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
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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
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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
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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
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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
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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).