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Chemical Signature Of A Major Merger In The Early Formation Of The Small Magellanic Cloud by Takuji Tsujimoto; Kenji Bekki is a Physics and Astronomy article available to read on EtoBox.

What is Chemical Signature Of A Major Merger In The Early Formation Of The Small Magellanic Cloud about?

The formation history of the Small Magellanic Cloud (SMC) is unraveled based on the results of our new chemical evolution models constructed for the SMC, highlighting the observed anomaly in the age-metallicity relation for star clusters in the SMC. We first propose that evidence of a major merger is imprinted in the agemetallicity relation as a dip in [Fe/H]. Our models predict that the major merger with a mass ratio of 1:1 to 1:4 occurred at ∼7.5 Gyr ago, with a good reproduction of the abundance distribution function of field stars in the SMC. Furthermore, our models predict a relatively large scatter in [Mg/Fe] for -1.4 [Fe/H] -1.1 as a reflection of a looping feature resulting from the temporally inverse progress of chemical enrichment, which can be tested against future observational results. Given that the observed velocity dispersion (∼30 km s -1 ) of the SMC is much smaller than that (∼160 km s -1 ) of the Galactic halo, our finding strongly implies that the predicted merger event happened in a small group environment that was far from the Galaxy and contained a number of small gas-rich dwarfs comparable to the SMC. This theoretical view is extensively discussed in the fra

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Author

Takuji Tsujimoto; Kenji Bekki

Publisher

University of Chicago Press; American Astronomical Society; Institute of Physics Publishing; IOP Publishing; Oxford University Press (OUP) (ISSN 0004-637X)

Published

2009

Language

EN

Field

Physics and Astronomy (Physical Sciences)