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| FSPS | |
|---|---|
| Name | FSPS |
| Developer | Conroy Laboratory |
| Released | 2009 |
| Latest release | 3.2.2 |
| Programming language | Fortran, Python |
| Operating system | Unix-like, Windows |
| Genre | Stellar population synthesis |
| License | BSD-style |
FSPS is a computational stellar population synthesis code designed to model the integrated spectral energy distributions, photometry, and stellar evolution outputs of composite stellar systems. It provides flexible prescriptions for stellar evolution tracks, spectral libraries, and dust attenuation to support interpretation of observations from ground- and space-based facilities. FSPS is used extensively in studies that connect stellar physics to extragalactic surveys, cosmological simulations, and population analyses.
FSPS produces synthetic spectra, colors, mass-to-light ratios, and stellar remnants for user-specified star formation histories and metallicities. It integrates inputs from stellar evolution models such as Padova, MIST, and BaSTI tracks and pairs them with empirical libraries including MILES, STELIB, and PHOENIX to compute observables across ultraviolet to infrared bands. The code supports nebular emission modeling in the fashion of CLOUDY-based calibrations and incorporates dust attenuation recipes inspired by Calzetti, Cardelli–Clayton–Mathis, and Charlot and Fall formalisms. FSPS is commonly coupled to population inference tools used in analyses at facilities such as Sloan Digital Sky Survey, Hubble Space Telescope, and James Webb Space Telescope.
FSPS traces origins to community efforts to provide a modular framework that could supplant rigid synthesis packages used in surveys like 2dF Galaxy Redshift Survey and DEEP2 Redshift Survey. Early development was influenced by methodologies from authors linked to Padova isochrone work and spectral calibrations used in SAURON and SDSS projects. Key enhancements occurred as teams incorporated updated isochrones from Dartmouth College groups, spectral libraries maintained at institutions such as Institute of Astronomy, Cambridge and Max Planck Institute for Astrophysics, and nebular computations validated against SINGS and CALIFA observations. Over successive releases FSPS adopted modern interfaces via Python wrappers and binding schemes resembling those used in Astropy affiliated packages.
FSPS is organized as a combination of Fortran cores for heavy numerical integration and Python front-ends for user interaction, paralleling design choices in projects like GALAXEV and PEGASE. The architecture separates stellar evolution modules (isochrone handlers), spectral synthesis modules (library selectors), dust and nebular modules, and output formatting. It enables swapping between isochrone sets such as PARSEC and MIST without altering downstream pipelines, and it interoperates with fitting frameworks like Prospector (software), Bagpipes, and CIGALE. Parallelization strategies follow paradigms used in MPI-enabled astrophysical codes and leverage optimization techniques from numerical libraries maintained by groups at Lawrence Berkeley National Laboratory.
FSPS offers extensive parametrization of initial mass functions, including implementations of Salpeter, Kroupa, and Chabrier forms, and provides options for binary fraction treatments inspired by work from Binary Population and Spectral Synthesis researchers. It computes time-dependent mass loss, remnant mass functions, and yields that tie into chemical evolution models used by Illustris and EAGLE simulation teams. Spectral synthesis outputs include high-resolution spectra compatible with instruments such as Keck Observatory spectrographs and photometric predictions across filters from SDSS, Pan-STARRS, WISE, and Spitzer Space Telescope. The code supports flexible star formation histories (exponential, bursty, delayed) commonly used in analyses from COSMOS and CANDELS collaborations.
FSPS is used to derive stellar masses, ages, metallicities, and star formation rates for galaxy samples in projects like GAMA and VIPERS. It underpins spectral fitting in studies that compare resolved stellar populations in systems observed by Hubble Space Telescope and integral field surveys such as MaNGA. Cosmological applications include generating synthetic galaxy catalogs for lightcone construction in surveys planned by Vera C. Rubin Observatory and Euclid. FSPS outputs feed chemical evolution and feedback prescriptions in semi-analytic models developed by teams associated with Millennium Simulation and hydrodynamical model comparisons to ALMA observations.
Performance profiling of FSPS emphasizes its computational efficiency for grid generation of spectral libraries and Monte Carlo sampling for parameter inference. Benchmarks reported by groups using FSPS compare runtime and memory usage against codes like GALAXEV and PEGASE, showing competitive scaling on multicore nodes typical of clusters at National Energy Research Scientific Computing Center and university HPC centers such as Princeton University and University of California, Berkeley. Accuracy benchmarks concentrate on reproducing observed color-magnitude diagrams from clusters studied at Keck Observatory and spectral indices calibrated in Lick Observatory analyses.
FSPS is distributed under a permissive BSD-style license and maintained by a community of contributors from institutions including University of California, Santa Cruz, Harvard University, and University of Arizona. Development discussions occur in venues frequented by developers of Astropy, yt (project), and other open-source astronomy software projects. The user community publishes validation studies in journals and presents at conferences such as American Astronomical Society meetings and IAU General Assembly symposia.
Category:Astrophysics software