Value-added catalog of physical properties for more than 1.3 million galaxies from the DESI survey

¹ Institute of Space Sciences, ICE-CSIC, Campus UAB, Carrer de Can Magrans s/n, 08913 Bellaterra, Barcelona, Spain
² Instituto Astrofisica de Canarias, Av. Via Lactea s/n, 38205 La Laguna, Spain
³ Department of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA
⁴ Steward Observatory, University of Arizona, 933 N, Cherry Ave, Tucson, AZ 85721, USA
⁵ Institut d’Estudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC, 08860 Castelldefels (Barcelona), Spain
⁶ NSF NOIRLab, 950 N. Cherry Ave., Tucson, AZ 85719, USA
⁷ Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA
⁸ Physics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USA
⁹ Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
¹⁰ Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
¹¹ Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
¹² Instituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510 Mexico
¹³ Department of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USA
¹⁴ Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
¹⁵ Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra Barcelona, Spain
¹⁶ Departamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, Colombia
¹⁷ Observatorio Astronómico, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio H, CP 111711 Bogotá, Colombia
¹⁸ Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK
¹⁹ Fermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USA
²⁰ Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA
²¹ Department of Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA
²² The Ohio State University, Columbus, OH 43210, USA
²³ School of Mathematics and Physics, University of Queensland, Queensland 4072, Australia
²⁴ Department of Physics, The University of Texas at Dallas, Richardson, TX 75080, USA
²⁵ Department of Physics, Southern Methodist University, 3215 Daniel Avenue, Dallas, TX 75275, USA
²⁶ Department of Physics and Astronomy, University of California, Irvine 92697, USA
²⁷ Sorbonne Université, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), 75005 Paris, France
²⁸ Departament de Física, Serra Húnter, Universitat Autònoma de Barcelona, 08193 Bellaterra (Barcelona), Spain
²⁹ Department of Astronomy, The Ohio State University, 4055 McPherson Laboratory, 140 W 18th Avenue, Columbus, OH 43210, USA
³⁰ Institució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, 08010 Barcelona, Spain
³¹ Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA
³² Departamento de Física, Universidad de Guanajuato – DCI, C.P. 37150, Leon, Guanajuato, Mexico
³³ Instituto Avanzado de Cosmología A. C., San Marcos 11 – Atenas 202. Magdalena Contreras, 10720. Ciudad de México, Mexico
³⁴ Kavli Institute for Astronomy and Astrophysics at Peking University, PKU, 5 Yiheyuan Road, Haidian District, Beijing 100871, P.R. China
³⁵ Department of Physics and Astronomy, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, Canada
³⁶ Perimeter Institute for Theoretical Physics, 31 Caroline St. North, Waterloo, ON N2L 2Y5, Canada
³⁷ Waterloo Centre for Astrophysics, University of Waterloo, 200 University Ave W, Waterloo, ON N2L 3G1, Canada
³⁸ Space Sciences Laboratory, University of California, Berkeley, 7 Gauss Way, Berkeley, CA 94720, USA
³⁹ University of California, Berkeley, 110 Sproul Hall #5800 Berkeley, CA 94720, USA
⁴⁰ Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, s/n, 18008 Granada, Spain
⁴¹ Department of Physics and Astronomy, Sejong University, Seoul, 143-747, Korea
⁴² CIEMAT, Avenida Complutense 40, 28040 Madrid, Spain
⁴³ Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
⁴⁴ University of Michigan, Ann Arbor, MI 48109, USA
⁴⁵ Department of Physics & Astronomy, Ohio University, Athens, OH 45701 USA
⁴⁶ National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Rd., Chaoyang District, Beijing 100012, P.R. China

^★ Corresponding author; msiudek@iac.es

Received: 1 August 2024
Accepted: 1 October 2024

Abstract

Aims. We present an extensive catalog of the physical properties of more than a million galaxies investigated with the Dark Energy Spectroscopic Instrument (DESI), one of the largest spectroscopic surveys to date. Spanning a full range of target types, including emission-line galaxies, luminous red galaxies, and quasars, our survey encompasses an unprecedented range of spectroscopic redshifts, all the way from 0 to 6.

Methods. The physical properties, such as stellar masses and star formation rates, were derived via the CIGALE spectral energy distribution (SED) fitting code accounting for the contribution coming from active galactic nuclei (AGNs). Based on the modeling of the optical-mid-infrared (grz supplemented with WISE photometry) SEDs, we studied the galaxy properties with respect to their location on the main sequence.

Results. We have revised the dependence of stellar mass estimates on model choices and on the availability of WISE photometry. Indeed, the WISE data are required to minimize the misclassification of star-forming galaxies as AGNs. The lack of WISE bands in SED fits leads to elevated AGN fractions for 68% of star-forming galaxies identified using emission line diagnostic diagrams, but this does not significantly affect their stellar mass or star formation estimates.