Astrophysics Source Code Library

Making codes discoverable since 1999

Searching for codes credited to 'Charlot, Stéphane'

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[ascl:1104.005] GALAXEV: Evolutionary Stellar Population Synthesis Models

GALAXEV is a library of evolutionary stellar population synthesis models computed using the new isochrone synthesis code of Bruzual & Charlot (2003). This code allows one to computes the spectral evolution of stellar populations in wide ranges of ages and metallicities at a resolution of 3 Å across the whole wavelength range from 3200 Å to 9500 Å, and at lower resolution outside this range.

[ascl:1106.010] MAGPHYS: Multi-wavelength Analysis of Galaxy Physical Properties

MAGPHYS is a self-contained, user-friendly model package to interpret observed spectral energy distributions of galaxies in terms of galaxy-wide physical parameters pertaining to the stars and the interstellar medium. MAGPHYS is optimized to derive statistical constraints of fundamental parameters related to star formation activity and dust content (e.g. star formation rate, stellar mass, dust attenuation, dust temperatures) of large samples of galaxies using a wide range of multi-wavelength observations. A Bayesian approach is used to interpret the SEDs all the way from the ultraviolet/optical to the far-infrared.

[ascl:2312.010] FORECAST: Realistic astronomical image and galaxy survey generator

FORECAST generates realistic astronomical images and galaxy surveys by forward modeling the output snapshot of any hydrodynamical cosmological simulation. It exploits the snapshot by constructing a lightcone centered on the observer's position; the code computes the observed fluxes of each simulated stellar element, modeled as a Single Stellar Population (SSP), in any chosen set of pass-band filters, including k-correction, IGM absorption, and dust attenuation. These fluxes are then used to create an image on a grid of pixels, to which observational features such as background noise and PSF blurring can be added. FORECAST provides customizable options for filters, size of the field of view, and survey parameters, thus allowing the synthetic images to be tailored for specific research requirements.