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Open clusters: their kinematics and metallicities

Published online by Cambridge University Press:  01 October 2007

L. Chen ,
J. L. Hou ,
J. L. Zhao  and
R. de Grijs
L. Chen
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China email: chenli@shao.ac.cn, houjl@shao.ac.cn, jlzhao@shao.ac.cn
J. L. Hou
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China email: chenli@shao.ac.cn, houjl@shao.ac.cn, jlzhao@shao.ac.cn
J. L. Zhao
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China email: chenli@shao.ac.cn, houjl@shao.ac.cn, jlzhao@shao.ac.cn
R. de Grijs
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK; and National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China email: r.degrijs@sheffield.ac.uk
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Abstract

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We review our work on Galactic open clusters in recent years, and introduce our proposed large program for the LOCS (LAMOST Open Cluster Survey). First, based on the most complete open clusters sample with metallicity, age and distance data as well as kinematic information, some preliminary statistical analysis regarding the spatial and metallicity distributions is presented. In particular, a radial abundance gradient of −0.058±0.006 dex kpc−1 is derived. By dividing clusters into the age groups we show that the disk abundance gradient was steeper in the past. Secondly, proper motions, membership probabilities, and velocity dispersions of stars in the regions of two very young open clusters are derived. Both clusters show clear evidence of mass segregation, which provides support for the “primordial” mass segregation scenario. Based on the advantages of the forthcoming LAMOST facility, we have proposed a detailed open cluster survey with LAMOST (the LOCS). The aim, feasibility, and the present development of the LOCS are briefly summarized.

Keywords

Galaxy: diskopen clusters and associations: generalopen clusters and associations: individual (NGC2244)open clusters and associations: individual (NGC6530)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S248: A Giant Step: from Milli- to Micro-arcsecond Astrometry , October 2007 , pp. 433 - 439
Copyright
Copyright © International Astronomical Union 2008

References

Bonnell, I. A., Bate, M. R., Clarke, C. J., & Pringle, J. E. 2001a, MNRAS, 323, 785CrossRefGoogle Scholar
Bonnell, I. A., Clarke, C. J., Bate, M. R., & Pringle, J. E. 2001b, MNRAS, 324, 573CrossRefGoogle Scholar
Brandl, B., Sams, B. J., Bertoldi, F., Eckart, A., Genzel, R., Drapatz, S., Hofmann, R., Löwe, M., & Quirrenbach, A. 1996, ApJ, 466, 254CrossRefGoogle Scholar
Bragaglia, A. & Tosi, Monica. 2006, AJ, 131, 1544CrossRefGoogle Scholar
Campbell, B., et al. 1992, AJ, 104, 1721CrossRefGoogle Scholar
Carraro, G., Ng, Y. K., & Portinari, L. 1998, MNRAS, 296, 1045CrossRefGoogle Scholar
Chen, L., de Grijs, R., & Zhao, J. L. 2007, AJ, 134, 1368CrossRefGoogle Scholar
Chen, L., Hou, J. L., & Wang, J. J. 2003, AJ, 125, 1397CrossRefGoogle Scholar
Chiappini, C., Matteucci, F., & Romano, D. 2001, ApJ, 550, 1044CrossRefGoogle Scholar
Deharveng, L., Peña, M., Caplan, J., Costero, R. 2000, MNRAS, 311, 329CrossRefGoogle Scholar
Dias, W. S., Alessi, B. S., Moitinho, A., & Lépine, J. R. 2002, A&A, 389, 871Google Scholar
Friel, E. D., Janes, K. A., Tavarez, M., et al. 2002, AJ, 124, 2693CrossRefGoogle Scholar
Hillenbrand, L. A. 1997, AJ, 113, 1733CrossRefGoogle Scholar
Hou, J. L., Prantzos, N., & Boissier, S. 2000, A&A, 362, 921Google Scholar
Janes, K. A., Tilley, C., & Lyngå, G. 1988, AJ, 95, 771CrossRefGoogle Scholar
Janes, K. A. & Phelps, R. L. 1994, AJ, 108, 1773CrossRefGoogle Scholar
Kharchenko, N. V., Piskunov, A. E., Roeser, S., Schilbach, E., & Scholz, R.-D. 2005, A&A, 438, 1163Google Scholar
Kharchenko, N. V., Piskunov, A. E., Roeser, S., Schilbach, E., & Scholz, R.-D. 2005, A&A, 440, 403Google Scholar
Larson, R. B. 1991, in: Falgarone, E., Boulanger, F., & Duvert, G., (eds.), Fragmentation of Molecular Clouds and Star Formation, IAU Symp. 147 (Dordrecht: Kluwer), p. 261CrossRefGoogle Scholar
Maciel, W. J., Lago, L. G., & Costa, R. D. D. 2006, A&A, 453, 587Google Scholar
Mathieu, R. D. 2000, in: Pallavicini, R., Micela, G., & Sciortino, S., (eds.), Stellar Clusters and Associations: Convection, Rotations, and Dynamos, ASP Conference Series, p. 517Google Scholar
Mermilliod, J.-C. & Paunzen, E. 2003, A&A, 410, 511Google Scholar
Phelps, R. L., Janes, K. A., & Montgomery, K. A. 1994, AJ, 107, 1079CrossRefGoogle Scholar
Twarog, B. A., Ashman, K. A., & Anthony-Twarog, B. J. 1997, AJ, 114, 2556CrossRefGoogle Scholar
Zhao, J. L., Chen, L., & Zu, Z. L. 2006, Chin. J.Astron.Astrophysics, 6, 287CrossRefGoogle Scholar