COMAP Pathfinder - Season 2 results III. Implications for cosmic molecular gas content at z ∼ 3

被引：2

作者：

Chung, D. T. ^{[1
,2
,3
]}

Breysse, P. C. ^{[4
,5
]}

Cleary, K. A. ^{[6
]}

Dunne, D. A. ^{[6
]}

Lunde, J. G. S. ^{[7
]}

Padmanabhan, H. ^{[8
]}

Stutzer, N. -O ^{[7
]}

Tolgay, D. ^{[1
,9
]}

Bond, J. R. ^{[1
,9
,10
]}

Church, S. E. ^{[11
,12
]}

Eriksen, H. K. ^{[7
]}

Gaier, T. ^{[13
]}

Gundersen, J. O. ^{[14
]}

Harper, S. E. ^{[15
]}

Harris, A. I. ^{[16
]}

Hobbs, R. ^{[17
]}

Ihle, H. T. ^{[7
]}

Kim, J. ^{[18
]}

Lamb, J. W. ^{[17
]}

Lawrence, C. R. ^{[13
]}

Murray, N. ^{[1
,9
,10
]}

Pearson, T. J. ^{[6
]}

Philip, L. ^{[19
]}

Readhead, A. C. S. ^{[6
]}

Rennie, T. J. ^{[15
,20
]}

Wehus, I. K. ^{[7
]}

Woody, D. P. ^{[17
]}

机构：

[1] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada

[2] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada

[3] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA

[4] NYU, Ctr Cosmol & Particle Phys, Dept Phys, 726 Broadway, New York, NY 10003 USA

[5] So Methodist Univ, Dept Phys, Dallas, TX 75275 USA

[6] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA

[7] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway

[8] Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermet, CH-1211 Geneva 4, Switzerland

[9] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada

[10] Univ Toronto, David A Dunlap Dept Astron, 50 St George St, Toronto, ON M5S 3H4, Canada

[11] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[12] Stanford Univ, Phys Dept, Stanford, CA 94305 USA

[13] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[14] Univ Miami, Dept Phys, 1320 Campo Sano Ave, Coral Gables, FL 33146 USA

[15] Univ Manchester, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Oxford Rd, Manchester M13 9PL, England

[16] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[17] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA

[18] Korea Adv Inst Sci & Technol KAIST, Dept Phys, 291 Daehak Ro, Daejeon 34141, South Korea

[19] Brookhaven Natl Lab, Upton, NY 11973 USA

[20] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 691卷

基金：

欧洲研究理事会; 美国国家科学基金会; 瑞士国家科学基金会; 新加坡国家研究基金会; 美国国家航空航天局; 加拿大自然科学与工程研究理事会;

关键词：

galaxies: high-redshift; diffuse radiation; radio lines: galaxies; ALMA SPECTROSCOPIC SURVEY; CO LUMINOSITY FUNCTIONS; STAR-FORMATION; HIGH-REDSHIFT; LINE; DENSITY; FIELD; EMISSION; GALAXIES; SEARCH;

D O I：

10.1051/0004-6361/202451122

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Carbon monOxide Mapping Array Project (COMAP) Pathfinder survey continues to demonstrate the feasibility of line-intensity mapping using high-redshift carbon monoxide (CO) line emission traced at cosmological scales. The latest COMAP Pathfinder power spectrum analysis is based on observations through the end of Season 2, covering the first three years of Pathfinder operations. We use our latest constraints on the CO(1-0) line-intensity power spectrum at z similar to 3 to update corresponding constraints on the cosmological clustering of CO line emission and thus the cosmic molecular gas content at a key epoch of galaxy assembly. We first mirror the COMAP Early Science interpretation, considering how Season 2 results translate to limits on the shot noise power of CO fluctuations and the bias of CO emission as a tracer of the underlying dark matter distribution. The COMAP Season 2 results place the most stringent limits on the CO tracer bias to date, at < T b > < 4.8 mu K, which translates to a molecular gas density upper limit of rho(H2) < 1.6 x 10(8) M-circle dot Mpc(-3) at z similar to 3 given additional model assumptions. These limits narrow the model space significantly compared to previous CO line-intensity mapping results while maintaining consistency with small-volume interferometric surveys of resolved line candidates. The results also express a weak preference for CO emission models used to guide fiducial forecasts from COMAP Early Science, including our data-driven priors. We also consider directly constraining a model of the halo-CO connection, and show qualitative hints of capturing the total contribution of faint CO emitters through the improved sensitivity of COMAP data. With continued observations and matching improvements in analysis, the COMAP Pathfinder remains on track for a detection of cosmological clustering of CO emission.

引用

页数：14

共 24 条

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