Target Selection and Validation of DESI Quasars

被引：81

作者：

Chaussidon, Edmond ^{[1
]}

Yeche, Christophe ^{[1
]}

Palanque-Delabrouille, Nathalie ^{[1
,2
]}

Alexander, David M. ^{[3
,4
]}

Yang, Jinyi ^{[5
]}

Ahlen, Steven ^{[6
]}

Bailey, Stephen ^{[2
]}

Brooks, David ^{[7
]}

Cai, Zheng ^{[8
]}

Chabanier, Solene ^{[2
]}

Davis, Tamara M. ^{[9
]}

Dawson, Kyle ^{[10
]}

de la Macorra, Axel ^{[11
]}

Dey, Arjun ^{[12
]}

Dey, Biprateep ^{[13
,14
]}

Eftekharzadeh, Sarah ^{[15
]}

Eisenstein, Daniel J. ^{[16
]}

Fanning, Kevin ^{[17
,18
]}

Font-Ribera, Andreu ^{[19
]}

Gaztanaga, Enrique ^{[20
,21
]}

Gontcho, Satya Gontcho A. ^{[2
]}

Gonzalez-Morales, Alma X. ^{[22
,23
]}

Guy, Julien ^{[2
]}

Herrera-Alcantar, Hiram K. ^{[23
]}

Honscheid, Klaus ^{[17
,24
]}

Ishak, Mustapha ^{[25
]}

Jiang, Linhua ^{[26
]}

Juneau, Stephanie ^{[12
]}

Kehoe, Robert ^{[27
]}

Kisner, Theodore ^{[2
]}

Kovacs, Andras ^{[28
,29
]}

Kremin, Anthony ^{[2
]}

Lan, Ting-Wen ^{[30
,31
]}

Landriau, Martin ^{[2
]}

Le Guillou, Laurent ^{[32
]}

Levi, Michael E. ^{[2
]}

Magneville, Christophe ^{[1
]}

Martini, Paul ^{[17
,18
]}

Meisner, Aaron M. ^{[12
]}

Moustakas, John ^{[33
]}

Munoz-Gutierrez, Andrea ^{[11
]}

Myers, Adam D. ^{[34
]}

Newman, Jeffrey A. ^{[13
,14
]}

Nie, Jundan ^{[35
]}

Percival, Will J. ^{[36
,37
,38
]}

Poppett, Claire ^{[2
,39
,40
]}

Prada, Francisco ^{[41
]}

Raichoor, Anand ^{[2
]}

Ravoux, Corentin ^{[1
]}

Ross, Ashley J. ^{[17
,18
]}

机构：

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

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

[3] Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England

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

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

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

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

[8] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China

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

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

[11] Univ Nacl Autonoma Mexico, Inst Fis, Ciudad De Mexico 04510, MI, Mexico

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

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

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

[15] Univ Space Res Assoc, NASA Ames Res Ctr, Moffett Field, CA USA

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

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

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

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

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

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

[22] Consejo Nacl Ciencia & Technol, Ave Insurgentes Sur 1582, Mexico City 03940, DF, Mexico

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

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

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

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

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

[28] Univ La Laguna ULL, Dept Astrofis, E-38206 Tenerife, Spain

[29] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Santa Cruz De Tenerife, San Cristobal D, Spain

[30] Natl Taiwan Univ, Grad Inst Astrophys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan

[31] Natl Taiwan Univ, Dept Phys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan

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

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 944卷 / 01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; BARYON ACOUSTIC-OSCILLATIONS; LY-ALPHA FOREST; REDSHIFT; 0.8; EMISSION; CATALOG; SAMPLE; WISE;

D O I：

10.3847/1538-4357/acb3c2

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dark Energy Spectroscopic Instrument (DESI) survey will measure large-scale structures using quasars as direct tracers of dark matter in the redshift range 0.9 < z < 2.1 and using Ly alpha forests in quasar spectra at z > 2.1. We present several methods to select candidate quasars for DESI, using input photometric imaging in three optical bands (g, r, z) from the DESI Legacy Imaging Surveys and two infrared bands (W1, W2) from the Wide-field Infrared Survey Explorer. These methods were extensively tested during the Survey Validation of DESI. In this paper, we report on the results obtained with the different methods and present the selection we optimized for the DESI main survey. The final quasar target selection is based on a random forest algorithm and selects quasars in the magnitude range of 16.5 < r < 23. Visual selection of ultra-deep observations indicates that the main selection consists of 71% quasars, 16% galaxies, 6% stars, and 7% inconclusive spectra. Using the spectra based on this selection, we build an automated quasar catalog that achieves a fraction of true QSOs higher than 99% for a nominal effective exposure time of similar to 1000 s. With a 310 deg(-2) target density, the main selection allows DESI to select more than 200 deg(-2) quasars (including 60 deg(-2) quasars with z > 2.1), exceeding the project requirements by 20%. The redshift distribution of the selected quasars is in excellent agreement with quasar luminosity function predictions.

引用

页数：17

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