2003MNRAS.343..585F


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST12:01:10

2003MNRAS.343..585F - Mon. Not. R. Astron. Soc., 343, 585-607 (2003/August-1)

Starburst and AGN activity in ultraluminous infrared galaxies.

FARRAH D., AFONSO J., EFSTATHIOU A., ROWAN-ROBINSON M., FOX M. and CLEMENTS D.

Abstract (from CDS):

We examine the power source of 41 local ultraluminous infrared galaxies (ULIRGs) using archival infrared (IR) and optical photometry. We fit the observed spectral energy distributions with starburst and active galactic nucleus (AGN) components, each component being drawn from a family of templates. We find that all of the sample require a starburst, whereas only half require an AGN. In 90 per cent of the sample the starburst provides over half the IR emission, with a mean fractional luminosity of 82 per cent. When combined with other galaxy samples we find that starburst and AGN luminosities correlate over six decades in IR luminosity, suggesting that a common factor governs both luminosities, plausibly the gas masses in the nuclear regions. We find no trend for increasing fractional AGN luminosity with increasing total luminosity, contrary to previous claims. We find that the mid-IR F7.7/C7.7line-continuum ratio is no indication of the starburst luminosity, or the fractional AGN luminosity, and therefore that F7.7/C7.7is not a reliable diagnostic of the power source in ULIRGs. The radio flux correlates with the starburst luminosity, but shows no correlation with the AGN luminosity, in line with previous results. We propose that the scatter in this correlation is due to a skewed starburst initial mass function and/or relic relativistic electrons from a previous starburst, rather than contamination from an obscured AGN. We show that most ULIRGs undergo multiple starbursts during their lifetime, and by inference that mergers between more than two galaxies may be common amongst ULIRGs. Our results support the evolutionary model for ULIRGs proposed by Farrah et al., where they can follow many different evolutionary paths of starburst and AGN activity in transforming merging spiral galaxies into elliptical galaxies, but that most do not go through an optical quasi-stellar object phase. The lower level of AGN activity in our local sample compared with z ∼ 1 hyperluminous infrared galaxies implies that the two samples are distinct populations. We postulate that different galaxy formation processes at high z are responsible for this difference.

Abstract Copyright: 2003 RAS

Journal keyword(s): galaxies: active - quasars: general - galaxies: Seyfert - galaxies: starburst - infrared: galaxies

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 2MASX J00215355-7910077 Sy2 00 21 53.5520857547 -79 10 08.021572343   17.33 16.3 15.19   ~ 74 0
2 IRAS 00199-7426 G 00 22 07.0041916624 -74 09 41.587896860   17.41   16.24   ~ 31 1
3 2MASX J00285413+4308149 LIN 00 28 54.132 +43 08 14.91     16.0     ~ 30 0
4 2MASX J00360040-2715342 G 00 36 00.3771700777 -27 15 33.878802388   17.18       ~ 39 0
5 2MASX J01405591-4602533 H2G 01 40 55.8716338374 -46 02 53.781173198   17.53   16.20   ~ 23 0
6 6dFGS gJ023813.1-473811 G 02 38 13.076 -47 38 11.34   17.402   17.336   ~ 20 1
7 6dFGS gJ030821.2-533514 G 03 08 21.448 -53 35 12.85   16.63   15.69   ~ 13 0
8 2MASX J04260482+1443360 LIN 04 26 04.829 +14 43 36.01           ~ 26 0
9 2MASX J05210136-2521450 Sy2 05 21 01.3987198411 -25 21 45.269338983   15.47 14.75     ~ 441 0
10 2MASX J06025406-7103104 LIN 06 02 54.066 -71 03 10.48   15.6       ~ 77 1
11 2MASX J06210118-6317238 Sy2 06 21 01.188 -63 17 23.81   16.70   15.27   ~ 56 1
12 NAME IRAS F08572+3915 NW LIN 09 00 25.364 +39 03 54.23     16.66     ~ 370 1
13 NAME IRAS 09111-1007W Sy2 09 13 36.4573260365 -10 19 29.982284396   15.7 16.10     ~ 74 1
14 UGC 5101 Sy1 09 35 51.599 +61 21 11.33   15.20 15.50     ~ 519 4
15 IRAS 09583+4714 Sy1 10 01 31.2251634762 +46 59 46.644273583   18.0       ~ 26 1
16 FIRST J100645.8+483741 rG 10 06 45.874 +48 37 43.34   15.7       ~ 28 0
17 3XMM J102142.6+130654 LIN 10 21 42.793 +13 06 56.04   17.51       ~ 67 3
18 2MASX J10522356+4408474 LIN 10 52 23.518 +44 08 47.60           ~ 60 0
19 2XMM J105918.1+243234 LIN 10 59 18.128 +24 32 34.74   15.7       ~ 243 1
20 LEDA 39024 LIN 12 13 46.107 +02 48 41.50           ~ 315 1
21 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1827 3
22 Mrk 273 Sy2 13 44 42.164 +55 53 13.53   15.68 14.91     ~ 840 3
23 2MASX J14373831-1500239 Sy1 14 37 38.317 -15 00 23.97   16.58 16.40     ~ 248 1
24 6dFGS gJ144059.0-370432 Sy2 14 40 59.0140344918 -37 04 31.937494895   17.72   16.48   ~ 95 0
25 2MASX J15265942+3558372 LIN 15 26 59.442 +35 58 37.01   15.61       ~ 248 1
26 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2739 4
27 2MASX J17142047+5310317 G 17 14 20.478 +53 10 31.80           ~ 83 0
28 6dFGS gJ172322.0-001701 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 379 0
29 2MASX J18485387+3237287 G 18 48 53.877 +32 37 28.75           ~ 20 0
30 NAME Superantennae Sy2 19 31 21.4252803168 -72 39 21.448768732   17.39 16.37 14.65   ~ 280 2
31 2MASX J19322229-0400010 EmG 19 32 22.2960198723 -04 00 01.793135107   18.85   17.04   ~ 90 0
32 LEDA 90339 G 19 48 15.7 +09 52 05           ~ 33 0
33 6dFGS gJ200718.8-061426 G 20 07 18.669 -06 14 27.32   17.24   16.18   ~ 21 1
34 6dFGS gJ204418.2-164017 LIN 20 44 18.186 -16 40 16.63   18.02   17.04   ~ 78 0
35 ESO 286-19 LIN 20 58 26.8182983654 -42 38 59.418569678   14.79 14.79 14.20   ~ 253 0
36 2MASX J21161852-4433374 G 21 16 18.5751356914 -44 33 37.140155607   17.48   16.24   ~ 25 1
37 2MASX J21530552-0614496 G 21 53 05.4954344394 -06 14 49.975194773           ~ 17 0
38 NAME South America H2G 22 51 49.307 -17 52 23.96   16.97       ~ 290 3
39 ESO 148-2 Sy2 23 15 46.772 -59 03 15.94   14.94 14.73 13.95   ~ 236 1
40 2MASX J23390127+3621087 SyG 23 39 01.274 +36 21 08.77   16.17       ~ 199 1
41 2MASX J23414354-6122526 Sy2 23 41 43.542 -61 22 52.62   17.70   16.71   ~ 20 1

    Equat.    Gal    SGal    Ecl

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2021.04.18-12:01:10

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