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Detect the density profile with LAMOST K giants

Published online by Cambridge University Press:  02 August 2018

Yan Xu
Affiliation:
Key laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences Da Tun Road 20A, BeiJing 100012, China email: [email protected], [email protected]
Chao Liu
Affiliation:
Key laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences Da Tun Road 20A, BeiJing 100012, China email: [email protected], [email protected]
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Abstract

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The density distribution of the Milky Way halo is detected with 5351 LAMOST DR3 metal poor K giants using a nonparametric method. The nonparametric fitting method is a model independent way to estimate the halo density distribution while to a large extent avoiding the influence of the halo substucture. We show that the K giants density profile can be fitted well by single power law. We found no indication of a break in the power law index. The powerlaw index n = 5.0−0.64+0.64. The data show that the stellar halo is flattened at smaller radii, and becomes more spherical farther from the Galactic center. The flattening q(r=15Kpc)is about0.64, q(20Kpc) is about 0.8, q(30Kpc) is about 0.96.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

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