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 ascl.net (*i.e.*, ascl.net/1201.001).

[submitted]
Vizic: A Jupyter-based Interactive Visualization Tool for Astronomical Catalogs

Vizic is a Python visualization library that builds the connection between images and catalogs through an interactive map of the sky region. Vizic visualizes catalog data over a custom background canvas using the shape, size and orientation of each object in the catalog. The displayed objects in the map are highly interactive and customizable comparing to those in the images. We can filter or apply colormaps to these objects by their property values, such as redshift and magnitude. We can also sub-select the objects using a lasso-like tool for further analysis through standard Python functions from inside a Jupyter notebook. Furthermore, Vizic allows custom overlays to be appended dynamically on top of the sky map. We have initially implemented several overlays, namely, Voronoi, Delaunay, Minimum Spanning Tree and HEALPix layers, which are helpful for visualizing large-scale structure. All these overlays can be generated, added or removed dynamically with just one line of code. The catalog data is kept in a non-relational database, and the interfaces were developed in JavaScript and Python to work within Jupyter Notebook, which allows to create custom widgets, user generated scripts to analyze and plot the data selected/displayed in the interactive map. This unique design makes Vizic a very powerful and flexible interactive analysis tool. Vizic can be adopted in variety of exercises, for example, data inspection, clustering analysis, galaxy alignment studies, outlier identification or simply large-scale visualizations.

[submitted]
KAULAKYS: inelastic collisions between hydrogen atoms and Rydberg atoms

Library of codes to calculate cross sections and rate coefficients for inelastic collisions with hydrogen atoms according to the free electron model of Kaulakys (1986, 1991). Written in IDL.

[submitted]
MSWAVEF: Momentum-Space Wavefunctions

Code to calculate hydrogenic and non-hydrogenic momentum-space electronic wavefunctions is presented. Such wavefunctions are often required to calculate various collision processes, such as excitation and line broadening cross sections. The hydrogenic functions are calculated using the standard analytical expressions. The non-hydrogenic functions are calculated within quantum defect theory according to the method of Hoang Binh and van Regemorter (1997). Required Hankel transforms have been determined analytically for angular momentum quantum numbers ranging from zero to 13 using Mathematica. Calculations for higher angular momentum quantum numbers are possible, but slow (since calculated numerically). The code is written in IDL.

[ascl:1701.001]
The Joker: A custom Monte Carlo sampler for binary-star and exoplanet radial velocity data

Given sparse or low-quality radial-velocity measurements of a star, there are often many qualitatively different stellar or exoplanet companion orbit models that are consistent with the data. The consequent multimodality of the likelihood function leads to extremely challenging search, optimization, and MCMC posterior sampling over the orbital parameters. The Joker is a custom-built Monte Carlo sampler that can produce a posterior sampling for orbital parameters given sparse or noisy radial-velocity measurements, even when the likelihood function is poorly behaved. The method produces correct samplings in orbital parameters for data that include as few as three epochs. The Joker can therefore be used to produce proper samplings of multimodal pdfs, which are still highly informative and can be used in hierarchical (population) modeling.

[submitted]
DiskSim: Modeling Accretion Disk Dynamics with SPH

DiskSim is a source-code distribution of the SPH accretion disk modeling code described in Simpson & Wood (1998) and Wood, Thomas, & Simpson (2009). The code had been released in a Windows executable form as FITDisk (Dolence, Wood & Simpson 2005; ascl:1305.011). The code released now is the full research code in Fortran, which can be modified as needed by the user.

[submitted]
Gala: Galactic astronomy and gravitational dynamics

Gala is a Python package (and Astropy affiliated package) for Galactic astronomy and gravitational dynamics. The bulk of the package centers around implementations of gravitational potentials, numerical integration, nonlinear dynamics, and astronomical velocity transformations (i.e. proper motions). Gala uses the Astropy units and coordinates subpackages extensively to provide a clean, pythonic interface to these features but does any heavy-lifting in C and Cython for speed.

[ascl:1612.022]
REPS: REscaled Power Spectra for initial conditions with massive neutrinos

Zennaro, Matteo; Bel, Julien; Villaescusa-Navarro, Francisco; Carbone, Carmelita; Sefusatti, Emiliano; Guzzo, Luigi

REPS (REscaled Power Spectra) provides accurate, one-percent level, numerical simulations of the initial conditions for massive neutrino cosmologies, rescaling the late-time linear power spectra to the simulation initial redshift.

[ascl:1612.021]
BaTMAn: Bayesian Technique for Multi-image Analysis

Casado, J.; Ascasibar, Y.; García-Benito, R.; Guidi, G.; Choudhury, O. S.; Bellocchi, E.; Sánchez, S. F.; Díaz, A. I.

Bayesian Technique for Multi-image Analysis (BaTMAn) characterizes any astronomical dataset containing spatial information and performs a tessellation based on the measurements and errors provided as input. The algorithm iteratively merges spatial elements as long as they are statistically consistent with carrying the same information (i.e. identical signal within the errors). The output segmentations successfully adapt to the underlying spatial structure, regardless of its morphology and/or the statistical properties of the noise. BaTMAn identifies (and keeps) all the statistically-significant information contained in the input multi-image (e.g. an IFS datacube). The main aim of the algorithm is to characterize spatially-resolved data prior to their analysis.

[ascl:1612.020]
Grackle: Chemistry and radiative cooling library for astrophysical simulations

Enzo Collaboration; AGORA Collaboration; Bryan, Greg L.; Norman, Michael L.; O'Shea, Brian W.; Kim, Ji-hoon; Abel, Tom; Agertz, Oscar; Anninos, Peter; Bordner, James; Bryan, Greg L.; Cen, Renyue; Ceverino, Daniel; Christensen, Charlotte; Collins, David C.; Conroy, Charlie; Dekel, Avishai; Emerick, Andrew; Glover, Simon C. O.; Gnedin, Nickolay Y.; Goldbaum, Nathan J.; Guedes, Javiera; Hahn, Oliver; Harkness, Robert P.; Hobbs, Alexander; Hopkins, Philip F.; Hummels, Cameron B.; Iannuzzi, Francesca; Keres, Dusan; Khochfar, Sadegh; Klypin, Anatoly; Kravtsov, Andrey V.; Kritsuk, Alexei G.; Krumholz, Mark R.; Kuhlen, Michael; Leitner, Samuel N.; Li, Yuan; Madau, Piero; Mayer, Lucio; Moody, Christopher E.; Nagamine, Kentaro; Norman, Michael L.; Oishi, Jeffrey S.; Onorbe, Jose; O'Shea, Brian W.; Pillepich, Annalisa; Primack, Joel R.; Quinn, Thomas; Read, Justin I.; Regan, John; Reynolds, Daniel R.; Robertson, Brant E.; Rocha, Miguel; Rudd, Douglas H.; Schive, Hsi-Yu; Shen, Sijing; Simpson, Christine M.; Skillman, Samuel W.; Skory, Stephen; Smith, Britton D.; So, Geoffrey C.; Szalay, Alexander S.; Tasker, Elizabeth; Teyssier, Romain; Thompson, Robert; Todoroki, Keita; Turk, Matthew J.; Wadsley, James W.; Wang, Peng; Wise, John H.; Xu, Hao; Zhao, Fen; Zolotov, Adi

The chemistry and radiative cooling library Grackle provides options for primordial chemistry and cooling, photo-heating and photo-ionization from UV backgrounds, and support for user-provided arrays of volumetric and specific heating rates for astrophysical simulations and models. The library provides functions to update chemistry species; solve radiative cooling and update internal energy; and calculate cooling time, temperature, pressure, and ratio of specific heats (gamma), and has interfaces for C, C++, Fortran, and Python codes.

[ascl:1612.019]
Trident: Synthetic spectrum generator

Trident creates synthetic absorption-line spectra from astrophysical hydrodynamics simulations. It uses the yt package (ascl:1011.022) to read in simulation datasets and extends it to provide realistic synthetic observations appropriate for studies of the interstellar, circumgalactic, and intergalactic media.