We are building an “astrometry engine” to create correct, standards-compliant astrometric meta data for every useful astronomical image ever taken, past and future, in any state of archival disarray. The astrometry engine will take any image and return the astrometry world coordinate system (WCS)—ie, a standards-based description of the (usually nonlinear) transformation between image coordinates and sky coordinates—with absolutely no “false positives” (but maybe some “no answers”). It will do its best, even when the input image has no—or totally incorrect—meta-data. We intend to install the engine for real-time operation on the web, at observatories, at plate-scanning projects, and at data archives.
celerite is a library for fast and scalable Gaussian Process (GP) Regression in one dimension with implementations in C++, Python, and Julia. The Python implementation is the most stable and it exposes the most features but it relies on the C++ implementation for computational efficiency. This documentation won’t teach you the fundamentals of GP modeling but the best resource for learning about this is available for free online: Rasmussen & Williams (2006).
Daft is a Python package that uses matplotlib to render pixel-perfect probabilistic graphical models for publication in a journal or on the internet. With a short Python script and an intuitive model-building syntax you can design directed (Bayesian Networks, directed acyclic graphs) and undirected (Markov random fields) models and save them in any formats that matplotlib supports (including PDF, PNG, EPS and SVG).
emcee is an MIT licensed pure-Python implementation of Goodman & Weare’s Affine Invariant Markov chain Monte Carlo (MCMC) Ensemble sampler and these pages will show you how to use it. This documentation won’t teach you too much about MCMC but there are a lot of resources available for that (try this one). We also published a paper explaining the emcee algorithm and implementation in detail.
starry enables the computation of fast and precise light curves for various applications in astronomy: transits and secondary eclipses of exoplanets, light curves of eclipsing binaries, rotational phase curves of exoplanets, light curves of planet-planet and planet-moon occultations, and more.
MESA is a suite of open-source, robust, efficient, thread-safe libraries extensively used in computational stellar astrophysics. Its wide-ranging capabilities allow the simulation of diverse stellar evolution scenarios, from low-mass to massive stars, including advanced evolutionary stages and binary interactions. It uses adaptive mesh refinement and sophisticated timestep controls and supports shared memory parallelism based on OpenMP. State-of-the-art modules provide equations of state, opacity, nuclear reaction rates, element diffusion data, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own explicitly defined public interface to facilitate independent development.
Galactic Dynamics is the study of the formation, history, and evolution of galaxies using the orbits of objects — numerically-integrated trajectories of stars, dark matter particles, star clusters, or galaxies themselves. Gala is an Astropy-affiliated Python package that aims to provide efficient tools for performing common tasks needed in Galactic Dynamics research. Much of this code uses Python for flexible, user-friendly interfaces that interact with wrappers around low-level code (primarily C) to enable fast computations. Common operations include gravitational potential and force evaluations, orbit integrations, dynamical coordinate transformations, and computing chaos indicators for nonlinear dynamics. Gala heavily uses the units and astronomical coordinate systems defined in the Astropy core package.