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Spectrum Fitting Code for LAMOST ExtraGAlactic Surveys (LEGAS)

Published online by Cambridge University Press:  13 April 2010

Xu Kong  and
Shanshan Su
Xu Kong
Affiliation:
Key Laboratory for Research in Galaxies and Cosmology, University of Science and Technology of China (USTC), CAS, China email: xkong@ustc.edu.cn Center for Astrophysics, USTC, Hefei, Anhui, 230026, China
Shanshan Su
Affiliation:
Center for Astrophysics, USTC, Hefei, Anhui, 230026, China
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Abstract

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The study of stellar populations in galaxies is entering a new era with the availability of large and high-quality data bases of both observed galactic spectra and state-of-the-art evolutionary synthesis models. The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) has a 4m primary, and a 5 degree field of view, accommodate as many as 4000 optical fibers. It can obtain the spectra of objects as faint as down to B = 20.5 mag with an exposure of 1.5 hour, promising a very high spectrum acquiring rate of ten-thousands of spectra per night. In this talk, we introduce the progress of the LAMOST project, its surveys and show the spectral synthesis code that we are developing for the LAMOST ExtraGAlactic Surveys (LEGAS).

Keywords

methods: data analysisgalaxies: fundamental parametersgalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 295 - 298
Copyright
Copyright © International Astronomical Union 2010

References

Brinchmann, J., Charlot, S., White, S. D. M., et al. 2004, MNRAS, 351, 1151CrossRefGoogle Scholar
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Cid Fernandes, R., Mateus, A., Sodré, L., et al. 2005, MNRAS, 358, 363CrossRefGoogle Scholar
Cui, X. 2009, Bulletin of the American Astronomical Society, 41, 473Google Scholar
Heavens, A. F., Jimenez, R., & Lahav, O. 2000, MNRAS, 317, 965CrossRefGoogle Scholar
Koleva, M., Prugniel, P., Bouchard, A., & Wu, Y. 2009, A&A, 501, 1269Google Scholar
Kong, X. & Cheng, F. Z. 1999, A&A, 351, 477Google Scholar
Kong, X., Charlot, S., Weiss, A., & Cheng, F. Z. 2003, A&A, 403, 877Google Scholar
Li, C., Wang, T.-G., Zhou, H.-Y., et al. 2005, AJ, 129, 669CrossRefGoogle Scholar
Lu, H., Zhou, H., Wang, J., et al. 2006, AJ, 131, 790CrossRefGoogle Scholar
Ocvirk, P., Pichon, C., Lançon, A., et al. 2006, MNRAS, 365, 74CrossRefGoogle Scholar
Tojeiro, R., Heavens, A. F., Jimenez, R., et al. 2007, MNRAS, 381, 1252CrossRefGoogle Scholar