Debian Astro ASCL packages

ALFA measures fluxes in emission line spectra, such as those of planetary nebulae and HII regions, using a genetic algorithm to rapidly optimise fits to large numbers of lines simultaneously. It can subtract night sky emission lines before fitting the nebular lines if necessary. It can read plain text files containing 1D spectral data, or FITS files containing 1D, 2D or 3D datasets.

• Wesson, R.: ALFA: an automated line fitting algorithm. Monthly Notice of the Royal Astronomical Society 456:3774-3781 (2016) (eprint)

• Debian Astronomy Team
• Roger Wesson

• 2.1-1 (bullseye)
• 2.2-1 (sid)
• 2.2-1 (bookworm)
• 1.0-3 (buster)
• 2.2-1 (trixie)
• 1.0-2 (stretch)

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The astrometry engine will take any image and return the astrometry world coordinate system (WCS), a standards-based description of the transformation between image coordinates and sky coordinates.

• 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

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

• 115 regular users
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• 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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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 236226 submissions)

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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.

• K. Banse, P. Grosbol and D. Baade: MIDAS as a Development Environment. Astronomical Data Analysis Software and Systems I 25:120 (1992)

• Debian Astro Team
• Ole Streicher

• 15.09pl1.0-2 (stretch)
• 13.09pl1.4-1 (jessie)
• 19.02pl1.1-6 (bullseye)
• 22.02pl1.0-2 (bookworm)
• 23.02pl1.0-2 (sid)
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This software package provides independent binary programs (so called tasks) which performs various steps of astronomical image reduction and data processing. These tasks are designed for execution from a UNIX command line shell or shell script. Each of these tasks performs a specific operation (e.g. transforming an image to another reference frame, search and identifiy stars or other point-like sources, do photometry, transform/display a FITS image to a popular graphics format, ...) while the details of a certain operation are specified via command switches and arguments. Therefore this package does not need any higher level operating environment than a standard UNIX shell, however, processing the related data might require a little more knowledge of the used shell itself. If you find this program useful in your research, please cite 2012MNRAS.421.1825P as "2012, MNRAS, 421, 1825". See also the web page of the project, found at http://fitsh.net/. That page gathers information about the program (including documentation and examples), this is the primary download source of the package itself, and additionally, serves a public forum for the program users in various topics. Bug reports, comments and ideas are welcomed!

• Andras Pal: FITSH - a software package for image processing. Monthly Notices of the Royal Astronomical Society 421:1825-1837 (2012) (eprint)

• Debian Astronomy Team
• Nilesh Patra

• 0.9.4-1 (bullseye)
• 0.9.2-1 (stretch)
• 0.9.2-1 (buster)
• 0.9.4-1 (bookworm)
• 0.9.4-1 (trixie)
• 0.9.4-1 (sid)

• 5 regular users
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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.

• Pence, W.: New Developments in the FITSIO and FV Software Packages. Astronomical Data Analysis Software and Systems VII 145:97 (1998)

• Debian Astro Team
• Ole Streicher

• 5.5.2+dfsg-1 (bullseye)
• 5.5.2+dfsg-3 (sid)
• 5.4+dfsg-2 (stretch)
• 5.5.2+dfsg-2 (bookworm)
• 5.5+dfsg-2 (buster)
• 5.3+dfsg-5 (jessie)

field

astronomy

interface

x11

role

program

science

visualisation

uitoolkit

tk

use

viewing

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file

x11

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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.

• Markwardt, C. B.: Non-Linear Least Squares Fitting in IDL with MPFIT. Astronomical Data Analysis Software and Systems XVIII 411:251 (2009)

• Debian Astro Team
• Ole Streicher

• 1.85+2017.01.03-4 (trixie)
• 1.85+2017.01.03-4 (sid)
• 1.84+2016.05.19-1 (stretch)
• 1.85+2017.01.03-3 (buster)
• 1.85+2017.01.03-4 (bullseye)
• 1.85+2017.01.03-4 (bookworm)

• 82 total installations (of 236226 submissions)

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GGobi is an open source visualization program for exploring high-dimensional data. It provides highly dynamic and interactive graphics such as tours, as well as familiar graphics such as the scatterplot, barchart and parallel coordinates plots. Plots are interactive and linked with brushing and identification.

See http://www.ggobi.org for more information.

• Dirk Eddelbuettel

• 2.1.11-2 (bookworm)
• 2.1.11-2 (bullseye)
• 2.1.11-2 (buster)
• 2.1.11-2 (stretch)
• 2.1.11-1 (jessie)
• 2.1.11-2 (trixie)
• 2.1.11-2 (sid)

field

statistics

role

program

uitoolkit

gtk

use

viewing

works-with-format

xml

• 28 regular users
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Glue is a Python project to link visualizations of scientific datasets across many files. Some of its features are:

• Interactive, linked statistical graphics of multiple files.
• Support for many file formats including common image formats, ascii tables, astronomical image and table formats (fits, vot, ipac), and HDF5. Custom data loaders can also be easily added.
• Highly scriptable and extendable.

• C. Beaumont, T. Robitaille, A. Goodman and M. Borkin: Multidimensional Data Exploration with Glue. Proceedings of the 12th Python in Science Conference :8 - 12 (2013)

• Debian Astronomy Maintainers
• Andreas Tille

• 1.0.1+dfsg-2 (bookworm)
• 1.17.1+dfsg-1 (sid)
• 1.0.1+dfsg-1 (bullseye)
• 0.14.1+dfsg-1 (buster)
• 0.9.1+dfsg-1 (stretch)
• 1.17.1+dfsg-1 (trixie)
• 1.18.0 (upstream)

• 2 regular users
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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, Python 3 and Yorick).

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

• F. H. Vincent, T. Paumard, E. Gourgoulhon and G. Perrin: GYOTO: a new general relativistic ray-tracing code. Classical and Quantum Gravity 28:225011 (2011) (eprint)

• Debian Astronomy Maintainers
• Lukas Märdian

• 1.4.4-3 (bullseye)
• 0.2.3-1 (jessie)
• 2.0.2-1.1 (sid)
• 2.0.2-1~bpo12+1 (bookworm-backports)
• 2.0.2-1~bpo11+1 (bullseye-backports-sloppy)
• 1.2.0-2 (stretch)
• 1.4.4-8 (bookworm)
• 1.3.1-1 (buster)

• 110 total installations (of 236226 submissions)

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It can display, edit, analyze, process, save and print 8-bit, 16-bit and 32-bit images. It can read many image formats including TIFF, GIF, JPEG, BMP, DICOM, FITS and "raw". It supports "stacks", a series of images that share a single window.

It can calculate area and pixel value statistics of user-defined selections. It can measure distances and angles. It can create density histograms and line profile plots. It supports standard image processing functions such as contrast manipulation, sharpening, smoothing, edge detection and median filtering.

Spatial calibration is available to provide real world dimensional measurements in units such as millimeters. Density or gray scale calibration is also available.

ImageJ is developed by Wayne Rasband (wayne@codon.nih.gov), is at the Research Services Branch, National Institute of Mental Health, Bethesda, Maryland, USA.

• Caroline A Schneider, Wayne S Rasband and Kevin W Eliceiri: NIH Image to ImageJ: 25 years of image analysis. Nature methods 9:671-675 (2012) (PubMed,eprint)

• Debian Med Packaging Team
• Andreas Tille

• 1.53t-1 (bookworm)
• 1.54g-1 (trixie)
• 1.52j-1 (buster)
• 1.54g-1 (sid)
• 1.53g-2 (bullseye)
• 1.51i+dfsg-2 (stretch)
• 1.49i+dfsg-1 (jessie)
• 1.54i (upstream)

role

program

use

analysing, editing, viewing

works-with

image, image:raster

works-with-format

gif, jpg, tiff

• 99 regular users
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This package obtains radial velocities and velocity dispersions using cross-correlation methods or emission line fits. It consists of several SPP tasks:

• XCSAO and PXCSAO: cross-correlate spectra,
• EMSAO and PEMSAO: find emission lines in spectra,
• BCVCORR: solar system barycentric velocity correction,
• SUMSPEC: add and/or modify spectra,
• LINESPEC: synthetic emission line templates,
• EQWIDTH: equivalent widths of lines in spectra,
• WLRANGE: wavelength overlap range for a list of spectra,
• LISTSPEC: list pixel, wavelength, delta wavelength, and/or pixel value for spectrum image,
• PIX2WL: wavelength at a given pixel in a spectrum,
• WL2PIX: pixel at a given wavelength in a spectrum,
• VELSET Artificially change the redshift of (log-wavelength) spectra

• M. J. Kurtz and D. J. Mink: RVSAO 2.0: Digital Redshifts and Radial Velocities. Publications of the Astronomical Society of the Pacific 110:934 - 977 (1998) (eprint)

• Debian Astro Team
• Ole Streicher

• 2.8.3-1 (bullseye)
• 2.8.5-2 (sid)
• 2.8.5-2 (trixie)
• 2.8.5-1 (bookworm)
• 2.8.3-1 (buster)

• 1 recent
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FITS (Flexible Image Transport System) is a data format most used in astronomy. 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 package contains utility programs, based on CFITSIO, namely fitscopy, fpack and funpack.

• Debian Astronomy Maintainers
• Benjamin Drung

• 3.410-1 (stretch)
• 3.450-3 (buster)
• 3.370-2+deb8u1 (jessie)
• 4.3.1-1 (trixie)
• 3.490-3 (bullseye)
• 4.2.0-3 (bookworm)
• 4.3.1-1.1 (sid)
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• 87 regular users
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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 the static library and headers for the C language implementation of HEALPix. The C library provides basic input/output of HEALPix maps as well as basic spatial operations like conversion between spherical coordinates and HEALPix pixels.

• Debian Astro Team
• Leo Singer

• 3.30.0-7 (buster)
• 3.11.4-2 (jessie)
• 3.30.0-9 (bookworm)
• 3.30.0-9 (trixie)
• 3.30.0-9 (sid)
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devel

library

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The FFTW library computes Fast Fourier Transforms (FFT) in one or more dimensions. It is extremely fast. This package contains the statically linked library, header files and test programs.

This package contains the header files and static libraries. For documentation, see libfftw3-doc.

• Matteo Frigo and Steven G. Johnson: The Design and Implementation of FFTW3. 93(2):216–231 (2005) (eprint)

• Debian Science Maintainers
• Andreas Tille

• 3.3.4-2 (jessie)
• 3.3.10-1 (sid)
• 3.3.10-1 (trixie)
• 3.3.10-1 (bookworm)
• 3.3.8-2 (bullseye)
• 3.3.8-2 (buster)
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devel

library

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devel-lib

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libnova is a general purpose, double precision, Celestial Mechanics, Astrometry and Astrodynamics library.

This package contains the development files.

• Debian Qt/KDE Maintainers
• Benjamin Drung

• 0.16-4 (buster)
• 0.16-2 (stretch)
• 0.14.0-2.1 (jessie)
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devel

lang:c, lang:c++, library

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SOPT is a C package to perform Sparse OPTimisation. It solves a variety of sparse regularisation problems, including the SARA algorithm.

SOPT is largely provided to support the PURIFY package, a companion open-source code to perform radio interferometric imaging, also written by the authors of SOPT.

This package contains the development files.

• L. Pratley, J. D. McEwen, M. d'Avezac, R. E. Carrillo, A. Onose and Y. Wiaux: Robust sparse image reconstruction of radio interferometric observations with PURIFY. Mon. Not. Roy. Astron. Soc., submitted (2016) (eprint)

• Debian Astro Team
• Benjamin Drung

• 3.0.1-11 (bullseye)
• 3.0.1+dfsg-3.1 (sid)
• 3.0.1+dfsg-1 (bookworm)
• 2.0.0-5 (buster)
• 2.0.0-2 (stretch)
• 4.0.0 (upstream)

• 1 regular users
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This library is a collection of code designed to aid in replacing the SLA library with code from NOVAS and ERFA.

Where possible the API is similar to the C SLA API except for the use of a "pal" prefix.

This package contains the development files.

• T. Jenness and D. S. Berry: PAL: A Positional Astronomy Library. Astronomical Data Analysis Software and Systems XXII 475:307 (2013) (eprint)

• Debian Astronomy Team
• Ole Streicher

• 0.9.10-1 (trixie)
• 0.9.8-1 (buster)
• 0.9.8-1 (bullseye)
• 0.9.10-1 (bookworm)
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MayaVi2 is a cross-platform tool for 2-D and 3-D scientific data visualization. Its features include:

• Visualization of scalar, vector and tensor data in 2 and 3 dimensions
• Easy scriptability using Python
• Easy extendability via custom sources, modules, and data filters
• Reading several file formats: VTK (legacy and XML), PLOT3D, etc.
• Saving of visualizations
• Saving rendered visualization in a variety of image formats.

MayaVi2 has been designed with scriptability and extensibility in mind. While the mayavi2 application is usable by itself, it may be used as an Envisage plugin which allows it to be embedded in user applications natively. Alternatively, it may be used as a visualization engine for any application.

This package also provides TVTK, which wraps VTK objects to provide a convenient, Pythonic API, while supporting Traits attributes and NumPy/SciPy arrays. TVTK is implemented mostly in pure Python, except for a small extension module.

• Debian Python Team
• Andreas Tille

• 4.8.1-3 (trixie)
• 4.3.1-3.1 (jessie)
• 4.5.0-1 (stretch)
• 4.5.0-1 (buster)
• 4.8.0-2 (bookworm)
• 4.7.1-2 (bullseye)
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devel

examples, lang:python

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viewing

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mocassin is a fully 3D or 2D photoionisation and dust radiative transfer code which employs a Monte Carlo approach to the transfer of radiation through media of arbitrary geometry and density distribution. It was originally developed for the modelling of photoionised regions like HII regions and planetary nebulae and has since expanded and been applied to a variety of astrophysical problems, including modelling clumpy dusty supernova envelopes, star forming galaxies, protoplanetary disks and inner shell fluorence emission in the photospheres of stars and disk atmospheres. The code can deal with arbitrary Cartesian grids of variable resolution, it has successfully been used to model complex density fields from SPH calculations and can deal with ionising radiation extending from Lyman edge to the X-ray. The dust and gas microphysics is fully coupled both in the radiation transfer and in the thermal balance.

• B. Ercolano, M.J. Barlow, P.J. Storey and X.-W. Liu: MOCASSIN: a fully three-dimensional Monte Carlo photoionization code. Monthly Notices of the Royal Astronomical Society 340:1136-1152 (2003) (eprint)

• Debian Astronomy Team
• Roger Wesson

• 2.02.73.2-1 (bookworm)
• 2.02.73-1 (buster)
• 2.02.72-2 (stretch)
• 2.02.73.2-1 (sid)
• 2.02.73.2-1 (trixie)
• 2.02.73.2-1 (bullseye)
• 2.02.73.3 (upstream)

• 2 regular users
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mpgrafic produces initial conditions files for N-body simulations of cosmological large-scale structure formation. It is a free-licensed, MPI-parallelised, rewritten version of Ed Bertschinger's grafic-1 program, producing output files in the grafic format. It includes options for an Eisenstein and Hu baryonic wiggles power spectrum, for using a low-resolution map for large-scale modes in the spirit of grafic-2, and together with constrfield, can be used for generating constrained initial conditions. Details are given in Prunet et al (2008) http://cdsads.u-strasbg.fr/abs/2008ApJS..178..179P.

• S. Prunet, C. Pichon, D. Aubert, D. Pogosyan, R. Teyssier and S. Gottloeber: Initial Conditions For Large Cosmological Simulations. Astrophysical Journal Supplement Series 178:179-188 (2008) (eprint)

• Debian Astro Team
• Boud Roukema

• 0.3.19-1 (trixie)
• 0.3.19-1 (sid)
• 0.3.19-1 (bullseye)
• 0.3.18-1 (buster)
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• 1 regular users
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NEAT analyses lists of emission line fluxes measured from the spectra of photoionised nebulae such as planetary nebulae and HII regions. It determines the extinction, and then adopts a three zone model to determine temperatures, densities, and ionic and total abundances, from collisionally excited lines and recombination lines. It calculates uncertainties if required, using a Monte Carlo technique.

• R. Wesson, D. Stock and P. Scicluna: Understanding and reducing statistical uncertainties in nebular abundance determinations. Monthly Notice of the Royal Astronomical Society 422:3516-3526 (2012) (eprint)

• Debian Astronomy Team
• Roger Wesson

• 2.2-1 (buster)
• 2.0-2 (stretch)
• 2.3.2-2 (sid)
• 2.3.2-2 (trixie)
• 2.3.2-2 (bookworm)
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• 2.4 (upstream)

• 3 regular users
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This is a satellite tracking program. It is probably mostly of interest to users of amateur satellites, but includes support for optionally announcing azimuth and elevation to help in manual antenna pointing, or optical observation of satellites.

The upstream predict sources include a front-end called 'map', which is called predict-map in the Debian package.

The 'ntp' package is suggested because accurate satellite tracking depends on precise knowledge of ground station time and location.

• A. Maitland Bottoms
• Bdale Garbee

• 2.2.3-4 (stretch)
• 2.2.3-4 (jessie)

field

astronomy

hardware

hamradio

interface

text-mode

network

server

role

program

uitoolkit

ncurses

• 2 regular users
• 50 total installations (of 236226 submissions)

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PURIFY is a collection of routines written in C that implements different tools for radio interferometric imaging including file handling (for both visibilities and fits files), implementation of the measurement operator and set-up of the different optimization problems used for image deconvolution. The code calls the generic Sparse OPTimization (SOPT) package to solve the imaging optimization problems.

• Luke Pratley, Jason D. McEwen, Mayeul d'Avezac, Rafael E. Carrillo, Alexandru Onose and Yves Wiaux: Robust sparse image reconstruction of radio interferometric observations with PURIFY. Mon. Not. Roy. Astron. Soc., submitted (2016) (eprint)

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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.

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Python 3 module is to provide an easy way to compute dendrograms of observed or simulated Astronomical data in Python 3.

• Debian Astronomy Maintainers
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Astroplan is an observation planning package for astronomers that can help you plan for everything but the clouds.

It is an Astropy affiliated package that seeks to make your life as an observational astronomer a little less infuriating.

This is the Python 3 version of the package.

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

This is the Python 3 version of the package.

• Debian Astro Team
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PyBDSF (the Python Blob Detection and Source Finder) is a tool designed to decompose radio interferometry images into sources and make available their properties for further use. PyBDSF can decompose an image into a set of Gaussians, shapelets, or wavelets as well as calculate spectral indices and polarization properties of sources and measure the psf variation across an image. PyBDSF uses an interactive environment based on CASA that will be familiar to most radio astronomers. Additionally, PyBDSF may also be used in Python scripts.

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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)

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EinsteinPy is an open source pure Python package dedicated to problems arising in General Relativity and relativistic physics, such as goedesics plotting for schwarzschild space-time model, calculation of schwarzschild radius for any mass given, symbolic calculation of various functions related to GR such as christoffel symbols. Features like visualization of geodesics of curved black holes and 3D visualizations are some of the features which are planned. It is released under the MIT license.

• Debian Astronomy Team
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PyEphem provides an ephem Python package for performing high-precision astronomy computations. The underlying numeric routines are coded in C and are the same ones that drive the popular XEphem astronomy application, whose author, Elwood Charles Downey, generously gave permission for their use in PyEphem.

The name ephem is short for the word ephemeris, which is the traditional term for a table giving the position of a planet, asteroid, or comet for a series of dates.

Nothe that this package will continue to be maintained, but it no longer stands at the cutting edge of astronomy in Python.

• Debian Astronomy Team
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Gammapy is an in-development affiliated package of Astropy that builds on the core scientific Python stack to provide tools to simulate and analyse the gamma-ray sky for telescopes such as CTA, H.E.S.S., VERITAS, MAGIC, HAWC and Fermi-LAT.

• C. Deil, R. Zanin, J. Lefaucheur, C. Boisson, B. Khélifi, R. Terrier, M. Wood, L. Mohrmann, N. Chakraborty, J. Watson, R. López Coto, S. Klepser, M. Cerruti, J.-P. Lenain, F. Acero, A. Djannati-Ataï, S. Pita, Z. Bosnjak, J. E. Ruiz, C. Trichard, T. Vuillaume, A. Donath, J. King, L. Jouvin, E. Owen, M. P. Arribas, B. Sipocz, D. Lennarz, A. Voruganti and M. Spir-Jacob: Gammapy - A prototype for the CTA science tools. ArXiv e-prints (2017) (eprint)

• Debian Astro Team
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Keras is a Python library for machine learning based on deep (multi- layered) artificial neural networks (DNN), which follows a minimalistic and modular design with a focus on fast experimentation.

Features of DNNs like neural layers, cost functions, optimizers, initialization schemes, activation functions and regularization schemes are available in Keras a standalone modules which can be plugged together as wanted to create sequence models or more complex architectures. Keras supports convolutions neural networks (CNN, used for image recognition resp. classification) and recurrent neural networks (RNN, suitable for sequence analysis like in natural language processing).

It runs as an abstraction layer on the top of Theano (math expression compiler) by default, which makes it possible to accelerate the computations by using (GP)GPU devices. Alternatively, Keras could run on Google's TensorFlow (not yet available in Debian).

• Debian Science Maintainers
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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
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PyMOC provides a Python compatible library for handling MOCs.

Frequently astronomical survey catalogues or images are sparse and cover only a small part of the sky. In a Multi-Order Coverage map the extent of data in a particular dataset is cached as a pre-calculated mask image. The hierarchical nature enables fast boolean operations in image space, without needing to perform complex geometrical calculations. Services such as VizieR generally offer the MOC masks, allowing a faster experience in graphical applications such as Aladin, or for researchers quickly needing to locate which datasets may contain overlapping coverage.

The MOC mask image itself is tessellated and stored in NASA HealPix format, encoded inside a FITS image container. Using the HealPix (Hierarchical Equal Area isoLatitude Pixelization) tessellation method ensures that more precision (pixels) in the mask are available when describing complex shapes such as approximating survey or polygon edges, while only needing to store a single big cell/pixel when an coverage is either completely inside, or outside of the mask. Catalogues can be rendered on the mask as circles.

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pysynphot simulates photometric data and spectra as they are observed with the Hubble Space Telescope (HST). Passbands for standard photometric systems are available, and users can incorporate their own filters, spectra, and data. pysynphot user interface allows you to:

• Construct complicated composite spectra from various grids of model atmosphere spectra, parameterized spectrum models, and atlases of stellar spectrophotometry.
• Simulate observations.
• Query the resulting structures for quantities of interest, such as countrate, effective wavelength, effective stimulus, as well as the wavelength and flux arrays.
• Plot HST sensitivity curves and calibration target spectra.
• Compute photometric calibration parameters for any HST instrument mode.

pysynphot can help HST observers to perform cross-instrument simulations, to examine the transmission curve of the HST Optical Telescope Assembly (OTA), and spectra of HST calibration targets. Expert users can take advantage of the control and data structures available in Python to easily perform repetitive operations such as simulate the observation of multiple type of sources through multiple observing modes.

• P. L. Lim, R. I. Diaz and V. Laidler: PySynphot User’s Guide. (2015)

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This is a package to reproject astronomical images using various techniques via a uniform interface. Reprojection means the re-gridding of images from one world coordinate system to another (for example changing the pixel resolution, orientation, coordinate system). Currently implemented are reprojection of celestial images by interpolation, as well as by finding the exact overlap between pixels on the celestial sphere. It can also reproject to/from HEALPIX projections.

This package contains the Python 3 version of the package.

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SNCosmo synthesizes supernova spectra and photometry from SN models, and has functions for fitting and sampling SN model parameters given photometric light curve data. It offers fast implementations of several commonly used extinction laws and can be used to construct SN models that include dust. The SNCosmo library includes supernova models such as SALT2, MLCS2k2, Hsiao, Nugent, PSNID, SNANA and Whalen models, as well as a variety of built-in bandpasses and magnitude systems, and provides convenience functions for reading and writing peculiar data formats used in other packages. The library is extensible, allowing new models, bandpasses, and magnitude systems to be defined using an object-oriented interface.

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SunPy is a community-developed free and open-source software package for solar physics. SunPy is meant to be a free alternative to the SolarSoft data analysis environment. The aim of the SunPy project is to provide the software tools necessary so that anyone can analyze solar data.

• T. SunPy Community, S.J. Mumford, S. Christe, D. Perez-Suarez, J. Ireland, A.Y. Shih, A.R. Inglis, S. Liedtke, R.J. Hewett, F. Mayer, K. Hughitt, N. Freij, T. Meszaros, S.M. Bennett, M. Malocha, J. Evans, A. Agrawal, A.J. Leonard, T.P. Robitaille, B. Mampaey, J. Ivan Campos-Rozo and M.S. Kirk: SunPy-Python for solar physics. Computational Science and Discovery 8(1):014009 (2015) (eprint)

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The yt project aims to produce an integrated science environment for collaboratively asking and answering astrophysical questions. To do so, it will encompass the creation of initial conditions, the execution of simulations, and the detailed exploration and visualization of the resultant data. It will also provide a standard framework based on physical quantities interoperability between codes.

This package contains the Python 3 version of the package.

• M.J. Turk, B.D. Smith, J.S. Oishi, S. Skory, S.W. Skillman, T. Abel and M.L. Norman: yt: A Multi-code Analysis Toolkit for Astrophysical Simulation Data. ApJS 192:9 (2011) (eprint)

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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.

• W. A. Joye and E. Mandel: New Features of SAOImage DS9. Astronomical Data Analysis Software and Systems XII 295:489 (2003)

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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).

• M.A. Albrecht, A. Brighton, T. Herlin, P. Biereichel and D. Durand: Access to Data Sources and the ESO SkyCat Tool. Astronomical Data Analysis Software and Systems VI 125:333 (1997)

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x11

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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.

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

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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.

• Bertin, E.: Displaying Digital Deep Sky Images. 461:263 (2012) (eprint)

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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)

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TOPCAT is an interactive graphical viewer and editor for tabular data. Its aim is to provide most of the facilities that astronomers need for analysis and manipulation of source catalogues and other tables, though it can be used for non-astronomical data as well. It understands a number of different astronomically important formats (including FITS and VOTable) and more formats can be added.

This package contains the executable.

• Taylor, M. B.: TOPCAT & STIL: Starlink Table/VOTable Processing Software. Astronomical Data Analysis Software and Systems XIV 347:29-33 (2005) (eprint)

• Debian Astro Team
• Ole Streicher

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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.

• Mink, Douglas J.: WCSTools: an Image Astrometry Toolkit. Astronomical Data Analysis Software and Systems VIII 172:498 (1999)

• Debian Astro Team
• Steve Langasek

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WSClean (w-stacking clean) is a fast generic widefield imager. It uses the w-stacking algorithm and can make use of the w-snapshot algorithm. As of Feb 2014, it is 2-12 times faster than CASA's w-projection, depending on the array configuration. It supports full-sky imaging and proper beam correction for homogeneous dipole arrays such as the MWA.

WSClean allows Hogbom and Cotton-Schwab cleaning, and can clean polarizations joinedly. All operations are performed on the CPU (it is not specialized for GPUs).

• A. R. Offringa, B. McKinley, N. Hurley-Walker, F. H. Briggs, R. B. Wayth, D. L. Kaplan, M. E. Bell, L. Feng, A. R. Neben, J. D. Hughes, J. Rhee, T. Murphy, N. D. R. Bhat, G. Bernardi, J. D. Bowman, R. J. Cappallo, B. E. Corey, A. A. Deshpande, D. Emrich, A. Ewall-Wice, B. M. Gaensler, R. Goeke, L. J. Greenhill, B. J. Hazelton, L. Hindson, M. Johnston-Hollitt, D. C. Jacobs, J. C. Kasper, E. Kratzenberg, E. Lenc, C. J. Lonsdale, M. J. Lynch, S. R. McWhirter, D. A. Mitchell, M. F. Morales, E. Morgan, N. Kudryavtseva, D. Oberoi, S. M. Ord, B. Pindor, P. Procopio, T. Prabu, J. Riding, D. A. Roshi, N. U. Shankar, K. S. Srivani, R. Subrahmanyan, S. J. Tingay, M. Waterson, R. L. Webster, A. R. Whitney, A. Williams and C. L. Williams: WSCLEAN: an implementation of a fast, generic wide-field imager for radio astronomy. Monthly Notices of the Royal Astronomical Society 444:606 - 619 (2014) (eprint)

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