Planck 2018 results
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Table 12.

Main characteristics of HFI full-mission maps.

Reference Frequency (GHz)(a1)
Quantity 100 143 217 353 545 857 Notes
Number of bolometers......... 8 11 12 12 3 4 a2
Effective beam solid angle Ω [arcmin2]......... 106.22 60.44 28.57 27.69 26.44 24.37 b1
Error in solid angle σΩ [arcmin2]......... 0.14 0.04 0.04 0.02 0.02 0.02 b2
Spatial variation (rms) ΔΩ [arcmin2]......... 0.20 0.20 0.19 0.20 0.21 0.12 b3
Effective beam FWHM1 [arcmin]......... 9.68 7.30 5.02 4.94 4.83 4.64 b4
Effective beam FWHM2 [arcmin]......... 9.66 7.22 4.90 4.92 4.67 4.22 b5
Effective beam ellipticity ϵ......... 1.186 1.040 1.169 1.166 1.137 1.336 b6
Variation (rms) of the ellipticity Δϵ......... 0.024 0.009 0.029 0.039 0.061 0.125 b7
expected for full-mission map sensitivity []......... 1.93 0.48 1.11 13.0 c1
[10−4kJy2 sr]......... 1.38 1.21 c1
map sensitivity from the 2018 release []......... 1.52 0.36 0.78 11.6 c2
[10−4kJy2 sr]......... 2.9–8 2.7–8 c3
map expected sensitivity from TOI white noise []..... 5.01 2.70 2.77 51.1 c1
map sensitivity from the 2018 release []......... 2.94 1.61 3.25 7.0 c2
Dipole absolute calibration accuracy [%]......... 0.008 0.021 0.028 0.024 ≃1 d1
Planet submm intercalibration accuracy [%]......... ≃3 d2
Intensity transfer function uncertainty (700 <   <  1000) [%]......... Ref. 0.12 0.36 0.78 4.3 d3
Polarization efficiency residual errors [%]......... 0.7 −1.7 1.9 d4
Galactic emission zero level uncertainty [MJy sr−1]......... 0.0008 0.0010 0.0024 0.0067 0.0165 0.0147 e1
CIB monopole assumption [MJy sr−1]......... 0.0030 0.0079 0.033 0.13 0.35 0.64 e2
CIB monopole uncertainty [%]......... 100 100 40 20 20 20 e3
Zodiacal emission monopole level [μKCMB]......... 0.43 0.94 3.8 34 e4
[MJy sr−1]......... 0.04 0.12 e4

Notes. (a1)Channel-map reference frequency, and channel identifier. (a2)Number of bolometers whose data were used in producing the channel map. At 353 GHz, only eight PSBs are used for polarization maps. (b1)Mean value over bolometers at the same frequency. (b2)As given by simulations. (b3)Variation (rms) of the solid angle across the sky. (b4)FWHM of the Gaussian whose solid angle is equivalent to that of the effective beams. (b5)Mean FWHM of the elliptical Gaussian fit. (b6)Ratio of the major to minor axis of the best-fit Gaussian averaged over the full sky. (b7)Variability (rms) on the sky. (c1)Estimate of the C map noise for the full mission, derived from the TOI white noise (see Sect. 2.1), (Table 5 of Planck Collaboration VII 2016). (c2)Estimate of the C map noise for the full mission, derived from the odd-even ring null-test noise (Fig. 17, multipole range  = 200–1000). (c3)Estimate of the C map noise for the full mission, derived from the odd-even ring null-test noise (Fig. 13, multipole range  = 200–2000). (d1)Absolute calibration accuracy from simulations with the Solar dipole (Table 7). The 545 GHz channel retains the 2015 planet calibration, and the accuracy is calculated a posteriori on the Solar dipole. (d2)The 857 GHz channel retains the 2015 planet calibration, and the accuracy is calculated a posteriori using the planet model (Planck Collaboration Int. LII 2017) and the 545 GHz data. (d3)Derived upper limits of the transfer function on the first three acoustic peaks (Table 8). (d4)The polarization efficiencies residual errors exceed somewhat the estimated uncertainty (1%). These are a posteriori tests, and have not been applied to the maps, but taken into account in the likelihoods (Table 9). (e1)The monopoles of the maps are built using a Galactic dust model extrapolated to a zero level for H I. Uncertainties are discussed in Planck Collaboration VIII (2014) and presented in Table 5 of that paper. (e2)The monopole of the Béthermin et al. (2012) CIB model (Table 6 of Planck Collaboration VIII (2016)). (e3)The CIB uncertainties are estimated by combining the absolute measurements of FIRAS (Puget et al. 1996; Fixsen et al. 1998) and the anisotropies from Planck HFI (Planck Collaboration XXX 2014), assuming the same SED for the absolute value and the anisotropies. (e4)Monopole contribution of the zodiacal emission, adjusted for high Galatic and ecliptic latitudes (Table 6 of Planck Collaboration VIII 2016).

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