Table 1.
Sample galaxies.
| Name | Typea | zb | DLc | LIRd |
|---|---|---|---|---|
| (Mpc) | (1011 L⊙) | |||
| NGC 4418 | Sy 2 | 0.0071 | 33.6 ± 2.5 | 1.32 ± 0.19 |
| IC 860 | H II | 0.0130 | 62.1 ± 4.3 | 1.60 ± 0.22 |
| IRAS 12224–0624 | L | 0.0264 | 119.5 ± 8.2 | 1.98 ± 0.27 |
| Zw 049.057 | H II | 0.0130 | 62.4 ± 4.3 | 2.04 ± 0.28 |
| NGC 7469 | Sy 1 | 0.0164 | 68.2 ± 4.7 | 4.13 ± 0.57 |
| I Zw 1 | Sy 1 | 0.0610 | 258.2 ± 17.7 | 8.22 ± 1.13 |
| UGC 5101 | L | 0.0394 | 169.7 ± 11.6 | 9.50 ± 1.30 |
| IRAS 20551–4250 | H II | 0.0430 | 185.2 ± 12.7 | 10.65 ± 1.46 |
| IRAS 15250+3609 | L | 0.0552 | 243.7 ± 16.7 | 11.08 ± 1.53 |
| IRAS 08572+3915 | L | 0.0584 | 253.1 ± 17.3 | 13.38 ± 1.84 |
| IRAS 05189–2524 | Sy 2 | 0.0428 | 180.2 ± 12.4 | 13.50 ± 1.85 |
| IRAS 22491–1808 | H II | 0.0778 | 337.0 ± 23.1 | 13.88 ± 1.92 |
| Mrk 273 | Sy 2 | 0.0378 | 165.6 ± 11.3 | 14.81 ± 2.03 |
| IRAS 20414–1651 | H II | 0.0871 | 383.4 ± 26.3 | 15.12 ± 2.18 |
| Arp 220 | L | 0.0181 | 84.1 ± 5.8 | 17.25 ± 2.36 |
| IRAS 13120–5453 | Sy 2 | 0.0308 | 137.8 ± 9.5 | 19.20 ± 2.65 |
| IRAS 12112+0305 | L | 0.0733 | 326.3 ± 22.4 | 20.35 ± 2.79 |
| IRAS 17208–0014 | H II | 0.0428 | 189.3 ± 13.0 | 26.21 ± 3.59 |
| Mrk 231 | Sy 1 | 0.0422 | 184.3 ± 12.6 | 34.30 ± 4.70 |
Notes.
Optical spectral types H II, L (for LINER), Sy 1 and Sy 2 (for Seyfert 1 and 2, respectively). When available, we used the classifications from Veilleux et al. (1995) and Kim et al. (1998), otherwise, we used classifications from Sanders et al. (1988b), Baan et al. (1998), and Véron-Cetty & Véron (2001).
In priority order, we used redshifts from Veilleux et al. (2013), Sanders et al. (2003), or Strauss et al. (1992), except for IRAS 05189–2524 where the redshift from Sanders et al. (1991) was used.
Luminosity distances were calculated from the redshifts following the same procedure as Sanders et al. (2003).
Infrared luminosities were calculated using the prescription in Table 1 of Sanders & Mirabel (1996; originally from Pérault 1987) using IRAS fluxes taken from Sanders et al. (2003), except for IRAS 20414–1651 where fluxes were taken from Moshir et al. (1992), and I Zw 1 where they were taken from Sanders et al. (1989).
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