Relative flux calibration for the Guoshoujing Telescope (LAMOST)

• Published in: Research in astronomy and astrophysics Vol. 12; no. 4; pp. 453 - 464
• Main Authors: Song, Yi-Han, Luo, A-Li, Comte, Georges, Bai, Zhong-Rui, Zhang, Jian-Nan, Du, Wei, Zhang, Hao-Tong, Chen, Jian-Jun, Zuo, Fang, Zhao, Yong-Heng
• Format: Journal Article
• Language: English
• Published: Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 01.04.2012; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China%National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; Observatoire Astronomique Marseille-Provence and Laboratoire d'Astrophysique de Marseille,F-13388 Marseille Cedex, France; National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; Graduate University of Chinese Academy of Sciences, Beijing 100049, China%National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; IOP Publishing
• Subjects: Astrophysics; Sciences of the Universe; spectroscopic-calibration; data; analysis; techniques; methods
• ISSN: 1674-4527; 2397-6209
• DOI: 10.1088/1674-4527/12/4/009

P111; This paper presents a relative flux calibration method for the Guoshoujing Telescope (LAMOST),which may be applied to connect a blue spectrum to a red spectrum to build the whole spectrum across the total wavelength range (3700 ～ 9000 (A)).In each spectrograph,we estimate the effective temperatures of selected stars using a grid of spectral line indices in the blue spectral range and a comparison with stellar atmosphere models.For each spectrograph,stars of types A and F are selected as pseudo-standard stars,and the theoretical spectra are used to calibrate both the blue (3700 ～ 5900 (A)) and red spectrograph arms (5700 ～ 9000 (A)).Then the spectral response function for these pseudo-standard stars could be used to correct the raw spectra provided by the other fibers of the spectrograph,after a fiber efficiency function has been derived from twilight flat-field exposures.A key problem in this method is the fitting of a pseudo stellar continuum,so we also give a detailed description of this step.The method is tested by comparing a small sample of LAMOST spectra calibrated in this way on stars also observed by the Sloan Digital Sky Survey.The result shows that the Teff estimation and relative flux calibration method are adequate.