ASCL.net

Astrophysics Source Code Library

Making codes discoverable since 1999

Welcome to the ASCL

The Astrophysics Source Code Library (ASCL) is a free online registry for source codes of interest to astronomers and astrophysicists, including solar system astronomers, and lists codes that have been used in research that has appeared in, or been submitted to, peer-reviewed publications. The ASCL is indexed by the SAO/NASA Astrophysics Data System (ADS) and Web of Science and is citable by using the unique ascl ID assigned to each code. The ascl ID can be used to link to the code entry by prefacing the number with ascl.net (i.e., ascl.net/1201.001).


Most Recently Added Codes

2021 Jul 27

[ascl:2107.020] Chem-I-Calc: Chemical Information Calculator

Chem-I-Calc evaluates the chemical information content of resolved star spectroscopy. It takes advantage of the Fisher information matrix and the Cramér-Rao inequality to quickly calculate the Cramér-Rao lower bounds (CRLBs), which give the best theoretically achievable precision from a set of observations.

[ascl:2107.019] PlaSim: Planet Simulator

PlaSim is a climate model of intermediate complexity for Earth, Mars and other planets. It is written for a university environment, to be used to train the next GCM (general circulation model) developers, to support scientists in understanding climate processes, and to do fundamental research. In addition to an atmospheric GCM of medium complexity, PlaSim includes other compartments of the climate system such as, for example, an ocean with sea ice and a land surface with a biosphere. These other compartments are reduced to linear systems. In other words, PlaSim consists of a GCM with a linear ocean/sea-ice module formulated in terms of a mixed layer energy balance. The soil/biosphere module is introduced analoguously. Thus, working with PlaSim is like testing the performance of an atmospheric or oceanic GCM interacting with various linear processes, which parameterize the variability of the subsystems in terms of their energy (and mass) balances.

[ascl:2107.018] ART: A Reconstruction Tool

ART reconstructs log-probability distributions using Gaussian processes. It requires an existing MCMC chain or similar set of samples from a probability distribution, including the log-probabilities. Gaussian process regression is used for interpolating the log-probability for the rescontruction, allowing for easy resampling, importance sampling, marginalization, testing different samplers, investigating chain convergence, and other operations.

[ascl:2107.017] PyCactus: Post-processing tools for Cactus computational toolkit simulation data

PyCactus contains tools for postprocessing data from numerical simulations performed with the Einstein Toolkit, based on the Cactus computational toolkit. The main package is PostCactus, which provides a high-level Python interface to the various data formats in a simulation folder. Further, the package SimRep allows the automatic creation of html reports for a simulation, and the SimVideo package allows the creation of movies visualizing simulation data.

[ascl:2107.016] shear-stacking: Stacked shear profiles and tests based upon them

shear-stacking calculates stacked shear profiles and tests based upon them, e.g. consistency for different slices of lensed background galaxies. The basic concept is that the lensing signal in terms of surface mass density (instead of shear) should be entirely determined by the properties of the lens sample and have no dependence on source galaxy properties.

[ascl:2107.015] shapelens: Astronomical image analysis and shape estimation framework

The shapelens C++ library provides ways to load galaxies and star images from FITS files and catalogs and to analyze their morphology. The main purpose of this library is to make several weak-lensing shape estimators publicly available. All of them are based on the moments of the brightness distribution. The estimators include DEIMOS, for analytic deconvolution in moment space, DEIMOSElliptical, a practical implemention of DEIMOS with an automatically matched elliptical weight function, DEIMOSCircular, which is identical to DEIMOSElliptical but with a circular weight function, and others.

[ascl:2107.014] Skylens++: Simulation package for optical astronomical observations

Skylens++ implements a Layer-based raytracing framework particularly well-suited for realistic simulations of weak and strong gravitational lensing. Source galaxies can be drawn from analytic models or deep space-based imaging. Lens planes can be populated with arbitrary deflectors, typically either from N-body simulations or analytic lens models. Both sources and lenses can be placed at freely configurable positions into the light cone, in effect allowing for multiple source and lens planes.

[ascl:2107.013] GUBAS: General Use Binary Asteroid Simulator

GUBAS (General Use Binary Asteroid Simulator) predicts binary asteroid system behaviors by implementing the Hou 2016 realization of the full two-body problem (F2BP). The F2BP models binary asteroid systems as two arbitrary mass distributions whose mass elements interact gravitationally and result in both gravity forces and torques. To account for these mass distributions and model the mutual gravity of the F2BP, GUBAS computes the inertia integrals of each body up to a user defined expansion order. This approach provides a recursive expression of the mutual gravity potential and represents a significant decrease in the computational burden of the F2BP when compared to other methods of representing the mutual potential.

[ascl:2107.012] PyROA: Modeling quasar light curves

PyROA models quasar light curves where the variability is described using a running optimal average (ROA), and parameters are sampled using Markov Chain Monte Carlo (MCMC) techniques using emcee (ascl:1303.002). Using a Bayesian approach, priors can be used on the sampled parameters. Currently it has three main uses: 1.) Determining the time delay between lightcurves at different wavelengths; 2.) Intercalibrating light curves from multiple telescopes, merging them into a single lightcurve; and 3.) Determining the time delay between images of lensed quasars, where the microlensing effects are also modeled. PyROA also includes a noise model, where there is a parameter for each light curve that adds extra variance to the flux measurments, to account for underestimated errors; this can be turned off if required. Example jupyter notebooks that demonstrate each of the three main uses of the code are provided.

[ascl:2107.011] AlignBandColors: Inter-color-band image alignment tool

AlignBandColors (ABC) aligns inter-color-band astronomical images to a 100th of a pixel accuracy using surrounding stars as guiding points. It has currently been tested with Sloan Digital Sky Survey (SDSS) Data Release 12 images, but is designed to be survey-independent. The code is part of the SpArcFiRe (ascl:2107.010) method.