Planck early results
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Fig.5

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The Planck ERCSC flux density limit quantified as the faintest ERCSC source at |b| < 10° (dashed black line) and at |b| > 30° (solid black line) is shown relative to other wide area surveys. Also shown are the spectra of known sources of foreground emission as red lines; these include a Sν ~ ν-0.7 synchrotron component, ν-0.1 free-free component, a Rayleigh-Jeans component and a ν2 emissivity blackbody of temperature 18K. The ERCSC sensitivity is worse in the Galactic plane due to the strong contribution of ISM emission especially at submillimetre wavelengths. In the radio regime, the effect is smaller. The faintest WMAP 7 year 5σ sources are derived from the catalogue of Gold et al. (2011); Wright et al. (2009). Although the flux density limits of WMAP and Planck appear to be comparable at the lowest frequencies, the Planck ERCSC is more complete as discussed in Sect. 4. The GB6 sensitivity value is from Gregory et al. (1996), AT20G flux limit from Murphy et al. (2010), SCUBA-2 All Sky Survey (SASSy) limit from the Joint Astronomy Center website while the IRAS flux density limits are from the IRAS explanatory supplement (Beichman et al. 1988).

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