Table 1
Sample of local ULIRGs.
| IRAS Name | Component | R.A.a | Dec.a | vsysb | zc | dLd | Scaled |  |
 |
|---|---|---|---|---|---|---|---|---|---|
| (ICRS) | (ICRS) | (km s−1) | (Mpc) | (pc arcsec−1) | |||||
| 12112+0305 | 0.0731 | 330 | 1390 | 11.4 | 12.19 | ||||
| SW | 12h13m45.939s | 2d48m39.10s | 21167 | ||||||
| NE | 12h13m46.056s | 2d48m41.53s | 21045 | ||||||
| 14348−1447 | 0.0825 | 375 | 1554 | 11.6 | 12.27 | ||||
| SW | 14h37m38.280s | –15d00m24.24s | 23766 | ||||||
| NE | 14h37m38.396s | –15d00m21.29s | 23676 | ||||||
| 22491−1808 | 0.0778 | 353 | 1469 | 11.5 | 12.03 | ||||
| E | 22h51m49.348s | –17d52m24.12s | 22412 | ||||||
| W* | ⋯ | ⋯ | ⋯ | ||||||
Notes. (a) Coordinates of the 248 GHz rest-frame continuum emission for each nucleus (see Sect. 3.1.2). The astrometric uncertainty is ~25 mas (see Sect. 3.2). (b) CO(2–1) systemic velocity using the relativistic velocity definition in the kinematic local standard of rest (LSRK; see Sect. 3.2). Typical uncertainties are ≲10 km s−1. (c) Redshift using the average systemic velocity of the system. (d)Luminosity distance and scale for the assumed cosmology (see Sect. 1). (e) Luminosity of the AGNin the system estimated from mid-IR spectroscopy (Veilleux et al. 2009). (f) IR luminosity of the system based on the SED fitting of the Spitzer and Herschel mid- and far-IR photometry (see Sect. 3.4.1). (*)No 248 GHz continuum is detected at the position of the near-IR W nucleus of IRAS 22491−1808.
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