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Table C.1

Best-fit parameters obtained for each galaxy, using an all-components model and the model where the AME component is excluded.

Parameters All components model No AME model
LMC SMC M31 M33 NGC 253 NGC 4945 LMC SMC M31 M33 NGC 253 NGC 4945
β 1.29 ± 0.18 0.86 ± 0.27 1.52 ± 0.15 0.98 ± 0.37 1.61 ± 0.34 1.37 ± 0.72 1.28 ± 0.18 0.84 ± 0.28 1.59 ± 0.14 1.12 ± 0.37 1.68 ± 0.31 1.49 ± 0.72
log10353) −5.19 ± 0.05 −5.70 ± 0.08 −5.50 ± 0.04 −6.15 ± 0.10 −6.54 ± 0.07 −6.33 ± 0.23 −5.19 ± 0.06 −5.69 ± 0.08 −5.50 ± 0.04 −6.14 ± 0.10 −6.53 ± 0.06 −6.35 ± 0.24
Td(K) 24.4 ± 2.33 27.3 ± 4.34 18.5 ± 1.17 24.2 ± 4.69 24.9 ± 3.97 24.7 ± 7.41 24.4 ± 2.31 27.6 ± 4.74 18.1 ± 1.07 22.9 ± 4.21 24.1 ± 3.38 23.9 ± 6.94
EM (pc cm−6) 27.9 ± 23.0 23.02 ± 6.98 4.75 ± 3.06 1.81 ± 1.38 2.78 ± 2.12 5.31 ± 3.36 34.3 ± 24.9 30.1 ± 3.63 7.08 ± 2.59 3.34 ± 1.55 4.84 ± 1.99 6.21 ± 3.22
Csyn 563 ± 47.1 43.2 ± 6.72 9.18 ± 0.83 3.45 ± 0.17 6.93 ± 0.34 7.21 ± 1.53 555 ± 51.0 37.3 ± 4.66 8.61 ± 0.71 3.29 ± 0.19 6.59 ± 0.32 7.00 ± 1.54
αsyn −0.49 ± 0.04 −1.14 ± 0.14 −0.67 ± 0.07 −0.91 ± 0.16 −0.81 ± 0.07 −0.81 ± 0.18 −0.49 ± 0.05 −1.27 ± 0.13 −0.70 ± 0.07 −1.06 ± 0.25 −0.89 ± 0.08 −0.79 ± 0.19
δCMB(μK) 64.7 ± 11.7 25.8 ± 10.4 19.9 ± 2.91 5.07 ± 4.06 5.15 ± 1.25 −34.74 ± 4.54 62.5 ± 11.6 22.2 ± 10.2 21.4 ± 2.46 6.63 ± 3.29 5.21 ± 1.20 −33.58 ± 4.01
CAME 0.20 ± 0.21 0.34 ± 0.25 0.13 ± 0.08 0.11 ± 0.08 0.12 ± 0.08 0.23 ± 0.18
χ2 8.85 4.97 1.55 8.55 4.52 2.90 7.13 5.02 2.28 6.56 5.63 1.68
χr2$\chi_{\mathrm{r}}^{2}$ 0.80 0.38 0.16 0.57 0.45 0.6 0.59 0.36 0.21 0.44 0.51 0.14
εAME(μK /(MJy/sr)) 0.91 ± 0.97 5.96 ± 4.96 4.50 ± 2.94 9.00 ± 7.16 5.88 ± 3.98 10.47 ± 10.00
εAME(K/τ353) 3.85 ± 0.64 13.72 ± 3.47 5.94 ± 0.69 34.13 ± 10.70 86.67 ± 20.28 53.13 ± 33.20

Notes. The all-components model consists of thermal dust, free–free, synchrotron, and AME emission for the galaxy as well as CMB temperature fluctuations in the background. For this model, the AME emissivities deduced from the AME best fit parameter, both normalized by the 3000 GHz flux density and by the dust optical depth τ353, are also added.

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