Orbital is a high level orbital mechanics package for Python.

astroterm is a terminal-based star map written in C. It displays the real-time positions of stars, planets, constellations, and more, all within your terminal - no telescope required!

The FITS "World Coordinate System" (WCS) standard defines keywords and usage that provide for the description of astronomical coordinate systems in a FITS (Flexible Image Transport System) image header.

H5plot is a small GUI to view the solutions in an H5parm interactively. It is a spiritual successor to ParmDBplot for quickly reviewing gain solutions generated by NDPPP.

healpy is a Python package to handle pixelated data on the sphere. It is based on the Hierarchical Equal Area isoLatitude Pixelization (HEALPix) scheme and builds with the HEALPix C++ library.

ChiantiPy is the Python interface to the CHIANTI atomic database for astrophysical spectroscopy. It provides the capability to calculate the emission line and continuum spectrum of an optically thin plasma based on the data in the CHIANTI database.

This package provides a Python definition and validation schemata for FITS files.

Stellarium shows a realistic sky in 3D, just like what you see with the naked eye, binoculars, or a telescope. It can be used to control telescopes over a serial port for tracking celestial objects.

This package implements a functionality to produce map based simulations for the Simons Observatory or other CMB experiments. It creates simulated maps in HEALPix and CAR pixelization based on:

• foreground models included in PySM

• custom foregrounds models from the so_pysm_models package

• precomputed Cosmic Microwave Background simulations

• noise simulations based on expected performance and simulated hitmaps

• effect of gaussian beam convolution

This package implements a reader for CORSIKA binary output files using NumPy.

This package provides a Python module to various STScI image array manipulation functions.

SNCosmo is a Python library for supernova cosmology analysis. It aims to make such analysis both as flexible and clear as possible.

This package provides a CLI and Python module to quickly calculate cosmological parameters e.g. redshift or luminosity-distance.

This package implements functionality of Point Spread Function describing how the optical system spreads light from sources.

This package provides tools for machine learning and data mining in astronomy.

PyERFA is the Python wrapper for the ERFA library (Essential Routines for Fundamental Astronomy), a C library containing key algorithms for astronomy, which is based on the SOFA library published by the International Astronomical Union (IAU). All C routines are wrapped as Numpy universal functions, so that they can be called with scalar or array inputs.

This package provides a Python client for interacting with a VirES server, of which there are two: VirES for Swarm and VirES for Aeolus

PetroFit is a package for calculating Petrosian properties, such as radii and concentration indices, as well as fitting galaxy light profiles. In particular, PetroFit includes tools for performing accurate photometry, segmentations, Petrosian profiling, and Sérsic fitting.

Package Raccoon cleans the "wiggles" (i.e., low-frequency sinusoidal artifacts) in the JWST-NIRSpec IFS (integral field spectroscopy) data. These wiggles are caused by resampling noise or aliasing artifacts.

This package provides base classes and command-line tools for implementing calibration pipeline software.

STPSF produces simulated PSFs for the James Webb Space Telescope, NASA's flagship infrared space telescope. STPSF can simulate images for any of the four science instruments plus the fine guidance sensor, including both direct imaging, coronagraphic, and spectroscopic modes.

This package provides a replacement for IRAF STSDAS SYNPHOT and ASTROLIB PYSYNPHOT, utilizing Astropy and covering the non-instrument specific portions of the old packages.

MissFITS is a program that performs basic maintenance and packaging tasks on FITS files:

• add/edit FITS header keywords

• split/join MEF files

• unpack/pack FITS data-cubes

• create/check/update FITS checksums, using R. Seaman's protocol

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.