A plausible link between dynamically unsettled molecular gas and the radio jet in NGC 6328

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Table C.1.

Outflow and AGN properties of galaxies with molecular outflows

Galaxy	z	V_out	Ṁ_out	log(L_AGN)	F_1.4GHz	log(P_jet)
		km s⁻¹	M_⊙ yr⁻¹	erg s⁻¹	Jy	erg s⁻¹
NGC1377	0.00578	110	5	42.93	< 0.0015 ¹	< 42.46
NGC1068	0.00379	150	28	43.94	4.85 ²	43.56
4C12.50	0.1217	800 ³	652 ³	45.7	5.1⁴	44.62 ^*
NGC1433	0.0036	100	0.7	42.24	0.0034 ⁵	42.45
Mrk231	0.04217	700	350	45.72	0.31⁴	...
IC5063	0.011	300	10	44.3	1.87 ²	43.74
M51	0.002	100	11	43.79	1.4 ⁶	43.17 ^**
Mrk1014	0.16311	268	93	45.29	0.0225 ¹	43.84
NGC1266	0.00719	177	11	43.31	0.115 ⁴	43.18
NGC5643	0.003999	500	85	42.91	0.203⁷	42.96
IRASF08572+3915	0.04311	800	403	45.72	0.0049 ¹	...
IRASF10565+2448	0.189	450	100	44.81	0.0576 ¹	...
IRASF11119+3257	0.06438	1000	203	46.2	0.106 ⁸	43.77
IRASF23365+3604	0.02448	450	57	44.67	0.0287 ⁴	...
NGC6240	0.123	400	267	45.38	0.427²	...
SDSSJ1356+1026	0.04256	500	118	46	0.49⁹	...
IRAS05189-2524	0.007268	491	219	44.47	0.0291 ¹	...
NGC4418	0.06764	134	19	43.81	0.0414⁴	...
IRASF14378-3651	0.030761	425	180	45.12	0.0349 ¹	...
IRAS13120-5453	0.08257	549	1115	44.35	0.065 ²	...
IRASF14348-1447	0.04295	450	420	44.59	0.018 ¹⁰¹¹	...
NGC613	0.00495	300 ¹²	19 ¹²	42.6 ¹³	0.223 ²	43.18
ESO420-613	0.01205	379 ¹⁴	14 ¹⁴	44.0 ¹⁴	0.1 ¹⁴	43.25
PKS1549-79	0.15	600 ¹⁵	1733 ¹⁵	44.7 ²⁵	5.36 ¹⁶	44.69
3C273	0.15834	245 ²⁴	439 ²⁴	46.06 ²⁶	55 ¹	45.06 ^***
HE1353-1917	0.03502	145 ¹⁷	22 ¹⁷	43.42 ¹⁸	0.0128 ¹
NGC6764	0.00807	170	1	42.23	0.113 ¹⁹	43.15
Circinus	0.0014	150	1	43.57	1.2 ²	42.89
Mrk273	0.03777	620	200	44.16	0.145 ¹	43.62
NGC3256S	0.00926	1400²¹	19 ²¹	42.04 ²⁰	0.0168 ^****	42.97
NGC3100	0.0088	200 ²²	0.12 ²²	42.78 ²²	0.5 ²³	43 ²²
NGC6328	0.014	150	3.1	42.11	0.32	42.35

Notes. are from Allison et al. (2014), unless otherwise indicated. For 4C12.50, properties are presented for the nuclear outflow component, as the extended components add little to the energetics (Fotopoulou et al. 2019). Likewise, the infrared luminosity fraction of the southern nucleus comes from resolved SF rates (Lira et al. 2002). The radio power, P_jet, (for the sources with a certain radio jet detection) is calculated as in Bîrzan et al. (2008) after the subtraction of the starburst contribution, as indicated in the text. Alternative radio power (P_jet) computations are as follows:

43.96 for the synchrotron radiation (Fotopoulou et al. 2019),

^**

39.3 for the X-ray cavity (Urquhart et al. 2018), and

^***

an averaged value of 43.86 Punsly & Kharb (2016).

^****

To find the 1.4GHz flux fraction assigned to the southern nucleus of this galaxy merger, we used the information from spatially resolved 5 GHz data (Neff et al. 2003).

Condon et al. (1998).

Allison et al. (2014).

Fotopoulou et al. (2019).

⁴

Baan & Klöckner (2006).

⁵

Ryder et al. (1996).

⁶

Dumas et al. (2011).

⁷

Condon et al. (1996).

⁸

Urrutia et al. (2009).

⁹

Greene et al. (2012).

¹⁰

Clemens et al. (2008).

¹¹

Clemens et al. (2010).

¹²

Audibert et al. (2019).

¹³

Davies et al. (2017).

¹⁴

Fernández-Ontiveros et al. (2020).

¹⁵

Oosterloo et al. (2019).

¹⁶

Drake et al. (2004).

¹⁷

Husemann et al. (2019a).

¹⁸

Shimizu et al. (2017).

¹⁹

Marvil et al. (2015).

²⁰

Ohyama et al. (2015).

²¹

Sakamoto et al. (2014).

²²

Ruffa et al. (2022).

²³

Ruffa et al. (2019b).

²⁴

Husemann et al. (2019b).

²⁵

Lanz et al. (2016).

²⁶

Gruppioni et al. (2016)

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