Статья

The Art of Measuring Physical Parameters in Galaxies: A Critical Assessment of Spectral Energy Distribution Fitting Techniques

Camilla PacificiSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected]Kartheik G. IyerColumbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USAB. MobasherDepartment of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USAElisabete da CunhaARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), AustraliaViviana AcquavivaCenter for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USAD. BurgarellaAix Marseille Univ, CNRS, CNES, LAM, Marseille, FranceG. Calistro RiveraEuropean Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching, GermanyAdam C. CarnallSUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UKYu-Yen ChangDepartment of Physics, National Chung Hsing University, Taichung, 40227, TaiwanNima ChartabDepartment of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USAKevin C. CookeAAAS S&T Policy Fellow hosted at the National Science Foundation, 1200 New York Avenue, NW, Washington, DC 20005, USACiaran FairhurstAstronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton, BN1 9QH, UKJ. S. KartaltepeSchool of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623, USAJoel LejaDepartment of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USAK. MałekAix Marseille Univ, CNRS, CNES, LAM, Marseille, FranceBrett SalmonSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected]M. TorelliINAF—Osservatorio Astronomico di Roma, via Frascati 33, I-00078 Monteporzio Catone, ItalyAlba Vidal-GarcíaSorbonne UniversitéM. BoquienCentro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, ChileGabriel BrammerCosmic Dawn Center (DAWN), DenmarkM. J. I. BrownSchool of Physics and Astronomy, Monash University, Clayton, VIC 3800, AustraliaP. CapakJacopo ChevallardCNRS, UMR7095, Institut d’Astrophysique de Paris, Sorbonne Université, F-75014, Paris, FranceChiara CircostaDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UKDarren CrotonARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), AustraliaI. DavidzonCosmic Dawn Center (DAWN), DenmarkMark DickinsonCommunity Science and Data Center/NSF’s NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAK. J. DuncanSUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UKS. M. FaberUCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA 95064, USAHenry C. FergusonSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected]A. FontanaINAF—Osservatorio Astronomico di Roma, via Frascati 33, I-00078 Monteporzio Catone, ItalyYicheng GuoDepartment of Physics and Astronomy, University of Missouri, Columbia, MO 65211, USAB. HaeusslerEuropean Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, ChileShoubaneh HemmatiIPAC, California Institute of Technology, 1200 E California Boulevard, Pasadena, CA 91125, USAMarziye JafariyazaniDepartment of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USASusan A. KassinSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected]Rebecca L. LarsonDepartment of Astronomy, The University of Texas at Austin, Austin, TX 78712, United StatesBomee LeeKorea Astronomy and Space Science Institute, Daedeokdae-ro 776, Yuseong-gu, Daejeon 34055, Republic of KoreaKameswara Bharadwaj ManthaMinnesota Institute for Astrophysics, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455, USAFrancesca MarchiINAF—Osservatorio Astronomico di Roma, Via di Frascati 33, I-00078, Monte Porzio Catone, ItalyHooshang NayyeriDepartment of Physics and Astronomy, University of California, Irvine, Irvine, CA 92697, USAJeffrey A. NewmanDepartment of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USAViraj PandyaDepartment of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USAJ. PforrScientific Support Office, Directorate of Science and Robotic Exploration, European Space Research and Technology Centre (ESA/ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, The NetherlandsNaveen A. ReddyDepartment of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USARyan L. SandersDepartment of Physics, University of California, Davis, One Shields Boulevard, Davis, CA 95616, USAEkta A. ShahDepartment of Physics, University of California, Davis, One Shields Boulevard, Davis, CA 95616, USAAbtin ShahidiDepartment of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, CA 92521, USAMatthew L. StevansDepartment of Astronomy, University of Texas at Austin, Austin, TX 78712, USADian P. TrianiARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), AustraliaK. D. TylerSchool of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623, USABrittany N. VanderhoofSchool of Physics and Astronomy, Rochester Institute of Technology, Rochester, NY 14623, USAAlexander de la VegaDepartment of Physics and Astronomy, Johns Hopkins University, Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USAWeichen WangCenter for Astrophysics Harvard & Smithshonian, 60 Garden Street, Cambridge, MA 02138, USAMadalyn E. WestonDepartment of Physics and Astronomy, University of Missouri-Kansas City, Kansas City, MO 64110, USA

2023en

ABI

Аннотация

Abstract The study of galaxy evolution hinges on our ability to interpret multiwavelength galaxy observations in terms of their physical properties. To do this, we rely on spectral energy distribution (SED) models, which allow us to infer physical parameters from spectrophotometric data. In recent years, thanks to wide and deep multiwave band galaxy surveys, the volume of high-quality data have significantly increased. Alongside the increased data, algorithms performing SED fitting have improved, including better modeling prescriptions, newer templates, and more extensive sampling in wavelength space. We present a comprehensive analysis of different SED-fitting codes including their methods and output with the aim of measuring the uncertainties caused by the modeling assumptions. We apply 14 of the most commonly used SED-fitting codes on samples from the CANDELS photometric catalogs at z ∼ 1 and z ∼ 3. We find agreement on the stellar mass, while we observe some discrepancies in the star formation rate (SFR) and dust-attenuation results. To explore the differences and biases among the codes, we explore the impact of the various modeling assumptions as they are set in the codes (e.g., star formation histories, nebular, dust and active galactic nucleus models) on the derived stellar masses, SFRs, and A V values. We then assess the difference among the codes on the SFR–stellar mass relation and we measure the contribution to the uncertainties by the modeling choices (i.e., the modeling uncertainties) in stellar mass (∼0.1 dex), SFR (∼0.3 dex), and dust attenuation (∼0.3 mag). Finally, we present some resources summarizing best practices in SED fitting.

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Идентификаторы

DOI: 10.3847/1538-4357/acacff

Цитирования и источники

Цитирований: 2Использованных источников: 0

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