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Chemical Evolution of Spiral Galaxies from Redshift 4 to the Present

Published online by Cambridge University Press:  19 July 2016

U. Fritze - v. Alvensleben ,
U. Lindner  and
K. J. Fricke
U. Fritze - v. Alvensleben
Affiliation:
Universitäts-Sternwarte, Göttingen, Germany
U. Lindner
Affiliation:
Universitäts-Sternwarte, Göttingen, Germany
K. J. Fricke
Affiliation:
Universitäts-Sternwarte, Göttingen, Germany

Extract

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ISM abundances in nearby spiral galaxies are well known from HII region studies (Zaritsky et al. 1994). While early type spirals, Sa, Sb, have rather uniform abundances and a narrow range of present star formation rates (SFR) the galaxy-to-galaxy variations both in HII region abundances and in present SFR increase towards late spiral types Sc, Sd (see e.g. Kennicutt & Kent 1983). ISM abundances of spiral galaxies or their progenitors up to the highest redshifts can be studied via the absorption properties imprinted in the spectra of background QSOs. While MgII- and CIV- absorption lines are produced in the low column density gas of the extended haloes around galaxies, the Damped Lyα Absorption (DLA) is believed to originate in (proto-)galactic disks. High resolution spectroscopy of a large number of metal lines associated with DLA systems reveal the redshift evolution of ISM abundances from z ≳ 4 to z ~ 0.6.

Type
Conference Papers in order of Presentation
Information
Symposium - International Astronomical Union , Volume 187: Cosmic Chemical Evolution , 2002 , pp. 147 - 151
Copyright
Copyright © 2002 

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