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Table 1.

Sample of local ULIRGs.

IRAS name Nucleus RA (a) Dec (a) vCO(b) z(c) dL(d) Scale (d) log LIR(e) Class. (f) Morph. (g)
(ICRS) (ICRS) (km s−1) (Mpc) (kpc arcsec−1) (L⊙)
00091−0738 0.1181 550 2.13 12.34 HII I
S 00 11 43.272 −07 22 07.35 31 637 …
N 00 11 43.302 −07 22 06.18 31 686 …
00188−0856 − 00 21 26.513 −08 39 25.99 34 136 0.1285 602 2.29 12.42 Sy2 M
00509+1225 – 00 53 34.934 +12 41 35.94 17 265 0.0611 273 1.18 11.87 Sy1 M
01572+0009 – 01 59 50.251 +00 23 40.88 42 077 0.1633 782 2.80 12.65 Sy1 M
F05189−2524 – 05 21 01.400 −25 21 45.30 12 285 0.0427 188 0.84 12.10 Sy2 M
07251−0248 0.0878 400 1.64 12.45 I
W 07 27 37.532 −02 54 54.38 24 201 HII
E 07 27 37.613 −02 54 54.25 24 193 HII
09022−3615 – 09 04 12.706 −36 27 01.93 16 856 0.0596 266 1.15 12.33 HII M
F10190+1322 0.0763 345 1.45 12.04 I
W 10 21 42.493 +13 06 53.83 21 336 HII
E 10 21 42.754 +13 06 55.61 21 167 HII
11095−0238 0.1064 491 1.95 12.33 I
SW 11 12 03.359 −02 54 23.29 28 806 LINER
NE 11 12 03.383 −02 54 22.94 28 863 LINER
F12072−0444 0.1284 601 2.29 12.48 I
S 12 09 45.13 −05 01 14.6 (†) Sy2
N 12 09 45.13 −05 01 13.5 (†) Sy2
F12112+0305 0.0730 329 1.39 12.32 LINER I
SW 12 13 45.940 +02 48 39.12 20 448 …
NE 12 13 46.057 +02 48 41.55 20 322 …
13120−5453 – 13 15 06.323 −55 09 22.82 9046 0.0311 136 0.62 12.27 Sy2 M
F13451+1232 0.1217 568 2.19 12.31 I
W 13 47 33.36 +12 17 24.2 (†) Sy2
E 13 47 33.50 +12 17 23.8 (†) LINER
F14348−1447 0.0826 375 1.55 12.41 I
SW 14 37 38.281 −15 00 24.23 22 911 LINER
NE 14 37 38.397 −15 00 21.27 22 809 LINER
F14378−3651 – 14 40 59.013 −37 04 31.93 19 113 0.0681 306 1.30 12.15 Sy2 M
F15327+2340 0.0181 78 0.37 12.19 M
W 15 34 57.224 +23 30 11.44 5290 LINER
E 15 34 57.293 +23 30 11.29 5380 LINER
16090−0139 – 16 11 40.419 −01 47 06.35 35 352 0.1337 629 2.37 12.62 HII M
16155+0146 0.1330 625 2.36 12.24 I
NW 16 18 09.364 +01 39 21.75 35 188 Sy2
SE 16 18 09.54 +01 39 19.7 (†) … …
17208−0014 – 17 23 21.957 −00 17 00.88 12 304 0.0428 189 0.84 12.43 LINER M
F19297−0406 0.0856 390 1.61 12.45 I
S 19 32 22.30 −04 00 01.8 (†) 236 85 HII
N 19 32 22.309 −04 00 01.03 23 589 HII
19542+1110 – 19 56 35.785 +11 19 05.03 17 629 0.0625 280 1.20 12.09 LINER M
20087−0308 – 20 11 23.866 −02 59 50.72 28 600 0.1055 487 1.93 12.47 LINER M
20100−4156 0.1298 609 2.31 12.66 I
NW 20 13 29.48 −41 47 32.6 (†) 34 428 HII
SE 20 13 29.556 −41 47 35.21 34 453 LINER
20414−1651 – 20 44 18.159 −16 40 16.82 23 962 0.0869 396 1.63 12.24 HII M
F22491−1808 0.0776 352 1.47 12.23 I
W 22 51 49.24 −17 52 23.7 (†) … HII
E 22 51 49.349 −17 52 24.13 21 600 HII

Notes.

(a)

Coordinates of the ∼220–250 GHz continuum detected by ALMA for each nucleus (see Sect. 4.1). The typical astrometric uncertainty is 25 mas.

(b)

CO(2–1) velocity of the nucleus using the radio definition in the kinematic local standard of rest (Lamperti et al., in prep.).

(c)

Redshift using the average velocity of the system.

(d)

Luminosity distance and scale for the assumed cosmology (see Sect. 1).

(e)

6–1500 μm IR luminosity derived from the SED fit. The typical uncertainty is 0.03 dex (see Sect. 4.4).

(f)

Nuclear activity classification based on optical spectroscopy (see Perna et al. 2021).

(g)

System morphology: I. Interacting system with nuclear separation > 1 kpc; M. Advanced merger with nuclear separation < 1 kpc (see Perna et al. 2021).

(†)For the four nuclei undetected in the ALMA images and the two systems (F12072−0444 and F13451+1232) not observed by ALMA, we used near-IR and optical HST images, whose astrometry was tied to Gaia DR2, to measure the nuclear position (see Sect. 3.1 of Perna et al. 2021).

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