An interactive, WebGPU-accelerated simulation of Large-Scale Structure (LSS) evolution. The software utilizes a "2.5D" Universe approach, projecting a thin slice of a 3D universe onto a 2D plane, to visualize the formation of cosmic filaments and voids from z = 10 to the present via a live web interface. It combines analytical 2LPT with a local quasi-N-body gravity scheme, incorporating rigorous background expansion and structure growth for LCDM and w0-wa dark energy models. To maintain smooth interactivity with up to 200k tracers, particle interactions are computed locally and include a phenomenological adhesion model. The tool features two distinct modes: a cosmological sandbox with realistic initial conditions and an "enhanced BAO" mode designed to highlight the emergence of Baryon Acoustic Oscillation signals. Optimized for high-performance browser rendering (WebGL/WebGPU), it is designed for professional scientific presentations, classroom teaching, and public outreach.

An interactive, browser-based tool for exploring gravitational lensing phenomena. The software implements rigorous mass models, including point-mass, NFW halos, elliptical halos, and cosmic void profiles, allowing users to visualize lensed images and critical curves in real-time via a live web interface. While the physics is strictly grounded in these models, the lensing effects are purposefully exaggerated to highlight phenomenological features for educational clarity. It is designed for professional presentations, scientific outreach, and teaching.

GpuFitsCrypt is a framework that integrates a flexible policy engine for fine-grained access control with a GPU-accelerated implementation of the AES-GCM authenticated encryption protocol for massive astronomical catalogs in FITS format. The system implements a novel parallel tree-reduction strategy to overcome the inherently sequential Galois/Counter Mode (GCM) authentication hash (GHASH) bottleneck, achieving authenticated encryption throughput exceeding 380 MB/s suitable for petabyte-scale astronomical data. The framework provides a robust mechanism for data providers to enforce access policies ensuring both confidentiality and integrity without hindering research workflows.

growpacity computes mean opacities for dust populations with arbitrary composition, maximum grain size a_max, and size distribution power-law index q. It uses optool (ascl:2104.010) to compute frequency-dependent absorption and scattering coefficients over a configurable parameter grid, which are averaged into Rosseland and Planck mean opacities as functions of a_max, q, and temperature. The results are stored in lightweight tables that can be efficiently interpolated via provided C and Python interfaces, enabling use in high-performance radiation hydrodynamics and dust evolution simulations with dynamically varying grain size distributions.

Skynet SOAP is a field-wide aperture photometry pipeline for astronomical observations from the Skynet Robotic Telescope Network. The software performs automated source extraction, background subtraction, aperture photometry, catalog cross-matching, and photometric calibration for all sources in an image. It supports SEP-based source extraction and photometry, forced photometry at user-specified sky positions, limiting-magnitude estimation, configurable aperture selection, calibration against catalogs including SkyMapper, APASS, and Pan-STARRS, and export to multiple tabular formats. Originally designed for follow-up observations of gamma-ray bursts, the pipeline enables science-ready photometric analysis of transient and time-domain observations made with Skynet.

SolRaT solves the polarized non-LTE radiative transfer problem in solar and stellar atmospheres within the multi-term atom model. The emergent Stokes profiles in the presence of arbitrary magnetic fields are calculated by solving the coupled non-LTE statistical equilibrium and polarized radiative transfer equations. The code includes a set of pre-configured atom models for selected spectral lines including He I D3, and provides a flexible modeling interface for prototyping of polarized non-LTE line formation.

This technical report describes the architecture and functionality of RunClass, a numerical engine developed to simulate cosmological background evolution. The system is optimized for Dynamical Dark Sector models, integrating dual-scalar-fields (Fuzzy Dark Matter and Quintessence) to address the H 0 and S 8 tensions within the ΛCDM framework.

TriPoDPy simulates the evolution of gas and dust in protoplanetary disks using a parametric dust-evolution model. It models the radial evolution of disk material, including viscous evolution of the gas and the advection, diffusion, and growth of dust particles. It implements the TriPoD dust model to represent dust size distributions and track their evolution across the disk. The code uses Simframe (ascl:2603.018) for running simulations, and its Simulation class inherits attributes from DustPy (ascl:2207.016). TriPoDPy can be used to explore the structure and dynamics of protoplanetary disks and the processes that influence dust growth and transport during planet formation.

Simframe facilitates setting up and running scientific simulations. The package organizes simulation data into fields derived from NumPy arrays, allowing users to define variables, parameters, and differential equations within a unified simulation frame. It includes numerical integration schemes—both explicit and implicit—to evolve model variables and supports adaptive step sizes and custom integration methods. simframe also provides tools for structuring simulation components, updating variables during integration, and writing or reading output data files. Example applications include solving coupled differential equations and modeling dynamical systems such as N-body problems or compartmental models.

easyspec streamlines long-slit spectroscopy. The code reduces raw long-slit spectroscopic data, and extracts and calibrates spectra in wavelegnth and flux. It can fit a model to each line of the spectrum with a MCMC approach and recover physical quantities such as redshift, dispersion velocity, FWHM, and line flux. easyspec can also be used to fit two Gaussian components, explore the MCMC posterior distributions, and stack several spectra of the same target collected with different instruments.