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Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument

Journal Article · · Astron.J.
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  1. Madrid, IFT
  2. LBL, Berkeley
  3. Boston U.
  4. TIFR, Mumbai, DHEP
  5. Durham U.; Durham U., ICC
  6. Portsmouth U., ICG
  7. Laguna U., Tenerife; IAC, La Laguna
  8. Michigan U.
  9. IRFU, Saclay
  10. Madrid, CIEMAT
  11. Barcelona, IFAE
  12. Conacyt, Mexico; CINVESTAV, IPN
  13. Yale U.
  14. UC, Irvine
  15. Marseille, CPPM
  16. Kansas State U.
  17. Guanajuato U.
  18. Rochester U.
  19. U. Michigan, Dept. Astron.; Michigan U.
  20. Utah U.
  21. UC, Berkeley, Space Sci. Dept.; BCCP, Berkeley
  22. Edinburgh U., Inst. Astron.
  23. Milan U.
  24. Swinburne U., Ctr. Astrophys. Supercomput.
  25. Natl. Solar Observ., Tucson
  26. University Coll. London
  27. Chicago U., Astron. Astrophys. Ctr.; Fermilab
  28. UC, Santa Cruz (main); UC, Santa Cruz, Inst. Part. Phys.; Tsinghua U., Beijing; Lick Observ.
  29. Barcelona, IEEC
  30. CINVESTAV, IPN
  31. Princeton, Inst. Advanced Study
  32. Utah U.; Stanford U., Phys. Dept.; SLAC
  33. Durham U., ICC
  34. Taiwan, Natl. Tsing Hua U.
  35. Chicago U., KICP; Ohio State U.
  36. Queensland U.
  37. Cambridge U., Inst. of Astron.; LBL, Berkeley
  38. UNAM, Mexico
  39. Pittsburgh U.
  40. Southern Methodist U.
  41. Lick Observ.
  42. Shanghai Jiaotong U.
  43. UC, Berkeley
  44. Universities Space Research Assoc.
  45. Harvard-Smithsonian Ctr. Astrophys.
  46. Ohio State U.
  47. Arizona U., Astron. Dept. - Steward Observ.
  48. Newcastle upon Tyne U.
  49. LBL, Berkeley; BCCP, Berkeley
  50. Granada U., Theor. Phys. Astrophys.
  51. Fermilab
  52. Ecole Polytechnique, Lausanne
  53. Andes U., Bogota
  54. Warwick U.
  55. Colombia, U. Natl.
  56. U. Texas, Dallas
  57. New York U., CCPP
  58. ICC, Barcelona U.; Barcelona, IEEC
  59. Conacyt, Mexico; Guanajuato U.
  60. Munich, Tech. U., Universe; Munich U.
  61. Princeton U.
  62. Florida U.
  63. U. Michigan, Ann Arbor; Michigan U.
  64. Cambridge U., Inst. of Astron.
  65. Peking U., CHEP
  66. Waterloo U.
  67. Marseille, Lab. Astrophys.
  68. Chicago U., KICP; Ohio State U., Dept. Astron.; Ohio State U.
  69. Seoul U.
  70. Edinburgh U., Inst. Astron.; Cambridge U.
  71. Wigner RCP, Budapest
  72. Waterloo U.; Perimeter Inst. Theor. Phys.
  73. Sejong U.
  74. Taiwan, Natl. Taiwan U.
  75. Perimeter Inst. Theor. Phys.
  76. Paris U., VI-VII
  77. UC, Santa Cruz (main); UC, Santa Cruz, Inst. Part. Phys.; Lick Observ.
  78. Toronto U., Astron. Dept.
  79. LBL, Berkeley; UC, Berkeley, Space Sci. Dept.; BCCP, Berkeley
  80. Harvard U.
  81. Barcelona, IFAE; Barcelona, Autonoma U.
  82. Imperial Coll., London; Warwick U.
  83. ICREA, Barcelona; Barcelona, Autonoma U.; Barcelona, IFAE
  84. Tsinghua U., Beijing
  85. Siena Coll., Loudonville
  86. Sussex U.
  87. Wyoming U.
  88. Beijing Observ.
  89. Guanajuato U.; Mexico U., ICN
  90. IRFU, Saclay; LBL, Berkeley
  91. Carnegie Mellon U.
  92. KASI, DaeJeon
  93. ICC, Barcelona U.
  94. Edinburgh U., Inst. Astron.; Ohio State U.
  95. Marseille, CPPM; IRFU, Saclay
  96. UC, Santa Cruz (main); UC, Santa Cruz, Inst. Part. Phys.; Lick Observ.; UC, Santa Cruz
  97. Swinburne U., Ctr. Astrophys. Supercomput.; Queensland U.
  98. Kansas State U.; Ilia State U.
  99. SLAC
  100. Baltimore, Space Telescope Sci.
  101. Ohio U., Athens
  102. UCLA
  103. LBL, Berkeley; Florida U.
  104. St. Andrews U.
  105. ICREA, Barcelona; Barcelona, Autonoma U.; ICC, Barcelona U.; Barcelona, IEEC
  106. Tsinghua U., Beijing; Beihang U.
  107. KIPAC, Menlo Park; Stanford U., Phys. Dept.; SLAC
  108. UC, Berkeley; BCCP, Berkeley
  109. Tsinghua U., Beijing; Ecole Polytechnique, Lausanne
  110. Chicago U., KICP; Shanghai Jiaotong U.; Shanghai Jiao Tong U.
+ Show Author Affiliations

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.

Research Organization:
UNAM, Mexico; Wyoming U.; Munich U.; Portsmouth U., ICG; Andes U., Bogota; University Coll. London; UC, Berkeley, Space Sci. Dept.; Taiwan, Natl. Taiwan U.; Seoul U.; Stanford U., Phys. Dept.; Beijing Observ.; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Universities Space Research Assoc.; Toronto U., Astron. Dept.; Paris U., VI-VII; Princeton, Inst. Advanced Study; Ecole Polytechnique, Lausanne; Carnegie Mellon U.; Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); U. Michigan, Dept. Astron.; Barcelona, IEEC; Waterloo U.; ICREA, Barcelona; Shanghai Jiao Tong U.; Baltimore, Space Telescope Sci.; Boston U.; Lick Observ.; Cambridge U.; Durham U., ICC; KASI, DaeJeon; Sussex U.; Munich, Tech. U., Universe; BCCP, Berkeley; Rochester U.; Madrid, IFT; Yale U.; Marseille, Lab. Astrophys.; UC, Santa Cruz; Swinburne U., Ctr. Astrophys. Supercomput.; Chicago U., Astron. Astrophys. Ctr.; Wigner RCP, Budapest; Ohio U., Athens; IRFU, Saclay; Madrid, CIEMAT; Newcastle upon Tyne U.; Shanghai Jiaotong U.; U. Texas, Dallas; Edinburgh U., Inst. Astron.; Peking U., CHEP; Barcelona, Autonoma U.; Taiwan, Natl. Tsing Hua U.; Warwick U.; Princeton U.; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Kansas State U.; Pittsburgh U.; Conacyt, Mexico; Siena Coll., Loudonville; Florida U.; Ilia State U.; Utah U.; Ohio State U.; Natl. Solar Observ., Tucson; UCLA; Imperial Coll., London; Marseille, CPPM; Harvard U.; UC, Berkeley; Tsinghua U., Beijing; Granada U., Theor. Phys. Astrophys.; Milan U.; Southern Methodist U.; Michigan U.; Barcelona, IFAE; TIFR, Mumbai, DHEP; IAC, La Laguna; Guanajuato U.; Arizona U., Astron. Dept. - Steward Observ.; Beihang U.; Durham U.; Cambridge U., Inst. of Astron.; Sejong U.; Mexico U., ICN; Laguna U., Tenerife; Colombia, U. Natl.; Perimeter Inst. Theor. Phys.; Harvard-Smithsonian Ctr. Astrophys.; UC, Santa Cruz (main); Ohio State U., Dept. Astron.; UC, Irvine; ICC, Barcelona U.; Queensland U.; CINVESTAV, IPN; Chicago U., KICP; U. Michigan, Ann Arbor; St. Andrews U.; New York U., CCPP; UC, Santa Cruz, Inst. Part. Phys.
Sponsoring Organization:
US Department of Energy
Grant/Contract Number:
AC02-07CH11359; 89243024CSC000002
OSTI ID:
1988475
Alternate ID(s):
OSTI ID: 2349431
OSTI ID: 2350767
OSTI ID: 2352714
OSTI ID: 2375037
OSTI ID: 2477984
OSTI ID: 2281914
Report Number(s):
FERMILAB-PUB-23-317-PPD; oai:inspirehep.net:2668108; arXiv:2306.06307
Journal Information:
Astron.J., Journal Name: Astron.J. Journal Issue: 2 Vol. 167
Country of Publication:
United States
Language:
English

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