Enter the query into the form above. You can look for specific version of a package by using @ symbol like this: gcc@10.
API method:
GET /api/packages?search=hello&page=1&limit=20
where search is your query, page is a page number and limit is a number of items on a single page. Pagination information (such as a number of pages and etc) is returned
in response headers.
If you'd like to join our channel webring send a patch to ~whereiseveryone/toys@lists.sr.ht adding your channel as an entry in channels.scm.
libskry implements the lucky imaging principle of astronomical imaging: creating a high-quality still image out of a series of many thousands) low quality ones
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.
Xplanet renders an image of a planet into an X window or file. All of the major planets and most satellites can be drawn and different map projections are also supported, including azimuthal, hemisphere, Lambert, Mercator, Mollweide, Peters, polyconic, orthographic and rectangular.
This package provides a python library to calculate IACT IRFs and Sensitivities.
Astrocut provides tools for making cutouts from sets of astronomical images with shared footprints. It is under active development.
Three main areas of functionality are included:
solving the specific problem of creating image cutouts from sectors of Transiting Exoplanet Survey Satellite full-frame images
general fits file cutouts including from single images and sets of images with the shared WCS/pixel scale
cutout post-processing functionality, including centering cutouts along a path (for moving targets) and combining cutouts
CRDS is a package used for working with astronomical reference files for the HST and JWST telescopes. CRDS is useful for performing various operations on reference files or reference file assignment rules. CRDS is used to assign, check, and compare reference files and rules, and also to predict those datasets which should potentially be reprocessed due to changes in reference files or assignment rules. CRDS has versioned rules which define the assignment of references for each type and instrument configuration. CRDS has web sites corresponding to each project http://hst-crds.stsci.edu or https://jwst-crds.stsci.edu/ which record information about reference files and provide related services.
PypeIt is a Python package for semi-automated reduction of astronomical spectroscopic data. Its algorithms build on decades-long development of previous data reduction pipelines by the developers.
It is designed to be used by both advanced spectroscopists with prior data reduction expertise and astronomers with no prior experience of data reduction. It is highly configurable and designed to be applied to any standard slit-imaging spectrograph, including long-slit, multi-slit, as well as cross-dispersed echelle spectra.
Provides DataModel, which is the base class for data models implemented in the JWST and Roman calibration software.
This package implements a functionality to match sky on image mosaic.
LibXISF is C++ library that can read and write XISF files produced by PixInsight. It implements XISF 1.0 specification.
Libnova is a general purpose, double precision, Celestial Mechanics, Astrometry and Astrodynamics library.
PyCPL provides Python3 language bindings for the complete programming API of the European Southern Observatory Common Pipeline Library toolkit, including the CPL plugin interface.
APLpy is a Python module aimed at producing publication-quality plots of astronomical imaging data in FITS format. The module uses matplotlib, a powerful and interactive plotting package. It is capable of creating output files in several graphical formats, including EPS, PDF, PS, PNG, and SVG.
Main features:
Make plots interactively or using scripts
Show grayscale, colorscale, and 3-color RGB images of FITS files
Generate co-aligned FITS cubes to make 3-color RGB images
Make plots from FITS files with arbitrary WCS (e.g. position-velocity)
Slice multi-dimensional FITS cubes
Overlay any number of contour sets
Overlay markers with fully customizable symbols
Plot customizable shapes like circles, ellipses, and rectangles
Overlay ds9 region files
Overlay coordinate grids
Show colorbars, scalebars, and beams
Customize the appearance of labels and ticks
Hide, show, and remove different contour and marker layers
Pan, zoom, and save any view as a full publication-quality plot
Save plots as EPS, PDF, PS, PNG, and SVG
FITS/XISF image viewer with multithreaded image loading. It is intended primarily for viewing astro photos and images with support of following formats:
FITS 8, 16 bit integer and 32 bit float
XISF 8, 16 bit integer and 32 bit float
RAW CR2, DNG, NEF
JPEG, PNG, BMP, GIF, PBM, PGM, PPM and SVG images
Features:
using same stretch function as PixInsight
OpenGL accelerated drawing
index and search FITS XISF header data
quick mark images and then copy/move marked files
convert FITS <-> XISF
convert FITS/XISF -> JPEG/PNG
image statistics mean, media, min, max
support for WCS
thumbnails
convert CFA images to colour - debayer
color space aware
GalSim is software for simulating images of astronomical objects (stars, galaxies) in a variety of ways.
This package provides a a simple program to predict the levels of background emission in JWST observations, for use in proposal planning.
It accesses a precompiled background cache prepared by Space Telescope Science Institute. The background cache is hosted by the Mikulski Archive for Space Telescopes (MAST), so you need internet access to run the tool with the remote cache. It is possible to download the full background cache to your local machine.
Radio Beam is a simple toolkit for reading beam information from FITS headers and manipulating beams. Some example applications include:
Convolution and deconvolution
Unit conversion (Jy to/from K)
Handle sets of beams for spectral cubes with varying resolution between channels
Find the smallest common beam from a set of beams
Add the beam shape to a matplotlib plot
radiospectra provides support for some type of radio spectra in solar physics.
Software for Calibrating AstroMetry and Photometry is a software that computes astrometric projection parameters from source catalogues derived from FITS images. The computed solution is expressed according to the WCS standard. The main features of SCAMP are:
compatibility with
SExtractorFITS or Multi-Extension FITS catalogue format in inputgeneration of WCS-compliant and
SWarp-compatible FITS image headers in outputautomatic grouping of catalogues on the sky
selectable on-line astrometric reference catalogue
automatic determination of scale, position angle, flipping and coordinate shift using fast pattern-matching
various astrometric calibration modes for single detectors and detector arrays
combined astrometric solutions for multi-channel/instrument surveys
highly configurable astrometric distortion polynomials
correction for differential chromatic refraction
proper motion measurements
multi-threaded code that takes advantage of multiple processors
VOTable-compliant XML output of meta-data
XSLT filter sheet provided for convenient access to metadata from a regular web browser
This package provides tools to read and analyze data from the IRIS solar-observing satellite.
This package provides astronomical interstellar dust extinction curves implemented using the astropy.modeling framework.
This package provides tools for machine learning and data mining in astronomy.
This package implement functionality for computation of non-thermal radiation from relativistic particle populations. It includes tools to perform MCMC fitting of radiative models to X-ray, GeV, and TeV spectra using emcee, an affine-invariant ensemble sampler for Markov Chain Monte Carlo.
Hubble Space Telescope image combination using the drizzle algorithm to combine astronomical images, to model image distortion, to remove cosmic rays, and generally to improve the fidelity of data in the final image.