Table 1.
Spectral mapping sources.
Name | RA | Dec | z | log(LIR/L⊙) | Merger class | |
---|---|---|---|---|---|---|
(1) | (2) | (3) | (4) | (5) | (6) | |
Mrk 938 | 00h11m06.56s | −12d06m28.2s | 0.01962 | 11.49 | d | |
MCG-02-01-051A | 00h18m49.85s | −10d21m34.0s | 0.02710 | 11.48 | b | |
Arp 236 B (VV 114 W) | 01h07m46.72s | −17d30m27.9s | 0.02007 | |||
Arp 236 A (VV 114 E) | 01h07m47.54s | −17d30m25.6s | 0.02007 | 11.71 | c | |
UCG 03410 (UGC03405) | 06h13m57.90s | +80d28m34.7s | 0.01247 | 11.10 | N | |
ESO557-G002 | 06h31m45.71s | −17d38m44.9s | 0.02099 | 11.25 | – | |
NGC 2342 A (NGC 2341) | 07h09m12.01s | +20d36m11.2s | 0.01722 | 11.31 | a | |
NGC 2369 | 07h16m37.7s | −62d20m37s | 0.01081 | 11.16 | a | |
NGC 2388 A (NGC 2389) | 07h29m04.59s | +33d51m38.0s | 0.01316 | 11.28 | a | |
Arp 299 B (NGC 3690) | 11h28m30.987s | 58d33m40.80s | 0.01041 | |||
Arp 299 A (IC 694) | 11h28m33.626s | 58d33m46.65s | 0.01041 | 11.93 | c | |
ESO320-G030 | 11h53m11.7s | −39d07m49s | 0.01078 | 11.17 | N | |
NGC 4922 | 13h01m25.27s | +29d18m49.5s | 0.02359 | 11.38 | c | |
MCG-03-34-063 | 13h22m19.02s | −16d42m30.0s | 0.02133 | 11.28 | d | |
NGC 5257 A (NGC 5258) | 13h39m57.72s | +00d49m53.0s | 0.02254 | 11.62 | b | |
NGC 5395 | 13h58m37.96s | +37d25m28.1s | 0.01158 | 11.08 | N | |
IC 4518 E | 14h57m45.33s | −43d07m57.0s | 0.01573 | 11.23 | a | |
ZW 049.057 | 15h13m13.1s | +07d13m32s | 0.01306 | 11.35 | N | |
IC 4687 | 18h13m39.80s | −57d43m30.7s | 0.01734 | 11.62 | b | |
NGC 6786 A | 19h11m04.37s | +73d25m32.5s | 0.02502 | 11.49 | c | |
NGC 6926 | 20h33m06.1s | −02d01m39s | 0.02001 | 11.32 | d | |
IC 5179 | 22h16m09.1s | −36d50m37s | 0.01141 | 11.24 | N | |
NGC 7552 | 23h16m10.7s | −42d35m05s | 0.00536 | 11.11 | N | |
NGC 7592 B (W) | 23h18m21.78s | −04d24m57.0s | 0.02444 | |||
NGC 7592 A (E) | 23h18m22.60s | −04d24m58.0s | 0.02444 | 11.40 | b | |
NGC 7674 | 23h27m56.71s | +08d46m44.3s | 0.02903 | 11.56 | a | |
NGC 7752 A (NGC 7753) | 23h47m04.84s | +29d29m00.5s | 0.01720 | 11.07 | c |
Notes. (1) source name; (2) source right ascension from GOALS targets (Armus et al. 2009); (3) source declination from GOALS targets; (4) redshift obtained from NED; (5) total infrared luminosity (many of these contain multiple nuclei; see Armus et al. 2009 for more details); (6) merger Class from Stierwalt et al. (2013) where N = non-merger, a = pre-merger, b = early stage merger, c = mid-stage merger, and d = late stage merger.
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