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COMAP Early Science. VII. Prospects for CO Intensity Mapping at Reionization

Breysse, Patrick C. and Chung, Dongwoo T. and Cleary, Kieran A. and Ihle, Håvard T. and Padmanabhan, Hamsa and Silva, Marta B. and Bond, J. Richard and Borowska, Jowita and Catha, Morgan and Church, Sarah E. and Dunne, Delaney A. and Eriksen, Hans Kristian and Foss, Marie Kristine and Gaier, Todd and Gundersen, Joshua Ott and Harris, Andrew I. and Hobbs, Richard and Keating, Laura and Lamb, James W. and Lawrence, Charles R. and Lunde, Jonas G. S. and Murray, Norman and Pearson, Timothy J. and Philip, Liju and Rasmussen, Maren and Readhead, Anthony C. S. and Rennie, Thomas J. and Stutzer, Nils-Ole and Viero, Marco P. and Watts, Duncan J. and Wehus, Ingunn Kathrine and Woody, David P. (2022) COMAP Early Science. VII. Prospects for CO Intensity Mapping at Reionization. Astrophysical Journal, 933 (2). Art. No. 188. ISSN 0004-637X. doi:10.3847/1538-4357/ac63c9.

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We introduce COMAP-EoR, the next generation of the Carbon Monoxide Mapping Array Project aimed at extending CO intensity mapping to the Epoch of Reionization. COMAP-EoR supplements the existing 30 GHz COMAP Pathfinder with two additional 30 GHz instruments and a new 16 GHz receiver. This combination of frequencies will be able to simultaneously map CO(1–0) and CO(2–1) at reionization redshifts (z ∼ 5–8) in addition to providing a significant boost to the z ∼ 3 sensitivity of the Pathfinder. We examine a set of existing models of the EoR CO signal, and find power spectra spanning several orders of magnitude, highlighting our extreme ignorance about this period of cosmic history and the value of the COMAP-EoR measurement. We carry out the most detailed forecast to date of an intensity mapping cross correlation, and find that five out of the six models we consider yield signal to noise ratios (S/Ns) ≳ 20 for COMAP-EoR, with the brightest reaching a S/N above 400. We show that, for these models, COMAP-EoR can make a detailed measurement of the cosmic molecular gas history from z ∼ 2–8, as well as probe the population of faint, star-forming galaxies predicted by these models to be undetectable by traditional surveys. We show that, for the single model that does not predict numerous faint emitters, a COMAP-EoR-type measurement is required to rule out their existence. We briefly explore prospects for a third-generation Expanded Reionization Array (COMAP-ERA) capable of detecting the faintest models and characterizing the brightest signals in extreme detail.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Breysse, Patrick C.0000-0001-8382-5275
Chung, Dongwoo T.0000-0003-2618-6504
Cleary, Kieran A.0000-0002-8214-8265
Ihle, Håvard T.0000-0003-3420-7766
Padmanabhan, Hamsa0000-0002-8800-5740
Silva, Marta B.0000-0003-0209-4816
Bond, J. Richard0000-0003-2358-9949
Dunne, Delaney A.0000-0002-5223-8315
Eriksen, Hans Kristian0000-0003-2332-5281
Foss, Marie Kristine0000-0001-8896-3159
Harris, Andrew I.0000-0001-6159-9174
Keating, Laura0000-0001-5211-1958
Lamb, James W.0000-0002-5959-1285
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
Stutzer, Nils-Ole0000-0001-5301-1377
Viero, Marco P.0000-0003-0545-4872
Watts, Duncan J.0000-0002-5437-6121
Wehus, Ingunn Kathrine0000-0003-3821-7275
Alternate Title:COMAP Early Science: VII. Prospects for CO Intensity Mapping at Reionization
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 March 7; 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. P.C.B. is supported by the James Arthur Postdoctoral Fellowship. D.T.C. 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. H.I. acknowledges support from the Research Council of Norway through grant 251328. H.P. acknowledges support from the Swiss National Science Foundation through Ambizione Grant PZ00P2_179934. Work at the University of Oslo is supported by the Research Council of Norway through grants 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 Keck Institute for Space Science, NSF AST-1517108 and University of Miami and Hugh Medrano for assistance with the cryostat design. J.L. acknowledges support from NSF Awards 1518282 and 1910999. L.K. was supported by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 885990. We thank Isu Ravi for contributions to the warm electronics and antenna drive characterization. The authors would like to thank Shengqi Yang, Anthony Pullen, Rachel Somerville, and Abhishek Maniyar for useful discussions. Finally, we would like to thank an anonymous referee whose comments and suggestions significantly improved 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
Science and Technology Facilities Council (STFC)ST/P000649/1
JPL Research and Technology Development FundUNSPECIFIED
New York University (NYU)UNSPECIFIED
Canadian Institute for Theoretical AstrophysicsUNSPECIFIED
Dunlap Institute for Astronomy and AstrophysicsUNSPECIFIED
University of TorontoUNSPECIFIED
Research Council of Norway251328
Swiss National Science Foundation (SNSF)PZ00P2_179934
Research Council of Norway274990
European Research Council (ERC)819478
University of MiamiUNSPECIFIED
Marie Curie Fellowship885990
Subject Keywords:CO line emission; Reionization; Cosmological evolution; High-redshift galaxies; Molecular gas; Radio astronomy
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: CO line emission (262); Reionization (1383); Cosmological evolution (336); High-redshift galaxies (734); Molecular gas (1073); Radio astronomy (1338)
Record Number:CaltechAUTHORS:20220722-769501000
Persistent URL:
Official Citation:Patrick C. Breysse et al 2022 ApJ 933 188
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115797
Deposited By: George Porter
Deposited On:26 Jul 2022 17:39
Last Modified:26 Jul 2022 17:39

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