2012A&A...541A.115G


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.14CET19:00:22

2012A&A...541A.115G - Astronomy and Astrophysics, volume 541A, 115-115 (2012/5-1)

VLT/X-shooter observations of blue compact galaxies Haro 11 and ESO 338-IG 004.

GUSEVA N.G., IZOTOV Y.I., FRICKE K.J. and HENKEL C.

Abstract (from CDS):

Strongly star-forming galaxies of subsolar metallicities are typical of the high-redshift universe. Here we therefore provide accurate data for two low-z analogs, the well-known low-metallicity emission-line galaxies Haro 11 and ESO 338-IG 004. Our main goal is to derive their spectroscopic properties and to examine whether a previously reported near-infrared (NIR) excess in Haro 11 can be confirmed. On the basis of Very Large Telescope/X-shooter spectroscopic observations in the wavelength range ~λλ3000-24000Å, we use standard direct methods to derive physical conditions and element abundances. Furthermore, we use X-shooter data together with Spitzer observations in the mid-infrared range to attempt to find hidden star formation. We derive interstellar oxygen abundances of 12+logO/H=8.33±0.01, 8.10±0.04, and 7.89±0.01 in the two HII regions B and C of Haro 11 and in ESO 338-IG 004, respectively. The observed fluxes of the hydrogen lines correspond to the theoretical recombination values after correction for extinction with a single value of the extinction coefficient C(Hβ) across the entire wavelength range from the near-ultraviolet to the NIR and mid-infrared for each of the studied H ii regions. Thus, we confirm our previous findings obtained for several low-metallicity emission-line galaxies (Mrk 59, II Zw 40, Mrk 71, Mrk 996, SBS 0335-052E, PHL 293B, and GRB HG 031203) that the extinction coefficient C(Hβ) is not higher in the NIR than in the optical range and therefore that there are no emission-line regions contributing to the line emission in the NIR range, which are hidden in the optical range. The agreement between the extinction-corrected and CLOUDY-predicted fluxes implies that a H ii region model including only stellar photoionisation is able to account for the observed fluxes, in both the optical and NIR ranges. No additional excitation mechanism such as shocks from stellar winds and supernova remnants is needed. All observed spectral energy distributions (SEDs) can be reproduced quite well across the whole wavelength range by model SEDs except for Haro 11B, where there is a continuum flux excess at wavelengths >1.6µm. It is possible that one or more red supergiant stars are responsible for the NIR flux excess in Haro 11B. We find evidence of a luminous blue variable (LBV) star in Haro 11C.

Abstract Copyright:

Journal keyword(s): galaxies: fundamental parameters - galaxies: starburst - galaxies: ISM - galaxies: abundances - stars: activity

Simbad objects: 20

goto Full paper

goto View the reference in ADS

Number of rows : 20

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 ESO 350-38 AGN 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 282 0
2 [VFT93] 0034-3349C HXB 00 36 52.660 -33 33 17.07           ~ 17 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9107 1
4 UGC 549 G 00 54 42.26 +36 45 53.4   15.70       ~ 34 0
5 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 355 1
6 QSO B0125-0635 QSO 01 27 35.5241670251 -06 19 35.428005150 14.75 15.05 14.48 14.06 13.70 ~ 85 0
7 SBSG 0335-052B G 03 37 44.04 -05 02 40.2   16.77 16.65   16.79 ~ 140 1
8 M 42 HII 05 35 17.3 -05 23 28           ~ 3658 0
9 UGCA 116 H2G 05 55 42.645 +03 23 32.23 10.74 11.68 11.46   11.82 ~ 492 0
10 NGC 2363A HII 07 28 42.8 +69 11 21           ~ 536 3
11 [DRR96] NGC 2363 V1 V* 07 28 43.37 +69 11 23.9   17.82 17.88     ~ 32 1
12 NGC 2366 H2G 07 28 51.85 +69 12 31.1 12.25 11.86 11.39 11.33   ~ 687 0
13 Anon J080230-3951 G 08 02 30.20 -39 51 03.0 22.31 22.32 20.53 20.44 19.40 ~ 20 0
14 UGC 5340 G 09 56 46.047 +28 49 43.77 14.82 14.74 14.59 14.55   ~ 170 1
15 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2150 0
16 Mrk 59 AGN 12 59 00.288 +34 50 42.45           ~ 309 2
17 ESO 338-4 IG 19 27 58.338 -41 34 30.81   13.55 13.21 13.14 13.43 ~ 204 1
18 [GPM2009] PHL293B EmG 22 30 36.8 -00 06 37           ~ 13 1
19 Feige 110 HS* 23 19 58.3995050606 -05 09 56.170282845 10.360 11.45 11.50 11.970 12.145 sdO8VIIIHe5 537 1
20 [OBR98] Inner23 GlC ~ ~           ~ 14 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2012A&A...541A.115G and select 'bookmark this link' or equivalent in the popup menu


2019.11.14-19:00:22

© Université de Strasbourg/CNRS

    • Contact