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Adaptive Wavelength Calibration Algorithm for LAMOST

Published online by Cambridge University Press:  02 January 2013

H. Q. Qin ,
J. Zhu ,
Z. Q. Zhu ,
Z. F. Ye  and
A. L. Luo
H. Q. Qin
Affiliation:
Institute of Statistical Signal Processing, Department of Electronic Engineering and Information Science, University of Science and Technology of China, Hefei 230027, P. R. China
J. Zhu
Affiliation:
Institute of Statistical Signal Processing, Department of Electronic Engineering and Information Science, University of Science and Technology of China, Hefei 230027, P. R. China
Z. Q. Zhu
Affiliation:
Institute of Statistical Signal Processing, Department of Electronic Engineering and Information Science, University of Science and Technology of China, Hefei 230027, P. R. China
Z. F. Ye*
Affiliation:
Institute of Statistical Signal Processing, Department of Electronic Engineering and Information Science, University of Science and Technology of China, Hefei 230027, P. R. China
A. L. Luo
Affiliation:
Department of LAMOST, National Astronomical Observatories of China, Beijing 100012, P. R. China
*
CCorresponding author. Email: yezf@ustc.edu.cn
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Abstract

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An adaptive algorithm is presented for the wavelength calibration of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). The new algorithm can identify emission lines of calibration lamp without manual interaction and then fit relationship between the pixel positions and the wavelengths by utilizing a polynomial function. In this study, experiments are performed both on the actual data observed by LAMOST and the simulated data to analyze the accuracy and the robustness.The experimental results show that the proposed automatic algorithm can perform the lines identification exactly and acquire the wavelength solution accurately. Thus, an applicable approach is provided for the wavelength calibration of LAMOST.

Keywords

instrumentation: spectrographsmethods: data analysistechniques: spectroscopicline: identification
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 27 , Issue 3 , 2010 , pp. 265 - 271
Copyright
Copyright © Astronomical Society of Australia 2010

References

Bai, L., Liao, N. F., Li, Z. J. & Yang, W. P., 2004, ChOpL, 2, 174Google Scholar
Burles, S. & Schlegel, D., 2007, SDSS Data Reduction Software, v5.3.12, http://das.sdss.org/softwareGoogle Scholar
Cui, X. Q., 2009, AAS Meeting, 213, 226.01Google Scholar
Lo, E. & Fountain, A. W., 2006, SPIE, 6233, 62330Google Scholar
Qin, H. Q., Ye, Z. F. & Luo, A. L., 2009, PASP, 121, 408CrossRefGoogle Scholar
Sanchez, S. F., 2006, AN, 327, 850Google Scholar
Thompson, R. I., Bechtold, J., Black, J. H. & Martins, C. J. A. P., 2009, NA, 14, 379Google Scholar
van Geffen, J. H. G. M. & van Oss, R. F., 2003, ApOpt, 42, 2739Google Scholar