2010A&A...517A..85L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST20:17:25

2010A&A...517A..85L - Astronomy and Astrophysics, volume 517, A85-85 (2010/7-1)

Massive star formation in Wolf-Rayet galaxies. IV. Colours, chemical-composition analysis and metallicity-luminosity relations.

LOPEZ-SANCHEZ A.R. and ESTEBAN C.

Abstract (from CDS):

We have performed a comprehensive multiwavelength analysis of a sample of 20 starburst galaxies that show a substantial population of very young massive stars, most of them classified as Wolf-Rayet (WR) galaxies. In this paper, the forth of the series, we present the global analysis of the derived photometric and chemical properties.We compare optical/NIR colours and the physical properties (reddening coefficient, equivalent widths of the emission and underlying absorption lines, ionization degree, electron density, and electron temperature) and chemical properties (oxygen abundances and N/O, S/O, Ne/O, Ar/O, and Fe/O ratios) with previous observations and galaxy evolution models. We compile 41 independent star-forming regions - with oxygen abundances between 12+log(O/H)=7.58 and 8.75 -, of which 31 have a direct estimate of the electron temperature of the ionized gas. According to their absolute B-magnitude, many of them are not dwarf galaxies, but they should be during their quiescent phase. We found that both c(Hβ) and Wabs increase with increasing metallicity. The differences in the N/O ratio is explained assuming differences in the star formation histories. We detected a high N/O ratio in objects showing strong WR features (HCG 31 AC, UM 420, IRAS 0828+2816, III Zw 107, ESO 566-8 and NGC 5253). The ejecta of the WR stars may be the origin of the N enrichment in these galaxies. We compared the abundances provided by the direct method with those obtained through empirical calibrations, finding that (i) the Pilyugin method is the best suited empirical calibration for these star-forming galaxies; (ii) the relations provided by Pettini & Pagel (2004MNRAS.348L..59P) give acceptable results for objects with 12+log(O/H)>8.0; and (iii) the results provided by empirical calibrations based on photoionization models are systematically 0.2-0.3dex higher than the values derived from the direct method. The O and N abundances and the N/O ratios are clearly related to the optical/NIR luminosity; the dispersion of the data is a consequence of the differences in the star-formation histories. The L-Z relations tend to be tighter when using NIR luminosities, which facilitates distinguishing tidal dwarf galaxies candidates and pre-existing dwarf objects. Galaxies with redder colours tend to have higher oxygen and nitrogen abundances. Our detailed analysis is fundamental to understand the nature of galaxies that show strong starbursts, as well as to know their star formation history and the relationships with the environment. This study is complementary -but usually more powerful- to the less detailed analysis of large galaxy samples that are very common nowadays.

Abstract Copyright:

Journal keyword(s): galaxies: starburst - galaxies: interactions - galaxies: dwarf - galaxies: abundances - galaxies: photometry - stars: Wolf-Rayet

Simbad objects: 42

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Number of rows : 42

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 Mrk 960 bCG 00 48 35.430 -12 42 59.77   15.5       ~ 102 0
2 IRAS F02183+0019 AGN 02 20 54.530 +00 33 24.46   16.50       ~ 55 1
3 Mrk 1187 Sy1 02 48 22.0110598415 +13 56 06.016374107   17.24 16.33     ~ 23 0
4 Mrk 1087 AGN 04 49 44.469 +03 20 02.67   15.49 15.04     ~ 75 1
5 2MFGC 4113 G 05 01 35.550 -04 15 47.42   15.35   14.73   ~ 58 0
6 HCG 31 CGG 05 01 37 -04 15.4           ~ 123 0
7 HCG 31e G 05 01 37.5 -04 15 57           ~ 24 0
8 NGC 1741 IG 05 01 38.3 -04 15 25   13.7   13.02 13.6 ~ 250 0
9 HCG 31f1 PoG 05 01 39.71 -04 16 22.2           ~ 10 0
10 HCG 31f G 05 01 40.0 -04 16 22           ~ 20 0
11 HCG 31f2 PoG 05 01 40.15 -04 16 27.5           ~ 9 0
12 IC 399 EmG 05 01 44.083 -04 17 19.28   15.0 14.8     ~ 65 0
13 Mrk 5 H2G 06 42 15.9 +75 37 40   17.0       ~ 108 0
14 Mrk 1199 GiG 07 23 43.462 +33 26 31.22   13.7 13.13     ~ 103 0
15 2MASX J08235499+2806223 EmG 08 23 54.9669334368 +28 06 21.605409814   15.5       ~ 55 0
16 2MASX J08382309+6507160 SBG 08 38 23.093 +65 07 16.05     14.16     ~ 116 1
17 LB 555 EmG 09 30 06.437 +60 26 53.34   17.0       ~ 34 0
18 LEDA 26955 G 09 30 09.041 +60 28 05.37           ~ 44 0
19 SBSG 0926+606B GiP 09 30 09.6 +60 28 04   18.0       ~ 12 0
20 APG 252 IG 09 44.8 -19 41           ~ 12 0
21 ESO 566-7 IG 09 44 58.4 -19 43 32   15.36   14.66   ~ 15 0
22 ESO 566-8 IG 09 44 59.65 -19 42 45.6   15.56   14.59   ~ 29 0
23 LEDA 28398 EmG 09 51 31.7633448632 +52 59 36.023024415   18       ~ 44 0
24 ESO 436-42 EmG 10 34 38.727 -28 34 59.80   14.44 14.41 13.26   ~ 49 0
25 VV 747 IG 10 57 47.0 +36 15 26           ~ 7 1
26 MCG+06-24-038 G 10 57 47.0058448322 +36 15 38.809066317   15.5 16     ~ 39 1
27 POX 4b EmO 11 51 11.0 -20 35 58           ~ 4 1
28 6dFGS gJ115111.7-203557 H2G 11 51 11.7 -20 35 56   15.67   15.35   ~ 81 1
29 LEDA 39055 EmG 12 14 02.479 +53 45 17.35   18       ~ 68 0
30 NGC 5113 G 13 21 22.4 +57 41 28   15.2       ~ 19 0
31 LEDA 2816050 G 13 21 22.6 +57 41 29   18.5       ~ 26 0
32 2MASX J13212499+5741501 GiP 13 21 24.045 +57 41 40.13   18.5       ~ 27 0
33 SBSG 1319+579C G 13 21 25.10 +57 42 38.0           ~ 17 0
34 KSRWR HII-2 H2G 13 39 55.9 -31 38 24           ~ 25 0
35 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1269 4
36 KSRWR HII-1 H2G 13 39 56.00 -31 38 25.8           ~ 17 0
37 [HCG2004] NGC 5253 C 4 H2G 13 39 56.020 -31 38 27.89           ~ 31 0
38 MCG+07-29-060 QSO 14 17 01.716 +43 30 13.52   15.6       ~ 152 0
39 NGC 5561 rG 14 17 22.815 +58 45 02.06   16.0       ~ 14 0
40 ESO 513-11 PaG 15 00 27.10 -26 26 57.0   15.85       ~ 52 0
41 LEDA 71605 EmG 23 30 09.7 +25 31 56   15.0       ~ 52 0
42 [LER2004] Mrk 1087 N G ~ ~   17.58       ~ 3 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-20:17:25

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