2009A&A...505.1319G


Query : 2009A&A...505.1319G

2009A&A...505.1319G - Astronomy and Astrophysics, volume 505, 1319-1343 (2009/10-3)

Integral field optical spectroscopy of a representative sample of ULIRGs. I. The data.

GARCIA-MARIN M., COLINA L., ARRIBAS S. and MONREAL-IBERO A.

Abstract (from CDS):

Ultraluminous infrared galaxies (ULIRGs) are among the brightest objects in the local Universe. They are powered by strong star formation and/or an AGN. As a result of the merger process, they are also likely to be the progenitors of elliptical galaxies. The study of the structure and kinematics of samples of local ULIRGs is necessary to understand the physical processes that these galaxies undergo, and their implications for our understanding of similar types of galaxies at high redshift. The goal of the project is to analyze the structure, dust distribution, ionization state, and kinematics of a representative sample of 22 ULIRGs. The galaxies in the sample undergo different merger phases (they are evenly divided between pre- and post-coalescence systems) and ionization stages (27% HII, 32% LINER, 18% Seyfert, and 23% mixed classifications) over a wide infrared luminosity range (11.8≤LIR/L≤12.6), which also includes some galaxies of low luminosity. The main aims of this paper are to present the sample and discuss the structure of the stellar and ionized gas components. Our study relies on the use of integral field optical spectroscopy data obtained with the INTEGRAL instrument at the 4.2m William Herschel Telescope. The structure of the ionized gas as traced by different emission lines has been studied and compared with that of the stellar continuum. We find structural variations between the gaseous and the stellar components, with offsets in the emission peaks positions of up to about 8kpc. The observed morphological differences are due to the spatial distribution of the ionization sources and the presence of dust. Young star formation (as traced by the Hα emission) is present in all regions of the galaxies. However, for 64% of ULIRGs in an early interaction phase, the young star formation peak does not coincide with the stellar maxima. In contrast, galaxies undergoing advanced mergers have a Hα peak that is located in their nuclear regions. In three of the studied ULIRGs (one pre- and two post-coalescents), hard ionizing photons traced by the [OIII]λ5007 line excite extra-nuclear nebulae out to distances of about 7kpc. These regions do not show bright stellar emission, but are rather dominated by nebular emission. These galaxies have nuclei classified as Seyfert in the literature. Approximately 40% of the pre-coalescence ULIRGs exhibit shifts between the peaks of their red continuum and that local to the [Oi]λ6300 line. However, some of these peaks are associated with the secondary stellar nucleus of the system. In contrast, the emission in post-coalescence ULIRGs is concentrated towards the nuclei. These results imply that evolution caused by a merger is ocurring in the ionized gas structure of ULIRGs.

Abstract Copyright:

Journal keyword(s): galaxies: interactions - galaxies: active - infrared: galaxies - techniques: spectroscopic

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 BD+33 26 * 00 19 04.6808346109 +34 29 11.973564021   10.00 9.23     G0 2 0
2 2MASX J06301333+3507498 H2G 06 30 13.332 +35 07 49.86           ~ 20 0
3 PSCz Q06487+2208 H2G 06 51 45.8 +22 04 27           ~ 31 0
4 NAME IRAS F08572+3915 NW LIN 09 00 25.364 +39 03 54.23     16.66     ~ 389 1
5 2MASS J09452922+1915486 Sy1 09 45 29.2306277280 +19 15 48.776302764   17.46 17.10     ~ 22 0
6 Feige 34 HS* 10 39 36.7358839104 +43 06 09.212615280 9.613 10.91 11.14 11.319 11.464 sdOp 637 0
7 2MASX J11113636+5334587 LIN 11 11 36.3453926088 +53 34 59.562127197           ~ 16 0
8 IC 694 G 11 28 27.312 +58 34 42.29   18.2       ~ 245 2
9 NAME NGC 3690 West GiP 11 28 30.69 +58 33 33.4   11.8       ~ 622 4
10 NGC 3690 IG 11 28 31.326 +58 33 41.80   13.19 12.86     ~ 931 4
11 NAME NGC 3690 East AGN 11 28 33.07 +58 33 54.2   11.8       ~ 625 4
12 LEDA 39024 LIN 12 13 46.107 +02 48 41.50           ~ 329 1
13 2MASX J12514092-1025242 G 12 51 40.920 -10 25 24.25           ~ 12 1
14 Mrk 231 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 1894 3
15 GD 153 WD* 12 57 02.3224909560 +22 01 52.634778240 11.883 13.060 13.349 13.488 13.669 DA1.2 333 0
16 2MASX J13181022+0419292 EmG 13 18 10.2114299688 +04 19 29.367069060           ~ 26 0
17 IRAS 13342+3932 Sy1 13 36 24.0619427808 +39 17 31.105014396     17.76     ~ 80 0
18 Mrk 273 Sy2 13 44 42.1883001096 +55 53 13.596220932   15.68 14.91     ~ 862 3
19 IRAS 13469+5833 H2G 13 48 40.0732515360 +58 18 52.024039452   17.5       ~ 43 0
20 Mrk 463 Sy2 13 56 02.9 +18 22 18   14.8 14.22     ~ 365 2
21 LEDA 84113 H2G 14 08 19.0356546744 +29 04 47.143121916           ~ 57 0
22 LEDA 52270 Sy1 14 37 38.2867288488 -15 00 24.087592692   16.58 16.40     ~ 257 1
23 IRAS 15206+3342 Sy2 15 22 38.104 +33 31 35.90           ~ 96 0
24 2MASX J15265942+3558372 LIN 15 26 59.442 +35 58 37.01   15.61       ~ 254 1
25 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2821 4
26 2MASX J16023279+3734532 LIN 16 02 32.798 +37 34 53.28           ~ 17 0
27 LEDA 60189 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 394 0
28 LEDA 62625 Sy2 18 58 13.813 +65 31 25.04   17.8       ~ 27 0
29 BD+28 4211 HS* 21 51 11.0221915656 +28 51 50.367627468 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 765 0

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2022.05.20-09:42:16

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