Planck 2018 results
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Table 14.

Dust-plus-CIB contamination level (in μK2) at each frequency, for different Galactic masks.

Frequencies [GHz] G70 G60 G50 G41 CIB
100 × 100 … 8.8 ± 1.7 4.3 ± 1.1 2.56 ± 0.88 1.61 ± 0.83 0.17 ± 0.023
143 × 143 … 25.7 ± 3.9 11.3 ± 2.2 6.5 ± 1.6 4.7 ± 1.6 0.75 ± 0.10
217 × 217 … 309.4 ± 39.9 151.7 ± 21.7 99.8 ± 16.0 73.9 ± 13.9 7.9 ± 1.1

(a)The levels reported in this table correspond to the amplitude of the dust-plus-CIB emission, 𝒟, at  = 200 in μK2. They are obtained at each frequency by fitting the 545 GHz cross-half-mission spectra against the CMB-corrected 545 × 100, 545 × 143, and 545 × 217 spectra over the range of multipoles 30 ≤  ≤ 500. The CMB correction is obtained using the 2015 CMB best-fit. This contamination is dominated by dust, with a small CIB contribution. The columns labelled with a Galactic mask name (G41, G50, G60, and G70) correspond to the results when combining those masks with the CO, extended-source, and frequency point-source mask specific to each frequency. The CIB contribution is shown in the last column. This is calculated in an iterative way, estimating the CIB amplitude at  = 3000 in the 217 × 217 spectrum from a full Markov chain Monte Carlo (MCMC) estimation of cosmological parameters in an ΛCDM model; the CIB contributions at different frequencies at  = 200 used here are then inferred using the spectral energy distribution and multipole templates described in Sect. 3.3.1.

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