COPSS II: THE MOLECULAR GAS CONTENT OF TEN MILLION CUBIC MEGAPARSECS AT REDSHIFT z∼ 3
AuthorKeating, Garrett K.
Marrone, Daniel P.
Bower, Geoffrey C.
Carlstrom, John E.
DeBoer, David R.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationCOPSS II: THE MOLECULAR GAS CONTENT OF TEN MILLION CUBIC MEGAPARSECS AT REDSHIFT z ∼ 3 2016, 830 (1):34 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe present a measurement of the abundance of carbon monoxide in the early universe, utilizing the final results from the CO Power Spectrum Survey (COPSS). Between 2013 and 2015, we performed observations with the Sunyaev-Zel'dovich Array to measure aggregate CO emission from z similar to 3 galaxies with the intensity mapping technique. Data were collected on 19 fields, covering an area of 0.7 square degrees, over the frequency range 27-35 GHz. With these data, along with data analyzed in COPSS I, we are able to observe the CO(1-0) transition within the redshift range z = 2.3-3.3 for spatial frequencies between k = 0.5-10 h Mpc(-1), spanning a comoving volume of 4.9 x 10(6) h(-3) Mpc(3). We present estimates of contributions from continuum sources and ground illumination within our measurement. We constrain the amplitude of the CO power spectrum to P-CO = 3.0(-1.3)(+1.3) x 10(3) mu K-2(h(-1) Mpc)(3), or Delta(2)(CO)(k=1 h Mpc(-1)) = 1.5(-0.7)(+0.7) x 10(3) mu K-2, at 68% confidence, and PCO > 0 at 98.9% confidence. These results are a factor of 10 improvement in sensitivity compared to those of COPSS I. With this measurement, we constrain on the CO(1-0) galaxy luminosity function at z similar to 3. Assuming that CO emission is proportional to halo mass and using theoretical estimates of the scatter in this relationship, we constrain the ratio of CO(1-0) luminosity to halo mass to A(CO) = 6.3(-2.1)(+1.4) x 10 (7) L circle dot M circle dot-1. Assuming a Milky Way-like linear relationship between CO luminosity and molecular gas mass, we estimate a mass fraction of molecular gas of f(H2) = 5.5(-2.2)(+3.4) x 10(-2) for halos with masses of similar to 10(12)M(circle dot). Using theoretical estimates for the scaling of molecular gas mass fraction and halo mass, we estimate the cosmic molecular gas density to be rho(z similar to 3) (H-2) = 1.1(-0.4)(+0.7) x 10(8) M(circle dot)Mpc(-3).
VersionFinal published version
SponsorsJames S. McDonnell Foundation; National Science Foundation (NSF); University of Chicago; NSF Physics Frontier Center [PHY-0114422]; state of California; state of Illinois; state of Maryland; James S McDonnell Foundation; Gordon and Betty Moore Foundation; Kenneth T and Eileen L Norris Foundation; Associates of the California Institute of Technology; National Science Foundation University Radio Observatories Program [AST-1140019, AST-1140031, AST-1140021]; CARMA partner universities