Table 1.

Summary of main parametric signal models for the temperature analysis.

Component Free parameters Spectral energy density, sν [ μKRJ] Additional information
and priors
CMB aCMB ∼ Uni(−∞,∞) g(ν)  =  (exp(x)−1)2/(x2exp(x)) TCMB = 2.7255 K
sCMB  =  aCMB/g(ν)
TCMB  =  2.7255K
Relativistic CMB g(ν)  =  (exp(x)−1)2/(x2exp(x)) βsun  =  1.2343  ×  10−3
quadrupole 𝒬(ν)  =  (x/2)(exp(x)+1)/(exp(x)−1)
squad  =  aquad 𝒬(ν)/g(ν)
as ∼  Uni(−∞,∞)
Synchrotron βs ∼  N(−3.3 ± 0.1), ν0, s 30 GHz
fullsky C = 0, low signal-to-noise
aff ∼  Uni(−∞,∞) ν0, ff 40.0 GHz
Free-free Te =  7000 K, gff log T4Te/104
fullsky ν9ν/(109 Hz)
e Euler’s number
AME/ aame ∼  Uni(−∞,∞) ν0, ame= 22.0 GHz
spinning dust νp ∼  N(22 ± 3 GHz), νp0= 30.0 GHz
fullsky fame(ν) = External template
ad ∼  Uni(−∞,∞)
Thermal dust βd ∼  N(1.56 ± 0.03), Td=NPIPE template
fullsky ν0, d  =  545 GHz
Radio sources asrc >  0 ν0, src =  30 GHz
αsrc ∼  N(−0.1 ± 0.3) UmJy(ν0, src) = Unit conversion

Notes. The symbol “∼” implies that the respective parameter has a prior as given by the right-hand side distribution; Uni denotes a uniform distribution within the indicated limits; N(μ, σ2) denotes a (normal) Gaussian distribution with the indicated mean and variance; and ai denotes the component amplitude of component i at the given reference frequency ν0, i, and si is spectral energy density, i.e., the observed signal at a given frequency, ν.

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