Branch (LLRGB) Stars Samuel Grunblatt, Daniel Huber, Eric Gaidos, Eric Lopez, Filipe Pereira, Tiago Campante Institute for Astronomy, University of Hawaii— Manoa, Honolulu, HI, USA
harmonic oscillator GP kernel functions to account for astrophysical noise Grunblatt et al. (2017) Simple Harmonic Oscillator GP Squared Exponential GP
GP model traces stellar granulation & oscillation signals: estimate of νmax from time-domain! Grunblatt et al. (in prep.) νmax, pipeline = 245.65 ± 3.51 μHz νmax, GP = 239.4 ± 1.8 μHz
1.27 +/- 0.02 RJup is in excellent agreement with the early predictions of Guillot et al. (1996), who calculated the radius for a strongly irradiated radiative/convective extrasolar planet for a variety of masses.”
of stars searched where SNR(transit) > some threshold (determined by injection/recovery here) Made grid of periods and planet radii, and for each grid cell, calculated whether SNR > SNRthreshold for every star in our sample to find n* Howard et al. (2012)
framework provides uniquely well- characterized exoplanet systems. Among ~4500 LLRGB stars, 2 (remarkably similar) close- in, transiting, likely re-inflated giant planets found: related to eccentricity? indicative of unique evolutionary pathway among evolved stars? Planet occurrence of LLRGB stars roughly comparable to MS, but effects of evolution could be appearing…TESS is the answer!