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Table 1

Properties of the nine regions used in this analysis, in terms of effective sky fraction and column density based on dust opacity (see Sect. 3.5).

LR16 LR24 LR33 LR42 LR53 LR63N LR63 LR63S LR72
16 24 33 42 53 33 63 30 72
NH i 1.32 1.65 2.12 2.69 3.45 4.14 4.41 4.70 6.02
  ℓ range
PTEHM [%] 50–700 ......................... 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.2 0.0
50–160 ......................... 2.5 2.4 2.6 1.6 0.6 6.2 1.0 5.6 0.6
160–320 ......................... 15.0 5.9 1.1 6.3 7.8 2.1 7.2 39.9 5.0
320–500 ......................... 93.3 68.5 59.8 34.1 49.4 36.5 43.4 59.2 40.2
500–700 ......................... ... 54.3 47.0 30.7 33.2 41.4 27.8 36.0 21.4
PTEDS [%] 50–700 ......................... 0.0 0.0 1.5 0.2 0.0 0.1 0.1 0.7 0.0
50–160 ......................... 1.7 1.6 10.8 3.0 1.6 11.2 3.2 6.2 4.0
160–320 ......................... 29.9 46.5 46.4 42.7 16.3 11.5 14.8 47.4 21.7
320–500 ......................... ... 84.9 72.8 54.4 42.8 19.2 41.9 73.5 39.4
500–700 ......................... ... ... 48.6 34.6 36.6 61.1 24.5 18.1 18.6

Notes. The PTE values obtained for each multipole bin and sky region are given for the HM and DS cases. They are defined as the probability of obtaining correlation ratios smaller than the Planck measurements, based on 1000 simulations with dust plus CMB signals and Gaussian noise, and expressed as a percentage. The PTE values are absent when the data ratio becomes imaginary (see Eq. (1)).

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