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The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies

By Maria-rosa L. Cioni

Abstract

Context. The stellar metallicity and its gradient pose constraints to the formation and evolution of galaxies. Aims. This is a study of the metallicity gradient of the LMC, SMC and M33 galaxies derived from their asymptotic giant branch (AGB) stars. Methods. The [Fe/H] abundance was derived from the ratio between C- and M-type AGB stars and its variation analysed as a function of galactocentric distance. Galaxy structure parameters were adopted from the literature. Results. The metallicity of the LMC decreases linearly as−0.047±0.003 dex kpc −1 out to ∼ 8 kpc from the centre. In the SMC, [Fe/H] has a constant value of∼−1.25±0.01 dex up to ∼ 12 kpc. The gradient of the M33 disc, until ∼ 9 kpc, is−0.078±0.003 dex kpc −1 while an outer disc/halo, out to∼25 kpc, has [Fe/H]∼−1.7 dex. Conclusions. The metallicity of the LMC, as traced by different populations, bears the signature of two major star forming episodes: the first one constituting a thick disc/halo population and the second one a thin disc and bar due to a close encounter with the MW and SMC. The [Fe/H] of the recent episode supports an LMC origin for the Stream. The metallicity of the SMC supports star formation, ∼ 3 Gyr ago, as triggered by LMC interaction and sustained by the bar in the outer region of the galaxy. The SMC [Fe/H] agrees with the present-day abundance in the Bridge and shows no significant gradient. The metallicity of M33 supports an “inside-out ” disc formation via accretion of metal poor gas from the interstellar medium. Key words. Keywords should be given 1

Year: 2009
OAI identifier: oai:CiteSeerX.psu:10.1.1.316.1458
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