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Identifying and Characterizing Stellar Clusters Toward the Galactic Anti-Center from Pan-STARRS1 Survey

Published online by Cambridge University Press:  31 March 2017

C.-C. Lin ,
W.-P. Chen ,
J. Hou ,
L. Chen  and
Z. Shao
C.-C. Lin
Affiliation:
Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai 200030, China email: cclin@shao.ac.cn Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, Taiwan
W.-P. Chen
Affiliation:
Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, Jhongli 32001, Taiwan
J. Hou
Affiliation:
Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai 200030, China email: cclin@shao.ac.cn
L. Chen
Affiliation:
Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai 200030, China email: cclin@shao.ac.cn
Z. Shao
Affiliation:
Shanghai Astronomical Observatory, CAS, 80 Nandan Road, Shanghai 200030, China email: cclin@shao.ac.cn
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Abstract

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The current sample of star clusters (SCs) is still incomplete beyond 1.8 kpc. The Pan-STARRS1 with its wide field of views and sensitive cameras provides us an opportunity to identify and characterize SCs as much as possible. By using a star counting algorithm, we obtained a total of 491 stellar density enhancements in a field of 20° × 20° toward the Galactic Anti-Center (GAC), of which 50 are known SCs. The remaining 441 candidates are verified with radii, interstellar reddening, distances, and ages with proper motions and multiple bands photometries. Our results push the completeness of SCs almost near the edge of GAC. With the revised SC sample, the separation between Sagittarius and Perseus arms are about 3.2 ± 0.2 kpc and the widths of the nearby spiral arms—Sagittarius, Orion, and Perseus—with are 1.4 ± 0.1, 1.6 ± 0.1, and 3.3 ± 0.2 kpc, respectively.

Keywords

Galaxy: structureopen clusters and associations: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S316: Formation, evolution, and survival of massive star clusters , August 2015 , pp. 163 - 164
Copyright
Copyright © International Astronomical Union 2017 

References

Kaiser, N., Burgett, W., Chambers, K., et al. 2010, in SPIE, Vol. 7733Google Scholar
Kharchenko, N. V., Piskunov, A. E., Schilbach, E., et al. 2013, A&A, 558, A53 Google Scholar
Lin, C. C., Chen, W. P., & Magnier, E. A. 2011, APRIM, V1, 181 Google Scholar
Piskunov, A. E., Kharchenko, N. V., Röser, S., et al. 2006, A&A, 445, 545 Google Scholar
Wang, P. F., Chen, W. P., Lin, C. C., et al. 2014, ApJ, 784, 57 CrossRefGoogle Scholar