Debian Science Astronomy packages

Le logiciel AstrOmatic est conçu pour être lancé en mode batch sur de grandes quantités de données, la plupart du temps sur des plateformes Unix, avec un minimum d'intervention humaine. Il est actuellement utilisé dans diverses infrastructures d'étude d'images dont TERAPIX, le système de gestion des données d'étude de l'énergie noire et Astro-WISE.

Ce métapaquet installe tous les logiciels d'AstrOmatic.net empaquetés pour Debian.

Le moteur astrometry prend n'importe quelle image et renvoie le système de coordonnées mondiales (WCS) d’astrométrie, une description basée sur les standards de la transformation entre les coordonnées de l'image et les coordonnées célestes.

Le programme aa calcule les positions orbitales des corps planétaires et réalise des réductions de coordonnées rigoureuses pour l'emplacement apparent géocentrique et topocentrique (altitude et azimuth locaux). Il réduit aussi les positions du catalogue d'étoiles données dans le système FK4 ou FK5. Les données pour les 57 étoiles de navigation sont incluses. La plupart des algorithmes employés viennent du l'Almanach Astronomique (AA) publié par le U.S. Government Printing Office.

Le programme aa suit les algorithmes rigoureux pour la réduction des coordonnées célestes exactement comme expliqué dans les éditions courantes de l'Almanach Astronomique. La réduction vers la place apparente géocentrique a été vérifiée par une version spéciale du programme (aa200) qui prend les positions planétaires directement depuis l'intégration numérique DE200 du système solaire du Jet Propulsion Laboratory. Les résultats sont exactement en accord avec les tables de l'Almanach Astronomique de 1987 et après (les almanachs précédents utilisaient des méthodes de réduction légèrement différentes).

Certains calculs, comme la correction de nutation, ne sont pas donnés explicitement dans le AA mais y sont référencés. Dans ces cas le programme fait les calculs complets qui sont utiles pour construire les tables de l'Almanach (des références sont données).

Le paquet astropy fournit des fonctionnalités centrales et quelques outils communs nécessaires à la conduite de recherches en astronomie et en astrophysique avec Python.

Ce paquet fournit les outils livrés avec astropy :

 − fitscheck : détecte et corrige les violations des standards FITS ;
 − fits2bitmap : crée un fichier bitmap à partir d'une image FITS ;
 − fitsdiff : compare deux fichiers image FITS et rapporte leurs
   différences dans les mots-clés en en-tête et les données ;
 − fitsheader : affiche le(s) en-tête(s) d'un ou plusieurs fichiers sur la
   sortie standard dans un format lisible par un humain ;
 − samp_hub : serveur SAMP Hub ;
 − volint : vérifie qu'un fichier VOTable respecte la spécification
   VOTable ;
 − wcslint : vérifie que les mots-clés WCS d'un fichier FITS respectent
   les standards.

The goal of Milkyway@Home is to use the BOINC platform to harness volunteered computing resources in creating a highly accurate three dimensional model of the Milky Way galaxy using data gathered by the Sloan Digital Sky Survey. This project enables research in both astroinformatics and computer science.

In computer science, the project is investigating different optimization methods which are resilient to the fault-prone, heterogeneous and asynchronous nature of Internet computing; such as evolutionary and genetic algorithms, as well as asynchronous newton methods. While in astroinformatics, Milkyway@Home is generating highly accurate three dimensional models of the Sagittarius stream, which provides knowledge about how the Milky Way galaxy was formed and how tidal tails are created when galaxies merge.

This package contains the Milkyway@home application for the BOINC distributed computing platform. Note that this package has been primarily created for users of architectures for which Milkyway@home does not provide its application. If your architecture is x86 or AMD64 the BOINC client automatically downloads the latest Milkyway@home application if you participate in this project. There is no need to install this package then.

SETI@home est un projet de calcul distribué utilisant des ordinateurs connectés à Internet pour la recherche d'une intelligence extraterrestre (« Search for Extraterrestrial Intelligence » − SETI). Il recherche des preuves potentielles d'intelligence extraterrestre dans les transmissions radio collectées par le télescope radio Arecibo.

Ce paquet fournit l'application SETI@home améliorée pour la plate-forme de calcul distribué BOINC. Le client BOINC télécharge les données radio que l'application SETI@home analyse en recherchant des signaux d'origine extraterrestre. Les résultats sont ensuite renvoyés vers le serveur de SETI@home par le client BOINC.

Ce paquet a été principalement créé pour les utilisateurs d'architectures pour lesquelles SETI@home ne fournit pas pas son application. Pour les architectures x86 et amd64, le client BOINC télécharge automatiquement la dernière application SETI@home si l'utilisateur participe à ce projet. Il n'est alors pas nécessaire d'installer ce paquet, sauf pour évaluer un correctif ou une compilation avec des options différentes sans devoir subir les contraintes techniques. La configuration de BOINC pour trouver l'exécutable local de SETI est accomplie par le paquet.

Ce paquet ne fournit que l'application en ligne de commande. Le paquet boinc-app-seti-graphics fournit l'application graphique.

Le paquet casacore fournit les bibliothèques principales de l'ancien paquet AIPS++/CASA (« Common Astronomy Software Applications »). Cette séparation permet de mieux isoler les bibliothèques principales des applications.

Ce paquet fournit les outils construits avec CASA core :

 – taql : langage de requête pour les tables casacore ;
 – measuresdata : création de tables de données pour les mesures ;
 – imageregrid ;
 – imagecalc ;
 – showtable ;
 – showtablelock ;
 – findmeastable ;
 – fits2table ;
 – imreorder ;
 – casahdf5support ;
 – msselect ;
 – image2fits ;
 – imageslice ;
 – etc.

Celestia est un logiciel libre d'astronomie en 3D. Basé sur le catalogue Hipparcos, il permet d'afficher des objets allant de la taille d'un satellite à celle de galaxies entières en 3 dimensions avec OpenGL. Contrairement à la plupart des logiciels de planétarium, l'utilisateur est libre de se déplacer à travers l'univers.

Ceci est un paquet factice qui sélectionne au moins un frontal pour Celestia.

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.

EsoRex veut dire European Southern Observatory (ESO) Recipe Execution Tool, outil d’exécution de procédés de l’ESO. Il peut lister, configurer et exécuter des « recipes » (procédés) basés sur CPL à partir de la ligne de commande.

CPL (Common Pipeline Library) se compose d’un ensemble de bibliothèques en C ISO fournissant une boîte à outils logicielle complète, efficace et fiable. Elle constitue une base pour la création de tâches automatisées de réduction des données pour l’astronomie.

Une des fonctions fournies par CPL est la possibilité de créer des algorithmes de réduction de données fonctionnant sous forme de greffons (bibliothèques dynamiques). Ceux-ci sont appelés « recipes » (procédés) et sont les éléments principaux de l’environnement CPL de développement de réduction de données.

fitscut is designed to extract cutouts from FITS image format files. FITS, PNG, and JPEG output types are supported. When multiple input files are specified and the output type is PNG or JPEG the resulting image is an RGB color image.

Fitsverify is a computer program that rigorously checks whether a FITS (Flexible Image Transport System) data file conforms to all the requirements defined in Version 3.0 of the FITS Standard document.

Fv provides a graphical user interface to data stored in FITS (Flexible Image Transport System) files. Local files can be created, viewed and edited, files on the internet can be opened read-only through the http and ftp protocols. Through the POWplot program, FITS data can be visualized in a large variety of styles. An interface to the SkyView online database allows for searching, downloading, and plotting of images and object lists for a region of the sky.

Funtools, is a "minimal buy-in" FITS library and utility package developed at the High Energy Astrophysics Division of SAO. The Funtools library provides simplified access to a wide array of file types: standard astronomical FITS images and binary tables, raw arrays and binary event lists, and even tables of ASCII column data. A sophisticated region filtering library (compatible with ds9) filters images and tables using boolean operations between geometric shapes, support world coordinates, etc. Funtools also supports advanced capabilities such as optimized data searching using index files.

This package contains the tools.

Gcx is an astronomical image processing and data reduction tool, with an easy to use graphical user interface. It provides a complete set of data reduction functions for CCD photometry, with frame WCS fitting, automatic star identification, aperture photometry of target and standard stars, single-frame ensemble photometry solution finding, multi-frame color coefficient fitting, extinction coefficient fitting, and all-sky photometry; as well as general-purpose astronomical image processing functions (bias, dark, flat, frame alignment and stacking); It can function as a FITS viewer.

The program can control CCD cameras and telescopes, and implement automatic observation scripting. Cameras are controlled through a hardware-specific server, to which gcx connects through a TCP socket. It generates FITS files with comprehensive header information.

The IDL Astronomy Users Library is a central repository for low-level astronomy software written in the GNU Data Language (GDL). The library is not meant to be an integrated package, but rather is a collection of procedures from which users can pick and choose (and possibly modify) for their own use. Submitted procedures are given a cursory testing, but are basically stored in the library as submitted.

The library was originally written for the commercial IDL interpreter, but large parts are usable with the GDL interpreter as well. Other names for the libraries are "astron" and "idlastro".

The Coyote Library evolved from work David Fanning was doing teaching IDL courses and answering IDL questions on the IDL newsgroup. It is meant to be a well-documented library that demonstrates how to write solid IDL/GDL programs that are easy to maintain and extend.

The main content of the library is the Coyote Graphics System (CGS), a collection of Coyote Library programs that turn the traditional GDL/IDL graphics commands (e.g., Plot, Contour, Surface, TV, etc.) into modern programs.

The most important features of Coyote Graphics System are:

• The commands work identically on the display, in PostScript, and in the Z-graphics buffer.
• The commands can be displayed automatically in resizable graphics windows.
• The commands automatically create high quality PostScript, PDF, and raster file output.
• CGS graphics visualizations can be saved and restore later, or e-mailed to colleagues.
• The commands work identically in an indexed or decomposed color environment.
• The commands can use colors by name (e.g., "red", "dodger blue").
• CGS commands are faster (often much faster) than the equivalent IDL function graphics commands.
• Greek letters and other symbols can be directly embedded in Coyote Graphics text.
• The commands fix the most annoying quirks (e.g., contour holes and levels) in traditional IDL commands.

These GDL routines provide a robust and relatively fast way to perform least-squares curve and surface fitting. The algorithms are translated from MINPACK-1, which is a rugged minimization routine found on Netlib, and distributed with permission. This algorithm is more desirable than CURVEFIT because it is generally more stable and less likely to crash than the brute-force approach taken by CURVEFIT, which is based upon Numerical Recipes.

MPFIT has additional capabilities not found in CURVEFIT. Model parameters can be "frozen" (that is, held constant during the fitting process). Simple boundary constraints can be imposed on parameter values, which can be helpful to keep parameters from becoming negative, for example. Please see the documentation for the PARINFO keyword if you wish to use this facility.

GNU Data Language (GDL) is a free IDL (Interactive Data Language) compatible incremental compiler. It has full syntax compatibility with IDL 7.1. IDL is a registered trademark of ITT Visual Information Solutions. From IDL 8.0, the following language elements are supported:

• FOREACH loop
• negative array indices
• garbage collection pointers and objects
• call methods on an object using "." (e. g. object.aMemberProcedure,arg1)

The file input output system is fully implemented. GUI support (widgets) is officially provided, but it's not complete yet.

This package contains the main commandline and interpreter frontend.

Gpredict is a real time satellite tracking and orbit prediction program for the Linux desktop. It uses the SGP4/SDP4 propagation algorithms together with NORAD two-line element sets (TLE).

Some core features of Gpredict include:

• Tracking of a large number of satellites only limited by the physical memory and processing power of the computer
• Display the tracking data in lists, maps, polar plots and any combination of these
• Have many modules open at the same either in a notebook or in their own windows. The modules can also run in full-screen mode
• You can use many ground stations
• Predict upcoming passes
• Gpredict can run in real-time, simulated real-time (fast forward and backward), and manual time control
• Detailed information both the real time and non-real time modes
• Doppler tuning of radios via Hamlib rigctld
• Antenna rotator control via Hamlib rotctld

Gyoto is a framework for computing geodesics in curved space-times. The gyoto utility program uses this framework to compute images of astronomical objects in the vicinity of compact objects (e.g. black-holes). Such images are distorted by strong gravitational lensing. The gyoto program takes a scenery description in XML format, computes this scenery using relativistic ray-tracing, and saves the result in FITS format.

This metapackage depends on all the Gyoto interfaces (command-line, Yorick, Python 2 and 3).

MPI parallelization requires the mpi-default-bin package. The Gyoto documentation is provided in the gyoto-doc package.

INDI (Instrument-Neutral Device Interface) is a distributed XML-based control protocol designed to operate astronomical instrumentation. INDI is small, flexible, easy to parse, scalable, and stateless. It supports common DCS functions such as remote control, data acquisition, monitoring, and a lot more.

This package contains the INDI server, the drivers for the supported astronomical instrumentation, and other INDI tools.

IRAF is the "Image Reduction and Analysis Facility". The main IRAF distribution includes a good selection of programs for general image processing and graphics.

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 the programmable Command Language scripting facility.

KStars is a scientifically accurate desktop planetarium, visualising a graphical simulation of the night sky from any location on Earth, at any date and time. The display includes 130,000 stars, 13,000 deep-sky objects, all 8 planets, the Sun and Moon, and thousands of comets and asteroids. KStars addresses students and amateur astronomers of all levels.

The database of known objects can be extended and updated from local or remote databases, which is prepared for in a user-extendable interface. KStars suggests observations of particular interest like conjunctions with respect to the location of the user. And for user-selected targets it proposes the ones that are best-observable.

The software may be used for planning experiments around the globe, e.g. for remote controlled commercial services. But KStars also features an INDI interface to control local telescopes and cameras. Users with programming experience can script it via the KDE desktop bus.

This package is part of the KDE education module.

Light Speed! is an OpenGL-based program which illustrates the effects of special relativity on the appearance of moving objects. When an object accelerates past a few million meters per second, these effects begin to grow noticeable, becoming more and more pronounced as the speed of light is approached. These relativistic effects are viewpoint-dependent, and include shifts in length, object hue, brightness and shape.

The moving object is, by default, a geometric lattice. 3D Studio and LightWave 3D objects may be imported as well. Best of all, the simulator is completely interactive, rendering the exotic distortions in real-time!

Lynkeos is an application dedicated to the processing of astronomical (mainly planetary) images taken with a webcam through a telescope. By stacking the best images, the signal to noise ratio is increased and details lost in the noise of individual images become visible in the resulting image.

MissFITS is a program that performs basic maintenance and packaging tasks on FITS files using an optimised FITS library. MissFITS can:

• add/edit/remove FITS header keywords
• split/join Multi-Extension-FITS (MEF) files
• unpile/pile FITS data-cubes
• create/check/update FITS checksums, using R. Seaman’s protocol.

Montage is a toolkit for assembling astronomical images into custom mosaics.

It uses algorithms that preserve the calibration and positional (astrometric) fidelity of the input images to deliver mosaics that meet user-specified parameters of projection, coordinates, and spatial scale. It supports all projections and coordinate systems in use in astronomy.

It contains independent modules for analyzing the geometry of images on the sky, and for creating and managing mosaics; these modules are powerful tools in their own right and have applicability outside mosaic production, in areas such as data validation.

OpenUniverse (OU pour faire court) est un simulateur d'espace OpenGL amusant, rapide et libre. Il est actuellement focalisé sur le système solaire et vous permet de visiter toutes ses planètes, la plupart des lunes majeures et un grand choix de petits corps en 3D colorisée, magnifique et temps réel. Si vous n'avez jamais eu la chance de visiter Mercure ou l'astéroïde Geographos, ici, vous allez les voir de la même manière, suivre exactement le même chemin que si vous y étiez.

Notez que OpenUniverse n'est actuellement plus maintenu activement et que les utilisateurs sont invités à utiliser Celestia à la place.

Predict est un programme de suivi de satellites. Il est principalement destiné aux utilisateurs de satellites amateurs, mais gère l'indication facultative de l’azimut et de l'élévation afin de permettre le pointage manuel d'antennes ou l'observation optique des satellites.

Les sources d’amont de predict incluent un frontal appelé « map », qui est appelé predict-map dans les paquets Debian.

Il est suggéré d'utiliser le paquet « ntp » car le suivi précis de satellites impose une connaissance précise de l'heure et emplacement de stations au sol.

Extract models of the Point Spread Function (PSF) from FITS images processed with SExtractor, and measures the quality of images. The generated PSF models can be used for model-fitting photometry or morphological analyses.

astLib is a set of Python modules that provides some tools for research astronomers. It can be used for astronomical plots, some statistics, common calculations, coordinate conversions, and manipulating FITS images with World Coordinate System (WCS) information through PyWCSTools - a simple wrapping of WCSTools by Jessica Mink. PyWCSTools is distributed (and developed) as part of astLib.

The astropy package contains core functionality and some common tools needed for performing astronomy and astrophysics research with Python. It can be extended by a number of "affiliated packages" that are intended to work with the core package.

Astroquery is a set of Python tools for querying astronomical web forms and databases.

This is the Python 2 version of the package.

This module can list, configure and execute CPL-based recipes from Python3. The input, calibration and output data can be specified as FITS files or as pyfits objects in memory.

The Common Pipeline Library (CPL) comprises a set of ISO-C libraries that provide a comprehensive, efficient and robust software toolkit. It forms a basis for the creation of automated astronomical data-reduction tasks.

One of the features provided by the CPL is the ability to create data-reduction algorithms that run as plugins (dynamic libraries). These are called "recipes" and are one of the main aspects of the CPL data-reduction development environment.

The XPA messaging system provides seamless communication between many kinds of Unix programs, including Tcl/Tk programs such as ds9. The pyds9 module uses a Python interface to XPA to communicate with ds9. It supports communication with all of ds9’s XPA access points.

This package provides the Python-2 version of the package.

FITS (Flexible Image Transport System) is a data format most used in astronomy. PyFITS is a Python module for reading, writing, and manipulating FITS files. The module uses Python's object-oriented features to provide quick, easy, and efficient access to FITS files. The use of Python's array syntax enables immediate access to any FITS extension, header cards, or data items.

Note that the development of PyFITS has been stopped and will not see any new upstream version. It is superseded by the module astropy.io which is almost a drop-in replacement. PyFITS should therefore only be used for compatibility reasons, astropy should be used instead for new developments.

This package provides PyFITS on the Python 2 module path. It is complemented by python3-pyfits.

This is a thin wrapper around the high- and mid-level interfaces of Dr. Mark Calabretta's WCSLIB for handling the World Coordinate System.

In addition, there are extensions (written in C) to support Spitzer Simple Imaging Polynomial (SIP) convention keywords and Paper IV table lookup distortion.

The spectral-cube package provides an easy way to read, manipulate, analyze, and write data cubes with two positional dimensions and one spectral dimension, optionally with Stokes parameters. It aims to be a versatile data container for building custom analysis routines.

This package contains the Python 2 version of the package.

astLib is a set of Python3 modules that provides some tools for research astronomers. It can be used for astronomical plots, some statistics, common calculations, coordinate conversions, and manipulating FITS images with World Coordinate System (WCS) information through PyWCSTools - a simple wrapping of WCSTools by Jessica Mink. PyWCSTools is distributed (and developed) as part of astLib.

The astropy package contains core functionality and some common tools needed for performing astronomy and astrophysics research with Python3. It can be extended by a number of "affiliated packages" that are intended to work with the core package.

Astroquery is a set of Python tools for querying astronomical web forms and databases.

This is the Python 3 version of the package.

FITS (Flexible Image Transport System) is a data format most used in astronomy. PyFITS is a Python module for reading, writing, and manipulating FITS files. The module uses Python's object-oriented features to provide quick, easy, and efficient access to FITS files. The use of Python's array syntax enables immediate access to any FITS extension, header cards, or data items.

Note that the development of PyFITS has been stopped and will not see any new upstream version. It is superseded by the module astropy.io which is almost a drop-in replacement. PyFITS should therefore only be used for compatibility reasons, astropy should be used instead for new developments.

This package provides PyFITS on the Python 3 module path. It is complemented by python-pyfits.

The spectral-cube package provides an easy way to read, manipulate, analyze, and write data cubes with two positional dimensions and one spectral dimension, optionally with Stokes parameters. It aims to be a versatile data container for building custom analysis routines.

This package contains the Python 3 version of the package.

Qfits est une bibliothèque autonome écrite en C pour interagir avec les fichiers se conformant au format FITS, celui-ci étant le format de données le plus utilisé en astronomie.

Ce paquet fournit des outils pour des manipulations simples de fichiers FITS.

Rawtran is an utility to convert of raw photos in .CR2, .CRW, MRW, NEF, RAF, etc. formats to the general astronomical FITS image format. The identification of raw photo type and decoding itself is done via DCRAW utility by D.Coffin.

SAOImage DS9 is an astronomical imaging and data visualization application. DS9 supports FITS images and binary tables, multiple frame buffers, region manipulation, and many scale algorithms and colormaps. It provides for easy communication with external analysis tasks and is highly configurable and extensible via XPA and SAMP.

All versions and platforms support a consistent set of GUI and functional capabilities.

DS9 supports advanced features such as 2-D, 3-D and RGB frame buffers, mosaic images, tiling, blinking, geometric markers, colormap manipulation, scaling, arbitrary zoom, cropping, rotation, pan, and a variety of coordinate systems.

The GUI for DS9 is user configurable. GUI elements such as the coordinate display, panner, magnifier, horizontal and vertical graphs, button bar, and color bar can be configured via menus or the command line.

SaVi permet de simuler l’orbite et la couverture de satellites, en deux ou trois dimensions. SaVi est particulièrement utile dans la simulation de constellations de satellites telles Iridium et Globalstar.

SaVi peut utiliser Geomview, un paquet facultatif mais utile, pour le rendu 3D.

SCAMP reads SExtractor catalogs and computes astrometric and photometric solutions for any arbitrary sequence of FITS images in a completely automatic way.

Seesat5 utilise l'algorithme sgp4 du NORAD pour calculer la position d'un satellite. Plusieurs méthodes de filtrage sont fournies par Seesat5 afin que seuls les satellites qui peuvent être réellement vus soient présentés dans le rapport. Ce dernier inclut l'orientation et le site en fonction de la position de l'observateur ainsi que d'autres informations pouvant lui être utiles.

Même si un observateur n'en a pas l'usage, le programme peut être utilisé pour rapporter la position même si elle se trouve sous l'horizon. Pour des satellites radio comme la série des Oscar, l'instant d'émergence au-dessus de l'horizon est l'une des informations intéressantes que ce programme peut fournir.

Find sources, such as stars and galaxies, in astronomical images. The input data files are in FITS file format, and are analyzed to compute the locations of sources, with the ability to distinguish between galaxies and stars using a neural-network technique.

Siril is an image processing tool specially tailored for noise reduction and improving the signal/noise ratio of an image from multiple captures, as required in astronomy. Siril can align automatically or manually, stack and enhance pictures from various file formats, even images sequences (movies and SER files).

The ESO/Starlink Skycat tool combines the image display capabilities of the RTD (Real-Time Display) with a set of classes for accessing astronomical catalogs locally and over the network using HTTP. The tool allows you to view FITS images from files or from the Digitized Sky Survey (DSS).

This (formerly SUPERSPHPLOT) is a visualisation tool for output from (astrophysical) simulations using the Smoothed Particle Hydrodynamics (SPH) method in one, two and three dimensions. It is written in Fortran 90 and can utilise the PGPLOT graphics subroutine library to do the actual plotting. It is based around a command-line menu structure but utilises the interactive capabilities of PGPLOT to manipulate data interactively in the plotting window.

This package allows the installation and removal of astronomy catalogues, converting those catalogues to astronomy programs' data formats.

All stardata catalogues conforming to stardata-common policy are converted automatically at installation time to the formats of astronomy programs that support stardata-common.

The register-stardata program is transparent for the user; this program is called automatically when any astronomy package conforming to the stardata-common policy is installed, upgraded or removed.

StarPlot est un programme basé sur GTK+ qui peut être utilisé de manière interactive pour voir les cartes stellaires en perspective 3D. Ces graphiques peut être recentrés, tournés, zoomés ou dézoomés avec un clic de la souris (ceci peut aussi bien sûr être réalisé avec des boîtes de dialogue pour plus de précision). Les étoiles peuvent être visualisées (ou ignorées) par classe spectrale ou magnitude absolue.

StarPlot et empaqueté avec starconvert, un utilitaire qui convertit les enregistrements stellaires orientés en ligne dans le format de StarPlot. La plupart des données d'étoiles disponibles peuvent être converties de cette manière si un petit fichier qui décrit le format initial est fourni à starconvert.

Stellarium réalise des rendus 3D photo réalistes du ciel en temps réel. Il permet de voir vraiment ce qui serait vu à l'œil nu, avec des jumelles ou un petit télescope.

Quelques caractéristiques :

 — catalogue d’étoiles par défaut avec plus de 600.000 étoiles ;
 — information sur les étoiles les plus brillantes (type spectral,
   distance, etc.) ;
 — suppléments du catalogue d’étoiles téléchargeable (plus de 210 millions
   d’étoiles) ;
 — objets du Nouveau Catalogue Général en entier ;
 — images de la plupart des objets du catalogue Messier et de la Voie lactée ;
 — positions en temps réel des planètes et de leurs satellites ;
 — 13 cultures différentes et leurs constellations ;
 — illustrations artistiques de 88 constellations occidentales ;
 — atmosphère très réaliste, lever et coucher de soleil ;
 — 7 panoramas (possibilité d’en créer d’autres ou d’en télécharger à partir du
   site web ;
 — création de scripts avec ECMAScript ;
 — prise en charge de greffons : Stellarium est fourni avec 8 greffons
   comprenant :
    — greffon pour les satellites artificiels (mise à jour à partir de la base
      de données en ligne TLE),
    — greffon de simulation oculaire (affichage de ce à quoi les objets
      ressemblent avec un oculaire donné),
    — greffon pour l’édition du Système solaire (importation des données de
      comètes et astéroïdes à partir du MPC),
    — greffon de contrôle de télescope (compatible avec LX200 de Meade et
      NexStar de Celestron).

Stellarium ne doit pas être utilisé pour des calculs de grande précision ou des éphémérides, tels que les prédictions d'éclipse. Cependant, c'est un programme idéal pour préparer une soirée d'observation à l'œil nu, aux jumelles, ou avec un petit télescope.

STIFF is a program that converts scientific FITS images to the TIFF format for illustration purposes. The main features of STIFF are:

• Accurate reproduction of the original surface brightnesses and colours
• Automatic or manual contrast and brightness adjustments
• Automatic sky background intensity and colour balance
• Adjustable colour saturation
• Colour-friendly gamma correction capabilities
• One or three input channels: gray-scale or true colour output
• Output with 8 or 16 bits per component
• Pixel rebinning and x/y flip options
• Support for arbitrarily large input and output images on standard hardware (BigTIFF support)
• Support for tiled, multiresolution pyramids
• Support for lossless and lossy compression methods
• Multi-threaded code with load-balancing to take advantage of multiple cores and processors.
• XML VOTable-compliant output of meta-data.

Resample and co-add together FITS images using any arbitrary astrometric projection defined in the WCS standard. The main features of SWarp are:

• FITS format (including multi-extensions) in input and output,
• Full handling of weight-maps in input and output,
• Ability to work with very large images (up to 500 Mpixels on 32-bit machines and 10^6 Tpixels with 64-bits), thanks to customized virtual-memory-mapping and buffering,
• Works with arrays in up to 9 dimensions (including or not two spherical coordinates),
• Selectable high-order interpolation method (up to 8-tap filters) in any dimension,
• Compatible with WCS and TNX (IRAF) astrometric descriptions,
• Support for equatorial, galactic and equatorial coordinate systems,
• Astrometric and photometric parameters are read from FITS headers or external ASCIIfiles,
• Built-in background subtraction,
• Built-in noise-level measurement for automatic weighting,
• Automatic centering and sizing functions of the output field,
• Multi-threaded code with load-balancing to take advantageof multiple processors.
• XML VOTable-compliant output of meta-data.

WCSLIB is a C library, supplied with a full set of Fortran wrappers, that implements the "World Coordinate System" (WCS) standard in FITS (Flexible Image Transport System).

This package contains the utility programs fitshdr, wcsware, HPXcvt, and wcsgrid that are included in wcslib.

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. Auxiliary programs search star catalogs and manipulate images.

This package contains the binary tools.

WeightWatcher est un programme qui combine les données des cartes de poids, cartes de marques et polygones dans le but de produire des « cartes de contrôle » pouvant être utilisées dans les paquets de traitement d’images pour l’astronomie tels Drizzle, Swarp or SExtractor.

Des seuils de poids ou les sélections de marques spécifiques sont appliqués par WeightWatcher à l’aide d’un fichier de configuration : cela allège les autres programmes d’un tel travail d’interprétation. WeightWatcher sera principalement utile comme partie dans un pipeline de levé d’image. Ses principales caractéristiques sont :

 – vitesse de traitement limitée par les performances d’E/S de la machine
 (valeur courante 50 Mpixel/s sur une station de travail) ;
 – possibilité de travailler de très grandes images (de l’ordre de
 10^8 × 10^9 pixels sur un système 64 bits) ;
 – utilisation du format FITS (avec différentes extensions) pour les entrées
 et sorties. La sélection du format de sortie carte de marques est
 automatique (8, 16 ou 32 bits) ;
 – gestion simultanée jusqu’à 30 cartes de poids, 30 cartes de marques et
 des milliers de polygones ;
 – matricialisation automatique des fichiers .reg DS9 ;
 – statistiques pour les régions traitées avec des marques et des poids ;
 – sortie des métadonnées au format XML-VOTable.

WxAstroCapture peut contrôler des appareils photographiques pour de l'imagerie de planète, lune, soleil et autres objets du ciel profond. De longues expositions sont prises en charge pour des caméras « SC-modified » avec contrôle de l'exposition par les ports série ou parallèle. Sont aussi pris en charge les appareils ATK et Artemis pour l'imagerie 16 bits du ciel profond et l'autoguidage d'appareils pour des expositions normales ou prolongées.

Orbit Reconstruction, Simulation and Analysis (ORSA) is a framework for Celestial Mechanics investigations. The main goals of the project are the implementation of state of the art orbit integration algorithms, with concerns on accuracy and performance, and the development of a number of analysis tools.

This package contains xorsa, the main graphical application provided by the ORSA project. It is an interactive tool for scientific grade Celestial Mechanics computations. Asteroids, comets, artificial satellites, Solar, and extra-Solar planetary systems can be accurately reproduced, simulated and analyzed.

Le système de messages XPA fournit des communications ininterrompues entre plusieurs types de programme Unix, y compris les programmes X et Tcl/Tk. Il fournit aussi une manière facile pour les utilisateurs de communiquer avec ces programmes compatibles XPA, en exécutant des commandes de client dans un interpréteur de commandes ou en utilisant de telles commandes dans des scripts. XPA, pouvant s’exécuter soit au niveau programmation, soit au niveau interpréteur de commandes, est donc un outil puissant pour unifier tout environnement d’analyse : les utilisateurs et les programmeurs peuvent choisir de manière très flexible le(s) meilleur(s) niveau(x) pour accéder aux services XPA, et l’accès client peut être étendu ou modifié facilement et n’importe quand.

Ce paquet ajoute des outils.

Xplanet crée une image de planète dans une fenêtre X ou dans un fichier. Toutes les principales planètes et la plupart des satellites peuvent être dessinés, et différentes projections cartographiques sont prises en charge, dont les types azimutal, hémisphérique, Lambert, Mercator, Mollweide, Peters, polyconique et rectangulaire.

Au moins un fichier de carte est nécessaire pour utiliser xplanet. Un certain nombre de cartes est fourni dans le paquet xplanet-images.

Xplanet crée une image de planète dans une fenêtre X ou dans un fichier.

Au moins un fichier de carte est nécessaire pour utiliser xplanet. Ce paquet contient un certain nombre de fichiers qui peuvent être utilisés avec xplanet.

Yorick est un langage de programmation interprété pour :

• les simulations scientifiques et les calculs ;
• le post-traitement ou le guidage de grands codes de simulation ;
• les graphiques scientifiques interactifs ;
• la lecture, l'écriture et la traduction de grands fichiers de nombres.

Le méta-paquet yorick-full installe yorick ainsi que tous les greffons empaquetés pour Debian.

Il peut être préférable de n'installer que le paquet yorick et les greffons yorick-* nécessaires.

Si vous désirez MPY, la version parallèle MPI de Yorick, veuillez installer en plus yorick-mpy-openmpi ou yorick-mpy-mpich2.

This is the data reduction pipeline for the AMBER instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

AMBER is a near-infrared, multi-beam interferometric instrument, combining simultaneously up to 3 telescopes. AMBER can be used in Period 82 and following with UTs or ATs. All possible triplets of UTs are available, and a number of selected AT combinations.

FORS pipeline recipes for the reduction of data obtained with the FORS1 and FORS2 instruments in the LSS, MOS, MXU, PMOS, and direct imaging instrument modes.

FORS is the visual and near UV FOcal Reducer and low dispersion Spectrograph for the Very Large Telescope (VLT) of the European Southern Observatory (ESO). Two versions of FORS have been built, upgraded and moved to the Cassegrain foci of different telescopes in the past years. In April 2009, FORS1 was dismounted to make room for X-shooter, so only FORS2 is in operation. FORS is designed as an all-dioptric instrument for the wavelength range from 330 nm to 1100 nm and provides an image scale of 0".25/pixel (or 0".125/pixel with the high resolution collimator) in the standard readout mode (2x2 binning). FORS2 is installed on UT1 (Antu) and is by default equipped with a detector system that is optimised for the red with a very low level of fringes thanks to a mosaic of two 2k x 4k MIT CCDs (with 15 μm pixels). However, the blue-optimised detector system that was previously available on FORS1 has been commissioned on FORS2 and can be requested for Visitor Mode observation. The geometries of both detector systems are similar, with the optical axis falling ~30" above the gap and offsets of a few arc-seconds between the two chips. FORS2 has many modes, including multi-object spectroscopy with exchangable masks, long-slit spectroscopy, imaging and spectro-polarimetry and high-time resolution imaging and spectroscopy.

This is the data reduction pipeline for the GIRAFFE instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

GIRAFFE is a medium-high resolution (R=7500-30000) spectrograph for the entire visible range 370-900 nm. GIRAFFE is aimed at carrying out intermediate and high resolution spectroscopy of galactic and extragalactic objects having a high spatial density. The name comes from the first design, where the spectrograph was standing vertically on a platform.

This is the data reduction pipeline for the HAWK-I instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

HAWK-I is a near-infrared (0.85-2.5 μm ) wide-field imager. It is being offered for the first time in Period 81. The instrument is cryogenic (120 K, detectors at 80 K) and has a full reflective design. The light passes four mirrors and two filter wheels before hitting a mosaic of four Hawaii 2RG 2048 * 2048 pixels detectors. The final F-ratio is F/4.36 ( 1 arcsec on the sky corresponds to 169 μm on the detector).

This is the data reduction pipeline for the KMOS instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

The K-band Multi Object Spectrograph (KMOS) is a second-generation instrument designed for operation on the VLT. The key feature of KMOS is its ability to perform Integral Field Spectroscopy in the near-infrared bands for 24 targets simultaneously.

This is the data reduction pipeline for the Muse instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

MUSE, the Multi-Unit Spectroscopic Explorer, is an Integral Field Spectrograph located at the Nasmyth B focus of Yepun, the VLT UT4 telescope. It has a modular structure composed of 24 identical IFU modules that together sample, in Wide Field Mode (WFM), a near-contiguous 1 squared arcmin field of view. Spectrally the instrument samples almost the full optical domain with a mean resolution of 3000. Spatially, the instrument samples the sky with 0.2 arcseconds spatial pixels in the currently offered Wide Field Mode with natural seeing (WFM-noAO).

This is the data reduction pipeline for the NaCo instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

NaCo is short for NAOS-CONICA. It was installed at the Nasmyth B focus of UT4 from 2001 through 2013. In 2014 it was reinstalled on UT1 at the Nasmyth A. It provides adaptive optics assisted imaging, imaging polarimetry, coronography and spectroscopy, in the 1-5 micron range.

This is the data reduction pipeline for the SINFONI instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

SINFONI is a near-infrared (1.1 - 2.45 µm) integral field spectrograph fed by an adaptive optics module, currently installed at the Cassegrain focus of UT4. The spectrograph operates with 4 gratings (J, H, K, H+K) providing a spectral resolution around 2000, 3000, 4000 in J, H, K, respectively, and 1500 in H+K - each wavelength band fitting fully on the 2048 pixels of the Hawaii 2RG (2kx2k) detector in the dispersion direction. The spatial resolution is selectable from 0.25", 0.1" to 0.025" per image slice, which corresponds to a field-of-view of 8"x8", 3"x3", or 0.8"x0.8" respectively. The instrument can be also used for seeing limited open loop observations.

This is the data reduction pipeline for the UVES instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

UVES is a cross-dispersed echelle spectrograph designed to operate with high efficiency from the atmospheric cut-off at 300 nm to the long wavelength limit of the CCD detectors (about 1100 nm). The light beam from the telescope is split in two arms (UV to Blue, and Visual to Red) within the instrument. The two arms can be operated separately, or in parallel via a dichroic beam splitter. The resolving power is about 40,000 when a 1-arcsec slit is used. The maximum (two-pixel) resolution is 80,000 or 110,000 in the Blue- and the Red Arm, respectively.

This is the data reduction pipeline for the Vimos instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

VIMOS is a multi-mode wide-field optical instrument mounted at the Nasmyth focus B of UT3. VIMOS allows imaging in UBVRIz and multi-object low (R ~ 200) to high (R ~ 2500) resolution spectroscopy. The wavelength range covered in the two spectroscopic modes goes from 360 to 1000 nm. VIMOS is made of 4 quadrants of 7'x8' each separated by a gap of about 2'.

This is the data reduction pipeline for the Visir instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

The VLT spectrometer and imager for the mid-infrared (VISIR) was built by CEA/DAPNIA/SAP and NFRA/ASTRON, and is located at the Cassegrain focus of UT3. It provides diffraction-limited imaging at high sensitivity in the two mid infrared (MIR) atmospheric windows: the N band between 8 to 13μm and the Q band between 16.5 and 24.5μm, respectively. In addition, it features a long-slitspectrometer with a range of spectral resolutions between 150 and 30000.

This is the data reduction pipeline for the XSHOOTER instrument of the Very Large Telescope (VLT) from the European Southern Observatory (ESO).

XSHOOTER is a multi wavelength (300-2500nm) medium resolution spectrograph mounted at the UT2 Cassegrain focus. XSHOOTER consists of 3 arms, each with optimized optics, dispersive elements and detectors:

• UVB, covering the wavelength range 300-559.5 nm,
• VIS, covering the wavelength range 559.5-1024 nm,
• NIR, covering the wavelength range 1024-2480 nm.

PDL gives standard perl the ability to COMPACTLY store and SPEEDILY manipulate the large N-dimensional data arrays which are the bread and butter of scientific computing. The idea is to turn perl in to a free, array-oriented, numerical language in the same sense as commercial packages like IDL and MatLab. One can write simple perl expressions to manipulate entire numerical arrays all at once. For example, using PDL the perl variable $a can hold a 1024x1024 floating point image, it only takes 4Mb of memory to store it and expressions like $a=sqrt($a)+2 would manipulate the whole image in a few seconds.

A simple interactive shell (perldl) is provided for command line use together with a module (PDL) for use in perl scripts.

HEALPix is an acronym for Hierarchical Equal Area isoLatitude Pixelization of a sphere. As suggested in the name, this pixelization produces a subdivision of a spherical surface in which each pixel covers the same surface area as every other pixel. It is commonly used to store all-sky astronomical images, most famously maps of the cosmic microwave background.

This package provides a Python wrapper around the C++ implementation of HEALPix.

ScientificPython is a collection of Python modules that are useful for scientific computing. Most modules are rather general, others belong to specific domains and will be of interest to only a small number of users (e.g. the module Scientific.IO.PDB). Almost all modules make extensive use of Numerical Python (NumPy)