Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-27T20:39:44.886Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar population analysis of galaxies in SDSS and LAMOST Pilot Survey

Published online by Cambridge University Press:  06 January 2014

Xiaoyan Chen ,
Ali Luo  and
Haifeng Yang
Xiaoyan Chen
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, 100012 Beijing, PR China (NAOC) email: [email protected] Key Laboratory of Optical Astronomy, NAOC, Chinese Academy of Sciences, PR China
Ali Luo
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, 100012 Beijing, PR China (NAOC) email: [email protected] Key Laboratory of Optical Astronomy, NAOC, Chinese Academy of Sciences, PR China
Haifeng Yang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, 100012 Beijing, PR China (NAOC) email: [email protected] Key Laboratory of Optical Astronomy, NAOC, Chinese Academy of Sciences, PR China School of Computer Science and Technology, Taiyuan University of Science and Technology, Taiyuan, PR China
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.

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, i.e. Guoshoujing Telescope) has finished its pilot survey (from October 2011 to June 2012). With about 3000 galaxy spectra collected during the pilot survey, we are planning to analyze the stellar populations of these galaxies in two different ways respectively. One is Lick indices (such as Hβ, Mgb, 〈Fe〉 etc., Worthey et al. 1994), which are not sensitive to the flux calibration, and another one is the full optical spectra fitting (Chen et al. 2009, 2010). Then we can evaluate the affects of flux calibration errors on stellar population analysis by comparing the results of the two methods′. Here we briefly show the early experiments aiming to test the consistency and/or difference between the two methods.

Keywords

galaxies: stellar contentgalaxies: evolutiongalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S298: Setting the scene for Gaia and LAMOST , May 2013 , pp. 399
Copyright
Copyright © International Astronomical Union 2014 

References

Chen, X. Y., Liang, Y. C., Hammer, F., Zhao, Y. H., & Zhong, G. H. 2009, A&A, 495, 457Google Scholar
Chen, X. Y., Liang, Y. C., Hammer, F., Prugniel, Ph.et al. 2010, A&A, 515, A101Google Scholar
Chen, X. Y., Luo, A. L., Liang, Y. C. 2012, IAU Symposium 292, 154CrossRefGoogle Scholar
Worthey, G., Faber, S. M.et al. 1994, ApJS, 94, 687Google Scholar