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Open cluster study in LAMOST DR3

Published online by Cambridge University Press:  02 August 2018

Jing Zhong
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, China email: jzhong@shao.ac.cn
Li Chen
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, China email: jzhong@shao.ac.cn
Chaoli Zhang
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, China email: jzhong@shao.ac.cn Rheinische Friedrich-Wilhelms-Universitat Bonn Argelander-Institut fur Astronomie Bonn, Nordrhein-Westfalen, Germany
Zhengyi Shao
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, China email: jzhong@shao.ac.cn
Jinliang Hou
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, China email: jzhong@shao.ac.cn
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Abstract

In studying Galactic open clusters based on LAMOST DR3, we deliberately selected several nearby cluster, which have relatively large projection area and reliable proper motion measurements. For each cluster, we firstly determine the typical proper motion distribution profiles in the cluster-core and the outskirt region, respectively, and perform field-star decontamination on the cluster area. We then calculate kinematic membership probability for each star in the cluster area and cross-match the highly probable members with LAMOST DR3 spectral catalog. Based on enhanced signal of cluster-member radial velocity distribution emerging from the whole field, we have also obtained reliable radial velocity membership probability for each star. Finally, we perform isochrones fitting with MCMC technique to study basic properties of these cluster, including age, metallicity, and distance modulus.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

Balaguer-Núnez, L., Tian, K. P., & Zhao, J. L., 1998, A&AS, 133, 387Google Scholar
Haario, H., Saksman, E., & Tamminen, J. 2001, Bernoulli, 223Google Scholar
Kharchenko, N. V., Piskunov, A. E., Schilbach, E., Röser, S., & Scholz, R.-D., 2012, A&A, 543, A156Google Scholar
Kharchenko, N. V., Piskunov, A. E., Schilbach, E., Röser, S., & Scholz, R.-D., 2013, A&A, 558, A53Google Scholar
Zhang, B., Chen, X.-Y., Liu, C., et al. 2015, RAA, 15, 1197Google Scholar
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