DPMhalo (Descriptive Parametric Model) generates profiles of gaseous halos (pressure, electron density, and metallicity) as functions of radius, halo mass, and redshift. The code assumes spherically symmetric, volume-filling warm/hot gas, and enables mock observations of the circumgalactic medium (CGM), group halos, and clusters across a number of wavebands including X-ray, sub-millimeter/millimeter, radio, and ultraviolet (UV).

PIRATES (Polarimetric Image Reconstruction AI for Tracing Evolved Structures) uses machine learning to perform image reconstruction. It uses MCFOST (ascl:2207.023) to generate models, then uses those models to build, train, iteratively fit, and evaluate PIRATES performance.

torchmfbd carries out multi-object multi-frame blind deconvolution (MOMFBD) of point-like or extended objects, and is especially tailored to solar images. The code is built on PyTorch and provides a high-level interface for adding observations, defining phase diversity channels, and adding regularization. It can deal with spatially variant PSFs either by mosaicking the images or by defining a spatially variant PSF. torchmfbd supports smooth solutions and solutions based on the ℓ 1 penalization of the isotropic undecimated wavelet transform of the object, and regularizations are easily extendable. The code also includes an API and a configuration file.

SPIBACK (SPIral arms & Bar bACKward integrations) generates Milky Way models through the backward integration method. The code allows users to plot the 2D local velocity space distribution at the Sun's position, as well as median Galactocentric radial velocity maps across the area of the Galactic disk probed with Gaia DR3. This can be done for different bar and spiral arms parameters. The parameters are set by default to be those of the "fiducial model" and can be adjusted as needed.

HYDRAD (HYDrodynamics and RADiation) computes solutions to field-aligned hydrodynamic equations in coronal loops. The code models a broad variety of phenomena, including multi-species plasma confined to full-length, magnetic flux tubes of arbitrary geometrical and cross-section variation in the field-aligned direction; solar flares driven by non-thermal electrons3 and Alfven waves4, and the non-thermal equilibrium response of the chromosphere; and coronal rain formed by condensations in thermal non-equilibrium where the adaptive grid is required to fully resolve and track multiple steep transition regions. HYDRAD also models ultracold, strongly coupled laboratory plasmas composed of weakly-ionized strontium. The code, written in C++, is modular in its structure; new capabilities can be added in a relatively straightforward way and handled robustly by the numerical scheme. HYDRAD is also intended to be fairly undemanding of computational resources, though its needs do depend strongly on the particular nature of each model run.

EXP performs and analyzes N-body simulations using biorthogonal and orthogonal expansions. The package also supports time series analysis of expansion coefficients using multivariate Singular Spectrum Analysis (mSSA) to discover new dynamical correlations, separate signal from noise, and visualize these in two- and three-dimensional renderings. EXP's object-oriented design enforces minimal consistency while retaining flexibility.

P-CORONA models the intensity and polarization of coronal atomic lines in any given three dimensional (3D) model of the solar corona. It takes into account the scattering of anisotropic radiation as well as the symmetry-breaking effects arising from the influence of magnetic fields, through the Hanle and Zeeman effects, and from non-radial solar wind velocities. The code solves the statistical equilibrium equations for the elements of the atomic density matrix corresponding to the multi-level atomic model under consideration, assuming complete frequency redistribution. The calculations are carried out assuming an optically thin plasma, with the emergent Stokes profiles resulting from the integration of the local emission coefficients along the line-of-sight in the chosen 3D coronal model. P-CORONA incorporates HDF5 input/output functionality and includes a graphical user interface.

Capivara implements a spectral-based segmentation method for Integral Field Unit (IFU) data cubes. The code uses hierarchical clustering in the spectral domain, grouping similar spectra to improve the signal-to-noise ratio without compromising astrophysical similarity among regions, and leverages advanced matrix operations via torch for GPU acceleration.

spherimatch performs efficient cross-matching and self-matching of astronomical catalogs in spherical coordinates. Designed for use in astrophysics, where data is naturally distributed on the celestial sphere, the package enables fast matching with an algorithmic complexity of O (N log N). It supports Friends-of-Friends (FoF) group identification and duplicate removal in spherical coordinates, and integrates easily with common data processing tools such as pandas.

PCM-HiPT (Planetary Climate Model for High Pressures and Temperatures) simulates the thermal structure of dense, hot terrestrial exoplanet atmospheres. This 1D line-by-line radiative-convective model uses a high-resolution spectral grid and HITRAN-based absorption data to model radiative energy transfer with high accuracy at elevated pressures and temperatures (>1000 K). PCM-HiPT extends the PCM_LBL model (ascl:2504.003) for early Mars conditions, and modifications allow PCM-HiPT to capture complex atmospheric structures, including detached convective zones and stable lower atmosphere layers driven by shortwave absorption.

SPAN (SPectral ANalysis) is a cross-platform graphical user interface (GUI) application for extracting, manipulating, and analyzing astronomical spectra. It is optimized for the study of galaxy spectra across the near-ultraviolet (NUV) to near-infrared (NIR) atmospheric windows.
SPAN extracts 1D spectra from FITS images and datacubes, performs spectral processing (e.g., Doppler correction, continuum modelling, denoising), and supports analyses such as line-strength measurements, stellar and gas kinematics, and stellar population studies, using both built-in routines and the widely adopted pPXF algorithm (ascl:1210.002) for full spectral fitting.
It runs on Windows, Linux, macOS, and Android, and features an intuitive, task-oriented interface. The goal of SPAN is to unify essential tools for modern spectral analysis into a single, user-friendly application that offers a flexible and accessible environment while maintaining scientific accuracy.

CosmoWAP (Cosmology with Wide-separation, relAtivistic and Primordial non-Gaussian contibutions) analyzes the Fourier power spectra and bispectra with wide-separation, relativistic and primordial non-Gaussian effects in large-scale structure cosmology. The analytical expressions themselves are computed analytically in Mathematica using MathWAP (ascl:2507.019) routines, which can be exported as .py files. CosmoWAP then takes these expressions and implements them for a given cosmology and set of survey parameters.

MathWAP contains Mathematica notebooks that compute the Fourier power spectrum and bispectrum, including contributions (up to second order) from wide-separation (WS) and relatativistic (GR) efects as well as primoridal non-Gaussianity (PNG). Outputs are stored from Mathematica in .json files in mathematica_expr. The read_mathematica notebook can be used to convert from Mathematica to Python formatting for use by CosmoWAP (ascl:2507.020).

Modern large scale cosmological hydrodynamic simulations require robust tools capable of analysing their data outputs in a parallel and efficient manner. We introduce SOAP (Spherical Overdensity and Aperture Processor), a Python package designed to compute halo and galaxy properties from SWIFT simulations after being post-processed with a subhalo finder. SOAP takes a subhalo catalogue as input and calculates a wide array of properties for each object. SOAP offers parallel processing capabilities via mpi4py for efficient handling of large datasets, and allows for consistent property calculation across multiple halo finders. SOAP supports various halo definitions, including spherical overdensities and fixed physical apertures, providing flexibility for diverse observational comparisons. The package is compatible with both dark matter-only and full hydrodynamic simulations, producing HDF5 catalogues that are integrated with the swiftsimio package for seamless unit handling.

QUIDS is a Python package for generating synthetic Stokes Q and U polarization maps using 3D dust density and Galactic Magnetic Field (GMF) shell data. It integrates polarized emission over log-spaced spherical shells, with polarization angles derived from GMF models such as UF23 or JF12. The goal is to explore whether small-scale structures in the GMF and dust distribution can reconstruct or preserve the large-scale polarization patterns observed across the sky. This package is particularly relevant for modeling and probing how local Galactic features contribute to or interfere with global polarization signals.

ysoisochrone handles the isochrones for young stellar objects (YSOs) and uses isochrones to derive the stellar mass and ages. The method uses a Bayesian inference approach. The code estimates the stellar masses, ages, and associated uncertainties by comparing their stellar effective temperature, bolometric luminosity, and their uncertainties with different stellar evolutionary models, including those specifically developed for YSOs. ysoisochrone also enables user-developed evolutionary tracks.

Spectool processes astronomical spectral data, offering a collection of common spectral analysis algorithms. The toolkit includes functions for spectral resampling, spectral flattening, radial velocity measurements, spectral convolution broadening, among others. Each function in the package is implemented independently, allowing users to select and utilize the desired features as needed. Spectool's functions have simple and intuitive interfaces, ensuring ease of use for various data sets and analysis tasks.

Spinifex is a pure Python tooling for ionospheric corrections in radio astronomy, e.g., getting total electron content and rotation measures. The code is in part a re-write of RMextract (ascl:1806.024). All existing features of RMextract have been re-implemented, but spinifex is not directly backwards compatible with RMextract.

nGIST (new Galaxy Integral-field Spectroscopy Tool) analyzes modern galaxy integral field spectroscopic (IFS) data. Borne out of the need for a robust but flexible analysis pipeline for an influx of MUSE and other galaxy IFS data, the code is the continuation of the archived GIST pipeline (ascl:1907.025). It improves memory and parallelization management and deals better with longer optical wavelength ranges and sky residuals that are particularly problematic at redder wavelengths (>7000 Angstrom). Performance improvements include memory and parallelization optimization, and smaller and more convenient output files. nGIST can create continuum-only cubes and offers better handling of cube variance and better bias estimation for stellar kinematics, and includes a pPXF-based emission line fitter and an updated version of Mapviewer for a quick-look interface to view results.

SAUSERO (Software to AUomatize in a Simple Environment the Reduction of Osiris+) processes raw science frames to address noise, cosmetic defects, and pixel heterogeneity, preparing them for photometric analysis for OSIRIS+ (Gran Telescopio Canarias). Correcting these artifacts is a critical prerequisite for reliable scientific analysis. The software applies observation-specific reduction steps, ensuring optimized treatment for different data types. Developed with a focus on simplicity and efficiency, SAUSERO streamlines the reduction pipeline, enabling researchers to obtain calibrated data ready for photometric studies.

Sapphire++ (Simulating astrophysical plasmas and particles with highly relativistic energies in C++) numerically solves the Vlasov–Fokker–Planck equation for astrophysical applications. It employs a numerical algorithm based on a spherical harmonic expansion of the distribution function, expressing the Vlasov–Fokker–Planck equation as a system of partial differential equations governing the evolution of the expansion coefficients. The code uses the discontinuous Galerkin method in conjunction with implicit and explicit time stepping methods to compute these coefficients, providing significant flexibility in its choice of spatial and temporal accuracy.

arctic_weather analyzes meteorological data recorded from High Arctic weatherstations (called Inuksuit) deployed on coastal mountains north of 80 degrees on Ellesmere Island Canada from 2006 through 2009, along with clear-sky fractions from horizon-viewing sky-monitoring cameras. The code calculates solar and lunar elevations, and so allows correlation of polar nighttime to the development of prevailing thermal inversion conditions in winter, and statistical comparison to other optical/infrared observatory sites.

COBRA (Cosmology with Optimally factorized Bases for Rapid Approximation) rapidly computes large-scale structure observables, separating scale dependence from cosmological parameters in the linear matter power spectrum while also minimizing the number of necessary basis terms. This enables direct and efficient computation of derived and nonlinear observables. Moreover, the dependence on cosmological parameters is efficiently approximated using radial basis function interpolation. COBRA opens a new window for efficient computations of higher loop and higher order correlators involving multiple powers of the linear matter power spectra. The resulting factorization can also be utilied in clustering, weak lensing and CMB analyses.

show_cube displays the results of reducing, aligning, and combining near-infrared integral field spectroscopy with the Gemini Observatory NIFS (Near-infrared Integral Field Spectrometer) instrument. Image slices are extracted from the raw data frames to make the input datacube. The code site also provides a tarfile containing all the raw NIFS FITS-format files for the observations of high-redshift radio galaxies 3C230, 3C294, and 4C+41.17, the last of which are reported, together with line-strengths using the MAPPINGS III (ascl:1306.008) shock models.

Coniferest implements anomaly detection algorithms and interactive active learning tools. The centerpiece of the package is an Isolation Forest algorithm, which operates by constructing random decision trees. Coniferest also offers two modified versions for active learning: AAD Forest and Pineforest. The AAD Forest modifies the Isolation Forest by reweighting its leaves based on responses from human experts, providing a faster alternative to the ad_examples package. Pineforest employs a filtering algorithm that builds and dismantles trees with each new human-machine iteration step. The Coniferest package provides a user-friendly interface for conducting interactive human-machine sessions; the code has been used for anomaly detection with a particular focus on light-curve data from large time-domain surveys.

Tayph analyzes high-resolution spectroscopic time-series observations of close-in exoplanets using a cross-correlation technique. The tool can be applied to transit observations of hot Jupiters made with echelle spectrographs at optical wavelengths. In particular, it can be applied to pipeline-reduced observations by HARPS, HARPS-N, ESPRESSO, CARMENES and to a certain extent UVES, with minimal interaction required. Tayph works on observations made with other instruments, provided the user provides these according to a specific format, and can also be used in conjunction with Molecfit (ascl:1501.013).

Nii-C implements a framework of automatic parallel tempering Markov Chain Monte Carlo. Parameters ensure an efficient parallel tempering process that is set by a control system during the initial stages of a sampling process. The autotuned parameters consist of two parts: the temperature ladders of all parallel tempering Markov Chains, and the proposal distributions for all model parameters across all parallel tempering chains. Written in C, Nii-C supersedes the Python code Nii (ascl:2111.010). Nii-C is parallelized using the message-passing interface protocol to optimize the efficiency of parallel sampling, which facilitates rapid convergence in the sampling of high-dimensional and multimodal distributions, as well as the expeditious code execution time. The code can be used to trace complex distributions due to its high sampling efficiency and quick execution speed.

The Opacity Wizard performs easy and fast visualizations of opacity and abundance data for exoplanet and brown dwarf atmospheres. It was designed to be used by observers studying these substellar objects as a way to explore which molecules are most important for a given planet and predict where the absorption features of those molecules will be. Opacity Wizard provides an iPython notebook with widgets for choosing a pressure, temperature, metallicity, and molecule list, and then create plots of the mixing ratios and opacities.

SysSimPyMMEN infers the minimum-mass extrasolar nebula (MMEN), a power-law profile for the minimum mass in disk solids required to form the existing exoplanets if they formed in their present locations. Designed to work with the SysSim clustered planetary system models (ascl:2507.001) that characterize the underlying occurrence and intra-system correlations of multi-planet systems, SysSimPyMMEN can also be applied to any other planetary system.

SysSimPyPlots loads, plots, and visualizes the simulated catalogs generated by ExoplanetsSysSim (ascl:2507.001), a comprehensive forward modeling framework for studying planetary systems based on the Kepler mission. In particular, it is designed to work with the SysSim clustered planetary system models (ascl:2507.003) that characterize the underlying occurrence and intra-system correlations of multi-planet systems. Unlike the SysSim codebase, which is written in Julia, SysSimPyPlot is written almost entirely in Python 3.

SysSimExClusters provides a comprehensive forward modelling framework for studying planetary systems in conjunction with ExoplanetsSysSim (ascl:2507.001). It includes several statistical models for describing the intrinsic planetary systems, their architectures, and the correlations within multi-planet systems using the Kepler population of exoplanet candidates.

LSCS (Lightweight Space Coronagraph Simulator) simulates realistic high-contrast space imaging instruments in their linear regime of small wavefront perturbations about the nominal dark hole. The code can be used for testing high-order wavefront sensing and control as well as post-processing algorithms. It models broadband images with sensor noise, wavefront drift, actuators drift, and residual effects from low-order wavefront sensing, and supports a model of the Roman Space Telescope Hybrid Lyot Coronagraph based on its FALCO (ascl:2304.004, ascl:2304.005) model. The LSCS package provides an example of dark hole maintenance using an Extended Kalman Filter and Electric Field Conjugation.

The ExoplanetsSysSim.jl package generates populations of planetary systems, simulates observations of those systems with a transit survey, and facilitates comparisons of simulated and observed catalogs of planetary systems. Critically, ExoplanetsSysSim accounts for intrinsic correlations in the sizes and orbital periods of planets within a planetary system.

We develop a Physics-Informed Neural Network (PINN) code to solve the modified Teukolsky equation under realistic astrophysical conditions. The code embeds domain-specific physics—spin-weighted curvature perturbations, quasi-normal mode (QNM) boundary conditions, and attenuation dynamics—directly into the training loss function. Applied to data from the GW190521 event, the model accurately infers complex QNM frequencies (ω = 0.2917 − 0.0389i) and learns an attenuation coefficient α = 0.04096, corresponding to a 14.4% decay rate. The code demonstrates strong predictive performance, reducing mean squared error by 50.3% (MSE = 0.2537 vs. 0.5310) compared to Bayesian baselines, and achieving a positive R² score. It further reveals non-trivial r–t coupling and gravitational memory effects, which standard exponential decay models fail to capture. This PINN-based implementation establishes a computationally efficient and accurate tool for environmental modeling in gravitational wave astrophysics and offers a path forward for black hole spectroscopy beyond vacuum assumptions.

Procoli extracts profile likelihoods in cosmology. It wraps MontePython (ascl:1805.027), the fast sampler written specifically for CLASS (ascl:1106.020). All likelihoods available for use with MontePython are hence immediately available for use. Procoli is based on a simulated-annealing optimizer to find the global maximum likelihoods value as well as the maximum likelihood points along the profile of any use input parameter.

CAMEL (Cosmological Analysis with Minuit Exploration of the Likelihood) performs cosmological parameters estimations using best fits, Monte-Carlo Markov Chains, and profile-likelihoods. Widely used in Planck satellite data analysis, by default it employs CLASS (ascl:1106.020) to compute all relevant cosmological quantities, but any other Boltzmann solver can easily be plugged in.

pinc ("profiles in cosmology") computes profile likelihoods in cosmology; it can also determine the (boundary-corrected) confidence intervals with the graphical construction. The code uses a simulated annealing scheme and interfaces with MontePython (ascl:1805.027). pinc consists of three short scripts; these automatically set the relevant parameters in MontePython, submit the minimization chains, and analyze the results.

OK Binaries is a tool for identifying suitable calibration binaries from the Washington Double Star (WDS) Sixth Orbit Catalog. It calculates orbital positions at any epoch, propagates uncertainties using Monte Carlo sampling, and generates orbit plots. The web app includes automated daily updates of binary positions and a searchable interface with filters for position, magnitude, separation, and other orbital parameters. OK Binaries can be used online, as a standalone offline browser app, or via the command line.

CLUES (CLustering UnsupErvised with Sequencer) analyzes spectral and IFU data. This fully interpretable clustering tool uses machine learning to classify and reduce the effective dimensionality of data sets. It combines multiple unsupervised clustering methods with multiscale distance measures using Sequencer (ascl:2105.006) to find representative end-member spectra that can be analyzed with detailed mineralogical modeling and follow-up observations. CLUES has been used on Spitzer IRS data and debris disk science, and can be applied to other high-dimensional spectral data sets, including mineral spectroscopy in general areas of astrophysics and remote sensing.

Bjet_MCMC automatically models multiwavelength spectral energy distributions of blazars, considering one-zone synchrotron-self-Compton (SSC) model with or without the addition of external inverse-Compton process from the thermal emission of the nucleus. The code also contains manual fitting functionalities for multi-zone SSC modeling. Bjet_MCMC is built as an MCMC python wrapper around the C++ code Bjet.

pynchrotron implements synchrotron emission from cooling electrons. It removes the need for GSL which was originally relied on for a quick computation of the synchrotron kernel. The code has been ported from GSL and written directly in python as well as accelerated with numba. pynchrotron also includes an astromodels (ascl:2506.019) function for direct use in 3ML (ascl:2506.018).

Astromodels defines models for likelihood or Bayesian analysis of astrophysical data. Though designed for analysis in the spectral domain, it can also be used as a toolbox containing functions of any variable. Astromodels is not a modeling package; it provides the tools to build a model as complex as one needs. A separate package such as 3ML (ascl:2506.018) is needed to fit the model to the data.

The Multi-Mission Maximum Likelihood framework (3ML) provides a common high-level interface and model definition for coherent and intuitive modeling of sources using all the available data, no matter their origin. Astrophysical sources are observed by different instruments at different wavelengths with an unprecedented quality, and each instrument and data type has its own ad-hoc software and handling procedure. 3ML's architecture is based on plug-ins; the package uses the official software of each instrument under the hood, thus guaranteeing that 3ML is always using the best possible methodology to deal with the data of each instrument. Though Maximum Likelihood is in the name for historical reasons, 3ML is an interface to several Bayesian inference algorithms such as MCMC and nested sampling as well as likelihood optimization algorithms.

Hydromass analyzes galaxy cluster mass profiles from X-ray and/or Sunyaev-Zel’dovich observations. It provides a global Bayesian framework for deprojection and mass profile reconstruction, including mass model fitting, forward fitting with parametric and polytropic models, and non-parametric log-normal mixture reconstruction. Hydromass easily loads public X-COP data products and applies reconstruction tools directly within a Jupyter notebook.

SBI++ is a complete methodology based on simulation-based (likelihood-free) inference that is customized for astronomical applications. Specifically, the code retains the fast inference speed of ∼1 sec for objects in the observational training set distribution, and additionally permits parameter inference outside of the trained noise and data at ~1 min per object. The package includes scripts for training and implementing SBI++ and is dependent on sbi (ascl:2306.002).

Octofitter performs Bayesian inference against a wide variety of exoplanet and binary star data. It is highly modular and allows users to easily adjust priors, change parameterizations, and specify arbitrary function relations between the parameters of one or more planets. Octofitter further supplies tools for examining model outputs including prior and posterior predictive checks and simulation based calibration.

M_-M_K- converts absolute 2MASS Ks-band magnitude (or a distance and a Ks-band magnitude) into an estimate of the stellar mass using the empirical relation derived from the resolved photometry and orbits of astrometric binaries. The code requires scalar values for K, distance, and corresponding uncertainties. M_-M_K- outputs errors based on the relationship's scatter and errors in the provided distance and Ks magnitude.

This One-Class Support Vector Machine (SVM) model detects exoplanet transit events. One-class SVMs fit data and make predictions faster than simple CNNs, and do not require specialized equipment such as Graphics Processing Units (GPU). The code uses a Gaussian kernel to compute a nonlinear decision boundary. After training, OCSVM-Transit-Detection requires that lightcurves classified as containing a transit have features very similar to the lightcurves in the training dataset, thus limiting misclassifications.

The Python wrapper pyTPCI couples newer versions of the hydrodynamics code PLUTO (ascl:1010.045) and the gas microphysics code CLOUDY (ascl:9910.001) to self-consistently simulate escaping atmospheres in 1D. Following TPCI (ascl:2506.012), on which pyTPCI is based, CLOUDY is modified to read in depth-dependent wind velocities, and to output useful physical quantities (including mass density, number density, and mean molecular weight as a function of depth).

The PLUTO CLOUDY Interface (TPCI) combines the PLUTO (ascl:1010.045) and CLOUDY (ascl.net:9910.001) simulation codes to simulate hydrodynamic evolution under irradiation from a source. The code solves the photoionization and chemical network of the 30 lightest elements. By combining an equilibrium photoionization solver with a general MHD code, TPCI provides an advanced simulation tool applicable to a variety of astrophysical problems.