Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-26T17:02:09.129Z Has data issue: false hasContentIssue false
  • English
  • Français

Characteristics of the Kepler target stars

Published online by Cambridge University Press:  21 October 2010

Natalie M. Batalha ,
William J. Borucki ,
David G. Koch ,
Timothy M. Brown ,
Douglas A. Caldwell  and
David W. Latham
Natalie M. Batalha
Affiliation:
Department of Physics and Astronomy, San Jose State University, San Jose, CA 95192
William J. Borucki
Affiliation:
Mailstop 244-30, NASA Ames Research Center, Moffett Field, CA 94035
David G. Koch
Affiliation:
Mailstop 244-30, NASA Ames Research Center, Moffett Field, CA 94035
Timothy M. Brown
Affiliation:
Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Ste 102, Goleta, CA
Douglas A. Caldwell
Affiliation:
SETI Institute, 515 N. Whisman Rd., Mountain View, CA 94043
David W. Latham
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The Kepler Mission successfully launched March 6, 2009, beginning its 3.5-year mission to determine the frequency of Earth-size planets in the habitable zones of late-type stars. The brightnesses of over 100,000 stars are currently being monitored for transit events with an expected differential photometric precision of 20 ppm at V=12 for a 6.5-hour transit. The same targets will be observed continuously over the mission duration in order to broaden the detection space to orbital periods comparable to that of Earth. This paper provides an overview of the selection and prioritization criteria used to choose the stars that Kepler is observing from the > 4.5 million objects in the 100 square degree field of view. The characteristics of the Kepler targets are described as well as the implications for detectability of planets in the habitable zone smaller than 2R⊕.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 712 - 713
Copyright
Copyright © International Astronomical Union 2010

References

Batalha, N. M., Jenkins, J., Basri, G. S., Borucki, W. J., & Koch, D. G. 2002, in: Favata, F., Roxburgh, I.W. & Galadi, D. (eds.), Stellar Structure and Habitable Planet Finding, ESA SP-485, p. 35Google Scholar
Borucki, W., Koch, D., Basri, G., Batalha, N., Brown, T., Caldwell, D., Christensen-Dalsgaard, J., Cochran, W., Dunham, E., Gautier, T. N., Geary, J., Gilliland, R., Jenkins, J., Kondo, Y., Latham, D., Lissauer, J. J., & Monet, D. 2008, in: Sun, Y.-S., Ferraz Mello, S. & Zhou, J.-L. (eds.), Exoplanets: Detection, Formation, and Dynamics, Proc. of IAU Symposium No 249 (Cambridge: CUP), p. 17Google Scholar
Castelli, F. & Kurucz, R. L. 2004, arXiv:astro-ph/0405087Google Scholar