Installing CYGWIN from the cd

In the example above the cd is in drive G:, and clicking it reveals
the cd contents.

Double-click the "Setup" item.

The introductory dialog will appear.

Click "Next"

The default option in the this dialog is "Install from Internet", but
you want to install from the cd , so change the selection to
"Install from local Directory", then click "Next".

This dialog selects where on your disk(s) to install all the CYGWIN
software. It requires about 500Mb, so make sure you choose a disk
with enough free space. Create a directory called "cygwin" on that disk,
and select it in this dialog.

Then click "Next"

In this dialog click the "Browse" button, and use the widget to select
the folder named "release" on the cygwin cd.

Then click "Next".

This dialog show the packages which will installed, just click "Next".

Clicking on "Misc" in the "Select Packages" results in a long list of
everything which will be installed. If you are low on disk space,
this is the place where you can deselect items you don't need.

A graphic showing the packages installation progress then
appears. The installation will take 15-20 minutes depending
upon your computer. Once installation is complete the
next dialog appears. Choose whether you want desktop icons and menu
entries, and then click "Next"

The "Setup" wizard on the cd can be used to update your cygwin installation
in the future. You can also visit the CYGWIN website (http://www.cygwin.com)
to download comprehensive documentation and new packages.

Extras

Install KDE

Answer the installer questions (defaults are usually correct), and
complete the installation. Once completed there will be 2 KDE icons
on the desktop.

If there are additional "setup-kde-3.1.1-b1-u?.exe" files on the cdrom
then double-click each one in numerical order. These small installers
apply the available bug-fix/patches to the KDE environment.

Once any patches have been installed, Double-click the "Start KDE (minimal)"
icon to start KDE. After a short interval whilst KDE runs its first
time initialization, the desktop window will appear.

Click on the Konsole icon on the taskbar at the bottom of the window.

This opens a terminal window form which you can invoke the rest of
the installation programs. The "df" command illustrated lists the
available partitions , along with their free space.

The large "K" icon at the left hand side of the taskbar acts like
the "Start" menu in windows, providing a menu of installed programs.

Install KStars

Once installation is complete, open the KDE desktop window and
click in the Konsole/Terminal window to make it the current focus
Then type

	kstars &

to start the KStars KDE desktop planetarium.

GNUWIN

The packages included are

• Apache - Fully featured webserver
• gnuplot - Scientific plotting package
• octave - Scientific data processing
• Python - General purpose scripting language
• R - Statistics package
• SciTE - Text editor
• gimp - Powerfull photo-editing, drawing
• MySQL - Database
• povray - Raytracing package
• qcad - CAD package
• scilab - Scientific data processing
• tightvnc - Remote desktop access
• wxPython - Graphics widgets for Python

Installing Open Source Astronomy packages

The Open Source Astronomy installation assistant is a graphical
user interface which let you browse the selection of packages
available on each cd. It runs under the CYGWIN environment.

Insert cd1 into your cdrom drive and then either

• Start the KDE desktop and open a Konsole window
• Start a CYGWIN shell using the desktop icon

  Now use the "df" command to list the available drives. The output
  will look something like this....

  

  In this case the cd drive is located at /cygdrive/g.

  cd to the cd drives root directory using a command such as
  

  	cd /cygdrive/g
  

  and then start the GUI by typing

  	./autorun
  

  A brief identification window will appear

  

  The first time you run the installation assistant, a small
  disk selection window will appear.

  

  Use this to choose which
  disk to install the Open Source Astronomy packages on. Note
  that installing all the packages will require 4Gb+ so make sure
  you select a disk with plenty of free space. This installer will
  create a link from your selected filesystem to /opt/astro in the
  CYGWIN disectory hierarchy.

  Once a base for the installations has been selected the main
  installation assistant window will appear.

  

  In this snapshot we see the GUI listing the packages
  for cd1. We have scrolled down to the opensourceastro-base
  package which is autoselected along with the opensourceastro-library
  package. It is suggested that you install these two packages
  first, and then browse the library to find out about the other
  packages. If you simply click on "Install selected" these two
  packages will be installed.

  ---

  Package specific information

  aa56

  Computes the orbital positions of planetary bodies

  Version : 5.4
  Author(s) : Stephen L. Moshier (moshier@na-net.ornl.gov)
  License : Free
  Website : http://www.moshier.net/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 451.62 Kb

  Summary

  This program computes the orbital positions of planetary bodies and performs rigorous coordinate reductions to apparent geocentric and topocentric place (local altitude and azimuth). It also reduces star catalogue positions given in either the FK4 or FK5 system. Most of the algorithms employed are from The Astronomical Almanac (AA) published by the U.S. Government Printing Office.

  ---

  accrete

  Accrete is a physical simulation of solar system planet formation

  Version : 1.0
  Author(s) : Chuck Swiger (chuck@pkix.net), Joe Nowakowski.
  License : Free
  Website : http://sourceforge.net/projects/accrete
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 87.75 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startaccrete
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Summary

  Accrete is a physical simulation of solar system planet formation, originally published to Usenet-- probably comp.sources.unix-- in 1991 by Joe Nowakowski. This software is in the public domain.

  This simulation works by modelling a dust cloud around a Sun-like star, injecting a series of masses which collect dust, and form planets. The simulation then determines what the planetary environments will be like in terms of temperature, atmospheric composition, and other factors. The system description is saved to a file named "New.System".

  ---

  adccdrom

  IRAF Tools for Accessing the ADC CDROM

  Version : 1.0
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.52 Mb

  This package requires prior installation of iraf

  Summary

  IRAF Tools for Accessing the ADC CDROM

  An IRAF external package for accessing many of the 114 catalogs in Volume I Astronomical Data Center (ADC) CD-ROM collection has been developed. The tasks are specific to the text file format disk. There are two tasks, one for selecting and printing data from tabular catalogs and one for extracting spectra to 1D IRAF spectral images. Below are excerpts from the help pages.

  ---

  apmcat

  

  APMCAT gets data from the APM catalogues server.

  Version : 1.0
  Author(s) : T. McGlynn Goddard Space Flight Center
  License : GSFC
  Website : http://www.ast.cam.ac.uk/~apmcat
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 40.06 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startapmcat
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  This is a standalone program which makes a remote request of the APM catalogues system based on command line arguments and returns either a list or a postscript finding chart on standard output.

  Usage: apmcat ra dec [optional arguments]

  where the optional arguments are of the form keyword=value. Valid arguments include:

  survey=poss1 [or ukst survey] box=5 [box size in arcmins] equinox=b1950 [or j2000] numbers=n [numbers on plot ? n/y] ps=image.ps [name of postscript image] list=image.lis [alternatively name of list file] email=null [email address]

  The above values are the defaults. The default is to return a postscript chart with the name image.ps Please specify either a list or a postscript image.

  Examples:

  apmcat "00 40 00.0 11 41 00" survey=poss1 ps=chart.ps apmcat "10 31 21.3 -5 10 23" survey=ukst list=chart.list

  Notes: If a field is absent from the catalogues you will be returned an appropriate message.

  ---

  ared

  Arcon data reduction

  Version : 1.0
  Author(s) : various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 3.69 Mb

  This package requires prior installation of iraf

  Summary

  This directory contains the code for the reduction of ARCON data. So far the package includes the QUAD package and the IRLINCOR task.

  ---

  ascfit

  Automatic Stellar Coordinate fitting

  Version : 1.2
  Author(s) : Peter Siegbjørn Jørgensen (psj@oersted.dtu.dk) , Andrew Pickles (pickles@ifa.hawaii.edu)
  License : GPL
  Website : http://www.ifa.hawaii.edu/users/pickles
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 491.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startascfit
  
       

  Screenshots

  

  Summary

  ascfit (Automatic Stellar Coordinate fitting) comprises a GNU bash script "ascfit" which calls a collection of C programs, all of which can be run individually. adds WCS coordinates to single or multiple files depending on whether is complete, or the root of multiple files. Type "ascfit" with no arguments for usage and list of options.

  The core program "starfit" matches stars (triangle fitting) between two lists: "asc_sextr.cat" is generated by "s_extractor" searching the FITS image, and "asc_ref.cat" is generated by "crect" searching the USNO-A2 catalog, or by "msqbin" searching a compressed version of the 2MASS catalog. Most computational time is spent in sextractor; starfit should work with image catalogs produced by other means if given in the right format.

  EXAMPLES --------

  Usage: ascfit fitsfile [-sw value]

  eg: ascfit ccd.030 - will fit one file

  eg: ascfit ccd.03 - will expand list & fit ccd.030-039

  eg: ascfit ccd.0 - will expand list & fit ccd.000-099

  Example: ascfit ccd.030 ccd.030:15h08:00.30+0.227X-0.0011Y -14d49:28.5-0.220Y- 0.0007X: 67/96/92*,0.40"RMS

  file:RA as f(X/Y) DEC as f(X/Y): Stars fitted/ found in image/catalog, RMS error (arcsec)

  ascfit himg.fits -ir -scale 0.3 (specify scale for infrared image) himg.fits:03h46:49.45-0.303X-0.0037Y +23d46:44.5+0.277Y-0.0029X: 9/10/22*,0.12"RMS

  ascfit aten.230 -roff 140 -doff 140 - fit 8 images from UH8K

  (pointing center is offset from mosaiic center)

  ---

  astcatx

  Astronomical Catalog and Surveys Access Package

  Version : 2004.02
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.64 Mb

  This package requires prior installation of iraf

  Summary

  The astcat package is a set of tasks for extracting astrometric and photometric calibration data from remote or local catalogs and filtering the catalog data, and for extracting FITS images from remote or local surveys and regularizing the header keywords in the extracted images. There is also a task for selecting images which contain catalog objects and locating the catalog objects in the image.

  The astcatx tasks are designed as a front end for the standard astrometric and photometric calibrations tasks and for use in automated pipelines where access to astrometric and photometric catalog data is often an important part of the reduction process.

  Astcat is a standard part of the IRAF 2.12 release. Astcatx should only be installed if there are no immediate plans to upgrade to IRAF 2.12, or in order to pick up any post 2.12 release bugs fixes.

  The current contents of the ASTCATX package are

  asttest - Run basic tests on the astcat package aclist - List the supported astrometric catalogs agetcat - Extract astrometry files from astrometric catalogs afiltcat - Filter astrometry files derived from astrometric catalogs adumpcat - Catalog access debugging task

  aslist - List the supported image surveys agetim - Extract FITS images from image surveys ahedit - Initialize the image wcs and set standard keywords aimfind - Select images containing catalog objects adumpim - Image survey access debugging task

  aregpars - Default region parameter set acatpars - Default astrometry file format parameter set afiltpars - Default astrometry file filtering parameters aimpars - Default image data parameters awcspars - Default image wcs parameters

  help ccsystems - Describe the supported celestial coordinate systems help catalogs - Describe the astrometric catalog configuration file help surveys - Describe the image surveys configuation file help afiles - Describe the standard astrometry file format

  ---

  astrolabe

  Astrolabe is a collection of subroutines and applications for calculating the positions of the sun, moon, planets and other celestial objects

  Version : 0.4
  Author(s) : Bill McClain (wmcclain@salamander.com)
  License : GPL
  Website : http://sourceforge.net/projects/astrolabe
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 855.70 Kb

  This package requires prior installation of python

  Summary

  Astrolabe is a collection of subroutines and applications for calculating the positions of the sun, moon, planets and other celestial objects. The emphasis is on high accuracy over a several thousand year time span. Note that the techniques used are overkill for most calendar applications. See the FAQ, Astronomical Calculations for the Amateur for pointers to other methods which are both faster and smaller in terms of code bulk.

  The subroutine library attempts to (someday) implement all the techniques described in Astronomical Algorithms, second edition 1998, by Jean Meeus, Willmann-Bell, Inc. For an alternative open-source implementation of Meeus in ANSI C, look here.

  Currently there are no graphical applications apart from some demo CGI interfaces. I may add graphics in the future, but I don't intend to create a planetarium program. For a very nice open-source example of such running on Unix/Linux systems, see XEphem. Graphical software for many platforms are linked at Planetarium Software.

  ---

  AstroMD

  

  A Multi Dimensional visualization and analysis toolkit for astrophysics

  Version : 3.1
  Author(s) : Fulvio Buonomo (buonomo@cineca.it)
  License : Free
  Website : http://www.cineca.it/astromd/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 29.18 Mb

  Screenshots

  

  Summary

  AstroMD is a visualization package built in collaboration by CINECA (Bologna - Italy) and the Astrophysical Observatory of Catania (Catania - Italy), with the specific object of supporting visualization and analysis of astrophysical three dimensional structures. Astrophysical data, in fact, have peculiarities that make them different from data coming from any other kind of simulation or experiment. Therefore they require a specific treatment. These characteristics can be summarized as follows:

  - several different physical species are treated. For example, cosmological simulations consider both baryonic matter and dark matter. Dark matter is usually described by N-body algorithms, while baryons have a fluid-dynamics description (either Eulerian or Lagrangian). Further components, like stars or different chemical species, can be introduced and followed in a specific way. These different species requires different types of visualization. Dark matter needs particles position or velocity rendering while baryons require mesh based visualization. Furthermore particle associated quatities, like the mass density or the gravitational potential, require their calculation and visualization on a mesh.

  - Simulated structures have a fully three-dimensional distribution. Therefore it is necessar to have a clear 3D representation and efficient and fast tools of navigation, selection, zoom and the possibilty of improving the resolution and the accuracy of calculations in specific, user-selected, regions

  - Evolution can change dramatically the properties of the simulated objects and the information that can be retrived, therefore it is important to control efficently sequences of time-frames.

  Moreover, in order to build a widely used product it was necessar to use a low cost software portable on a number of different platforms. We have chosen to use the Visualization Toolkit (VTK) by Kitware. VTK is an open source, freely available software system for 3D computer graphics, image processing, and visualization. It includes a C++ class library and several interpreted interface layers. VTK has been ported on nearly every Unix-based platform (e.g. Linux or IRIX) and PC's (Windows NT and Windows 98). The design and implementation of the library has been strongly influenced by object-oriented principles. The graphics model in VTK is at a higher level of abstraction than rendering libraries like OpenGL or PEX. This means it is much easier to create useful graphics and visualization applications. In VTK applications can be written directly in C++, Tcl, Java, or Python. Using these languages it is possible to build powerful, fast and portable applications. VTK supports a wide variety of visualization algorithms including scalar, vector, tensor, texture, and volumetric methods and advanced modeling techniques. It supports stereographic rendering and can be used for virtual realty visualization. Furthermore, being easily extensible, the system allows ad hoc implementation of specific modules.

  All the features described above are integrated in the AstroMD package. Furthermore efficent manipulation and analysis tools, like smoothing of the particle masses on a mesh or calculation of the power spectrum and correlation functions, are parts of the basic functionalities. AstroMD has also stereographic rendering capabilities, which makes it usable for immersive visualization (presently implemented at the Virtual Theater of CINECA). This completes and improve its capabilities in the representation of three dimensional data set.

  ---

  astroperl

  astroperl is a collection of perl routines for astronomical catalog access

  Version : 1.0
  Author(s) : Alasdair Allan (aa@astro.ex.ac.uk)
  License : GPL
  Website : http://www.estar.org.uk/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 2.81 Mb

  This package requires prior installation of perl

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startastroperl
  
       

  Summary

  astroperl is a collection of perl routines for astronomical catalog access

  Make sure that you have Perl installed and then run /opt/astro/astroperl/buildall.sh to complete the installation.

  ---

  avsomat

  A small utility to automate the reduction of variable stars,

  Version : 0.4
  Author(s) : Alexandru (radu@corlan.net)
  License : GPL
  Website : http://astro.corlan.net/avsomat
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 250.64 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startavsomat
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Summary

  This is avsomat, a small utility to automate the reduction of variable stars, currently for the purpose of reporting them to AAVSO (www.aavso.org).

  ---

  BCR

  

  Cooperative Data Sharing library

  Version : 0.7.1
  Author(s) : feedback@elepar.com
  License : Elepar
  Website : http://www.elepar.com/CDS/product.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1.42 Mb

  Summary

  Cooperative Data Sharing (CDS) is a fast, flexible, and free* API used to write portable programs for clusters, parallel computers, peer-to-peer, and computational grids.

  o CDS can often deliver higher network bandwidth, higher memory- based bandwidth, and lower latency to the application than message passing interfaces

  o CDS supports several programming styles (including demand-driven, real-time, shared-memory, and message-passing) all with a single simple API

  o CDS uses the programmer's expressed intentions to help hide latency and minimize copying AT THE SAME TIME, thus making programs more portable beteen high-latency, low-latency, and hybrid (e.g. cluster of SMP) environments than they would be with message-passing or shared-memory APIs.

  BCR is Elepar's newly-available C-based CDS offering, a simplified dialect similar to that developed earlier at NASA Ames Research Center. Free information, including some performance data and a "Principles of Operation" white paper, is available without registration at: http://www.elepar.com/CDS/product.html

  ---

  cdc

  Cartes de ciel is a skychart program

  Version : 2.76
  Author(s) : Patrick Chevalley
  License : GPL
  Website : http://www.stargazing.net/astropc/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 9.34 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcdc
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  This program enables you to draw sky charts, making use of the data in 16 catalogs of stars and nebulae. In addition the position of planets, asteroids and comets are shown.

  The purpose of this program is to prepare different sky maps for a particular observation. A large number of parameters help you to choose specifically or automatically which catalogs to use, the colour and the dimension of stars and nebulae, the representation of planets, the display of labels and coordinate grids, the superposition of pictures, the condition of visibility and more. All these features make this celestial atlas more complete than a conventional planetarium.

  ---

  celestia

  

  Solar System visualization

  Version : 1.3.2
  Author(s) : Chris Laurel,Clint Weisbrod,Fridger Schrempp,Christophe Teyssier,Deon Ramsey (UNIX installer, Gtk interface),Bob Ippolito (Mac OS X version),Christopher ANDRE (Eclipse finder),Colin Walters (endianness fixes),Grant Hutchison (solarsys.ssc guru),James Holmes
  License : GPL
  Website : http://www.shatters.net/celestia/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 35.00 Mb

  This package has it's own installer

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcelestia
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Summary

  Celestia will start up in a window, and if everything is working correctly, you'll see Jupiter's moon Io in front of a field of stars. In the left corner is a welcome message and some information about your target (Io), your speed, and the current time (Universal Time, so it'll probably be a few hours off from your computer's clock.) Right drag the mouse to orbit Io and you should see Jupiter and some familiar constellations. Left dragging the mouse changes your orientation too, but the camera rotates about its center instead of rotating around Io. Rolling the mouse wheel will change your distance to the space station--you can move light years away, then roll the wheel in the opposite direction to get back to your starting location. If your mouse lacks a wheel, you can use the Home and End keys instead.

  ---

  cfitsio

  C library for read/write FITS format files

  Version : 2.4.10
  Author(s) : William D. Pence (pence@tetra.gsfc.nasa.gov)
  License : cfitsio
  Website : http://heasarc.gsfc.nasa.gov/docs/software/fitsio/fitsio.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 10.69 Mb

  The following printable documents will be installed :

  • /opt/astro/doc/cfitsio.ps

  Summary

  CFITSIO is a library of ANSI C routines for reading and writing FITS format data files. A set of Fortran-callable wrapper routines are also included for the convenience of Fortran programmers. This README file gives a brief summary of how to build and test CFITSIO, but the CFITSIO User's Guide, found in the files cfitsio.doc (plain text), cfitsio.tex (LaTeX source file), or cfitsio.ps (postscript format), should be referenced for the latest and most complete information.

  ---

  CHIANTI

  A Database for Astrophysical Emission Line Spectroscopy

  Version : 4.2
  Author(s) : Enrico Landi (landi@poppeo.nrl.navy.mil)
  License : Free
  Website : http://www.damtp.cam.ac.uk/user/astro/chianti/chianti.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 10.48 Mb

  Screenshots

  

  Summary

  The continued development of the CHIANTI database is dependent on continued funding which is generally available if we can demonstrate that the CHIANTI database is of use to astrophysical research. If you find CHIANTI useful, it would be helpful to us if you could email a short description (a single sentence is fine) of how you employ CHIANTI.

  We are also aware that CHIANTI data is being ingested into other databases and this is fine. However, it would be useful for us if some acknowledgement of this use of CHIANTI can be given, such as in publications etc.

  ---

  cloudy

  Simulate emission line regions

  Version : 96
  Author(s) : Gary J. Ferland. (gary@cloud9.pa.uky.edu)
  License : cloudy
  Website : http://www.nublado.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 36.85 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcloudy
  
       

  Screenshots

  

  

  Summary

  Cloudy is designed to simulate emission line regions ranging from the intergalactic medium to the Broad Line regions of Quasars. It can be used to predict either the structure or the observed spectrum from such regions.

  ---

  cmbfast

  

  A microwave anisotropy code

  Version : 3.0
  Author(s) : Uros Seljak (useljak@cfa.harvard.edu) , Matias Zaldarriaga (matiasz@arcturus.mit.edu)
  License : cmbfast
  Website : http://www.cmbfast.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1021.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcmbfast
  
       

  Screenshots

  

  Summary

  CMBFAST is the most extensively used code for computing cosmic microwave background anisotropy, polarization and matter power spectra. This package contains cosmological linear perturbation theory code to compute the evolution of various cosmological matter and radiation components, both today and at high redshift. The code has been tested over a wide range of cosmological parameters. We are continuously testing and updating the code based on suggestions from the cosmological community.

  ---

  color

  IRAF Tools for Color Image Display

  Version : 4
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.30 Mb

  Screenshots

  

  Summary

  A prototype IRAF color image display package, COLOR, is now available. Currently this package provides conversion of 3 bandpass IRAF images to a Sun 24-bit RGB rasterfile format, a 24-bit to 8-bit compression algorithm and Floyd-Steinberg dithering, and an RGB 8-bit pixel dithering algorithm. The Sun rasterfiles are displayed using non-IRAF tools and the others use only IRAF images and SAOimage or IMTOOL. These tasks are usable with the currently common 8-bit color workstations and are provided for those users which don't have more capable hardware such as 24-bit workstations, IIS displays, and 24-bit addon cards. Addtional functionality will be added to the COLOR package in time.

  The task RGBSUN takes three input IRAF images and produces a 24-bit Sun rasterfile. Though this file type was developed by Sun Microsystems it is a relatively simple format which may useful on other machines having software designed to use it. The color image may be displayed with a variety of non-IRAF tools such as XV (a very powerful and generic viewer for X-window systems), XLOADIMAGE (another X-window display tool), SCREENLOAD (a simple displayer on Sun computers), and SNAPSHOT (an Open-Look tool). Also some color printers can be used with this format such as a Shinko color printer.

  ---

  cora

  line fitting tool designed for emission line spectra with low count numbers

  Version : 3.2
  Author(s) : Jan-Uwe Ness - (jness@hs.uni-hamburg.de) , Rainer Wichmann - (rwichmann@hs.uni-hamburg.de)
  License : GPL
  Website : http://www.hs.uni-hamburg.de/DE/Ins/Per/Ness/Cora/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 8.11 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcora
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/cora.ps

  Summary

  The cora line fitting package consists of seven programs. Help on command line options can be obtained with the option -h.

  cora_fit - this is the main fitting program. It can be used as a standalone command-line application, or it can be used from the graphical user interface. cora_fit requires a parameter file, and a spectrum. cora - this is the optional graphical user interface, which acts as a graphical front-end to cora_fit, and significantly facilitates the use of the latter. Basically, with cora you can: browse the spectrum and interactively choose lines to fit interactively set all parameters required by cora_fit, easily switch between different parameter settings, call cora_fit with the currently selected parameter settings obtain updated parameters and graphical output (i.e. plots). cora_inp - this is a helper application that writes a parameter file (see below) that is specifically adapted to a particular spectrum. This program is useful if you do not use the GUI. It is also used by the GUI itself. cora_spec - a small program to create an artificial spectrum with a few lines; for testing purposes. cora_rgs - converts a fits data file in the format returned by the XMM SAS task rgsproc into a CORA file cora_tex - converts the log file into a LATEX table cora_flux - creates a data file in the CORA format with fluxes using a given file with effective areas (two columns: wavelengths, area in cm) and exposure time. WARNING: Not recommended for obtaining line fluxes with CORA.

  In addition, two scripts are provided with the package.

  cora_setup.ksh and cora_setup.tcsh can be modified to your system and executed in order to set environment variables. This customizes the installation. cora_rgspipe.sh will reduce XMM-RGS data using the SAS software. The user has to modify environment variables indicating where SAS is installed and where the data to be processed are located.

  ---

  cosmics

  

  Cosmological Initial Conditions and Microwave Anisotropy Codes

  Version : 1.0
  Author(s) : Edmund Bertschinger (bertschinger@mit.edu) and Paul Bode (pbode@mit.edu)
  License : cosmics
  Website : http://arcturus.mit.edu/cosmics/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 3.64 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startcosmics
  
       

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/cosmics.ps

  Summary

  COSMICS is a package of programs for computing cosmological initial conditions for nonlinear structure formation codes as well as microwave background anisotropy. For detailed information please read cosmics.tex (cosmics.ps).

  ---

  crutil

  COSMIC RAY REMOVAL UTILITY PACKAGE

  Version : 1.4
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.81 Mb

  Summary

  The cosmic ray package provides tools for identifying and removing cosmic rays in images. The tasks are:

  cosmicrays - Remove cosmic rays using flux ratio algorithm craverage - Detect CRs against average and avoid objects crcombine - Combine multiple exposures to eliminate cosmic rays credit - Interactively edit cosmic rays using an image display crfix - Fix cosmic rays in images using cosmic ray masks crgrow - Grow cosmic rays in cosmic ray masks crmedian - Detect and replace cosmic rays with median filter crnebula - Detect and replace cosmic rays in nebular data

  The best way to remove cosmic rays is using multiple exposures of the same field. When this is done the task crcombine is used to combine the exposures into a final single image with cosmic rays removed. The images are scaled (if necessary) to a common data level either by multiplicative scaling, an additive background offset, or some combination of both. Cosmic rays are then found as pixels which differ by some statistical amount away for the average or median of the data.

  A median is the simplest way to remove cosmic rays. This is an option with crcombine. But this does not make optimal use of the data. An average of the pixels remaining after some rejection operation is better. If the noise characteristics of the data can be described by a gain and read noise then cosmic rays can be optimally rejected using the "crreject" algorithm. This works on two or more images. There are a number of other rejection algorithms which can be used as described in the task help.

  The rest of the tasks in the package are used when only a single exposure is available. These include interactive editing with credit. The replacement algorithms in this task may also be used non-interactively if you have a list of pixel coordinates as input. Other tasks automatically identifying pixels which are significantly higher than surrounding pixels.

  ---

  ctio

  IRAF Tools for CTIO telescope data

  Version : 4
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 10.29 Mb

  Summary

  ctio.amplot - Plot critical airmass versus UT ctio.apropos - List all the tasks related with a given subject ctio.bin2iraf - Convert binary files into IRAF images ctio.bitstat - Perform bit statistics of image frames ctio.chpixfile - Change pixel file name in image headers ctio.colselect - Extract selected columns from a list. ctio.compairmass - Compute air mass ctio.compression.fitsread - Create an IRAF image from a compressed FITS file. ctio.compression.fitswrite - Create a compressed FITS file from an IRAF image. ctio.compression.imcompress - Compress IRAF image pixel file ctio.compression.imuncompress - Uncompress IRAF image pixel files ctio.coords - Compute celestial coordinates ctio.cureval - Evaluate the fit computed by curfit. ctio.dfits - display FITS file headers ctio.eqwidths - Equivalent widths ctio.ezimtool - Call IRAF tasks interactivelly from image cursor mode ctio.fabry.avgvel - determine velocity by averaging pixels ctio.fabry.findsky - determine the sky levels at each band of an image cube ctio.fabry.fitring - compute the dispersion solution using the ring parameters ctio.fabry.fpspec - Plot pixel value for a set of images ctio.fabry.icntr - determine centers for a star in a set of images ctio.fabry.icur - get image cursor coordinates ctio.fabry.intvel - determine velocity by averaging pixels interactively ctio.fabry.mkcube - combine a group of 2D images into an image cube ctio.fabry.mkshift - generate a script file to shift many images to a reference image ctio.fabry.normalize - add normalization factors to the cube image header ctio.fabry.ringpars - determine the parameters of the calibration rings ctio.fabry.velocity - construct velocity maps from the fabry-perot image cube ctio.fabry.zeropt - determine the zero point in wavelength for each band in the cube ctio.fft1d - One dimensional Fast Fourier Transform ctio.filecalc - File calculator ctio.findfiles - Find files ctio.fitrad - Fit a function to circular image subrasters ctio.fixtail - Fix last image lines or columns. ctio.focus - Compute telescope focus ctio.gki2cad - Convert GKI metacode files into autoCAD DXF files ctio.gkitocad - Convert GKI metacode files into autoCAD DXF files ctio.growthcurve - Correct magnitudes using the growth curve for them ctio.imcreate - Create an image. ctio.imextract - Extract a list of image sections from an image ctio.immatch - Match one or two dimensional images ctio.imsort - Sort images by header parameter values ctio.imspace - determine disk space used by IRAF images. ctio.imtest - test image headers an pixel files ctio.iraf2bin - Convert IRAF images into binary files ctio.irlincor - Correct IR imager frames for non-linearity. ctio.irproc - Sky substract, transpose, and mosaic IR imager frames ctio.lambda - Print pixel values and wavelengths ctio.magavg - Average output from magband for a single object ctio.magband - Compute the average magnitude for a list of bandpasses ctio.mapkeyword - Replace image header keyword values with other values. ctio.midut - Compute UT for midpoint of observation ctio.mjoin - Join lines in text files by matching them ctio.mkapropos - make the apropos database ctio.pixselect - List pixel values within a certain range ctio.spcombine - Combine spectra interactively ctio.sphot - star photometry ctio.statspec - Compute statistical error spectra from object and sky spectra. ctio.wairmass - Compute weighted airmass

  ---

  cutout

  extract FITS cutout images from a survey using world coordinate information

  Version : 2000.12
  Author(s) : Various
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.71 Mb

  This package requires prior installation of iraf

  Summary

  The CUTOUT task extracts FITS cutout images from a list of survey images input and writes the output images to output. The survey images are described in the database file dbfile which is created or updated when CUTOUT is run with opmode ="scan".

  The database file contains a description of every survey image. At present this description includes the name of the image, the filter id, the right ascension and declination of the image center in hours and degrees, the coordinate system of the image, the size of the image in pixels, the image projection type, the coordinates of the projection reference point in degrees and degrees, the coordinates of the reference point in pixels and pixels, the x and y image scale in "/pixel, the x and y axes rotation in degrees, and the image extent in ra and dec in degrees and degrees. The database filter ids are read from the image keyword defined by the kwfilter parameter.

  A single cutout region is specified by the ra, dec, rawidth, decwidth, fcsystem, and filters parameters. Multiple cutout regions may be defined in the regions file regions which has the following format.

  ra1 dec1 ra/xwidth1 [dec/ywidth1 [fcsystem1 [filters1]]] ra2 dec2 ra/xwidth2 [dec/ywidth2 [fcsystem2 [filters2]]] ... raN decN ra/xwidthN [dec/ywidthN [fcsystemN [filtersN]]]

  The right ascension and declination values define the center of the extraction region and must be hours and degrees. The right ascension and declination widths must be in arcminutes. The x and y widths must be in pixels. X and Y pixel width values are distinguished from ra and dec width values by a trailing 'p' character. The decwidth / ywidth, coordinate system, and filter id values are optional, and default to the value of rawidth, and the values of the fcsystem and filters parameters respectively.

  If opmode = "list" then the names, offsets from the extraction region center in arcminutes or pixels, and filter ids are printed on the screen.

  If opmode = "cutout" the FITS image cutouts output are created, one cutout for each filter in filters. If cutmode = "largest" the cutout is extracted from the survey image which has the largest overlap with the extraction region. If cutmode is "collage" then the cutouts are created from all the images which overlap the extraction regions, with images with larger overlap regions taking precedence over those with smaller overlap regions. The survey images are assumed to have a common projection system and cutouts are aligned to the nearest pixel. Undefined pixels in the cutouts are assigned the value blank. If trim = yes then undefined pixels around the edges of the cutout images are removed.

  By default the cutout image names are of the form "imroot_coords_filter.fits" where imroot is the values of the parameter imroot, coords is an IAU-like coordinate designation, and filter is the filter id. Users can also specify their own output image names in output. If there are more output images than output image names then default output image names are constructed for the "extra" images.

  ---

  deitab

  DEIMOS TABLE FORMAT TOOLS

  Version : 1.1
  Author(s) : Various
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 2.04 Mb

  This package requires prior installation of iraf

  Summary

  The DEITAB external package is used to convert Deimos pipeline reduced 2D table format to multiextension image format. It also allows applying the 2D pipeline reduced dispersion solution to extracted 1D spectra.

  ---

  Dexter

  

  Dexter is a little java applet that is used by the ADS to let users extract data from figures on scanned images

  Version : 0.4
  Author(s) : (msdemlei@tucana.harvard.edu)
  License : GPL
  Website : http://dexter.sourceforge.net/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 231.00 Kb

  This package requires Java installation

  Summary

  Dexter is a little java applet that is used by the ADS (http://adswww.harvard.edu) to let users extract data from figures on scanned images. As such, it is rather tightly bound to the ADS through the AppletImageGetter and AppletDataDeliverer classes.

  However, by implementing different classes implementing the ImageGetter and DataDeliverer classes, standalone versions can be provided. The PlainImageGetter and PlainDataDeliverer classes show how one would go about doing that with a main program named Debuxter.

  ---

  digiphotx

  Photometry package for IRAF

  Version : 1.0
  Author(s) : davis@noao.edu
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 22.45 Mb

  This package requires prior installation of IRAF

  Summary

  The IRAF external package, DIGIPHOTX (a new version of the DIGIPHOT package), is being made available prior to its official release in IRAF 2.10.3. DIGIPHOTX contains: 1) a new version of the DAOPHOT package, DAOPHOTX, which is the IRAF implementation of Peter Stetson's DAOPHOT II package, 2) a new curve of growth analysis task in the PHOTCALX package, 3) several new tasks in the PTOOLSX package, 4) minor enhancements and bug fixes to existing tasks that have been discovered since the last exported version.

  The installation instructions that follow describe how to retrieve the DIGIPHOTX archive file, unpack the source files, build, and link the package. If your IRAF system has been stripped of the IRAF libraries (via 'mkpkg stripall') you will not be able to build the DIGIPHOTX executable as described here. You must either reload the required libraries or request a binary distribution of DIGIPHOTX for your operating system.

  Some DIGIPHOTX tasks make use of the STSDAS TABLES package library routines. In order to successfully link all the DIGIPHOTX executables, the STSDAS TABLES package must be installed. A copy of the ST TABLES package retrieval and installation instructions is included at the end of the file.

  ---

  ds9

  

  FITS data viewer

  Version : 2.1
  Author(s) : William Joye , Eric Mandel , Steve Murray , John Roll
  License : GPL
  Website : http://hea-www.harvard.edu/RD/ds9/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 10.63 Mb

  This package has it's own installer

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startds9
  
       

  Screenshots

  

  Summary

  DS9 is the next version of the popular SAOtng display program. It is a Tk/Tcl application which utilizes the SAOTk widget set. It also incorporates the new X Public Access (XPA) mechanism to allow external processes to access and control its data, GUI functions, and algorithms. DS9 supports the direct display of FITS images and binary tables, multiple frame buffers, region cursor manipulation, many scale algorithms and colormaps, and easy communication with external analysis tasks. It is highly configurable and extensible to meet the evolving needs of the astronomical community.

  DS9 supports advanced features such as multiple frame buffers, mosaic images, tiling, blinking, geometric markers, colormap manipulation, scaling, arbitrary zoom, rotation, pan, and a variety of coordinate systems (including Image, Physical, Detector, and WCS). DS9 also supports FTP and HTTP access. The GUI for DS9 is user configurable.

  ---

  dusty

  

  solves the problem of radiation transport in a dusty environment

  Version : 1.0
  Author(s) : Ivezic, Z., Nenkova
  License : dusty
  Website : http://hea-www.harvard.edu/RD/ds9/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 2.86 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startdusty
  
       

  The following printable documents will be installed :

  • /opt/astro/doc/dusty.ps

  Summary

  DUSTY solves the problem of radiation transport in a dusty environment. The code can handle both spherical and planar geometries. The user specifies the properties of the radiation source and dusty region, and the code calculates the dust temperature distribution and the radiation field in it. The solution method is based on a self-consistent equation for the radiative energy density, including dust scattering, absorption and emission, and does not introduce any approximations. The solution is exact to within the specified numerical accuracy.

  DUSTY has built in optical properties for the most common types of astronomical dust and comes with a library for many other grains. It supports various analytical forms for the density distribution, and can perform a full dynamical calculation for radiatively driven winds around AGB stars. The spectral energy distribution of the source can be specified analytically as either Planckian or broken power-law. In addition, arbitrary dust optical properties, density distributions and external radiation can be entered in user supplied files. Furthermore, the wavelength grid can be modified to accommodate spectral features. A single DUSTY run can process an unlimited number of models, with each input set producing a run of optical depths, as specified. The user controls the detail level of the output, which can include both spectral and imaging properties as well as other quantities of interest.

  ---

  eclipse

  

  Astronomical image processing package

  Version : 4.9.0
  Author(s) : Nicolas Devillard and Yves Jung, ESO
  License : ESO
  Website : http://www.eso.org/projects/aot/eclipse/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 12.18 Mb

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/eclipse/ps/devel.ps.gz
  • /opt/astro/doc/eclipse/ps/eug.ps.gz
  • /opt/astro/doc/eclipse/ps/devel.ps.gz
  • /opt/astro/doc/eclipse/ps/eug.ps.gz
  • /opt/astro/doc/gildas/doc/program.ps

  Summary

  eclipse is not IRAF. It is a data reduction engine written in C for portability and speed reasons. From this C library, the ISAAC pipeline team has built a number of Unix commands that are specialized for ISAAC imaging and spectroscopy data processing. We have put into it the know-how of the instrument scientist, and many other contributing people. We do believe that what is actually done by these routines is representative of what most people will want to do with the data.

  You do not "learn" eclipse. The commands are more or less dedicated, one per template. What you have to learn is more or less similar to learning new IRAF commands (what to put in 'epar', how to launch it, learn what is happening in the algorithm, etc.). You do not have to learn a new language, because what it takes is launching a Unix command, not more.

  Now, if you think you have better routines, IRAF scripts or whatever, you will probably be more efficient with tools you have written, you know where they fail and where they work. If you have no clue about ISAAC data reduction or if what you want to do is already performed by an eclipse command, you will be faster and more efficient using it. If you want to do something non-trivial that is not supported in the eclipse commands, or if you need any kind of interactive algorithm, you have no choice but use interactive environments like IRAF. Anyway, past some point you will need something like IRAF to interact with your data to see what is in there. eclipse only covers the first stages of data reduction, until an astronomical knowledge of the data is required to go further. Then it is the astronomer's job and no software can do it in your place.

  ---

  egodata

  Reference data set for the Extreme Ultraviolet Explorer (EUVE) spectrometers.

  Version : 1.17
  Author(s) : Various
  License : Free
  Website : http://heasarc.gsfc.nasa.gov/docs/euve/euve.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 3.02 Mb

  This package requires prior installation of iraf

  Summary

  The reference data set consists of calibration information, in addition to detector characteristics. These data are intended for use with the IRAF layered package EUV, which is also provided by the EUVE program. All files are either simple ASCII texts files, NASA standard FITS files, or IRAF pixel list files. Don't forget to convert the FITS tables to ST tables before using the reference data set.

  This reference data set requires EUV version 1.9 or later.

  ---

  emb

  

  Earth-Moon barycenter calculator

  Version : 1
  Author(s) : Steve Moshier
  License : free
  Website :
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 141.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startemb
  
       

  Summary

  Earth-Moon barycenter calculator

  ---

  eSTAR

  

  The eScience Telescopes for Astronomical Research (eSTAR) Project is a programme to build a prototype robotic telescope network

  Version : 1.x.y
  Author(s) : http://www.estar.org.uk
  License : GPL
  Website : http://www.estar.org.uk
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1.74 Mb

  Summary

  eSTAR Software The eScience Telescopes for Astronomical Research (eSTAR) Project is a programme to build a prototype robotic telescope network, to test computing infrastructure and software which could be used for larger scale projects. The prototype will include telescopes which carry out observing requests sent across the internet and a system which performs rapid reduction of the data. Intelligent agents will then examine the results and, if required, request follow-up observations.

  eSTAR is a joint project between the Astrophysics Research Institute at Liverpool John Moores University, the Astrophysics Rearch Group of the School of Physics at the University of Exeter and the Department of Physics at the University of Liverpool. It is funded as a demonstrator project through the UK's joint Department of Trade and Industry and the Engineering and Physical Sciences Research Council's e-science core programme.

  Work is ongoing on the software front, some of the middleware written by the project that we feel will be generally useful will be distributed to the community under the GNU General Public License (GPL).

  Astro::ADS

  The Astro::ADS module is an object-orientated Perl interface to the Astrophysics Data System (ADS) abstract service. The ADS is a NASA-funded project whose main resource is an Abstract Service, which includes four sets of abstracts: astronomy and astrophysics, instrumentation, physics and geophysics, and Los Alamos preprint server.

  As of November 2001, ADS discontinued support of its own adswww Perl4 based library, in favour of the Astro::ADS module. It is therefore now the official way to access ADS via the Perl language.

  Astro::SIMBAD

  The Astro::SIMBAD module is an object-orientated Perl interface to the SIMBAD astronomical database. SIMBAD provides basic data, cross-identifications and bibliography for astronomical objects outside the solar system.

  Astro::DSS

  The Astro::DSS module is an object-orientated Perl interface to the first and second Digital Sky Surveys at the ESO-ECF online archive. While the first sky survey is 100% complete, the second survey covers 98% of the sky in Red, 45% of the sky in Blue and 27% of the sky in the Infra-red.

  Astro::Corlate

  The Astro::Corlate module is an pseudo-object orientated interface to the Fortran 95 Corlate package. A F95 compiler is needed to compile the module.

  Corlate compares two CLUSTER format catalogue files, one typically being the results of a new observation, and the other a reference catalogue such as the USNO-A2. It returns an array of files with information on any variable objects found during the cross-corelation of the two catalogues. CLUSTER format files can be handled using the Astro::Catalog.

  Astro::Catalog

  A generic catalog object, along with wrappers to allow you to connect to the online Guide Star Catalogue (GSC) and the USNO-A2 catalogue provided by ESO/ST-ECF. The module also allows read/write access to ARK CLUSTER files.

  eSTAR::Globus

  A skeleton module demonstrating how we went about wrapping the Globus API in Perl. Requires that Globus is installed.

  eSTAR::LDAP::Search

  The Globus Perl CoG module Grid::Info::Search, customised for use with the eSTAR project. Requires that Globus is installed.

  eSTAR::RTML

  A module which parses Robotic Telescope Markup Language (RTML) which is the communication protocol used between the agent and the node.

  Intelligent Agent

  The current release includes only the testbed clients for the intelligent agent (IA). The Field Correlation Client (FCC) is the current testbed for the low level and middleware Perl classes and wrappers underpinning the intelligent agent (IA) software.

  ---

  euv

  IRAF Tools for EUV data reduction

  Version : 1.9
  Author(s) : Center for EUV Astrophysics
  License : euv
  Website : http://www.hypography.com/info.cfm/15292.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 19.49 Mb

  This package requires prior installation of iraf

  Summary

  The Extreme Ultraviolet Explorer (EUVE) was a NASA-funded astronomy mission operating in the relatively unexplored extreme ultraviolet (70-760 Å) band. The science payload, which has been designed and built at the Space Sciences Laboratory at the University of California, Berkeley, under the direction of Dr. Roger F. Malina, consists of three grazing incidence scanning telescopes and an extreme ultraviolet (EUV) spectrometer/deep survey instrument. The science payload is attached to a Multi-Mission Modular spacecraft.

  The EUVE mission, which launched on June 7, 1992 on a Delta II rocket from Cape Canaveral, is the culmination of nearly thirty years of effort at the University of California at Berkeley to create the field of EUV Astronomy. EUVE opens up this last unexplored spectral window in astrophysics.

  The first six months of the mission were dedicated to mapping the EUV sky with the scanning telescopes. The mission is now in the Guest Observer phase.

  Contents Previous Next

  ---

  eye

  

  Eye stands for ``Enhance your Extraction'': a software for training SExtractor's retina

  Version : 1.1
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/sextractor/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1.86 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/starteye
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  The following printable documents will be installed :

  • /opt/astro/doc/eye.ps

  Summary

  Eye is a program which generates non-linear image filters using machine learning. The resulting filter can then be loaded in Sextractor.

  ---

  fftw

  

  Fastest Fourier Transform in the West.

  Version : 3.0.1
  Author(s) : M. Frigo and S. G. Johnson,
  License : GPL
  Website : http://www.fftw.org/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 2.30 Mb

  Summary

  FFTW is a comprehensive collection of fast C routines for computing the discrete Fourier transform (DFT) in one or more dimensions, of both real and complex data, and of arbitrary input size. FFTW also includes parallel transforms for both shared- and distributed-memory systems. We assume herein that the reader is already familiar with the properties and uses of the DFT that are relevant to her application. Otherwise, see e.g. The Fast Fourier Transform by E. O. Brigham (Prentice-Hall, Englewood Cliffs, NJ, 1974). Our web page also has links to FFT-related information online.

  FFTW is usually faster (and sometimes much faster) than all other freely-available Fourier transform programs found on the Net. For transforms whose size is a power of two, it compares favorably with the FFT codes in Sun's Performance Library and IBM's ESSL library, which are targeted at specific machines. Moreover, FFTW's performance is portable. Indeed, FFTW is unique in that it automatically adapts itself to your machine, your cache, the size of your memory, the number of registers, and all the other factors that normally make it impossible to optimize a program for more than one machine. An extensive comparison of FFTW's performance with that of other Fourier transform codes has been made. The results are available on the Web at the benchFFT home page.

  In order to use FFTW effectively, you need to understand one basic concept of FFTW's internal structure. FFTW does not used a fixed algorithm for computing the transform, but it can adapt the DFT algorithm to details of the underlying hardware in order to achieve best performance. Hence, the computation of the transform is split into two phases. First, FFTW's planner is called, which "learns" the fastest way to compute the transform on your machine. The planner produces a data structure called a plan that contains this information. Subsequently, the plan is passed to FFTW's executor, along with an array of input data. The executor computes the actual transform, as dictated by the plan. The plan can be reused as many times as needed. In typical high-performance applications, many transforms of the same size are computed, and consequently a relatively-expensive initialization of this sort is acceptable. On the other hand, if you need a single transform of a given size, the one-time cost of the planner becomes significant. For this case, FFTW provides fast planners based on heuristics or on previously computed plans.

  The pattern of planning/execution applies to all four operation modes of FFTW, that is, I) one-dimensional complex transforms (FFTW), II) multi-dimensional complex transforms (FFTWND), III) one-dimensional transforms of real data (RFFTW), IV) multi-dimensional transforms of real data (RFFTWND). Each mode comes with its own planner and executor.

  Besides the automatic performance adaptation performed by the planner, it is also possible for advanced users to customize FFTW for their special needs. As distributed, FFTW works most efficiently for arrays whose size can be factored into small primes (2, 3, 5, and 7), and uses a slower general-purpose routine for other factors. FFTW, however, comes with a code generator that can produce fast C programs for any particular array size you may care about. For example, if you need transforms of size 513 = 19*33, you can customize FFTW to support the factor 19 efficiently.

  FFTW can exploit multiple processors if you have them. FFTW comes with a shared-memory implementation on top of POSIX (and similar) threads, as well as a distributed-memory implementation based on MPI. We also provide an experimental parallel implementation written in Cilk, the superior programming tool of choice for discriminating hackers (Olin Shivers). (See the Cilk home page.)

  ---

  finder

  IRAF catalog search tools

  Version : 2.2
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 4.54 Mb

  This package requires prior installation of iraf

  Summary

  Catalog search tools

  finder.catpars - Catalog description pset for the finder package finder.cdrfits - modified version of strfits finder.disppars - finder package image display parameters finder.dssfinder - TFINDER tailored for Digital Sky Survey images finder.finderlog - generate a text log file from a tfinder table finder.gscfind - search the index of the GSC for regions overlapping a field finder.mkgscindex - unpack a GSC FITS format index into a table finder.mkgsctab - Make a GSC format table from a text coordinate list finder.mkobjtab - convert objects on input to catalog sources on output finder.objlist - print a text listing of TFINDER object coordinate finder.selectpars - pset containing registration source selection criteria finder.tastrom - perform a plate solution given a table of coordinates finder.tfield - extract a field and predict X,Y positions from GSC tables finder.tfinder - search the GSC catalog - predict, center {&} fit coords finder.tpltsol - perform a plate solution given a table of coordinates

  ---

  fitsutil

  IRAF FITS utilities

  Version : Dec99
  Author(s) : Nelson Zarate (zarate@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.72 Mb

  This package requires prior installation of iraf

  Summary

  The MEF interface is a set of routines to manipulate single FITS files or Multiple Extensions FITS files. This interface complies with the FITS standard set by the NOST document.

  ---

  foucault

  

  Foucault Test Image Analyzer

  Version : 1.2
  Author(s) : Dejan Vucinic dvucinic (at) users.sourceforge.net
  License : GPL
  Website : http://prdownloads.sourceforge.net/foucault
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 9.81 Mb

  This package requires Java installation

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startfoucault
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  Foucault Test Image Analyzer. If you are an amateur telescope maker, this software can take the tedium out of measuring the shape of your mirror.

  Traditionally, amateur mirror makers use a Couder screen, nimble fingers and keen eyesight to quantify the results of the Foucault test by finding the exact knife locations where a zone is equally illuminated on the opposite sides of a mirror.

  In this day and age, however, sophisticated illumination detectors (i.e. digital cameras) are inexpensive and readily available, thus eliminating the dependence on a highly subjective illumination comparison with the naked eye. This program, furthermore, eliminates the need for accurate knife position measurement. Simply take a sequence of photos at pre-set knife offsets, which need not be known with great accuracy, and let the software reduce the measurements and fit the theoretical illumination curves to best match the data.

  ---

  ftools

  

  FITS data processing package

  Version : 5.3
  Author(s) : NASA/HEASARC
  License : Free/GPL
  Website : http://heasarc.gsfc.nasa.gov/docs/software/ftools/ftools_menu.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 172.84 Mb

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/lheasoft/src/qdp/manual/split/pages-001.ps.Z
  • /opt/astro/lheasoft/src/qdp/manual/split/pages-026.ps.Z
  • /opt/astro/lheasoft/src/qdp/manual/split/pages-051.ps.Z
  • /opt/astro/lheasoft/src/qdp/manual/split/pages-076.ps.Z

  Summary

  FTOOLS is a collection of utility programs used to create, examine, or modify the contents of FITS data files. There are also user friendly GUI tools which allow interactive browsing of FITS files and provide a more intuitive interface for running the FTOOLS. The FTOOLS package forms the core of the HEASARC software system for reducing and analyzing data in the FITS format.

  Each FTOOLS task is a separate program that performs a single simple operation. The FTOOLS are primarily a Unix based package, although a Windows version was created for version 4.2 (a 5.0 version is in the works). Most of the powerful GUI interfaces run only on Unix, although the core GUI tool, fv, is available for Unix, Windows, and MacOS. Further discussion of supported platforms is available in the FTOOLS FAQ. Scripts are available for combining several FTOOLS to perform complex tasks. All of the core FTOOLS programs share several common design features:

  All are written in ANSI Fortran or C; All use a simple standardized subroutine interface for getting the value of program parameters (e.g., the name of the input FITS file), and; All data I/O is restricted to FITS files via the FITSIO subroutine interface (or to simple ASCII format in certain cases). All scripts are written in Perl5 (although many will work in Perl4). Note: The official Perl5.001 release doesn't work with all ftools scripts (due to a bug in the Perl code). To run ftools perl scripts, you will need "unofficial patchlevel" 5.001m or higher. The GUI tools are written in Tcl/Tk: Currently there are fv (an interactive FITS file browser/editor), flaunch (a powerful GUI interface to the FTOOLS), and xdf (the XTE Data Finder). The FTOOLS distribution contains the source for the Tcl/Tk interpreters that these tools need to run and will build them for you. You do not need to install Tcl or Tk separately on your system.

  These design decisions have resulted in a software package that is exceptionally portable and can be integrated into new environments with a minimum of modification to the source code.

  ---

  funtools

  Funtools, is a minimal buy-in FITS library and utility package from the SAO/HEAD R&D group.

  Version : 1.2.3
  Author(s) : SAO/HEAD (saord@cfa.harvard.edu)
  License : GPL
  Website : http://hea-www.harvard.edu/RD/funtools/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 127.85 Mb

  Screenshots

  

  Summary

  Today's astronomical software systems are sophisticated, powerful, and diverse, but they are not easy to learn or use. Astronomers often struggle with complex analysis tasks to achieve even the simplest meaningful results. Wide-spread NASA data distribution and growing interest in multi-wavelength studies will exacerbate this problem, as astronomers find themselves contending with multiple analysis systems tailored to different wavelengths.

  We therefore have built a suite of easily mastered tools to promote initial quantitative understanding of astronomical data before moving on to more complex traditional analysis systems. Our tools are based on a simplified FITS library that offers essential FITS access without the complexity of existing libraries. We also have built a sophisticated region filtering library (compatible with our SAOtng and IRAF regions) that filters images and tables using boolean operations between geometric shapes, support world coordinates, etc.

  ---

  gadget

  

  A code for collisionless and gas dynamical cosmological simulations

  Version : 1.1
  Author(s) : Volker Springel (vspringel@cfa.harvard.edu) , Naoki Yoshida (naoki@mpa-garching.mpg.de)
  License : GPL
  Website : http://www.mpa-garching.mpg.de/gadget/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 23.32 Mb

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/S-Gadget.ps

  Summary

  In its current implementation, the serial and parallel versions of GADGET (GAlaxies with Dark matter and Gas intEracT1) support collisionless simulations and smoothed particle hydrodynamics on serial or massively parallel computers. While the parallel code required substantial changes in certain parts of the computational algorithms, we have nevertheless tried to keep the structure of the two codes, and their usuage, as similar as possible. In principle, it would be possible to merge the codes into one source, and employ large numbers of compiler directives to generate serial or parallel behaviour as desired. However, we think that would make the code much more opaque, and would compromise one of our objectives, which is to provide a clean, well-documented code that can be easily understood and modified by users. We therefore provide two separate versions of the code, one for serial and one for parallel computations.

  The code can be used for plain Newtonian dynamics, or for cosmological integrations in arbitrary cosmologies, both with or without periodic boundary conditions. The modeling of hydrodynamics is optional. The code is fully adaptive both in space and in time.

  The main reference for numerical and algorithmic aspects of the code is the paper `GADGET: A code for collisionless and gas-dynamical cosmological simulations', Springel, Yoshida & White, 2000, submitted to New Astronomy (see preprint at astro-ph/0003162). In the following, this paper will be frequently referenced, and I recommend reading it before you attempt to use the code.

  Features

  Hierarchical multipole expansion (tree method) for gravitational forces (geometrical oct-tree, Barnes&Hut-style)

  Optional periodic boundary conditions (Ewald summation technique)

  Smoothed particle hydrodynamics with fully adaptive smoothing lengths

  Shear-reduced artificial viscosity

  Individual timesteps of arbitrary size for all particles

  Work-load balancing and dynamic tree updates

  Efficient cell-opening criteria

  Highly efficient integrator in the linear regime of gravitational clustering

  Flexible control of all code options by a free-format parameterfile

  Portable, well documented code, relying only on standard language/communication features

  High raw computational speed and good scalability

  ---

  gax

  

  A user-friendly tool to search, sort, and report galaxy information

  Version : 1.1
  Author(s) : mark anderson (manders1@csc.com)
  License : GPL
  Website : http://sal.kachinatech.com/Z/4/GAX.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 9.38 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startgax
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  First a word about why I wrote this program. I am mainly interested in observing galaxies, as of this writing I have a 15" Tectron Dob, and was wanting something to tell me what might be visible on a given night and to be able to filter the data on other criteria.

  At first I tried some "commercial" software like Deep Sky Planner, Hypersky, and even NED online but they weren't very flexible. I also wanted something free that would run on Linux. So I wrote my own.

  The user interface uses the standard Unix philosophy, lots of command line switches to control program behavior. This resulted in the main search program, Gax, have quite a few switches and it may be daunting at first site. Never fear though, the manual page has examples that let you see some of the possibilities. Also, typing 'gax' gives a short command synopsis.

  If you are using bash then the history feature makes it very easy to try a search, see the results, and then modify the search parameters. Also, piping the output to other utilities is a big plus of GUI-based programs.

  The other feature found lacking in the commercial programs was that their output format was determined by the developer, who apparently has different likes and dislikes than me. Gax was designed so that you can specify what the output format looks like to a great extent. I'm sure that it won't please everyone but I figured that I would put this program out and see what kind of feedback, if any, I received.

  A major goal was for Gax to be fast. Gax has been used on a Toshiba T4400C laptop with a i486DX2/25Mhz CPU, 20MB RAM and 200MB disk (100MB for Linux) and Gax is fast even on it.

  Obviously, the larger the database you have to search the longer it is going to take. Gax has the ability to look through a large database, select certain objects according to your criteria, and create a new database file with only those objects. By creating these subsets, even faster searches are possible.

  The ASCII input file that is used to create the Gax database file contains catalog names from the following catalogs: NGC, IC, Messier, UGC, MCG, ESO, CGCG, Arp, Markarian, VV, PGC

  I got the data from the NASA National Space Sciences Data Center in the Paturel Galaxy Catalog.

  When Gax is compiled, a macro defined in the Makefile specifies which catalog names to keep in the database file. By compiling Gax with fewer catalog names the database file size is further reduced. Out of the box, Gax will maintain names for NGC, IC, and Messier galaxies.

  Gax is not done. Some of the documented features related to time are not yet implemented. These are noted on the manual page. At some point I may get around to it unless someone beats me to it.

  I hope that you find this program useful. If so, or you don't like it, let me know. Comments, Criticisms and Code (C3) welcomed.

  ---

  ggobi

  

  GGobi is a data visualization system for viewing high-dimensional data

  Version : 1.0.4
  Author(s) : GGOBI team (ggobi-help@ggobi.org)
  License : GPL
  Website : http://www.ggobi.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 13.28 Mb

  This package has it's own installer

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startggobi
  
       

  Screenshots

  

  

  The following printable documents will be installed :

  • /opt/astro/doc/ggobi/Embedded.pdf
  • /opt/astro/doc/ggobi/DBMS.pdf
  • /opt/astro/doc/ggobi/RGGobi.pdf
  • /opt/astro/doc/ggobi/XML.pdf
  • /opt/astro/doc/ggobi/manual.pdf
  • /opt/astro/doc/ggobi/plotLayout.html
  • /opt/astro/doc/ggobi-manual.pdf

  Summary

  GGobi is a data visualization system for viewing high-dimensional data and is the next edition of xgobi. It provides a new interface to many of the features of xgobi, built using Gtk, the GIMP toolkit and provides several new features: A new, simpler and more modern interface; Better portability to Microsoft Windows; Direct access from R Perl and Python; New input format using XML; Database (Postgres and MySQL) support; Works as a Gnumeric plugin; Plugin mechanism for providing extended functionality and support for additional input sources and formats. Plugins can be implemented in Java.

  ---

  gmisc

  Miscellaneous Gemini Related Tasks

  Version : 2004.04
  Author(s) : Various
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 6.39 Mb

  This package requires prior installation of iraf

  Summary

  GMISC contains the development versions of those Gemini reduction packages, scripts, and tasks written by the NOAO IRAF group.

  ---

  god

  Gravitational Orbital Dynamics

  Version : 1.0
  Author(s) : Filippo Portera (fportera@oink.dsi.unive.it) , Claudio Rossi (crossi@moo.dsi.unive.it)
  License : GPL
  Website : http://dsi.unive.it
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 291.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startgod
  
       

  Screenshots

  

  Summary

  G.O.D. INSTRUCTIONS

  MENU BAR

  -FILE: SAVE a system to disk, OPEN one previously saved on disk, or EXIT the program

  -NEW: creates a new configuration (see below for more)

  -CONFIGURE: configures the system When you choose this option a new edit window will appear with the current system. The default editor is joe, but you can change it uncommenting the appropriate line in the proc called by the config button command.

  -ZOOM: zooms a region of the space 2D mode: choose the ZOOM menu-bar option, then select the region to zoom by clicking the left mouse button in the top-left corner of the region; move the cursor to the bottom-right corner, then click again. The region selected will be zoomed to fit the window. 3D mode: sorry, still under development HOW TO UNZOOM: press the pause button, then the zoom menu button.

  CONTROL SECTION

  SPINNING CUBE These three scales set the viewpoint. They are active only in 3D mode.

  MODE These buttons select the display mode: 2D or 3D

  SCHEME These buttons choose the numeric scheme used to compute the objects' positions. There are 3 schemes: Prof., sucker and art. The first is the correct one, the others are modifications that generate very interesting drawings.

  PARAMETERS Gravitational const. : sets the gravitational constant dt : time step for numeric integration max acc. : maximum acceleration allowed for the objects

  PALETTE This scale sets the palette of colors to use to draw objects' trajectories

  REW/PLAY/PAUSE buttons The play button starts simulation, or restart it after that the pause button has been pressed; the pause button suspends simulation (e.g., to change some parameters); the rew button "rewinds" the system to its initial configuration.

  DOMAIN Entries to set the integration domain

  TRACK You can choose to track trajectories with a color proportional to the VELOCITY You can choose to track trajectories with a color proportional to the VELOCITY of the object, to use a different color for each OBJECT, or not to track trajectories (NONE -- this is not too much interesting, but allows you to change the viewpoint while the system is running...)

  COLLISION You can choose what have to happen when two objects collide. They may never collide (treated as 0-dimensional points) have an elastic collision (not too realistic, but very funny ! :-).

  SPACE This sets the kind of space where the system runs. It can be a real space (RxR or RxRxR -- depend on the mode selected) or an hipertoroidal space, that is when an object exits the space from one side it will re-enter it by the opposite side.

  ---

  gsc-north

  

  Hubble Guide Star Catalog (north) compressed

  Version : 1.0
  Author(s) : STSCI
  License : Free
  Website : http://www.stsci.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 104.87 Mb

  Summary

  This version of the Guide Star Catalog is a highly compressed version suitable for use with fast search techniques.

  ---

  gsc-south

  

  Hubble Guide Star Catalog (south) compressed

  Version : 1.0
  Author(s) : STSCI
  License : Free
  Website : http://www.stsci.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 132.16 Mb

  Summary

  This version of the Guide Star Catalog is a highly compressed version suitable for use with fast search techniques.

  ---

  gsl

  

  GNU Scientific subroutine library

  Version : 1.6
  Author(s) : Mark Galassi (rosalia@lanl.gov) , Jim Davies (jimmyd@nis.lanl.gov) , James Theiler (jt@nis.lanl.gov) ,Brian Gough (bjg@network-theory.co.uk) , Reid Priedhorsky (rp@lanl.gov) ,Gerard Jungman (jungman@lanl.gov) ,Michael Booth (booth@debian.org), Fabrice Rossi (rossi@ufrmd.dauphine.fr)
  License : GPL
  Website : http://sources.redhat.com/gsl/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 95.21 Mb

  The following printable documents will be installed :

  • /opt/astro/doc/gsl-ref.ps

  Summary

  The GNU Scientific Library (GSL) is a collection of routines for numerical analysis. The routines are written from scratch by the GSL team (see Section Contributors to GSL) in C, and are meant to present a modern Applications Programming Interface (API) for C programmers, while allowing wrappers to be written for very high level languages.

  ---

  guiapps

  IRAF GUIs

  Version : 1
  Author(s) : IRAF team
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 27.66 Mb

  Screenshots

  

  

  Summary

  XHELP -- a GUI browser for the IRAF help system providing navigation through the familiar CL package structure and HTML interface, a search capability, history mechanism, and on-the-fly conversion of help documents to HTML or PostScript.

  xguiphot -- Do aperture photometry on a list of objects through circular, elliptical, rectangular, or polygonal apertures using a GUI

  Spectool -- an interactive one-dimensional spectrum display and analysis tool. It responds to user input through cursor keys, colon commands, mouse buttons, menus, push buttons, and other window-style graphical user interface controls. Its major functions are to display spectra in a graphical format, to modify them, and to perform various analysis operations. The display capabilities provide complete control over the graph format, convenient zoom and panning, graph and spectral line labeling, and overplotting and stacking of multiple spectra. The editing functions include pixel editing, arithmetic operations, smoothing and fitting, and dispersion solutions. Analysis functions include spectral line measures, profile fitting, radial velocity measurements, and statistics.

  ---

  HDF

  

  The HDF software includes I/O libraries and tools for analyzing, visualizing, and converting scientific data

  Version : 4.2r1,5-1.6.4
  Author(s) : HDF help (hdfhelp@ncsa.uiuc.edu)
  License : NCSA
  Website : http://hdf.ncsa.uiuc.edu/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 36.15 Mb

  Summary

  The HDF project involves the development and support of software and file formats for scientific data management. The HDF software includes I/O libraries and tools for analyzing, visualizing, and converting scientific data. The HDF software is developed and supported by NCSA and is freely available. It is used world-wide in many fields, including Environmental Science, Neutron Scattering, Non-Destructive Testing, and Aerospace, to name a few. Scientific projects that use HDF include NASA's HDF-EOS project, and the DOE's Advanced Simulation and Computing Program.

  ---

  hipparcos

  

  Process Hipparcos transit data from CD-ROM

  Version : 1.0
  Author(s) : Lennart Lindegren (lennart@astro.lu.se), Carl Fredrik Quist ( fredrikq@astro.lu.se)
  License : Free
  Website : http://nastol.astro.lu.se/~lennart/TD/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 301.00 Kb

  Summary

  This directory contains two small Fortran programs to process Hipparcos transit data from CD-ROM (which is assumed to be mounted at /cdrom). For more details please see:

  http://nastol.astro.lu.se/~lennart/TD/

  The executables are in /opt/astro/bin and will be automatically in the user path. They are called td2gf and td2uv.

  ---

  ifocas

  IRAF Tools Faint Object Classification

  Version : 3
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 3.08 Mb

  This package requires prior installation of iraf

  Screenshots

  

  

  Summary

  The Faint Object Classification and Analysis System, called FOCAS, is a set of programs for creating and manipulating catalogs of objects from digital astronomical images. The creation of a catalog is accomplished by an automatic threshold detector where the threshold is measured relative to a simultaneously determined background. The manipulation of catalogs includes the separation of merged objects, the measurement of various position, shape, and photometric parameters, the astronomical classification of the objects, and the display and analysis of the catalogs. This paper describes much of the workings of FOCAS with reference to the FOCAS User's Manual.

  ifocas.detect - detect images in a field ifocas.evaluate - evaluate the objects in a catalog ifocas.resolution - fit resolution templates and make a classification ifocas.sky - evaluate and set the local sky for objects in a catalog ifocas.splits - separate merged objects

  ---

  immatchx

  Package of Image Matching and Image Coordinates Tasks

  Version : 2001.10
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 6.27 Mb

  This package requires prior installation of iraf

  Summary

  The new immatchx package contains those tasks in images.imcoords and images.immatch which have had major bug fixes or enhancements since 2.11.3 was released. Two new tasks ccget and ccstd are also included. The current package menu looks like:

  ccfind - Generate a matched coordinate list using image wcs information ccget - Extract objects from a text file catalog ccmap - Compute image plate solutions using matched coordinate lists ccsetwcs - Create an image wcs from the plate solution ccstd - Transform from astrometric standard coordinates cctran - Transform from x-y to ra-dec and vice versa using plate solutions ccxymatch - Match celestial and pixel coordinate lists using various methods geomap - Compute geometric transforms using matched coordinate lists imcctran - Transform from one image celestial wcs to another psfmatch - Match the point-spread functions of 1-D or 2-D images skyctran - Transform coordinate lists from one celestial wcs to another skyxymatch - Generate matched x-y lists using image celestial wcs information xregister - Register 1-D or 2-D images using x-correlation techniques

  ---

  indilib

  

  An Instrument-Neutral Device Interface protocol

  Version : 0.1
  Author(s) : Elwood C. Downey (ecdowney@clearskyinstitute.com) , Jasem Mutlaq (mutlaqja@ikarustech.com)
  License : LGPL
  Website : http://www.clearskyinstitute.com/INDI
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 5.03 Mb

  Summary

  Indiserver is the public network access point where one or more INDI Clients may contact one or more INDI Drivers. Indiserver launches each driver process and arranges for it to receive the INDI protocol from Clients on its stdin and expects to find commands destined for Clients on the driver's stdout. Anything arriving from a driver process' stderr is copied to indiserver's stderr.

  Indiserver only provides convenient port, fork and data steering services. If desired, a Client may run and connect to INDI Drivers directly.

  ---

  iraf

  Image reduction and Analysis Facility

  Version : 2.12
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 186.75 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startiraf
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Summary

  IRAF is the Image Reduction and Analysis Facility, a general purpose software system for the reduction and analysis of astronomical data. IRAF is written and supported by the IRAF programming group at the National Optical Astronomy Observatories (NOAO) in Tucson, Arizona. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under cooperative agreement with the National Science Foundation

  IRAF is the "Image Reduction and Analysis Facility". The main IRAF distribution includes a good selection of programs for general image processing and graphics, plus a large number of programs for the reduction and analysis of optical and IR astronomy data (the "noao" packages). Other external or layered packages are available for applications such as data acquisition or handling data from other observatories and wavelength regimes such as the Hubble Space Telescope (optical), EUVE (extreme ultra-violet), or ROSAT and AXAF (X-ray). These external packages are distributed separately from the main IRAF distribution but can be easily installed. The IRAF system also includes a complete programming environment for scientific applications, which includes a programmable Command Language scripting facility, the IMFORT Fortran/C programming interface, and the full SPP/VOS programming environment in which the portable IRAF system and all applications are written.

  ---

  ISIS

  

  Optimal Image Subtraction implementation

  Version : 2.1
  Author(s) : C. Alard (alard@iap.fr), R. H. Lupton
  License : Free
  Website : http://www.iap.fr/users/alard/package.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 68.01 Kb

  Summary

  A new method designed for optimal subtraction of two images with different seeing. Using image subtraction appears to be essential for the full analysis of the microlensing survey images, however a perfect subtraction of two images is not easy as it requires the derivation of an extremely accurate convolution kernel. Some empirical attempts to find the kernel have used the Fourier transform of bright stars, but solving the statistical problem of finding the best kernel solution has never really been tackled. We demonstrate that it is possible to derive an optimal kernel solution from a simple least square analysis using all the pixels of both images, and also show that it is possible to fit the differential background variation at the same time. We also show that PSF variations can also be easily handled by the method. To demonstrate the practical efficiency of the method, we analyzed some images from a Galactic Bulge field monitored by the OGLE II project. We find that the residuals in the subtracted images are very close to the photon noise expectations. We also present some light curves of variable stars, and show that, despite high crowding levels, we get an error distribution close to that expected from photon noise alone. We thus demonstrate that nearly optimal differential photometry can be achieved even in very crowded fields. We suggest that this algorithm might be particularly important for microlensing surveys, where the photometric accuracy and completeness levels could be very significantly improved by using this method

  There are 3 essential steps to follow to make light curves of variables objects

  Image registration

  The goal of image registration is to re-map each image on the same grid. The reference system, or common grid is usually one of the image. The output of this procedure will be a FITS image interpolated on the reference grid.

  This procedure involve 2 steps:

  - Getting the astrometric transform, X=f(x_ref,y_ref )

  - Making image interpolation (Bicubic Splines)

  Image Subtraction

  This is the main program, and the core of the new method presented in the 2 papers. Before you run the code, you need to make a good reference image by stacking some of your best images. Then you can use the image subtraction code to adjust the reference image to the seeing of each individual image (which have been previously registered and interpolated).

  The image subtraction code can process the whole frame by small pieces, it is especially useful in case of large images which can be processed with limited memory ressources.

  The code has 2 level of rejection for variable objects:

  - Checking that each individual star does not show flux variations

  - Checking the chi-square for each individual star

  The final output of the code will a subtracted image of the flux variation beween the individualimage and the reference frame.

  Photometry

  This package will make photometry of variable objects by using the subtracted images. The flux of the variable will be calculated using profile fitting photometry at fixed position. As for the image subtraction code, the frame can be also treated by small pieces. The profile of each frame is calculated by making median stacking of a few reference stars.

  ---

  jday

  

  Astronomical Julian Date calculator

  Version : 1.3
  Author(s) : Hiram Clawson - curator@hiram.ws.NoSpam
  License : jday
  Website : http://jday.sourceforge.net/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1.34 Mb

  Summary

  Astronomical Julian Date calculator

  TESTING: After the jday and j2d binaries are built, run the shell script: RunTest to test both of those binaries.

  The PERL examples can be tested with JdayTest.pl

  The dbd - days between dates example can be tested with Testdbd

  jday - with no arguments will print out the current Julian date based on your system clock and timezone. If your timezone or system clock are inaccurate, the output of jday will also be inaccurate

  ---

  lheasoft

  XIMAGE 4.0, XRONOS 5.18, and XSPEC 11.1.0. XANADU 5.1

  Version : 5
  Author(s) : NASA GSFC
  License : Free
  Website : http://heasarc.gsfc.nasa.gov/docs/software/lheasoft/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 29.38 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startlheasoft
  
       

  Screenshots

  

  Summary

  A suite of High Energy Astrophics applications

  ---

  libAstronomy

  

  Basic Astronomical Package

  Version : 0.1.6
  Author(s) : Alexander Roalter (roalter@in.tum.de)
  License : GPL
  Website : http://www.in.tum.de/~roalter/libAstronomy
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 751.00 Kb

  Summary

  The libAstronomy Package provides a set of functions for use in astronomical programs. Target of the package is making available routines for all purposes by providing function for calculating ephemerides with only one function call, but also providing all the functions needed to do this to allow the user to make his own functions if he wants to.

  I

  ---

  libnova

  

  Celestial Mechanics and Astronomical Calculation Library

  Version : 0.10.0
  Author(s) : Liam Girdwood (liam@gnova.org)
  License : LGPL
  Website : http://www.gnova.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 27.76 Mb

  Summary

  libnova is a general purpose, double precision, celestial mechanics and astronomical calculation library.

  The intended audience of libnova is C / C++ programmers, astronomers and anyone else interested in calculating positions of astronomical objects or celestial mechanics. libnova is the calculation engine used by the Nova project and most importantly, is free software. Features The current version of libnova can calculate:

  * Aberration * Nutation * Apparent Position * Dynamical Time * Julian Day * Precession * Proper Motion * Sidereal Time * Solar Coordinates (using VSOP87) * Coordinate Transformations * Planetary Positions Mercury - Pluto (Mercury - Neptune using VSOP87) * Planetary Magnitude, illuminated disk and phase angle. * Lunar Position (using ELP82), phase angle. * Elliptic Motion of bodies (Asteroid + Comet positional and orbit data) * Asteroid + Comet magnitudes * Parabolic Motion of bodies (Comet positional data) * Orbit velocities and lengths * Atmospheric refraction * Rise, Set and Transit times. * Semidiameters of the Sun, Moon, Planets and asteroids. * Angular separation of bodies * Hyperbolic motion of bodies

  ---

  MarsProject

  

  Mars colony simulation

  Version : 2.75
  Author(s) : Scott Davis
  License : GPL
  Website : http://mars-sim.sourceforge.net/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 13.24 Mb

  This package requires Java installation

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startMarsProject
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  The Mars Simulation Project is a free software Java project to create a simulation of future human settlement of Mars.

  The simulation is a multi-agent artificial society set in a detailed virtual world.

  XML configuration files allow the user to modify the simulation properties.

  ---

  mem0

  IRAF Maximum Entropy image restoration tools

  Version : C
  Author(s) : Dr. Nailong Wu (nailong@stsci.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.44 Mb

  This package requires prior installation of iraf

  Summary

  MEM0 was developed by Dr. Nailong Wu while a visiting scientist at NOAO. It has been tested on several platforms and is believed to be stable. Should you find any problems or have questions please contact Dr. Nailong Wu via email at nailong@stsci.edu.

  This is a task for 1-D or 2-D image restoration by MEM. In search of the maximum point of the objective function, the approximate Newton-Raphson method for optimization is used. Data fit and the total power are controlled by the Lagrange multipliers \fIalpha\fR and \fIbeta\fR, respectively, to meet the constraints. (See REFERENCES.)

  The program uses a double iteration scheme: the values of \fIalpha\fR and \fIbeta\fR are changed in the outer iteration, while the inner iteration is for finding the ME solution for the particular \fIalpha\fR and \fIbeta\fR.

  ---

  midas

  

  European Southern Observatory Munich Image Data Analysis System

  Version : 05FEBp11.2
  Author(s) : ESO
  License : GPL
  Website : http://www.eso.org/projects/esomidas/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 252.10 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startmidas
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  The ESO-MIDAS system provides general tools for image processing and data reduction with emphasis on astronomical applications including imaging and special reduction packages for ESO instrumentation at La Silla and the VLT at Paranal. In addition it contains applications packages for stellar and surface photometry, image sharpening and decomposition, statistics and various others.

  ---

  mscred

  IRAF Tools for Mosaic image processing

  Version : 4.5
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 20.47 Mb

  This package requires prior installation of iraf

  Summary

  The MSCRED external package is used to reduce CCD mosaic data in which the data is in the mosaic MEF data format.

  The data format used by the NOAO Mosaic Data Handling Software (MDHS) is a multiextension FITS (MEF) file. This format is produced by the the Data Capture Agent (DCA) when observing with the NOAO Mosaic. The MEF file for the NOAO Mosaic currently consists of nine FITS header and data units (HDU). The first HDU, called the primary or global header unit, contains only header information which is common to all the CCD images. The remaining eight HDUs, called extensions, contain the images from the eight CCDs.

  The fact that the image data is stored as a FITS file is not significant. Starting with IRAF V2.11, FITS files consisting of just a single primary image may be used in the same way as any other IRAF image format. The significant feature of the mosaic format is its multi-image structure.

  With multiextension FITS files you must either use tasks which are specifically designed to operate on these files as a unit or explicitly specify the image within the file that is to be operated upon by general IRAF image processing tasks. The tasks in the \fBmscred\fR package are designed to operate on the mosaic MEF files and so you only need to specify the filename.

  ---

  mtools

  MTOOLS package (version 5Mar98) contains a hodge-podge of various IRAF tasks by Jeff Munn

  Version : 1.0
  Author(s) : Jeff Munn (jam@nofs.navy.mil)
  License : Free
  Website : http://
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 4.95 Mb

  This package requires prior installation of iraf

  Summary

  The MTOOLS package (version 5Mar98) contains a hodge-podge of various IRAF tasks by Jeff Munn (send bug reports to jam@nofs.navy.mil), combined together in this one package. Some of these are simply variations of other IRAF tasks. The package is comprised of the following tasks:

  airchart - Plot airmass curves chart - Interactively chart 2-dimensional data defitize - Convert all FITS files in currect directory to images fitize - Convert all images in current directory to FITS files format - Format the standard input and pass it to the standard output gki2mng - Convert a GKI metacode file to MONGO input mysplot - Version of SPLOT with line identifying features pca - Principal components analysis

  The tasks span a range of usefulness and robustness, from the silly (fitize, defitize) to "I couldn't do anything without it" (chart), and from the robust (chart) to the semi-robust (gki2mng). This distribution was really put together for old grad-school colleagues, who wanted copies after obtaining their freedom and flying off to greener pastures. Thus, harbor no illusions about this being a well supported, elegantly structured, bug free package. Its simply a collection of tasks which are general in nature and proved sufficiently useful at some point that they haven't been purged. Its made available here primarily because of continued interest in the tasks chart, airchart, and mysplot. Below is a short critique of the usefulness and robustness of each task:

  airchart -- Very useful for planning observing runs. Robust. chart -- Very useful for maintaining and interacting with simple text file relational databases. Robust. defitize/fitize -- Mostless useless. Used primarily when transporting large numbers of FITS files, but it became much less interesting once one was able to set imhdr=HDR$, and even less interesting with the FITS kernel in v2.11. Still useful to copy directories with ".imh" files across machines with different byte ordering. Robust. format -- Outdated. New printf routines in IRAF 2.10 mostly supercede it. Semi-robust. gki2mng -- Useful. Doesn't convert everything, but enough that its easy to generate publication quality plots from IRAF plots. Semi-robust. mysplot -- Useful. Robust. Works with 2.11. pca -- Useful. Robust. Just an IRAF wrapper for Murtaugh and Heck code.

  ---

  mxtools

  IRAF MX version of Quick and Dirty PHOTometry

  Version : 2001.04.11_12:37
  Author(s) : Kenneth J. Mighell (mighell@noao.edu)
  License : AURA
  Website : http://www.noao.edu/staff/mighell/mxtools
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 23.19 Mb

  This package requires prior installation of iraf

  Screenshots

  

  Summary

  mxtools.mxdemo - MX Demo program mxtools.mxqdphot - MX version of Quick and Dirty PHOTometry

  mxtools.qdphot - Quick and Dirty CCD stellar PHOTometry (QDPHOT)

  ---

  ncarg

  

  NCAR graphics utilities and libraries

  Version : 4.4.0
  Author(s) : University Corporation for Atmospheric Research
  License : GPL
  Website : http://ngwww.ucar.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 59.31 Mb

  Summary

  NCAR Graphics (see also mirror sites below) is thoroughly documented in:

  The introductory user guide to the Ngmath library - a collection of mathematical procedures for which there are equivalent Fortran and C entries.

  The NCAR Graphics GKS manual User's Guide for NCAR GKS-0A Graphics

  Programmer documents for some of the graphical utilities (also known as the Low Level Utilites or LLUs) - these documents are the software developers' reference notes and are provided for users who want to explore the information that developers use to maintain a utility's source code. They can also be very helpful to users and contain many examples:

  Areas, A Package that Solves Certain Practical Problems in Topology
  Autograph, A Package of Routines to Draw X/Y Plots
  CGM, Graphcap, and Fontcap Supplement
  Conpack, A Contouring Package
  Dashpack, A Software Package for Drawing Dashed Lines
  Ezmap, A Map-Drawing Package
  Gflash, A Graphics Instruction Manipulation Package
  Gridal, A Package to Draw Backgrounds for X/Y Plots
  Isosurface, A Package of Routines used to Draw Isosurfaces
  Labelbar, A Package of Routines to Draw Labelled Bars
  Plotchar, A Character-Plotting Package
  Polypack, A Package of Routines to Manipulate Polygons
  SPPS, An NCAR System Plot Package Simulator
  Stitle, A Package to Create Scrolled Movie Titles
  Seter, A Centralized Error-Handling Package for NCAR Graphics
  Softfill, A Software Fill Package
  Streamlines, A Field Flow Visualization Utility
  Tdpack, A Three-Dimensional Plotting Utility
  Vectors, A Vector Field Plotting Utility
  Wmap, A Package for Producing Daily Weather Maps and Plotting Station Model Data
  

  The introductory user guide NCAR Graphics Fundamentals - this document contains important information for all users of NCAR Graphics: a glossary of terms, explanation of the structure of NCAR Graphics programs, strategies for learning to use NCAR Graphics, instructions for compiling, linking, and running programs, instructions for producing and editing output from NCAR Graphics programs, and guidelines for using the utilities. While it also introduces the Fortran interface to some of the traditional NCAR Graphics utilities, we recommend that you read the programmer documents (when available) instead. The programmer docs provide the most up-to-date information and the latest examples.

  ---

  nemo

  

  NEMO is a Stellar Dynamics Toolbox

  Version : 3.2.2
  Author(s) : Peter Teuben (nemo@astro.umd.edu) Joshua Barnes, Piet Hut
  License : GPL
  Website : http://bima.astro.umd.edu/nemo/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 67.68 Mb

  Screenshots

  

  

  Summary

  These are the tasks currently available under to run under NEMO. They are a collection of program to do N-body calculations and some simple 2/3-D image processing, connected with the N-body calculations. If program names are preceded by a dash (-) they do not have NEMO's user interface and are sometimes not even found in NEMO's bin area on disk (usually referred to as $NEMOBIN). Program names ending on a star (*) are available under this and sometimes more wildcard names (e.g. snapplot and snapplot_ps) Program names ending in a questionmark (?) are not available yet, but we're thinking of making them. Check the futureplan software(8NEMO) document to see if anyone is working on them yet.

  ---

  nightfall

  

  Light Curve Synthesis Program

  Version : 1.32
  Author(s) : Rainer Wichmann (rwichman@lsw.uni-heidelberg.de)
  License : GPL
  Website : http://www.lsw.uni-heidelberg.de/~rwichman/Nightfall.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 4.90 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startnightfall
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  NIGHTFALL is an interactive application that introduces into the fascinating realm of eclipsing binary stars. Apart from their light variations that make them interesting objects for observations, eclipsing binaries are of fundamental importance for astrophysics, e.g. for measuring the mass of stars. NIGHTFALL is capable of producing:

  animated views of eclipsing binary stars, lightcurves and radial velocity curves, best-fit binary star parameters for a given set of observational data.

  It is, however, not able to fry your breakfast egg on your harddisk.

  Eclipsing binary stars are most often very close systems. In such systems, owing to tidal forces, the shapes of both stars can be highly nonspherical, up to the possible formation of an 'overcontact' system, where both stars form a single, dumbell-shaped object.

  NIGHTFALL is a mildly ultramundane program of baroque complexity (I like Verdi and Händel on lazy sunday mornings - friday evenings are better with Iron Maiden and a good whisky). NIGHTFALL is based on a physical model that takes into account the nonspherical shape of stars in close binary systems, as well as mutual irradiance of both stars, and a number of additional physical effects.

  NIGHTFALL can handle a large range of configurations, including overcontact systems, eccentric (non-circular) orbits, surface spots and asynchroneous rotations (stars rotating slower or faster than the orbital period), and the possible presence of a third star in the system.

  NIGHTFALL supports the GNOME desktop (if installed), but does not require it. Also, NIGHTFALL supports internationalization. Currently, besides the default language (english), only german is supported. The language is selected by the environment variable LANG (must be set before starting the program, in sh, bash: LANG=de; export LANG in csh, tcsh: setenv LANG de). If used in non-interactive mode, unless a configuration file is read in at startup (see info on configuration files), NIGHTFALL requires at least the following six numerical arguments on the command line (in that order):

  (1) the mass ratio of both stars (mass(Secondary)/mass(Primary), allowed range 0.0001 - 10000.0. For Roche lobe fill factors (see below) above one, the mass ratio is restricted to 0.003 - 50. (2) orbital inclination ( = viewing angle of orbital plane, range 0 - 90 degree), where 0 deg corresponds to face-on view (no eclipse possible), and 90 deg to edge-on view (eclipse guaranteed). For angles in between, the occurence of an eclipse depends on the mass ratio and the Roche fill factors (see below). (3,4) Roche lobe fill factors. The Roche lobe is the maximum volume a star can fill in a binary system. Its size is, in general, different for the two stars, and depends on the mass ratio (see details on 'Roche lobe' for an explanation). The Roche lobe fill factor is in units of the polar radius of the Roche lobe. The allowed range is 0.001 - 1.3. For values above 1.0, both stars merge into a common envelope/overcontact system. (5,6) surface temperatures of both stars (in Kelvin, range 350 - 350000; Kelvin = degree Celsius + 273.15). Just for comparison, the surface temperature of the sun is 5780 K. If you use the 'model atmosphere' option, the allowed range shrinks to 3000 - 35000K.

  These six numerical arguments are always required, if NIGHTFALL is used in command-line (i.e. non-interactive) mode without reading in a configuration file (see below)

  $ nightfall -U -C ty_boo.cfg

  will read parameters from a configuration file and start NIGHTFALL in interactive mode. The configuration file is a simple text file that can be edited by hand. In interactive mode, you can also write out the current parameters to a configuration file.

  $ nightfall (without arguments) will produce a full list of options (many).

  By default, NIGHTFALL will do nothing more than run in non-interactive mode, compute the lightcurve, write it to an output file 'NightfallCurve.dat', and exit silently. If you want more (nifty plots, etc.), read on.

  ---

  nmisc

  Package of NOAO miscellaneous tasks

  Version : 2003.05
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 6.26 Mb

  This package requires prior installation of iraf

  Summary

  This external package contains NOAO developed tasks which by themselves are too minor to form their own external package. These tasks are made available in this package prior to distribution as part of the standard IRAF core system or NOAO package. Thus the contents of this package will vary with time. The current contents of the package are:

  -- Beta version tasks for creating and using pixel masks -- ccdmask - Create a pixel mask from a CCD image fixpix - Fix pixels defined by a pixel mask text2mask - Convert text description to pixel mask

  -- Focusing and PSF measuring tasks -- kpnofocus - Determine the best focus from KPNO focus images psfmeasure - Measure PSF sizes from stellar images specfocus - Determine spectral focus and alignment variations starfocus - Determine direct focus variations from stellar images

  -- New version with additional FWHM measurements from the V2.11 TV package -- newimexamine - IMEXAMINE with new FWHM measurements

  -- New task from the V2.10.4 IMAGES package -- xregister - Register 1-D pr 2-D images using x-correlation techniques

  ---

  opensourceastro-base

  Libraries and basic installation prep for Open Source Astronomy

  Version : 10.0
  Author(s) : Dave Mills (djm@openastro.com)
  License : GPL
  Website : http://www.openastro.com
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 21.27 Mb

  Summary

  This package should be installed first and contains the basic shared libraries and tools to support installation of the rest of the Open Source Astronomy distribution.

  The default location for all non-rpm packages is in the /opt/astro directory tree. If you do not have sufficient space on the / partition you can create a link to another partition. The GUI installer offers to do this the first time it is used. You must login as root to run the installer for this step. If you wish to install subsequent packages using you normal login, make sure that you change the owner/group permissions on /opt/astro to allow it.

  ---

  opensourceastro-library

  Comprehensive html format documentation for Open Source Astronomy

  Version : 10.0
  Author(s) : Various
  License : GPL
  Website : http://www.openastro.com
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 117.67 Mb

  Summary

  This package contains the full html format documentation for all packages included in the Open Source Astronomy distribution. It also contains a set of printable (postscript and pdf) documents in the /opt/astro/doc directory.

  It is recommended that this package is loaded first so that you can browse the library and decide which packages to install next. Installing everything will require ~8Gb.

  ---

  openuniverse

  

  Solar system simulation

  Version : 1.0beta3
  Author(s) : Raul Alonso (amil.las.es) , Axel Groll (axel_groll@engineer.com)
  License : GPL
  Website : http://www.openniverse.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 13.37 Mb

  This package has it's own installer

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startopenuniverse
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  What is OpenUniverse?

  Strictly spoken it's a piece of software, simulating the Solar System's bodies in 3D on your Windows or Linux PC (will work in most *NIX's as well). In difference to quite a few other programs it does so in realtime. Meaning you can view all the planets, moons and spaceships move along their paths, trace them, follow them, orbit them and even control them (time and spaceship contol). And you won't have to fight your way through hordes of green, slimey and one-eyed aliens for that ;-)

  History

  OpenUniverse (OU) was formely known as Solar System Simulator (Ssystem). It was initially released on Nov 1997 with the intention to create a rotating Earth display on a main stream PC. Since these early roots a continuing development and expansion has taken place. Was version 1.0 only aware of the major bodies (planets), version 1.2 added a whole bunch of moons. Solar System v1.6 then added more ways of movement for the user's eye (camera) within Solar System's virtual universe and last but not least better textures for a lot of bodies. This version, called OpenUniverse (OU) finally has been renamed to underline the concept behind the further development of the program: Open for the whole Universe, not just the solar system. Open to use, extend and change. Finally open for all users, programmers and for you. :)

  ---

  OrbitViewer

  

  OrbitViewer is an interactive applet that displays the orbit of small bodies (comets or asteroids) in the solar system in 3D

  Version : 1.3
  Author(s) : Osamu Ajiki, Ron Baalke
  License : GPL
  Website : http://www.astroarts.com/products/orbitviewer
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 221.00 Kb

  This package requires Java installation

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startOrbitViewer
  
       

  Screenshots

  

  Summary

  OrbitViewer is an interactive applet that displays the orbit of small bodies (comets or asteroids) in the solar system in 3D. The orbit may be played forwards or backwards like a movie.

  History: This applet was created by Osamu Ajiki (AstroArts Inc.) in 1996. It was further modified by Ron Baalke (NASA/JPL) in 2000-2001.

  ---

  partiview

  partiview is an advanced 4D-visualization tool

  Version : 0.7.06
  Author(s) : Peter Teuben, Stuart Levy
  License : NCSA2
  Website : http://bima.astro.umd.edu/nemo/amnh/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 4.86 Mb

  Screenshots

  

  

  The following printable documents will be installed :

  • /opt/astro/doc/partiview/partiview.ps.gz
  • /opt/astro/doc/partiview.pdf.gz

  Summary

  partiview is an advanced 4D-visualization tool, which also understands Starlab ``worldline'' (tdyn) datasets. Although is has been derived from VirDir, partiview can be compiled and run on relatively cheap hardware, and therefore facilitate development of new visualization algorithms.

  ---

  PGC

  

  This is a binary representation of some of the fields in the the PGC galaxy catalog.

  Version : 1.0
  Author(s) : Various
  License : GPL
  Website :
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 7.47 Mb

  Summary

  This "catalog of principal galaxies" constitutes the basis of the "Third Reference Catalogue of Bright Galaxies" (RC3). It lists equatorial coordinates for the equinoxes 1950 and 2000 and cross identifications for 73197 galaxies. Of the 73197 galaxies, 40932 have coordinates with standard deviations of less than ten arcsec. Listed are 131,601 names from the 38 most common sources. These data are given when available: morphological descriptions, apparent major and minor axes, apparent magnitudes, radial velocities, and position angles.

  ---

  phat

  Pat Hall's Add-on Tasks

  Version : 2.11
  Author(s) : Pat Hall
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 641.00 Kb

  This package requires prior installation of iraf

  Summary

  This is my compilation of personal miscellaneous add-on IRAF tasks and their help files, including some tasks for defringing and coadding optical CCD data, and tasks specifically designed for data from the CTIO 4-meter using the Big Throughput Camera (BTC) of Bernstein et al. This version is supplementary to PHIIRS, and in fact requires it. Any task listed in the PHAT package menu which is not in this PHAT package can be found in the PHIIRS package. PHIIRS should always be loaded before PHAT in IRAF. The entire package available as a compressed tarfile from "www.astro.utoronto.ca/~hall/phat211.tar.gz".

  ---

  phiirs

  Pat Hall's Infrared Imaging Reduction Software

  Version : 2.11.1
  Author(s) : Pat Hall
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.11 Mb

  This package requires prior installation of iraf

  Summary

  Spawned from original tasks by Doug Williams & Anne Turner and including many cannibalized parts from DIMSUM (Dickinson et al).

  v.0 950714 Spawned from original tasks by Doug Williams & Anne Turner and including many cannibalized parts from the DIMSUM package (Dickinson et al.). Read "phiirs.hlp" for an introduction.

  v.1 960226 Minor revisions. Read "phiirs.hlp" for an introduction.

  v.2 960711 Major revisions and additions; tasks are now available for complete reduction from raw data to images suitable for input to FOCAS or such. Read "phiirs.hlp" for an introduction. The entire package is available as a compressed tarfile from "http://www.astro.utoronto.ca/~hall/phiirsold.tar.gz". Replace "iterstat.cl" with "iterstatold.cl" if problems occur.

  v.2.10 980314 Final release for IRAF Version 2.10. Read "phiirs.hlp" for an introduction and overview. NOTE that several perl scripts (included with the package) are used for image coaddition if the CTIO package is unavailable. Several awk scripts are also used for photometric scaling tasks. Entire package available as a compressed tarfile from "http://www.astro.utoronto.ca/~hall/phiirs.tar.gz". To install, enter the proper pathnames in "phiirs.cl" and "phiirs.hd", load the softools IRAF package, and type "mkhelpdb root.hd helpdb.mip", deleting the old helpdb.mip if necessary. See "sample.loginuser.cl" for how to include the package in your default IRAF startup.

  For this & subsequent versions PHIIRS can now handle the DATE-OBS keyword in both "old" format "dd/mm/yy" and the new millenium format "yyyy-mm-dd" (affects first.cl, irimfirst.cl, and irtffirst.cl only). Currently I believe the IRAF astutil.setairmass task only accepts old format, but presumably any update to it will be backwards compatible.

  v.2.11 980805 IRAF V2.11 + FITS kernel release. Read "phiirs.hlp" for an introduction and overview. Default image extension is now assumed to be "fits" instead of "imh". I don't guarantee that all tasks are 100% compatible with V2.11, but all problems I've encountered in 5+ months of use have been fixed. NOTE that several perl scripts (included with the package) are used for image coaddition if the CTIO package is unavailable. Several awk scripts are also used for photometric scaling tasks. Entire package available as a compressed tarfile from "http://www.astro.utoronto.ca/~hall/phiirs211.tar.gz". To install, enter the proper pathnames in "phiirs.cl" and "phiirs.hd", load the softools IRAF package, and type "mkhelpdb root.hd helpdb.mip", deleting the old helpdb.mip if necessary. See "sample.loginuser.cl" for how to include the package in your default IRAF startup.

  v.2.11.1 990415/990519 New V2.11 release including "dophiirs.cl" script task. Read "phiirs.hlp" and "doc/dophiirs.hlp" for an introduction and overview. Other changes from v.2.11 (besides inevitable bug fixes): renamed task "irflat2.cl" to "domeflat.cl"; added tasks "cfhtfirst.cl", "onisfirst.cl", & "piscesfirst.cl" for use with particular telescope/ instrument combinations; better "irshift.cl", "qkflat.cl" & "qksky.cl"; "nshift.cl" task added for finding offsets for N images or image sets overlapping a central image, and "onis6ew.cl" & "onis3ew.cl" included as examples of how to build a large mosaic from individual image sets; and streamlined tasks for faster reduction of large IR arrays (e.g. iterstat can be run for single parameters only; irshift includes an imsection parameter to avoid displaying every image; & minv is faster). NOTE that several perl scripts (included with the package) are used for image coaddition if the CTIO package is unavailable. Several awk scripts are also used for photometric scaling tasks. Entire package available as a compressed tarfile from "http://www.astro.utoronto.ca/~hall/phiirs211.1.tar.gz". To install, enter the proper pathname in "phiirs.cl", load the IRAF softools package, and type "mkhelpdb root.hd helpdb.mip", deleting the old "helpdb.mip" if necessary. See "sample.loginuser.cl" for how to include the package in your default IRAF startup.

  ---

  photom

  

  Match lists of stars/galaxies

  Version : 0.7
  Author(s) : Michael W. Richmond (mwrsps@rit.edu)
  License : GPL
  Website :
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 1.21 Mb

  Summary

  This package contains software to match one list of objects against another list, allowing for arbitrary translation, rotation, scaling, and some distortion. The code is designed specifically for astronomical data: list of stars or galaxies. There is a small "pre-processor" to put astronomical data into the proper format for matching, and a "post-processor" to apply a transformation to the astronomical coordinates in a list. Most of the real work is done by the "match" program itself.

  ---

  pyraf

  PyRAF is a command language for IRAF

  Version : 1.1.2
  Author(s) : Space Telescope Science Institute (help@stsci.edu)
  License : pyraf
  Website : http://www.stsci.edu/resources/software_hardware/pyraf/what_is_pyraf
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 289.90 Mb

  This package requires prior installation of iraf

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startpyraf
  
       

  Screenshots

  

  Summary

  PyRAF is a command language for IRAF based on the Python scripting language that can be used in place of the existing IRAF CL. Why a new IRAF CL?

  The current IRAF CL has some shortcomings as a scripting language that make it difficult to use in writing scripts, particularly complex scripts. The major problem is that the IRAF CL has no error or exception handling. If an error occurs, the script halts immediately with an error message that has little or no information about where the error occurred. This makes it difficult to debug scripts, impossible to program around errors that can be anticipated, and difficult to provide useful error messages to the user.

  But there are other important reasons for wanting to replace the CL. We want to develop a command language that is a stronger environment for general programming and that provides more tools than the existing IRAF CL. Python (www.python.org), like Perl and Tcl, is a free, popular scripting language that is useful for a very wide range of applications (e.g., writing CGI scripts, text processing, file manipulation, graphical programming, etc.). Python is also an open system that can be easily extended by writing new modules in Python, C, or Fortran. By developing a Python interface to IRAF tasks, we open up the IRAF system and make it possible to write scripts that combine IRAF tasks with the numerous other capabilities of Python.

  Ultimately, we plan for PyRAF to have command-line data access and manipulation facilities comparable to those of IDL (the Interactive Data Language, www.rsinc.com, which has extensive array-processing and image manipulation capabilities). It should eventually be possible to write applications in PyRAF that can manipulate the data directly in memory and display it much as IDL does. We are hoping that Python and PyRAF will become the programming language of first resort, so that programmers and astronomers will only infrequently need to write programs in C or Fortran. Moreover, when it is necessary to use compiled languages, programs written in C, C++, and Fortran can be easily linked with and integrated into PyRAF.

  ---

  PySBIG

  

  SBIG data import for python

  Version : 0.02
  Author(s) : Russell Valentine (russ@coldstonelabs.org)
  License : GPL
  Website : http://coldstonelabs.org
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 41.00 Kb

  Summary

  This module can read SBIG files and give you a Numeric array for the data and a dictionary for the headers.

  ---

  radial

  

  This program calculates the radial velocities of both stars in a binary system

  Version : 1.0
  Author(s) : J Hegarty (hegarty@nhn.ou.edu)
  License : Free
  Website : http://www.nhn.ou.edu/~hegarty/radial
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 201.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startradial
  
       

  Summary

  This program calculates the radial velocities of both stars in a binary system, allowing for user configuration of stellar masses, semimajor axis, inclination of orbital plane, orbital eccentricity, time to collect data, and calculation frequency.

  For your convenience, default values have been added to the program, so you can run it with nothing other than variable eccentricity, if you like.

  ---

  rvsao

  An IRAF package to obtain radial velocities from spectra

  Version : 2.1.28
  Author(s) : Doug Mink
  License : Free
  Website : http://tdc-www.harvard.edu/iraf/rvsao/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 3.83 Mb

  This package requires prior installation of iraf

  Summary

  The package RVSAO defined in this directory was developed by Doug Mink at the Harvard-Smithsonian Center for Astrophysics from the redshift package originally written by Gerard Kriss at Johns Hopkins University and modified significantly by Steve Levine at the University of Wisconsin. It obtains radial velocities and velocity dispersions using cross-correlation methods or emission line fits. It consists of five tasks: XCSAO, EMSAO, BCVCORR, SUMSPEC, and LINESPEC. If you have any problems, please contact Doug Mink, mink@cfa.harvard.edu. This package has not been tested on a VMS system. A task, RELEARN, has been provided to aid in updating parameters. Run it instead of UNLEARN to keep your current parameters settings while adding new parameters.

  After the Revision Notes, you will find installation instructions.

  A fairly complete description of this package has been published in the August 1998 issue of the Publications of the Astronomical Society of the Pacific. For further updates, see http://tdc-www.harvard.edu/iraf/rvsao/

  ---

  rvx

  Radial Velocity analysis package.

  Version : 1.0
  Author(s) : Various
  License : Free
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.97 Mb

  This package requires prior installation of iraf

  Summary

  This archive contains the Radial Velocity analysis package. Package PSET support code as well as the source for the cross-correlation task, FXCOR, are included.

  ---

  scilab

  

  Scientists mathematical toolbox

  Version : 2.6
  Author(s) : INRIA (scilab@inria.fr)
  License : scilab
  Website : http://www-rocq.inria.fr/scilab
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 18.50 Mb

  This package has it's own installer

  Screenshots

  

  

  The following printable documents will be installed :

  • /opt/astro/doc/scilab/comm.pdf
  • /opt/astro/doc/scilab/internals.pdf
  • /opt/astro/doc/scilab/intro.pdf
  • /opt/astro/doc/scilab/lmi.pdf
  • /opt/astro/doc/scilab/manual.pdf
  • /opt/astro/doc/scilab/metanet.pdf

  Summary

  Developed at INRIA, Scilab has been developed for system control and signal processing applications. It is freely distributed in source code format (see the copyright file).

  Scilab is made of three distinct parts: an interpreter, libraries of functions (Scilab procedures) and libraries of Fortran and C routines. These routines (which, strictly speaking, do not belong to Scilab but are interactively called by the interpreter) are of independent interest and most of them are available through Netlib. A few of them have been slightly modified for better compatibility with Scilab's interpreter.

  A key feature of the Scilab syntax is its ability to handle matrices: basic matrix manipulations such as concatenation, extraction or transpose are immediately performed as well as basic operations such as addition or multiplication. Scilab also aims at handling more complex objects than numerical matrices. For instance, control people may want to manipulate rational or polynomial transfer matrices. This is done in Scilab by manipulating lists and typed lists which allows a natural symbolic representation of complicated mathematical objects such as transfer functions, linear systems or graphs (see Section ??).

  Polynomials, polynomials matrices and transfer matrices are also defined and the syntax used for manipulating these matrices is identical to that used for manipulating constant vectors and matrices.

  Scilab provides a variety of powerful primitives for the analysis of non-linear systems. Integration of explicit and implicit dynamic systems can be accomplished numerically. The scicos toolbox allows the graphic definition and simulation of complex interconnected hybrid systems.

  There exist numerical optimization facilities for non linear optimization (including non differentiable optimization), quadratic optimization and linear optimization.

  Scilab has an open programming environment where the creation of functions and libraries of functions is completely in the hands of the user (see Chapter ??). Functions are recognized as data objects in Scilab and, thus, can be manipulated or created as other data objects. For example, functions can be defined inside Scilab and passed as input or output arguments of other functions.

  In addition Scilab supports a character string data type which, in particular, allows the on-line creation of functions. Matrices of character strings are also manipulated with the same syntax as ordinary matrices.

  Finally, Scilab is easily interfaced with Fortran or C subprograms. This allows use of standardized packages and libraries in the interpreted environment of Scilab.

  The general philosophy of Scilab is to provide the following sort of computing environment:

  To have data types which are varied and flexible with a syntax which is natural and easy to use. To provide a reasonable set of primitives which serve as a basis for a wide variety of calculations. To have an open programming environment where new primitives are easily added. A useful tool distributed with Scilab is intersci which is a tool for building interface programs to add new primitives i.e. to add new modules of Fortran or C code into Scilab.

  To support library development through ``toolboxes'' of functions devoted to specific applications (linear control, signal processing, network analysis, non-linear control, etc.)

  ---

  sextractor

  

  Source Extractor, locates astronomical objects in images

  Version : 2.3.2
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/sextractor/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 11.45 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startsextractor
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  The following printable documents will be installed :

  • /opt/astro/doc/sexarticle.ps.gz
  • /opt/astro/doc/sexarticle.ps

  Summary

  SExtractor (Source-Extractor) is a program that builds a catalogue of objects from an astronomical image. It is particularly oriented towards reduction of large scale galaxy-survey data, but it also performs well on moderately crowded star fields. Its main features are:

  Simplicity of usage and configuration. ffl Speed: typically 500 kpixel/s with a Pentium2@450MHz. Ability to work with very large images (up to 65k pixels on 32bit machines, or 2G pixels on 64bit machines), thanks to buffered image access. Robust deblending of overlapping extended objects. Real-time filtering of images to improve detectability. Neural-Network-based star/galaxy classifier. Flexible catalogue output of desired parameters only. Pixel-to-pixel photometry in dual-image mode. Handling of weight-maps and flag-maps. Optimum handling of images with variable S/N. Special mode for photographic scans. Modularity of the code that enables one to implement new parameters.

  ---

  sky2000

  

  This is a binary representation of some of the fields in the the Sky 2000.0 catalog.

  Version : 0.2
  Author(s) : Myers J.R., Sande C.B., Miller A.C., Warren Jr. W.H., Tracewell D.A. Goddard Space Flight Center, Flight Dynamics Division (2002)
  License : GPL
  Website :
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 46.92 Mb

  Summary

  The SKYMAP Star Catalog System consists of a Master Catalog stellar database and a collection of utility software designed to create and maintain the database and to generate derivative mission star catalogs (run catalogs). It contains an extensive compilation of information on almost 300000 stars brighter than 8.0 mag.

  The original SKYMAP Master Catalog was generated in the early 1970's. Incremental updates and corrections were made over the following years but the first complete revision of the source data occurred with Version 4.0. This revision also produced a unique, consolidated source of astrometric information which can be used by the astronomical community. The derived quantities were removed and wideband and photometric data in the R (red) and I (infrared) systems were added.

  Version 4 of the SKY2000 Master Catalog was completed in April 2002; it marks the global replacement of the variability identifier and variability data fields. More details can be found in the description file sky2kv4.pdf.

  ---

  skymaker

  

  Aprogram that simulates astronomical images.

  Version : 2.3.4
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/sextractor/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 311.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startskymaker
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Summary

  The general SYNTAX is similar to that of SExtractor:

  sky [] [-c ] [- ] ...

  - A list file is an ASCII file containing a list of objects that can be added to the simulated image. An example is provided in the sample.list file. Note that only stars (code = 100) and galaxies (code = 200) are recognized in this version. - Keyword parameters given in the command line override those from the configuration file. - If the list-file is given as unique argument, Skymaker searches for a default configuration file called ``default.sky''. - SkyMaker creates 2 files in output: the image itself, and a catalog containing the objects it contains (with name toto.list if IMAGE_NAME was set to toto.fits). - Currently, the following TYPEs can be used with the IMAGE_TYPE keyword: PUPIL_REAL, PUPIL_IMAGINARY, PUPIL_MODULUS, PUPIL_PHASE, PUPIL_MTF, PSF_MTF, PSF_FULLRES, PSF_FINALRES, SKY_NONOISE and SKY. The two latter keywords should be used for creating actual instrument images. - A FITS header (any FITS image, or even an ASCII dump) can be provided through the IMAGE_HEADER keyword: simply replace "INTERNAL" by the file name. SkyMaker2 will then make a copy of this header for the simulated image, enabling the latter to be easily processed through your usual reduction tools. - Thanks to Pascal Fouque, parameters describing common optical aberrations (including defocus, spheric, astigmatism and coma) have been included in the description of the pupil phase-plane. Their normalisation follow the ESO convention (equivalent angular diameter of a circle, in the focal plane, which encloses 80% of the PSF flux; this is generally slightly more than the FWHM). However the user is invited to check this normalisation, and report any unexpected result. - Please look at the denisI.sky, denisJ.sky and denisK.sky configuration examples for more information. - If a SEED_* parameter is set to 0, the corresponding random generator is initialized to a ``random'' (function of time) value. - Beware of large AUREOLE_RADIUS values: during the calculation of the image, a temporary border of pixels in thickness is added all around the image, and can significantly affect the computation time.

  ---

  spectime

  IRAF SPECTRAL EXPOSURE TIME CALCULATOR

  Version : 2.0
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.26 Mb

  This package requires prior installation of iraf

  Summary

  The SPECTIME external package provides a spectral exposure time calculation engine, SPTIME, that is driven by database files describing the various components of a spectroscopic system. SPTIME can be used directly or with different user interfaces for specific spectrographs. These include IRAF scripts and a web interface.

  ---

  spectrum

  

  A stellar spectral synthesis program

  Version : 2.65
  Author(s) : Richard O. Gray
  License : Free
  Website : http://www1.appstate.edu/dept/physics/spectrum/spectrum.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 2.93 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startspectrum
  
       

  Screenshots

  

  

  Summary

  SPECTRUM ((C) Richard O. Gray, 2001) is a stellar spectral synthesis program which runs on a number of platforms, including most flavors of UNIX and LINUX . It will also run under Windows 9x/ME/NT/2000 using the Cygwin tools. The code for SPECTRUM has been written in the C language. SPECTRUM computes the LTE synthetic spectrum given a stellar atmosphere model. SPECTRUM can use as input the new, fully blanketed stellar atmosphere models of Robert Kurucz (1993), but any other stellar atmosphere model which can be cast into the format of Kurucz's models can be used as well.

  SPECTRUM can be programmed with "command-line switches" to give a number of different outputs. In the default mode, SPECTRUM computes the stellar-disk-integrated normalized-intensity spectrum, but in addition, SPECTRUM will compute the absolute monochromatic flux from the stellar atmosphere or the specific intensity from any point on the stellar surface.

  SPECTRUM and a number of auxiliary programs can be run under batch mode, making automated computation of a large number of synthetic spectra possible.

  SPECTRUM is distributed with an atomic and molecular line list for the optical spectral region 3000 A to 6800 A, called luke.lst, suitable for computing synthetic spectra with temperatures between about 4500K and 20,000K.

  SPECTRUM currently supports most atomic elements important in stellar spectra and their first or second ions. SPECTRUM also supports the following diatomic molecules: CH, NH, OH, MgH, SiH, CaH, SiO, C2, CN, CO and TiO. Other molecules and atoms will be added in the future.

  ---

  spptools

  A package of SPP programming and debugging tools

  Version : 2.12
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 2.75 Mb

  This package requires prior installation of iraf

  Summary

  SPPTOOLS - A package of SPP programming and debugging tools made up of the following tasks.

  chcount -- compare the number of non-white chars in a pair of files fid -- query ID database for specific files iid -- interactive query of ID database memcheck -- check SPP code for possible memory errors mkid -- make and ID database pkgcreate -- create an external package pkgrename -- rename an external package qid -- query ID database sppcalls -- print a list of SPP code calling sequences sppfmt -- indent and format a SPP program source file spplint -- a SPP program verifier

  ---

  starbase

  

  Starbase Data Tables - An Ascii Relational Database for UNIX

  Version : 3.2.2
  Author(s) : John B. Roll jr.
  License : GPL
  Website : http://cfa-www.harvard.edu/~john/starbase/starbase.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 17.60 Mb

  Screenshots

  

  Summary

  Starbase is a set of filter programs and an ascii table format for UNIX. The current release contains over 95 programs for manipulating data tables. The ascii database concepts are outlined in the book Unix Relational Database Management by Manis, Schaffer and Jorgensen. This implementation has been written at the Smithsonian Astrophysical Observatory and contains many extensions for use with scientific and astrophysical data sets.

  ---

  starjava

  Starlink Java Infrastructure and Applications Set

  Version : 1.1
  Author(s) : Starlink Project
  License : GPL
  Website : http://www.starlink.ac.uk/star/docs/sun251.htx/node2.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 52.79 Mb

  This package requires Java installation

  Summary

  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.

  ASTGUI - AST specific UI components.

  AXIS - Third generation Apache SOAP.

  COCO - Java UI for Coco.

  DOM4J - 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 - Positional 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.

  ---

  starlab

  A package for simulating the evolution of dense stellar systems

  Version : 4.3.2
  Author(s) : Piet Hut (IAS), Steve McMillan (Drexel U.), Jun Makino (U. Tokyo) Simon Portegies Zwart (U. of Amsterdam)
  License : GPL
  Website : http://www.sns.ias.edu/~starlab/starlab.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 3.07 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startstarlab
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  

  Summary

  Starlab is a software package for simulating the evolution of dense stellar systems, and analyzing the resultant data. It is a collection of loosely coupled programs, linked at the level of the UNIX operating system, that share a common data structure, and can be combined in arbitrarily complex ways to study the dynamics of star clusters and galactic nuclei. Current improvements in both the quality and the quantity of observational data, together with ongoing and anticipated increases in available computational power, combine to make this project both necessary and feasible.

  All stellar-dynamical $N$-body simulations rely on sophisticated integration schemes to follow the motion of all particles in the system under study. It is the job of the $N$-body program to deliver a faithful representation of the dynamical evolution of the system, along with information on all stellar interactions of interest, to the user, subject only to the fundamental limitations imposed by the chaotic equations of motion and the laws of physics. It is becoming increasingly clear that, in order to make detailed comparisons between simulations and the high-quality data now available, $N$-body (and perhaps also detailed Monte-Carlo) simulations are really the only viable option.

  Performing $N$-body simulations is already is a complex and demanding task. However, generating data is only half the job. The other half of the work of a computational theorist parallels that of the observer, and lies in the job of data reduction. As in the observational case, a good set of tools is essential, and unless the tools can be used in a flexible and coherent software environment, their usefulness will be severely limited. Three requirements are central in handling the data flow from a full-scale globular cluster simulation: modularity, flexibility, and compatibility. Starlab incorporates these three requirements.

  To some extent, Starlab is modeled on NEMO, a stellar dynamics software environment developed six years ago at the Institute for Advanced Study, in large part by Josh Barnes, with input from Peter Teuben and Piet Hut (and subsequently maintained and extended by Peter Teuben). Starlab differs from NEMO mainly in the following areas: it emphasizes the use of UNIX pipes, rather than temporary files; its use of tree structures rather than arrays to represent $N$-body systems; and its guarantee of data conservation---data which are not understood by a given module are simply passed on rather than filtered out.

  How to perform specific common tasks using Starlab tools. --------------------------------------------------------

  Note: Most tools are just simple interfaces onto the corresponding library functions, so the tasks listed below could in principle also be carried out by compiled programs rather than by pipes. However, the use of pipes is in many ways clearer and much more flexible.

  For more information on Starlab tools, see the file TOOLS in this directory. For details on a specific tool, type

  tool-name --help

  * Create a linked list of 100 equal-mass nodes of unit total mass

  mknode -n 100 -m 1

  * Create a system of 100 nodes with a Salpeter mass spectrum with masses in the range 0.5 to 10

  mknode -n 100 | mkmass -f 1 -x -2.35 -l 0.5 -u 10

  * Create a system of 100 nodes with a mass spectrum and evolve the stars without dynamics

  mknode -n 100 | mkmass -f 1 -x -2.35 -l 0.5 -u 10 | ???Simon???

  * Create a 500-particle Plummer model, with numbered stars, scaled to standard dynamical units

  mkplummer -n 500 -i

  * Create a 500-particle W0 = 5 King model, with numbered stars, unscaled

  mkking -n 500 -w 5 -i -u

  * Create a 500-particle W0 = 5 King model with a Miller-Scalo mass spectrum between 0.1 and 20 solar masses, then rescale to unit total mass, total energy -0.25, and virial ratio 0.5 and display the results graphically

  mkking -n 500 -w 5 -i -u \ | mkmass -f 2 -l 0.1 -u 20 \ | scale -m 1 -e -0.25 -q 0.5 \ | xstarplot -l 5 -P .5

  * Create a 500-particle W0 = 5 King model with a Miller-Scalo mass spectrum between 0.1 and 20 solar masses, add in a 10 percent 1-10 kT binary population, then rescale to unit total mass, total energy (top-level nodes) -0.25, and virial ratio (top-level nodes) 0.5, and finally verify the results by analyzing the final snapshot

  mkking -n 500 -w 5 -i -u \ | mkmass -f 2 -l 0.1 -u 20 \ | mksecondary -f 0.1 -l 0.25 \ | mkbinary -l 1 -u 10 \ | scale -m 1 -e -0.25 -q 0.5 \ | sys_stats -n -s

  * Evolve this model without stellar evolution for 100 dynamical times, with log output ever dynamical time and snapshot output every 10 dynamical times, with a self-consistent tidal field, removing escapers when they are more than two Jacobi radii from the cluster center

  mkking -n 500 -w 5 -i -u \ | mkmass -f 2 -l 0.1 -u 20 \ | mksecondary -f 0.1 -l 0.25 \ | mkbinary -l 1 -u 10 \ | scale -m 1 -e -0.25 -q 0.5 \ | dstar_kira -t 100 -d 1 -D 10 -Q -G 2

  * Create a King model with a power-law mass spectrum and a binary population, then evolve it with stellar and binary evolution

  mkking -n 500 -w 5 -i -u \ | mkmass -f 1 -x -2.0 -l 0.1 -u 20 \ | mksecondary -f 0.1 -l 0.1 \ | addstar -Q 0.5 -R 5 \ | scale -M 1 -E -0.25 -Q 0.5 \ | mkbinary -f 1 -l 1 -u 1000 -o 2 \ | dstar_kira -t 100 -d 1 -D 10 -f 0.3 -n 10 -q 0.5 -Q -G 2 -S -B

  * Perform a series of 100 3-body scattering experiments involving an equal-mass circular binary and a double-mass incomer, with impact parameter equal to the binary semimajor axis, relative velocity at infinity half that needed for zero total energy, and all other parameters chosen randomly, and display the results as a movie

  scatter3 -m 0.5 -e 0 -M 1 -r 1 -v 0.5 -n 100 -C 5 -D 0.1 \ | xstarplot -l 4

  * Compute cross-sections for interactions between a circular binary with component masses 0.75 and 0.25 and an incoming star of mass 1 and velocity at infinity 0.1, all stars having radius 0.05 binary semimajor axes

  sigma3 -d 100 -m 0.25 -e 0 -M 1 -v 0.1 -x 0.05 -y 0.05 -z 0.05

  * Create a scattering configuration involving a head-on collision between a circular binary and a stable hierarchical triple, and verify the result

  mkscat -M 1.5 -r 0 -v 1 -t -a 1 -e 0 -p -a 1 -e 0 -p1 -a 0.1 -e 0 \ | flatten | make_tree -D 1 | pretty_print_tree

  * Create a scattering configuration involving a head-on collision between a circular binary and a stable hierarchical triple, and integrate it forward in time

  scatter -i "-M 1.5 -r 0 -v 1 -t -a 1 -e 0 -p -a 1 -e 0 -p1 -a 0.1 -e 0" \ -t 100 -d 1 -v

  (etc.)

  ---

  Starlink

  Comprehensive suite of Astronomical data reduction programs

  Version : 2005
  Author(s) : UK Starlink Project
  License : GPL
  Website : http://www.starlink.rl.ac.uk
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 4
  Disk space required for installation is 1184.38 Mb

  Summary

  The Starlink suite contains the following libraries and applications.

  A2PS Ascii to PostScript converter ADAM The Control Subsystem AGI A graphics database system AMS The Unix ADAM Message System ARD ASCII Region Definition system provides a textual language for describing regions within a data array ARY A Subroutine Library for Accessing ARRAY Data Structures AST A Library for Handling World Coordinate Systems in Astronomy ASTROM Basic astrometry program ASURV Astronomical Survival Statistics CATREMOTE a Tool for Querying Remote Catalogues CCDPACK CCD data processing CFITSIO Disk FITS Input/Output Functions CHR Character Handling Routines COCO Conversion of Celestial Coordinates CURSA Catalogue and Table Manipulation Applications DAOPHOT Stellar Photometry Package Datacube A package which includes the IFU Data Product Cookbook DIPSO A friendly spectrum analysis program DOCFIND Starlink document index searching ECHOMOP Echelle Data Reduction Package ECHWIND UCL Echelle Spectrograph Observation Planning Program EMS Error Message Service Err Error and message reporting library ESP Extended Surface Photometry EXTRACTOR An Astronomical Source Detection Program FIGARO A general data reduction system FINDCOORDS Finding the Coordinates of a Named Object FIO Subroutine package that allows a FORTRAN programmer to access sequential and direct access data files in a machine independent manner. FITSIO Disk FITS Input/Output Subroutines FLUXES JCMT Position and Flux Density Calibration GAIA Graphical Astronomy and Image Analysis Tool GKS Graphical Kernel System GNS Graphics Workstation Name Service GRP Routines for Managing Groups of Objects GSD The Global Section Datafile (GSD) access library GWM X Graphics Window Manager HDS Hierarchical data system HDSPAR HDS Parameter Routines HDSTOOLS Tools To Display and Edit HDS Objects HDSTRACE Listing HDS Data Files HLP Interactive Help System ICL The Interactive Command Language for ADAM IFD Interface Definition Files IMG Simple Image Data Access IUEDR IUE Data Reduction package v3.2-0 JPEG The JPEG library and utilities JPL Solar System Ephemeris KAPLIBS Internal subroutines used within the KAPPA package. KAPPA Kernel Application Package MAG Access to magnetic tapes MERS (MSG and ERR) Message and Error Reporting Systems MESSGEN Starlink Facility Error Message Generation NAOS Finding NAOMI Guide Stars NBS The Noticeboard System NCAR Graphics Utilities NDF N-dimensional data format ONE Odds and Ends Library ORACDR integral field spectroscopy data reduction PAR Interface to the ADAM Parameter System PCS The Parameter and Communication Subsystems PDA Public Domain Algorithms PERIOD A Time-Series Analysis Package PERL Practical Extraction and Report Language PHOTOM A Photometry Package PISA Position Intensity and Shape Analysis POLMAP An interactive data analysis package for linear POLPACK A package of applications for reducing imaging polarimetry or spectropolarimetry data PONGO A Set of Applications for Interactive Data Plotting Version PSMERGE Encapsulated PostScript Handling Utility PSX POSIX interface routines REF Routines for Handling References to HDS Objects RV Radial Components of Observer's Velocity SAE Starlink Applications Environment special files SLALIB Positional Astronomy Library SPECX A general purpose mm and sub-mm spectral line data reduction system SPT Software Porting Tools Star2HTML Converting Starlink Documents to Hypertext STARPERL Starlink perl modules STARTCL Starlink Extensions to Tcl & Tk STARX X Library linking SURF SCUBA User Reduction Facility TRANSFORM Coordinate Transformation Facility XDISPLAY Setting remote X windows

  NOTE :

  PPARC's Review of Astronomical Software, chaired by Paul Hewett, reported to Science Committee at the end of April. The Review recommended, amongst other things, that support for core infrastructure and strategic software should continue. Science Committee declined to accept that recommendation.

  One consequence of this decision is that Starlink will cease to exist at the end of June 2005, i.e. in about 6 weeks' time. The Starlink programming team will be disbanded and programmer contracts will finish at that time. The Starlink QUICK and News services will cease.

  The Starlink Software Collection of 100+ applications and libraries will no longer be supported, including for example GAIA, TOPCAT, KAPPA, CCDPACK, CONVERT, SPLAT, FIGARO, PHOTOM, POLPACK and the SLALIB, AST, HDS and NDF libraries.

  The Starlink collection was released under the GNU GPL prior to the end of the project.

  ---

  stecf

  

  IRAF Tools for reduction and analysis of Hubble Space Telescope data

  Version : 2005
  Author(s) : Various
  License : ESO
  Website : http://www.stecf.org/software/stecf-iraf/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 11.33 Mb

  This package requires prior installation of iraf

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/odc/stecf.pdf

  Summary

  We have collected together many of the astronomical applications developed as Iraf tasks at the Space Telescope European Coordinating Facility (ST-ECF) into an Iraf layered package called "stecf". This package contains several subpackages. One contains a variety of image restoration algorithms including multiple channel and photometric variants of the Richardson Lucy method. In addition a wholly new package ("impol") for the reduction of polarimetric imaging from HST (and ground-based instruments) is made available for the first time. Software for the post-pipeline processing of HST NICMOS data, with particular emphasis on the association and pre-processing of images to be used for grism spectral extraction, and finally a general purpose grism spectral extraction tool are also included.

  ---

  stellarium

  

  Real-time photorealistic sky simulator

  Version : 0.6.2
  Author(s) : Fabien Chereau (stellarium@free.fr)
  License : GPL
  Website : http://stellarium.free.fr
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 27.95 Mb

  This package has it's own installer

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startstellarium
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  Stellarium is a free software available for Windows, Linux/Unix and MacOSX. It renders 3D photo-realistic skies in real time. With stellarium, you really see what you can see with your eyes, binoculars or a small telescope.

  ---

  stsdas

  IRAF Tools for Hubble Space Telescope data reduction

  Version : 2.3
  Author(s) : STSCI team
  License : STSCI
  Website : http://stsdas.stsci.edu/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 268.69 Mb

  This package requires prior installation of iraf

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/stsdas-UserGuide.ps

  Summary

  The Space Telescope Science Data Analysis System (STSDAS) is software for calibrating and analyzing data from the Hubble Space Telescope (HST). STSDAS includes the same calibration routines as are used in the routine data processing pipeline, as well as general-purpose tools and enhancements to the Image Analysis and Reduction Facility (IRAF).

  IRAF provides the user interface (command language, or CL) and general purpose graphic and image display facilities. Because STSDAS is layered on IRAF, the system runs on any computing platform for which an IRAF port is available, including most Unix and VMS systems.

  The CL provides a wide range of functions typically provided by an operating system, and uses a syntax similar to Unix. Some of the CL features include input/output redirection and piping, command buffers and history editing, minimum matching of commands, host-independent file naming, parameter range checking, background and batch processing modes, an integrated online help system, and a script authoring environment.

  ---

  stuff

  

  SkyStuff is a program that generates artificial but realistic catalog of astronomical sources

  Version : 1.05
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/sextractor/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 25.73 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startstuff
  
       

  Summary

  SkyStuff is a program that generates artificial but realistic catalog of astronomical sources. These catalogs can be loaded by SkyMaker to generate image simulations.

  ---

  sunwait

  

  Wait until specified interval before sunrise

  Version : 1.0
  Author(s) : Daniel Risacher
  License : GPL
  Website :
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 181.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startsunwait
  
       

  Summary

  usage: sunwait [options] [sun|civ|naut|astr] [up|down] [+/-offset] [latitude] [longitude]

  latitude/longigude are expressed in floating-point degrees, with [NESW] appended example: sunwait sun up -0:15:10 38.794433N 77.069450W This example will wait until 15 minutes and 10 seconds before the sun rises in Alexandria, VA options: -p prints a summary of relevant times -z changes the printout to Universal Coordinated Time (UTC) -V prints the version number -v increases verbosity -h prints this help

  ---

  swarp

  SWarp is a program that resamples and co-adds together FITS images using any arbitrary astrometric projection defined in the WCS standard.

  Version : 2.15
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/soft/swarp/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 301.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startswarp
  
       

  The following printable documents will be installed :

  • /opt/astro/doc/swarp.ps

  Summary

  Resample and combine FITS images in an arbitrary World Coordinate System.

  ---

  tables

  IRAF Tools for processing FITS table data

  Version : 2.3
  Author(s) : STSCI team
  License : STSCI
  Website : http://stsdas.stsci.edu/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 38.10 Mb

  This package requires prior installation of iraf

  Screenshots

  

  Summary

  The TABLES package consists of tasks for handling binary table format data and tasks for reading and writing data in FITS format. The TABLES package is used by other external packages, including STSDAS and the XRAY package available from the Smithsonian Astrophysical Observatory.

  ---

  tinytim

  

  HST PSF generator

  Version : 6.3
  Author(s) : John Krist STSCI
  License : STSCI
  Website : http://www.stsci.edu/software/tinytim/tinytim.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 6.70 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/starttinytim
  
       

  The following printable documents will be installed :

  • /opt/astro/doc/tinytim.ps
  • /opt/astro/doc/tinytim.pdf

  Summary

  Tiny Tim is a program which generates simulated Hubble Space Telescope point spread functions (PSFs). It is written in C and distributed as source code and runs on a wide variety of UNIX and VMS systems. Tiny Tim was written by John Krist. Early NICMOS support was provided by Richard Hook (ST-ECF/ESO).

  Tiny Tim includes mirror zonal errors, time dependent aberrations (for the pre-repair instruments), field dependent obscuration patterns (for WF/PC-1 and WFPC2), and filter passband effects. It can produce a normally sampled or subsampled PSF. Output is a FITS image file.

  ---

  vol

  IRAF Tools for manipulating and viewing 3d or in some cases 4d volume images

  Version : 2.8
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 1.70 Mb

  This package requires prior installation of iraf

  Screenshots

  

  Summary

  The VOLumes package is a possibly temporary collection of tasks related to manipulating and viewing 3d or in some cases 4d "volume" images, and a few other things.

  IMJOIN joins sets of N-dimensional images together along a specified axis. IM3DTRAN performs 3d image transposes; if appropriate [*,-*,*] type image sections are given as input, it also accomplishes rotates. Tasks such as these may later be integrated into a standard IRAF package.

  PVOL projects through volume images, casting rays onto a set of output 2d images distributed along a great circle around the volume image. When the output images are displayed or recorded onto video and played back, the volume image appears to rotate. Various translucency and opacity algorithms are employed.

  I2SUN is a temporary task for converting IRAF images into Sun rasterfiles, primarily to take advantage of a Sun-specific MOVIE utility for viewing digital movies on a workstation screen; it will no longer be necessary when the IRAF image display servers can display movies.

  ---

  wcstools

  

  display and manipulate the world coordinate system of a FITS or IRAF images

  Version : 3.5.3
  Author(s) : Doug Mink (dmink@cfa.harvard.edu)
  License : GPL
  Website : http://tdc-www.harvard.edu/software/wcstools/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 31.16 Mb

  Screenshots

  

  Summary

  WCSTools is a set of software utilities, written in C, which create, display and manipulate the world coordinate system of a FITS or IRAF image, using specific keywords in the image header which relate pixel position within the image to position on the sky. Auxillary programs search star catalogs and manipulate images.21074834

  The 1998 ADASS paper is the best published description of the other tools in the WCSTools package, including SAOimage when used for WCS work: "WCSTools: An Image Astrometry Toolkit", Douglas J. Mink (1998), in Astronomical Data Analysis Software and Systems VIII, A.S.P. Conference Series, Vol. 172, 1999, Dave Mehringer, Ray Plante, Doug Roberts, eds., pp. 498-501.

  Program Descriptions

  addpix Add a constant value(s) to specified pixel(s)

  conpix Operate on all of the pixels of an image

  cphead Copy keyword values between FITS or IRAF images

  delhead Delete specified keywords from FITS or IRAF image file headers

  delwcs Delete the WCS keywords from an image. If both EPOCH and EQUINOX are present, EQUINOX is also deleted.

  edhead Edit the header of a FITS file or the user parameters of an IRAF image file using a the text editor specified by the EDITOR environment variable.

  getcol Extract specified fields from an space-separated ASCII table file

  getdate Convert dates and times between various formats

  gethead Return values for keyword(s) specified after filename.

  getpix Return value(s) of specified pixel(s)

  gettab Extract values from tab table data base files

  i2f Read two-dimensional IRAF image file and write FITS image file

  imcat List catalog sources which should be found in the area of the sky covered by a specific image. Special catalogs supported include the HST Guide Star Catalog, the USNO-A2.0 Catalog, the Tycho-2 Catalog, the SAO Catalog, and the PPM Catalog.

  imextract Extract 1- or 2-dimensional images from 2- or 3-dimensional images

  imhead Print FITS or IRAF header

  immatch Match catalog and image stars using the WCS in the image file.

  imrot Rotate and/or reflect FITS or IRAF image files

  imsize Print center and size of image using WCS keywords in header imcat List catalog sources which should be found in the area of the sky covered by a specific image. Special catalogs supported include the HST Guide Star Catalog, the USNO-A2.0 Catalog, the Tycho-2 Catalog, the SAO Catalog, and the PPM Catalog.

  imextract Extract 1- or 2-dimensional images from 2- or 3-dimensional images

  imhead Print FITS or IRAF header

  immatch Match catalog and image stars using the WCS in the image file.

  imrot Rotate and/or reflect FITS or IRAF image files

  imsize Print center and size of image using WCS keywords in header

  imstack Stack 1-dimensional images into a 2-dimensional image

  imstar Find and list the n brightest stars in an IRAF or FITS image, with their sky coordinates if there is WCS information in the image header.

  imwcs Automaticaly find stars in a FITS or IRAF image, match them to HST Guide or UJC Stars, compute the relation between sky coordinates and image coordinates, and write in in the image header.

  keyhead Change keyword names in headers of FITS or IRAF images.

  newhead Create dataless FITS image header files with BITPIX=0

  remap Remap an image from one WCS into another, rebinning as necessary

  sethead Set header keyword values in FITS or IRAF images.

  setpix Set specified pixel(s) to specified value(s)

  scat Search a source catalog given a region on the sky. Special catalogs supported include the HST Guide Star Catalog, the USNO A and ACT Catalogs, the SAO Catalog, and the PPM Catalog.

  sky2xy Print image pixel coordinates for given sky coordinates on the command line or in a list file.

  skycoor Convert between J2000, B1950, and Galactic coordinates from the command line or a file.

  sumpix Total pixel values over an image row or column or a specified area

  wcshead Print basic world coordinate system information on one line per image

  xy2sky Print sky coordinates for given image pixel coordinates on the command line or in a list file.

  ---

  weightwatcher

  

  WeightWatcher is a program that combines weight-maps, flag-maps and polygon data

  Version : 1.3
  Author(s) : Emmanuel Bertin (bertin@iap.fr)
  License : GPL
  Website : http://terapix.iap.fr/sextractor/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 581.00 Kb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startweightwatcher
  
       

  The following printable documents will be installed :

  • /opt/astro/doc/ww.ps

  Summary

  WeightWatcher is a program that combines weight-maps, flag-maps and polygon data in order to produce control maps which can directly be used in astronomical image-processing packages like Swarp or SExtractor.

  SYNTAX: ww [-c ] [- ]

  ---

  xccdred

  XCCDRED -- Experimental version of CCDRED Package

  Version : 1.0
  Author(s) : Frank Valdes (fvaldes@noao.edu)
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 3.99 Mb

  This package requires prior installation of iraf

  Screenshots

  

  

  Summary

  This external package is an experimental version of the CCDRED package which supports the ARCON multiple readout image format. The only task which has been modified from the V2.10.3beta version is CCDPROC. Note that to make preparing and using this experimental version as easy as possible the task names are unchanged. Therefore, you should avoid loading both XCCDRED and CCDRED at the same time.

  ---

  XDF

  

  Metadata tools

  Version : 1.0
  Author(s) : Various
  License : GPL
  Website : http://xml.gsfc.nasa.gov/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 16.41 Mb

  Summary

  A set of metadeta standards and software aimed at adding an XML dialect for space science and astronomy.

  Includes the following

  jXDF-017-stable-rc1
  XDF_017.dtd
  jFITSML-alpha1_0
  txt2XML-1.61-BETA

  ---

  xdimsum

  Experimental Deep Infrared Mosaicing Software

  Version : 2.12
  Author(s) : Various
  License : AURA
  Website : http://iraf.noao.edu
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 2.26 Mb

  This package requires prior installation of iraf

  Summary

  XDIMSUM is a package for creating accurate sky subtracted images from sets of dithered observations. While the observations need not be in the infrared, the dominance of the variable sky background in infrared data requires dithering of many short exposures and recombination with careful sky subtraction to produce deep images. Hence the package is called "Experimental Deep Infrared Mosaicing Software" or XDIMSUM.

  XDIMSUM is a variant of the DIMSUM package developed by P. Eisenhardt, M. Dickensen, S.A. Stanford, and J. Ward. F. Valdes (IRAF group) modified DIMSUM to support FITS format images, added the DIMSUM tutorial demos script, wrote the original version of this document, and repackaged DIMSUM for distribution as an IRAF external package. L. Davis (IRAF group) rewrote the the major DIMSUM scripts to improve their clarity, robustness, and efficiency, added new scripts for computing relative offsets, and documented the tasks. The new package uses the same default algorithms as DIMSUM but is sufficiently different in format that it has been renamed XDIMSUM. A short summary of the major differences between XDIMSUM and DIMSUM is provided below and is duplicated in the on-line user's guide. XDIMSUM is being made available to the community as an external pacakge in the hope that some of the new features may prove useful to others. Users should direct XDIMSUM installation questions, bug reports, questions about technical details, and comments and suggestions to the the IRAF group (iraf@noao.edu) not the original authors.

  ---

  xite

  

  X based Image processing Tools and Environment

  Version : 3.45
  Author(s) : Svein Bøe. (svein@ifi.uio.no)
  License : GPL
  Website : http://www.ifi.uio.no/~blab/Software/Xite/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 30.92 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startxite
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  XITE consists of display programs with image widget and graphical user interface as well as more than 200 command line programs and 600 subroutines for, all documented on-line. XITE uses its own image file format (BIFF), but comes with converters between BIFF and TIFF, pnm, sunraster, raw, MATLAB and ascii.

  The command line programs and subroutine library are written in C and run under UNIX, Windows NT and Windows 95.

  The display programs run under UNIX. They work with images of arbitrary size and pixel type on 8-bit PseudoColor and 24-bit DirectColor and TrueColor X11 displays. Images can be zoomed and panned, and colortables can be selected from a menu. The main display program, xshow, gives access to most of the other command line programs via a menu interface which the user can customize and extend to include local programs. Input images for the menu entries can be selected with the mouse, and output images appear on the display.

  The available programs include operations such as statistics, merging, resampling, arithmetic/logical/relational operations, rotation, mirroring, affine transformations, convolution, filter design, Fourier/Hartley/Haar/Hough transforms, color manipulation, histogram transformations, global and local thresholding, binary thinning, edge detection, morphological operations, classification, image analysis and texture estimation.

  A toolkit is supplied to simplify development of X11 based applications.

  ---

  xpa

  The XPA messaging system provides seamless communication between many kinds of Unix programs

  Version : 2.1.5
  Author(s) : Doug Mink
  License : GPL
  Website : http://hea-www.harvard.edu/RD/xpa/index.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 2.33 Mb

  Summary

  The XPA messaging system provides seamless communication between many kinds of Unix programs, including X programs and Tcl/Tk programs. It also provides an easy way for users to communicate with these XPA-enabled programs by executing XPA client commands in the shell or by utilizing such commands in scripts. Because XPA works both at the programming level and the shell level, it is a powerful tool for unifying any analysis environment: users and programmers have great flexibility in choosing the best level or levels at which to access XPA services, and client access can be extended or modified easily at any time.

  A program becomes an XPA-enabled server by defining named points of public access through which data and commands can be exchanged with other client programs (and users). Using standard TCP sockets as a transport mechanism, XPA supports both single-point and broadcast messaging to and from these servers. It supports direct communication between XPA clients and servers, or indirect communication via an intermediate message bus emulation program. Host-based access control is implemented, as is as the ability to communicate with XPA servers across a network.

  Because XPA consists of a library and a set of user programs, it is most appropriately built from source. XPA has been ported to Solaris, Linux, Mac OSX (darwin) and Windows 98/NT/2000/XP. Once the source code tar file is retrieved, XPA can be built and installed easily using standard commands:

  ---

  xray

  

  Multi-mission x-ray analysis software system

  Version : 2.5.1
  Author(s) : (rsdc@cfa.harvard.edu)
  License : AURA
  Website : http://hea-www.harvard.edu/PROS/pros.html
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 2
  Disk space required for installation is 41.44 Mb

  This package requires prior installation of iraf

  Screenshots

  

  The following printable documents will be installed :

  • /opt/astro/doc/xray.ps

  Summary

  PROS/XRAY is a multi-mission x-ray analysis software system designed to run under the Image Reduction and Analysis Facility (IRAF).

  The analysis of x-ray data differs from that of other wavelengths due to the nature of x-ray data. The scarcity of data, the low signal-to-noise ratio and the large gaps in exposure time make data screening and masking an important part of the analysis process.

  The PROS software includes spatial, spectral, timing, data I/O and conversion routines, plotting applications, and general algorithms for performing arithmetic operations with imaging data.

  A more complete description of PROS can be found in the PROS User's GUIDE (PUG).

  How PROS is organized

  Programs in PROS are called tasks. Tasks are grouped by function into packages. The major packages in PROS include:

  xdataio - Tasks to convert data to/from FITS format xplot - Plotting routines for XRAY data ximages - Additions to IRAF images package xspatial - X-ray spatial analysis package xspectral - X-ray spectral analysis package xtiming - X-ray timing analysis package

  A diagram of the current package organization is available.

  Brief Overview of PROS analysis tasks

  tv display Tasks display and xdisplay will produce a TV display of the data.

  sky grids The imcontour task calculates and graphs the iso-intensity areas of the images and displays them on a skygrid.

  coordinates Support for the World Coordinate System (WCS) is provided in all the IRAF and PROS tasks. PROS provides additional interfaces to facilitate conversions, including an interactive mode from the image display.

  graphics All non-image output data files from PROS analysis are produced in TABLE format which can be graphed either with the TABLES sgraph task or with the Interactive Graphics Interpreter (igi).

  source detection The detect package is designed to perform Maximum Likelihood Source detection on data exhibiting Poisson statistics. It uses a signal-to-noise threshold calculation.

  PRF modeling The imcalc, immodel and imsmooth tasks provide the ability to generate complex Point Response Function model images that can be convolved with observations.

  data extraction The imcnts task is a utilitarian tool used to extract background subtracted counts from complex regions.

  timing corrections The timcor package provides the conversions from spacecraft clock to UTC and calculation of the barycenter timing correction.

  periodic analysis The tasks ltcurv and fft provide general capabilities to examine periodic data. The period and fold tasks include a provision for a decaying period. The qpphase task generates a QPOE files with an additional event attribute, phase, that then allows the data to be split according to phase.

  spectrum extraction The qpspec task allows users to extract a background corrected spectrum from a QPOE file for use in PROS or for export to other analysis systems.

  model specification and fitting PROS has a flexible spectral model specification language which allows multi-component model fitting. Also, the fit task allows fitting of multiple data sets.

  flux conversion Fluxes for any object can be calculated from the xflux task.

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  xsil

  XSIL means eXtensible Scientific Interchange Language.

  Version : 1.0
  Author(s) : Roy Williams, Caltech, roy@caltech.edu
  License : GPL
  Website : http://www.cacr.caltech.edu/XSIL/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 9.09 Mb

  The following printable documents will be installed :

  • /opt/astro/doc/xsil_spec.pdf

  Summary

  XSIL means eXtensible Scientific Interchange Language.

  How to run the code:

  (1) First unpack the distribution, then set the environment. -- Make sure the JAVA_HOME is correct in the and setup.bat (Windows) or setup.source (Unix) script. This is NOT the location of the executable "java", but the place where the /bin and /lib directories. The "java" executable should be in $JAVA_HOME/bin/java.

  -- Make sure the WEB_BROWSER location is correct in the setup.bat (Windows) or setup.source (Unix) script.

  (2) For Unix users, % source setup.source % Xlook.sh samples/all.xml

  (3) For Windows users, tart a command window, then run the setup, then the batch file Xlook.bat: c: setup c: xlook samples\all.xml

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  xspace

  

  Space Physics Visualization Software Package

  Version : 2.0
  Author(s) : C. T. Russell1 and J. G. Luhmann2, Bryan Littlefield (bryan@igpp.ucla.edu)
  License : UCLA
  Website : http://hdf.ncsa.uiuc.edu/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 1
  Disk space required for installation is 34.52 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startxspace
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  The UCLA Space Physics Group has developed educational software composed of a series of modules to assist students with understanding basic concepts of space plasmas and charged particle motion. Present modules cover planetary magnetospheres, charged particle motion, cold plasma waves, collisionless shock waves, solar wind, magnetospheric currents and the ionosphere. The software is designed around the principle that students can learn more by doing rather than by reading or listening. The programs provide a laboratory-like environment in which the student can control, observe and measure complex behavior. The interactive graphics environment allows the student to visualize the results of his or her experimentation and to try different parameters as desired. Two versions of the software presently exist. One runs on UNIX-based operating systems in an X-windows environment. The other runs on a PC under Linux. This latter version also may be made to run on a Mac.

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  xstar

  N-body simulator

  Version : 2.2
  Author(s) : Wayne Schlitt, (wayne@midwestcs.com)
  License : GPL
  Website : http://www.midwestcs.com/xstar/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 35.18 Mb

  After the package is installed it can be accessed using the command

  
  		/opt/astro/bin/startxstar
  
       

  A shortcut will be installed in the KDE/GNOME desktop menu system,
  as an entry in the Astronomy submenu

  Screenshots

  

  Summary

  This program solves the n-body problem, and displays the results on the screen. It starts by putting a bunch of stars on the screen, and then it lets the inter-body gravitational forces move the stars around. The result is a lot of neat wandering paths, as the stars interact and collide.

  XStar can be used to animate the root window, as a screen saver or just to display stuff in a regular window.

  The XStar N-body Solver

  XStar is a Unix program that simulates the movement of stars. It starts by putting a bunch of stars on the screen, and then it lets the inter-body gravitational forces move the stars around. The result is a lot of neat wandering paths, as the stars interact and collide.

  Figuring out what paths these stars should take is called the "N-Body Problem", and when there are more than 3 stars involved (N>3), this can be a very hard problem to solve. XStar is just a "toy" N-body solver, but it generates a lot of pretty pictures and gives you an idea of how stars interact. "Real" N-body solvers have to work with many thousands, or even millions of stars, while XStar works with dozens.

  Along with the program, there is a fairly large document that explains the N-Body problem in a fair amount of detail. It doesn't get into the gory details of the "real" N-body solvers, but it does give you an overview of the techniques they use.

  All comments, bug reports, bug fixes, enhancements, etc are welcome. Send them to me at wayne@midwestcs.com.

  This program is really a heavily modified version of XGrav, which was written by David Flater (dave@case50.ncsl.nist.gov) and posted to alt.sources on 1/21/95. I liked the program enough that I was really interested in it, but I didn't like it enough to leave it alone. The idea was Dave's, but I don't think too much of his code has been left unchanged. There is probably more untouched code from XSwarm, which Dave used to implement the X port of his n-body problem solving code.

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  YM

  Yale Observatory iMAge Manipulation Application

  Version : 1.4
  Author(s) : David Goldberg (goldberg@astro.yale.edu)
  License : Free
  Website : http://www.astro.yale.edu/yomama/
  

  Installs from Open Source Astronomy for Win32/Cygwin cd 3
  Disk space required for installation is 160.33 Kb

  This package requires Java installation

  Summary

  Welcome to the wonderful world of the Yale Observatory iMAge Manipulation Application, the only tool of its kind which does not require any sort of advanced scripting knowledge for its use!

  Currently, it reads 2 dimensional standard fits files, allows for flat-fielding, dark subtraction, linear and logarithmic scaling of images, arbitrary RGB color scales, combining color images (though, due to security restrictions on Java, the combined images can only be saved in application, not applet form), saving images in progress to a buffer, aperture photometry, centroiding and calculation of radial profiles.

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