Table A.3
P(3σ) probabilities and averaged p-values for the power law models, multi-component, and single component.
| Galaxy | Allp–law | Allmulti | Allsingle | PDRp–law | PDRmulti | PDRsingle | COp–law | COmulti | COsingle |
|---|---|---|---|---|---|---|---|---|---|
| Haro2 | 91.50 | 88.00 | 78.30 | 55.54 | 57.83 | 53.59 | 92.00 | 4.60 | 20.20 |
| (0.749) | (0.750) | (0.750) | (0.754) | (0.576) | (0.896) | (0.816) | (1.000) | (1.000) | |
| Haro3 | 74.20 | 81.6 | 71.70 | 68.62 | 75.62 | 79.07 | 86.20 | 35.05 | 3.90 |
| (0.750) | (0.750) | (0.747) | (0.583) | (0.414) | (0.334) | (0.010) | (0.571) | (0.994) | |
| Haro11 | 87.60 | 85.00 | 72.80 | 48.90 | 45.45 | 53.00 | 57.23 | 67.77 | 70.62 |
| (0.750) | (0.750) | (0.7500) | (0.478) | (0.515) | (0.720) | (0.752) | (0.390) | (0.811) | |
| He2-10 | 77.30 | 79.20 | 65.60 | 63.90 | 61.97 | 55.18 | 51.55 | 45.65 | 97.20 |
| (0.749) | (0.750) | (0.750) | (0.502) | (0.389) | (0.729) | (0.230) | (0.237) | (0.754) | |
| IIZw40 | 95.60 | 92.80 | 83.90 | 80.75 | 80.39 | 81.18 | 85.60 | 52.20 | 0.00 |
| (0.750) | (0.750) | (0.750) | (0.415) | (0.383) | (0.565) | (0.080) | (0.162) | (1.000) | |
| IZw18 | 93.00 | 89.00 | 80.70 | 79.64 | 68.56 | 79.68 | 87.75 | 90.95 | 0.00 |
| (0.700) | (0.702) | (0.750) | (0.629) | (0.724) | (0.615) | (0.150) | (0.756) | (1.000) | |
| Mrk209 | 86.80 | 80.60 | 78.70 | 79.18 | 79.53 | 81.26 | 71.50 | 0.00 | 0.00 |
| (0.744) | (0.750) | (0.750) | (0.559) | (0.454) | (0.460) | (0.318) | (1.000) | (1.000) | |
| Mrk930 | 98.70 | 99.30 | 99.3 | 90.53 | 87.08 | 87.08 | 99.95 | 100.0* | 100.0* |
| (0.750) | (0.750) | (0.750) | (0.371) | (0.576) | (0.576) | (0.950) | (1.000) | (1.000) | |
| Mrk1089 | 88.00 | 84.30 | 79.30 | 64.35 | 67.25 | 63.31 | 76.30 | 55.15 | 57.70 |
| (0.750) | (0.746) | (0.658) | (0.358) | (0.384) | (0.614) | (0.559) | (0.842) | (0.421) | |
| NGC1140 | 77.4 | 81.70 | 75.20 | 61.21 | 65.66 | 66.12 | 53.35 | 58.25 | 0.55 |
| (0.742) | (0.704) | (0.748) | (0.567) | (0.486) | (0.615) | (0.165) | (0.129) | (0.997) | |
| NGC1569 | 76.40 | 74.60 | 74.60 | 49.02 | 51.26 | 51.26 | 82.70 | 98.80 | 98.80 |
| (0.750) | (0.750) | (0.750) | (0.403) | (0.678) | (0.678) | (0.396) | (0.940) | (0.940) | |
| NGC1705 | 87.60 | 84.70 | 84.70 | 99.95 | 100.0 | 100.0 | 45.94 | 45.37 | 45.37 |
| (0.740) | (0.750) | (0.750) | (0.981) | (1.000) | (1.000) | (0.433) | (0.430) | (0.430) | |
| NGC5253 | 80.10 | 82.30 | 79.40 | 97.40 | 72.65 | 67.95 | 65.23 | 62.55 | 58.12 |
| (0.750) | (0.750) | (0.750) | (0.204) | (0.463) | (0.128) | (0.624) | (0.429) | (0.577) | |
| NGC625 | 70.90 | 70.90 | 64.10 | 41.88 | 44.4 | 44.96 | 52.20 | 10.25 | 0.00 |
| (0.749) | (0.749) | (0.750) | (0.777) | (0.705) | (0.785) | (0.828) | (0.999) | (1.000) | |
| SBS0335-052 | 70.60 | 77.20 | 74.40 | 79.13 | 82.56 | 82.90 | 100.0* | 100.0* | 100.0* |
| (0.749) | (0.750) | (0.725) | (0.543) | (0.397) | (0.590) | (0.500) | (0.500) | (0.500) | |
| UM448 | 78.80 | 88.30 | 80.30 | 71.33 | 79.83 | 61.11 | 69.25 | 91.5 | 64.15 |
| (0.750) | (0.750) | (0.698) | (0.754) | (0.345) | (0.603) | (0.200) | (0.448) | (0.896) | |
| UM461 | 90.70 | 88.8 | 88.8 | 82.83 | 83.22 | 83.22 | 100.0* | 100.0* | 100.0* |
| (0.734) | (0.750) | (0.750) | (0.385) | (0.615) | (0.615) | (0.500) | (0.500) | (0.500) | |
| VIIZw403 | 92.5 | 95.00 | 72.90 | 86.67 | 88.46 | 83.47 | 100.0* | 100.0* | 100.0* |
| (0.748) | (0.742) | (0.731) | (0.546) | (0.569) | (0.610) | (0.499) | (0.500) | (0.500) |
Notes. P(3σ) represents the probability that the inferred value from MCMC sampling fall within 3σ from the observed value. We report P(3σ) as averaged percentages for all lines, PDR lines, and the CO(1–0) line alone. We provide averaged values for the following PDR lines: [C II] 158 µm, [Si II] 34 µm, [O I] 63 µm, [O I] 145 µm, [Fe II]17 µm, and [Fe II] 25 µm. P(3σ) below 50% are shown in bold and below 25% in red. The averaged p-values are reported between parenthesis; they should ideally be close to 0.5. Very low p-value (near 0) or very high (near 1) can be used to identify overfitting or underfitting.(*): P(3σ)= 100% correspond to observed upper limits which are well matched by the models.
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