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2003ApJ...599.1006K - Astrophys. J., 599, 1006-1030 (2003/December-3)
The DEEP Groth Strip Survey. VII. The metallicity of field galaxies at 0.26 < z < 0.82 and the evolution of the luminosity-metallicity relation.
KOBULNICKY H.A., WILLMER C.N.A., PHILLIPS A.C., KOO D.C., FABER S.M., WEINER B.J., SARAJEDINI V.L., SIMARD L. and VOGT N.P.
Abstract (from CDS):
Subsets of DGSS galaxies binned by redshift also exhibit L-Z correlations with slopes and zero points that evolve smoothly with redshift. DGSS galaxies in the highest redshift bin (z=0.6-0.82) are brighter, on average, by ∼1 mag at fixed metallicity than those in the lowest DGSS redshift bin (z=0.26-0.40) and by up to ∼2.4 mag compared to local (z<0.1) emission-line field galaxies. Alternatively, DGSS galaxies in the highest redshift bin (z=0.6-0.82) are, on average, 40% (0.15 dex) more metal-poor at fixed luminosity than local (z<0.1) emission-line field galaxies. For 0.6<z<0.8 galaxies, the offset from the local L-Z relation is greatest for objects at the low-luminosity (MB>-19) end of the sample and is vanishingly small for objects at the high-luminosity end of the sample (MB~-22). We compare these data to simple single-zone, exponential-infall PÉGASE2 models, which follow the chemical and luminous evolution of galaxies from formation to z=0. A narrow range of model parameters can qualitatively produce the slope of the L-Z relation and the observed evolution of slope and zero point with redshift when at least two of the following are true: (1) low-mass galaxies have lower effective chemical yields than massive galaxies, (2) low-mass galaxies assemble on longer timescales than massive galaxies, and (3) low-mass galaxies begin the assembly process at a later epoch than massive galaxies. The single-zone models do a reasonable job of reproducing the observed evolution for the low-luminosity galaxies (MB~-19) in our sample but fail to predict the relative lack of evolution in the L-Z plane observed for the most luminous galaxies (MB~-22). More realistic multizone models will be required to explain the chemoluminous evolution of large galaxies.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Abundances - Galaxies: Evolution - Galaxies: Fundamental Parameters - Galaxies: Starburst - ISM: H II Regions - ISM: Abundances
VizieR on-line data: <Available at CDS (J/ApJ/599/1006): table1.dat>
Errata: erratum, vol. 610, p. 1234 (2004)
CDS comments: t. 1 : col (1) : numbering not used in SIMBAD, col (2) : ID is DEEP-GSS
Simbad objects: 70
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