Table 2
Summary of the resolved IGL, its contribution to the CIRB down to specific flux density limit Slim in each SPIRE band for the GOODS-North field.
Wavelength | S > Slim | Resolved IGL | Fraction of CIRB | Comments | Reference CIRB |
(μm) | (mJy) | (nWm-2sr-1) | (nWm-2sr-1) | ||
|
|||||
100 | 1.1 | 6.9 | 54% | after completeness corr. | 12.61 [–1.74;+8.31] a |
100 | 1.1 | 6.1 | 48% | before completeness corr. | |
100 | 1.2 | 8.35 | 66% | Berta et al. (2011) | |
100 | 0.54 | 9.45 | 75% | Magnelli et al. (2013) | |
|
|||||
160 | 2.2 | 8.2 | 60% | after completeness corr. | 13.63 [–0.85;+3.53] a |
160 | 2.2 | 7.2 | 53% | before completeness corr. | |
160 | 2.0 | 9.49 | 70% | Berta et al. (2011) | |
160 | 1.29 | 10.27 | 75% | Magnelli et al. (2013) | |
|
|||||
250 | 2.5 | 6.0 | 55% | after completeness corr. | 10.13 [–2.33;+2.60] b |
250 | 2.5 | 3.4 | 34% | before completeness corr. | |
250 | 20 | 1.73 | 17% | Oliver et al. (2010) | [resolved sources] |
250 | 20 | 1.55 | 15% | Béthermin et al. (2012) | [resolved sources] |
250 | 2.0 | 7.4 | 73% | Béthermin et al. (2012) | [using stacking] |
|
|||||
350 | 5.0 | 2.1 | 33% | after completeness corr. | 6.46 [–1.57;+1.74] b |
350 | 5.0 | 1.5 | 24% | before completeness corr. | |
350 | 20 | 0.63 | 10% | Oliver et al. (2010) | [resolved sources] |
350 | 20 | 0.77 | 12% | Béthermin et al. (2012) | [resolved sources] |
350 | 2.0 | 4.50 | 70% | Béthermin et al. (2012) | [using stacking] |
|
|||||
500 | 9.0 | 0.37 | 13% | after completeness corr. | 2.80 [–0.81;+0.93] b |
500 | 9.0 | 0.30 | 11% | before completeness corr. | |
500 | 20 | 0.15 | 5% | Oliver et al. (2010) | [resolved sources] |
500 | 20 | 0.14 | 5% | Béthermin et al. (2012) | [resolved sources] |
500 | 2.0 | 1.54 | 55% | Béthermin et al. (2012) | [using stacking] |
Notes. The percentages correspond to the fractions of the IGL with respect to the total extrapolated estimations of the CIRB reported by (a)Berta et al. (2011) and by (b)Béthermin et al. (2012). The new flux limits Slim in the PACS bands are similar to Elbaz et al. (2011) but the SPIRE depths are deeper.
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