Table 1. Open in new tab AGNs and their...

Name	D	Hubble	Spectral	log M_BH	\|$\log {L_{[\rm O\,{\small IV}]}}$\|	\|$\log {L_{[\rm Ne\,{\small V}]}}$\|	log L_12 μm	\|$\log {L_{[\rm O\,{\small III}], corr}}$\|	log L_IR
ESO 121-G6	14.5	Sc	H ii	6.10	39.04	38.21	40.28^c	–	9.70
NGC 660	12.3	Sa	L	7.35	39.71	38.85	41.18^c	40.03	10.49
NGC 3486	9.2	Sc	S2	6.50^a	38.53	37.71^b	<40.10^d	38.19^f	9.31
NGC 5195	8.3	Irr	L	7.31	37.89	37.22	<41.90^e	37.12	9.50

Name

Hubble

Spectral

log M_BH

|$\log {L_{[\rm O\,{\small IV}]}}$|

|$\log {L_{[\rm Ne\,{\small V}]}}$|

log L_12 μm

|$\log {L_{[\rm O\,{\small III}], corr}}$|

log L_IR

(Mpc)

type

class

(M_⊙)

(erg s⁻¹)

(L_⊙)

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

(9)

(10)

ESO 121-G6

14.5

H ii

6.10

39.04

38.21

40.28^c

–

9.70

NGC 660

12.3

7.35

39.71

38.85

41.18^c

40.03

10.49

NGC 3486

9.2

6.50^a

38.53

37.71^b

<40.10^d

38.19^f

9.31

NGC 5195

8.3

Irr

7.31

37.89

37.22

<41.90^e

37.12

9.50

Name	D	Hubble	Spectral	log M_BH	\|$\log {L_{[\rm O\,{\small IV}]}}$\|	\|$\log {L_{[\rm Ne\,{\small V}]}}$\|	log L_12 μm	\|$\log {L_{[\rm O\,{\small III}], corr}}$\|	log L_IR
ESO 121-G6	14.5	Sc	H ii	6.10	39.04	38.21	40.28^c	–	9.70
NGC 660	12.3	Sa	L	7.35	39.71	38.85	41.18^c	40.03	10.49
NGC 3486	9.2	Sc	S2	6.50^a	38.53	37.71^b	<40.10^d	38.19^f	9.31
NGC 5195	8.3	Irr	L	7.31	37.89	37.22	<41.90^e	37.12	9.50

Table 1.

Open in new tab

AGNs and their basic properties.

Name	D	Hubble	Spectral	log M_BH	\|$\log {L_{[\rm O\,{\small IV}]}}$\|	\|$\log {L_{[\rm Ne\,{\small V}]}}$\|	log L_12 μm	\|$\log {L_{[\rm O\,{\small III}], corr}}$\|	log L_IR
	(Mpc)	type	class	(M_⊙)	(erg s⁻¹)	(erg s⁻¹)	(erg s⁻¹)	(erg s⁻¹)	(L_⊙)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
ESO 121-G6	14.5	Sc	H ii	6.10	39.04	38.21	40.28^c	–	9.70
NGC 660	12.3	Sa	L	7.35	39.71	38.85	41.18^c	40.03	10.49
NGC 3486	9.2	Sc	S2	6.50^a	38.53	37.71^b	<40.10^d	38.19^f	9.31
NGC 5195	8.3	Irr	L	7.31	37.89	37.22	<41.90^e	37.12	9.50

Name	D	Hubble	Spectral	log M_BH	\|$\log {L_{[\rm O\,{\small IV}]}}$\|	\|$\log {L_{[\rm Ne\,{\small V}]}}$\|	log L_12 μm	\|$\log {L_{[\rm O\,{\small III}], corr}}$\|	log L_IR
	(Mpc)	type	class	(M_⊙)	(erg s⁻¹)	(erg s⁻¹)	(erg s⁻¹)	(erg s⁻¹)	(L_⊙)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
ESO 121-G6	14.5	Sc	H ii	6.10	39.04	38.21	40.28^c	–	9.70
NGC 660	12.3	Sa	L	7.35	39.71	38.85	41.18^c	40.03	10.49
NGC 3486	9.2	Sc	S2	6.50^a	38.53	37.71^b	<40.10^d	38.19^f	9.31
NGC 5195	8.3	Irr	L	7.31	37.89	37.22	<41.90^e	37.12	9.50

Notes. Column (1) Galaxy name; (2) distance in Mpc; (3) Hubble classification of the host galaxy – S: Seyfert, L: LINER, and H ii: H ii region; (4) optical spectral class on the basis of emission line diagnostic diagrams (e.g. Kewley et al. 2001); (5) black hole mass relative to the mass of the Sun, M_⊙; (6)–(9) [O iv], [Ne v], 12 μm continuum, and [O iii] (corrected for the Balmer decrement) luminosities in units of erg s⁻¹, respectively; (10) total IR luminosity relative to the luminosity of the Sun, L_⊙. All data are taken from Goulding & Alexander (2009) or Goulding et al. (2010), unless indicated by additional references.

References. ^aMcKernan, Ford & Reynolds (2010); ^bpredicted from the [O iv]:[Ne v] luminosity relationship derived by Goulding & Alexander (2009); ^cthis work; ^dhigh-angular resolution 12 μm luminosity from Asmus et al. (2014); ^eWISE 12 μm luminosity; ^fHo, Filippenko & Sargent (1997).

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