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Why do disk galaxies present a common gas-phase metallicity gradient?

Published online by Cambridge University Press:  21 March 2017

R. Chang ,
Shuhui Zhang ,
Shiyin Shen ,
Jun Yin  and
Jinliang Hou
R. Chang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: [email protected]
Shuhui Zhang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: [email protected]
Shiyin Shen
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: [email protected]
Jun Yin
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: [email protected]
Jinliang Hou
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: [email protected]
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CALIFA data show that isolated disk galaxies present a common gas-phase metallicity gradient, with a characteristic slope of -0.1dex/re between 0.3 and 2 disk effective radius re (Sanchez et al. 2014). Here we construct a simple model to investigate which processes regulate the formation and evolution.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 134
Copyright
Copyright © International Astronomical Union 2017 

References

Chang, R. X., Shen, S. Y., & Hou, J. L. 2012, ApJL, 753, L10 CrossRefGoogle Scholar
Sanchez, S. F., Rosales-Ortega, F. F., Iglesias-Paramo, J., et al. 2014, A&A, 563, 49 Google Scholar