Table 3
Non-dwarf galaxies with IR signatures of active massive black holes.
| Name | RA | Dec | Redshift | Distance | log(Mstellar) | W1 − W2 | W2 − W3 | log(MBHIR) | Image |
| J2000 | J2000 | Mpc | M ⊙ | [mag] | [mag] | M ⊙ | |||
|
|
|||||||||
| CIRCINUS | 14h13m09.30s | −65d20m21.0s | 0.001448 | 4.207 | − | 1.038 | 2.325 | 6.306a | 8 |
| NGC 2964 | 09h42m54.23s | +31d50m50.6s | 0.004430 | 20.429 | 10.201 | 0.667 | 1.780 | 6.497a | 17 |
| NGC 4194 | 12h14m09.47s | +54d31m36.6s | 0.008178 | 39.100 | 9.684 | 0.531 | 3.761 | 7.235a | 29 |
| NGC 3690 NED01 | 11h28m31.02s | +58d33m40.7s | 0.009990 | 40.240 | 10.357 | 1.183 | 2.617 | 7.877a | 30 |
| NGC 3690 NED02 | 11h28m33.63s | +58d33m46.6s | 0.010456 | 42.133 | 10.461 | 0.983 | 4.036 | 7.864a | 31 |
| Moran08 | 10h05m51.19s | +12d57m40.6s | 0.009375 | 43.300 | 9.777 | 1.124 | 2.838 | 6.466 | − |
| NGC 1275 | 03h19m48.16s | +41d30m42.1s | 0.017559 | 68.180 | 11.067 | 0.911 | 3.429 | 7.752a | 36 |
| Greene137+Dong164 | 11h53m41.77s | +46d12m42.2s | 0.024251 | 98.744 | 10.329 | 0.518 | 2.270 | 6.576 | − |
| Dong222 | 14h00m40.57s | −01d55m18.3s | 0.025049 | 102.052 | 9.661 | 0.665 | 3.809 | 6.678 | − |
| Greene47 | 08h24m43.28s | +29d59m23.5s | 0.025420 | 103.594 | 9.674 | 1.171 | 2.888 | 7.379 | − |
| Reines3NL | 03h22m24.64s | +40d11m19.8s | 0.026084 | 106.352 | 9.565 | 0.854 | 3.647 | 5.988 | − |
| MRK 0315 | 23h04m02.62s | +22d37m27.5s | 0.027278 | 111.319 | 10.854 | 0.527 | 2.796 | 7.259 | 38 |
| Greene203 | 15h59m09.62s | +35d01m47.4s | 0.031024 | 126.958 | 10.600 | 0.743 | 2.338 | 7.279a | − |
Notes. Column (1): name. Columns (2) and (3); right ascension and declination (J2000). Column (4): redshift. Column (5): distance in Mpc. Col. (6): log of stellar mass measured from SED fit. Columns (7) and (8): WISE colours. Column (9): log of central black hole mass estimates based on IR luminosity (assuming Lbol = 0.1 LEdd). Column (10): image number in Fig. 2.
These sources are extended and larger than the largest WISE aperture (24.75 arcsec radius aperture); therefore, the infrared black hole mass estimates for these sources are only lower limits. The full table is available at the CDS. A portion is shown here for guidance regarding its form and content.
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