Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument

被引：65

作者：

Adame, A. G. ^{[1
]}

Aguilar, J. ^{[2
]}

Ahlen, S. ^{[3
]}

Alam, S. ^{[4
]}

Aldering, G. ^{[2
]}

Alexander, D. M. ^{[5
,6
]}

Alfarsy, R. ^{[7
]}

Allende Prieto, C. ^{[8
,9
]}

Alvarez, M. ^{[2
]}

Alves, O. ^{[10
]}

Anand, A. ^{[2
]}

Andrade-Oliveira, F. ^{[10
]}

Armengaud, E. ^{[11
]}

Asorey, J. ^{[12
]}

Avila, S. ^{[13
]}

Aviles, A. ^{[14
,15
]}

Bailey, S. ^{[2
]}

Balaguera-Antolinez, A. ^{[8
,9
]}

Ballester, O. ^{[13
]}

Baltay, C. ^{[16
]}

Bault, A. ^{[17
]}

Bautista, J. ^{[18
]}

Behera, J. ^{[19
]}

Beltran, S. F. ^{[20
]}

BenZvi, S. ^{[21
]}

Beraldo E Silva, L. ^{[10
,22
]}

Bermejo-Climent, J. R. ^{[21
]}

Berti, A. ^{[23
]}

Besuner, R. ^{[24
,25
]}

Beutler, F. ^{[26
]}

Bianchi, D. ^{[27
]}

Blake, C. ^{[28
]}

Blum, R. ^{[29
]}

Bolton, A. S. ^{[29
]}

Brieden, S. ^{[26
]}

Brodzeller, A. ^{[23
]}

Brooks, D. ^{[30
]}

Brown, Z. ^{[21
]}

Buckley-Geer, E. ^{[31
,32
]}

Burtin, E. ^{[11
]}

Cabayol-Garcia, L. ^{[13
]}

Cai, Z. ^{[33
,34
,35
]}

Canning, R. ^{[7
]}

Cardiel-Sas, L. ^{[13
]}

Carnero Rosell, A. ^{[8
,9
]}

Castander, F. J. ^{[36
,37
]}

Cervantes-Cota, J. L. ^{[15
]}

Chabanier, S. ^{[2
]}

Chaussidon, E. ^{[11
]}

Chaves-Montero, J. ^{[13
]}

机构：

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

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

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

[4] Tata Inst Fundamental Res, Homi Bhabha Rd, Mumbai 400005, Maharashtra, India

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

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

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

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

[9] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 Tenerife, Spain

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

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

[12] CIEMAT, Ave Complutense 40, E-28040 Madrid, Spain

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

[14] Consejo Nacl Ciencia & Technol, Av Insurgentes Sur 1582, Mexico City 03940, DF, Mexico

[15] Inst Nacl Invest Nucl, Dept Fis, Carreterra Mexico Toluca S-N, Ocoyoacac 52750, Edo De Mexico, Mexico

[16] Yale Univ, Phys Dept, POB 208120, New Haven, CT 06511 USA

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

[18] Aix Marseille Univ, CPPM, CNRS IN2P3, Marseille, France

[19] Kansas State Univ, Dept Phys, 116 Cardwell Hall, Manhattan, KS 66506 USA

[20] Univ Guanajuato DCI, Dept Fis, Guanajuato 37150, Mexico

[21] Univ Rochester, Dept Phys & Astron, 206 Bausch & Lomb Hall,POB 270171, Rochester, NY 14627 USA

[22] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

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

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

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

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

[27] Univ Milan, Dipartimento Fis Aldo Pontremoli, Via Celoria 16, I-20133 Milan, Italy

[28] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia

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

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

[31] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA

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

[33] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95065 USA

[34] Tsinghua Univ, Dept Astron, 30 Shuangqing Rd, Beijing 100190, Peoples R China

[35] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA

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

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

[38] Inst Adv Study, 1 Einstein Dr, Princeton, NJ 08540 USA

[39] Stanford Univ, Phys Dept, Stanford, CA 93405 USA

[40] SLAC Natl Accelerator Lab, Menlo Pk, CA 94305 USA

[41] Natl Tsing Hua Univ, Inst Astron & Dept Phys, 101 Kuang Fu Rd,Sec 2, Hsinchu 30013, Taiwan

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

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

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

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

[46] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[47] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico

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

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

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

来源：

ASTRONOMICAL JOURNAL | 2024年 / 167卷 / 02期

基金：

美国国家科学基金会; 英国科学技术设施理事会;

关键词：

BARYON ACOUSTIC-OSCILLATIONS; GALAXY REDSHIFT SURVEY; DIGITAL SKY SURVEY; ANISOTROPIC POWER SPECTRUM; SCALE STRUCTURE CATALOGS; BODY SIMULATION PROJECT; HUBBLE-SPACE-TELESCOPE; LUMINOUS RED GALAXIES; STAR-FORMATION RATE; TARGET-SELECTION;

D O I：

10.3847/1538-3881/ad0b08

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg(2) over 5 yr to constrain the cosmic expansion history through precise measurements of baryon acoustic oscillations (BAO). The scientific program for DESI was evaluated during a 5 month survey validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar Milky Way Survey (MWS), Bright Galaxy Survey (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the 5 yr program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a One-Percent Survey conducted at the conclusion of SV covering 140 deg(2) using the final target selection algorithms with exposures of a depth typical of the main survey. The SV indicates that DESI will be able to complete the full 14,000 deg(2) program with spectroscopically confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval z < 1.1, 0.39% over the redshift interval 1.1 < z < 1.9, and 0.46% over the redshift interval 1.9 < z < 3.5.

引用

页数：33

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