The Kepler Mission

A wide field of view photometer designed to determine the frequency of earth-size planets around solar-like stars

William J. Borucki, David G. Koch, Jack J. Lissauer, Gibor B. Basri, John F. Caldwell, William D. Cochran, Edward W. Dunham, John C. Geary, D. W. Latham, Ronald Lynn Gilliland, Douglas A. Caldwell, Jon M. Jenkins, Yoji Kondo

Research output: Contribution to journalConference article

30 Citations (Scopus)

Abstract

NASA's Kepler Mission is designed to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. It uses transit photometry from space to determine planet size relative to its star and orbital period. From these measurements, and those of complementary ground-based observations of planet-hosting stars, and from Kepler's third law, the actual size of the planet, its position relative to the habitable zone, and the presence of other planets can be deduced. The Kepler photometer is designed around a 0.95 m aperture wide field-of-view (FOV) Schmidt type telescope with a large array of CCD detectors to continuously monitor 100,000 stars in a single FOV for four years. To detect terrestrial planets, the photometer uses differential relative photometry to obtain a precision of 20 ppm for 12th magnitude stars. The combination of the number of stars that must be monitored to get statistically significant estimate of the frequency of Earth-size planets, the size of Earth with respect to the Sun, the minimum number of photoelectrons required to recognize the transit signal while maintaining a low false-alarm rate, and the areal density of target stars of differing brightness are all critical to the photometer design.

Original languageEnglish (US)
Pages (from-to)129-140
Number of pages12
JournalProceedings of SPIE - The International Society for Optical Engineering
Volume4854
DOIs
StatePublished - Dec 1 2002
EventFuture EUV/UV and Visible Space Astrophysics Missions and Instrumentation - Waikoloa, HI, United States
Duration: Aug 22 2002Aug 23 2002

Fingerprint

Kepler mission
Photometers
Kepler
Wide-field
Planets
Field of View
Stars
field of view
photometers
planets
Star
Earth (planet)
stars
Photometry
transit
photometry
Kepler laws
False Alarm Rate
Brightness
NASA

All Science Journal Classification (ASJC) codes

  • Electronic, Optical and Magnetic Materials
  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering

Cite this

Borucki, William J. ; Koch, David G. ; Lissauer, Jack J. ; Basri, Gibor B. ; Caldwell, John F. ; Cochran, William D. ; Dunham, Edward W. ; Geary, John C. ; Latham, D. W. ; Gilliland, Ronald Lynn ; Caldwell, Douglas A. ; Jenkins, Jon M. ; Kondo, Yoji. / The Kepler Mission : A wide field of view photometer designed to determine the frequency of earth-size planets around solar-like stars. In: Proceedings of SPIE - The International Society for Optical Engineering. 2002 ; Vol. 4854. pp. 129-140.
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abstract = "NASA's Kepler Mission is designed to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. It uses transit photometry from space to determine planet size relative to its star and orbital period. From these measurements, and those of complementary ground-based observations of planet-hosting stars, and from Kepler's third law, the actual size of the planet, its position relative to the habitable zone, and the presence of other planets can be deduced. The Kepler photometer is designed around a 0.95 m aperture wide field-of-view (FOV) Schmidt type telescope with a large array of CCD detectors to continuously monitor 100,000 stars in a single FOV for four years. To detect terrestrial planets, the photometer uses differential relative photometry to obtain a precision of 20 ppm for 12th magnitude stars. The combination of the number of stars that must be monitored to get statistically significant estimate of the frequency of Earth-size planets, the size of Earth with respect to the Sun, the minimum number of photoelectrons required to recognize the transit signal while maintaining a low false-alarm rate, and the areal density of target stars of differing brightness are all critical to the photometer design.",
author = "Borucki, {William J.} and Koch, {David G.} and Lissauer, {Jack J.} and Basri, {Gibor B.} and Caldwell, {John F.} and Cochran, {William D.} and Dunham, {Edward W.} and Geary, {John C.} and Latham, {D. W.} and Gilliland, {Ronald Lynn} and Caldwell, {Douglas A.} and Jenkins, {Jon M.} and Yoji Kondo",
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Borucki, WJ, Koch, DG, Lissauer, JJ, Basri, GB, Caldwell, JF, Cochran, WD, Dunham, EW, Geary, JC, Latham, DW, Gilliland, RL, Caldwell, DA, Jenkins, JM & Kondo, Y 2002, 'The Kepler Mission: A wide field of view photometer designed to determine the frequency of earth-size planets around solar-like stars', Proceedings of SPIE - The International Society for Optical Engineering, vol. 4854, pp. 129-140. https://doi.org/10.1117/12.460266

The Kepler Mission : A wide field of view photometer designed to determine the frequency of earth-size planets around solar-like stars. / Borucki, William J.; Koch, David G.; Lissauer, Jack J.; Basri, Gibor B.; Caldwell, John F.; Cochran, William D.; Dunham, Edward W.; Geary, John C.; Latham, D. W.; Gilliland, Ronald Lynn; Caldwell, Douglas A.; Jenkins, Jon M.; Kondo, Yoji.

In: Proceedings of SPIE - The International Society for Optical Engineering, Vol. 4854, 01.12.2002, p. 129-140.

Research output: Contribution to journalConference article

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T1 - The Kepler Mission

T2 - A wide field of view photometer designed to determine the frequency of earth-size planets around solar-like stars

AU - Borucki, William J.

AU - Koch, David G.

AU - Lissauer, Jack J.

AU - Basri, Gibor B.

AU - Caldwell, John F.

AU - Cochran, William D.

AU - Dunham, Edward W.

AU - Geary, John C.

AU - Latham, D. W.

AU - Gilliland, Ronald Lynn

AU - Caldwell, Douglas A.

AU - Jenkins, Jon M.

AU - Kondo, Yoji

PY - 2002/12/1

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N2 - NASA's Kepler Mission is designed to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. It uses transit photometry from space to determine planet size relative to its star and orbital period. From these measurements, and those of complementary ground-based observations of planet-hosting stars, and from Kepler's third law, the actual size of the planet, its position relative to the habitable zone, and the presence of other planets can be deduced. The Kepler photometer is designed around a 0.95 m aperture wide field-of-view (FOV) Schmidt type telescope with a large array of CCD detectors to continuously monitor 100,000 stars in a single FOV for four years. To detect terrestrial planets, the photometer uses differential relative photometry to obtain a precision of 20 ppm for 12th magnitude stars. The combination of the number of stars that must be monitored to get statistically significant estimate of the frequency of Earth-size planets, the size of Earth with respect to the Sun, the minimum number of photoelectrons required to recognize the transit signal while maintaining a low false-alarm rate, and the areal density of target stars of differing brightness are all critical to the photometer design.

AB - NASA's Kepler Mission is designed to determine the frequency of Earth-size and larger planets in the habitable zone of solar-like stars. It uses transit photometry from space to determine planet size relative to its star and orbital period. From these measurements, and those of complementary ground-based observations of planet-hosting stars, and from Kepler's third law, the actual size of the planet, its position relative to the habitable zone, and the presence of other planets can be deduced. The Kepler photometer is designed around a 0.95 m aperture wide field-of-view (FOV) Schmidt type telescope with a large array of CCD detectors to continuously monitor 100,000 stars in a single FOV for four years. To detect terrestrial planets, the photometer uses differential relative photometry to obtain a precision of 20 ppm for 12th magnitude stars. The combination of the number of stars that must be monitored to get statistically significant estimate of the frequency of Earth-size planets, the size of Earth with respect to the Sun, the minimum number of photoelectrons required to recognize the transit signal while maintaining a low false-alarm rate, and the areal density of target stars of differing brightness are all critical to the photometer design.

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