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Nearby Hills ejecta as a probe of the gravitational potential of the Milky Way

Published online by Cambridge University Press:  14 May 2020

Y. Q. Zhang Open the ORCID record for Y. Q. Zhang [Opens in a new window] ,
M. C. Smith  and
P. J. McMillan
Y. Q. Zhang
Affiliation:
Ningbo University of Technology, Zhejiang325211, China email: yanqiongz@icloud.com Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai200030, China email: dr.mcsmith@me.com
M. C. Smith
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai200030, China email: dr.mcsmith@me.com
P. J. McMillan
Affiliation:
Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, SE-22100 Lund, Sweden email: paul@astro.lu.se
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Abstract

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Stars ejected from the Galactic Center can be used to place important constraints on the Milky Way potential. We have used Hills stars to constrain models for the Galactic potential, demonstrating that meaningful constraint can be obtained if we have samples of around 50 nearby Hills stars.

Keywords

stars: kinematicsgravitationblack hole physics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 54 - 56
Copyright
© International Astronomical Union 2020

References

Hills, J. G. 1988, Nature, 331, 687.CrossRefGoogle Scholar
Brown, W. R., Geller, M. J., Kenyon, S. J., & Kurtz, M. J. 2005, ApJ, 622, L33.CrossRefGoogle Scholar
Brown, W. R., Geller, M. J., & Kenyon, S. J. 2014, ApJ, 787, 89.10.1088/0004-637X/787/1/89CrossRefGoogle Scholar
Hirsch, H. A., Heber, U., O’Toole, S. J., et al. 2005, A&A, 444, L61Google Scholar
Edelmann, H., Napiwotzki, R., Heber, U., et al. 2005, ApJ (Letters), 634, L181Google Scholar
Zheng, Z., Carlin, J. L., Beers, T. C., et al. 2014, ApJ, 785, L23.CrossRefGoogle Scholar
Huang, Y., Liu, X.-W., Zhang, H.-W., et al. 2017, ApJ (Letters), 847, L9Google Scholar
Li, Y.-B., Luo, A.-L., Zhao, G., et al. 2018, ApJ, 156, 8710.3847/1538-3881/aad09aCrossRefGoogle Scholar
Heber, U., Edelmann, H., Napiwotzki, R., et al. 2008, A&A, 483, L21Google Scholar
Li, Y.-B., Luo, A.-L., Zhao, G., et al. 2015, Research in Astronomy and Astrophysics, 15, 1364CrossRefGoogle Scholar
Boubert, D., Guillochon, J., Hawkins, K., et al. 2018, MNRAS, 479, 2789CrossRefGoogle Scholar
McMillan, P. J. 2017, MNRAS, 465, 7610.1093/mnras/stw2759CrossRefGoogle Scholar
Koposov, S. E., Boubert, D., Li, T. S., et al. 2019, arXiv e-prints, arXiv:1907.11725Google Scholar
Zhang, Y., Smith, M. C., & Carlin, J. L. 2016, ApJ, 832, 10CrossRefGoogle Scholar