The Metallicity of Redshift 0.5<z<1 Field Galaxies

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dc.creatorCarollo, C. Marcella
dc.creatorLilly, Simon J.
dc.creatorStockton, Alan
dc.date2001-08-15
dc.date.accessioned2026-07-07T01:59:40Z
dc.date.available2026-07-07T01:59:40Z
dc.descriptionWe are undertaking a program to measure emission line ratios in a selected sample of $0.5 < z < 1.0$ CFRS starforming galaxies in order to compute their Interstellar Medium metallicities. The latter are derived by means of the empirically-calibrated $R_{23}$ estimator introduced by Pagel et al. (1979). Here we focus on a subsample of 15 galaxies with $L_{Hβ} > 1.2 \times 10^{41}$ erg s$^{-1}$. In addition to the optical CFHT spectra discussed in Carollo & Lilly (2001), where a preliminary account of this work can be found, in this paper we also refer to new $J$-band Keck spectroscopy of the $Hα$ and [NII]6583 lines for several objects. These lines allow us to break the degeneracy between low ($\lta 0.1Z_\odot$) and high ($\gta 0.5Z_\odot$) metallicity of the $R_{23}$ estimator, and put on solid ground the finding that the $0.5 < z < 1.0$ blue galaxies in the high-$L_{Hβ}$ sample are significantly metal-enriched ($Z \gta 0.3Z_\odot$ up to $Z_\odot$). Therefore, our results do not support previous suggestions in which the $0.5 < z < 1.0$ starforming galaxies are dwarf galaxies brightened by large bursts of star-formation, but support instead a picture where at least a significant fraction of them evolves to become today's massive metal-rich systems.
dc.description6 pages, 3 figures, to appear in "Chemical Enrichment of Intracluster and Intergalactic Medium", Vulcano, Italy, 14-18 May 2001, ASP Conference Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0108256
dc.identifierhttp://arxiv.org/abs/astro-ph/0108256
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3205
dc.subjectAstrophysics
dc.titleThe Metallicity of Redshift 0.5<z<1 Field Galaxies
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