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First Results from COPSS: The CO Power Spectrum Survey

Keating, Garrett K. and Bower, Geoffrey C. and Marrone, Daniel P. and DeBoer, David R. and Heiles, Carl and Chang, Tzu-Ching and Carlstrom, John E. and Greer, Christopher H. and Hawkins, David and Lamb, James W. and Leitch, Erik and Miller, Amber D. and Muchovej, Stephen and Woody, David P. (2015) First Results from COPSS: The CO Power Spectrum Survey. Astrophysical Journal, 814 (2). Art. No. 140. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20160324-112710383

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Abstract

We present constraints on the abundance of carbon monoxide in the early universe from the CO Power Spectrum Survey. We utilize a data set collected between 2005 and 2008 using the Sunyaev–Zel'dovich Array (SZA), which was previously used to measure arcminute-scale fluctuations of the cosmic microwave background. This data set features observations of 44 fields, covering an effective area of 1.7 square degrees, over a frequency range of 27–35 GHz. Using the technique of intensity mapping, we are able to probe the CO(1–0) transition, with sensitivity to spatial modes between k = 0.5–2 h Mpc^(−1) over a range in redshift of z = 2.3–3.3, spanning a comoving volume of 3.6 × 10^6 h^(−3) Mpc^3. We demonstrate our ability to mitigate foregrounds, and present estimates of the impact of continuum sources on our measurement. We constrain the CO power spectrum to P_(CO) < 2.6 × 10^4 μK^2 (h^(−1) Mpc)^3, or Δ^2_(CO)(k = 1 h Mpc^(−1)) < 1.3 × 10^3 μK^2, at 95% confidence. This limit resides near optimistic predictions for the CO power spectrum. Under the assumption that CO emission is proportional to halo mass during bursts of active star formation, this corresponds to a limit on the ratio of CO(1–0) luminosity to host halo mass of A_(CO) < 1.2 × 10^(−5) L⊙_ M_⊙^(−1). Further assuming a Milky Way-like conversion factor between CO luminosity and molecular gas mass (α_(CO) = 4.3 M_⊙ (K km s^(−1) pc^(−2))^(−1)), we constrain the global density of molecular gas to ρ_(z~3) (M_H_2) ⩽ 2.8 x 10^8 M_☉ Mpc^(-3).


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/814/2/140DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/814/2/140PublisherArticle
http://arxiv.org/abs/1510.06744arXivDiscussion Paper
ORCID:
AuthorORCID
Bower, Geoffrey C.0000-0003-4056-9982
Marrone, Daniel P.0000-0002-2367-1080
Carlstrom, John E.0000-0002-2044-7665
Greer, Christopher H.0000-0002-9590-0508
Additional Information:© 2015 American Astronomical Society. Received 2015 August 25; accepted 2015 October 22; published 2015 November 30. The authors would like to thank F. M. Fornasini and R. L. Plambeck for their valuable feedback during the preparation of this manuscript. This work was supported in part by the National Science Foundation University Radio Observatories Program, AST-1140031. We gratefully acknowledge the James S. McDonnell Foundation, the National Science Foundation, and the University of Chicago for funding to construct the SZA. The operation of the SZA was supported by NSF through award AST-0604982. Partial support was provided by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, and by NSF grants AST-0507545 and AST-0507161 to Columbia University.
Funders:
Funding AgencyGrant Number
NSFAST-1140031
James S. McDonnell FoundationUNSPECIFIED
NSFUNSPECIFIED
University of ChicagoUNSPECIFIED
NSFAST-0604982
NSF Physics Frontier CenterPHY-0114422
NSFAST-0507545
NSFAST-0507161
Subject Keywords:galaxies: evolution; galaxies: high-redshift; ISM: molecules; methods: statistical
Issue or Number:2
Record Number:CaltechAUTHORS:20160324-112710383
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20160324-112710383
Official Citation:Garrett K. Keating et al 2015 ApJ 814 140
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65660
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:25 Mar 2016 14:39
Last Modified:09 Mar 2020 13:19

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