INITIAL CHARACTERISTICS OF KEPLER SHORT CADENCE DATA

被引：260

作者：

Gilliland, Ronald L. ^{[1
]}

Jenkins, Jonm. ^{[2
,3
]}

Borucki, William J. ^{[2
]}

Bryson, Stephen T. ^{[2
]}

Caldwell, Douglas A. ^{[2
,3
]}

Clarke, Bruce D. ^{[2
,3
]}

Dotson, Jessie L. ^{[2
]}

Haas, Michael R. ^{[2
]}

Hall, Jennifer ^{[2
,4
]}

Klaus, Todd ^{[2
,4
]}

Koch, David ^{[2
]}

McCauliff, Sean ^{[2
,4
]}

Quintana, Elisa V. ^{[2
,3
]}

Twicken, Joseph D. ^{[2
,3
]}

van Cleve, Jeffrey E. ^{[2
,3
]}

机构：

[1] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[2] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[3] SETI Inst, Moffett Field, CA 94035 USA

[4] Orbital Sci Corp, Moffett Field, CA 94035 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 713卷 / 02期

关键词：

planetary systems; stars: oscillations; techniques: photometric; PLANET; STAR;

D O I：

10.1088/2041-8205/713/2/L160

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Kepler Mission offers two options for observations-either long cadence (LC) used for the bulk of core mission science, or short cadence (SC) which is used for applications such as asteroseismology of solar-like stars and transit timing measurements of exoplanets where the 1 minute sampling is critical. We discuss the characteristics of SC data obtained in the 33.5 day long Quarter 1 observations with Kepler which completed on 2009 June 15. The truly excellent time series precisions are nearly Poisson limited at 11th magnitude providing per-point measurement errors of 200 parts-per-million per minute. For extremely saturated stars near seventh magnitude precisions of 40 ppm are reached, while for background limited measurements at 17th magnitude precisions of 7 mmag are maintained. We note the presence of two additive artifacts, one that generates regularly spaced peaks in frequency, and one that involves additive offsets in the time domain inversely proportional to stellar brightness. The difference between LC and SC sampling is illustrated for transit observations of TrES-2.

引用

页码：L160 / L163

页数：4

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