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 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 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 (i.e.,

Most Recently Added Codes

2014 Nov 27

[submitted] POSTMORTEM -- visibility data reduction and map making package

POSTMORTEM is the visibility data reduction and map making package from MRAO, for use with the Ryle and CLFST telescopes at Cambridge. It contains sub-systems for:

- Monitoring telescope performance
- Displaying and editing the visibility data
- Performing calibrations
- Removing flux from interfering bright sources
- Map-making

[submitted] Anmap -- An image and data analysis system

Anmap is a system for the analysis and processing of images and spectral data. Originally written for use in Radio Astronomy, much of its functionality is applicable to other disciplines and the package is being enhanced by the addition of new algorithms and analysis procedures of direct use in, for example, NMR imaging and spectroscopy. The unique feature of Anmap is the emphasis placed on the analysis of data with an aim to extracting quantitative results for comparison with theoretical models and/or other experimantal data. To achieve this Anmap provides:

- A wide range of tools for analysis, fitting and modelling (including standard image and data processing algorithms);

- A powerful environment for users to develop their own analysis/processing tools either by combining existing algorithms and facilities with the very powerful command (scripting) language or by writing new routines in FORTRAN which integrate seemlessly with the rest of Anmap.

2014 Nov 26

[submitted] JCMT COADD -- UKT14 continuum and photometry data reduction

Used to reduce photometry and continuum data from the UKT14 instrument that was on the James Clerk Maxwell Telescope in the 1990s. The software can co-add multiple observations, and perform sigma clipping and Kolmogorov-Smirnov statistical analysis.

2014 Nov 22

[ascl:1411.014] NAFE: Noise Adaptive Fuzzy Equalization

NAFE (Noise Adaptive Fuzzy Equalization) is an image processing method allowing for visualization of fine structures in SDO AIA high dynamic range images. It produces artifact-free images and gives significantly better results than methods based on convolution or Fourier transform.

[ascl:1411.013] NEAT: Nebular Empirical Analysis Tool

NEAT is a fully automated code which carries out a complete analysis of lists of emission lines to estimate the amount of interstellar extinction, calculate representative temperatures and densities, compute ionic abundances from both collisionally excited lines and recombination lines, and finally to estimate total elemental abundances using an ionization correction scheme. NEAT uses a Monte Carlo technique to robustly propagate uncertainties from line flux measurements through to the derived abundances.

[ascl:1411.012] util_2comp: Planck-based two-component dust model utilities

The util_2comp software utilities generate predictions of far-infrared Galactic dust emission and reddening based on a two-component dust emission model fit to Planck HFI, DIRBE and IRAS data from 100 GHz to 3000 GHz. These predictions and the associated dust temperature map have angular resolution of 6.1 arcminutes and are available over the entire sky. Implementations in IDL and Python are included.

[ascl:1411.011] PyMGC3: Finding stellar streams in the Galactic Halo using a family of Great Circle Cell counts methods

PyMGC3 is a Python toolkit to apply the Modified Great Circle Cell Counts (mGC3) method to search for tidal streams in the Galactic Halo. The code computes pole count maps using the full mGC3/nGC3/GC3 family of methods. The original GC3 method (Johnston et al., 1996) uses positional information to search for 'great-circle-cell structures'; mGC3 makes use of full 6D data and nGC3 uses positional and proper motion data.

2014 Nov 19

[submitted] PyPHOT: Simple DAOPHOT-Type photometry in Python

PyPhot is a simple Python translation of DAOPHOT-type (ascl:1104.011) photometry procedures from the IDL AstroLib (Landsman 1993), including aperture and PSF-fitting algorithms, with a few modest additions to increase functionality and ease of use. These codes allow fast, easy, and reliable photometric measurements and are currently used in the Pan-STARRS supernova pipeline and the HST CLASH/CANDELS supernova analysis.

[submitted] AMADA: Analysis of Multidimensional Astronomical DAtasets

AMADA allows an iterative exploration and information retrieval of high-dimensional data sets. This is done by performing a hierarchical clustering analysis for different choices of correlation matrices and by doing a principal components analysis in the original data. Additionally, AMADA provides a set of modern visualization data-mining diagnostics. The user can switch between them using the different tabs.

2014 Nov 11

[ascl:1411.010] Raga: Monte Carlo simulations of gravitational dynamics of non-spherical stellar systems

Raga (Relaxation in Any Geometry) is a Monte Carlo simulation method for gravitational dynamics of non-spherical stellar systems. It is based on the SMILE software (ascl:1308.001) for orbit analysis. It can simulate stellar systems with a much smaller number of particles N than the number of stars in the actual system, represent an arbitrary non-spherical potential with a basis-set or spline spherical-harmonic expansion with the coefficients of expansion computed from particle trajectories, and compute particle trajectories independently and in parallel using a high-accuracy adaptive-timestep integrator. Raga can also model two-body relaxation by local (position-dependent) velocity diffusion coefficients (as in Spitzer's Monte Carlo formulation) and adjust the magnitude of relaxation to the actual number of stars in the target system, and model the effect of a central massive black hole.