BRIEF COMMAND DESCRIPTIONS In the help library (HELPLIB.HLB) the commands are listed by general area of use. These are listed when the user asks for help. To see the command descriptions themselves one can enter either: HE SU where SU represents the first two letters of one of the subdivisions listed below. This will give a list of the options available within that subdivision category, e.g., entering HE AR will give a list of the ARithmetic commands. or HE * This returns ALL of the command descriptions. Entering HE DOC OP where OP represents the first two letters of the selected option will give a detailed description of that option. The information can be printed or displayed on the monitor, e.g., enter HE DOC AT to see a detailed description of AT. SUBDIVISIONS: AR Arithmetic (real, complex, and flatfields) CA Calibration (flux, photographic, wavelength) CO Coordinates, Transforms (XY, RA and DEC) and Velocities DI Display (line plots and images) ED Edit (headers and data) FI Filter (1D, 2D, real or complex) PH Photometry (stellar, surface, or spectral) TO Topology (rotate or move maps,lines, or bits) UT Utilities (statistics, curve fits, etc.) 2 ARithmetic Does arithmetic on maps AD Adds and subtracts maps within a file and writes the results to the same file or a different file. Provides for scaling factors. AP Adds UM power spectra speckle frames AR Does arithmetic on maps, e.g., A<1:5>=B<21:25>*K The allowed operators are +, -, *, /, **, LOG, LN, and SUM. The total number of characters in the expression must not exceed 80. AV Averages pixel values within each column producing one average for each column for a specified set of rows for a map(s) and replaces (default) or creates a new map(s) or file of the same size. FS Flattens a spectrum MT Multiplies and divides fourier transforms which are in REAL*4 maps, as produced by option P2 Page 2 NO Normalizes pixels by a row average, map average, or an average of all the maps NS Normalizes rows to specified average value in channel region RS Scales individual rows in maps - can accept file input S3 Flat fields all maps in a file (used for speckle images) WI Averages pixel values within each column, producing an average for each subset of rows specified by the respective start and end rows for a map(s) and replaces (default) or creates a new map(s) or file of the same size. 2 CAlibration Does calibrations for photometry and spectroscopy AF Converts wavelength scrunched maps to absolute flux BP Finds an atmospheric calibration for broadband photometry with or without a color term and plots the results CA Calibrates PDS data according to curve from PD CO Determines the centroided or least squares-fitted positions for a set of spectral comparison lines selected manually or automaticlly for a range of rows and writes the positions to a SAD file. A polynomial fit to the positions is written to another SAD file for use with option RE. MC Derives average magnitudes of stars over the passband of a system, derives effective wavelengths, computes an absolute calibration, computes the K-correction, and does plotting of data files. ND Applies or removes effect of tabulated filters OK Calibrates wavelength scrunched standards against Oke magnitudes PD Finds a calibration curve for photographic measures 2 COordinates_Transforms_Redshifts Derives coordinates, Fourier transforms, and redshifts AN Computes the angular separation of two objects, given their coordinates AS Does astrometric calculations in order to derive object coordinates BT Does a backward transform when deriving redshifts CC Corrects for coincidence in high count rates CN Normalizes a CCF when deriving redshifts CQ Finds a CCF peak (where derivative equals zero) when deriving redshifts CR Cross correlates maps with their template when deriving redshifts CS Cosbell masks maps and includes a template as the last row when deriving redshifts CT Finds object positions using centroid weighting FI Finds objects in a map and writes their position to a data file of type 2 FO Finds the offset of one row from one file relative to a Page 3 second row from a second file by means of a least squares fit to the minimum in the variance, or to the maximum in the cross correlation FT Does a forward transform when deriving redshifts GC Computes new and old galactic coordinates from user input RA and Dec, and vice versa P1 Converts a two-dimensional power spectrum to a one-dimensional SAD file. P2 Computes the power spectrum of a map and optionally calculates the fourier transform. This is useful for speckle files. PE Precesses coordinates input coordinates RD Computes an average weighted cz of a single galaxy or an average cz and dispersion for a cluster of galaxies. RE Rebins (scrunches) data from one of pixel, wavelength, log(wavelength), frequency, or log(frequency) to one of pixel, wavelength, log(wavelength), frequency, or log(frequency) according to coefficients produced by option CO, or input manually. RT Computes the inverse fourier transform of a file in the format produced by P2 SF Fits various functions to a row of a SAD file. SM Divides object transform by template transform to give the broadening transform when deriving velocity dispersions S1 Finds the centroid of all images in a UM speckle file 2 DIisplay Displays lineplots and 2-dimensional pictures AC Does several kinds of contour and threshold plotting on devices included in the plotting package CG Displays surface brightnesses of two formulas or up to two data files prepared by options EA or PR. Ratios, differences, and simultaneous plots with error bars are possible. DA Displays data files of type 1 (from options EA and PR) DG Displays radius parameter, surface brightness, magnitude, luminosity functions, colors, etc. for a data file(s) of galaxies (type 3). DP Creates a shaded plot of a map on an Apple LaserWriter, a Lasergrafix, a graphics teminal, a Printronix, or a Versatek. DT Outputs pixel values from row(s) into a file which can then be sent to a lineprinter or the terminal. GR Allows one to add annotation to the Grinnell display IP Does simple image processing on a Grinnell, Trapix, Ramtek, or SAOimage after it has been loaded. PI Produces a simple contour plot on a line printer PL Plots one or more lines of pixel values from a map or maps on any supported plot device. One can plot horizontally (a row), vertically (a column), or at any angle. Cursor feedback is supported. PT Prints data values on a terminal SU Creates a surface brightness mesh plot of a map on any supported plot device. T2 Overlays circles for objects in data file of type 2 on any Page 4 supported display device. TV Does a gray scale display on a Grinnell, Trapix, Ramtek, or SAOimage 2 EDit Edits data or headers CF Revalues all pixel values which are below a chosen lower limit and above a chosen upper limit and which are within a selected area of a map(s) E2 Edits data within a data file prepared by option CT (type 2) E3 Edits data within a data file of galaxy parameters (type 3) EC Edits data within a circular area of a map ED Edits data within a data file prepared by options EA and PR (type 1) EH Edits SAD headers by using FITS keywords. EP Edits data one point at a time ER Edits data within a rectangular area MF Takes the mean and/or median of 3 night sky flat field exposures mutually offset from each other and thereby removes offending objects MH Edits Headers for direct (RA, DEC) maps without making use of FITS keywords. OF Removes offending objects by two-dimensional linear interpolation PH Displays the header information of a SAD file on a terminal RV Revalues pixel values within a specified range within a manually given area of a map(s) to a new value. TY Allows entering of entire lines of data into a SAD file 2 FIlters Filters real and complex data in 1 and 2 dimensions FD Does boxcar, gaussian, unsharp mask, and user input filtering of SAD files in the spatial domain. FF Filters Fourier transforms in one and two dimensions. OP Does an optimum filter from Brault and White on complex maps 2 PHotometry Does spectral, stellar, and surface photometry BB Does aperture photometry on stars or small galaxy images BK Fits a two-dimensional polynomial of any degree to a map. TV cursor box input is possible. C1 Fits splines to a spectrum continuum by means of a graphics terminal crosshairs EA Does averaging of surface brightness in elliptical annulae and saves and displays the results EM Measures emission line equivalent widths LI Calculates line indexes for spectra PM Does photometry on F(wavelength) maps using systems Page 5 tabulated in [_.MIIPS.DOC]PHOTOM.SYS PR Computes the center, inclination, eccentricity, average surface brightness, and integrated surface brightness for annuli of an elliptical galaxy. RF Corrects a spectrum for differential refraction along slit RG Solves for the coefficients of a chosen galaxy surface brightness law from a file prepared by options EA or PR. SG Smooths the X and Y locations, the inclination, and the eccentricity of galaxy as solved for by PROFILE; the surface brightness is then recomputed. 2 TOpology Contracts, expands, and rotates maps and shifts bits BI Bins up pixel values within rectangular areas CM Copys maps from one file to another CU Cuts out a region of a map to another map FM Flips maps in X or Y or both (=180 degree rotation) IN Interpolates spectral maps to -> same origin and increment ME Merges data of different dispersions or grating settings RO Rotates maps about any center and places them at any new center. S2 Removes selected speckle images from a UM speckle file S4 Registers all speckle maps in a file to first map in the file SH Moves rows, with scaling, from one map to another (the same,smaller, or larger). XC Expands or contracts maps in column and/or row direction XY Shifts maps in X and/or Y directions 2 UTilities Converts formats, fits curves, and does statistics DEB Turns on the DEBUG trace (to find where an error is) DEF Constructs a sequence of commands DSK Gives access to disk and the VAX commands; use LO to return to MIIPS. FA Creates a map with artificial two-dimensional images. A gaussian formula or data from a file may be used and speckle images of a binary can also be created. FE Creates a map with an artificial spectrum, containing a continuum, absorption lines, and/or emission lines. FG Allows one to create a map with artificial galaxy images using a chosen surface brightness law or data from a file FS Flattens a spectrum by fitting a polynomial to it or by interpolating with polynomials GA Calculates gaussian statistics LR Does linear regression of one row on another MM Calculates the minimum and maximum in specified areas MP Imports foreign disk files, e.g. FITS, to the SAD format NI Adds artificial gaussian noise to a map or data file RW Writes "SYS:RT11RD" files to SAD files, including Page 6 headers SA Uses one SAD map as a mask for determining pixel values for a second SAD map. Regions equal to zero in the mask result in zeros for an output file. SI Converts VAX unformated files to SAD files SS Models overlapping stars in a map with a standard light distribution and subtracts SVE Allows one to inspect .SVE files on disk TI Calculates the Julian Day number, sidereal time, azimuth, altitude, and zenith distance XP Exports a SAD file to an 8-bit or 16-bit binary file with one row per record. There is no header included at present. DETAILED COMMAND DESCRIPTIONS The individual commands are documented in more detail as separate files, *.DOC, in [MIIPS.DOC] or DTAB:. Each file contains a brief description of the operation and an example of its use (with prompts answered and brief explainations).