COMAP Early Science. I. Overview
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Published:2022-07-01
Issue:2
Volume:933
Page:182
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ISSN:0004-637X
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Container-title:The Astrophysical Journal
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language:
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Short-container-title:ApJ
Author:
Cleary Kieran A.ORCID, Borowska Jowita, Breysse Patrick C.ORCID, Catha Morgan, Chung Dongwoo T.ORCID, Church Sarah E., Dickinson Clive, Eriksen Hans KristianORCID, Foss Marie KristineORCID, Gundersen Joshua Ott, Harper Stuart E.ORCID, Harris Andrew I.ORCID, Hobbs Richard, Ihle Håvard T.ORCID, Kim JunhanORCID, Kocz Jonathon, Lamb James W.ORCID, Lunde Jonas G. S., Padmanabhan HamsaORCID, Pearson Timothy J.ORCID, Philip LijuORCID, Powell Travis W., Rasmussen Maren, Readhead Anthony C. S.ORCID, Rennie Thomas J.ORCID, Silva Marta B.ORCID, Stutzer Nils-OleORCID, Uzgil Bade D.ORCID, Watts Duncan J.ORCID, Wehus Ingunn KathrineORCID, Woody David P., Basoalto Lilian, Bond J. RichardORCID, Dunne Delaney A.ORCID, Gaier Todd, Hensley BrandonORCID, Keating Laura C.ORCID, Lawrence Charles R., Murray Norman, Paladini RobertaORCID, Reeves RodrigoORCID, Viero Marco P.ORCID, Wechsler Risa H.ORCID
Abstract
Abstract
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.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
26 articles.
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