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1. C compiler Generic Fortran subroutine compiler Error message generator Fortran code improver Software porting tools X library linker FTNCHEK SUN 172 MUD 153 Detect errors in Fortran 77 source code especially mistakes that tend to be missed by compilers and linkers Probably its most valuable feature is the careful checks it performs on subprogram interfaces It examines the actual arguments in each CALL statement or FUNCTION call and compares them with the correspond ing formal arguments of the SUBROUTINE or FUNCTION subprogram It warns of mismatches in the number of arguments and incompatibilities in the data type and dimensions of each one It also checks that arguments used before being set in a subprogram have defined values on entry and correspondingly that arguments are set on exit when their values are used later in the calling program GCC The GNU C compiler GENERIC Support generic subroutines Preprocesses a generic Fortran subroutine one written to cover several different data types into one routine per data type and concatenates these routines into a file The file is then compiled by the Fortran compiler to produce an object module MESSGEN Associate error messages with status values returned by Starlink infrastructure routines This works in conjunction with the Starlink Error Message Service EMS It enables more informative error messages to be sent to the user S
2. Coherent storage of fit results The results of line or continuum fits are stored with the data When a hyper cube is a coherent set of spectra fit results are also stored coherently For example in a 3 d data set the 2 d map of line integrals is immediately available to display routines Bad values and variance Bad values or quality information are recognised and ignored or propagated as appropriate If variance information is preset it is propagated or used in the processing Analysis of line profiles Analysis of calibrated long slit spectra fitting of Gaussians either manually or automatically in batch handling of data with two spatial dimensions such as Taurus data The topics addressed by the applications are mainly ASCII I O The data and errors of hyper cubes can be written to or read from printable editable tables Bad values are converted between the two formats Single spectra can be read even if the axis data are not linear or monotonic Graphics Displays allow full control of the plot including font colour line styles error bars etc Overlay on previous plots according to their world coordinates is possible including overlays on grey colour line plots made using KAPPA PONGO etc Cube processing You can extract averaged hyper planes from hyper cubes assemble hyper cubes from hyper planes or fill in a hyper cube from several given hyper cubes Arc line axis wavelength calibration While full u
3. HDX V0 1 A flexible extensible data model for astronomical images tables and other metadata new JAIUTIL V1 0 Utility classes for JAI new JETTY V4 0 4 HTTP Server and Servlet Container new JNIAST V2 0 4 Java Native interface to AST update JNIHDS V0 3 Java Native Interface to HDS update JSKY V2 0 Java Components for Astronomy new JUNIT V3 7 Third party unit testing framework junit new NDX V0 1 N dimensional astronomical object manipulation and I O new PAL V0 1 Positional Astronomy Library new RV V1 0 Java UI for RV new TABLE V0 3 Generic table manipulation and I O new TAMFITS V0 93 Third party basic FITS access nom tam new UTIL V0 1 Miscellaneous utillity classes new VOTABLE V1 0 VOTable I O new The STARJAVA package can be considered to be independent of the standard USSC and in future will be distributed separately All the STARJAVA applications and classes are distributed under the GPL licence The SPLAT documentation SUN 243 SPLAT A Spectral Analysis Tool has been updated and can be found in star starjava docs splat sun243 htx sun243 html It also appears in the DOCS package and can be seen with the command showme sun243 STARJAVA is not available under Tru64 Unix SUN 1 24 Changes since the last issue 4 2 2 Withdrawn Packages No packages have been withdrawn at this release 2 3 Package details Some packages listed in this document are not distributed on Starlink CDs
4. SUN 1 24 Packages 14 Its core is a suite of programs to process large amounts of data Consequently all the routines process lists of data and also record progress using a log system As well as performing the usual instrumental corrections you can also remove defects and generate and propagate data errors Debiassing can be performed using only the bias strips as well as using bias frames combined to reduce noise levels Calibration data can be combined using many different techniques mean median trimmed mean etc so you can pick a method that makes the most efficient use of your data Data registration is based primarily on the linear transformation allowing offsets scalings rotation and shear although more general transformations can be used General linear transforms can easily be determined using an interactive procedure to display and select image features Alternatively if your datasets are just shifted with respect to each other you may be able to register them by using a series of commands which locate all the objects in all the frames determine the object object correspondence and then derive the transforms A graphical application is also provided that allows you to select the objects to be used by identifying image pairs that overlap and have some objects in common Data resampling uses registering transforms which it stores inside your data removing the need to remember them They may also be applied to ru
5. e Display graphs showing the profiling cross section results e Detect faint diffuse objects in an image It processes images in NDF format so you can use it in conjunction with packages like K APPA CCDPACK FIGARO PHOTOM JJCMTDR and PISA You can define areas to exclude or include in the analysis using keyword descriptions in text files Extractor Locate and parameterize objects in a 2 d image EXTRACTOR is a program for automatically detecting objects on an astronomical image and building a catalogue of their properties It is particularly suited for the reduction of large scale galaxy survey data but also performs well on other astronomical images EXTRACTOR is a development of Emmanuel Bertin s SExtractor Source Extractor program repackaged for use in the Starlink Software Environment This means that it uses the Starlink parameter system accepts images in NDF format and uses the AST library for astrometry A traditional image display tool like SAOIMAGE but which can integrate other programs It is derived from the RTD Real Time Display tool developed as part of the project at RTD is free software under the terms of the GNU copyright The current version is a preliminary release which is intended to assess the impact of GAIA RTD s enhancements for performing highly interactive graphical image analysis It provides the following functions Display images in FITS and formats it will display many other forma
6. It is biased towards data reduction and can handle several different instruments POLMAP on the other hand does no data reduction but was designed with data analysis in mind POLMAP can also display data that TSP cannot handle and can read and write TSP polarization spectrum format files POLPACK Imaging Polarimetry data reduction POLPACK is a package of applications for mapping the linear or circular polarization of extended astronomical objects Data from both single and dual beam polarimeters can be processed POLPACK processes data in NDF format Other astronomical data formats may also be processed using transparent on the fly data conversion facilities provided by the NDF subroutine library and the CONVERT package The facilities provided by POLPACK include e alignment of images on the sky extraction of O and E images from a single frame e sky subtraction calculation of Stokes parameters binning of Stokes parameters creation of catalogues of polarization vectors graphical display of vector maps POLPACK does not provide facilities for performing instrumental corrections such as flat fielding de biassing etc Such corrections should be applied to the data before using POLPACK so that POLPACK can assume that pixel values are proportional to the combined intensity of sky and object Corrections can be made however to take account of any differences in the exposure times between raw frames and any differe
7. MEMSYS SUN 117 MUD 53 Quantified maximum entropy image reconstruction The MEMSYS libraries are commercial software and are licenced for UK Starlink sites only MEMSYS is not distributed on Starlink CDs Access restrictions apply at Starlink sites see below Two versions are available MEMSYS3 and MEMSYS5 The algorithms used in both are similar but the programming interfaces are quite different New applications should be written using MEMSYS5 which provides more functionality than MEMSYS3 MEMSYS3 is retained primarily for the benefit of people who want to maintain old applications They find and use maximum entropy reconstructions of images power spectra and other such additive distributions from arbitrary sets of data They were written by J Skilling and S Gull of Maximum Entropy Data Consultants Ltd and embody their Classic Maximum Entropy algorithm described in more detail in the MEMSYS3 user s manual The algorithms of both MEMSYS3 and MEMSYS5 differ greatly from their previous MEM algorithms in that they are based on a fully Bayesian analysis of the image reconstruction problem They provide the following extra functions e Calculate automatically the most probable noise level in the input data SUN 1 24 Subroutine Libraries 56 e Estimate errors in the output reconstruction e Handle negative data values e Handle limited non linearities in the data e Calculate Poisson or Gaussian statistics for input d
8. Spelling checker JED Text editor TEX to HTML converter Text editor PostScript file manipulator Starlink document to HTML converter Document preparation system Convert Ascii format files to PostScript format for printing on PostScript printers This gives a nicer looking output EMACS MUD 102 A powerful text editor with many advanced customizable features It is fairly easy to make it emulate EDT and EVE This makes it convenient for users familiar with these VAX VMS editors GHOSTSCRIPT SUN 197 PostScript interpreter This provides e An interpreter for the PostScript language e A set of C procedures that implement the graphics capabilities that appear as primitive operations in the PostScript language HTX Hypertext cross reference utilities These are used to maintain large sets of documents which use HTML the Hypertext Markup Language They can also form the basis for hypertext help systems for other software There are three components e hlink a hypertext linker This establishes hypertext links between documents which use HTML and maintains the integrity of these links when the documents are changed e findme searches for documents by keyword and displays a list of those found e showme displays a specified part of a document using a web browser SUN 1 24 Utilities 50 ISPELL Check spelling A screen oriented spell checker that shows spelling errors in the conte
9. HDSTOOLS HDSTRACE HELP see HLP HLP HTX findme hlink HTML showme ICL 787 IDI 70 IDL i6 IMG 63 INIT 78 IRAE TRAS90 34 IRCAMDR 4 IRCAMPACK 35 ISPELL 50 TUEDR 35 JCMTDR 36 JED 51 EDT JPL BS JRE 8 KAPLIBS 74 KAPPA 16 KAPRH LATEX 2 LATEX2HTML BI 81 MAG 63 MAPLE MEMSYS 55 MEMSYS3 55 MEMSYSS5 MERS 74 EMS 73 ERR 74 MSG 74 MESSGEN 3 MIDAS 7 MONGO 40 MSG 74 NAG Naos 55 NBS 63 NCAR 70 SNX 70 NDF 64 ARY 60 NDFPERL 48 NDG 64 NDPROGS 26 NEWS 48 NUTPU I EDT OBSERVE 46 ONE 5 ORAC DR 1 PAR 64 PCS PDA 57 PERIOD 27 PERL 28 PERLMODS 8 PGPLOT T GRPCKG 77 Native Starlink 71 PHOTOM 8 PINE 3 PISA T8 POLMAP 28 POLPACK PONGO 0 PRIMDAT 65 PSMERGE PSX 75 QDP IT REF SUN 1 24 Index REPACK 6 RIO 61 RV 46 SAE SAOIMAGE SGS showme SKYCAL SKYCALC SKYCALENDAR SKYCALENDAR SLALIB SM SNX SPAG SPECX SPT STAR2HTML STARADMIN STARJAVA STARMAN STARPERL NDFPERL STARTCL STARX 54 SURE Sx Bi TCL 78 TEX 2 LATEX TK 73 TRANSFORM 66 TSP 28 WECPACK 7 XANADU 9 FITSIO 1 PGPLOT II QDP TT XIMAGE 10 XRONOS 10 XSPEC p XDISPLAY 48 XIMAGE 10 XRONOS 10 XRT XSPEC P
10. In particular programs from packages written to do completely different things can process each other s data thereby avoiding unnecessary duplication of software with the attendant waste of effort both in writing the program and in maintaining it Finally it should not be forgotten that ADAM originated as a telescope and instrument control system The way that ADAM programs are written when used in these circumstances is rather different from when they are used for data analysis Use of ADAM for instrument control is not the province of this document However it is interesting to note that programs written for data acquisition tasks are rather like windows programs which have become common EXPECT Emulate a user sitting at a terminal When combined with TK it can put a GUI in front of an existing application without modifying it ICL A programmable user interface to an astronomical data reduction or data acquisition system It is one of the main user interfaces for the ADAM software environment In some ways it is similar to a high level programming language such as Fortran or Pascal but it has some important differences e It is a command language One of its main uses is to let you type commands with few restrictions on the format e Itis an interactive language It provides a complete environment for entering editing and debugging programs rather than relying on external editors linkers etc e It is a programming langu
11. all mathematical levels and can provide solutions to many types of problem e Arithmetic with integers fractions and polynomials e Power series e Differentiation and integration of functions e Systems of equations e Differential equations e Linear optimization e Tensor manipulation e Symbolic and numeric approximation e Automatic generation of Fortran code and ATEX source for mathematical expressions In addition it can generate plots to illustrate graphically any function including user defined functions You can also extend or redefine the numerous functions by writing MAPLE programs in the built in Pascal like language to create specialized functions More general information about computer algebra software is available in SGP 47 It is marketed by WATCOM Waterloo Ontario CANADA SUN 1 24 Packages 40 3 11 Graphics MONGO Interactive data plotting Not distributed PONGO Interactive data plotting Interactive data plotting MONGO MUD 54 Plot data interactively You can build up a complicated diagram including graphics text axes and so on and then create publishable quality output In general it has been superseded by PONGO PONGO SUN 137 Plot data interactively It is like MONGO but uses Starlink PGPLOTIas the plotting package It is more powerful than MONGO and is Starlink compliant which means you can use it in conjunction with and Features include e Read data from a text file
12. applications Use of NDF means that data files can be exchanged between different packages without the need to convert file formats This is very useful as having to change file formats is very annoying and takes up extra disk space NDF is layered on HDS the hierarchical data system By using HDS version 4 0 or later it becomes possible to read and write data files on different computer systems completely transparently so no explicit data conversion needs be done even when moving from one computer to another ADAM programs can generally be run either from the command language of the host or from the ICL command language ICL is a simple programming language in itself somewhat along the lines of BASIC It can be quite useful for doing simple operations but is not fast enough for any major processing Use of ICL makes it easier to build sequences of operations into ICL procedures It is generally quicker to 77 SUN 1 24 Infrastructure run ADAM programs from ICL if they are to be run several times since the programs only have to be activated once On the other hand the ability to run ADAM programs from the shell is very useful for debugging One of the most distinctive features of ADAM is the parameter system This provides a method whereby a program can interact with a user or with other programs For a single program a series of write and read statements could sometimes be used instead but for anything more complex this becomes unac
13. certain conditions NAG SUN 28 29 MUD 55 56 57 58 128 Mathematical subroutine library The NAG libraries are commercial software and are licensed to UK Starlink sites only The software is not distributed on Starlink CDs The Numerical Algorithms Group NAG library is commercial software The current versions are Mark 18 for the Numerical library and Mark 4 for the Graphics library Double precision versions of the Numerical Library are provided and where available single precision versions are also provided The Graphics Library is in double precision form The routines cover a very wide area of numerical and statistical mathematics They are extensively documented in a reference manual guide and introductory book These are available at every Starlink site and copies of the NAG newsletters are kept at RAL The standard library organises its routines into the following chapters e A02 Complex arithmetic 57 SUN 1 24 Subroutine Libraries e C02 Zeros of polynomials e C05 Roots of one or more transcendental equations e C06 Summation of series e D01 Quadrature e D02 Ordinary differential equations e D03 Partial differential equations e D04 Numerical differentiation e D05 Integral equations e E01 Interpolation e E02 Curve and surface fitting e E04 Minimizing or maximizing a function e F01 Matrix operations including inversion e F02 Eigenvalues and eigenvectors e F03 Determi
14. csp Global Section Datafile GSD access library This library provides read only access to Global Section Data files GSD files created at the James Clerk Maxwell Telescope A description of GSD itself is presented in addition to descriptions of the library routines Its main use is in SPECX to read the GSD files created by the heterodyne instruments used on the JCMT HDs Store and retrieve data flexibly The Hierarchical Data System is the basic Starlink data system and is of great importance to the Project Its most significant features are the following e It manipulates entities called data objects These can be scalars or arrays of up to seven dimensions e A data object has a tree like shape whose components comprise other objects The only restriction is that the leaves must be primitive data types The degenerate form of an HDS tree is a single scalar or array of a primitive data type The non degenerate form is called a structure which comprises two or more components SUN 1 24 Subroutine Libraries 62 The primitive data types include the usual Fortran numeric logical and character types together with signed and unsigned bytes and words You can tree walk Any branch or sub branch of a tree can be treated as a data object in its own right Data objects are dynamic in the sense that programs can add modify or delete components to or from a tree Subsets of primitive arrays can be defined and manipulated as sep
15. loaded Stretch the contrast e Change gamma 7 to give non linear contrast so that the display assigns more shades of grey to the darker or lighter end of the scale This may suit the eye better that a linear scale e Type text on an image Other features e Blink between images e Regions A description of a region of an image can be saved This can be used to flag regions as bad or to examine only the counts within a certain region This is mainly useful in conjunction with the and PROS X ray packages e Tracking The pixel coordinates and values under the mouse pointer and the region around it can be displayed and constantly updated e RAFlimage display e Hard copy STARMAN SUN 141 Stellar photometry STARMAN is not distributed on Starlink CDs and has not been ported to Linux It is optionally available at UK Starlink sites Starman s many image and table handling programs have other uses but its main applications are e Crowded field photometry e Aperture photometry e Star finding e CCD data reduction The package is a coherent whole for use in the entire process of stellar photometry from raw images to the final standard system magnitudes and their plotting as colour magnitude and colour colour diagrams Its functions are e Stellar Photometry Convert raw CCD images to calibrated ones Dust ring flat field dealer Find star positions Determine stellar profiles Crowde
16. referenced object e Create an empty reference object e Puta reference into a reference object e Annul a locator which may have been obtained via a reference Its two main uses are e To maintain a catalogue of HDS objects e To avoid duplicating a large dataset SUN 1 24 Subroutine Libraries 66 TRANSFORM Relate different coordinate systems Provides a standard flexible method for manipulating coordinate transformations and for transferring information about them between programs It can handle coordinate systems with any number of dimensions and can efficiently process large i e image sized arrays of coordinate data using a variety of numerical precisions No specific support for astronomical coordinate transformations or map projections is included at present but routines for handling these should appear in future The current system provides tools for creating a wide variety of coordinate transformations so it should be possible to construct some of the simpler astronomical transformations explicitly if required It can e Define linear and non linear graphics coordinate systems e Attach coordinate systems to datasets e g relating image pixels to sky positions e Describe distortion in images and spectra e Store and apply instrument calibration functions It uses to store information in standard data structures for interchange between applications These may be used as building blocks when constructing larg
17. statistics MAPLE Mathematical manipulation Not distributed ASURV MUD 5 6 Analyse statistically astronomical data with upper limits Observational astronomers frequently encounter the situation where they observe a particular property of a previously defined sample of objects but fail to detect them all The data then contains upper limits as well as detections preventing the use of simple and familiar statistical techniques in the analysis However a variety of other statistical methods exist to deal with these problems which are collectively called survival analysis or the analysis of lifetime data from their origin in actuarial and related fields The upper limits are called censored data points ASURV is a menu driven stand alone computer package to help astronomers use some of these methods No statistical procedure can magically recover information that was never measured at the telescope However frequently there is important information implicit in the failure to detect some objects which can be partially recovered under reasonable assumptions ASURV provides several two sample tests correlation tests and linear regressions each based on different models of where upper limits truly lie so that you can judge the importance of the different assumptions MAPLE SUN 107 SGP 47 MUD 52 137 139 144 145 Interactive symbolic algebra computation It can perform hundreds of algebraic functions for use at
18. the X library linking strategy to be changed easily without changing any of the other Starlink environment components 55 SUN 1 24 Subroutine Libraries 5 Subroutine Libraries 5 1 Astronomical amp Mathematical JPL Solar system ephemeris Maximum entropy image reconstruction Mathematics statistics and graphics PDA Public domain algorithms Positional astronomy JPL SUN 87 Provide extremely accurate position and velocity data for any of the nine planets the Moon and the solar system and Earth Moon barycentres also nutation components for any given epoch in the range of the ephemeris 1960 to 2025 For many years the Jet Propulsion Laboratory has distributed definitive solar system ephemeris tapes containing files of ephemeris data plus Fortran programs to read them The ephemerides come from direct numerical integration of the equations of motion of the large bodies in the solar system subject to fitting to a variety of observations For distribution they are expressed in terms of Chebyshev polynomials The version distributed by Starlink is the DE200 LE200 the one most consistent with the latest AU resolutions Users of the old VMS only version should note that this new version differs in some important respects Existing applications will need to be changed before they can be linked against the new library and existing executable programs are not compatible with the new format of ephemeris file
19. to the AST library CCDPACK Reduce CCD like data and mosaic frames together You can debias remove dark current pre flash flatfield register resample and normalize your data Perhaps the most important and useful feature of the package is its ability to handle large numbers of data files automatically so that repetitive reduction procedures can be handled in a straightforward and efficient way This uses a scheduling system that only requires knowledge of the frame types bias flatfield etc and important CCD geometric features Using this information it can decide how to reduce your data and may then run the necessary programs The frame types and detector characteristics can be obtained from FITS headers for certain telescopes CCDs so your job could be reduced to identifying the telescope detector used and the frames you want reducing The automated reduction system can be controlled from an X based GUI that has been specifically designed to help novice and or occasional users of CCD data although it is expected to appeal to the more experienced as well Ease of use is achieved by limiting the options to those of immediate concern by providing a selection of known detectors and by having a context sensitive help system It also aims to be complete by allowing you to define the necessary geometric characteristics of your data interactively if they cannot be obtained elsewhere An equivalent command line interface is also available
20. PAG MUD 127 Improve the structure of the source code of a poorly organised Fortran program SPAG is commercial software and is not distributed on Starlink CDs Access is available to registered Starlink users on the central service machine at RAL contact Hiten Patel hiten star rl ac uk for access SPAG stands for Spaghetti Unscrambler It re orders blocks of statements in such a way that the structure of the code is improved while remaining logically equivalent to the original program The result improves the readability and maintainability of badly written Fortran code It is marketed by Polyhedron Software SUN 1 24 Utilities 54 Software porting tools A set of tools to convert code between operating systems principally between VMS and Unix and between different flavours of Unix They e Convert file name specifications in Fortran INCLUDE statements and escape backslash characters The output file on VMS is in Stream_lf format so it can be read on Unix systems using NFS e Manage the creation and removal of soft links on Unix systems Generally these will point to Fortran INCLUDE files thereby providing a machine independent way of writing INCLUDE statements STARX Link X libraries A Starlink environment package that provides a system independent method of linking with X libraries This relieves other libraries and applications from having to worry about the various complications involved It allows
21. PSFs Enhance detail using histogram equalisation and Laplacian convolution enhance edges via a shadow effect threshold Calculate polarimetry images There are also many applications for data visualisation A graphics database AGI to pass information about pictures between tasks tools to create label select pictures and obtain world and data co ordinate information from them Image and greyscale plots with a selection of scaling modes and many options such as axes Create select save and manipulate colour tables and palettes for axes annotation coloured markers and borders Snapshot an image display to hardcopy Blink and control visibility of image display planes Line graphics contouring including overlay columnar and hidden line plots of images histogram line plots of 1 d arrays and multiple line plot of images pie sections and slices through an image vector plot of image all of which offer some control of the appearance of plots KAPPA handles bad pixels and processes quality variance and other information stored within NDFs In order to achieve generality it does not process non standard extensions however it does not lose non standard ancillary data since it copies extensions to any NDFs that it creates Although oriented towards image processing many commands will work on NDFs of arbitrary dimen sion and others operate on both spectra and images Many applications handle all non complex data type
22. SUN 1 24 Starlink Project Starlink User Note 1 24 ed S E Rankin 5 August 2003 STARLINK Software Collection SUN 1 24 Abstract ii Abstract The Starlink Software Collection is a set of software which is managed and distributed by the Starlink Project Some of the software was written by members of the Project but some of it comes from outside the Project This note describes the functions of the individual items in the Collection and provides an overview of the software so that readers can identify the items they need The software is classified into four main divisions e Packages are large collections of programs for people who want to analyse convert and display data They are subdivided into eleven classes to help you find what you want e Utilities are small programs devoted to a specific purpose For example they help you prepare for observations write documents and write programs e Subroutine Libraries are for programmers writing astronomical software They provide facilities such as astronomical calculations data management and graphics e Infrastructure are items which are mainly of interest to people writing programs within the Starlink Software Environment They are included for completeness Each item is described in sufficient detail for you to decide whether or not to investigate it further If you want to find out more about an item follow the document references given opposite the item
23. Starlink sites ask you Site Manager The SX enhancements have a number of purposes They e Fill a few minor omissions in the functionality of basic DX e Provide easy to use functions to accomplish common tasks in a single step e Allow standard Starlink NDF data structures and data in other common astronomical formats to be imported into DX SUN 1 24 Packages 22 3 4 Spectroscopy IFU datacube analysis Spectrum analysis and plotting Echelle data reduction General data reduction n dimensional data analysis IFS datacube manipulation and visualisation DATACUBE is a new package which provides a set of tools for manipulating and visualising IFS Integral Field Spectrograph datacubes Also known as an IFU Integral Field Unit the IFS is relatively new in astronomical instrumentation and is therefore rapidly developing The DATACUBE package has been implemented mainly as a series of scripts which drive existing Starlink packages to manipulate IFU data This approach allows changes to be made to tasks quickly as data analysis requirements evolve There are also a small number of IFU specific tasks implemented in Fortran IFU data analysis is discussed in detail in the cookbook The IFU Data Product Cookbook SC 16 23 SUN 1 24 Packages DIPSO Analyse and visualise spectroscopic data A powerful and versatile package specifically tailored to the requirements of modern astronomical research It
24. a number of ICL procedures are provided to perform some of the more commonly required operations such as extracting background subtracted lightcurves XRT ROSAT XRT data access The XRT is a package provides access to ROSAT XRT data stored in FITS files for analysis by other Starlink Packages The tools are based on the ASTERIX ROSAT XRT toolset from version 2 3 b1 but do not include the ASTERIX analysis tools At present the documentation and Help facilities are copies of the ASTERIX files so that some of the tools used in examples may be no longer available SUN 1 24 Packages 38 3 9 Format Conversion CONVERT Data format conversion CONVERT SUN 55 Convert the standard Starlink n d data format NDFijto and from other formats A major advantage of this package is that it deals sensibly as far as possible with header information which can be lost during translation by less robust software Currently the Unix version can handle these formats e Text Ascii e FIGARO version 2 DST file e GASP image e GIF image e RAF image e IRCAMPACK data file e FITS including some IUE final archive products and ISO datasets e PBMPLUS PGM output only e TIFF image output only e Sequential unformatted The following formats can only be handled by the VMS version e Starlink Interim BDF file e DIPSO file 39 SUN 1 24 Packages 3 10 Mathematics amp Statistics ASURV Astronomical survival
25. a structures built using Details of these structures and the design philosophy behind them can be found in SGP 38 although familiarity with that document is not necessarily required in order to use the routines ARY is an essential component of the system which contains routines for accessing Starlink NDF structures The main reason for using it is to access ARRAY structures stored in NDF extensions At present it only supports the primitive and simple forms of the ARRAY data structure It can e Access existing arrays e Create and delete arrays e Create and control identifiers e Create placeholders e Copy arrays e Enquire and set array attributes e Use message system routines AST A library for handling World Coordinate Systems in astronomy The AST library may be used for attaching world coordinate systems to astronomical data for retrieving and interpreting that information and for generating graphical output based on it The should be of interest to anyone writing astronomical applications which need to manipulate coordinate system data especially celestial coordinate systems AST is portable and environment independent Create read and write astronomical catalogues and similar tabular datasets It supports the following formats e FITS tables Ascii and binary e STL Small Text List simple lists in text files e CHI HDS e SCAR ADC on VAX VMS only 61 SUN 1 24 Subroutine Librari
26. age suitable for relatively simple and straightforward programs SUN 1 24 Infrastructure 78 INIT A grouping of the Starlink login resource files and other associated bits and pieces The cshre and login files are now handled like standard packages and are edited by the install procedure to contain the correct root path for the USSC set This allows easy installation on systems where the directory star does not exist Starlink application environment INIT gathers together the global include and error files needed by the infrastructure and applications It is purely an administrative grouping STARTCL Extend TCL and TK A public domain utility called is in wide use as a command language and user interface builder STARTCL comprises three extensions to TCL and the TK Toolkit that enable TCL TK applications to cooperate with Starlink applications These are e A TK widget that displays Starlink graphics by emulating the gwm graphics window server and a gwm canvas item e An interface to the ADAM message system e An interface to the ADAM notice board system TCL MUD 164 Control and extend applications using a scripting language TCL stands for Tool Command Language TK MUD 164 Build GUIs An X window toolkit for use with and EXPECT It can build Motif like user interfaces using TCL scripts instead of C code 79 SUN 1 24 Acknowledgements The majority of the text for this document was plundered from existin
27. alised feature of GKS is needed It can e Control workstations and zones e Plot lines text and markers e Control character attributes e Accept graphical input e Do GKS inquires SNX SUN 90 Starlink extensions toINCAR They provide more convenient access to certain features of NCAR without sacrificing flexibility Begin ners may be daunted by the mass of features offered by NCAR and unless they take the extreme step of reading the manual they may give up before realising what the package can do for them SUN 1 24 Subroutine Libraries 72 The AUTOGRAPH part of NCAR used in conjunction with SNX and offers an alternative to Starlink PGPLOT for graphing one variable against another SNX enhances the power of AUTOGRAPH and makes it easier for the beginner It can Open AUTOGRAPH SGS GKS with a single call Plot a finished graph with annotation by means of a single call Include special characters in graph labels Greek subscripts mathematical symbols etc e Plot character strings anywhere on the graph Manage the graphics device display surface via the SGS system of zones while using AUTOGRAPH to do the plotting Align the AUTOGRAPH and SGS coordinate systems e Save and restore the state of AUTOGRAPH so that multiple active plots can be managed e Perform cursor input 73 SUN 1 24 Subroutine Libraries 5 4 Other Character handling Mixed C and Fortran programming Error message ser
28. arate data objects and arrays can be mapped as vectors More powerful data systems have been built on top of HDS in order to make specific types of data object easier to handle These include for handling arrays and for handling objects in the standard Starlink data format 63 SUN 1 24 Subroutine Libraries IMG Easy access to astronomical image data and associated headers It is of most interest to astronomers who write their own software and require uncomplicated access to their image data In this context an image may be an ordinary 2 d image but could also be a spectrum 1 d or data cube 3 d Because of Starlink s automatic format conversion facilities this library also gives programmers straight forward access to a wide range of astronomical data formats including FITS and IRAF files as well as Starlink NDF data T Handle magnetic tapes Astronomical data on magnetic tapes can be in many formats The MAG library allows you to write programs to read this data on any type of computer and tape drive It doesn t interpret the data format it deals in tape blocks and knows nothing about FITS VMS BACKUP tar etc MAG lets you write portable software This is very useful since different computers can differ greatly in their facilities for handling magnetic tapes For example on VMS it is quite common to treat magnetic tapes as normal Fortran sequential files that can be opened read written and close
29. are used to search data for periodicities data points do not have to be equally spaced You don t need in depth knowledge of the methods employed in order to use them They can be treated as black boxes These include e Chi squared analysis of a folded sine fit versus frequency e Cleaned and discrete Fourier power spectra e Phase dispersion minimization PDM Stellingwerf e Lomb Scargle normalized periodograms e String length Dworetsky versus frequency estimates e Periods from the periodogram e Significance estimates Significance estimates for periods derived by most methods are notoriously unreliable In PERIOD the Fisher randomisation method one of the best is employed SUN 1 24 Packages 28 POLMAP Analyse linear spectropolarimetry data A linear polarization spectrum is a set of Stokes vectors I Q U Hence linear spectropolarimetric data is 4 d 6 d if the variance arrays of the Stokes parameters are included and cannot be manipulated using standard spectral analysis packages such as DIPSO Its user interface is similar to DIPSO s but doesn t provide its wealth of spectral analysis routines It is designed specifically for the spectropolarimetrist The manual includes a simple step by step guide to the program and some example data analysis recipes It is complimentary to TSP like FIGARO is to DIPSO TSP runs under the Starlink software environment and can handle time series and polarimetric data
30. ata noise MEMSYS deals with data sets and images A data set holds information corresponding to the available experimental data and an image holds information corresponding to the true image from which the data was generated It handles problems where the relationship between data and image can described as follows Mk Fy Raj fj n 1 j 1 where F is the kth data value M is the number of data values fi is the jth image value Ry is the response of sample F to pixel fj and n is the noise on sample k This is a linear relationship between data and image It can also cope with non linear data so long as the data Dx can be expressed as follows Dy F 2 where is some known function with known derivative and F is linearly dependent on the data The image and data set are described as 1 d arrays purely for ease of access within the package In fact they could be of any dimensionality The calling program needs to set up the correspondence between n d coordinates and the 1 d coordinate used above For instance for a 2 d image with coordinates pix lin the relationship may be j pix NPIX x lin 1 3 where NPIX is the number of pixels per line of the image A common use is to deconvolve a 2 d image given a Point Spread Function PSF In this case the data is linear and the matrix Ry embodies the PSF Before using it you must sign a form available from your Site Manager accepting
31. bber sheet the data into novel configurations Normalisation and combination often called mosaicing is provided in a single comprehensive application which is designed to deal with very large datasets This uses robust methods to determine scale and or zero point corrections The CCDPACK package my be run from the IRAF CL DAOPHOT SUN 42 MUD 9 10 Stellar photometry of crowded fields It does the following tasks e Find objects e Aperture photometry e Obtain the point spread function e Profile fitting photometry Profile fitting in crowded regions is performed iteratively which improves the accuracy of the photometry It does not directly use an image display which aids portability although three additional routines allow results to be displayed on an image device It uses image data in NDF format which means it is interoperable with other Starlink packages Photometry of galaxies and other extended objects It can e Detect identify flatfielding faults e Remove cosmic ray events e Median filter images on a defined scale e Determine whole image statistics including median and modal count kurtosis and skewness 15 SUN 1 24 Packages e Determine the local background value on a number of different parts of an image e Perform galaxy profiling using intensity analysis e Perform galaxy profiling using contour analysis e Perform 2 d Gaussian profiling GAUFIT e Generate galaxy pie slice cross sections
32. c astrometry Autoastrometry for Mosaics CHART Finding chart and stellar data system Celestial coordinate converter Echelle observation planning Find coordinates of named objects HDS file manipulation NEW HDS object lister NAOMI guide star tool Star observability checker Radial components of observer s velocity Interactive almanac and calculator ASTROM Basic astrometry simple plate reduction It is designed to allow the non specialist to get good results with a minimum of trouble and esoteric knowledge You supply a text file containing information about the exposure and the positions of reference and unknown stars it performs the various coordinate transformation and fitting operations required displays a synopsis report on your terminal and prepares a detailed report for printing AUTOASTROM We describe the autoastrom package which provides an interface to the ASTROM application This creates a semi automatic route to doing astrometry on CCD images THIS IS BETA SOFTWARE Some features work only partially or unreliably It does not have all the functionality of a production release The interface may well change Starlink s ASTROM application provides powerful astrometry facilities for analysing astronomical images it is however rather cumbersome to use As described in SUN 5 ASTROM can e obtain the plate centre and plate scale of a CCD image by comparing plate po
33. can access a large number of spectra simultaneously This lets you perform the same operations repeat edly on successive spectra either manually or using scripts ensuring uniformity in the data especially important for time series spectroscopy It can plot spectroscopic data rapidly and conveniently and combines analysis and high quality graphical output in a simple command line driven environment It began as a simple plotting package incorporating some basic astronomical applications Indeed if you just want to read in some data plot them and measure some equivalent widths or fluxes you can do this easily To make more complicated things possible a number of extra functions and parameters are provided A macro facility allows convenient execution of regularly used sequences of commands and a simple Fortran interface permits personal software to be integrated with the program User programs can be added to the system and defined as new commands The following operations are available Arithmetic e Fit emission lines e Measure equivalent widths e Measure fluxes Fourier analysis Interstellar line analysis e Model atmospheres e Model nebular continua e Fit polynomials e Simple statistics ECHOMOP Reduce chelle spectra data frames Options range from full scale automated reduction to step by step order by order manually assisted pro cessing It was written originally to reduce data from the University C
34. ceptable It is particularly difficult to maintain a standard style and ad hoc fixes to problems abound Use of the parameter system provides a consistent user interface a means of storing the value of a parameter between invocations of a program and the facility to pass the values of parameters from one program to another From the perspective of a programmer ADAM provides many subroutine libraries that perform common functions They provide such diverse functions as character handling access to hierarchical relational and simple data graphics the parameter system error and message reporting numerical calculations etc Some of these libraries are provided purely for use in ADAM programs whereas others such as the NAG library and graphics libraries have a much wider use Although any subroutine library can be used in an ADAM program those that have been written specifically with this in mind are much easier to use ADAM libraries conform to the Starlink standard on the use of inherited status which greatly reduces the amount of code needed to test for error conditions They also report any error conditions via the error message service This lets the programmer get at the error messages as well the error code to see if the error can be handled internally or whether to send the error report on to the user By using the facilities provided in a consistent manner simple programs can be easily linked together to perform complex operations
35. ckages via FITS files but in the case of IRAF this data interchange capability will be extended by enabling Starlink applications to read and write IRAF data files This will mean that a user can run IRAF in one window on their screen and a Starlink package e g CCDPACK in another processing the same datasets with each A further capability currently being investigated would be to run Starlink applications from the IRAF command line just as if they were native IRAF applications MIDAS Reduce and analyse optical astronomy data within a basic image processing environment The Munich Image Data Analysis System MIDAS was developed by the Image Processing Group of the European Southern Observatory ESO It consists of a monitor which controls the execution of individual tasks and a large set of image processing applications Since the results of reducing astronomical images are usually numbers not other images a comprehensive and flexible table system forms an essential part of the system New applications can be added easily even by non professional programmers Its main features are SUN 1 24 Packages 8 Support for computers with VMS and Unix operating systems Device independent interfaces to peripherals by using special libraries e g AGL for graphics ID for image display and TW for terminals Support for display and hard copy standards like X11 and PostScript e Easy and flexible integration of user software written in
36. coords will only work on computers with a suitable Internet connection Also the name given must be recognised by SIMBAD though the latter s dictionary of names is very extensive 45 SUN 1 24 Utilities HDSTOOLS HDS file editing and manipulating tools HDSTOOLS is a suite of tools for editing and manipulating HDS files They are updated versions of the tools once available in the ASTERIX package The following tools are available e HCOPY Copy HDS data objects e HCREATE Create an HDS data object of specified type and dimensions e HDELETE Delete an HDS object e HDIR Produce a simple summary of an HDS object HDISPLAY Display the contents of a primitive HDS object HFILL Fill an HDS data object with a specified value e HGET Return information about an object e HHELP Obtain HELP on the HDSTOOLS package e HMODIPY Modify the value of an HDS object e HREAD Read a file into an HDS object e HRENAME Rename an HDS data object e HRESET Change state of a primitive HDS object to undefined e HRESHAPE Reshape an HDS object e HRETYPE Change the type of an HDS structure object e HTAB Display one or more vector objects in table form e HWRITE Write an HDS object into formatted or unformatted file HDSTRACE SUN 102 List the contents of an HDS data structure The Hierarchical Data System HDS is one of the most popular features of the Starlink environment as it enables associated data item
37. ctical almost all the routines have been written to satisfy real needs encountered during the development of real life applications Environment independent the package is completely free of pauses stops I O etc Self contained it calls no other libraries 59 5 2 Data Access amp Management Region description language World Coordinate System data handling ARRAY data structure access Catalogue access Disk FITS I O C and Fortran Fortran I O Disk FITS I O Manipulation of groups of objects Read Global Section Datafiles Hierarchical data system Simple image data access Magnetic tape handling Noticeboard system NDE NDF data structure access Access to groups of NDFs Parameter system Primitive numerical data processing HDS object referencing Coordinate transformation SUN 1 24 Subroutine Libraries SUN 1 24 Subroutine Libraries 60 ARD Describe regions of a data array The Ascii Region Definition system provides a textual language for describing regions within a data array together with software for converting a textual description into a pixel mask The textual language is based on a set of keywords identifying simple shapes boxes circles lines etc These can be combined using Boolean operators AND OR NOT etc to create more complex shapes Data arrays can be multi dimensional Access Starlink ARRAY dat
38. d FIGARO or NDF formats is recommended as this allows other Starlink packages to process the data IRCAMPACK can also access the main data arrays although other parts of the data structure will be inaccessible REPACK SUN 208 Handle ROSAT Wide Field Camera survey data REPACK is not distributed on Starlink CDs though it may remain as a legacy package at UK Starlink sites There is no linux Port With the demise of the ROSAT satellite there is no support for REPACK During the period from July 1990 to January 1991 the ROSAT Wide Field Camera WFC performed the first all sky survey at extreme ultraviolet EUV wavelengths The whole sky or 96 of it was imaged in two passbands S1 and S2 covering the ranges 60 140A and 110 200A respectively An initial bright source catalogue BSC of 383 sources was produced by Pounds et al A new list the 2RE Catalogue of 37 SUN 1 24 Packages 479 sources has recently been published The survey data images and raw photon event files are now in the public domain REPACK fully exploits this data The data is available through the Leicester Data Archive Service LEDAS Images were sorted from the event files and screened for high background and moon in WFC field of view and named after the ecliptic latitude and longitude of the region of sky that they covered They are 2 7 x 2 7 in extent with a resolution of 1 x 1 arcmin per pixel The photon event files are overlai
39. d field and also simple stellar photometry measurers SUN 1 24 Packages 20 Average photometry estimates from different images Plot colour magnitude and colour colour diagrams Add fake stars to an image Automatic aperture photometry for all bright well isolated stars e Image Handling Image display Interactive image work Display zoom pan pixel value slice solid body plots colour crowded field stellar photometry output etc Measurement interactive aperture photome try interactive position file making Manipulation maths rotation weeding etc GUI like interaction Extensive general programs Maths joining cutting reading etc e Table Handling Spreadsheet Calculator Input Output Listing Graphical plot Star chart Joining Extensive general programs sort weed statistics matching position transforming etc 21 SUN 1 24 Packages sx Enhancements to DX DX Data Explorer is a scientific data visualisation and analysis package marketed by IBM It can visualise and display many sorts of astronomical data It employs a data flow driven client server execution model and provides a comprehensive range of data manipulation visualisation and display functions Visualisations can be generated using a visual programming editor or a text based scripting language Starlink recommends DX for displaying 3 d scalar and vector data However it is not available at all
40. d on a similar ecliptic grid system Some 13 000 image pairs and 13 000 event files were produced by this scheme covering almost the whole sky Images can be retrieved in various formats HDS FITS and GIF REPACK only operates on HDS format images Event files available just in FITS format can be sorted to ASTERIX HDS datasets such as images and light curves SCUBA data re reduction facility SURF is a set of programs for reducing demodulated Submillimetre Common User Bolometer Array aka SCUBA data obtained from the James Clerk Maxwell Telescope The facilities provided by SURF include e nod compensation e flatfielding e extinction correction e single beam restoration e sky noise removal e despiking e array overlay WFCPACK Produce ASTERIX HDS datasets from Wide Field Camera data collected during the pointed phase of the ROSAT mission WFCPACK is not distributed on Starlink CDs though it may remain as a legacy package at UK Starlink sites There is no linux Port With the demise of the ROSAT satellite there is no support for WECPACK A sort program generates datasets such as time series and images from pre processed event data supplied as part of the ROSAT WFC Observation Datasets RWODs An exposure program corrects them allowing for instrument characteristics In addition a simple database manager allows an index of RWODs to be maintained and searched The programs make use of the ADAMJ ICLenvironment and
41. d using the Fortran statements OPEN READ WRITE and CLOSE On Suns this is not the case and special routines are provided for processing magnetic tapes These differences are hidden from the programmer by the MAG package It can e Allocate a tape drive and mount a tape e Open and close tape devices e Read and write data contained in tape blocks e Move tapes relatively skip files blocks and rewind e Position tapes absolutely Not all operations are available on all types of tape deck Also the status values returned by different machines can differ NBs Share data between processes NBS stands for Noticeboard System A given process may own many noticeboards and may access ones owned by others Normally the only process that writes to a noticeboard is its owner but other processes subvert this rule if necessary Noticeboards are identified by name and each can contain a hierarchy of items Each item has a name type structure primitive attribute and if primitive a maximum number of dimensions maximum number of bytes current shape and value The type and shape are not used by the routines but their values can be put and got and they can be used when implementing higher level routines on top of the noticeboard routines Noticeboards are self defining a process can find and access data from a noticeboard without knowing anything about what it contains SUN 1 24 Subroutine Libraries 64 NDF Access
42. data stored in NDF format The Extensible n Dimensional Data Format is the standard Starlink format for n d arrays of numbers such as spectra images etc and it forms the basis of most Starlink spectral and image processing applications A stand alone version is available for programs which do not use the Starlink software environment The main reason for using NDF is to simplify data exchange between applications In principle it should enable you to process the same data with any Starlink package In practice previous attempts to define a standard data format for this purpose have met with two serious obstacles Firstly different software authors have interpreted the meaning of data items differently so that although several packages might be capable of reading the same data files they actually perform incompatible operations on the data Secondly many authors have found a pre defined data format to be too restrictive and have ignored it The NDF data structure has therefore had to satisfy two apparently contradictory requirements e Its interpretation should be closely defined so different and usually geographically separated programmers can process it in consistent and mutually compatible ways e It should be adaptable so it can hold data associated with many software systems whose detailed requirements vary considerably This problem has been solved by introducing the concept of extensibility and by dividing the data struc
43. er HDS datasets and also when designing extensions to the standard Starlink data structure 67 SUN 1 24 Subroutine Libraries 5 3 Graphics Applications graphics interface Graphical kernel system Graphical workstation name service ADAM graphics GWM X graphics window manager Image display interface High level graphics High level graphics High level graphics SGS Simple graphics system Starlink extensions to NCAR Graphics database Used in Starlink programs to store between applications information about the various plots on a graphics device It records their position and extent These can be recalled later either to overlay plots or to recreate the picture Obvious uses are to align pictures or to obtain cursor coordinates from an existing picture But it has other uses e g to slice up the screen into areas for subsequent plotting using more complicated patterns than just a regular grid the areas can be different sizes or overlap GKS MUD 27 SSNI59 Low level graphics library The Graphical Kernel System is an international standard The current version is 7 4 and this what you should use It has two major advantages over other graphics packages e It is an international standard and thus portable e No other package provides the ability to write such device independent graphics programs Only with GKS can you write a program that will run and produce good p
44. eractive data language Not distributed IRAF Image reduction and analysis facility Munich image data analysis Not distributed GSFC software system Starlink Java Infrastructure and Applications Set AIPS SUN 207 MUD 101 Calibrate and edit radio interferometric data construct images using Fourier synthesis techniques and display and analyse these images The Astronomical Image Processing System AIPS is in widespread use by radioastronomers It has a richer set of general image processing functions than any other astronomical software package It can e Deconvolve a point spread function from an image e Transform one image into the coordinate system of another Fourier transform an image into the complementary Fourier domain allowing you to edit the transformed image and transform it back again useful for removing stripes from IRAS images e Enhance various features in an image using gradient filters or even the Sobel edge enhancement filter e Display successive planes of a data cube as a continuous movie Display a spectral line data set using hue to denote velocity and intensity to denote integral brightness IDL MUD 29 30 31 161 Explore and manipulate data using a comprehensive set of tools The Interactive Data Language IDL is proprietary package written by Dave Stern of Research Systems Inc Denver It is only available on some Starlink nodes At its simplest level it can be used as a very pow
45. eral nature and usefulness but which are not appropriate to be included in any of the more focussed Starlink libraries The routines are written in C but are callable direct from Fortran Parameter and communication system Application programs often need to obtain parameter values from a variety of sources and to communicate with other programs The Parameter and Communication Subsystems PCS are a set of closely related subroutine libraries which provide these facilities for many Starlink applications and associated user interfaces These libraries will not generally be called directly by application programs but form a basic part of ADAM the Starlink Software Environment Use the POSIX and X OPEN libraries Lets you use operating system facilities in a machine independent way SUN 1 24 Infrastructure 76 6 Infrastructure ADAM Starlink software environment Interactive program control Command language INIT Starlink initialisation files SAE Starlink applications environment base files Starlink additions to TCL Embeddable tool command language X window toolkit for TCL ADAM SGA 6l SUN01 T13 115134 14 SGP A5 SSNV6d Starlink s main software environment It has many aspects which taken together provide users with a coordinated environment for analysing data and writing programs ADAM software also controls many telescopes and instruments at observato ries In the minds of us
46. erful arithmetic and graphics utility for processing data arrays It provides e A programming language e Easy graphics and image display e Mathematical and transcendental functions e Array and string manipulation 7 SUN 1 24 Packages e Input output e Type conversion e Other complex operations It can be used with minimal effort for many applications or developed into more complex procedures as required IRAF SUN 179 MUD 104 105 154 156 157 Reduce and analyse data general purpose The Image Reduction and Analysis Facility RAF was developed by the National Optical Astronomical Observatory Kitt Peak and has been adopted by the Space Telescope Science Institute in Baltimore as the principal data analysis environment for Hubble Space Telescope HST data This data can also be reduced by KAPPA and FIGARO It contains general image processing and graphics applications plus programs for reducing and analysing optical astronomical data It is as portable and device independent as possible for example it includes its own programming language Although it runs on a variety of computers in practice it usually runs best on one particular type Suns at present It is a very large system which is supported by extensive documentation Every Starlink node should have a copy of the User Handbook IRAF is one of several major software environments which are available to Starlink users and upon which entire data analysi
47. ers doing data analysis ADAM is usually identified with its application programs such as KAPPA and CCDPACK However it is really just the kernel of the system in other words the subroutine libraries Many of the libraries associated with ADAM are also available as stand alone libraries thereby making it easier to take code to non Starlink computers Some of the libraries used in ADAM programs are Starlink libraries that predate ADAM while others are commercial packages In fact it is impossible to have a perfect definition of what is or is not an ADAM program The best one seems to be an ADAM program is one that uses the ADAM parameter system to interact with the user The fact that different groups of users have different ideas of what constitutes an ADAM program is not a failing of ADAM it demonstrates the different ways in which it can be used As mentioned above ADAM applications are really distinct from the ADAM kernel However without application programs ADAM would only be half a system Most of the packages described in this note are ADAM programs There are also software tools to aid in writing ADAM programs and data analysis tools to browse data files One of ADAM s most important features is that it provides a standard method of data storage called NDF extensible n d data format NDF files have standard components that all programs recognise while also allowing for any extensions that may become necessary for particular
48. es CFITSIO SUN 227 MUD 166 167 Access FITS format files on disk This new library provides both a C implementation of a FITS i o library and a Fortran wrapper for it Thus one can use it from C or Fortran as required The CFITSIO library is written and actively maintained by William Pence of HEASARC High Energy Astrophysics Science Archive Research Center at the Goddard Space Flight Center USA It is fully compliant with the FITS Year 2000 directive This is the recommended library for access to FITS files Access sequential and direct access data files in a machine independent way It consists of stand alone FIO and RIO routines which can be used independently of the Starlink software environment plus routines to interface to the Starlink parameter system FITSIO SUN 136 MUD 16 162 Access FITS format files on disk This is a Fortran only library for access to FITS files It is no longer being developed and is not compliant with the FITS Year 2000 directive Users requiring a library for FITS access are recommended to use the CFITSIO library Handle groups of objects which can be described by character strings These objects can be things like file names astronomical objects numerical values etc It can store and retrieve such strings within groups and pass groups of strings between applications by means of a text file It can also create groups in which each element is a modified version of an element in another group
49. et describes the package and star starjava javadocs index html describes the Starlink STARJAVA classes API There are miscellaneous documents in star starjava docs for individula package information and third party application documentation The STARJAVA package contains the following applications and classes Note SPLAT TREEVIEW JNIAST and JNIHDS have been moved to the STARJAVA package instead of being individual packages APPLICATIONS UTILITIES FROG Display and analysis of time series data SOG Son of GAIA SPLAT Spectral Analysis Tool TABLECOPY Copy tables from one format to another TOPCAT Tool for OPerations on Catalogues and Tables TREEVIEW Hierarchical data viewer CLASS LIBRARIES ARRAY N dimensional array manipulation and I O 9 SUN 1 24 Packages ASTGUI AST specific UI components AXIS Third generation Apache SOAP COCO Java UI for Coco DOM4 Third party DOM access library org dom4j FITS STARJAVA specific FITS access HDS Non native HDS utility classes HDX A flexible extensible data model for astronomical images tables and other metadata JAIUTIL Utility classes for JAI JETTY HTTP Server and Servlet Container JNIAST Java Native interface to AST JNIHDS Java Native Interface to HDS JSKY Java Components for Astronomy JUNIT Third party unit testing framework junit NDX N dimensional astronomical object manipulation and I O PAL Posit
50. files for input into other packages 33 SUN 1 24 Packages 3 8 Specific Instruments CGS4 UKIRT data reduction JCMT flux density calibration IRAS data reduction IRCAM UKIRT data reduction IRCAM UKIRT data reduction TUEDR IUE data reduction JCMTDR JCMT UKT14 data reduction ROSAT WFC data reduction SURF SCUBA data reduction ROSAT WFC data reduction XRT data tools CGS4DR Reduce CGS4 data Cgs4dr is not available on Linux The fourth generation cooled grating spectrometer CGS4 operates on UKIRT in the 1 5 um region at resolutions in the range A AA 300 20000 To reduce background noise it is maintained on the telescope in vacuum at cryogenic temperatures It achieved first light at UKIRT on 4 February 1991 On 22 April 1995 a new InSb 256 x 256 array was commissioned The new array is much more sensitive than previous detectors and on a good night you can acquire and reduce 100 Mb of high quality data CGS4DR was designed and tested within the FIGARO and ADAMJenvironments The output data is readable by standard FIGARO applications although not all may handle the quality and error arrays correctly It can reduce spectrographic data automatically No system however will do everything you want so some post processing may be needed The aim is to produce publishable quality spectra at the telescope via an automated reduction paradigm It can e Allow a wide va
51. for various reasons including the lack of a Linux port These packages are mainly older packages which are not used much and which have little or no support available These packages have amended descriptions to indicate their availability 5 SUN 1 24 Packages 3 Packages Starlink aims to provide maintainable portable and extensible applications packages that work in harmony by sharing a common infrastructure toolkit standards conventions and above all a standard data format Individual packages are no longer required to perform all functions so they are easier to change and are more adaptable to outside developments New functions and user interfaces can be added as required A recent example of this flexibility is the introduction of the ability to access foreign data formats from all Starlink packages because they use a common infrastructure library Applications are unified by sharing the same basic data structure the NDF extensible n dimensional data format This contains an n dimensional data array that can store most astronomical data such as spectra images and spectral line data cubes The NDF may also contain information like a title axis labels and units error and quality arrays There are also places in the NDF called extensions to store any ancillary data associated with the data array even other NDFs SUN 1 24 Packages 6 3 1 General Purpose AIPS Image processing Not distributed IDL Int
52. g Starlink documents by Mike Lawden who compiled and edited editions up to 1997 The current form of this document was developed by Martin Bly who was editor from 1997 to 2002 Most of the raw material came from the introductory sections of appropriate Starlink User Notes but material was also grabbed from other sources such as Starlink Bulletin articles and Starlink Panel papers where these provide extra insight into the significance and functions of a software item As this note covers all Starlink s software I acknowledge and thank all the authors of Starlink documents for providing the source material Thanks particularly to Mike Lawden for his work on pervious editions SUN 1 24 Index Index A2PS 49 ADAM 76 AGI 67 AIPS 6 ARD 60 ARY 60 AST 60 ASTERIX BI ASTROM 2 ASURV B9 ATOOLS 13 AUTOASTROM 22 CAT 60 CATPAC B0 CCDPACK 13 CFITSIO 61 CGS4DR 33 CHART CHR 3 CNF Coco 43 CONVERT CURSA BO DAOPHOT 4 DATACUBE 22 DIPSO 23 DOCFIND 47 DX ECHOMOP 23 ECHWIND 44 EDT 49 51 EMACS 49 EDT EVE EMAIL 7 EMS 73 ERR 74 ESP 14 EVE 49 EXPECT 77 EXTRACTOR 15 FIGARO 24 FINDCOORDS iJ findme FIO 61 FIO 61 RIO 61 80 FITSIO 161 FLUXES 34 FORUM 47 FTNCHEK 53 GAIA 5 GCC B3 GENERIC GKS 67 GNS 68 GRAPHPAR 68 GRP 6T GRPCKG 71 GSD 61 GWM 68 HDS
53. greater extent than can be done with GKS and its offspring Thus it does not supersede GKS but offers features not available in GKS It is not as good as GKS for producing line plots or character annotation it does have routines to draw lines and plot text but these are primitive and offer you little control over how the result will appear in terms of character size style of line width etc Its major strength is its ability to perform many types of interaction using the mouse Like GKS it can display an image move the cursor and rotate the look up table However it can also scroll and zoom blink the memories and read back a representation of the whole display which can then be used to obtain hardcopy It allows these functions to be programmed in a device independent way so a program can use any device for which IDI has been implemented It is not possible at present to mix GKS and IDI calls on the same display because the two packages use completely different display models However it is possible to run the packages one after the other For example IDI could follow GKS and the display could be opened without resetting it However this is an undesirable approach since the results could be unpredictable A better solution is to use AGI to mediate between them NCAR MUD 59 High level graphics utilities This extensive suite was obtained from the National Center for Atmospheric Research in Boulder Colorado An associated sof
54. h level graphics packages such as and Starlink PGPLOT call GNS to do the required name translation when a workstation is opened so unless you are writing programs that open GKS workstations directly or need to make specialised device inquiries you will not need to call GNS routines yourself It can e Translate workstation names to their GKS equivalents e Generate a list of the names and types of available graphics devices e Answer a variety of enquiries about the properties of a particular graphics device for example its category pen plotter image display etc or its VMS device name It is used internally inIDIjand but this isn t normally apparent to the programmer GRAPHPAR SUN 113 Access the graphics libraries and Starlink PGPLOT from Starlink programs These are the components of GKS SGS and Starlink Pgplot that provide the interface to the respective libraries from ADAM programs own Create graphics windows on an X display that do not disappear when a program terminates X was designed to support GUIs and it has two properties that make an X window fundamentally different from a traditional graphics device Firstly windows belong to application programs and are deleted when the application exits unlike the picture on an image display which remains there until replaced by something else Secondly application programs are expected respond to events occurring in their windows things like key presses mou
55. highly interactive environment for placing rotating and resizing apertures Locate and parameterize objects in a 2 d image The Position Intensity and Shape Analysis package PISA is applicable in most areas of astronomy where direct imaging is required It is particularly intended for faint object detection and can do this automatically based on software used with the APM automatic plate measuring machine Its core is a routine which performs image analysis on a 2 d data frame It searches for objects having a minimum number of connected pixels above a given threshold and extracts the image parameters position intensity shape for each object The parameters can be determined using thresholding techniques or an analytical stellar profile can be used to fit the objects In crowded regions it can deblend overlapping sources SAOIMAGE SUN 166 MUD 140 Display astronomical images You can manipulate images in a number of ways see the changes applied and when you are happy with the result print it on a Postscript printer It uses X window hardware It can e Scale between limits e Magnify zoom pan 19 SUN 1 24 Packages Do histogram equalisation e Scale Log and square root e Use false colour with built in or user specified colour tables Clicking on a colour bar pops up a graphical representation of the colour table s RGB values These can be adjusted interactively or a previously saved colour table can be
56. ictures on all devices supported by the implementation including devices not supported at the time the program was written Nonetheless programs can still fully exploit all the facilities offered by the hardware In addition the Starlink implementation has several advantages of its own e It is likely to be well supported SUN 1 24 Subroutine Libraries 68 e It is used on several thousand computers of many different types throughout the UK academic community This means that the software has received a large amount of testing under a wide variety of conditions and should be highly reliable e It contains features which are not all found in any other single package Area fill with several fill styles on all devices Cell array supported on dot matrix printers Multiple fonts Selective clearing of display surface The advantages of GKS also apply to graphics software which use it such as GNS Support names for GKS graphics devices Almost any graphics program requires you to identify a graphics device to use When it uses GKS they are identified by two integers a workstation type and a connection identifier Workstation is GKS terminology for a graphics device of any description You can t remember the workstation types of all Starlink s graphics devices so the Graphics Name Service has been provided to translate friendly and easy to remember names into their GKS equivalents Most hig
57. iles and or adding new calls and relinking XIMAGE XRONOS Analyse timing general purpose Although designed mostly for X ray astronomy it is basically detector and wavelength independent It has been used to analyse data from the Einstein Observatory EXOSAT and Ginga as well as optical photometry and helioseismology data It includes programs for e Light curve s e Hardness ratio and colour colour plotting e Epoch folding e Power spectrum e Autocorrelation and cross correlation e Time skewness and statistical analysis It consists of a collection of programs each dedicated to one task which can be run from the control environment provided by the XRONOS program This is characterised by three different user interfaces question answer partial question answer and command driven Command files are supported by the last two Its applications can be run in command driven fashion within the EXOSAT Database System XANADU also contains native versions of 11 SUN 1 24 Packages e PGPLOT High level graphics e QDP Data plotter e FITSIO FITS I O on disk Of these PGPLOT and FITSIO are also distributed independently by Starlink SUN 1 24 Packages 12 3 2 Pipeline systems ORAC DR UKIRT and JCMT instrument data reduction pipeline ORAC DR General purpose data reduction pipeline ORAC DR is the data reduction component of the ORAC system used for telescope and instrument cont
58. image and finishing with the fully calibrated spectrum The International Ultraviolet Explore IUE is an ultraviolet telescope in geosynchronous orbit It can e Examine the contents of IUE tapes to find what images are present e Read RAW GPHOT and PHOT images from IUE tapes onto disk Provide them with default calibrations Can also read extracted spectra from IUESIPS e Display images for assessment of validity and quality Various interactive operations can be performed including bad pixel marking image modification and feature identification e Extract spectra from IUE images This uses techniques that are enhancements of those in the TRAK program Spectra exposed in either resolution mode HIRES or LORES can be extracted from RAW GPHOT or PHOT images the latter being the newer style Photometric images that retain geometric distortion You can correct photometric LORES images obtained with the SWP and LWR cameras for defects in the original ITF calibration SUN 1 24 Packages 36 Produce line by line spectra corresponding to the IUESIPS product Produce fully calibrated spectra This includes various forms of wavelength correction absolute calibration and for HIRES ripple correction There is also a semi empirical correction for the HIRES background order overlap problem Display graphs to aid spectrum extraction and calibration Various types of graphics terminals can be used e Combine spectra from groups
59. ional Astronomy Library RV Java UI for RV TABLE Generic table manipulation and I O TAMFITS Third party basic FITS access nom tam UTIL Miscellaneous utillity classes VOTABLE VOTable I O The STARJAVA package can be considered to be independent of the standard USSC and in future will be distributed separately All the STARJAVA applications and classes are distributed under the GPL licence The SPLAT documentation SUN 243 SPLAT A Spectral Analysis Tool has been updated and can be found in star starjava docs splat sun243 htx sun243 html It also appears in the DOCS package and can be seen with the command showme sun243 STARJAVA is not available under Tru64 Unix XANADU Analyse spectra timing and images of X ray astronomical data obtained from multiple missions It was obtained from GSFC Its home page is http heasarc gsfc nasa gov docs xanadu xanadu html Its principal components are XSPEC Fit X ray spectra command driven interactive It is detector independent so it can be used for any spectrometer It has been used to analyze data from HEAO 1 A2 Einstein Observatory EXOSAT Ginga ROSAT BBXRT ASCA CGRO and IUE It has also been used for simulations for XTE and AXAF SUN 1 24 Packages 10 XIMAGE Display and analysis of multi mission X ray images It is instrument independent and analyses data from any X ray imaging detector provided cali bration files are available It s
60. ionally it is very similar to the VAX VMS Help system Major differences e Implemented in a portable way and not tied to the VAX e Allows independent creation of multiple libraries which are bound together at run time and appear to the user as a single tree It is free standing and does not call any other Starlink packages KAPLIBS General purpose KAPPA libraries KAPLIBS is a new package containing several Fortran subroutine libraries that were previously dis tributed as part of the KAPPA package These libraries contain general purpose subroutines which may be of use to anyone developing their own KAPPA like applications SUN 238 contains brief documenta tion but users of KAPLIBS will probably find it useful to examine the source code of relevant KAPPA commands Report messages and errors There is a general need for programs to inform the user about e What they do for example what is going on e What results have been obtained final or intermediate if this would be helpful e What errors have occurred why the program crashed or to ask for more sensible parameter values MERS comprises two libraries to help you do this e MSG Message Reporting System used for reporting non error information e ERR Error Reporting System used specifically for reporting error messages 75 SUN 1 24 Subroutine Libraries ONE Odds and Ends library The ONE library is a small set of Fortran and C routines of a gen
61. k and SUN 132 Applications for Reducing JCMT GSD Data 1 2 2 User s manual describe the package e STARJAVA Starlink Java Infrastructure and Applications Set The new document SUN 251 Getting Started with the Starlink Java Infrastructure and Applications Set describes the package and star starjava javadocs index html describes the Starlink STARJAVA classes API There are miscellaneous documents in star starjava docs for individula package information and third party application documentation The STARJAVA package contains the following applications and classes Note SPLAT TREEVIEW JNIAST and JNIHDS have been moved to the STARJAVA package instead of being individual packages SUN 1 24 Changes since the last issue APPLICATIONS UTILITIES in STARJAVA FROG V0 1a Display and analysis of time series data new SOG V0 1 Son of GAIA new SPLAT V2 0 Spectral Analysis Tool update TABLECOPY V0 3 Copy tables from one format to another new TOPCAT V0 3b Tool for OPerations on Catalogues and Tables new TREEVIEW V2 1 3 Hierarchical data viewer update CLASS LIBRARIES in STARJAVA ARRAY V0 2 N dimensional array manipulation and I O new ASTGUI V1 0 AST specific UI components new AXIS V1 0b2 Third generation Apache SOAP new COCO V1 0 Java UI for Coco new DOMYJ V0 1 Third party DOM access library org dom4j new FITS V0 1 STARJAVA specific FITS access new HDS V0 1 Non native HDS utility classes new
62. keyword You can display or print any document that is found Unfortunately it will not print ATEX documents in a satisfactory form Thus its main use is to find documents not print them Stocks of Starlink Notes and Papers are kept at every Starlink site so you can get a paper copy It has been superseded by the more powerful showme and findme commands provided by the utility Look up information needed to send e mail The program searches the Starlink user database and the on line World E mail Guide for usernames and sitenames Starlink s conferencing software It is based on the World Wide Web and provides similar capabilities under Unix to those provided by the DEC product VAXnotes under VMS Its main features are that it e Retains an archive of entries or notes organized in a hierarchy e Restricts access Users can both read existing notes and submit new ones One difference to VAXnotes is that while VAXnotes could maintain an index of all Conferences even when they were located on separate systems at several Starlink sites FORUM maintains an index only for each instance of FORUM SUN 1 24 Utilities 48 JRE Java Runtime Environment JRE is a copy of the standard Java Runtime Environment which has been wrapped to allow installation in the Starlink software The JRE is included to provide a standard stable base on which to base Starlink Java tools NEWS Starlink s News service Just type news and follow the i
63. low level graphics package known as GRPCKG It has the same user interface as Starlink PGPLOT and non ADAM applications can be moved from one version to the other simply by re linking using the appropriate libraries Starlink PGPLOT SUN 15 113 MUD 61 A high level graphics package for plotting x y plots functions histograms bar charts contour maps and grey scale images Complete diagrams can be produced with a minimal number of subroutine calls but control over colour line style character font etc is available if required It was written with astronomical applications in mind and has become a de facto standard for graphics in astronomy Starlink PGPLOT is the version based on the Starlink library and has the same user interface as Native PGPLOT Non ADAM applications can be moved from one version to the other simply by re linking with the appropriate libraries This is the version supported by Starlink for its applications scs A friendly interface to a subset of GKS SGS stands for Simple Graphics System Many of its features are low level e g draw a line but there are some routines of a slightly higher level drawing arcs formatted numbers etc It does not include routines for high level operations like drawing annotated axes or complete graphs Many plotting programs can be written entirely with SGS or higher level calls There will however be occasions when GKS routines are used as well usually because a speci
64. m within the IRAF command language you should be able to pick the best or relevant tools from both systems to get the job done Currently about 180 commands are available from both the Unix C shell and from the command language They provide the following facilities Generate NDFs and text tables using FITS readers and import and export ancillary data through the NDF FITS extension Generate test data and create NDFs from text files e Set and examine NDF components e Define or calculate a sky co ordinate system for use in conjunction with IRAS tools e Arithmetic including a powerful application that handles expressions e Edit pixels and regions including polygons and circles re flag bad pixels by value or median filtering and paste arrays over others 17 SUN 1 24 Packages Mask regions and pixels whose variances are too large Change configuration flip rotate shift subset change dimensionality Mosaic images normalise NDF pairs Compress and expand images Generalised resampling of NDFs using arbitrary transformations Filter box Gaussian and median smoothing very efficient Fourier transform convolution Deconvolution maximum entropy Lucy Richardson Wiener filter Two dimensional surface fit Statistics including ordered statistics histograming pixel by pixel statistics over a sequence of images Inspect image values Centroids of features particularly stars fit stellar Point Spread Functions
65. mensions is imposed by the software which interfaces with HDS and has no other significance The package can read FIGARO images and images written by NDPROGS can be read by any FIGARO program which can handle the number of dimensions involved It duplicates the functions of standard FIGARO programs as far as 1 d 2 d and 3 d images are concerned but with new features It will also accept NDF format files Most NDPROGS routines now handle data quality and error arrays thus widening the scope and accessibility of the package 27 SUN 1 24 Packages 3 5 Time Series amp Polarimetry Time series analysis Linear spectropolarimetry Dual beam imaging polarimetry Time series amp polarimetry PERIOD Search for periodicities in data It is menu driven You can Read and write data e Read raw data from both Ascii tables and FITS format OGIP files e Store calculated fits in a log file e Output power spectra to Ascii files e Output modelled modified data e Invoke the QDP plotting fitting package allows labelling Examine data e Generate a power spectrum showing periodicities e Fold the data on a given period e Fit sine curves to the input data e Set data points to unity to investigate spectral leakage Manipulate data e Remove background trends in the data via polynomial fits e Create test data e Add noise to data e Add or subtract known periods to from data Many sophisticated techniques
66. metry package at the AAT SUN 1 24 Packages 30 3 6 Database Management CATPAC Catalogue and table manipulation CURSA Catalogue and table manipulation CATPAC SUN 120 Manipulate catalogues and tables CATPAC is no longer supported and is not distributed on Starlink CDs CATPAC may remain as a legacy package at UK Starlink sites It can input process and report tabular data including astronomical catalogues In particular it can e Create and delete catalogues e Report catalogues e Manipulate information about catalogues e Manipulate data in catalogues CATPAC was designed as a replacement for SCA but is being superseded by CURSA see below CURSA SUN 190 Manipulate catalogues and tables It can e Browse or examine catalogues e Select subsets from a catalogue e Sort catalogues e Copy catalogues e Pair two catalogues Subsets can be extracted from a catalogue in a format suitable for plotting by other Starlink packages such as PONGO It can access catalogues held in the following formats e FITS e Small Text List STL e CHI HDS format used byJCATPAC Catalogues in the STL format are simple Ascii text files 31 SUN 1 24 Packages 3 7 Specific Wavelengths ASTERIX X ray data processing SPECX Millimetre wave spectral reduction ASTERIX SUN 98 MUD 4 Analyse astronomical data in the X ray waveband ASTERIX has been withdrawn from the Starlink Software distribu
67. n and display e Mathematical manipulations e Time series analysis e Image processing Spectral analysis Statistical analysis Data quality analysis e HDS editor e Source searching Graphical and textual display SUN 1 24 Packages 32 SPECX SUN 17 MUD 69 70 Reduce and display mm and sub mm data Although it can process spectra from many different instruments it is particularly applicable to JCMT data It can Process up to eight spectra simultaneously Save current status of system after each command is executed List and display spectra on a graphics terminal and print hardcopy on many printers Do single and multiple scan arithmetic scan averaging etc Store and retrieve intermediate spectra in storage registers Fit and remove polynomial harmonic and Gaussian baselines Filter and edit spectra Determine important line parameters peak intensity width etc Calculate Fourier transforms and power spectra Calibrate data Assemble a number of reduced individual spectra into a map file and contour any plane or planes of the resulting cube Execute macro command sequences and indirect command files It uses its own data format so it is not possible to access directly reduced spectra from other packages However it can import data from GSD format data files as produced by the JCMT write out maps and spectra in the file formats of FIGARO and KAPPA and write spectra and maps to Ascii
68. name If you are using the hypertext version of this document the most up to date document references can be found by following the link from the software item name Contents 2 Changes since the last issue 2 2 Withdrawn Packages 2 3 Package details 3 1 General Purpose 3 2 Pipeline systems 3 3 Image Processing amp Photometry 3 4 Spectroscopy 3 5 Time Series amp Polarimetry 3 6 Database Managemen 3 7 Specific Wavelengths 3 8 Specific Instruments 3 9 Format Conversion 3 10 Mathematics amp Statistics 3 11 Graphics 4 Utilities 4 1 Astronomical Utilities 4 2 General Utilities 4 3 Document Preparation 4 4 Programming Support 5 Subroutine Libraries 5 1 Astronomical amp Mathematical 5 2 Data Access amp Management 6__Infrastructure 7 Acknowledgements Index 2 1 New packages SUN 1 24 Contents 1 SUN 1 24 Introduction 1 Introduction This document contains a survey of the complete Starlink Software Collection The level of detail should enable you to decide whether or not to investigate a specific software item further Full details of individual items can be found in the document references Installation instructions are contained inSUN 212 The strategy guiding the development of Starlink software is described inSGP 42 A major influence on this strategy is the set of Starlink Softwa
69. nants e F04 Simultaneous linear equations e F05 Orthogonalisation e F06 Linear algebra support routines e F07 Linear equations LAPACK e F08 Least squares and eigenvalue problems LAPACK e G01 Simple calculations and statistical data e G02 Correlation and regression analysis e G03 Multivariate methods e G04 Analysis of variance e G05 Random number generators e G07 Univariate estimation e G08 Nonparametric statistics e G10 Smoothing in statistics e G11 Contingency table analysis e G12 Survival analysis e G13 Time series analysis e H Operations research e M01 Sorting e P01 Error trapping e S Approximations of special functions e X01 Mathematical constants e X02 Machine constants e X03 Innerproducts e X04 Input output utilities e X05 Date and time utilities PDA SUN 194 Mathematical subroutine library This is intended to replace the library in Starlink application code It is coded in Fortran and has a Fortran 77 binding The interface is mostly double precision although the Fourier transform part provides for both double and single precision and the routines from DIERCKX exist only for single precision SUN 1 24 Subroutine Libraries 58 SLALIB Positional astronomy library SLALIB makes accurate and reliable positional astronomy applications easier to write Most of the routines are concerned with astronomical position and time but s
70. nce in the sensitivity of the two channels of a dual beam polarimeter These corrections rely on redundancy in the supplied data and require a specific set of analyser positions to be used Reduce time series and polarimetric data Time series and polarimetry facilities are missing from most existing data reduction packages which are usually oriented towards either spectroscopy or image processing or both TSP however can process the following data 29 SUN 1 24 Packages Spectropolarimetry obtained with the AAO spectropolarimeters using wave plate or Pockels cell modulators in conjunction with either IPCS or CCD detectors Infrared spectropolarimetry obtained with the IRPOL polarimeter module in conjunction with the CGS82 grating spectrometer and the UKT6 and UKT9 CVF systems at UKIRT Infrared imaging polarimetry obtained with the IRIS instrument at the AAT and with similar instruments Time series imaging and polarimetry obtained with the AAO Faint Object Polarimeter Time series polarimetry obtained with the Hatfield Polarimeter at either UKIRT or AAT Time series polarimetry obtained with the University of Turku UBVRI polarimeter Five channel time series photometry obtained with the Hatfield polarimeter at the AAT in its high speed photometry mode Time series infrared photometry data obtained with the AAO Infrared Photometer Spectrometer IRPS Time series optical photometry data obtained using the HSP3 high speed photo
71. nstructions A language for manipulating text files and processes easily It provides a more concise and readable way to do many jobs that were formerly accomplished with difficulty by programming in the C language or one of the shells There are several O Reilly books on Perl that will help you understand and use it Learning Perl and Programming perl are two of these books Chapter 39 of Unix Power Tools gives an introduction to Perl PERLMODS Additional CPAN modules for the Perl package PERLMODS is a package of additional modules from CPAN Comprehensive Perl Archive Network which are added to the standard PERL installation to provide extra facilities needed by the STARPERL modules and by the SURF package PINE MUD 141 Read e mail Just type pine to start it A lot of on line help is available STARADMIN Build and maintain a database of Starlink users Used by Starlink Site Managers to manage their user lists Additional modules for the Perl package STARPERL is a package of additional Starlink modules which are added to the standard PERL installation to provide facilities such as NDF access NDFPERL XDISPLAY Get output from an X client to display on the screen of your X terminal In other words it provides an easy way to use remote X windows 49 SUN 1 24 Utilities 4 3 Document Preparation Ascii to PostScript converter Text editor PostScript previewer Hypertext utilities
72. of chelle orders HIRES or from different apertures LORES by mapping and averaging them onto an evenly spaced wavelength grid e Write spectra to Starlink NDF files which can then be processed by DIPSO and other Starlink software Output includes individual extracted order and aperture spectra or combined spectra Files can also be created in the same format as that written by TRAK JCMTDR Reduce continuum mapping data obtained with the UKT14 instrument on the JCMT JCMTDR is now distributed on Starlink CDs There is now a Linux port The James Clerk Maxwell Telescope JCMT at Mauna Kea Observatory observes in the millimetre wave part of the spectrum The program can Transform JCMT map data into a tangent plane image centred on a given position Optionally rebin each input dataset individually before coadding them into the result e Append an IRAS astrometry structure to a rebinned map so that IRAS90 can be used on it to overlay coordinate grids object positions etc e Correct JCMT data for the effect of atmospheric extinction e Convert JCMT data from GSD format to FIGARO format e Convert a JCMT map file into a format suitable for further processing deconvolution and resam pling by DBMEM e Convert an image into a time spectrum with map pixels sorted in order of increasing LST of observation and vice versa Deconvolve the chopped beam from a dual beam map of a source Data files can be read in either ol
73. ollege London Echelle Spectrograph UCLES but the algorithms are sufficiently flexible to reduce spectra from many sources It can e Locate spectral orders e Remove cosmic rays e Detect bad image rows columns and saturated pixels e Trace spectral orders e Determine object channels e Generate flat field balance model SUN 1 24 Packages Model scattered light Extract optimal spectrum Correct chelle blaze Extract quick look spectra Locate lines in arc spectra automatically Calibrate wavelengths of arc spectra Fit distortion for spectral orders Extract distorted orders Scrunch extracted spectral orders Produce distortion free image Plot data used for a reduction Output products FIGARO Reduce and analyse astronomical data 24 SUN 86 MUD 12 13 14 FIGARO is a general purpose data reduction package It contains particularly extensive facilities for reducing spectroscopic data but also has powerful facilities for manipulating direct images and data cubes Starlink recommends it as the most complete spectroscopic data reduction system in the Collection It can be used interoperably with other packages most notably KAPPA because it supports the NDF data format and therefore all foreign formats for which conversion utilities exist These include its old DST format FITS and IRAF The use of NDF also means that you can automatically record data processing history and can operate on sub sets of s
74. ome have wider trigono metrical numerical or general applications and RVJall make extensive use of SLALIB as do several telescope control systems around the world Current versions are written in Fortran 77 and run on VAX VMS several Unix platforms and PC A generic ANSI C version is also available from its author Its main functions are String decoding sexagesimal conversions Angles vectors rotation matrices Calendars timescales Precession nutation Proper motion FK4 5 elliptic aberration Geocentric coordinates Apparent and observed place Azimuth elevation Refraction air mass Ecliptic galactic and supergalactic coordinates Ephemerides Astrometry Numerical methods It gives programmers a basic set of positional astronomy tools which are accurate and easy to use It is Readily available including source code and documentation Supported and maintained Portable coded in standard languages and available for multiple computers and operating systems Thoroughly commented both for maintainability and to assist those wishing to cannibalize the code Stable Trustworthy some care has gone into testing it both by comparison with published data and by checks for internal consistency Rigorous corners are not cut even where the practical consequences would in most cases be negligible Comprehensive without including too many esoteric features required only by specialists Pra
75. or no support There is no Linux port IRCAMDR may remain as a legacy package at UK Starlink sites Reduction of IRCAM data is now best performed using the ORAC DRIdata reduction facility 35 SUN 1 24 Packages IRCAMS is a camera on the United Kingdom Infra red Telescope UKIRT In addition to handling IRCAMS images of 256 x 256 pixel size it can handle IRCAM1 and IRCAM2 images of 6258 pixels Almost all the applications with the exception of med3d will work on NDF images of any physical pixel dimensions for example 1024 x 1024 CCD images can be processed med3d median filters stacks of images up to 256 x 256 in size at present It can Display images line graphics colour tables Reduce data including automatic single star photometry and bad hot pixel removal Register and mosaic images and determine positions Extract and smooth images do arithmetic change dimensions Statistical analysis Photometry Polarimetry IRCAMPACK Process IRCAM data IRCAM is an infrared camera on the United Kingdom Infra red Telescope UKIRT CCDPACKJand KAPPA will probably do most of the processing you require IRCAMPACK provides extra facilities It can e Interpret and process the specific header information stored within IRCAM data files e Normalise frames to unit total exposure time e Provide a simple imaging polarimetry reduction procedure Process data from the IUE chelle spectrograph starting with the raw
76. page e Pictures to be scaled before insertion into a TEX document STAR2HTML Convert Starlink documents to Hypertext Processes Starlink document ATEX source files into a set of Hypertext Markup Language HTML files suitable for browsing with hypertext viewers and web browsers This is a major component of Starlink s system for producing hypertext documents which also includes GHOSTSCRIPT the dvips processor and PERL The processing to hypertext is performed by IATIEX2HTML which is bundled with STAR2ZHTML I4TRX2HTML is not used directly becuase Starlink documents use a series of additional macros to allow inter document cross referencing within the Starlink document collection SUN 1 24 Utilities 52 TEX MUD 48 51 72 3 79 80 126 132 3 152 SSN 24 Produce high quality text and diagrams by type setting I4TEX is a document preparation system based on T X but easier to use The current versions are TEX v3 1415 and IATRx2e Dec 1994 The final output is usually produced by a laser printer Starlink recommends that you create your documents using ATEX2e with formats based on skeleton files such as star docs sun tex SUN 12 is a cookbook showing how to generate common kinds of format using IATEX this is a quick way to learn how to use it SGP 28 and SGP 50 give advice on how to produce documents in a suitable style for Starlink 53 SUN 1 24 Utilities 4 4 Programming Support Fortran source code checker
77. parameter interface and a more robust file reading system A script FLUXNOW runs the program for the current time and date This gives you current positions and flux levels for all the planets Process IRAS data IRAS90 is not distributed on Starlink CDs and is no longer supported though it may remain as a legacy package on UK Starlink sites There is no Linux port The Infrared Astronomical Satellite IRAS flew in 1983 It carried three instruments a main detector array a low resolution spectrometer LRS and a chopped photometric channel CPC Most of the observations were part of a whole sky survey but some pointed observations of specific objects were made Raw data was calibrated and cleaned up to produce a data set called the Calibrated Reconstructed Detector Data CRDD This was the source of the final data products which include catalogues and images Several items of Starlink software can be used to process and examine IRAS data Use KAPPA to process and display images DIPSO to analyse LRS spectra CURSA to access and report on the catalogues However the most closely related software is I RAS90 This can process CRDD data to produce an image of a region of the sky or search for and examine an object at a given position IRCAMDR Reduce analyse and display data from IRCAM3 It can also handle any 2 d image in the standard Starlink NDF data format IRCAMDER is not distributed on Starlink CDs and there is little
78. pectra and images Another feature is the propagation of error data quality arrays through the data reduction calculations It can Analyse absorption lines interactively Do aperture photometry Calibrate B stars Calibrate flat fields Calibrate using flux calibration standards Calibrate wavelengths of spectra Correct S distortion Extract spectra from images and images from data cubes and insert spectra into images and images into data cubes Extract spectra from images taken using optical fibres Fit Gaussians to lines in a spectrum interactively Generate and apply a spectrum of extinction coefficients Input output and display data 25 SUN 1 24 Packages Look at the contents of data arrays other than graphically Manipulate complex data structures mainly connected with Fourier transforms Manipulate data arrays by hand Manipulate images and spectra arithmetic and more complicated Process data taken using FIGS the AAO s Fabry Perot infra red grating spectrometer Process chelle data in particular the UCL chelle in use at the AAO The programs from the old SPECDRE and TWODSPEC packages have been merged with FIGARO and provide additional facilities Hyper cubes In general the data being processed are a hyper cube where each row or hyper column is a spectrum A single spectrum can be an appropriate section of the hyper cube cut out on the fly as the data are accessed
79. re Strategy Groups Guidelines for members of these groups is given in SGP 44 New users of Starlink facilities should read the Starlink User s Guide SUG The World Wide Web is an important tool for informing users about the Starlink Project and its software and Starlink has published comprehensive documentation in this medium Eventually this will be linked together as a single hyper linked document by utilising the HTXlutilities SUN 188 One of the greatest advantages of the Web is its potential for updating and distributing documents more frequently and rapidly than is practicable on paper For current information about the Starlink software and documenta tion you should refer to the information on the Starlink Web Site http www starlink ac uk This edition describes the Collection as available in the Autumn 2002 CD ROM distribution of December 2002 SUN 1 24 Changes since the last issue 2 2 Changes since the last issue 2 1 New packages Two new items have been added to the Collection since the previous edition of this document SUN 1 23 5 August 2003 and are indicated as such in the heading of the appropriate sections The new packages are e AUTOASTROM Autoastrometry of mosaics The new document SUN 242 AUTOASTROM Autoastrometry for Mosaics describes the package AUTOASTROM is not available under Tru64 Unix e JCMTDR Applications for reducing JCMT GSD on the fly data The documents SC 1 JCMTDR Cookboo
80. riety of data reduction configurations e Interlace oversampled data frames e Reduce known BIAS DARK FLAT ARC OBJECT and SKY frames e Wavelength calibrate via suitable ARC lines e Flux calibrate via a suitable STANDARD e Remove the SKY residual sky OH lines A lt 2 3 um and thermal emission A gt 2 3 um from data SUN 1 24 Packages 34 e Add data into groups for improved signal to noise e Extract and de ripple a spectrum e Maintain an index of reduced observations e Maintain if required an archive of observations e Plot data in a variety of ways FLUXES Calculate accurate topocentric positions of the planets and also integrated flux densities of five of them at a number of wavelengths for the JCMT telescope on Mauna Kea Hawaii It provides calibration information at the effective frequencies and beam sizes employed by the UKT14 and SCUBA receivers on this telescope The filter centre and widths are shown for each wavelength used The filter frequencies are the effective frequencies for 1mm of water vapour The calculated planet positions should normally be accurate to better than 1 of arc The value for the Moon is less accurate than this and for critical applications requiring sub arc second accuracy you should use a different method The version distributed by Starlink has been modified to employ the highly accurate JPL ephemeris in all planetary position calculations It also adopts the Starlink
81. rol at the United Kingdom Infrared Telescope UKIRT and the James Clerk Maxwell Telescope JCMT on Hawaii It provides a general purpose automatic data reduction pipeline for the CGS4 UFTI and IRCAM instruments on UKIRT and the SCUBA instrument on JCMT ORAC DR recipes to drive the reduction of a set of observations made to a known observation pattern at the telescopes The headers data of each dataset is read to discover which data processing recipe to apply to it The data reduction is performed by tasks from other Starlink packages such as KAPPA CCDPACK POLPACK and PHOTOM It can also use GAIA for image display 13 SUN 1 24 Packages 3 3 Image Processing amp Photometry Coodinate frame manipulation CCD data reduction Stellar photometry ESP Extended surface photometry Automatic detection of objects on an astronomical image Graphical image analysis KAPPA Image processing amp visualisation Retired KAPPA tasks Aperture photometry Position intensity and shape analysis Astronomical image display Stellar photometry Data visualisation ATOOLS Manipulation of coordinate frame descriptions ATOOLS is a new package of applications which manipulate descriptions of coordinate frames mappings etc in the form of Objects Each application within the ATOOLS package corresponds closely to one of the functions within the AST library ATOOLS thus provides a high level interface
82. s campaigns can be based Other examples include AIPS and MIDAS as well as Starlink s own large collection of infrastructure tools and application packages and the various forms of the FIGARO system Each has its own particular strengths and special capabilities and AIPSjare the most comprehensive overall The excellent support provided by IRAF s home institute with which Starlink maintains close contact means that comparatively little national UK Starlink support is called for and provided the same is true for the other overseas environments mentioned above IRAF is a sound choice for many Starlink users doing data analysis especially where compatibility with overseas collaborators is a requirement The choice is harder for those wishing to develop major applications of their own who may be reluctant to adopt IRAF s non industry standard SPP programming language or who feel uncomfortable with the limitations of the flat IRAF data formats Those who need formal guarantees of future support should also be very wary about committing themselves to any package which is not under UK control However IRAF is an important weapon in the armoury of the average Starlink data analysis user and likely to remain so for some years An important part of Starlink s present software plans is to enhance interoperability with other envi ronments IRAF being of special importance Starlink applications can already share data with other pa
83. s directly for efficient memory and disk usage Those that do not will usually undergo automatic data conversion to produce the desired result Its graphics are device independent X windows and overlays are supported The KAPPA package may also be run from the IRAF CL SUN 1 24 Packages 18 KAPRPH Retired KAPPA commands KAPRH is a package containing commands retired from the KAPPA package see SUN 95 These commands have been removed from KAPPA but are retained in KAPRH to satisfy any occasional need there may be for them KAPRH is documented in SUN 239 KAPRH contains the following retired KAPPA commands CONTOVER GREYPLOT INSPECT MOSAIC QUILT SNAPSHOT TURBOCONT as well as a help command KRHHELP PHOTOM Aperture photometry It has two basic operating modes e Use an interactive display to specify the positions for the measurements e Obtain those positions from a file The aperture is circular or elliptical and the size and shape can be varied interactively on the display or by entering values from the keyboard or parameter system The background sky level can be sampled interactively by manually positioning the aperture or automatically from an annulus surrounding the object It is used by the Graphical Astronomy and Image Analysis tool GAIA which integrates the tasks of aperture photometry with an image display tool This allows the detailed inspection of objects and their environments and provides a
84. s quickly as your hardware CPU combination allows or cycle through them by hand The GAIA package may be run from the IRAF CL KAPPA General purpose functions particularly suitable for image processing data visualisation and ma nipulating components KAPPA is the backbone of Starlink s application packages Its facilities integrate with the more specialised Starlink packages described in this survey Thus the functionality of KAPPA should not be regarded in isolation It can process data in formats other than NDF such as FITS and IRAF by using an on the fly conversion scheme Many commands can process data arrays of arbitrary dimension and others work on both spectra and images It operates from both the Unix C shell and the ICL command language KAPPA should not be perceived as a rival to FIGARO Now that FIGARO is integrated with other Starlink packages they should be seen as complementary with FIGARO concentrating on spectroscopy and KAPPA on image processing In a wider context KAPPA offers facilities which are not in IRAF for instance handling data errors qual ity masking a graphics database availability from the shell as well as more n dimensional applications widespread use of data axes and a different style It also integrates with instrument packages developed at UK observatories With the automatic data format conversion and the likelihood that KAPPA and other Starlink packages will be available fro
85. s to be stored together in a single file but in a structured fashion NAOS SUN 235 Finding Guide Stars for use with NAOMI on the WHT The NAOS package may be used to find guide stars suitable for use with the NAOMI adaptive optics system available on the William Hershell Telescope WHT on La Palma NAOMI usually requires a relatively bright guide star located close to the target object being observed You prepare a list of potential target objects and NAOS remotely searches a version of the USNO PMM astrometric catalogue to find suitable guide stars for these targets You would usually use NAOS at your home institution prior to travelling to La Palma to observe with NAOMI SUN 1 24 Utilities 46 OBSERVE Show the observability of a star through the year from a given geographical location It generates a plot that shows for a complete year the e Star rising amp setting times e Times the star is 30 above the horizon e Times of astronomical twilight e Phase rising and setting times of the Moon e Distance of the Moon from the star RV List the components in a given direction of the observer s velocity on a given date This allows an observed radial velocity to be referred to an appropriate standard of rest It also com putes light time components to the Sun allowing the times of phenomena observed from a terrestrial observatory to be referred to a heliocentric frame of reference The accuracies of better
86. se movements etc One event type that all applications must handle is the window expose event which occurs whenever part of a window that was invisible because another application s window was obscuring it for example becomes visible The application is 69 SUN 1 24 Subroutine Libraries responsible for restoring the contents of the newly exposed part of the window but only an application designed as an X application can do this an application that is using X via a graphics package such as or but is otherwise a conventional application that knows nothing of X cannot The X graphics window managey makes a window on an X display behave like a traditional graphics device by making the lifetime of the window independent of any applications program and by handling window expose events Applications still send plotting commands directly to the window they don t have to go via a server process so there is no adverse impact on performance All communication between the window manager and the application is via the X server and the graphics window manager does not have to run on the same machine as the application Not to be confused with the Window Manager which allows you to move windows around the screen iconize them etc SUN 1 24 Subroutine Libraries 70 IDI MUD 28 An international standard for displaying astronomical data on an image display It is intended for programs that need to manipulate images to a
87. ser interaction via graphics is granted auto matic arc line identification is also possible Re sampling You can either re sample all spectra in a hyper cube or re sample and average into one spectrum any number of input spectra Information about the covariance between pixels can be carried through to a line fit routine Spectral fits You can fit polynomials blended Gaussian or triangle profiles Fit results are stored along with the data and can be turned into fake data sets for later subtraction division etc The FIGARO programs may be run from the IRAF CL but the former SPECDRE and TWODSPEC programs are not yet available under the IRAF CL SUN 1 24 Packages 26 NDPROGS Manipulate and display images of up to six dimensions The NDPROGS package is no longer supported and will be withdrawn if operating system or compiler changes cause it to fail It is not distributed on Starlink CDs but may be installed at UK Starlink sites as a legacy package Primarily it is designed to manipulate Taurus spectral line data cubes which are 3 d images in which two of the dimensions are spatial and the third is spectral However it contains no instrument specific features and can therefore be used to analyse similar data The term image here simply means a regular data array which might be anything from a 1 d spectrum or profile to a 4 d array consisting of several long slit spectra with polarization vectors The upper limit of six di
88. sitions of objects with those in a reference catalogue and fitting with both four and six component distortion models e with enough data obtain cubic distortion and plate tilt using seven to nine component models 43 SUN 1 24 Utilities e if enough information is available it will do the reductions in observed place correcting for atmospheric refraction Autoastrom provides a shell around ASTROM so that as well as the core astrometric facilities of ASTROM autoastrom will e work on a CCD image provided as an NDF as long as it has at least rough astrometry plate centre and scale automatically download appropriate reference catalogue information from catalogue servers supported by the SkyCat library insert the astrometric results into the original NDF as a WCS component alternatively or additionally make the astrometry available as a set of FITS WCS header cards CHART Plot star fields positions magnitudes and other data from the CSI79 SAO AGK3 PERTH70 and Dixon non stellar objects catalogues CHART is not distributed on Starlink CDs but it may remain as a legacy package at UK Starlink sites There is no Linux port an little support available CHART will be superceeded by facilities in CURSA in the near future You can specify a series of search areas place magnitude or total number limits on the search and chose which source catalogues to include or exclude After the search is made you may list the res
89. spectral lines can also be marked on the display You can then move the detector window around by moving a crosshair cursor to the desired centre of the detector and then clicking the left hand mouse button to set the detector position or else by explicitly specifying the desired central wavelength At each position the screen displays the minimum central and maximum wavelengths and order numbers falling on the detector as well as an estimate of the length of the detector in Angstroms The position of the box can be marked on the screen so as to ease preparation of observations where multiple overlapping wavelength ranges are required You can also save the current detector position in a text file FINDCOORDS Finding the Coordinates of a Named Object FINDCOORDS is a new utility for using the name of an astronomical object to look up its equatorial coordinates You simply enter the name of the object and its coordinates are displayed Type findcoords object name For example findcoords ngc3379 If the name is recognised then the equatorial coordinates of the object will be displayed The Right Ascension is shown in sexagesimal hours and the Declination in sexagesimal degrees both are for equinox J2000 FINDCOORDS works by submitting a remote query via the Internet to the version of the SIMBAD name resolver provided by ESO the basic SIMBAD is maintained by the Centre de Donnees astronomiques de Strasbourg CDS Consequently find
90. standard Fortran and C Full support for data exchange in FITS format On line help history and logging facilities Flexible command and control language with full flow control and debugging facilities e Extensive interface libraries in Fortran and C for access to the MIDAS database It also contains extensive packages in the areas of spectral reduction including data in long slit and chelle formats CCD observations crowded field photometry object search and classification fitting and modeling of data astrometry and statistical analysis STARJAVA Starlink is developing a set of Java data reduction and analysis tools and Java data access classes The new Java tools and classes are needed to produce applications in the Virtual Observatory VO era and to complement the AstroGrid and other VO capabilities such as the International Virtual Observatory Alliance Data Model You can view a section of a proposed International Virtual Observatory Alliance Data Model including HDX NDX and Table data structures with the WCS astrometry library at http www starlink ac uk java java htm The Starlink Java Software STARJAVA has had numerous changes and additions STARJAVA can now be considered as a separate entity from the classic Starlink applications and libraries although in this release it is provided as a standard Starlink package The document SUN 251 Getting Started with the Starlink Java Infrastructure and Applications S
91. than 0 01 km stand 0 1 s are adequate for most classes of work the notable exception being some pulsar observations The input output arrangements are flexible to allow a variety of operating styles interactive input from a file batch etc All input is free format The normal operating style is interactive prompts appear on a terminal data are entered specifying the report required and a listing is sent to disk for later printing SKYCAL SUN 187 MUD 158 Almanac and calculator interactive This consists of two programs e SKYCALC an Interactive Almanac It helps you plan and execute observing runs and allows easy calculation of airmasses twilight lunar interference coordinate transformations and such nearly everything except the weather e SKYCALENDAR a Nighttime Astronomical Calendar to calculate and print astronomical calendars Both programs have several preset Observatory locations to choose from You can also specify your own 47 SUN 1 24 Utilities 4 2 General Utilities Starlink document search EMAIL E mail address search Computer conferencing JRE Java Runtime Environment Starlink news system Practical extraction and report language Additional CPAN Modules for Perl PINE E mail interface User database maintainer Additional Modules for Perl X window display setup DOCFIND Search Starlink document and keyword indexes for a specified
92. ties include setting a prompt string and suggested defaults 65 SUN 1 24 Subroutine Libraries PRIMDAT Process primitive data Does arithmetic mathematical operations type conversion and inter comparison of any of the primitive numerical data types supported by Provides e Processing facilities which are not normally available e A uniform interface e Improved portability and efficiency e Facilities for processing bad data e Numerical error handling e A set of constants A distinction is drawn between three classes of primitive data which differ in their interpretation and in the algorithms best suited to processing them e Values scalar data which may take one of the defined bad values sometimes called magic values whose presence signifies that the affected datum is undefined e Vectorised arrays 1 d arrays of values or arrays treated as 1 d whose elements are processed in the way described above e Numbers always interpreted literally as scalar numerical quantities i e bad values are not recog nised on input and are not explicitly generated on output Handle references to HDS objects Stores references to data objects in special HDS reference objects and lets you obtain locators to reference objects Helps make your software portable You can e Create a reference object and put a reference in it e Obtain a locator to an object possibly via a reference e Obtain a locator to a
93. tion and is no longer included on Starlink CDs from Spring 2000 due to the end of funding for the ROSAT satellite program It may remain as a legacy package at UK Starlink sites Continued best efforts support may be provided by the Space Research group at the University of Birmingham for the recent development version This may be found on the Asterix Home Page see http www sr bham ac uk asterix No support will be provided for the Starlink version Many of its programs are general purpose and are capable of analysing any data in the correct format It is instrument independent and currently has interfaces to the EXOSAT and ROSAT instruments Its data are stored in files and are therefore compatible with many other Starlink packages There are basically two different types Binned data e g time series spectra images are stored in format Data errors stored in the form of variances and quality are catered for Event data store information about a set of photon events Each event will have a set of properties e g X position Y position time raw pulse height The input data are first processed by an instrument interface Event data are then processed and binned and the binned data are processed Finally graphical output is generated The commands may be classified as follows e Interface to particular instruments EXOSAT ROSAT etc e Event dataset and binned dataset processing e Data conversio
94. ts using the on the fly data conversion ability of NDF Pan zoom and manipulate data range and colour table Continuously display of cursor position and image data value Continuously display of the RA and DEC coordinates for suitable images i e FITS images with WCS headers Guide Star Catalog images for instance Display many images clones each in its own window Annotate in colour using text and line graphics Print the displayed image and annotations to a PostScript file Profile in real time i e move a line around on the image and see the image data values displayed as a profile change Real time pixel value table the data values in a region about the cursor SUN 1 24 Packages 16 Aperture photometry A highly interactive environment for controlling the positions sizes and orientations of circular and elliptical apertures The sky estimates can be made from annuli of these apertures or from related sky apertures The measurements can be in either instrumental magnitudes or mean counts Patch images Select arbitrarily shaped regions on an image and replace them with a surface fit to other regions together with an artificial noise component An ideal way to remove cosmetic defects from an image Interactive regions Calculate statistics mask out and extract arbitrarily shaped parts of your images define ARD regions for other programs to use Blink images Animate displayed images a
95. ture into two parts a set of standard components and a set of extensions each of which individually satisfies one of the two requirements The structure consists of a central core of information whose interpretation is well defined and for which general purpose software can be written with wide applicability together with an arbitrary number of extensions which may be used by specialist software but whose interpretation is not otherwise defined Those who wish to know more of the background to this philosophy can find a detailed discussion in SGP 38 NDG SUN 2 Routines for Accessing Groups of NDFs The NDG package provides a means of giving the user the ability to specify a list or Group of NDFs as a reply to a single prompt for an parameter NDG can process NDFs which are stored as components within an HDS container file and can also process foreign data formats using the CONVERT utilities that the library uses as described in SSN 20 PAR SUN 114 Parameter system A convenient way for programs to exchange information with the outside world through I O channels called parameters These enable a user to control a program s behaviour It supports numeric character and logical parameters and is currently implemented only on top of the ADAM parameter system Parameter values may be obtained with or without a variety of constraints Results may be put into parameters to be passed to other applications Other facili
96. tware item called contains some Starlink extensions to it The routines are thoroughly documented and just a few simple calls will produce graphs of excellent appearance They also very flexible with dozens of plot details independently controllable to give you exactly the result required The plots provided are e Annotated curves or families of curves e Contours for 1 d and 2 d data with labels e Dashed lines with labels Continental national and US state boundaries in nine map projections e Graph paper axes etc Halftone greyscale pictures from 2 d arrays e Histograms e Iso value surfaces with hidden lines removed from 3 d arrays e Software characters 3 d displays of a surface with hidden lines removed from 2 d arrays e Vector flows of fields for which planar vector components are given on regular rectangular lattices Lines in three space 2 d velocity fields 71 SUN 1 24 Subroutine Libraries Native PGPLOT SUN 15 MUD 61 A high level graphics package for plotting x y plots functions histograms bar charts contour maps and grey scale images Complete diagrams can be produced with a minimal number of subroutine calls but control over colour line style character font etc is available if required It was written with astronomical applications in mind and has become a de facto standard for graphics in astronomy Native PGPLOT is the original version from Tim Pearson at Caltech based on the
97. ults at a terminal or on a printer Positional information may be precessed to a specified equinox In the case of astrometric data proper motions may be applied up to a specified epoch You can plot the results in the form of an overlay or finding chart Extra objects i e with positions supplied by you may be added to the plot at this stage The plot may be made on any GKS device anda number of different plot options are available such as scale and area an RA and Dec coordinate grid and various forms of error box You may also use the results as input to an astrometry program i e it can be used to select astrometric stars as positional references In this case you will be asked to supply x y positions for the reference stars from a measuring machine and can then convert unknown x y positions to RA Dec or vice versa ASTROM performs the actual astrometry from within CHART if necessary Convert star coordinates from one system to another Both the improved IAU system post 1976 and the old pre 1976 system are supported It can transform between the following coordinate systems e mean a old system with E terms loosely FK4 e mean old system no E terms some radio positions e mean a new system loosely FK5 e geocentric apparent a new system e ecliptic coordinates A B new system mean of date e galactic coordinates I b LAU 1958 system SUN 1 24 Utilities 44 The input o
98. upports detailed analysis of EXOSAT CMA Einstein HRI and IPC ROSAT PSPC and HRI and ASCA GIS and SIS data It also supports some basic analysis of optical infrared and radio images It has a built in data simulation program that can simulate images of current and future X ray missions e g SAX AXAF and XMM It can e Read images and event files e Rebin images smooth and display Detect and remove sources statistical analysis Correct for vignetting exposure background and point spread function e Mosaic images Contour plots and overlays Convert sky grids and pixel coordinates e Change equinox Slice x y image Generate point spread functions Select circular annular and box regions Interface to saoimage e Extract spectra and lightcurves from event data e Simulate images Its display and graphic capabilities are based on the PGPLOT graphics package which supports most terminals and workstations The saoimage package can also be spawned to display images and select regions While XIMAGE is a multimission package it must first know about the calibration information associated with a mission in order to be able to make a detailed image analysis Some functions are mission independent e g display but others are not e g source detect It will read images from an unknown mission but beware of trying to make a detailed analysis adding new missions usually requires either adding new f
99. using a command with the following features the ability to read character strings as well as numeric values support for comment lines and column headings error trapping during file input user specification of column delimiters allowing ATEX and TeX format tables to be read selective reading of data e Use Fortran like statements to perform mathematical manipulations on data Specialised extra data columns Interactive cursor functions Error ellipses Vector plots e Simple statistical analyses e Resample data e Draw user specified functions defined by Fortran like statements e Plot astronomical positional data in one of several geometries e Read positions as Right Ascension and Declination The PONGO package may be run from the IRAF CL 41 SUN 1 24 Packages SM MUD 159 160 Draw graphs and plots interactively It has some image handling capability but works mostly with vectors It can e Generate a nice looking plot with a minimal number of simple commands e View the plot on screen then with a simple set of commands generate hardcopy e Build and save your own plot routines which can then be invoked with a single user defined command e Keep a history of your plot commands which you can edit and define as a plot routine for reuse e Specify plot data from within the program or read it from a simple file SUN 1 24 Utilities 42 4 Utilities 4 1 Astronomical Utilities Basi
100. utput arrangements are flexible to allow a variety of operating styles interactive input from a file report to a file batch etc Also in addition to the report which is produced the results are available in raw form to a fixed resolution and free from extraneous formatting this file is intended to be read easily by other programs It offers control over report resolution and has simple online help All input is free format and defaults are provided where this is meaningful In order to comply with the IAU 1976 recommendations all position data published from 1984 on should be given in the new system using equinox J2000 0 However for years to come positions will frequently be given in the old system using equinox B1950 0 Discriminating astronomers and astrophysicists are best advised to give both B1950 and J2000 positions for sources mentioned in their publications the conversion can be done using COCO ECHWIND Plan observations with either the Utrecht chelle spectrograph UES or the UCL coud chelle spec trograph UCLES It can be run at your home institution when preparing an observing proposal or before or during an observing run It lets you view interactively that part of the spectrum which will fall on the detector for a given central wavelength This is achieved by drawing a complete chellogram in an X window along with a box representing the exact size and shape of the detector The positions of individual
101. vice HLP Interactive help system General purpose KAPPA routines Message and error reporting Odds and Ends library Parameters and communications POSIX interface cHR Augment the limited character handling facilities of Fortran 77 Converts Fortran data types into text strings and the reverse does wild card matching string sort ing paragraph reformatting and justification It can be used for building text strings for interactive applications or as a basis for more complex text processing applications It can e Change case e Compare and edit strings e Encode and decode Fortran data types e Make enquires about character strings e Enhance portability e Search for strings cNF Mix program segments written in Fortran and C in a portable manner It provides e C macros to hide the different ways that computers pass information between subprograms e C functions to handle Fortran character strings and logical values EMS Construct and store error messages for future delivery to a user via ERR ERR is the Starlink Error Reporting System which is part of MERS It can be regarded as a simplified version of ERR without the binding to any software environment e g for message output or access to the parameter and data systems It conforms to the error reporting conventions of MERS SUN 1 24 Subroutine Libraries 74 HP Retrieve named items from a hierarchical library of text Funct
102. xt of the original file and suggests possible corrections when it can figure them out 51 SUN 1 24 Utilities JED Edit text A text editor which provides a reasonably good emulation of EDT together with a few extra facilities such as cut and paste of rectangular regions unlimited undo horizontal scroll and display of two or more windows LATEX2HTML SUN 201 MUD 152 Convert JATEX to HTML LATEX2HTML is now included in the STAR2ZHTML package Processes ATEX source files into a set of Hypertext Markup Language HTML files suitable for browsing with hypertext viewers and web browsers NUTPU Process text A fully programmable text processing utility It can build new text processors and batch oriented text manipulation routines Its main value for Starlink users is its close emulation of EDT PSMERGE Merge PostScript files Merges one or more EPSFs into a single PostScript file An EPSF Encapsulated PostScript File is a PostScript file structured so that it can be incorporated or included into another PostScript file so that for example a diagram created with a graphics application can be inserted into a text document created with a word processor Input files can be individually rotated scaled and shifted Output files can be either EPSF or normal PostScript suitable for a printer This allows e Pictures created by different applications to be overlayed e Multiple pictures to be pasted onto a single

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