Figure 11 from Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65

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Asteroseismic Determination of Obliquities of the Exoplanet Systems Kepler-50 and Kepler-65

Authors: W. J. Chaplin, R. Sanchis-Ojeda, T. L. Campante, R. Handberg, D. Stello, J. N. Winn, S. Basu, J. Christensen-Dalsgaard, G. R. Davies, T. S. Metcalfe, L. A. Buchhave, D. A. Fischer, T. R. Bedding, W. D. Cochran, Y. Elsworth, R. L. Gilliland, S. Hekker, D. Huber, H. Isaacson, C. Karoff, S. D. Kawaler, H. Kjeldsen, D. W. Latham, M. N. Lund, M. Lundkvist, G. W. Marcy, A. Miglio, T. Barclay, and J. J. Lissauer

Chaplin et al. 2013 The Astrophysical Journal 766 101.

Provider: AAS Journals

Caption: Figure 11.

Left-hand panels: three-month segments of the long-cadence PDC-MAP data (from Q5), in which intrinsic stellar variability on timescales of days is evident. The dots show the de-trended data (see text), and the thick line represents a smoothed version (10 hr boxcar). Right-hand panels: Lomb–Scargle periodograms of the PDC-MAP data of both stars. Thick black lines: periodograms from using all corrected data. Dashed, colored lines: periodograms of three independent three-quarter-long segments of data. Confidence intervals on the quoted average periods are marked by the vertical dotted lines.

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