Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

被引：181

作者：

Abareshi, B. ^{[1
]}

Aguilar, J. ^{[2
]}

Ahlen, S. ^{[3
]}

Alam, Shadab ^{[4
]}

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

Alfarsy, R. ^{[7
]}

Allen, L. ^{[1
]}

Allende Prieto, C. ^{[8
]}

Alves, O. ^{[9
]}

Ameel, J. ^{[9
,10
]}

Armengaud, E. ^{[11
]}

Asorey, J. ^{[12
]}

Aviles, Alejandro ^{[13
,14
]}

Bailey, S. ^{[2
]}

Balaguera-Antolinez, A. ^{[8
,15
]}

Ballester, O. ^{[16
]}

Baltay, C. ^{[17
]}

Bault, A. ^{[18
]}

Beltran, S. F. ^{[19
]}

Benavides, B. ^{[20
]}

BenZvi, S. ^{[21
]}

Berti, A. ^{[22
]}

Besuner, R. ^{[23
,24
]}

Beutler, Florian ^{[4
]}

Bianchi, D. ^{[25
,26
]}

Blake, C. ^{[27
]}

Blanc, P. ^{[28
]}

Blum, R. ^{[1
]}

Bolton, A. ^{[1
]}

Bose, S. ^{[29
]}

Bramall, D. ^{[6
]}

Brieden, S. ^{[25
,30
]}

Brodzeller, A. ^{[22
]}

Brooks, D. ^{[31
]}

Brownewell, C. ^{[1
]}

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

Cahn, R. N. ^{[2
]}

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

Canning, R. ^{[7
]}

Capasso, R. ^{[35
,36
]}

Carnero Rosell, A. ^{[8
,15
]}

Carton, P. ^{[11
]}

Casas, R. ^{[37
]}

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

Cervantes-Cota, J. L. ^{[14
]}

Chabanier, S. ^{[2
]}

Chaussidon, E. ^{[11
]}

Chuang, C. ^{[22
,38
,39
]}

Circosta, C. ^{[31
]}

Cole, S. ^{[6
]}

机构：

[1] NSFs Natl Opt Infrared Astron Res Lab, 950 N Cherry Ave, Tucson, AZ 85719 USA

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

[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] Inst Astrofis Canarias, C Via Lactea S-N, E-38205 San Cristobal La Laguna, Santa Cruz De T, Spain

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

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

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

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

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

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

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

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

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

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

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

[20] Univ Nacl Autonoma Mexico, Inst Fis, Cd De Mexico 04510, Mexico

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

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

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

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

[25] Univ Barcelona IEEC UB, ICCUB, Inst Ciencias Cosmoc, Marti i Franques 1, E-08028 Barcelona, Spain

[26] Univ Milan, Milan, Italy

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

[28] Aix Marseille Univ, OHP, CNRS, F-04870 St Michel lObservatoire, France

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

[30] Univ Barcelona, Dept Fis Quant & Astrofis, Marti i Franques 1, E-08028 Barcelona, Spain

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

[32] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 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] Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81677 Munich, Germany

[36] Ludwig Maximilians Univ Munchen, Fac Phys, Univ Observ, Scheinerstr 1, E-08913 Barcelona, Spain

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

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

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

[40] Natl Tsing Hua Univ, Inst Astron, Taipei, Taiwan

[41] Lab Interinst E Astron, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

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

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

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

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

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

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

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

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

[50] Shanghai Jiao Tong Univ, Sch Phys & Astron, Dept Astron, Shanghai 200240, Peoples R China

来源：

ASTRONOMICAL JOURNAL | 2022年 / 164卷 / 05期

基金：

美国国家科学基金会; 美国安德鲁·梅隆基金会;

关键词：

POWER-SPECTRUM; GALAXY SAMPLE; REDSHIFT; 0.6; GROWTH-RATE; SPACE; DISTORTIONS; PEAK;

D O I：

10.3847/1538-3881/ac882b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Dark Energy Spectroscopic Instrument (DESI) embarked on an ambitious 5 yr survey in 2021 May to explore the nature of dark energy with spectroscopic measurements of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the baryon acoustic oscillation method to measure distances from the nearby universe to beyond redshift z > 3.5, and employ redshift space distortions to measure the growth of structure and probe potential modifications to general relativity. We describe the significant instrumentation we developed to conduct the DESI survey. This includes: a wide-field, 3.degrees 2 diameter prime-focus corrector; a focal plane system with 5020 fiber positioners on the 0.812 m diameter, aspheric focal surface; 10 continuous, high-efficiency fiber cable bundles that connect the focal plane to the spectrographs; and 10 identical spectrographs. Each spectrograph employs a pair of dichroics to split the light into three channels that together record the light from 360-980 nm with a spectral resolution that ranges from 2000-5000. We describe the science requirements, their connection to the technical requirements, the management of the project, and interfaces between subsystems. DESI was installed at the 4 m Mayall Telescope at Kitt Peak National Observatory and has achieved all of its performance goals. Some performance highlights include an rms positioner accuracy of better than 0.'' 1 and a median signal-to-noise ratio of 7 of the [O ii] doublet at 8 x 10(-17) erg s(-1) cm(-2) in 1000 s for galaxies at z = 1.4-1.6. We conclude with additional highlights from the on-sky validation and commissioning, key successes, and lessons learned.

引用

页数：62

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