Target Selection and Validation of DESI Emission Line Galaxies

被引：72

作者：

Raichoor, A. ^{[1
]}

Moustakas, J. ^{[2
]}

Newman, Jeffrey A. ^{[3
,4
]}

Karim, T. ^{[5
]}

Ahlen, S. ^{[6
]}

Alam, Shadab ^{[7
]}

Bailey, S. ^{[1
]}

Brooks, D. ^{[8
]}

Dawson, K. ^{[9
]}

de la Macorra, A. ^{[10
]}

de Mattia, A. ^{[11
]}

Dey, A. ^{[12
]}

Dey, Biprateep ^{[3
,4
]}

Dhungana, G. ^{[13
]}

Eftekharzadeh, S. ^{[14
]}

Eisenstein, D. J. ^{[5
]}

Fanning, K. ^{[15
,16
]}

Font-Ribera, A. ^{[17
]}

Garcia-Bellido, J. ^{[18
]}

Gaztanaga, E. ^{[19
,20
]}

Gontcho, S. Gontcho A. ^{[1
]}

Guy, J. ^{[1
]}

Honscheid, K. ^{[15
,16
]}

Ishak, M. ^{[21
]}

Kehoe, R. ^{[13
]}

Kisner, T. ^{[1
]}

Kremin, Anthony ^{[1
]}

Lan, Ting-Wen ^{[22
,23
]}

Landriau, M. ^{[1
]}

Le Guillou, L. ^{[24
]}

Levi, Michael E. ^{[1
]}

Magneville, C. ^{[11
]}

Manera, M. ^{[17
,25
]}

Martini, P. ^{[16
,26
]}

Meisner, Aaron M. ^{[12
]}

Myers, Adam D. ^{[27
]}

Nie, Jundan ^{[28
]}

Palanque-Delabrouille, N. ^{[1
,11
]}

Percival, W. J. ^{[29
,30
,31
]}

Poppett, C. ^{[1
,32
,33
]}

Prada, F. ^{[34
]}

Ross, A. J. ^{[16
]}

Ruhlmann-Kleider, V. ^{[11
]}

Sabiu, C. G. ^{[35
]}

Schlafly, E. F. ^{[36
]}

Schlegel, D. ^{[1
]}

Tarle, Gregory ^{[37
]}

Weaver, B. A. ^{[12
]}

Yeche, Christophe ^{[11
]}

Zhou, Rongpu ^{[1
]}

机构：

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

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

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

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

[5] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

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

[7] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Scotland

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

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

[10] Univ Nacl Autonoma Mexico, Inst Fis, 3700 San Martin Dr, Mexico City 04510, MD, Mexico

[11] Univ Paris Saclay, IRFU, CEA, F-91191 Gif Sur Yvette, France

[12] NSFs NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA

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

[14] NASA Ames Res Ctr, Univ Space Res Assoc, Mountain View, CA USA

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

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

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

[18] Univ Autonoma Madrid, Inst Fis Teor IFT UAM, CSIC, E-28049 Madrid, Spain

[19] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[20] CSIC, Inst Space Sci, ICE, Campus UAB,Carrer Can Magrans S-N, E-08913 Barcelona, Spain

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

[22] Natl Taiwan Univ, Grad Inst Astrophys, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan

[23] Natl Taiwan Univ, Dept Phys, 1,Sect 4,Roosevelt Rd, Taipei 10617, Taiwan

[24] Sorbonne Univ, CNRS, IN2P3, Lab Phys Nucl & Hautes Energies LPNHE, F-75005 Paris, France

[25] Univ Auonoma Barcelona, Dept Fis, Bellaterra, Spain

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

[27] Univ Wyoming, Dept Phys & Astron, 1000 E Univ Dept 3905, Laramie, WY 82071 USA

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

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

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

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

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

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

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

[35] Univ Seoul, Nat Sci Res Inst, 163 Seoulsiripdae Ro, Seoul, South Korea

[36] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

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

来源：

ASTRONOMICAL JOURNAL | 2023年 / 165卷 / 03期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

OSCILLATION SPECTROSCOPIC SURVEY; DIGITAL SKY SURVEY; RESOLUTION; SCIENCE;

D O I：

10.3847/1538-3881/acb213

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dark Energy Spectroscopic Instrument (DESI) will precisely constrain cosmic expansion and the growth of structure by collecting similar to 40 million extragalactic redshifts across similar to 80% of cosmic history and one-third of the sky. The Emission Line galaxy (ELG) sample, which will comprise about one-third of all DESI tracers, will be used to probe the universe over the 0.6 < z < 1.6 range, including the 1.1 < z < 1.6 range, which is expected to provide the tightest constraints. We present the target selection for the DESI Survey Validation (SV) and Main Survey ELG samples, which relies on the imaging of the Legacy Surveys. The Main ELG selection consists of a g-band magnitude cut and a (g - r) versus (r - z) color box, while the SV selection explores extensions of the Main selection boundaries. The Main ELG sample is composed of two disjoint subsamples, which have target densities of about 1940 deg(-2) and 460 deg(-2), respectively. We first characterize their photometric properties and density variations across the footprint. We then analyze the DESI spectroscopic data that have been obtained from 2020 December to 2021 December in the SV and Main Survey. We establish a preliminary criterion for selecting reliable redshifts, based on the [O ii] flux measurement, and assess its performance. Using this criterion, we are able to present the spectroscopic efficiency of the Main ELG selection, along with its redshift distribution. We thus demonstrate that the Main selection 1940 deg(-2) subsample alone should provide 400 deg(-2) and 460 deg(-2) reliable redshifts in the 0.6 < z < 1.1 and the 1.1 < z < 1.6 ranges, respectively.

引用

页数：25

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