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Proceedings Paper

Test of multi-object exoplanet search spectral interferometer
Author(s): Kai Zhang; Liang Wang; Haijiao Jiang; Yongtian Zhu; Yonghui Hou; Songxin Dai; Jin Tang; Zhen Tang; Yizhong Zeng; Yi Chen; Lei Wang; Zhongwen Hu
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Paper Abstract

Exoplanet detection, a highlight in the current astronomy, will be part of puzzle in astronomical and astrophysical future, which contains dark energy, dark matter, early universe, black hole, galactic evolution and so on. At present, most of the detected Exoplanets are confirmed through methods of radial velocity and transit. Guo shoujing Telescope well known as LAMOST is an advanced multi-object spectral survey telescope equipped with 4000 fibers and 16 low resolution fiber spectrographs. To explore its potential in different astronomical activities, a new radial velocity method named Externally Dispersed Interferometry (EDI) is applied to serve Exoplanet detection through combining a fixed-delay interferometer with the existing spectrograph in medium spectral resolution mode (R=5,000-10,000). This new technology has an impressive feature to enhance radial velocity measuring accuracy of the existing spectrograph through installing a fixed-delay interferometer in front of spectrograph. This way produces an interference spectrum with higher sensitivity to Doppler Effect by interference phase and fixed delay. This relative system named Multi-object Exoplanet Search Spectral Interferometer (MESSI) is composed of a few parts, including a pair of multi-fiber coupling sockets, a remote control iodine subsystem, a multi-object fixed delay interferometer and the existing spectrograph. It covers from 500 to 550 nm and simultaneously observes up to 21 stars. Even if it’s an experimental instrument at present, it’s still well demonstrated in paper that how MESSI does explore an effective way to build its own system under the existing condition of LAMOST and get its expected performance for multi-object Exoplanet detection, especially instrument stability and its special data reduction. As a result of test at lab, inside temperature of its instrumental chamber is stable in a range of ±0.5degree Celsius within 12 hours, and the direct instrumental stability without further observation correction is equivalent to be ±50m/s every 20mins.

Paper Details

Date Published: 24 July 2014
PDF: 8 pages
Proc. SPIE 9147, Ground-based and Airborne Instrumentation for Astronomy V, 914758 (24 July 2014); doi: 10.1117/12.2055566
Show Author Affiliations
Kai Zhang, Nanjing Institute of Astronomical Optics and Technology (China)
Liang Wang, National Astronomical Observatories (China)
Haijiao Jiang, Nanjing Institute of Astronomical Optics and Technology (China)
Yongtian Zhu, Nanjing Institute of Astronomical Optics and Technology (China)
Yonghui Hou, Nanjing Institute of Astronomical Optics and Technology (China)
Songxin Dai, Nanjing Institute of Astronomical Optics and Technology (China)
Jin Tang, Nanjing Institute of Astronomical Optics and Technology (China)
Zhen Tang, Nanjing Institute of Astronomical Optics and Technology (China)
Yizhong Zeng, Nanjing Institute of Astronomical Optics and Technology (China)
Yi Chen, Nanjing Institute of Astronomical Optics and Technology (China)
Lei Wang, Nanjing Institute of Astronomical Optics and Technology (China)
Zhongwen Hu, Nanjing Institute of Astronomical Optics and Technology (China)


Published in SPIE Proceedings Vol. 9147:
Ground-based and Airborne Instrumentation for Astronomy V
Suzanne K. Ramsay; Ian S. McLean; Hideki Takami, Editor(s)

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