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The Velocity Distribution in the Solar Neighborhood from LAMOST Pilot Survey

Published online by Cambridge University Press:  06 January 2014

Qiran Xia ,
Chao Liu ,
Yan Xu ,
Shude Mao  and
Shuang Gao
Qiran Xia
Affiliation:
National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China email: [email protected] University of Chinese Academy of Sciences, Beijing 100049, China
Chao Liu
Affiliation:
National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China email: [email protected] Key Laboratory of Optical Astronomy, National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China
Yan Xu
Affiliation:
National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China email: [email protected] Key Laboratory of Optical Astronomy, National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China
Shude Mao
Affiliation:
National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China email: [email protected] Jodrell Bank Centre for Astrophysics, The University of Manchester, Alan Turing Building, Manchester M13 9PL, UK
Shuang Gao
Affiliation:
National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China email: [email protected] Key Laboratory of Optical Astronomy, National Astronomical Observatories, CAS, 20A Datun Road, Chaoyang District, 100012, Beijing, China
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Abstract

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We use 63,774 F/G dwarf stars from the LAMOST pilot survey to explore the velocity distribution in the solar neighborhood. The intrinsic UV distribution is reconstructed with a 20-Gaussian model using extreme deconvolution. We find at least two arcs, one extending from (−106, −3) to (94, −27) km/s and the other from (29, −9) to (78, −51) km/s. The arcs are qualitatively consistent with numerical simulations of the resonance induced by the Galactic bar and can be used to constrain its dynamical properties.

Keywords

Solar NeighbourhoodStarsVelocities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S298: Setting the scene for Gaia and LAMOST , May 2013 , pp. 447
Copyright
Copyright © International Astronomical Union 2014 

References

Antoja, T., et al. 2011, MNRAS, 418, 1423CrossRefGoogle Scholar
Antoja, T., et al. 2011, MNRAS, 426L, 1Google Scholar
Bovy, J., Hogg, D. W., & Roweis, S. T. 2009, astro-ph, 0905.2979Google Scholar
Dehnen, W. 2000, AJ, 119, 800CrossRefGoogle Scholar
Fux, R. 2001, A&A, 373, 511Google Scholar
Hou, J., Chang, R., & Fu, C. 1998, ASP-CS, 138, 143Google Scholar
Quillen, A. C., et al. 2011, MNRAS, 417, 762CrossRefGoogle Scholar
Roeser, S., Demleitner, M., & Schilbach, E. 2010, AJ, 139, 2440CrossRefGoogle Scholar
Zhao, J., et al. 2009, ApJ, 692, L113CrossRefGoogle Scholar