Table 2
Magphys results from the SED fitting.
| Region | log LIR | SFR | sSFR | log M∗ | log Md | τ V | T cold | ξ cold | T warm | ξ warm | ξ hot | ξ PAH | f μ | |
| (L⊙) | (M⊙ yr-1) | (Gyr-1) | (M⊙) | (M⊙) | (K) | (K) | ||||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | |
|
|
||||||||||||||
| Entire host |
|
|
0.53 |
|
|
0.16 |
|
|
|
|
|
|
|
|
| WR region |
|
|
2.37 |
|
|
0.47 |
|
|
|
|
|
|
|
|
| % | 25 | 7 | ··· | 2 | 5 | ··· | ··· | ··· | ··· | ··· | ··· | ··· | ··· | |
| Host-WR |
|
|
0.27 |
|
|
0.10 |
|
|
|
|
|
|
|
|
Notes. (1) The entire host galaxy/only the WR region/percentage contribution of the WR region to the cumulative properties of the galaxy/the host with WR fluxes subtracted. (2) 8 − 1000 μm infrared luminosity. (3) Star formation rate from SED modelling. (4) Specific star formation rate (≡SFR/M∗). (5) Stellar mass. (6) Dust mass. (7) Average V-band optical depth (AV = 1.086τV). (8) Temperature of the cold dust component. (9) Contribution of the cold component to the infrared luminosity. (10) Temperature of the warm dust component. (11) Contribution of the warm component to the infrared luminosity. (12) Contribution of the hot (130–250 K, mid-IR continuum) component to the infrared luminosity. (13) Contribution of the PAH component to the infrared luminosity. (14) Contribution of the ISM dust (as opposed to birth clouds) to the infrared luminosity.
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