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.
Coordinates of the ∼220–250 GHz continuum detected by ALMA for each nucleus (see Sect. 4.1). The typical astrometric uncertainty is 25 mas.
CO(2–1) velocity of the nucleus using the radio definition in the kinematic local standard of rest (Lamperti et al., in prep.).
Luminosity distance and scale for the assumed cosmology (see Sect. 1).
6–1500 μm IR luminosity derived from the SED fit. The typical uncertainty is 0.03 dex (see Sect. 4.4).
Nuclear activity classification based on optical spectroscopy (see Perna et al. 2021).
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).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.