2011A&A...529A.149G


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.19CET18:16:02

2011A&A...529A.149G - Astronomy and Astrophysics, volume 529A, 149-149 (2011/5-1)

VLT spectroscopy of low-metallicity emission-line galaxies: abundance patterns and abundance discrepancies.

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

Abstract (from CDS):

We present deep spectroscopy of a large sample of low-metallicity emission-line galaxies. The main goal of this study is to derive element abundances in these low-metallicity galaxies. We analyze 121 VLT spectra of HII regions in 46 low-metallicity emission-line galaxies. Of these spectra 83 are archival VLT/FORS1+UVES spectra of HII regions in 31 low-metallicity emission-line galaxies that are studied for the first time with standard direct methods to determine the electron temperatures, the electron number densities, and the chemical abundances. The oxygen abundance of the sample lies in the range 12+logO/H=7.2-8.4. We confirm previous findings that Ne/O increases with increasing oxygen abundance, likely because of a higher depletion of oxygen in higher-metallicity galaxies. The Fe/O ratio decreases from roughly solar at the lowest metallicities to about one tenth of solar, indicating that the degree of depletion of iron into dust grains depends on metallicity. The N/O ratio in extremely low-metallicity galaxies with 12+logO/H<7.5 shows a slight increase with decreasing oxygen abundance, which could be the signature of enhanced production of primary nitrogen by rapidly rotating stars at low metallicity. We present the first empirical relation between the electron temperature derived from [SIII]λ6312/λ9069 or [NII]λ5755/λ6583 and the one derived from [OIII]λ4363/λ(4959+5007) in low-metallicity galaxies. We also present an empirical relation between te derived from [OII]λ3727/(λ7320+λ7330) or [SII]λ4068/(λ6717+λ6730) and [OIII]λ4363/λ(4959+5007). The electron number densities Ne(ClIII) and Ne(ArIV) were derived in a number of objects and are found to be higher than Ne(OII) and Ne(SII). This has potential implications for the derivation of the pregalactic helium abundance. In a number of objects, the abundances of C++ and O++ could be derived from recombination lines. Our study confirms the discrepancy between abundances found from recombination lines (RLs) and collisionally excited lines (CELs) and that C/O increases with O/H.

Abstract Copyright:

Journal keyword(s): galaxies: starburst - methods: observational - galaxies: abundances - galaxies: dwarf - galaxies: ISM

VizieR on-line data: <Available at CDS (J/A+A/529/A149): tables 1-10>

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 - 2020
#notes
1 2MASX J00313427-0209165 AGN 00 31 34.276 -02 09 16.57   17   16.01   ~ 19 0
2 LEDA 3034 Sy1 00 51 49.409 +00 33 53.02   17.22 16.65     ~ 31 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9111 1
4 NGC 346 Cl* 00 59 05.090 -72 10 33.24           ~ 441 0
5 NGC 456 HII 01 13 44.4 -73 17 26           ~ 112 0
6 LIN 500 Em* 01 13 50.896 -73 18 01.03   13.36 12.5 13.78 14.62 ~ 62 0
7 LHA 115-N 83C SNR 01 14 00.0 -73 17 08           ~ 67 0
8 MCG+01-05-030 H2G 01 44 41.3 +04 53 26 15.07 15.50 15.16 14.86 14.58 ~ 77 0
9 LEDA 7422 EmG 01 58 09.388 -00 06 37.22           ~ 29 0
10 LEDA 8377 H2G 02 11 23.5 +02 20 30   18       ~ 39 0
11 UM 417 EmO 02 19 30.236 -00 59 06.46 17.71 18.15 17.57 17.44 17.35 ~ 28 0
12 UVQS J022054.52+003324.3 AGN 02 20 54.530 +00 33 24.46   16.50       ~ 55 1
13 Mrk 600 G 02 51 04.57 +04 27 13.9 14.76 15.07 14.70 14.50 14.29 ~ 115 0
14 [PBT2001] SBSG 0335-052 W G 03 37 38.40 -05 02 37.5   19.14     18.85 ~ 97 1
15 SBSG 0335-052B G 03 37 44.04 -05 02 40.2   16.77 16.65   16.79 ~ 140 1
16 Cambridge 0357-392 H2G 03 59 08.90 -39 06 23.0           ~ 20 0
17 SCHG 0513-393 H2G 05 15 19.7789 -39 17 41.149           ~ 18 0
18 [GPM2009] J0519+0007 G 05 19 02.6953532514 +00 07 29.106797166           ~ 20 0
19 SCHG 0618-402 H2G 06 20 03.8353 -40 16 42.997           ~ 25 0
20 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 484 3
21 NGC 3125 H2G 10 06 33.318 -29 56 07.32 13.03 13.45 13.00 12.50 13.4 ~ 212 1
22 IC 630 GiP 10 38 33.6294325169 -07 10 14.545721683   13.3   12.9 12.3 ~ 55 0
23 Mrk 1271 EmG 10 56 09.1156462299 +06 10 22.394369445   14.8       ~ 50 0
24 6dFGS gJ115111.7-203557 H2G 11 51 11.7 -20 35 56   15.67   15.35   ~ 80 1
25 LEDA 39402 H2G 12 17 17.093 -28 02 32.67   17       ~ 123 0
26 ESO 380-27 H2G 12 25 46.9 -36 14 01   17.47   16.52   ~ 95 1
27 6dFGS gJ125306.0-031300 AGN 12 53 05.965 -03 12 58.88   16.64   16.05   ~ 26 0
28 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1247 4
29 Tol 89 HII 14 01 20.082 -33 04 11.06           ~ 37 1
30 NGC 5408 EmG 14 03 20.907 -41 22 39.75   12.59   11.96 12.2 ~ 307 3
31 ESO 513-11 PaG 15 00 27.10 -26 26 57.0   15.85       ~ 52 0
32 ESO 338-4 IG 19 27 58.338 -41 34 30.81   13.55 13.21 13.14 13.43 ~ 204 1
33 [H25] V HII 19 44 52.84 -14 43 09.8           ~ 57 0
34 NGC 6822 G 19 44 56.199 -14 47 51.29   18 8.1     ~ 1408 0
35 KD D26 HII 19 45 05.2 -14 43 13           ~ 46 0
36 SCHG 2138-405 AGN 21 41 21.960 -40 18 54.69   17.68   17.62   ~ 21 1
37 LEDA 85193 H2G 21 49 48.2196 -38 54 08.587           ~ 19 0
38 [GPM2009] PHL293B EmG 22 30 36.8 -00 06 37           ~ 13 1
39 SCHG 2240-384 H2G 22 43 32.3816 -38 11 23.851           ~ 10 0
40 NGC 7667 H2G 23 24 22.839 -00 06 30.16 13.52 14.47 14.05 13.89 13.58 ~ 63 1

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2019.11.19-18:16:02

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