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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 = out∕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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