<i>KEPLER MISSION</i>
                    DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE

Koch, David; Borucki, W. J.; Basri, Gibor; Batalha, Natalie M.; Brown, Timothy M.; Caldwell, Douglas A.; Christensen‐Dalsgaard, J.; Cochran, William D.; DeVore, Edna; Dunham, E. W.; Gautier, T. N.; Geary, John C.; Gilliland, Ronald L.; Gould, A.; Jenkins, Jon M.; Kondo, Y.; Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Monet, D. G.; Sasselov, Dimitar; Boss, Alan P.; Brownlee, D. E.; Caldwell, John; Dupree, A. K.; Howell, Steve B.; Kjeldsen, H.; Meibom, S.; Morrison, David; Owen, Tobias; Reitsema, H. J.; Tarter, Jill; Bryson, Stephen T.; Dotson, Jessie L.; Gazis, P. R.; Haas, Michael R.; Kolodziejczak, J.; Rowe, Jason F.; Cleve, Jeffrey E. Van; Allen, Christopher S.; Chandrasekaran, Hema; Clarke, Bruce; Li, Jie; Quintana, Elisa V.; Tenenbaum, P.; Twicken, Joseph D.; Wu, Hayley

doi:10.1088/2041-8205/713/2/l79

Cited by 1,027 publications

(473 citation statements)

References 40 publications

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“…We find that 11 ± 4% of Sun-like stars harbor an Earthsize planet receiving between one and four times the stellar intensity as Earth. We also find that the occurrence of Earth-size planets is constant with increasing orbital period (P), within equal intervals of logP up to ∼200 d. Extrapolating, one finds 5:7 +1:7 −2:2 % of Sun-like stars harbor an Earth-size planet with orbital periods of 200-400 d. Kepler mission was launched in 2009 to search for planets that transit (cross in front of) their host stars (1)(2)(3)(4). The resulting dimming of the host stars is detectable by measuring their brightness, and Kepler monitored the brightness of 150,000 stars every 30 min for 4 y.…”

mentioning

confidence: 71%

Prevalence of Earth-size planets orbiting Sun-like stars

Petigura

Howard

Marcy

2013

Proc. Natl. Acad. Sci. U.S.A.

752

718

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mentioning

confidence: 71%

Prevalence of Earth-size planets orbiting Sun-like stars

Petigura

Howard

Marcy

2013

Proc. Natl. Acad. Sci. U.S.A.

752

718

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“…The observations yield an evenly sampled, minimally gapped flux time series that can be searched for periodic diminutions of light due to the transit of an exoplanet across the stellar disk in an aligned geometry. The photometer was engineered to achieve 20-ppm relative precision in 6.5 h for a 12th magnitude G-type main-sequence star (1). For reference, the Earth orbiting the Sun would produce an 84-ppm signal lasting ∼13 h.…”

Section: Nasa's 10th Discovery Missionmentioning

confidence: 99%

Exploring exoplanet populations with NASA’s Kepler Mission

Batalha

2014

Proc. Natl. Acad. Sci. U.S.A.

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233

168

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The Kepler Mission is exploring the diversity of planets and planetary systems. Its legacy will be a catalog of discoveries sufficient for computing planet occurrence rates as a function of size, orbital period, star type, and insolation flux. The mission has made significant progress toward achieving that goal. Over 3,500 transiting exoplanets have been identified from the analysis of the first 3 y of data, 100 planets of which are in the habitable zone. The catalog has a high reliability rate (85-90% averaged over the period/radius plane), which is improving as follow-up observations continue. Dynamical (e.g., velocimetry and transit timing) and statistical methods have confirmed and characterized hundreds of planets over a large range of sizes and compositions for both single-and multiple-star systems. Population studies suggest that planets abound in our galaxy and that small planets are particularly frequent. Here, I report on the progress Kepler has made measuring the prevalence of exoplanets orbiting within one astronomical unit of their host stars in support of the National Aeronautics and Space Administration's long-term goal of finding habitable environments beyond the solar system. planet detection | transit photometry

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“…In the automated Kepler data processing pipeline, the flux of the object is calculated by simple aperture photometry (SAP) [14]. The center of its observing wavelength is λ = 6600 Å [15,16]. We used the calibrated "SAP_FLUX" light curve with 1-min time resolution.…”

Section: The Kepler Light Curvementioning

confidence: 99%

Study of the Time-Series of Microvariability in Kepler Blazar W2R 1926+42

et al. 2017

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Abstract:One of the remarkable features of blazars is violent variability over a wide wavelength range. The variation mechanism causing the observed complex behavior is still under debate. The variability timescales range from less than a day to decades. Variation on timescales less than a day is known as "microvariability." Such short-term variations can provide insights regarding the origin of the variability after they are distinguished from longer-term variational components. We select about 195 microvariability events from the continuous light curve of blazar W2R 1926+42 with 1-min time resolution obtained by the Kepler spacecraft, and estimate the timescale and amplitude of each event. The rise and decay timescales of the events reveal random variations over short timescales less than a day, but they indicate systematic variations on timescales longer than several days. This result implies that the events are not independent, but rather mutually correlated.

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KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE

Cited by 1,027 publications

References 40 publications

Prevalence of Earth-size planets orbiting Sun-like stars

Prevalence of Earth-size planets orbiting Sun-like stars

Exploring exoplanet populations with NASA’s Kepler Mission

Study of the Time-Series of Microvariability in Kepler Blazar W2R 1926+42

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