Table 9
Outflows and nuclear SFR.
| Object | log SFR(IR)a | log SFR(1.4 GHz)b | logηc |  |
 |
|---|---|---|---|---|---|
| (M⊙ yr−1) | (M⊙ yr−1) | ||||
| I12112 SW | 1.12 | 1.57 | –0.02 | –0.65 | –1.4 |
| I12112 NE | 2.26 | 2.21 | 0.34 | –0.12 | –0.67 |
| I14348 SW | 2.14 | 2.36 | 0.26 | –0.28 | –0.91 |
| I14348 NE | 1.97 | 2.12 | –0.07 | –0.58 | –1.2 |
| I22491 E | 2.04 | 1.76 | 0.26 | –0.32 | –0.99 |
Notes. (a) SFR derived from the IR luminosity assigned to each nucleus (see Sect. 3.4.1) using the calibration of Kennicutt & Evans (2012). This is the adopted SFR for these nuclei. (b)SFR derived from the non-thermal radio continuum using the Murphy et al. (2011) SFR calibration (see Sect. 3.4.2). (c) Logarithm of the mass loading factor η = Ṁout∕SFR(IR). (d) Ratio between theoutflow momentum rate and the momentum injected by supernova explosions. We assume that the PSN per SN is 1.3 × 105 M⊙ km s−1 × (n0∕100 cm−3)−0.17 (Kim & Ostriker 2015) using n0 = 100 cm−3 and that the SN rate, νSN (yr−1), is 0.012 × SFR(IR) (M⊙ yr−1) for the adopted IMF (Leitherer et al. 1999). (e)Ratio between thetotal kinetic luminosity of the molecular outflow and that injected by supernova explosions (LSNe (erg s−1) = 9 × 1041 SFR(IR) (M⊙ yr−1); Leitherer et al. 1999, adapted for a Kroupa 2001 IMF).
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