2013ApJ...776...38F


Query : 2013ApJ...776...38F

2013ApJ...776...38F - Astrophys. J., 776, 38 (2013/October-2)

Far-infrared fine-structure line diagnostics of ultraluminous infrared galaxies.

FARRAH D., LEBOUTEILLER V., SPOON H.W.W., BERNARD-SALAS J., PEARSON C., RIGOPOULOU D., SMITH H.A., GONZALEZ-ALFONSO E., CLEMENTS D.L., EFSTATHIOU A., CORMIER D., AFONSO J., PETTY S.M., HARRIS K., HURLEY P., BORYS C., VERMA A., COORAY A. and SALVATELLI V.

Abstract (from CDS):

We present Herschel observations of 6 fine-structure lines in 25 ultraluminous infrared galaxies at z < 0.27. The lines, [O III]52 µm, [N III]57 µm, [O I]63 µm, [N II]122 µm, [O I]145 µm, and [C II]158 µm, are mostly single Gaussians with widths <600 km/s and luminosities of 107-109 L. There are deficits in the [O I]63/LIR, [N II]/LIR, [O I]145/LIR, and [C II]/LIR ratios compared to lower luminosity systems. The majority of the line deficits are consistent with dustier H II regions, but part of the [C II] deficit may arise from an additional mechanism, plausibly charged dust grains. This is consistent with some of the [C II] originating from photodissociation regions or the interstellar medium (ISM). We derive relations between far-IR line luminosities and both the IR luminosity and star formation rate. We find that [N II] and both [O I] lines are good tracers of the IR luminosity and star formation rate. In contrast, [C II] is a poor tracer of the IR luminosity and star formation rate, and does not improve as a tracer of either quantity if the [C II] deficit is accounted for. The continuum luminosity densities also correlate with the IR luminosity and star formation rate. We derive ranges for the gas density and ultraviolet radiation intensity of 101 < n < 102.5 and 102.2 < G0< 103.6, respectively. These ranges depend on optical type, the importance of star formation, and merger stage. We do not find relationships between far-IR line properties and several other parameters: active galactic nucleus (AGN) activity, merger stage, mid-IR excitation, and SMBH mass. We conclude that these far-IR lines arise from gas heated by starlight, and that they are not strongly influenced by AGN activity.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: evolution - galaxies: ISM - galaxies: starburst - infrared: galaxies

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 2MASX J00212652-0839261 LIN 00 21 26.5135306416 -08 39 25.967117268   18.37       ~ 107 1
2 6dFGS gJ004215.5-125604 H2G 00 42 15.54 -12 56 03.0   19.45       ~ 67 0
3 IRAS 01003-2238 Sy2 01 02 49.9920152640 -22 21 57.262136544   18.62 18.9 17.83   ~ 155 0
4 Mrk 1014 Sy1 01 59 50.2534701768 +00 23 40.864244784   16.08 15.87     ~ 554 0
5 IRAS 03158+4227 G 03 19 11.9490689880 +42 38 25.463172912           ~ 55 0
6 IRAS 03521+0028 LIN 03 54 42.146 +00 37 03.33           ~ 86 0
7 IRAS 04103-2838 LIN 04 12 19.4458581600 -28 30 24.933273876     16.9     ~ 68 0
8 LEDA 17155 Sy2 05 21 01.3994605776 -25 21 45.321827832   15.47 14.75     ~ 475 0
9 LEDA 89499 LIN 06 02 54.066 -71 03 10.48   15.6       ~ 85 1
10 LEDA 89500 Sy2 06 21 01.188 -63 17 23.81   16.70   15.27   ~ 62 1
11 IRAS 07598+6508 Sy1 08 04 30.4643108040 +64 59 52.789588188   14.3 15.5     ~ 225 0
12 2MASX J08332058-2509332 Sy1 08 33 20.588 -25 09 33.29   16.4       ~ 31 0
13 NAME IRAS F08572+3915 NW LIN 09 00 25.364 +39 03 54.23     16.66     ~ 405 1
14 LEDA 90127 Sy1 10 40 29.1640944744 +10 53 18.202070076   17.79 17.18     ~ 92 0
15 LEDA 33083 LIN 10 59 18.128 +24 32 34.74   15.7       ~ 261 1
16 LEDA 125693 LIN 11 12 03.4 -02 54 23   17.45 17.40     ~ 95 1
17 SDSS J120424.54+192509.7 Sy2 12 04 24.5432777064 +19 25 09.773024772   16.63 19.16     ~ 76 0
18 LEDA 90164 Sy2 12 09 45.1187842872 -05 01 13.431047484   17.52 17.8 16.56   ~ 99 1
19 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5637 1
20 Mrk 231 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 1930 3
21 IRAS 13342+3932 Sy1 13 36 24.0619427808 +39 17 31.105014396     17.76     ~ 81 0
22 NAME OKM2018 SWIFT J1344.7+5588 Sy2 13 44 42.1883001096 +55 53 13.596220932   15.68 14.91     ~ 883 3
23 ICRF J134733.3+121724 Sy2 13 47 33.36161873 +12 17 24.2398927   19.28 18.44 15.718   ~ 564 3
24 Mrk 463E Sy2 13 56 02.886 +18 22 18.84   15.01 14.22     ~ 148 1
25 Mrk 463 Sy2 13 56 02.897 +18 22 18.66   14.8 14.22     ~ 377 2
26 LEDA 90196 Sy2 15 02 31.9755844913 +14 21 34.926031528   20.69 20.13     ~ 53 0
27 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2872 4
28 LEDA 90222 Sy1 15 48 56.8020209304 -04 59 33.598051584   16.4 16.40 16.85   ~ 92 0
29 LEDA 90237 LIN 16 11 40.4280459768 -01 47 06.566246232   16.6       ~ 75 0
30 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1589 2
31 LEDA 60189 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 410 0
32 NAME Super Antennae Sy2 19 31 21.4272801984 -72 39 21.442847832   17.39 16.37 14.65   ~ 289 2
33 IRAS 20037-1547 Sy1 20 06 31.7 -15 39 08     16.00     ~ 34 0
34 LEDA 90352 LIN 20 11 23.862 -02 59 50.33   17.80   16.41   ~ 62 0
35 [VV2000] J201329.8-414735 QSO 20 13 29.509 -41 47 35.48   17.0       ~ 121 2
36 6dFGS gJ204418.2-164017 LIN 20 44 18.186 -16 40 16.63   18.02   17.04   ~ 85 0
37 ESO 286-19 LIN 20 58 26.8183783008 -42 38 59.411838156   14.79 14.79 14.20   ~ 276 0
38 ESO 148-2 Sy2 23 15 46.772 -59 03 15.94   14.94 14.73 13.95   ~ 252 1
39 LEDA 90424 LIN 23 26 03.6867143064 -69 10 18.422274828   16.6       ~ 44 0
40 LEDA 90425 H2G 23 28 06.0899186859 -53 58 30.679199450   17.19   16.10   ~ 32 0

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2023.01.30-05:22:50

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