Table 1
The sample.
Name | RA | Dec | cza | DLb | Spectral | [N ii]/Hαd | Ref.e | log LIRf | LAGN/LIRg |
(J2000.0) | (J2000.0) | (km s-1) | (Mpc) | classc | (L⊙) | ||||
|
|||||||||
NGC 23 | 00 09 53.4 | +25 55 27 | 4478 | 64.7 | composite | 0.57 | 1 | 11.0 | 0.02 |
MCG +12-02-001 | 00 54 04.0 | +73 05 05 | 4722 | 68.3 | H ii | 0.42 | 1 | 11.4 | <0.05 |
NGC 876 | 02 17 53.2 | +14 31 19 | 3916 | 56.5 | composite | 0.57 | 2 | 10.4 | ··· |
NGC 877 | 02 17 59.7 | +14 32 39 | 3963 | 57.2 | composite | 0.52 | 3 | 11.1 | ··· |
UGC 01845 | 02 24 08.0 | +47 58 11 | 4600 | 66.5 | composite | 0.72 | 1 | 11.1 | <0.05 |
NGC 992 | 02 37 25.5 | +21 06 02 | 4065 | 58.7 | H ii | 0.43 | 4 | 11.0 | ··· |
UGC 02982 | 04 12 22.6 | +05 32 50 | 5354 | 77.6 | H ii | 0.43 | 5 | 11.2 | <0.05 |
NGC 1614 | 04 34 00.0 | –08 34 45 | 4778* | 69.1 | composite | 0.60 | 5 | 11.7 | <0.05 |
CGCG 468-002 NED01 | 05 08 19.7 | +17 21 48 | 5267 | 76.3 | Sy1.9 | 0.98 | 2 | 10.6 | 0.40 |
CGCG 468-002 NED02 | 05 08 21.2 | +17 22 08 | 4951 | 71.6 | composite | 0.51 | 2 | 11.0 | <0.05 |
NGC 1961 | 05 42 04.7 | +69 22 43 | 3908 | 56.4 | LINER | 1.96 | 6 | 11.1 | ··· |
UGC 03351 | 05 45 47.9 | +58 42 03 | 4433 | 64.1 | Sy2 | 1.34 | 7 | 11.2 | 0.02 |
UGC 03405 | 06 13 57.6 | +80 28 35 | 3799 | 54.8 | composite? | 0.75 | 2 | 10.3 | <0.05 |
UGC 03410 | 06 14 29.6 | +80 27 00 | 3871 | 55.9 | H ii | 0.45 | 2 | 10.9 | <0.05 |
NGC 2388 | 07 28 53.5 | +33 49 09 | 4078 | 58.9 | H ii | 0.56 | 1 | 11.2 | <0.05 |
NGC 2389 | 07 29 04.7 | +33 51 40 | 3956* | 57.1 | composite | 0.53 | 2 | 10.5 | ··· |
MCG +02-20-002 | 07 35 41.5 | +11 36 44 | 5100* | 73.8 | ··· | ··· | ··· | 10.2 | ··· |
MCG +02-20-003 | 07 35 43.4 | +11 42 35 | 4907 | 71.0 | composite | 0.45 | 1 | 11.0 | <0.05 |
NGC 3110 | 10 04 02.1 | –06 28 30 | 5013 | 72.6 | H ii | 0.42 | 5 | 11.3 | <0.05 |
NGC 3221 | 10 22 20.0 | +21 34 10 | 3959 | 57.1 | H ii | 0.40 | 8 | 11.0 | ··· |
Arp 299 | 11 28 31.0 | +58 33 41 | 3056 | 44.0 | Sy2 | 0.35 | 9 | 11.8 | 0.04 |
MCG –02-33-098 | 13 02 19.6 | –15 46 04 | 4713 | 68.2 | composite | 0.33 | 5 | 10.9 | 0.16 |
IC 860 | 13 15 03.6 | +24 37 08 | 3858 | 55.7 | no | 7.8 | 1 | 11.0 | <0.05 |
NGC 5653 | 14 30 10.5 | +31 12 55 | 3512 | 50.6 | H ii | 0.38 | 3 | 11.0 | 0.01 |
Zw 049-057 | 15 13 13.1 | +07 13 32 | 3858 | 55.7 | H ii | 0.46 | 8 | 11.0 | <0.05 |
NGC 5936 | 15 30 00.9 | +12 59 21 | 3989 | 57.6 | H ii | 0.48 | 1 | 11.0 | 0.03 |
NGC 5990 | 15 46 16.4 | +02 24 56 | 3793 | 54.7 | Sy2 | 0.74 | 10 | 11.0 | 0.05 |
NGC 6052 | 16 05 13.0 | +20 32 33 | 4739 | 68.5 | H ii | 0.23 | 3 | 10.9 | ··· |
NGC 6701 | 18 43 12.5 | +60 39 12 | 3895 | 56.2 | composite | 0.67 | 1 | 11.0 | <0.05 |
NGC 6921 | 20 28 28.9 | +25 43 24 | 4329 | 62.5 | AGN | ··· | 11, 12 | 10.2 | <0.05 |
MCG +04-48-002 | 20 28 35.1 | +25 44 00 | 4198 | 60.6 | H ii/AGN | 0.42 | 11 | 11.0 | 0.06 |
NGC 7591 | 23 18 16.3 | +06 35 09 | 4907 | 71.0 | composite | 0.85 | 1 | 11.0 | <0.05 |
NGC 7679 | 23 28 46.7 | +03 30 41 | 5161 | 74.7 | Sy2/Sy1 | 0.59 | 5 | 11.1 | 0.18 |
NGC 7752 | 23 46 58.5 | +29 27 32 | 4943 | 71.5 | composite | 0.33 | 2 | 10.7 | ··· |
NGC 7753 | 23 47 04.8 | +29 29 01 | 5201 | 75.3 | composite? | 1.02 | 2 | 10.9 | ··· |
NGC 7769 | 23 51 04.0 | +20 09 02 | 4157 | 60.0 | composite | 0.56 | 2 | 10.9 | 0.10 |
NGC 7770 | 23 51 22.6 | +20 05 49 | 4127 | 59.6 | H ii | 0.40 | 13 | 10.4 | 0.17 |
NGC 7771 | 23 51 24.9 | +20 06 43 | 4276 | 61.8 | H ii | 0.55 | 1 | 11.3 | 0.02 |
Notes.
Heliocentric velocity from the Spitzer/IRS high-resolution spectra (Alonso-Herrero et al. 2012a).
Classification of the nuclear activity from optical spectroscopy based on the classification scheme of Kewley et al. (2006).
Logarithm of the total 4–1000 μm IR luminosity in solar units calculated in this paper. The AGN torus IR luminosity is included.
Ratio between the bolometric AGN luminosity and the total IR luminosity from Alonso-Herrero et al. (2012a).
Reference. (1) Alonso-Herrero et al. (2009); (2) this work (Appendix A); (3) Moustakas & Kennicutt (2006); (4) Keel (1984); (5) Veilleux et al. (1995); (6) Ho et al. (1997); (7) Baan et al. (1998); (8) Aihara et al. 2011; (9) García-Marín et al. (2006); (10) Kewley et al. (2001); (11) Masetti et al. (2006); (12) Tueller et al. (2008); (13) Alonso-Herrero et al. (2012b).
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