Hostname: page-component-586b7cd67f-t8hqh Total loading time: 0 Render date: 2024-11-24T20:31:25.009Z Has data issue: false hasContentIssue false
  • English
  • Français

Properties of abundance gradient along the Galactic disk and the role of LAMOST

Published online by Cambridge University Press:  06 January 2014

J.L. Hou ,
L. Chen ,
J.C. Yu ,
J. Sellwood  and
C. Pryor
J.L. Hou
Affiliation:
Shanghai Astronomical Observatory, CAS, Shanghai, 200030, China email: [email protected], [email protected], [email protected]
L. Chen
Affiliation:
Shanghai Astronomical Observatory, CAS, Shanghai, 200030, China email: [email protected], [email protected], [email protected]
J.C. Yu
Affiliation:
Shanghai Astronomical Observatory, CAS, Shanghai, 200030, China email: [email protected], [email protected], [email protected]
J. Sellwood
Affiliation:
Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA email: [email protected]
C. Pryor
Affiliation:
Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854, USA email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this paper, we present our recent work on the evolution of abundance gradients along the Milky Way disk based on the Geneva Copenhagen Survey (GCS) and Radial Velocity Experiment (RAVE) data. We will also discuss the role of the LAMOST Milky Way disk survey in clarifying the properties of metallicity breaks observed through open clusters and young tracers along the Milky Way disk. It is believed that the Galactic disk forms inside-out, in which the stellar population at increasing radii is younger and more metal poor. This picture is consistent with most Galactic Chemical Evolution (GCE) models which also predict a tight correlation between the metallicity and age of stars at a given radius. However, it is only a result of “steady state" and no dynamical evolution effects were taken into account. We have selected two stellar samples from GCS and RAVE, each sample contains about 10,000 local thin-disk, main-sequence stars. We use the guiding radius which is determined by the conservation of z-direction angular momentum, to eliminate the blurring effects. And also use the effective temperature of the main sequence stars as a proxy of stellar age. It is shown that the metallicity gradient flattens as the age increases. This is not consistent with our previous GCE prediction, but can be explained by radial mixing effects. In order to further demonstrate the abundance breaks observed in the Galactic disk we have proposed, and have been carrying out, an open cluster survey project based on LAMOST. We plan to observe at least 400 open clusters in the northern Galactic sky. From the observations, we will get uniform parameters for those clusters with radial velocity and metallicities. We anticipate that this uniform open cluster sample could clarify the observed abundance break around the Milky Way disk corotation radius and also give a more robust result concerning the evolution of the abundance gradient.

Keywords

Open ClustersAbundanceGradientsSurveys
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S298: Setting the scene for Gaia and LAMOST , May 2013 , pp. 304 - 309
Copyright
Copyright © International Astronomical Union 2014 

References

Andrievsky, S. M., Luck, R. E., Martin, P., Lépine, J. R. D. 2004, A&A, 413, 159Google Scholar
Carraro, G., Ng, Y. K. & Portinari, L. 1998, MNRAS, 296, 1045CrossRefGoogle Scholar
Chen, L., Hou, J. L., & Wang, J. J. 2003, AJ, 125, 1397Google Scholar
Chen, L., Hou, J. L. & Zhao, J. L. 2008, IAUS, 248, 433Google Scholar
Chen, L., Hou, J. L., Yu, J. C., Liu, C., Deng, L. C.et al. 2012, RAA, 12, 805Google Scholar
Deng, L. C., Newberg, H. J., Liu, C.et al. 2012, RAA, 12, 735Google Scholar
Coşkunoğlu, B., Ak, S., Bilir, S.et al. 2012, MNRAS, 419, 2844Google Scholar
Friel, E. D. 1999, ApSS, 265, 271Google Scholar
Fu, J., Hou, J. L., Yin, J. & Chang, R. X. 2009, ApJ, 696, 668Google Scholar
Haywood, M. 2008, MNRAS, 388, 1175Google Scholar
Holmberg, J., Nordström, B. & Andersen, J. 2009, A&A, 501, 941Google Scholar
Hou, J. L., Prantzos, N., & Boissier, S. 2000, A&A, 362, 921Google Scholar
Lépine, J. R. D., Cruz, P., Scarano, S. Jr.et al. 2011, MNRAS, 417, 698CrossRefGoogle Scholar
Maciel, W. J., Lago, L. G., Costa, R. D .D. 2006, A&A, 453, 587Google Scholar
Magrini, L., Sestito, P., Randich, S., Galli, D. 2009, A&A, 494, 95Google Scholar
Nordström, B., Mayor, M., Andersen, J.et al. 2004, A&A, 418, 989Google Scholar
Pedicelli, S., Bono, G., Lemasle, B.et al. 2009, A&A, 504, 81Google Scholar
Rudolph, A. L., Fich, M., Bell, G. R., et al. 2006, ApJS, 162, 346Google Scholar
Scarano, S. Jr. & Lepine, J. R. D. 2013, MNRAS, 428, 625Google Scholar
Sellwood, J. A. & Binney, J. J. 2002, MNRAS, 336, 785Google Scholar
Simpson, J. P., Colgan, S. W. J., Rubin, R. H.et al. 1995, ApJ, 444, 721Google Scholar
Stanghellini, L. & Haywood, M. 2010, ApJ, 714, 1096Google Scholar
Steinmetz, M., Zwitter, T., Siebert, A., et al. 2006, AJ, 132, 1645Google Scholar
Twarog, B. A., Ashman, K. M., & Anthony-Twarog, B. J. 1997, AJ, 114, 2556Google Scholar
Wyse, R. & Silk, J. 1989, ApJ, 339, 700Google Scholar
Yao, S., Liu, C., Zhang, H. T., et al. 2012, RAA, 12, 772Google Scholar
Yu, J. C., Sellwood, J. A., Pryor, C., Chen, L., & Hou, J. L. 2012, ApJ, 754, 124Google Scholar