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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
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: crx@shao.ac.cn
Shuhui Zhang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: crx@shao.ac.cn
Shiyin Shen
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: crx@shao.ac.cn
Jun Yin
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: crx@shao.ac.cn
Jinliang Hou
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai, 200030, China email: crx@shao.ac.cn
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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
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 ScholarPubMed
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