SELECTION, PRIORITIZATION, AND CHARACTERISTICS OF
                    <i>KEPLER</i>
                    TARGET STARS

Batalha, Natalie M.; Borucki, W. J.; Koch, David; Bryson, Stephen T.; Haas, Michael R.; Brown, Timothy M.; Caldwell, Douglas A.; Hall, Jennifer R.; Latham, David W.; Meibom, S.; Monet, D. G.

doi:10.1088/2041-8205/713/2/l109

Cited by 471 publications

(581 citation statements)

References 15 publications

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“…However, the KIC sample was explicitly selected to contain only low-activity, large surface gravity (dwarf and sub-giant) stars (Batalha et al 2010). WASP-46 has an estimated age of 1.4 Gyr (Anderson et al 2011).…”

Section: Debris Disks In the Transiting Planet Samplementioning

confidence: 99%

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Warm debris disks candidates in transiting planets systems

Ribas

Merın

Ardila

et al. 2012

A&A

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We have bandmerged candidate transiting planetary systems (from the Kepler satellite) and confirmed transiting planetary systems (from the literature) with the recent Wide-field Infrared Survey Explorer (WISE) preliminary release catalog. We have found 13 stars showing infrared excesses at either 12 μm and/or 22 μm. Without longer wavelength observations it is not possible to conclusively determine the nature of the excesses, although we argue that they are likely due to debris disks around the stars. If confirmed, our sample ∼doubles the number of currently known warm excess disks around old main sequence stars. The ratios between the measured fluxes and the stellar photospheres are generally larger than expected for Gyr-old stars, such as these planetary hosts. Assuming temperature limits for the dust and emission from large dust particles, we derive estimates for the disk radii. These values are comparable to the planet's semi-major axis, suggesting that the planets may be stirring the planetesimals in the system.

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Section: Debris Disks In the Transiting Planet Samplementioning

confidence: 99%

“…The target stars are determined by the Kepler Input Catalog (KIC, Latham et al 2005;Batalha et al 2010). These are mostly main-sequence G type field dwarfs.…”

Section: Introductionmentioning

confidence: 99%

Warm debris disks candidates in transiting planets systems

Ribas

Merın

Ardila

et al. 2012

A&A

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“…Basri et al (2011, hereafter B11) went on to demonstrate that periodic variable stars have significantly larger amplitudes, as a sample, than aperiodic variables. Finally, Ciardi et al (2011, hereafter C11) performed a complementary study of the same sample using dispersion rather than amplitude as a variability statistic, and studying likely dwarfs and giants separately using the stellar parameters provided in the Kepler Input Catalog (KIC, Brown et al 2011;Batalha et al 2010). Variability statistics have also been determined using the 10 days of commissioning data (Q0), with the aim of developing methods to characterise and select specific types of variable .…”

Section: Introductionmentioning

confidence: 99%

Statistics of stellar variability fromKepler

McQuillan

Aigrain

Roberts

2012

A&A

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We investigate the variability properties of main sequence stars in the first month of Kepler data, using a new astrophysically robust systematics correction. We find that the fraction of stars with variability greater than that of the Sun is 60%, which is marginally consistent with previous studies, and confirm the trend of increasing variability with decreasing effective temperatures. We define low and high variability samples, with a cut corresponding to twice the variability level of the active Sun, and compare the properties of the stars belonging to each sample. We show tentative evidence that the more active stars have lower proper motions and may be located closer to the galactic plane. We also investigate the frequency content of the variability, finding clear evidence for periodic or quasi-periodic behaviour in 16% of stars, and showing that there exist significant differences in the nature of variability between spectral types. Of the periodic objects, most A and F stars have short periods (<2 days) and highly sinusoidal variability, suggestive of pulsations, whilst G, K and M stars tend to have longer periods (>5 days, with a trend towards longer periods at later spectral types) and show a mixture of periodic and stochastic variability, indicative of activity. Finally, we use auto-regressive models to characterise the stochastic component of the variability, and show that its typical amplitude and time-scale both increase towards later spectral types, which we interpret as a corresponding increase in the characteristic size and life-time of active regions.

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“…5 of Chaplin et al 2011a). The Kepler Input Catalog 2 (KIC; e.g., Latham et al 2005;Batalha et al 2010;Brown et al 2011), from which all 1 Within the Kepler Asteroseismic Science Consortium (KASC), KIC 10273246 is referred to as "Mulder" and KIC 10920273 as "Scully". 2 http://archive.stsci.edu/kepler/kepler_fov/search.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismology from multi-monthKeplerphotometry: the evolved Sun-like stars KIC 10273246 and KIC 10920273

Campante

Handberg

Mathur

et al. 2011

A&A

101

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Context. The evolved main-sequence Sun-like stars KIC 10273246 (F-type) and KIC 10920273 (G-type) were observed with the NASA Kepler satellite for approximately ten months with a duty cycle in excess of 90%. Such continuous and long observations are unprecedented for solar-type stars other than the Sun. Aims. We aimed mainly at extracting estimates of p-mode frequencies -as well as of other individual mode parameters -from the power spectra of the light curves of both stars, thus providing scope for a full seismic characterization. Methods. The light curves were corrected for instrumental effects in a manner independent of the Kepler science pipeline. Estimation of individual mode parameters was based both on the maximization of the likelihood of a model describing the power spectrum and on a classic prewhitening method. Finally, we employed a procedure for selecting frequency lists to be used in stellar modeling. Results. A total of 30 and 21 modes of degree l = 0, 1, 2 -spanning at least eight radial orders -have been identified for KIC 10273246 and KIC 10920273, respectively. Two avoided crossings (l = 1 ridge) have been identified for KIC 10273246, whereas one avoided crossing plus another likely one have been identified for KIC 10920273. Good agreement is found between observed and predicted mode amplitudes for the F-type star KIC 10273246, based on a revised scaling relation. Estimates are given of the rotational periods, the parameters describing stellar granulation and the global asteroseismic parameters Δν and ν max .

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SELECTION, PRIORITIZATION, AND CHARACTERISTICS OF KEPLER TARGET STARS

Cited by 471 publications

References 15 publications

Warm debris disks candidates in transiting planets systems

Warm debris disks candidates in transiting planets systems

Statistics of stellar variability fromKepler

Asteroseismology from multi-monthKeplerphotometry: the evolved Sun-like stars KIC 10273246 and KIC 10920273

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