COMAP Early Science. V. Constraints and Forecasts at z ∼ 3
- Creators
- Chung, Dongwoo T.
- Breysse, Patrick C.
- Cleary, Kieran A.
- Ihle, Håvard T.
- Padmanabhan, Hamsa
- Silva, Marta B.
- Bond, J. Richard
- Borowska, Jowita
- Catha, Morgan
- Church, Sarah E.
- Dunne, Delaney A.
- Kristian Eriksen, Hans
- Kristine Foss, Marie
- Gaier, Todd
- Gundersen, Joshua Ott
- Harper, Stuart E.
- Harris, Andrew I.
- Hensley, Brandon
- Hobbs, Richard
- Keating, Laura C.
- Kim, Junhan
- Lamb, James W.
- Lawrence, Charles R.
- Lunde, Jonas Gahr Sturtzel
- Murray, Norman
- Pearson, Timothy J.
- Philip, Liju
- Rasmussen, Maren
- Readhead, Anthony C. S.
- Rennie, Thomas J.
- Stutzer, Nils-Ole
- Uzgil, Bade D.
- Viero, Marco P.
- Watts, Duncan J.
- Wechsler, Risa H.
- Kathrine Wehus, Ingunn
- Woody, David P.
- COMAP Collaboration
Abstract
We present the current state of models for the z ∼ 3 carbon monoxide (CO) line intensity signal targeted by the CO Mapping Array Project (COMAP) Pathfinder in the context of its early science results. Our fiducial model, relating dark matter halo properties to CO luminosities, informs parameter priors with empirical models of the galaxy–halo connection and previous CO (1–0) observations. The Pathfinder early science data spanning wavenumbers k = 0.051–0.62 Mpc⁻¹ represent the first direct 3D constraint on the clustering component of the CO (1–0) power spectrum. Our 95% upper limit on the redshift-space clustering amplitude A_(clust) ≲ 70 μK² greatly improves on the indirect upper limit of 420 μK² reported from the CO Power Spectrum Survey (COPSS) measurement at k ∼ 1 Mpc⁻¹. The COMAP limit excludes a subset of models from previous literature and constrains interpretation of the COPSS results, demonstrating the complementary nature of COMAP and interferometric CO surveys. Using line bias expectations from our priors, we also constrain the squared mean line intensity–bias product, (T_b)₂ ≲ 50 μK², and the cosmic molecular gas density, ρ_(H2) < 2.5 x 10⁸ M_⊙ Mpc⁻³ (95% upper limits). Based on early instrument performance and our current CO signal estimates, we forecast that the 5 yr Pathfinder campaign will detect the CO power spectrum with overall signal-to-noise ratio of 9–17. Between then and now, we also expect to detect the CO–galaxy cross-spectrum using overlapping galaxy survey data, enabling enhanced inferences of cosmic star formation and galaxy evolution history.
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 4; published 2022 July 13. Focus on Early Science Results from the CO Mapping Array Project (COMAP) This material is based on work supported by the National Science Foundation under grant Nos. 1518282, 1517108, 1517598, 1517288, and 1910999; by the Keck Institute for Space Studies under "The First Billion Years: A Technical Development Program for Spectral Line Observations"; and by a seed grant from the Kavli Institute for Particle Astrophysics and Cosmology. 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. The University of Toronto operates on the traditional land of the Huron-Wendat, the Seneca, and, most recently, the Mississaugas of the Credit River; D.T.C. is grateful to have the opportunity to work on this land. P.C.B. is supported by the James Arthur Postdoctoral Fellowship at New York University. K.C., J.W.L., A.C.S.R., B.D.U., and D.P.W. acknowledge support from NSF awards 1518282 and 1910999. 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). 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. H.P. acknowledges support from the Swiss National Science Foundation through Ambizione grant PZ00P2_179934. J.O.G. acknowledges support from the Keck Institute for Space Science, NSF AST-1517108, and the University of Miami. S.E.H. acknowledges support from an STFC Consolidated grant (ST/P000649/1). L.C.K. was supported by the European Union's Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 885990. J.K. is supported by a Robert A. Millikan Fellowship from Caltech. We thank Riccardo Pavesi for access to the COLDz ABC posterior sample used in this work. This research made use of NASA's Astrophysics Data System Bibliographic Services. Some of the computing for this project was performed on the Sherlock cluster. D.T.C. would like to thank Stanford University and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results. The Scientific color maps acton and tokyo (Crameri 2021) are used in this study to prevent visual distortion of the data and exclusion of readers with color-vision deficiencies (Crameri et al. 2020). Finally, we would like to thank an anonymous referee whose comments and suggestions significantly improved this manuscript. Software: hmf (Murray et al. 2013); Matplotlib (Hunter 2007); corner.py (Foreman-Mackey 2016); Astropy, a community-developed core Python package for astronomy (Astropy Collaboration et al. 2013).Attached Files
Published - Chung_2022_ApJ_933_186.pdf
Accepted Version - 2111.05931.pdf
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Additional details
- Eprint ID
- 115794
- Resolver ID
- CaltechAUTHORS:20220722-769356000
- AST-1518282
- NSF
- AST-1517108
- NSF
- AST-1517598
- NSF
- AST-1517288
- NSF
- AST-1910999
- NSF
- Kavli Institute for Particle Astrophysics and Cosmology
- Canadian Institute for Theoretical Astrophysics
- Dunlap Institute for Astronomy and Astrophysics
- University of Toronto
- New York University (NYU)
- 251328
- Research Council of Norway
- 274990
- Research Council of Norway
- 819478
- European Research Council (ERC)
- NASA/JPL/Caltech
- JPL Research and Technology Development Fund
- PZ00P2_179934
- Swiss National Science Foundation (SNSF)
- University of Miami
- 885990
- Marie Curie Fellowship
- Robert A. Millikan Fellowship
- Created
-
2022-07-22Created from EPrint's datestamp field
- Updated
-
2022-07-22Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, Infrared Processing and Analysis Center (IPAC), Keck Institute for Space Studies, Owens Valley Radio Observatory