LAMOST OBSERVATIONS IN THE KEPLER FIELD. I. DATABASE OF LOW-RESOLUTION SPECTRA

被引：100

作者：

De Cat, P. ^{[2
]}

Fu, J. N. ^{[1
]}

Ren, A. B. ^{[2
]}

Yang, X. H. ^{[2
]}

Shi, J. R. ^{[3
]}

Luo, A. L. ^{[3
]}

Yang, M. ^{[3
]}

Wang, J. L. ^{[3
]}

Zhang, H. T. ^{[3
]}

Shi, H. M. ^{[3
]}

Zhang, W. ^{[3
]}

Dong, Subo ^{[4
]}

Catanzaro, G. ^{[5
]}

Corbally, C. J. ^{[6
]}

Frasca, A. ^{[5
]}

Gray, R. O. ^{[7
]}

Molenda-Zakowicz, J. ^{[8
,9
]}

Uytterhoeven, K. ^{[10
,11
]}

Briquet, M. ^{[12
,13
]}

Bruntt, H. ^{[14
]}

Frandsen, S. ^{[14
]}

Kiss, L. ^{[15
]}

Kurtz, D. W. ^{[16
]}

Marconi, M. ^{[17
]}

Niemczura, E. ^{[8
]}

Ostensen, R. H. ^{[18
]}

Ripepi, V. ^{[17
]}

Smalley, B. ^{[19
]}

Southworth, J. ^{[19
]}

Szabo, R. ^{[15
]}

Telting, J. H. ^{[20
]}

Karoff, C. ^{[14
,21
]}

Aguirre, V. Silva ^{[14
]}

Wu, Y.

Hou, Y. H. ^{[22
]}

Jin, G. ^{[23
]}

Zhou, X. L. ^{[24
]}

机构：

[1] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China

[2] Royal Observ Belgium, B-1180 Brussels, Belgium

[3] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China

[4] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[5] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[6] Steward Observ, Vatican Observ Res Grp, Tucson, AZ 85721 USA

[7] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA

[8] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland

[9] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA

[10] Inst Astrofis Canarias, E-38200 Tenerife, Spain

[11] Univ La Laguna, E-38206 Tenerife, Spain

[12] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium

[13] Univ Paris 06, Sorbonne Univ, PSL Res Univ, LESIA,Observ Paris,CNRS,Univ Paris Diderot,Sorbon, F-75252 Paris 05, France

[14] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark

[15] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary

[16] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England

[17] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy

[18] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium

[19] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[20] Nord Opt Telescope, E-38711 Brena Baja, Spain

[21] Aarhus Univ, Dept Geosci, DK-8000 Aarhus, Denmark

[22] Chinese Acad Sci, Natl Astron Observ, Nanjing Inst Astron Opt & Technol, Nanjing 210042, Jiangsu, Peoples R China

[23] Univ Sci & Technol China, Hefei 230026, Peoples R China

[24] Chinese Acad Sci, Key Lab Space Astron & Technol, Natl Astron Observ, Beijing 100012, Peoples R China

来源：

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES | 2015年 / 220卷 / 01期

基金：

欧洲研究理事会; 新加坡国家研究基金会; 美国国家科学基金会; 中国国家自然科学基金;

关键词：

astronomical databases: miscellaneous; stars: fundamental parameters; stars: general; stars: statistics; ATMOSPHERIC PARAMETERS; DATA RELEASE; TELESCOPE; STARS; ASTEROSEISMOLOGY; CLASSIFICATION; SAMPLE;

D O I：

10.1088/0067-0049/220/1/19

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The nearly continuous light curves with micromagnitude precision provided by the space mission Kepler are revolutionizing our view of pulsating stars. They have revealed a vast sea of low-amplitude pulsation modes that were undetectable from Earth. The long time base of Kepler light curves allows for the accurate determination of the frequencies and amplitudes of pulsation modes needed for in-depth asteroseismic modeling. However, for an asteroseismic study to be successful, the first estimates of stellar parameters need to be known and they cannot be derived from the Kepler photometry itself. The Kepler Input Catalog provides values for the effective temperature, surface gravity, and metallicity, but not always with sufficient accuracy. Moreover, information on the chemical composition and rotation rate is lacking. We are collecting low- resolution spectra for objects in the Kepler field of view with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong observatory, China). All of the requested fields have now been observed at least once. In this paper, we describe those observations and provide a useful database for the whole astronomical community.

引用

页数：18

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