Spitzer deep and wide legacy mid- and far-infrared number counts and lower limits of cosmic infrared background

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Volume 512 (March-April 2010)

A&A, 512 (2010) A78

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Table 3:

Differential number counts at 70 $\mu$ m.
$\langle S\rangle$	$S_{\rm min}$	$S_{\rm max}$	d $N/{\rm d}S.S^{2.5}$	$\sigma_{\rm poisson}$	$\sigma_{\rm clustering}$	$\sigma_{\rm clus.+calib.}$	$\Omega_{\rm used}$
(in mJy)			(in gal Jy^1.5 sr^-1)				deg²
4.197	3.500	4.894	2073.	264.	309.	342.	0.2
5.868	4.894	6.843	2015.	249.	298.	330.	0.2
8.206	6.843	9.569	1690.	289.	332.	353.	0.2
11.474	9.569	13.380	2105.	123.	202.	250.	2.6
16.044	13.380	18.708	2351.	148.	228.	281.	2.6
22.434	18.708	26.159	1706.	153.	208.	240.	2.6
31.369	26.159	36.578	2557.	69.	124.	218.	38.1
43.862	36.578	51.146	2446.	73.	123.	211.	45.5
61.331	51.146	71.517	2359.	90.	141.	217.	45.5
85.758	71.517	100.000	2257.	112.	164.	228.	45.5
157.720	100.000	215.440	2354.	121.	198.	257.	45.5
339.800	215.440	464.160	2048.	200.	276.	311.	45.5
732.080	464.160	1000.000	2349.	381.	500.	526.	45.5

Notes. $\sigma_{\rm clustering}$ is the uncertainty taking into account clustering (see Sect. 4.5). $\sigma_{\rm clus.+calib.}$ takes into account both clustering and calibration (Gordon et al. 2007).

Source LaTeX | All tables | In the text

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