Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-14T18:32:33.903Z Has data issue: false hasContentIssue false
  • English
  • Français

A comparison of star formation history between NGC 300 and M33

Published online by Cambridge University Press:  10 June 2020

Xiaoyu Kang ,
Fenghui Zhang  and
Ruixiang Chang
Xiaoyu Kang
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China email: kxyysl@ynao.ac.cn Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, P. R. China
Fenghui Zhang
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China email: kxyysl@ynao.ac.cn Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, P. R. China
Ruixiang Chang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

NGC 300 is a near-optical twin of the Local Group galaxy M33, which are benchmarks for understanding late-type spiral galaxies. They are two bulgeless and low-mass spiral galaxies in different environments. In order to explore the common properties and differences between the two nearby low-mass systems, we first use the simple chemical evolution model to explore the star formation history (SFH) of NGC300 and M33, and then compare the feasible model predicted SFH of NGC 300 with that of M33. Through comparing the SFHs between them, it can be found that the mean stellar age of NGC 300 is older than that of M33, there is a recent lack of primordial gas infall onto the disk of NGC 300, recent star formation along the disk of NGC 300 is less active than that of M33, and the local environment may play a key role in the secular evolution of a galaxy.

Keywords

galaxies: evolutiongalaxies: spiralgalaxies: individual: NGC 300 and M33
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 275 - 276
Copyright
© International Astronomical Union 2020

References

Guglielmo, V., Poggianti, B. M., Moretti, A., et al. 2015, MNRAS, 450, 274910.1093/mnras/stv757CrossRefGoogle Scholar
Kang, X. Y., Zhang, F. H., Chang, R. X., et al. 2016, A&A, 585, A20Google Scholar
Kang, X. Y., Chang, R. X., Yin, J., et al. 2012, MNRAS, 426, 145510.1111/j.1365-2966.2012.21778.xCrossRefGoogle Scholar
Leroy, A. K., Walter, F., Brinks, E., et al. 2008, AJ, 136, 278210.1088/0004-6256/136/6/2782CrossRefGoogle Scholar