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Mean age gradient and asymmetry in the star formation history of the small magellanic cloud

Citation

Cignoni, M and Cole, AA and Tosi, M and Gallagher, JS and Sabbi, E and Anderson, J and Grebel, EK and Nota, A, Mean age gradient and asymmetry in the star formation history of the small magellanic cloud, Astrophysical Journal, 775, (2) Article 83. ISSN 0004-637X (2013) [Refereed Article]


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Copyright Statement

Copyright 2013 The American Astronomical Society. All rights reserved.

DOI: doi:10.1088/0004-637X/775/2/83

Abstract

We derive the star formation history (SFH) in four regions of the Small Magellanic Cloud (SMC) using the deepest VI color-magnitude diagrams (CMDs) ever obtained for this galaxy. The images were obtained with the Advanced Camera for Surveys on board the Hubble Space Telescope (HST) and are located at projected distances of 0fdg5-2° from the SMC center, probing the main body and the wing of the galaxy. We derived the SFHs of the four fields using two independent procedures to fit synthetic CMDs to the data. We compare the SFHs derived here with our earlier results for the SMC bar to create a deep pencil-beam survey of the global history of the central SMC. We find in all the six fields observed with HST a slow star formation (SF) pace from 13 to 5-7 Gyr ago, followed by a ≈2-3 times higher activity. This is remarkable because dynamical models do not predict a strong influence of either the Large Magellanic Cloud (LMC) or the Milky Way at that time. The level of the intermediate-age SF rate enhancement systematically increases toward the center, resulting in a gradient in the mean age of the population, with the bar fields being systematically younger than the outer ones. SF over the most recent 500 Myr is strongly concentrated in the bar, the only exception being the area of the SMC wing. The strong current activity of the latter is likely driven by interaction with the LMC. At a given age, there is no significant difference in metallicity between the inner and outer fields, implying that metals are well mixed throughout the SMC. The age-metallicity relations we infer from our best-fitting models are monotonically increasing with time, with no evidence of dips. This may argue against the major merger scenario proposed by Tsujimoto and Bekki in 2009, although a minor merger cannot be ruled out.

Item Details

Item Type:Refereed Article
Keywords:galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: individual (Small Magellanic Cloud); galaxies: star formation; galaxies: stellar content; galaxies: structure; Hertzsprung-Russell and C-M diagrams; Magellanic Clouds; stars: st
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Cosmology and Extragalactic Astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Cole, AA (Associate Professor Andrew Cole)
ID Code:87033
Year Published:2013
Web of Science® Times Cited:28
Deposited By:Mathematics and Physics
Deposited On:2013-11-06
Last Modified:2017-11-30
Downloads:20 View Download Statistics

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