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An Ancient Extrasolar System with Five Sub-Earth-size Planets

  • Authors: T. L. Campante, T. Barclay, J. J. Swift, D. Huber, V. Zh. Adibekyan, W. Cochran, C. J. Burke, H. Isaacson, E. V. Quintana, G. R. Davies, V. Silva Aguirre, D. Ragozzine, R. Riddle, C. Baranec, S. Basu, W. J. Chaplin, J. Christensen-Dalsgaard, T. S. Metcalfe, T. R. Bedding, R. Handberg, D. Stello, J. M. Brewer, S. Hekker, C. Karoff, R. Kolbl, N. M. Law, M. Lundkvist, A. Miglio, J. F. Rowe, N. C. Santos, C. Van Laerhoven, T. Arentoft, Y. P. Elsworth, D. A. Fischer, S. D. Kawaler, H. Kjeldsen, M. N. Lund, G. W. Marcy, S. G. Sousa, A. Sozzetti, and T. R. White

Campante et al. 2015 The Astrophysical Journal 799 170.

  • Provider: AAS Journals

Caption: Figure 6.

Wavelet analysis of the oscillation power spectrum. Bottom panel: wavelet transform using a Morlet wavelet. The transform is affected by two priors. The first is that Δν and νmax must be consistent with a simple scaling relation (alternate blue-and-red curve; Stello et al. 2009a). This allows us to reduce the impact of power that lies well away from the scaling relation (by imposing a Gaussian fall-off with a characteristic scale on either side of this curve). The second prior is applied to νmax and kept wide enough as νmax = 4500 ± 800 μHz (represented by a dash-dotted curve in the top panel). The estimate of νmax returned by this analysis is represented by a vertical dashed line. The slanted solid lines toward the edges of the plotting area delimit the cone of influence. Top panel: same power wavelet spectrum with priors applied, but now integrated over the ordinate frequency (i.e., over all scales). The dashed curve represents a Gaussian fit to the wavelet spectrum.

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