PROSPECTS FOR DETECTING C II EMISSION DURING THE EPOCH OF REIONIZATION

	PROSPECTS FOR DETECTING C II EMISSION DURING THE EPOCH OF REIONIZATION
	Silva, Marta 1,2,3,5; Santos, Mario G.1,3,4; Cooray, Asantha 2; Gong, Yan2,6
刊名	ASTROPHYSICAL JOURNAL
	2015-06-20
卷号	806 期号:2
关键词	galaxies: high-redshift galaxies: ISM galaxies: luminosity function mass function large-scale structure of universe quasars: emission lines
英文摘要	We produce simulations of the atomic C II line emission in large sky fields in order to determine the current and future prospects for mapping this line during the high-redshift epoch of reionization. We calculate the C II line intensity, redshift evolution, and spatial fluctuations using observational relations between C II emission and the galaxy star formation rate over the frequency range 200-300 GHz. We estimate an averaged intensity of I-C II = (4 +/- 2) x 10(2) Jy sr(-1) in the redshift range z similar to 5.3-8.5. Observations of the C II emission in this frequency range will suffer contamination from emission lines at lower redshifts, in particular CO rotational lines. Using simulations, we estimated the CO contamination to be I-CO approximate to 10(3) Jy sr(-1) (originating from galaxies at z < 2.5). Using detailed simulations of the C II and CO emission across a range of redshifts, we generate maps as a function of angle and frequency, fully taking into account this resolution and light-cone effects. In order to reduce the foreground contamination, we find that we should mask galaxies below redshifts similar to 2.5 with a CO(J:2-1) to CO (J: 6-5) line flux density higher than 5 x 10(-22) W m(-2) or an AB magnitude lower than m(K) = 22. We estimate that the additional continuum contamination originating in emission from stars and in dust, free-free, free-bound, and two-photon emission in the interstellar medium is of the order of 10(5) Jy sr(-1), which is well above the expected C II signal. We also consider the possibility of cross-correlating foreground lines with galaxy surveys in order to probe the intensity of the foregrounds. Finally, we discuss the expected constraints from two experiments capable of measuring the expected C II power spectrum.
收录类别	SCI
语种	英语
WOS记录号	WOS:000357129500064
内容类型	期刊论文
源URL	[http://ir.bao.ac.cn/handle/114a11/5653]
专题	国家天文台_星系宇宙学研究部
作者单位	1.Univ Tecn Lisboa, CENTRA, Inst Super Tecn, P-1049001 Lisbon, Portugal 2.Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA 3.Univ Western Cape, Dept Phys & Astron, ZA-7535 Cape Town, South Africa 4.SKA SA, ZA-7405 Cape Town, South Africa 5.Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands 6.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
推荐引用方式 GB/T 7714	Silva, Marta,Santos, Mario G.,Cooray, Asantha,et al. PROSPECTS FOR DETECTING C II EMISSION DURING THE EPOCH OF REIONIZATION[J]. ASTROPHYSICAL JOURNAL,2015,806(2).
APA	Silva, Marta,Santos, Mario G.,Cooray, Asantha,&Gong, Yan.(2015).PROSPECTS FOR DETECTING C II EMISSION DURING THE EPOCH OF REIONIZATION.ASTROPHYSICAL JOURNAL,806(2).
MLA	Silva, Marta,et al."PROSPECTS FOR DETECTING C II EMISSION DURING THE EPOCH OF REIONIZATION".ASTROPHYSICAL JOURNAL 806.2(2015).