Poster Abstracts - Kepler - NASA

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POSTER ABSTRACTSP0106. POSTER SESSION IThe Search for Jupiter Analogs in Kepler’s First Three Quarters J. A. Burt 1 , G. Laughlin 2 , P.Nutzman 2 , 1 University of California at Santa Cruz, Santa Cruz, CA, 95064; jaburt@ucsc.edu 2 Lick Observatory;laugh@ucolick.org, pnutzman@ucolick.orgIn the past three years the Kepler team has begunto determine the commonality of Earth-likeplanets in our galaxy through their use of phasefoldinglightcurve analysis [1]. While these detectionshelp astronomers to understand the frequencywith which short period planets occur,they are insensitive to planets with long orbitalperiods [2] (figure 1). Thus we are unable to assessthe commonality of our solar system as awhole because the data processing method ishighly unlikely to detect the signature of planetswith periods exceeding the current observationalbaseline, such as our Jupiter. These “true Jupiteranalogs” are an important factor in understandingthe dynamics of other star systems and as suchmerit a focused attempt at detection.We adopt an analysis method focused on detectinglong duration, single transit events. Thetraditional starting point of fitting high order polynomialsto the entire lightcurve poses the possibilityof also fitting a long duration transit and istherefore avoided. Thus the algorithm must berobust enough to deal with numerous changes incurvature due to both stellar variability and largeflux discontinuities caused by the equipment thatcannot be divided out. The magnitude of theseaffects varies strongly between stars, so the algorithmmust be able to handle such transitionsquickly and proficiently.Lightcurves are searched piecewise for evidenceof large scale changes in the photometricscatter that characterize of planetary transits.Once a transit is detected, the code works throughsuspected transit points, verifying them one at atime through an iterative fitting process. Whilethe code is currently tuned for Jupiter-sizedevents, its thresholds can be manipulated tosearch for planets on shorter-period orbits as well.Work is currently in progress to apply the algorithmto the publicly released Kepler data (Q1 –Q3). Preliminary results will be presented.References:[1] Jenkins et al. (2010) Proc. of SPIE, 7740. D1-D11[2] Borucki et al (2011) ApJ, 736:19Figure 1: Periods of Kepler's planet candidates. Forcomparison, Jupiter's period is ~4332 days.1162011 Kepler Science Conference - NASA Ames Research Center
POSTER ABSTRACTSP0107. POSTER SESSION ILINEAR AND NONLINEAR NOISE REDUCTION TECHNIQUES FOR KEPLER DATA. D. L. Buzasi 1 ,1Eureka Scientific, 2452 Delmer St., Ste. 100, Oakland, CA 94602, dbuzasi@gmail.com.The Kepler pipeline produces simple aperture photometryon each target, and engineering data and otherdiagnostics are used to remove systematic errors in theresulting time series. Time series are then searched forplanet signatures using an adaptive matched filter(Jenkins et al. 2010), and for stellar oscillations andother astrophysically interesting phenomena using avariety of techniques (Hekker et al. 2011, Mathur et al.2011). Noise levels found in these time series are up to50% higher than originally anticipated for the mission,with a large contribution to the noise level comingfrom intrinsic stellar signals such as activity and granulation(Gilliland et al. 2011).Buzasi (2007) suggested that use of a Wiener filterbased on the known signature of stellar granulationmight improve noise characteristics of the time series.However, this appears to be a significant improvementon the current (mostly time domain) filtering approachonly in certain portions of parameter space. Alternatively,nonlinear noise reduction techniques can beused for such broadband noise spectra. In this paper,we compare the performance of linear and nonlinearnoise reduction on Kepler data, with both planetary detectionand stellar oscillation applications in mind.2011 Kepler Science Conference - NASA Ames Research Center 117
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Poster Abstracts - Kepler - NASA

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