Table 1.
Sources in the PUMA survey.
| IRAS ID (Other) | RA | Dec | D | log LIR | q | SB-AGN | αAGN | Optical | Morph | IC | NS | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (h:m:s) | (° : ′: ″) | (Mpc) | (L⊙) | type |
(kpc) | |||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) |
| F00091−0738 | 00:11:43.27 | −07:22:07.34 | 519 | 12.27 ± 0.03 | 2.81 | AGN | 0.46(0.58) | HII | – | I | IIIb | 2.3 |
| F00188−0856 | 00:21:26.51 | −08:39:25.99 | 563 | 12.41 ± 0.04 | 2.32 | AGN | 0.50(0.35) | LI(N)ER | Sy 2 | M | V | < 0.3 |
| F00509+1225 (IZw1) | 00:53:34.93 | +12:41:35.94 | 243 | 11.30 ± 0.05 (a) | 2.51 | AGN | 0.92 | Sy 1 | Sy 1 | M | IVb | < 0.2 |
| F01572+0009 (Mrk 1014) | 01:59:50.25 | +00:23:40.88 | 717 | 12.63 ± 0.03 | 2.01 | AGN | 0.65(0.27) | Sy 1 | Sy 1 | M | IVb | < 0.4 |
| F05189−2524 | 05:21:01.40 | −25:21:45.30 | 189 | 12.17 ± 0.01 | 2.72 | AGN | 0.72(0.30) | Sy 2 | Sy 2 | M | IVb | < 0.1 |
| 07251−0248 | 07:27:37.61 | −02:54:54.25 | 390 | 12.41 ± 0.04 | 2.76 | SB | 0.30(0.39) | – | HII | I | IIIb | 1.8 |
| 09022−3615 | 09:04:12.71 | −36:27:01.93 | 268 | 12.30 ± 0.01 | 2.21 | AGN ? | 0.54(0.09) | HII | HII | M | IVa | < 0.1 |
| 10190+1322 | 10:21:42.94 | +13:06:53.83 | 343 | 12.05 ± 0.03 | 2.41 | SB | 0.17 | HII | HII | I | IIIb | 7.2 |
| F11095−0238 | 11:12:03.38 | −02:54:22.94 | 477 | 12.28 ± 0.03 | 2.15 | AGN | 0.44(0.60) | LI(N)ER | ? | I | IIIb | 1.1 |
| F12072−0444 | 12:09:45.12 | −05:01:13:31 | 573 | 12.40 ± 0.03 | 2.55 | AGN | 0.75(0.41) | Sy 2 | Sy 2 | I | IIIb | 2.3 |
| F12112+0305 | 12:13:46.06 | +02:48:41.53 | 329 | 12.33 ± 0.02 | 2.65 | SB | 0.17 | LI(N)ER | – | I | IIIb | 4.18 |
| 13120−5453 (WKK 2031) | 13:15:06.32 | −55:09:22.82 | 139 | 12.25 ± 0.03 | 2.91 | AGN | 0.33(0.01) | Sy 2 | Sy 2 | M | IVb | < 0.1 |
| F13451+1232 | 13:47:33.36 | +12:17:24.24 | 542 | 12.31 ± 0.04 | −0.34 | AGN | 0.82(0.60) | Sy 2 | Sy 2 | I | IIIb | 4.3 |
| F14348−1447 | 14:37:38.28 | −15:00:24.24 | 370 | 12.35 ± 0.02 | 2.37 | SB | 0.17(0.04) | LI(N)ER | ? | I | IIIb | 5.45 |
| F14378−3651 | 14:40:59.01 | −37:04:31.93 | 302 | 12.13 ± 0.02 | 2.35 | AGN | 0.21(0.01) | Sy 2 | Sy 2 | M | IVa | < 0.1 |
| F15327+2340 (Arp220) | 15:34:57.22 | +23:30:11.50 | 82 | 12.17 ± 0.01 | 2.61 | SB | 0.06(0.17) | LI(N)ER | LI(N)ER | I | IIIb | 0.37 |
| F16090−0139 | 16:11:40.42 | −01:47:06.35 | 592 | 12.57 ± 0.02 | 2.34 | SB | 0.41(0.24) | LI(N)ER | HII | M | IVa | < 0.7 (b) |
| F16156+0146 | 16:18:09.37 | +01:39:21.76 | 585 | 12.11 ± 0.06 | 2.18 | AGN | 0.70(0.40) | Sy 2 | – | I | IIIb | 8.26 |
| 17208−0014 | 17:23:21.96 | −00:17:00.86 | 189 | 12.50 ± 0.02 | 2.70 | SB | 0.00 (0.11) | HII | LI(N)ER | M | IVb | < 0.1 |
| F19297−0406 | 19:32:22.30 | −04:00:01.80 | 376 | 12.40 ± 0.02 | 2.49 | SB | 0.23(0.01) | HII | ? | I | IIIb (c) | 1.1 |
| 19542+1110 | 19:56:35.78 | +11:19:05.03 | 284 | 12.12 ± 0.04 | 2.55 | SB | 0.26(0.04) | LI(N)ER | LI(N)ER | M | IVb | < 0.1 |
| 20087−0308 | 20:11:23.87 | −02:59:50.71 | 463 | 12.44 ± 0.03 | 3.01 | SB | 0.20(0.03) | LI(N)ER | LI(N)ER | M | IVa | < 0.9 |
| 20100-4156 | 20:13:29.56 | −41:47:35.21 | 571 | 12.64 ± 0.02 | 2.49 | SB | 0.26(0.20) | HII | LI(N)ER | I | IIIb | 6.5 |
| F20414−1651 | 20:44:18.16 | −16:40:16.82 | 381 | 12.30 ± 0.08 | 2.47 | SB | 0.00 | HII | – | M | IVb | < 0.2 |
| F22491−1808 | 22:51:49.24 | −17:52:23.66 | 339 | 12.19 ± 0.03 | 3.03 | SB | 0.15 | HII | HII | I | IIIb | 2.7 |
Notes. Column (1): IRAS identification code (alternative name); (2) and (3): RA and Dec coordinates of the ULIRG nuclei from this work; for binary systems, we report the coordinates of the near-IR brightest nucleus; (4): Hubble distance (from the NED); (5): IR luminosity; (6): q radio-IR parameter (Condon et al. 1991); (7): simplified AGN-SB classification based on the information provided in Cols. (8) and (9); (8): fraction of AGN contribution to Lbol derived from the 30 to 15 μm flux ratio (f30/f15). This ratio gives a good first-order approach to the contribution of the AGN to Lbol because it agrees to within 10 − 15% with the average value of the six methods considered in Veilleux et al. (2009). In order to homogenise the various calibrations of this ratio, we took the results of Veilleux et al. (2013) as reference and fit a second-order polynomial to the log(f30/f15) function. The flux ratio values are from Veilleux et al. (2009, 2013) and Spoon et al. (2013). Values in brackets are derived according to the method of Nardini et al. (2010), which is based on the analysis of the 5 − 8 μm spectral range; (9–10) optical spectral type according to Veilleux et al. (2009, 2013) in Col. 9, and according to our classification obtained from nuclear spectra (Sect. 6) in Col. 10; (11): simplified morphology classes (I: interacting, M: mergers); see text for details. (12): IC according to the scheme by Veilleux et al. (2002), obtained from Veilleux et al. (2009) or derived from HST imaging; (13): Nuclear separation from Veilleux et al. (2009), Duc et al. (1997), and Kim et al. (2013).
[40 − 500] μm IR luminosity from Petric et al. (2015). This target does not meet the IR luminosity criterion for being a ULIRG (although Lbol > 1012 L⊙), but it has been included because it is usually considered an archetypical type 1 AGN.
No HST images are available for F16090−0139, therefore the NS upper limit has been obtained on the basis of our ALMA images (Pereira-Santaella et al., in prep.).
F19297−0406, originally associated with a single nucleus (Kim et al. 2013), is here classified as a IIIb system because two nuclei in near-IR HST and ALMA (Pereira-Santaella et al., in prep.) images are detected.
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