Table 4.
Herschel/SPIRE shot-noise levels as measured from CIB anisotropies and predicted using the integral of the number counts as modelled by Béthermin et al. (2012a).
| Wavelength | Flux limit (1) | Measured (1) | Predicted | Predicted | Flux limit (2) | Measured (2) | Predicted | Predicted |
|---|---|---|---|---|---|---|---|---|
| point source | extended | point source | extended | |||||
| [μm] | [mJy] | [Jy2 sr−1] | [Jy2 sr−1] | [Jy2 sr−1] | [mJy] | [Jy2 sr−1] | [Jy2 sr−1] | [Jy2 sr−1] |
| 250 | 300 | 8.2 × 103 | 9983 | 9485 | 600 | < 7063 | 11033 | 10455 |
| 350 | 300 | 5.8 × 103 | 5631 | 5122 | 600 | 4571 | 5929 | 5386 |
| 500 | 300 | 2.3 × 103 | 2193 | 1745 | 600 | 1518 | 2262 | 1799 |
Notes. Values for the shot noise are given in the photometric convention νIν = cst, obtained using either the point source or the extended emission RSRF (see text for more details). Flux limits are coming from CIB power spectra analyses and are much higher than SPIRE sensitivity.
From Viero et al. (2013).
From Serra et al. (2016).
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