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COMAP Early Science. I. Overview

Cleary, Kieran A. and Borowska, Jowita and Breysse, Patrick C. and Catha, Morgan and Chung, Dongwoo T. and Church, Sarah E. and Dickinson, Clive and Eriksen, Hans Kristian and Foss, Marie Kristine and Gundersen, Joshua Ott and Harper, Stuart E. and Harris, Andrew I. and Hobbs, Richard and Ihle, Håvard T. and Kim, Junhan and Kocz, Jonathon and Lamb, James W. and Lunde, Jonas G. S. and Padmanabhan, Hamsa and Pearson, Timothy J. and Philip, Liju and Powell, Travis W. and Rasmussen, Maren and Readhead, Anthony C. S. and Rennie, Thomas J. and Silva, Marta B. and Stutzer, Nils-Ole and Uzgil, Bade D. and Watts, Duncan J. and Wehus, Ingunn Kathrine and Woody, David P. and Basoalto, Lilian and Bond, J. Richard and Dunne, Delaney A. and Gaier, Todd and Hensley, Brandon and Keating, Laura C. and Lawrence, Charles R. and Murray, Norman and Paladini, Roberta and Reeves, Rodrigo and Viero, Marco P. and Wechsler, Risa H. (2022) COMAP Early Science. I. Overview. Astrophysical Journal, 933 (2). Art. No. 182. ISSN 0004-637X. doi:10.3847/1538-4357/ac63cc.

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The CO Mapping Array Project (COMAP) aims to use line-intensity mapping of carbon monoxide (CO) to trace the distribution and global properties of galaxies over cosmic time, back to the Epoch of Reionization (EoR). To validate the technologies and techniques needed for this goal, a Pathfinder instrument has been constructed and fielded. Sensitive to CO(1–0) emission from z = 2.4–3.4 and a fainter contribution from CO(2–1) at z = 6–8, the Pathfinder is surveying 12 deg² in a 5 yr observing campaign to detect the CO signal from z ∼ 3. Using data from the first 13 months of observing, we estimate P_(CO)(k) = −2.7 ± 1.7 × 10⁴ μK² Mpc³ on scales k = 0.051 −0.62 Mpc⁻¹, the first direct three-dimensional constraint on the clustering component of the CO(1–0) power spectrum. Based on these observations alone, we obtain a constraint on the amplitude of the clustering component (the squared mean CO line temperature bias product) of ⟨Tb⟩² < 49 μK², nearly an order-of-magnitude improvement on the previous best measurement. These constraints allow us to rule out two models from the literature. We forecast a detection of the power spectrum after 5 yr with signal-to-noise ratio (S/N) 9–17. Cross-correlation with an overlapping galaxy survey will yield a detection of the CO–galaxy power spectrum with S/N of 19. We are also conducting a 30 GHz survey of the Galactic plane and present a preliminary map. Looking to the future of COMAP, we examine the prospects for future phases of the experiment to detect and characterize the CO signal from the EoR.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Cleary, Kieran A.0000-0002-8214-8265
Breysse, Patrick C.0000-0001-8382-5275
Chung, Dongwoo T.0000-0003-2618-6504
Dickinson, Clive0000-0002-0045-442X
Eriksen, Hans Kristian0000-0003-2332-5281
Foss, Marie Kristine0000-0001-8896-3159
Gundersen, Joshua Ott0000-0002-7524-4355
Harper, Stuart E.0000-0001-7911-5553
Harris, Andrew I.0000-0001-6159-9174
Ihle, Håvard T.0000-0003-3420-7766
Kim, Junhan0000-0002-4274-9373
Kocz, Jonathon0000-0003-0249-7586
Lamb, James W.0000-0002-5959-1285
Padmanabhan, Hamsa0000-0002-8800-5740
Pearson, Timothy J.0000-0001-5213-6231
Philip, Liju0000-0001-7612-2379
Readhead, Anthony C. S.0000-0001-9152-961X
Rennie, Thomas J.0000-0002-1667-3897
Silva, Marta B.0000-0003-0209-4816
Stutzer, Nils-Ole0000-0001-5301-1377
Uzgil, Bade D.0000-0001-8526-3464
Watts, Duncan J.0000-0002-5437-6121
Wehus, Ingunn Kathrine0000-0003-3821-7275
Bond, J. Richard0000-0003-2358-9949
Dunne, Delaney A.0000-0002-5223-8315
Hensley, Brandon0000-0001-7449-4638
Keating, Laura C.0000-0001-5211-1958
Paladini, Roberta0000-0002-5158-243X
Reeves, Rodrigo0000-0001-5704-271X
Viero, Marco P.0000-0003-0545-4872
Wechsler, Risa H.0000-0003-2229-011X
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 November 19; revised 2022 February 24; accepted 2022 April 1; published 2022 July 13. Focus on Early Science Results from the CO Mapping Array Project (COMAP). This material is based upon work supported by the National Science Foundation under grant Nos. 1517108, 1517288, 1517598, 1518282, and 1910999, and by the Keck Institute for Space Studies under "The First Billion Years: A Technical Development Program for Spectral Line Observations." Parts of the work were carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and funded through the internal Research and Technology Development program. DTC is supported by a CITA/Dunlap Institute postdoctoral fellowship. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. C.D. and S.H. acknowledge support from an STFC Consolidated grant (ST/P000649/1). J.B., H.K.E., M.K.F., H.T.I., J.G.S.L., M.R., N.O.S., D.W., and I.K.W. acknowledge support from the Research Council of Norway through grant Nos. 251328 and 274990, and from the European Research Council (ERC) under the Horizon 2020 Research and Innovation Program (grant agreement No. 819478, Cosmoglobe). J.G. acknowledges support from the University of Miami and is grateful to Hugh Medrano for assistance with cryostat design. L.K. was supported by the European Unions Horizon 2020 research and innovation program under the Marie Skodowska-Curie grant agreement No. 885990. J.K. is supported by a Robert A. Millikan Fellowship from Caltech. At JPL, we are grateful to Mary Soria for assembly work on the amplifier modules and to Jose Velasco, Ezra Long, and Jim Bowen for the use of their amplifier test facilities. H.P. acknowledges support from the Swiss National Science Foundation through Ambizione Grant PZ00P2_179934. P.C.B. is supported by the James Arthur Postdoctoral Fellowship. R.R. acknowledges support from ANID-FONDECYT grant No. 1181620. L.B. was supported by ANID-PFCHA/DOCTORADO NACIONAL 2019-21192138. M.V. acknowledges support from the Kavli Institute for Particle Astrophysics and Cosmology. We thank Isu Ravi for her contributions to the warm electronics and antenna drive characterization. Finally, we thank the anonymous referee, whose comments and suggestions have helped to improve and clarify this manuscript.
Group:Astronomy Department, Keck Institute for Space Studies, Owens Valley Radio Observatory (OVRO)
Funding AgencyGrant Number
Keck Institute for Space Studies (KISS)UNSPECIFIED
JPL Research and Technology Development FundUNSPECIFIED
Canadian Institute for Theoretical AstrophysicsUNSPECIFIED
Dunlap Institute for Astronomy and AstrophysicsUNSPECIFIED
University of TorontoUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/P000649/1
Research Council of Norway251328
Research Council of Norway274990
European Research Council (ERC)819478
Marie Curie Fellowship885990
Robert A. Millikan FellowshipUNSPECIFIED
Swiss National Science Foundation (SNSF)PZ00P2_179934
American Astronomical SocietyUNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1181620
Agencia Nacional de Investigación y Desarrollo (ANID)2019-21192138
Kavli Institute for Particle Astrophysics and CosmologyUNSPECIFIED
Subject Keywords:CO line emission; Cosmological evolution; High-redshift galaxy clusters; Molecular gas; Radio astronomy; Astronomical instrumentation
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: CO line emission (262); Cosmological evolution (336); High-redshift galaxy clusters (2007); Molecular gas (1073); Radio astronomy (1338); Astronomical instrumentation (799)
Record Number:CaltechAUTHORS:20220322-205028700
Persistent URL:
Official Citation:Kieran A. Cleary et al 2022 ApJ 933 182
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:113986
Deposited By: George Porter
Deposited On:23 Mar 2022 14:26
Last Modified:29 Jul 2022 21:25

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