Table 1
PCCS characteristics.
Channel | ||||||||||
|
||||||||||
30 | 44 | 70 | 100 | 143 | 217 | 353 | 545 | 857 | ||
|
||||||||||
Frequency [GHz] ...................... | 28.4 | 44.1 | 70.4 | 100.0 | 143.0 | 217.0 | 353.0 | 545.0 | 857.0 | |
Wavelength, λ [μm] ...................... | 10 561 | 6807 | 4260 | 3000 | 2098 | 1382 | 850 | 550 | 350 | |
Beam FWHMa [arcmin] ...................... | 32.38 | 27.10 | 13.30 | 9.65 | 7.25 | 4.99 | 4.82 | 4.68 | 4.33 | |
Pixel size [arcmin] ...................... | 3.44 | 3.44 | 3.44 | 1.72 | 1.72 | 1.72 | 1.72 | 1.72 | 1.72 | |
S/N thresholds: | ||||||||||
Full sky ................. | 4.0 | 4.0 | 4.0 | 4.6 | 4.7 | 4.8 | ... | ... | ... | |
Extragalactic zoneb ................. | ... | ... | ... | ... | ... | ... | 4.9 | 4.7 | 4.9 | |
Galactic zoneb ................. | ... | ... | ... | ... | ... | ... | 6.0 | 7.0 | 7.0 | |
Full sky ................. | 1256 | 731 | 939 | 3850 | 5675 | 16 070 | 13 613 | 16 933 | 24 381 | |
| b | > 30deg ................. | 572 | 258 | 332 | 845 | 1051 | 1901 | 1862 | 3738 | 7536 | |
N( >S)c: | ||||||||||
Full sky ................. | 934 | 535 | 689 | 3425 | 5229 | 15 107 | 13 184 | 15 781 | 23 561 | |
| b | > 30deg ................. | 373 | 151 | 191 | 629 | 857 | 1409 | 1491 | 2769 | 6773 | |
| b | ≤ 30deg ................. | 561 | 384 | 498 | 2796 | 4422 | 13 698 | 11 693 | 13 012 | 16 788 | |
Flux densities: | ||||||||||
Minimumd [mJy] ................. | 461 | 825 | 566 | 266 | 169 | 149 | 289 | 457 | 658 | |
90% completeness [mJy] ................. | 575 | 1047 | 776 | 300 | 190 | 180 | 330 | 570 | 680 | |
Uncertainty [mJy] ................. | 109 | 198 | 149 | 61 | 38 | 35 | 69 | 118 | 166 | |
Position uncertaintye [arcmin] ................. | 1.8 | 2.1 | 1.4 | 1.0 | 0.7 | 0.7 | 0.8 | 0.5 | 0.4 |
Notes.
FEBeCoP band-averaged effective beam. This table shows the
exact values that were adopted for the PCCS. For HFI channels, these are the FWHM of
the mean best-fit Gaussian. For the LFI channels, we use
,
where Ωeff is
the FEBeCoP band-averaged effective solid angle (see Planck Collaboration IV 2014 and Planck Collaboration VII 2014 for a full
description of the Planck beams). When we constructed the PCCS for
the LFI channels we used a value of the effective FWHM slightly different (by
≪1%) than the final
value specified in the Planck Collaboration IV
(2014) paper. This small correction will be made in later versions of the
catalogue.
The Galactic and extragalactic zones are defined in Sect. 2.3.
Minimum flux density of the catalogue at | b | > 30deg after excluding the faintest 10% of sources.
Positional uncertainty (median value) derived by comparison with PACO sample (Massardi et al. 2011; Bonavera et al. 2011; Bonaldi et al. 2013) up to 353 GHz and with Herschel samples in the other channels (see Sect. 3.2.3 for more details).
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