TY - JOUR
T1 - Validation of the scientific program for the Dark Energy Spectroscopic Instrument
AU - DESI Collaboration
AU - Adame, A. G.
AU - Aguilar, J.
AU - Ahlen, S.
AU - Alam, S.
AU - Aldering, G.
AU - Alexander, D. M.
AU - Alfarsy, R.
AU - Allende Prieto, C.
AU - Alvarez, M.
AU - Alves, O.
AU - Anand, A.
AU - Andrade-Oliveira, F.
AU - Armengaud, E.
AU - Asorey, J.
AU - Avila, S.
AU - Aviles, A.
AU - Bailey, S.
AU - Balaguera-Antolínez, A.
AU - Ballester, O.
AU - Baltay, C.
AU - Bault, A.
AU - Bautista, J.
AU - Behera, J.
AU - Beltran, S. F.
AU - BenZvi, S.
AU - Beraldo e Silva, L.
AU - Bermejo-Climent, J. R.
AU - Berti, A.
AU - Besuner, R.
AU - Beutler, F.
AU - Bianchi, D.
AU - Blake, C.
AU - Blum, R.
AU - Bolton, A. S.
AU - Brieden, S.
AU - Brodzeller, A.
AU - Brooks, D.
AU - Brown, Z.
AU - Buckley-Geer, E.
AU - Burtin, E.
AU - Cabayol-Garcia, L.
AU - Cai, Z.
AU - Canning, R.
AU - Cardiel-Sas, L.
AU - Carnero Rosell, A.
AU - Castander, F. J.
AU - Cervantes-Cota, J. L.
AU - Chen, S.
AU - Moore, S.
AU - Tojeiro, R.
N1 - Funding: This material is based upon work supported by the U.S. Department of Energy (DOE), Office of Science, Office of High-Energy Physics, under contract No. DE-AC02-05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract.
Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under contract No. AST-0950945 to the NSFʼs National Optical-Infrared Astronomy Research Laboratory; the Science and
Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions.
PY - 2024/2/1
Y1 - 2024/2/1
N2 - The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg2 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 deg2 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 deg2 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.
AB - The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg2 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 deg2 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 deg2 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.
KW - Cosmology
KW - Redshift surveys
U2 - 10.3847/1538-3881/ad0b08
DO - 10.3847/1538-3881/ad0b08
M3 - Article
SN - 0004-6256
VL - 167
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 62
ER -