Debian Astro Data Reduction packages

Ce paquet fournit un solveur en ligne de commande compact compatible avec la version avec interface graphique d'astap.

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Il n'accepte pas les fichiers bruts et ne fonctionne pas avec SharpCap dans la mesure où le champ de vue n'est pas mémorisé.

• Debian Astronomy Team
• Thorsten Alteholz

• 2022.12.09-1 (bookworm)
• 2024.01.17-1 (trixie)
• 2024.01.17-1 (sid)

• 2 recent
• 43 total installations (of 236266 submissions)

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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.

• D. Lang, D. W. Hogg, K. Mierle, M. Blanton and S. Roweis: Astrometry.net: Blind Astrometric Calibration of Arbitrary Astronomical Images. aj 139:1782-1800 (2010) (eprint)

• Debian Astronomy Team
• Steve Langasek

• 0.76+dfsg-3 (buster)
• 0.93+dfsg-1.1 (sid)
• 0.93+dfsg-1 (trixie)
• 0.93+dfsg-1 (bookworm)
• 0.82+dfsg-1 (bullseye)
• 0.70+dfsg-1 (stretch)
• 0.94 (upstream)

• 110 regular users
• 59 recent
• 1082 total installations (of 236266 submissions)

• astrometry-data-2mass
• astrometry-data-2mass-00
• astrometry-data-2mass-01
• astrometry-data-2mass-02
• astrometry-data-2mass-03
• astrometry-data-2mass-04
• astrometry-data-2mass-05
• astrometry-data-2mass-06
• astrometry-data-2mass-07
• astrometry-data-2mass-08-19
• astrometry-data-tycho2
• astrometry-data-tycho2-07
• astrometry-data-tycho2-08
• astrometry-data-tycho2-09
• astrometry-data-tycho2-10-19

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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.

• Debian Astronomy Team
• Ole Streicher

• 3.13.1-1+deb10u1 (buster)
• 3.13.3+ds-1 (bullseye)
• 3.13.7+ds-1 (trixie)
• 3.13.7+ds-1 (sid)
• 3.13.6+ds-1 (bookworm)
• 3.11-1 (jessie)
• 3.12.3-1 (stretch)

field

astronomy

interface

commandline

role

program

science

calculation

use

converting, organizing

works-with

image, image:raster

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GNU Astronomy Utilities (Gnuastro) is a collection of libraries and programs for astronomical data analysis and manipulation. The programs can be run on the command-line for efficient and easy usage and the libraries can be used within C and C++ programs.

This package contains Gnuastro's programs.

• M. Akhlaghi and T. Ichikawa: Noise-based detection and segmentation of nebulous objects. Astrophysical Journal Supplement Series 220:1 (2015)

• Debian Astro Team
• Steve Langasek

• 0.22-3 (trixie)
• 0.8-1 (buster)
• 0.22-3.1 (sid)
• 0.2.33-1 (stretch)
• 0.14-1 (bullseye)
• 0.19-1 (bookworm)

• 5 regular users
• 2 recent
• 95 total installations (of 236266 submissions)

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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.

• Joseph C. Jacob, Daniel S. Katz, G. Bruce Berriman, John C. Good, Anastasia C. Laity, Ewa Deelman, Carl Kesselman, Gurmeet Singh, Mei-Hui Su, Thomas A. Prince and Roy Williams: Montage - a Grid Portal and Software Toolkit for Science-Grade Astronomical Image Mosaicking. Int. J. Comput. Sci. Eng. 4(2):73-87 (2009)

• Debian Astro Team
• Ole Streicher

• 4.0+dfsg-3 (stretch)
• 6.0+dfsg-9 (sid)
• 6.0+dfsg-6 (buster)
• 6.0+dfsg-7 (bullseye)
• 6.0+dfsg-7 (bookworm)

• 11 regular users
• 2 recent
• 116 total installations (of 236266 submissions)

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This package contrains software to produce a sharp image of a planetary system object (moon, sun, planets) from many seeing-affected frames using the "lucky imaging" technique._

The program is mainly targeted at extended objects (moon, sun), but it works as well for planets. Results obtained in many tests show at least the same image quality as with the established software AutoStakkert!3.

Input to the program can be either video files or directories containing still images. The following algorithmic steps are performed:

• First, all frames are ranked by their overall image quality.
• On the best frame, a rectangular patch with the most pronounced structure in x and y is identified automatically. (Alternatively, the user can select the patch manually as well.)
• Using this patch, all frames are aligned globally with each other.
• A mean image is computed by averaging the best frames.
• An alignment point mesh covering the object is constructed automatically. Points, where the image is too dim, or has too little contrast or structure, are discarded. The user can modify the alignment points, or set them all by hand as well.
• For each alignment point, all frames are ranked by their local contrast in a surrounding image patch.
• The best frames up to a given number are selected for stacking. Note that this list can be different for different points.
• For all frames, local shifts are computed at all alignment points.
• Using those shifts, the alignment point patches of all contributing frames are stacked into a single average image patch.
• Finally, all stacked patches are blended into a global image, using the background image in places without alignment points.
• After stacking is completed, the stacked image can be postprocessed (sharpened) either in a final step of the stacking workflow, or in a separate postprocessing job.

• Debian Astronomy Team
• Thorsten Alteholz

• 0.8.32~git20221019.66d7558-2 (bookworm)
• 0.8.32~git20221019.66d7558-2 (sid)
• 0.8.32~git20221019.66d7558-2 (trixie)
• 0.8.32~git20230901.01f3625 (upstream)

• 3 regular users
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• 38 total installations (of 236266 submissions)

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Astro-SCRAPPY est conçu pour la détection des rayons cosmiques dans des images (tableaux numpy), basée sur l’algorithme L.A.Cosmic de Pieter van Dokkum. La parallélisation est réalisée en utilisant OpenMP.

• van Dokkum, P. G.: Cosmic-Ray Rejection by Laplacian Edge Detection. Publications of the Astronomical Society of the Pacific 113:1427 - 1420 (2001) (eprint)

• Debian Astronomy Team
• Ole Streicher

• 1.0.8-1 (buster)
• 1.0.8-1 (bullseye)
• 1.1.0-2 (bookworm)
• 1.1.0-2 (trixie)
• 1.1.0-2 (sid)
• 1.0.5-1 (stretch)

• 9 regular users
• 3 recent
• 157 total installations (of 236266 submissions)

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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 astropy fits 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.

• O. Streicher and P. M. Weilbacher: Python Bindings for the Common Pipeline Library. Astronomical Data Analysis Software and Systems XXI 461:853 (2012)

• Debian Astronomy Maintainers
• Ole Streicher

• 0.7.4-2 (sid)
• 0.7.4-2 (bookworm)
• 0.7.4-2 (trixie)
• 0.7.2-1 (stretch)
• 0.7.4-2 (buster)
• 0.7.4-2 (bullseye)

• 7 regular users
• 2 recent
• 137 total installations (of 236266 submissions)

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Photutils contains functions for:

• estimating the background and background rms in astronomical images
• detecting sources in astronomical images
• estimating morphological parameters of those sources (e.g., centroid and shape parameters)
• performing aperture and PSF photometry

This package contains the Python 3 version of the package.

• Debian Astronomy Team
• Ole Streicher

• 1.12-1 (sid)
• 1.0.2-1 (bullseye)
• 0.3-3 (stretch)
• 1.6.0-1 (bookworm)
• 0.6-1 (buster)
• 1.11.0-1 (trixie)

• 7 regular users
• 6 recent
• 163 total installations (of 236266 submissions)

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Ce paquet retrouve les sources, telles que les étoiles et les galaxies dans des images astronomiques. Les fichiers de données en entrée sont au format de fichier FITS et sont analysés pour déterminer la position des sources, avec la possibilité de faire la distinction entre une galaxie et une étoile en utilisant une technique de réseau neuronal.

• E. Bertin and S. Arnouts: SExtractor: Software for source extraction. Astronomy and Astrophysics Supplement 117:393-404 (1996) (eprint)

• Debian Astronomy Maintainers
• Ole Streicher

• 2.25.0+ds-3 (bookworm)
• 2.25.0+ds-3 (bullseye)
• 2.28.0+ds-1 (sid)
• 2.28.0+ds-1 (trixie)

• 69 regular users
• 63 recent
• 880 total installations (of 236266 submissions)

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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.

• E. Bertin, Y. Mellier, M. Radovich, G. Missonnier, P. Didelon and B. Morin: The TERAPIX Pipeline. 281:228 (2002)

• Debian Astronomy Maintainers
• Nilesh Patra

• 2.41.5-1 (trixie)
• 2.41.5-1 (sid)
• 2.41.5-1 (bookworm)
• 2.41.4-2 (bullseye)
• 2.38.0+dfsg-4 (buster)
• 2.38.0+dfsg-3 (stretch)
• 2.19.1-1 (jessie)

• 4 regular users
• 2 recent
• 103 total installations (of 236266 submissions)

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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.

• C. Marmo and E. Bertin: MissFITS and WeightWatcher: Two Optimised Tools for Managing FITS Data. 394:619 (2008) (eprint)

• Debian Astronomy Maintainers
• Ole Streicher

• 1.12-1 (stretch)
• 1.12+dfsg-3 (sid)
• 1.12+dfsg-3 (bookworm)
• 1.12+dfsg-2 (bullseye)
• 1.12+dfsg-1 (buster)
• 1.12+dfsg-3 (trixie)

• 3 regular users
• 2 recent
• 90 total installations (of 236266 submissions)

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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 exchangeable masks, long-slit spectroscopy, imaging and spectro-polarimetry and high-time resolution imaging and spectroscopy.

• Debian Astronomy Maintainers
• Ole Streicher

• 5.3.11+dfsg-1 (stretch)
• 5.5.6+dfsg-4 (bullseye)
• 5.5.7+dfsg-2 (sid)
• 5.0.0+dfsg-2 (jessie)
• 5.3.32+dfsg-1 (buster)
• 5.6.5 (upstream)

• 44 total installations (of 236266 submissions)

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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).

• Debian Astronomy Maintainers
• Ole Streicher

• 2.4.11+dfsg-1 (bookworm)
• 2.4.8+dfsg-4 (bullseye)
• 2.4.3+dfsg-1 (buster)
• 1.8.21+dfsg-1 (stretch)
• 1.8.14+dfsg-2 (jessie)
• 2.4.11+dfsg-1 (sid)
• 2.4.11+dfsg-1 (trixie)
• 2.4.13 (upstream)

• 83 total installations (of 236266 submissions)

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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).

• P. M. Weilbacher, O. Streicher, T. Urrutia, A. Jarno, A. Pecontal-Rousset, R. Bacon and P. Böhm: Design and capabilities of the MUSE data reduction software and pipeline. Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series 8451:84510B (2012)

• Debian Astro Team
• Ole Streicher

• 1.6.2+dfsg-1 (stretch)
• 2.8.7+dfsg-3 (trixie)
• 2.8.3+dfsg-4 (bullseye)
• 2.8.7+dfsg-3 (bookworm)
• 2.6+dfsg-1 (buster)
• 2.8.7+dfsg-3 (sid)
• 2.8.9 (upstream)

• 82 total installations (of 236266 submissions)

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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.

• F. Eisenhauer, R. Abuter, K. Bickert, F. Biancat-Marchet, H. Bonnet, J. Brynnel, R.D. Conzelmann, B. Delabre, R. Donaldson, J. Farinato, E. Fedrigo, R. Genzel, N.N. Hubin, C. Iserlohe, M.E. Kasper, M. Kissler-Patig, G.J. Monnet, C. Roehrle, J. Schreiber, S. Stroebele, M. Tecza, N.A. Thatte and H. Weisz: SINFONI - Integral field spectroscopy at 50 milli-arcsecond resolution with the ESO VLT. Instrument Design and Performance for Optical/Infrared Ground-based Telescopes 4841:1548-1561 (2003) (eprint)

• Debian Astronomy Maintainers
• Ole Streicher

• 2.5.2+dfsg-2 (jessie)

• 3 total installations (of 236266 submissions)

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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'.

• Debian Astronomy Maintainers
• Ole Streicher

• 4.1.7+dfsg-2 (sid)
• 4.1.1+dfsg-4 (bullseye)
• 2.9.15+dfsg-1 (jessie)
• 4.1.7+dfsg-2 (trixie)
• 4.1.7+dfsg-2 (bookworm)
• 3.1.7+dfsg-1 (stretch)
• 3.2.3+dfsg-2 (buster)
• 4.1.8 (upstream)

• 81 total installations (of 236266 submissions)

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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.

• Debian Astronomy Maintainers
• Ole Streicher

• 3.2.0+dfsg-1 (buster)
• 3.5.0+dfsg-4 (bullseye)
• 3.5.3+dfsg-1 (sid)
• 2.5.2+dfsg-1 (jessie)
• 2.8.4+dfsg-3 (stretch)
• 3.6.3 (upstream)

• 43 total installations (of 236266 submissions)

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