Table 3
Star formation rates for M 31, derived from synthetic broad band fluxes from our model SED.
| Band | SFR [M⊙ yr-1] | Recipe |
|
|
||
| FUV | 0.24 | a, b |
| NUV | 0.31 | a, b |
| 24 μm | 0.23 | c |
| 70 μm | 0.19 | d |
| TIR (3−1000 μm) | 0.92 | a, b |
| FUV + 24 μm | 0.31 | e |
Notes. For the FUV and NUV estimates, the intrinsic UV fluxes were used to avoid the problem of dust extinction. Conversions are based on the Kroupa & Weidner (2003) initial mass function. (a) Murphy et al. (2011); (b) Hao et al. (2011); (c) Rieke et al. (2009); (d) Calzetti et al. (2010); (e) Leroy et al. (2008).
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