Table 1
SFR estimators.
| Monochromatic | ||||||||
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| Band | log Cband | k | Method | Reference | ||||
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| FUV | −36.355 | 1.0000 | Theoreticala | 1 | ||||
| Hα | −34.270 | 1.0000 | Theoreticala | 1 | ||||
| 24 μm | −29.134 | 0.8104 | Hαb | 2 | ||||
| 70 μm | −29.274 | 0.8117 | Hαb | 3 | ||||
| 100 μm | −37.370 | 1.0384 | Hαb | 3 | ||||
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| Hybrid | ||||||||
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| Band | log Cband1 | kband1−band2 | Method | Reference | ||||
|
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| Hα+24 μm | −34.270 | 0.031 | Hα | 2 | ||||
| FUV+24 μm | −36.355 | 6.175 | Hα+24 μm | 4 | ||||
Notes. Monochromatic: log ΣSFR = log Cband + k × log Sband; hybrid: log ΣSFR = log Cband1 + log [Sband1 + kband1−band2 × Sband2], with ΣSFR in M⊙ yr-1 kpc-2, S defined as νSν in W kpc-2, and C in M⊙ yr-1 W-1. Empirical estimators were calibrated on individual star-forming regions on typical scales of the order of ~200−500 pc.
Based on Starburst99 (Leitherer et al. 1999).
Extinction corrected, calibrated against near-infrared hydrogen recombinations lines (e.g., Paα or Brγ).
Reference. (1) Murphy et al. (2011); (2) Calzetti et al. (2007); (3) Li et al. (2013); (4) Leroy et al. (2008).
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