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ASCL.NET


ASTROPHYSICS SOURCE CODE LIBRARY


MAKING CODES DISCOVERABLE SINCE 1999


Home About Resources Browse Submissions News Dashboard


WELCOME TO THE ASCL

The Astrophysics Source Code Library (ASCL) is a free online registry and
repository 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


2023 DEC 31

[ascl:2312.036] SubGen2: Subhalo population generator
He, Feihong; Han, Jiaxin; Gao, Hongyu; Zhang, Jiajun

The SubGen2 subhalo population generator works for both CDM and WDM of arbitrary
DM particle mass. It can be used to generate a population of subhaloes according
to the joint distribution of subhalo bound mass, infall mass and halo-centric
distance in a halo of a given mass. SubGen2 is an extension to SubGen
(ascl:2312.035), which works only for CDM subhaloes.

[ascl:2312.035] SubGen: Fast subhalo sampler
Han, Jiaxin

SubGen generates Monte-Carlo samples of dark matter subhaloes. It fully
describes the joint distribution of subhaloes in final mass, infall mass, and
radius; it can be used to predict derived distributions involving combinations
of these quantities, including the universal subhalo mass function, the subhalo
spatial distribution, the gravitational lensing profile, the dark matter
annihilation radiation profile and boost factor. SubGen works only for CDM
subhaloes; for an extension of the code to also work with WDM subhaloes, see
SubGen2 (ascl:2312.036).

[ascl:2312.034] pycheops: Light curve analysis for ESA CHEOPS data
Maxted, P. F. L.; Ehrenreich, D.; Wilson, T. G.; Alibert, Y.; Cameron, A.
Collier; Hoyer, S.; Sousa, S. G.; Olofsson, G.; Bekkelien, A.; Deline, A.;
Delrez, L.; Bonfanti, A.; Borsato, L.; Alonso, R.; Anglada Escudé, G.; Barrado,
D.; Barros, S. C. C.; Baumjohann, W.; Beck, M.; Beck, T.; Benz, W.; Billot, N.;
Biondi, F.; Bonfils, X.; Brandeker, A.; Broeg, C.; Bárczy, T.; Cabrera, J.;
Charnoz, S.; Corral Van Damme, C.; Csizmadia, Sz; Davies, M. B.; Deleuil, M.;
Demangeon, O. D. S.; Demory, B. -O.; Erikson, A.; Florén, H. G.; Fortier, A.;
Fossati, L.; Fridlund, M.; Futyan, D.; Gandolfi, D.; Gillon, M.; Guedel, M.;
Guterman, P.; Heng, K.; Isaak, K. G.; Kiss, L.; Laskar, J.; Lecavelier des
Etangs, A.; Lendl, M.; Lovis, C.; Magrin, D.; Nascimbeni, V.; Ottensamer, R.;
Pagano, I.; Pallé, E.; Peter, G.; Piotto, G.; Pollacco, D.; Pozuelos, F. J.;
Queloz, D.; Ragazzoni, R.; Rando, N.; Rauer, H.; Reimers, C.; Ribas, I.; Salmon,
S.; Santos, N. C.; Scandariato, G.; Simon, A. E.; Smith, A. M. S.; Steller, M.;
Swayne, M. I.; Szabó, Gy M.; Ségransan, D.; Thomas, N.; Udry, S.; Van Grootel,
V.; Walton, N. A.

pycheops analyzes CHEOPS light curve data. The models in the package can also be
applied to other types of data. pycheops includes a "cook book" and examples; in
addition, it provides a command-line tool that aids in the preparation of
observing requests for CHEOPS observers.

[ascl:2312.033] RADIS: Fast line-by-line code for high-resolution infrared
molecular spectra
Pannier, E.; Laux, C.O.; van den Bekerom, D.C.M.; Minesi, N.; Soref, J.; Kumar,
A.; Misra, P.; Verma, S.; Grimaldi, C.; Sharma, S.; Huy, T.H.N.; Aryan, G.;
Kawahara, H.

RADIS resolves spectra with millions of lines within seconds on a single-CPU and
can be GPU-accelerated. It supports HITRAN, HITEMP and ExoMol out-of-the-box
(auto-download), and therefore is particularly suitable to compute
cross-sections or transmission spectra at high-temperature. RADIS includes
equilibrium calculations for all species, and non-LTE for CO2 and CO.

[ascl:2312.032] gaia_tools: Tools for working with Gaia and related data sets
Bovy, Jo

gaia_tools contains codes for working with the ESA/Gaia data and related data
sets (APOGEE, GALAH, LAMOST DR2, and RAVE). Written in Python, it includes tools
to read catalogs, perform cross-matching, read RVS or XP spectra, and query the
Gaia archive. gaia_tools also contains various matching recipes, such as
matching APOGEE or APOGEE-RC to Gaia DR2, and RAVE to TGAS (taking into account
the epoch difference).

[ascl:2312.031] AM3: Astrophysical Multi-Messenger Modeling
Klinger, Marc; Rudolph, Annika; Rodrigues, Xavier; Yuan, Chengchao; Fichet de
Clairfontaine, Gaëtan; Fedynitch, Anatoli; Winter, Walter; Pohl, Martin; Gao,
Shan

AM3 simulates lepto-hadronic interactions in astrophysical environments. It
solves the time-dependent partial differential equations for the energy spectra
of electrons, positrons, protons, neutrons, photons, neutrinos as well as
charged secondaries (pions and muons), immersed in an isotropic magnetic field.
The code accounts for the emission of photons and charged secondaries in
electromagnetic and hadronic interactions feed back into the interaction rates
in a time-dependent manner, therefore grasping non-linear effects including
electromagnetic cascades. AM3 is computationally efficient, making it possible
to scan vast source parameter scans and fit the observational data, and has been
deployed to explain multi-wavelength observations from blazars, gamma-ray bursts
and tidal disruption events.

[ascl:2312.030] matvis: Fast matrix-based visibility simulator
Kittiwisit, Piyanat; Murray, Steven G.; Garsden, Hugh; Bull, Philip; Cain,
Christopher; Parsons, Aaron R.; Sipple, Jackson; Abdurashidova, Zara; Adams,
Tyrone; Aguirre, James E.; Alexander, Paul; Ali, Zaki S.; Baartman, Rushelle;
Balfour, Yanga; Beardsley, Adam P.; Berkhout, Lindsay M.; Bernardi, Gianni;
Billings, Tashalee S.; Bowman, Judd D.; Bradley, Richard F.; Burba, Jacob;
Carey, Steven; Carilli, Chris L.; Chen, Kai-Feng; Cheng, Carina; Choudhuri,
Samir; DeBoer, David R.; de Lera Acedo, Eloy; Dexter, Matt; Dillon, Joshua S.;
Dynes, Scott; Eksteen, Nico; Ely, John; Ewall-Wice, Aaron; Fagnoni, Nicolas;
Fritz, Randall; Furlanetto, Steven R.; Gale-Sides, Kingsley; Gehlot, Bharat
Kumar; Ghosh, Abhik; Glendenning, Brian; Gorce, Adelie; Gorthi, Deepthi; Greig,
Bradley; Grobbelaar, Jasper; Halday, Ziyaad; Hazelton, Bryna J.; Hewitt,
Jacqueline N.; Hickish, Jack; Huang, Tian; Jacobs, Daniel C.; Josaitis, Alec;
Julius, Austin; Kariseb, MacCalvin; Kern, Nicholas S.; Kerrigan, Joshua; Kim,
Honggeun; Kohn, Saul A.; Kolopanis, Matthew; Lanman, Adam; La Plante, Paul; Liu,
Adrian; Loots, Anita; Ma, Yin-Zhe; MacMahon, David H. E.; Malan, Lourence;
Malgas, Cresshim; Malgas, Keith; Marero, Bradley; Martinot, Zachary E.;
Mesinger, Andrei; Molewa, Mathakane; Morales, Miguel F.; Mosiane, Tshegofalang;
Neben, Abraham R.; Nikolic, Bojan; Devi Nunhokee, Chuneeta; Nuwegeld, Hans;
Pascua, Robert; Patra, Nipanjana; Pieterse, Samantha; Qin, Yuxiang; Rath,
Eleanor; Razavi-Ghods, Nima; Riley, Daniel; Robnett, James; Rosie, Kathryn;
Santos, Mario G.; Sims, Peter; Singh, Saurabh; Storer, Dara; Swarts, Hilton;
Tan, Jianrong; Thyagarajan, Nithyanandan; van Wyngaarden, Pieter; Williams,
Peter K. G.; Xu, Zhilei; Zheng, Haoxuan

matvis simulates radio interferometric visibilities at the necessary scale with
both CPU and GPU implementations. It is matrix-based and applicable to wide
field-of-view instruments such as the Hydrogen Epoch of Reionization Array
(HERA) and the Square Kilometre Array (SKA), as it does not make any
approximations of the visibility integral (such as the flat-sky approximation).
The only approximation made is that the sky is a collection of point sources,
which is valid for sky models that intrinsically consist of point-sources, but
is an approximation for diffuse sky models. The matvix matrix-based algorithm is
fast and scales well to large numbers of antennas. The code supports both CPU
and GPU implementations as drop-in replacements for each other and also supports
both dense and sparse sky models.

[ascl:2312.029] RRLFE: Metallicity calibrations for RR Lyrae variable stars
Spalding, Eckhart; Wilhelm, Ronald; De Lee, Nathan; Long, Stacy; Beers, Timothy
C.; Placco, Vinicius M.; Kielkopf, John; Lee, Young Sun; Pepper, Joshua;
Carrell, Kenneth

RRLFE generates and applies calibrations for retrieving [Fe/H] from low-res
spectra of RR Lyrae variable stars. The code can generate a metallicity
calibration anew, from real or synthetic spectra; it can also apply a
metallicity calibration to low-resolution (R ~2000) RR Lyrae spectra spanning
3911 to 4950 angstroms.

[ascl:2312.028] SAGE: Stellar Activity Grid for Exoplanets
Chakraborty, Hritam; Lendl, Monika; Akinsanmi, Babatunde; Petit dit de la Roche,
Dominique J. M.; Deline, Adrien

SAGE corrects the time-dependent impact of stellar activity on transmission
spectra. It uses a pixelation approach to model the stellar surface with spots
and faculae, while accounting for limb-darkening and rotational line-broadening.
The code can be used to evaluate stellar contamination for F to M-type hosts,
test various spot sizes and locations, and quantify the impact of
limb-darkening. SAGE can also retrieve the properties and distribution of active
regions on the stellar surface from photometric monitoring, and connect the
photometric variability to the stellar contamination of transmission spectra.

[ascl:2312.027] galclaim: GALaxy Chance of Local Alignment algorIthM
Ducoin, Jean-Grégoire

galclaim identifies association between astrophysical transient sources and host
galaxy. This association is made by estimating the chance alignment between a
given transient sky localization and nearby galaxies. The code can be used with
various catalogs, including Pan-STARRS, HSC, AllWISE and GLADE. galclaim also
pre-checks for nearby bright galaxy using the RC3 catalog
(https://heasarc.gsfc.nasa.gov/w3browse/all/rc3.html). When a nearby galaxy is
found, a warning is raised and the properties of the galaxy are saved in a
dedicated output file. The package can create plots displaying the computed pval
for the found objects for each transient and each catalog; plots are stored in
the result/plots directory.

T F

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