Figaro: Commands

Keith Shortridge, AAO

28th April 1995


1. Alphabetic list of commands

This is a list of all the Figaro commands included in Figaro 4.2.

ABCONV Convert spectrum from Janskys into AB magnitudes

ABLINE Interactive absorption line analysis

ADJOIN Append two spectra (strictly a merge by wavelength value)

ALASIN Read a spectrum in ALAS (Abs. Line Analysis System) format

ALASOUT Output a spectrum in ALAS (Abs. Line Analysis System) format

ARC Interactive manual arc line identification

BCLEAN Automatic removal of bad lines & cosmic rays from CCD data

BFFT Takes the reverse FFT of a complex data structure

BPLOT Plots out a 'build' file generated by SPLOT

BSMULT Atmospheric band removal using a B star calibration spectrum

CALDIV Generate calibration spectrum from continuum standard spectra

CCDLIN Applies a linearity correction to AAO CCD data

CCUR After SPLOT, uses graphics cursor to indicate data values

CENTERS Generate file of object centroids from CPOS output

CDIST S-distortion correction using SDIST results

CFIT Generate a spectrum using the cursor

CLEAN Interactive patching of bad lines, bad pixels in an image

CLIP Clip data above and below a pair of threshold values

CMPLX2I Extracts the imaginary part of a complex data structure

CMPLX2M Extracts the modulus of a complex data structure

CMPLX2R Extracts the real part of a complex data structure

CMPLXADD Add two complex structures

CMPLXCONJ Produce the complex conjugate of a complex structure

CMPLXDIV Divide two complex structures

CMPLXFILT Create a mid-pass filter for complex data

CMPLXMULT Multiply two complex structures

CMPLXSUB Subtract two complex structures

COADD Form the spectrum which is the mean of the rows in an image

COLOUR Set image display colour table

COMBINE Combine two spectra, adding with weights according to errors

COSBELL Create data that goes to zero at the edges in a cosine bell

COSREJ Reject cosmic rays from a set of supposedly identical spectra

CPOS Select points with image display cursor

CROBJ Create a data object or file

CSET Interactively set regions of a spectrum to a constant value

CSPIKE Create calibration spiketrum given spiketrum & standard spectrum

DELOBJ Delete a data object or a file

DVDPLOT Plot the data in one file against the data in another

ECHARC Fit an echelle arc

ECHFIND Locate spectra in echelle data

ECHMASK Produce an extraction mask from an SDIST analysis

ECHMERGE Merge echelle spectra into a single long spectrum

ECHSELECT Interactive selection of sky and object spectra for an echelle

ELSPLOT Produces a long (<3m) error bar plot of a spectrum

EMLT Fits gaussians to the strongest lines in a spectrum

ERRCON Converts percentage error values to absolute values

ESPLOT Produces an error bar plot of a spectrum

EXAM Examines the contents of a data object

EXTIN Correct spectrum for atmospheric extinction

EXTLIST Adds a number of non-contiguous lines in an image -> a spectrum

EXTRACT Adds contiguous lines of an image -> a spectrum

FET321 Extracts a spectrum from 1 detector from etalon mode FIGS data

FF Flat field an image (uses JT's algorithm)

FFCROSS Cross-correlate an image and a flat field (mainly IPCS data)

FFT Takes the forward FFT of a complex data structure

FIGINFO Describes the contents of a Figaro data file

FIGS321 Processes a FIGS data cube down to a single spectrum

FIGS322 Processes a FIGS data cube down to an image

FIGS422 Process a FIGS image-mode hypercube down to an image

FIGS423 Process a FIGS image-mode hypercube down to a cube

FIGS424 Sort a FIGS image-mode hypercube into wavelength order

FIGSEE Generate a seeing ripple spectrum from a FIGS spectrum

FIGSFLUX Flux calibrates a FIGS spectrum

FINDSP Locate fibre spectra in an image

FITS Read data from a FITS format tape

FITSET Set the value of a FITS keyword

FITSKEYS List the FITS keywords in a data file

FLAG2QUAL Converts a quality array into `flagged' values

FLCONV Convert a spectrum in Janskys into one in Ergs/cm**2/s/A

FOTO Perform aperture photometry given CENTERS output

FSCRUNCH Rebin data with a disjoint wavelength coverage to a linear one

FWCONV General unit conversion for spectra

GAUSS Interactive fit of Gaussians to emission or absorption lines

GROWX Performs reverse function to that of EXTRACT

GROWXT Copies an image into contiguous XT planes of a cube

GROWXY Copies an image into contiguous XY planes of a cube

GROWY Performs reverse function to that of YSTRACT

GROWYT Copies an image into contiguous YT planes of a cube

GSPIKE Generates a 'spiketrum' from a table of values

HARD Sets the file name for hard copy output

HIST Produce histogram of data value distribution in an image

HOPT Histogram optimization of an image

I2CMPLX Copies an array into the imaginary part of a complex structure

IADD Adds two images (or two spectra)

IARC Given fit to single spectrum, fit all spectra in a 2D arc

ICADD Adds a constant to an image

ICDIV Divides an image by a constant

ICMULT Multiplies an image by a constant

ICONT Produces a contour map of an image

ICONV3 Convolve an image with a 3x3 convolution kernel

ICOR16 Corrects 16 bit data from signed to unsigned range

ICSUB Subtracts a constant from an image

ICUR Uses ARGS cursor to show x,y and data values

IDIFF Takes the 'differential' of an image

IDIV Divides two images (or two spectra)

IGCONV Convolve an image with a specified filter

IGREY Produces a grey-scale plot of an image

ILASER Produce a postscript file showing an image

ILIST List the data in an image (or spectrum)

ILOG Takes the logarithm of an image

IMAGE Display an image on the selected image display

IMAGEPS Create a Postscript file giving a grey scale image picture

IMULT Multiplies two images (or two spectra)

INTERP Interpolates between the points of a 'spiketrum' -> a spectrum

IPLOTS Plots successive cross-sections of an image, several to a page

IPOWER Raises an image to a specified power

IRCONV Converts data in Janskys to W/m**2/um

IREVX Reverse an image (or spectrum) in the X-direction

IREVY Reverse an image in the Y-direction

IRFLAT Generates a ripple spectrum from an IR spectrum

IRFLUX Flux calibrates an IR spectrum using a black-body model

ISCRUNCH Rebin an image to linear wavelength scale given IARC results

ISCRUNI Like ISCRUNCH, but interpolates between two IARC result sets

ISEDIT Allows interactive editing of a 1D or 2D spectrum

ISHIFT Applies a linear x and a linear y shift to an image

ISMOOTH 2D smooth of image using 9-point smoothing algorithm

ISPLOT Plots successive cross-sections through an image

ISTAT Provides some statistics about an image (max, min etc.)

ISTRETCH Stretches and shifts an image in X and Y.

ISUB Subtracts two images (or two spectra)

ISUBSET Produces a subset of an image

ISUPER Produces a superset of an image

ISXADD Adds a spectrum to each X direction x-section of an image

ISXDIV Divides a spectrum into each X direction x-section of an image

ISXMUL Multiplies each X direction image x-sect by a spectrum

ISXSUB Subtracts a spectrum from each X direction x-section of an image

ISYADD Adds a spectrum to each Y direction x-section of an image

ISYDIV Divides a spectrum into Y direction x-section of an image

ISYMUL Multiplies each Y direction image x-sect by a spectrum

ISYSUB Subtracts a spectrum from Y direction x-section of an image

IXSMOOTH Smooth in x-direction by gaussian convolution

LET Assign a value to a named data object or variable

LINTERP Linear interpolation between spiketrum points -> spectrum

LSPLOT Hardcopy spectrum plot of specified size (up to 3 metres)

LXSET Set X array of spectrum/image to specified range

LYSET Set Y array of spectrum/image to specified range

MASK Generate a mask spectrum given a spectrum and a mask table

MASKEXT Extracts echelle orders using a mask created by ECHMASK

MCFIT Fit a continuum to a spectrum, given a mask spectrum

MEDFILT Applies a square median filter to an image

MEDFILTR Applies a rectangular median filter to an image

MEDSKY Take the median of a number of images

MSPLOT Plots a long spectrum as a series of separate plots

NCSET Set a region of a spectrum to a constant

OFFDIST Applies an offset to an SDIST fit

OPTEXTRACT Extracts a long slit spectrum using Horne's optimal extraction

OVERPF Overlays a FINDSP fit on another image

PEAK Determines position of highest peak in a spectrum

POLEXT Extract fibre spectra from an image after a FINDSP analysis

POLYSKY Fits and subtracts sky from a long slit spectrum

PROFILE Determines a long slit spectrum profile for use by OPTEXTRACT

QUAL2FLAG Converts `flagged values' to produce a quality array

R2CMPLX Creates a complex data structure from a real data array

RDFITS Read FITS format disk file

RDIPSO Read file in DIPSO/IUEDR/SPECTRUM format

REMBAD Removes pixels that have been flagged as bad from data

RENOBJ Changes the name of a data object

RESAMPLE Rebin an image to different dimensions and/or orientation

RETYPE Changes the type of the main data array in a file

REWIND Rewinds either the input or output tape

ROTATE Rotates an image through 90 degrees

ROTX Rotate data along the X-axis

RSPDM Reads a spectrum in FORTH PDM/TYB format

SCNSKY Calculates a sky spectrum for a scanned CCD image

SCROSS Cross-correlate two spectra & get relative shift

SCRUNCH Rebin a spectrum to a linear wavelength range

SDIST Analyse an image containing spectra for S-distortion

SFIND Reads data from a tape in SDRSYS format

SFIT Fit a polynomial to a spectrum

SKIP Skips files on tape

SOFT Sets the device/type for terminal graphics

SLICE Takes a slice with arbitrary end points through an image

SPFLUX Applies a flux calibration spectrum to an observed spectrum

SPIED Interactive spiketrum editor

SPIFIT Fits a global polynomial to a spiketrum -> a spectrum

SPLOT Plots a spectrum

SQRTERR Generates an error array as Error = Square Root of (Data/Const)

SURFIT Fits an image using bi-cubic splines

TAPE Sets the tape drive to be used for input

TAPEO Sets the tape drive to be used for output

TIPPEX Modify individual pixel values with cursor

TRIMFILE Cuts down the size of a Figaro file by removing any deadwood

VACHEL Air to vacuum, and/or recession velocity wavelength conversion

VSHOW Displays the values of Figaro user variables

WDFITS Writes out a disk file in FITS format

WDIPSO Writes a file in DIPSO/IUEDR/SPECTRUM format

WIFITS Writes an image (or spectrum) to tape in FITS format

XCADD Adds a constant to the X data in a file

XCDIV Divides the X data in a file by a constant

XCMULT Multiplies the X data in a file by a constant

XCOPI Like XCOPY but interpolates X-data from 2 files

XCOPY Copy X-info (eg wavelengths) into a spectrum

XCSUB Subtracts a constant from the X data in a file

XCUR Uses cursor to delimit part of a spectrum

XTPLANE Adds contiguous XT planes of a data cube -> an image

XYPLANE Adds contiguous XY planes of a data cube -> an image

YSTRACT Adds contiguous columns of an image -> a spectrum

YTPLANE Adds contiguous YT planes of a data cube -> an image

2. Classified commands

A list of the Figaro commands, broken down into rather rough and ready groups. If you can find what you're looking for here in the section you expect then that's fine; if not, try the alphabetic list to be found earlier in this document. Note that some commands turn up under more than one heading.

2.1. Data input

Commands connected with reading data either from tape or from disk files output by other data reduction programs. Most tape input routines require that the input tape be defined first using 'TAPE'. RDIPSO is able to read a number of very simple data formats, and text files of data can often be easily edited to allow it to read them.

ALASIN Read a spectrum in ALAS (Abs. Line Analysis System) format

FITS Read data from a FITS format tape

FITSET Set the value of a FITS keyword

FITSKEYS List the FITS keywords in a data file

ICOR16 Corrects 16 bit data from signed to unsigned range

RDFITS Read file in AAO de facto 'Disk FITS' format

RDIPSO Read file in DIPSO/IUEDR/SPECTRUM format

REWIND Rewinds either the input or output tape

SKIP Skips files on tape

TAPE Sets the tape drive to be used for input

2.2. Data output

Routines that write out Figaro data in other formats, either to tape or to disk. The routines that output to tape require the output tape to be selected using the 'TAPEO' command first.

ALASOUT Output a spectrum in ALAS (Abs. Line Analysis System) format

TAPEO Sets the tape drive to be used for output

WDFITS Writes an image out in the AAO de facto 'Disk FITS' format

WDIPSO Writes a file in DIPSO/IUEDR/SPECTRUM format

WIFITS Writes an image (or spectrum) to tape in FITS format

2.3. Display commands

Routines that display the data in Figaro files, either on the image display or on a graphics device. Most of the line graphics routines take a 'HARD' keyword to force output to the current hardcopy device. The 'HARD' and 'SOFT' commands set respectively the current hardcopy and softcopy graphics devices. LSPLOT will only plot to a hardcopy device, and has that device as a command parameter.

BPLOT Plots out a 'build' file generated by SPLOT

CCUR After SPLOT, uses graphics cursor to indicate data values

COLOUR Set image display colour table

CPOS Select points with image display cursor

DVDPLOT Plot the data in one file against the data in another

ELSPLOT Produces a long (<3m) error bar plot of a spectrum

ESPLOT Produces an error bar plot of a spectrum

HARD Sets the file name for hard copy output

HOPT Histogram optimization of an image

ICONT Produces a contour map of an image

ICUR Uses ARGS cursor to show x,y and data values

IGREY Produces a grey-scale plot of an image

ILASER Produce a postscript file showing an image

IMAGE Display an image on the selected image display

IMAGEPS Create a Postscript file giving a grey scale image picture

IPLOTS Plots successive cross-sections of an image, several to a page

ISPLOT Plots successive cross-sections through an image

LSPLOT Hardcopy spectrum plot of specified size (up to 3 metres)

MSPLOT Plots a long spectrum as a series of separate plots

SOFT Sets the device/type for terminal graphics

SPLOT Plots a spectrum

XCUR Uses cursor to delimit part of a spectrum

2.4. Wavelength calibration

Routines connected with wavelength calibration of spectra. for further details see the `Techniques' documentation.

ARC Interactive manual arc line identification

ECHARC Fit an echelle arc

EMLT Fits gaussians to the strongest lines in a spectrum

FSCRUNCH Rebin data with a disjoint wavelength coverage to a linear one

IARC Given fit to single spectrum, fit all spectra in a 2D arc

ISCRUNCH Rebin an image to linear wavelength scale given IARC results

ISCRUNI Like ISCRUNCH, but interpolates between two IARC result sets

LXSET Set X array of spectrum/image to specified range

SCRUNCH Rebin a spectrum to a linear wavelength range

VACHEL Air to vacuum, and/or recession velocity wavelength conversion

XCOPI Like XCOPY but interpolates X-data from 2 files

XCOPY Copy X-info (eg wavelengths) into a spectrum

2.5. B star calibration

Routines connected with B star calibration. See the section on this topic in the `techniques' documentation for more information.

BSMULT Atmospheric band removal using a B star calibration spectrum

CFIT Generate a spectrum using the cursor

CSET Interactively set regions of a spectrum to a constant value

MASK Generate a mask spectrum given a spectrum and a mask table

MCFIT Fit a continuum to a spectrum, given a mask spectrum

NCSET Set a region of a spectrum to a constant

2.6. Arithmetic operations

Routines connected with general 'arithmetic' manipulation of images and spectra. Note that generally anything that works on an image will also work on a spectrum, since a spectrum is just a special case of an image. See also the classification called `Data manipulation'.

CLIP Clip data above and below a pair of threshold values

IADD Adds two images (or two spectra)

ICADD Adds a constant to an image

ICDIV Divides an image by a constant

ICMULT Multiplies an image by a constant

ICONV3 Convolve an image with a 3x3 convolution kernel

ICSUB Subtracts a constant from an image

IDIFF Takes the 'differential' of an image

IDIV Divides two images (or two spectra)

ILOG Takes the logarithm of an image

IMULT Multiplies two images (or two spectra)

IPOWER Raises an image to a specified power

IREVX Reverse an image (or spectrum) in the X-direction

IREVY Reverse an image in the Y-direction

ISHIFT Applies a linear x and a linear y shift to an image

ISMOOTH 2D smooth of image using 9-point smoothing algorithm

ISTRETCH Stretches and shifts an image in X and Y.

ISUB Subtracts two images (or two spectra)

ISUBSET Produces a subset of an image

ISUPER Produces a superset of an image

ISXADD Adds a spectrum to each X direction x-section of an image

ISXDIV Divides a spectrum into each X direction x-section of an image

ISXMUL Multiplies each X direction image x-sect by a spectrum

ISXSUB Subtracts a spectrum from each X direction x-section of an image

ISYADD Adds a spectrum to each Y direction x-section of an image

ISYDIV Divides a spectrum into each Y direction x-section of an image

ISYMUL Multiplies each Y direction image x-sect by a spectrum

ISYSUB Subtracts a spectrum from each Y direction x-section of an image

IXSMOOTH Smooth in x-direction by gaussian convolution

RESAMPLE Rebin an image to different dimensions and/or orientation

ROTX Rotate data along the X-axis

2.7. Flat fields

Routines connected with Flat field calibrations. See also the section on this topic in the `techniques' documentation.

CFIT Generate a spectrum using the cursor

FF Flat field an image (uses JT's algorithm)

FFCROSS Cross-correlate an image and a flat field (mainly IPCS data)

MASK Generate a mask spectrum given a spectrum and a mask table

MCFIT Fit a continuum to a spectrum, given a mask spectrum

ISXDIV Dividesa spectrum into each X direction x-section of an image

2.8. Data manipulations

Routines that manipulate images or spectra in more complicated ways that are covered under `arithmetic operations'

ADJOIN Append two spectra (strictly a merge by wavelength value)

BCLEAN Automatic removal of bad lines & cosmic rays from CCD data

CFIT Generate a spectrum using the cursor

CLEAN Interactive patching of bad lines, bad pixels in an image

COADD Form the spectrum which is the mean of the rows in an image

COMBINE Combine two spectra, adding with weights according to errors

COSREJ Reject cosmic rays from a set of supposedly identical spectra

CROBJ Create a data object or file

FSCRUNCH Rebin data with a disjoint wavelength coverage to a linear one

HIST Produce histogram of data value distribution in an image

HOPT Histogram optimization of an image

ICONV3 Convolve an image with a 3x3 convolution kernel

ICOR16 Corrects 16 bit data from signed to unsigned range

IDIFF Takes the 'differential' of an image

IREVX Reverse an image (or spectrum) in the X-direction

IREVY Reverse an image in the Y-direction

MEDFILT Applies a square median filter to an image

MEDFILTR Applies a rectangular median filter to an image

MEDSKY Take the median of a number of images

POLYSKY Fits and subtracts sky from a long slit spectrum

ROTATE Rotates an image through 90 degrees

SCNSKY Calculates a sky spectrum for a scanned CCD image

SCROSS Cross-correlate two spectra & get relative shift

SCRUNCH Rebin a spectrum to a linear wavelength range

SFIT Fit a polynomial to a spectrum

SURFIT Fits an image using bi-cubic splines

2.9. Aperture photometry

Routines connected with aperture photometry.

CENTERS Generate file of object centroids from CPOS output

CPOS Select points with image display cursor

FOTO Perform aperture photometry given CENTERS output

2.10. Absorption line analysis

Figaro has one routine specially designed for interactive absorption line analysis (ABLINE), but GAUSS can also be used for this.

ABLINE Interactive absorption line analysis

GAUSS Interactive fit of Gaussians to emission or absorption lines

2.11. Gaussian fitting

One routine designed for interactive fitting of Gaussians to lines, and one fast routine to fit lines in a spectrum -- often used to check on instrument focus during observing.

EMLT Fits gaussians to the strongest lines in a spectrum

GAUSS Interactive fit of Gaussians to emission or absorption lines

2.12. S-distortion and echelle order straightening

Routines connected with S-distortion corrections. The Fibre extraction routines are also included here. Nowadays the S-dirtortion routines are mainly used for straightening echelle orders.

CDIST S-distortion correction using SDIST results

ICUR Uses display cursor to show indicate points in image

FINDSP Locate fibre spectra in an image

OFFDIST Applies an offset to an SDIST fit

OVERPF Overlays a FINDSP fit on another image

POLEXT Extract fibre spectra from an image after a FINDSP analysis

SDIST Analyse an image containing spectra for S-distortion

2.13. Fudging data

A dirty set of routines connected with manipulating data arrays etc `by hand'.

CSET Interactively set regions of a spectrum to a constant value

DELOBJ Delete a data object or a file

ISEDIT Allows interactive editing of a 1D or 2D spectrum

LET Assign a value to a named data object or variable

LXSET Set X array of spectrum/image to specified range

LYSET Set Y array of spectrum/image to specified range

NCSET Set a region of a spectrum to a constant

RENOBJ Changes the name of a data object

SPIED Interactive spiketrum editor

TIPPEX Modify individual pixel values with cursor

XCADD Adds a constant to the X data in a file

XCDIV Divides the X data in a file by a constant

XCMULT Multiplies the X data in a file by a constant

XCSUB Subtracts a constant from the X data in a file

2.14. Examining data

Routines for looking at the contents of data arrays, other than through the use of graphics devices.

EXAM Examines the contents of a data object

FIGINFO Describes the contents of a Figaro data file

FITSKEYS List the FITS keywords in a data file

ILIST List the data in an image (or spectrum)

ISTAT Provides some statistics about an image (max, min etc.)

2.15. Slicing through images and cubes

Routines that extract spectra from images, and routines that plug spectra into images. Also routines that extract images from data cubes, and those that plug images into cubes. The optimal extraction routines are also included here.

EXTLIST Adds a number of non-contiguous lines in an image -> a spectrum

EXTRACT Adds contiguous lines of an image -> a spectrum

GROWX Performs reverse function to that of EXTRACT

GROWXT Copies an image into contiguous XT planes of a cube

GROWXY Copies an image into contiguous XY planes of a cube

GROWY Performs reverse function to that of YSTRACT

GROWYT Copies an image into contiguous YT planes of a cube

OPTEXTRACT Extracts a long slit spectrum using Horne's optimal extraction

PROFILE Determines a long slit spectrum profile for use by OPTEXTRACT

SLICE Takes a slice with arbitrary end points through an image

XTPLANE Adds contiguous XT planes of a data cube -> an image

XYPLANE Adds contiguous XY planes of a data cube -> an image

YSTRACT Adds contiguous columns of an image -> a spectrum

YTPLANE Adds contiguous YT planes of a data cube -> an image

2.16. Fibre data

Routines connected with obtaining spectra from images take using fibres (either with aperture plates or using AUTOFIB or similar instruments).

FINDSP Locate fibre spectra in an image

POLEXT Extract fibre spectra from an image after a FINDSP analysis

OVERPF Overlays a FINDSP fit on another image

2.17. Flux calibration

Routines connected with the use of flux calibration standards. Note that the type of calibration data available affects the choice of routines. FIGS data has to be treated separately; FIGSFLUX is a rather specialised routine. For more details, see the section on this topic in the `Techniques' documentation.

ABCONV Convert spectrum from Janskys into AB magnitudes

CALDIV Generate calibration spectrum from continuum standard spectra

CFIT Generate a spectrum using the cursor

CSET Interactively set regions of a spectrum to a constant value

CSPIKE Create calibration spiketrum given spiketrum & standard spectrum

FIGSFLUX Flux calibrates a FIGS spectrum

FLCONV Convert a spectrum in Janskys into one in Ergs/cm**2/s/A

FWCONV General unit conversion for spectra

GSPIKE Generates a 'spiketrum' from a table of values

INTERP Interpolates between the points of a 'spiketrum' -> a spectrum

IRFLUX Flux calibrates an IR spectrum using a black-body model

LINTERP Linear interpolation between spiketrum points -> spectrum

NCSET Set a region of a spectrum to a constant

SFIT Fit a polynomial to a spectrum

SPFLUX Applies a flux calibration spectrum to an observed spectrum

SPIED Interactive spiketrum editor

SPIFIT Fits a global polynomial to a spiketrum -> a spectrum

2.18. Extinction

Commands connected with generating a spectrum of extinction coefficients and applying them. For more details, see the section on this topic in the `Techniques' documentation.

EXTIN Correct spectrum for atmospheric extinction

GSPIKE Generates a 'spiketrum' from a table of values

LINTERP Linear interpolation between spiketrum points -> spectrum

2.19. Complex data and FFTs

Routines that manipulate complex data structures, mainly connected with Fourier transforms.

BFFT Takes the reverse FFT of a complex data structure

CMPLX2I Extracts the imaginary part of a complex data structure

CMPLX2M Extracts the modulus of a complex data structure

CMPLX2R Extracts the real part of a complex data structure

CMPLXADD Add two complex structures

CMPLXCON Produce the complex conjugate of a complex structure

CMPLXDIV Divide two complex structures

CMPLXFILT Create a mid-pass filter for complex data

CMPLXMULT Multiply two complex structures

CMPLXSUB Subtract two complex structures

COSBELL Create data that goes to zero at the edges in a cosine bell

FFT Takes the forward FFT of a complex data structure

I2CMPLX Copies an array into the imaginary part of a complex structure

PEAK Determines position of highest peak in a spectrum

R2CMPLX Creates a complex data structure from a real data array

ROTX Rotate data along the X-axis

2.20. Infra-red data

Commands connected specially with infra-red instruments. These particularly include commands to handle data from FIGS (the AAO's Fabry-Perot Infra-Red Grating Spectrometer) whose data comes in strange forms (data cubes and data hypercubes) and needs special processing, but also additional commands designed to handle general IR data. Note that a set of Figaro programs designed for use with data from the AAO IRIS detector is available separately.

FET321 Extracts a spectrum from 1 detector from etalon mode FIGS data

FIGS321 Processes a FIGS data cube down to a single spectrum

FIGS322 Processes a FIGS data cube down to an image

FIGS422 Process a FIGS image-mode hypercube down to an image

FIGS423 Process a FIGS image-mode hypercube down to a cube

FIGS424 Sort a FIGS image-mode hypercube into wavelength order

FIGSEE Generate a seeing ripple spectrum from a FIGS spectrum

FIGSFLUX Flux calibrates a FIGS spectrum

IRCONV Converts data in Janskys to W/m**2/um

IRFLAT Generates a ripple spectrum from an IR spectrum

IRFLUX Flux calibrates an IR spectrum using a black-body model

REMBAD Removes pixels that have been flagged as bad from data

2.21. Quality information

A set of routines that explicitly manipulate the quality information held in a file, in particular converting the way the quality information is held from a `flagged' value representation to a separate quality array -- and vice-versa.

FIGINFO Describes the contents of a Figaro data file

FLAG2QUAL Converts a quality array into `flagged' values

QUAL2FLAG Converts `flagged values' to produce a quality array

2.22. Echelle data

A set of commands used for processing echelle data - particularly

aimed at the UCL echelle (UCLES) in use at AAO.

CDIST S-distortion correction using SDIST results

ECHARC Fit an echelle arc

ECHFIND Locate spectra in echelle data

ECHMASK Produce an extraction mask from an SDIST analysis

ECHMERGE Merge echelle spectra into a single long spectrum

ECHSELECT Interactive selection of sky and object spectra for an echelle

ICUR Uses display cursor to show indicate points in image

IMAGE Display an image on the selected image display

MASKEXT Extracts echelle orders using a mask created by ECHMASK

OFFDIST Applies an offset to an SDIST fit

SDIST Analyse an image containing spectra for S-distortion

2.23. Miscellany

Miscellaneous commands that didn't seem to fit anywhere else.

CCDLIN Applies a linearity correction to AAO CCD data

ERRCON Converts percentage error values to absolute values

RETYPE Changes the type of the main data array in a file

SQRTERR Generates an error array as Error = Square Root of (Data/Const)

TRIMFILE Cuts down the size of a Figaro file by removing any deadwood

VSHOW Displays the values of Figaro user variables