RAD is package which defines schemas for the Nancy Grace Roman Space Telescope shared attributes for processing and archive. These schemas are schemas for the ASDF file file format, which are used by ASDF to serialize and deserialize data for the Nancy Grace Roman Space Telescope.

Regions is an Astropy package for region handling.

This package provides an Updated and improved version of the Sparse Lens Inversion Technique, developed within the framework of lens modelling software lenstronomy.

casa_cube is a python package that provides an interface to data cubes generates by CASA or Gildas. It allows the user to perform simple tasks such plotting given channel maps, moment maps, line profile in various units, correcting for cloud extinction, reconvolving with a beam taper, trimming a cube. The syntax is similar to pymcfost to perform quick and easy comparison with models.

This package provides a Square Kilometre Array (SKA) Science Data Processor (SDP) function library for radio astronomy.

This package provides functions to import data from the Madrigal database (upper atmospheric science database) into pysat.

Cesium is an end-to-end machine learning platform for time-series, from calculation of features to model-building to predictions. Cesium has two main components - a Python library, and a web application platform that allows interactive exploration of machine learning pipelines. Take control over the workflow in a Python terminal or Jupyter notebook with the Cesium library, or upload your time-series files, select your machine learning model, and watch Cesium do feature extraction and evaluation right in your browser with the web application.

AOFlagger is a tool that can find and remove radio-frequency interference (RFI) in radio astronomical observations. It can make use of Lua scripts to make flagging strategies flexible, and the tools are applicable to a wide set of telescopes.

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.

LibXISF is C++ library that can read and write XISF files produced by PixInsight. It implements XISF 1.0 specification.

The GNU Astronomy Utilities (Gnuastro) is a suite of programs for the manipulation and analysis of astronomical data.

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.

The CALCEPH Library is designed to access the binary planetary ephemeris files, such INPOPxx and JPL DExxx ephemeris files, (called original JPL binary or INPOP 2.0 or 3.0 binary ephemeris files in the next sections) and the SPICE kernel files (called SPICE ephemeris files in the next sections). At the moment, supported SPICE files are:

• text Planetary Constants Kernel (KPL/PCK) files;

• binary PCK (DAF/PCK) files;

• binary SPK (DAF/SPK) files containing segments of type 1, 2, 3, 5, 8, 9, 12, 13, 17, 18, 19, 20, 21, 102, 103 and 120;

• meta kernel (KPL/MK) files;

• frame kernel (KPL/FK) files (only basic support).

This package contains a pure-python drop-in replacement for the Python wrapper around the original LOFAR ParameterSet that is written in C++. It supports only the basic features of the original.

This package provides a librari for spherical harmonic transforms (SHTs), which evolved from the libpsht library, addressing several of its shortcomings, such as adding MPI support for distributed memory systems and SHTs of fields with arbitrary spin, but also supporting new developments in CPU instruction sets like the Advanced Vector Extensions (AVX) or fused multiply-accumulate (FMA) instructions. The library is implemented in portable C99 and provides an interface that can be easily accessed from other programming languages such as C++, Fortran, Python etc. Generally, libsharp's performance is at least on par with that of its predecessor; however, significant improvements were made to the algorithms for scalar SHTs, which are roughly twice as fast when using the same CPU capabilities.

Supporting paper is available at https://arxiv.org/abs/1303.4945

The DKIST package aims to help you search, obtain and use DKIST data as part of your Python software.

The drizzle library is a Python package for combining dithered images into a single image. This library is derived from code used in DrizzlePac. Like DrizzlePac, most of the code is implemented in the C language. The biggest change from DrizzlePac is that this code passes an array that maps the input to output image into the C code, while the DrizzlePac code computes the mapping by using a Python callback. Switching to using an array allowed the code to be greatly simplified.

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.

Tempo analyzes pulsar timing data. Pulse times of arrival (TOAs), pulsar model parameters, and coded instructions are read from one or more input files. The TOAs are fitted by a pulse timing model incorporating transformation to the solar-system barycenter, pulsar rotation and spin-down and, where necessary, one of several binary models. Program output includes parameter values and uncertainties, residual pulse arrival times, chi-squared statistics, and the covariance matrix of the model. In prediction mode,ephemerides of pulse phase behavior (in the form of polynomial expansions) are calculated from input timing models.

This package provides source-only AOCommon collection of functionality that is reused in several astronomical applications, such as wsclean, aoflagger, DP3 and everybeam.

Event reconstruction framework for Imaging Atmospheric Cherenkov Telescopes developed for CTAO.

Python Tools for HST ACS (Advanced Camera for Surveys) Data.

ndcube is a package for manipulating, inspecting and visualizing multi-dimensional contiguous and non-contiguous coordinate-aware data arrays.

It combines data, uncertainties, units, metadata, masking, and coordinate transformations into classes with unified slicing and generic coordinate transformations and plotting/animation capabilities. It is designed to handle data of any number of dimensions and axis types (e.g. spatial, temporal, spectral, etc.) whose relationship between the array elements and the real world can be described by WCS translations.

This package implements functionality for hierarchical analysis of strong lensing systems to infer lens properties and cosmological parameters simultaneously. It allows fitting lenses with measured time delays, imaging information, kinematics constraints and standardizable magnifications with parameters described on the ensemble level.