarily designed for scanning stellar occultation data, you provide the data (y), the independent variable (x) and the filter widths. The equivalent width within the sliding window is computed and returned alone with the x location for the window. The spacing in x does not need to be precisely constant but should not vary by much across the window.
• SLOPE Compute slope of a line using part of the data. The left and right hand values are computed from the mean of the input data array from -width to +width about the mid-point of the bin. The slope is derived from these means and the uncertainty comes from propagating the uncertainties.
• SSGEOM Compute Sun and Earth distance and phase angle for solar system object.
• SSHIFT Shift data using a damped sinc function for fractional part.
• SSHIFT2D Shift a 2-D array using a damped sinc function for the fractional part.
• SSPOS Interactive program for generating solar system body ephemerides. Interactive front-end for EPHEM. Given object code (format described in EPHEM), this will compute positions and give local circumstances of the object. Reads the current time from the system clock which may or may not be accurate.
• STARCAT Retreive coordinates from the star catalogs.
• STARFIT Single gaussian fit to a stellar image. Fit the equation y=f(i) where:
• STARPROC Collect and process final (standard) star photometry This program processes the accumulated stellar photometry into final averages. The data are generated by REDUCTOR and have been saved to the final output directory (set via PATH keyword). This program can reduce all stars in this directory or just one star.
• STAR_FUN Single 2-d gaussian image, support routine for STARFIT. Evaluate the sum of one 2-d guassian and a 2-d 2nd order polynomial and optionally return the value of it's partial derivatives.
• STATS Compute and print statistics plus plot histogram of data. This computes basic statistical information regarding the input data and prints it to the screen. It is intended for purely interactive work, use MOMENT if you want to save the results to a variable.
• STDCHECK Determine if object is in a given standard catalog.
• STRB36 Convert an integer into a Base 36 formatted string.
• SUMANN Integrate over an annulus.
• SYNSTAR Compute a synthetic (gaussian) star image.
• SYNSTAR2 Compute a synthetic (Lorentizian) star image. This uses the functional form of a Lorentzian point-spread function as described in Bosh et. al., Icarus, 95, 319-324 (1992).
• TBLPARSE Determine properties and problems from the table file with OSIRIS data The beginning and ending spectra files for a group of spectra are determined for later processing. Spectra which need a mate and have probably not been processed by xdspec are flagged. Spectra sets that have inequal exposure are flagged as inhomogenous.
• TOBACKSL Convert forward slash (/) to backslash ($\backslash$) in string.
• TRANSF Determine transformation coefficients from instrumental to standard mags.
• TVMAPS Display a full set of Pluto/Charon model .til maps on the current display.
• TVTIL Display a Pluto/Charon .til map as an image on the current display.
• VIEWTEXT View a string, or string array, of text in a scrollable text widget.
• WEDGE Compute and return a gray scale step wedge.
• WRBOPHOT Write a simple photometry data file.
• WRCALIR Write calibration information for OSIRIS XD data to a calib file.
• WRMATCH Write a standard name --- non-standard name correspondence file.
• WROBLIST Write an object list to a file.
• WRPHOCAT Write a photometry standard catalog file.
• WRPHOT Write a standard raw photometry data file (Pluto format). This creates a .001 format Pluto-Charon format file from the input photometry. As a suggestion, use .000 as a suffix if these are NOT standard magnitudes (such as differential to some star), and use .001 if they are magnitudes on a standard system.
• WRTBL Update the table file of a night's OSIRIS data
• XDAVG Interactive tool for combining and correcting OSIRIS XD spectra.
• XDSPEC End-to-end reduction tool for OSIRIS XD spectral data.
• XORACLE Display ``oracle'' animation image sequences.
• XRUNPLOT Display a complete graphical summary of ``plutomem'' output logs.
• ZPLOT Plot differential refraction as a function of wavelength.