CoRoT Symposium 3, Kepler KASC-7 joint meeting
6-11 Jul 2014 Toulouse (France)

Abstracts > De Cat Peter

Tuesday 8
Session 1 - Probing stellar structure and evolution with asteroseismology
Dennis Stello (chair)
› 17:30 - 17:50 (20min)
LAMOST observations in the Kepler field
Peter De Cat  1@  , Jian-Ning Fu  2  , Xiaohu Yang  2  , Anbing Ren  2  , Antonio Frasca  3  , Joanna Molenda-Zakowicz  4  , Richard O. Gray  5  , Christopher J. Corbally  6  , Jianrong Shi  7  , Huatong Zhang  7  , Ali Luo  7  
1 : Royal Observatory of Belgium  (ROB)  -  Website
Ringlaan 3 B-1180 Brussels -  Belgium
2 : Beijing Normal University  (BNU)
3 : Osservatorio Astrofisico di Catania  (INAF)
4 : Uniwersytet Wroclawski
5 : Appalachian State University
6 : University of Arizona
7 : Key Lab for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences  (LAMOST)

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) is new instrument with 4000 optical fibers attachted to a 4-m telescope at the Xinglong observatory in China. In 2010, we initiated the LAMOST-Kepler project. We requested to observe the full field-of-view of the nominal Kepler mission with the LAMOST to collect low-resolution spectra for as many objects from the KIC10 catalogue as possible. The list of targets with a specific scientific interest consists of ~250 "standard targets" (MK secondary standard stars), ~7,000 "KASC targets'' (targets of the Kepler Asteroseismic Science Consortium) and ~150,000 "planet targets'' (targets from the planet search group). As these LAMOST spectra allow an independent and homegeneous determination of stellar parameters, they are providing extra constraints for asteroseismic modelling. During the first three years of operation, 10 of the 14 requested LAMOST fields have been observed resuling in more than 60,000 low-resolution spectra. In this talk, we present the results derived from the data gathered during the test phase and the pilot survey (2011 & 2012) by three different groups of collaborators: the Chinese team (ULySS code), the European team (ROTFIT code) and the American team (MKCLASS code). The resulting stellar parameters are compared to those given in the KIC10 catalogue and to those derived from other types of ground-based follow-up data already available in the literature.



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