The first spectral line surveys searching for signals from the dark ages

C. M. Persson; R. Maoli; P. Encrenaz; Å. Hjalmarson; M. Olberg; G. Rydbeck; M. Signore; U. Frisk; Aa. Sandqvist; J. Y. Daniel

doi:10.1051/0004-6361/200913395

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Volume 515 (June 2010)

A&A, 515 (2010) A72

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Table 18:

Estimated required background temperatures to produce absorption lines with $T_{\rm b}=-10$ mK at an observing frequency of 550 GHz assuming $T_{\rm ex} \ll T_{\rm bg}$ , and an opacity of one or 10^-3.
Transition	Redshift	Opacity	$T_{\rm bg}$	$T_{\rm CMB}$
	z	$\tau$	[K]	[K]
H₂(2-0)	18.3	1	58	53
		10^-3	260
H₂(3-1)	31.0	1	96	87
		10^-3	430
H₂(4-2)	43.4	1	132	121
		10^-3	595
H₂(5-3)	55.4	1	168	154
		10^-3	756
HD(4-3)	18.1	1	57	52
		10^-3	257
HD(5-4)	22.7	1	71	65
		10^-3	317
HeH⁺(4-3)	13.4	1	43	39
		10^-3	194
HeH⁺(5-4)	16.7	1	54	48
		10^-3	240

Notes. Note, that since the observing frequencies are the same for all transitions the source redshift is different for every transition. As a comparison, the CMB temperatures are listed for each redshift.

Source LaTeX | All tables | In the text

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