2006MNRAS.369..891M

Query : 2006MNRAS.369..891M

2006MNRAS.369..891M - Mon. Not. R. Astron. Soc., 369, 891-908 (2006/June-3)

The metallicities of luminous, massive field galaxies at intermediate redshifts.

MOUHCINE M., BAMFORD S.P., ARAGON-SALAMANCA A., NAKAMURA O. and MILVANG-JENSEN B.

Abstract (from CDS):

We derive oxygen abundances for a sample of 40 luminous (M_B_≲ -19), star-forming, mostly disc, field galaxies with redshifts in the range 0.2 ≲ z ≲ 0.8, with a median of <z> = 0.45. Oxygen abundances, relative to hydrogen, of the interstellar emitting gas are estimated by means of the empirically calibrated strong emission-line ratio technique. The derived 12 + log (O/H) values range from 8.4 to 9.0, with a median of 8.7. Twenty of these galaxies have securely measured rotation velocities, in the range 50-244 km/s.

The measured emission-line equivalent widths and diagnostic ratios for the intermediate redshift galaxies cover similar ranges to those observed across a large sample of local galaxies. The estimated oxygen abundances for our luminous star-forming intermediate redshift galaxies cover the same range as their local counterparts. However, at a given galaxy luminosity, many of our galaxies have significantly lower oxygen abundances, i.e. 12 + log (O/H) ∼8.6, than local galaxies with similar luminosities. Interestingly, these luminous, massive, intermediate redshift, star-forming galaxies with low oxygen abundances exhibit physical conditions, i.e. emission-line equivalent width and ionization state, very similar to those of local faint and metal-poor star-forming galaxies. The oxygen abundance of the interstellar gas does not seem to correlate with the maximum rotation velocity or the emission scalelength of the parent galaxy. This suggests that there is diversity in the intrinsic properties of the massive field galaxy population at intermediate redshifts.

The distribution of the colour excess, derived from the ratio of extinction-uncorrected Hβ and [Oii]λ3727 star formation rate indicators, covers a similar range to that observed locally, but exhibits a lower mean than is observed for local optically selected star-forming galaxies. Luminous field galaxies at intermediate redshifts show similar star formation rates to their local counterparts. However, metal-poor, massive, star-forming galaxies tend to be systematically less affected by internal reddening than metal-rich, massive galaxies, which cover similar range of colour excess to local metal-rich luminous galaxies. Finally, the correlation between oxygen abundance and colour excess for intermediate redshift galaxies is found to be similar to what is observed locally. This result indicates that the dust content of galaxies is more regulated by their chemical evolution rather than by galaxy luminosity.


Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS

Journal keyword(s): galaxies: abundances - galaxies: evolution - galaxies: fundamental parameters

Nomenclature: Tables 1, 2: [MBA2006b] NN (Nos 1-44).

Simbad objects: 45

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Number of rows : 45
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 [NAM2006] J001815.6+162504 EmG 00 18 15.60 +16 25 03.7           ~ 3 0
2 [NAM2006] J001817.2+162534 GiC 00 18 17.15 +16 25 33.3           ~ 3 0
3 [MBA2006b] 36 G 00 18 18.203 +16 23 57.89       21.22   ~ 3 0
4 [NAM2006] J001819.2+162543 EmG 00 18 19.18 +16 25 43.2           ~ 3 0
5 CNOC MS 0015 100972 EmG 00 18 20.99 +16 26 13.3           ~ 3 0
6 [NAM2006] J001827.0+162658 G 00 18 27.0 +16 26 59           ~ 2 0
7 [NAM2006] J001832.8+162609 G 00 18 32.8 +16 26 10           ~ 3 0
8 [NAM2006] J001832.8+162218 GiC 00 18 32.89 +16 22 18.9           ~ 4 0
9 [NAM2006] J001837.8+162455 G 00 18 37.8 +16 24 56           ~ 2 0
10 [MBA2006b] 14 G 00 56 46.3 -27 42 50           ~ 1 0
11 [MBA2006b] 16 G 00 56 47.2 -27 38 33           ~ 1 0
12 [MBA2006b] 11 G 00 56 48.2 -27 40 13           ~ 1 0
13 [MBA2006b] 12 G 00 56 48.6 -27 40 01           ~ 2 0
14 [MBA2006b] 15 G 00 56 50.9 -27 38 01           ~ 1 0
15 [MBA2006b] 17 G 00 56 55.6 -27 39 08           ~ 1 0
16 [MBA2006b] 13 G 00 56 58.9 -27 43 53           ~ 1 0
17 [MBA2006b] 10 G 00 56 59.1 -27 40 41           ~ 1 0
18 [MBA2006b] 19 G 00 57 07.9 -27 39 28           ~ 1 0
19 [MBA2006b] 18 G 00 57 11.5 -27 39 48           ~ 1 0
20 [MBA2006b] 3 G 02 39 48.1 -01 38 16           ~ 1 0
21 [LRB2019] 5398 EmG 02 39 51.8261 -01 35 21.544           ~ 4 0
22 [MBA2006b] 5 G 02 39 54.5 -01 35 04           ~ 1 0
23 [BMA2005] A370-650 GiC 02 39 57.8726 -01 33 10.592           ~ 3 0
24 [MBA2006b] 6 G 02 40 00.9 -01 36 16           ~ 1 0
25 [MBA2006b] 4 G 02 40 03.6 -01 37 56           ~ 1 0
26 [MBA2006b] 7 G 02 40 06.7 -01 36 55           ~ 1 0
27 [MBA2006b] 20 G 04 43 06.7 +02 12 15           ~ 1 0
28 [MBA2006b] 21 G 04 43 14.4 +02 10 30           ~ 1 0
29 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 458 0
30 [MBA2006b] 27 G 10 57 01.2 -03 34 20           ~ 1 0
31 [NAM2006] J162336.0+263417 G 16 23 36.0 +26 34 17           ~ 2 0
32 [MBA2006b] 40 GiC 16 23 40.1218 +26 34 04.278           ~ 3 0
33 [NAM2006] J162342.6+263114 G 16 23 42.6 +26 31 14           ~ 2 0
34 [MBA2006b] 30 G 18 32 06.0 +16 25 22           ~ 1 0
35 [NAM2006] J205619.6-043847 GiC 20 56 19.6 -04 38 48           ~ 3 0
36 [MBA2006b] 24 G 20 56 20.2 -04 37 50           ~ 1 0
37 [MBA2006b] 23 G 20 56 22.4 -04 37 49           ~ 1 0
38 [MBA2006b] 25 G 20 56 22.6 -04 41 32           ~ 1 0
39 [MBA2006b] 22 G 20 56 23.2 -04 34 41           ~ 1 0
40 [MBA2006b] 26 G 20 56 24.4 -04 39 53           ~ 1 0
41 [NAM2006] J205624.9-043737 G 20 56 24.9 -04 37 38           ~ 2 0
42 [NAM2006] J205625.2-043559 G 20 56 25.2 -04 36 00           ~ 2 0
43 [NAM2006] J205632.5-043627 G 20 56 32.5 -04 36 27           ~ 2 0
44 [MBA2006b] 8 G 22 58 33.7 -34 47 43           ~ 1 0
45 [MBA2006b] 9 G 22 58 41.9 -34 47 21           ~ 1 0

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