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

被引：1

作者：

Siudek, M. ^{[1
,2
]}

Pucha, R. ^{[3
,4
]}

Mezcua, M. ^{[1
,5
]}

Juneau, S. ^{[6
]}

Aguilar, J. ^{[7
]}

Ahlen, S. ^{[8
]}

Brooks, D. ^{[9
]}

Circosta, C. ^{[9
]}

Claybaugh, T. ^{[7
]}

Cole, S. ^{[10
]}

Dawson, K. ^{[3
]}

de la Macorra, A. ^{[11
]}

Dey, A. ^{[6
]}

Dey, B. ^{[12
,13
]}

Doel, P. ^{[9
]}

Font-Ribera, A. ^{[9
,14
]}

Forero-Romero, J. E. ^{[15
,16
]}

Gaztanaga, E. ^{[1
,5
,17
]}

Gontcho, S. Gontcho A. ^{[7
]}

Gutierrez, G. ^{[18
]}

Honscheid, K. ^{[19
,20
,21
]}

Howlett, C. ^{[22
]}

Ishak, M. ^{[23
]}

Kehoe, R. ^{[24
]}

Kirkby, D. ^{[25
]}

Kisner, T. ^{[7
]}

Kremin, A. ^{[7
]}

Lambert, A. ^{[7
]}

Landriau, M. ^{[7
]}

Le Guillou, L. ^{[26
]}

Manera, M. ^{[14
,27
]}

Martini, P. ^{[19
,21
,28
]}

Meisner, A. ^{[6
]}

Miquel, R. ^{[14
,29
]}

Moustakas, J. ^{[30
]}

Newman, J. A. ^{[12
,13
]}

Niz, G. ^{[31
,32
]}

Pan, Z. ^{[33
]}

Percival, W. J. ^{[34
,35
,36
]}

Poppett, C. ^{[7
,37
,38
]}

Prada, F. ^{[39
]}

Rossi, G. ^{[40
]}

Saintonge, A. ^{[9
]}

Sanchez, E. ^{[41
]}

Schlegel, D. ^{[7
]}

Scholte, D. ^{[9
]}

Schubnell, M. ^{[42
,43
]}

Seo, H. ^{[44
]}

Speranza, F. ^{[9
]}

Sprayberry, D. ^{[6
]}

机构：

[1] CSIC, Inst Space Sci, ICE, Campus UAB,Carrer Can Magrans s-, Catalonia 08193, Barcelona, Spain

[2] Inst Astrofis Canarias, Av Via Lactea s-n, E-38200 San Cristobal la Laguna, Spain

[3] Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA

[4] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[5] Inst Estudis Espacials Catalunya IEEC, Edifici RDIT,Campus UPC, Castelldefels 08860, Barcelona, Spain

[6] NSF NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA

[7] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

[8] Boston Univ, Phys Dept, 590 Commonwealth Ave, Boston, MA 02215 USA

[9] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[10] Univ Durham, Inst Computat Cosmol, Dept Phys, South Rd, Durham DH1 3LE, England

[11] Univ Nacl Autonoma Mexico, Inst Ingn, Mexico City 04510, Mexico

[12] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA

[13] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, 3941 OHara St, Pittsburgh, PA 15260 USA

[14] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, Barcelona 08193, Spain

[15] Univ Los Andes, Dept Fis, Cra 1 18A-10 Edificio Ip, Bogota 111711, Colombia

[16] Univ Los Andes, Observ Astron, Cra 1 18A-10,Edificio H, Bogota 111711, Colombia

[17] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, England

[18] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[19] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA

[20] Ohio State Univ, Dept Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA

[21] Ohio State Univ, Columbus, OH 43210 USA

[22] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[23] Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA

[24] Southern Methodist Univ, Dept Phys, 3215 Daniel Ave, Dallas, TX 75275 USA

[25] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

[26] Sorbonne Univ, Lab Phys Nucl & Hautes Energies LPNHE, CNRS, IN2P3, Paris, France

[27] Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Barcelona, Spain

[28] Ohio State Univ, Dept Astron, 4055 McPherson Lab,140 W 18th Ave, Columbus, OH 43210 USA

[29] Inst Catalana Recerca & Estudis Avancats, Passeig Lluis Co 23, Barcelona 08010, Spain

[30] Siena Coll, Dept Phys & Astron, 515 Loudon Rd, Loudonville, NY 12211 USA

[31] Univ Guanajuato DCI, Dept Fis, Leon 37150, Guanajuato, Mexico

[32] Inst Avanzado Cosmol AC, San Marcos 11 Atenas 202 Magdalena Contreras, Mexico City 10720, Mexico

[33] Peking Univ, Kavli Inst Astron & Astrophys, PKU, 5 Yiheyuan Rd, Beijing 100871, Peoples R China

[34] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada

[35] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada

[36] Univ Waterloo, Waterloo Ctr Astrophys, 200 Univ Ave, Waterloo, ON N2L 3G1, Canada

[37] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA

[38] Univ Calif Berkeley, 110 Sproul Hall 5800, Berkeley, CA 94720 USA

[39] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, Granada 18008, Spain

[40] Sejong Univ, Dept Phys & Astron, Seoul 143747, South Korea

[41] CIEMAT, Ave Complutense 40, Madrid 28040, Spain

[42] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[43] Univ Michigan, Ann Arbor, MI 48109 USA

[44] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA

[45] Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

基金：

美国国家科学基金会; 中国国家自然科学基金; 英国科学技术设施理事会; 美国国家航空航天局;

关键词：

catalogs; galaxies: active; galaxies: evolution; galaxies: general; galaxies: nuclei; galaxies: Seyfert; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; STELLAR MASS FUNCTION; STAR-FORMATION HISTORIES; SIMILAR-TO; LYMAN BREAK GALAXIES; DIGITAL SKY SURVEY; TARGET-SELECTION; LEGACY SURVEY; PHOTOMETRIC REDSHIFTS;

D O I：

10.1051/0004-6361/202451761

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：25

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