The CASSL pipeline
1) forecasts galaxy-scale strong lenses for JWST, including Einstein radii down to θ_E=0.02″ system (generalizable to other telescopes and selection criteria).
2) simulates galaxy-scale strong lenses in the range 0.02″

The PANIC Pipeline (PAPI) is an open-source Python-based software package designed for the automated reduction of near-infrared imaging data from the PAnoramic Near-Infrared Camera (PANIC) at the Calar Alto Observatory (CAHA). Initially developed for the HAWAII-2RG detectors of PANIC, PAPI has been updated to support the HAWAII-4RG detector installed in 2025. It provides a comprehensive suite of tools for processing raw astronomical images, including basic calibration, cosmic-ray removal, crosstalk correction, sky subtraction, non-linearity correction, and astrometric calibration. PAPI also includes the PANIC Quick-Look Tool (PQL), a graphical user interface for prompt data quality assessment during observations. Available under the GNU General Public License, PAPI is a versatile tool optimized for broadband imaging of extragalactic sources, such as galaxy surveys and cluster studies.

We present a Python-based tool for simulating and fitting Galactic Rotation Curves (GRCs) using a modular framework of physically motivated mass models. This tool directly analyzes raw observational data—either from tabulated sources or raw FITS velocity maps—by modeling contributions from the bulge, disk, and dark matter halo using Hernquist, de Vaucouleurs, exponential disk, Navarro-Frenk-White (NFW), and Burkert profiles. It supports three fitting techniques: non-linear least squares, bootstrap resampling, and Markov Chain Monte Carlo (MCMC) with full uncertainty propagation. The tool outputs best-fit parameters, confidence intervals, and a suite of diagnostic plots including rotation curve fits, residuals, and posterior distributions. Designed to address long-standing challenges in GRC analysis—such as rigid model architectures, poor error handling, and lack of component-wise transparency—our tool enables accurate, reproducible mass decomposition across diverse galaxy types. Its flexibility, efficiency, and user-friendly interface make it suitable for both pedagogical and research applications in galactic dynamics and dark matter studies.