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The Spatial Structure of the Galactic outer disk with LAMOST DR3 K giant stars

Published online by Cambridge University Press:  02 August 2018

Haifeng Wang Open the ORCID record for Haifeng Wang [Opens in a new window] ,
Chao Liu  and
Licai Deng
Haifeng Wang
Affiliation:
Key laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China; email: hfwang@bao.ac.cn University of Chinese Academy of Sciences, Beijing, 100012, China(UCAS)
Chao Liu
Affiliation:
Key laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China; email: hfwang@bao.ac.cn
Licai Deng
Affiliation:
Key laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China; email: hfwang@bao.ac.cn
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Abstract

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The spatial structure of the Milky Way outer disk is characterized with ~ 70000 LAMOST DR3 K giants after carefully correction of their selection effects. By slicing the data into various Galactocentric radius bins, we are able to fit the vertical stellar density profile with a models composed of two isothermal-sheet disks and an oblate power-law halo. We find that although the thin disk is significantly flared, the radial surface density profile can extend to as far as 19 kpc. Beyond 12 kpc, only one thicker disk, rather than two disk components, are found in the samples. Moreover, the residual of the density profiles after subtracting the best fit models show different oscillation patterns in almost all range of detecting radius.

Keywords

Galaxy: structureGalaxy: diskGalaxy: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 378 - 380
Copyright
Copyright © International Astronomical Union 2018 

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