K2-99 revisited: a non-inflated warm Jupiter, and a temperate giant planet on a 522-d orbit around a subgiant. (arXiv:2111.14660v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Smith_A/0/1/0/all/0/1">A. M. S. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breton_S/0/1/0/all/0/1">S. N. Breton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Csizmadia_S/0/1/0/all/0/1">Sz. Csizmadia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_F/0/1/0/all/0/1">F. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gandolfi_D/0/1/0/all/0/1">D. Gandolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_R/0/1/0/all/0/1">R. A. García</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_A/0/1/0/all/0/1">A. W. Howard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isaacson_H/0/1/0/all/0/1">H. Isaacson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korth_J/0/1/0/all/0/1">J. Korth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lam_K/0/1/0/all/0/1">K. W. F. Lam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathur_S/0/1/0/all/0/1">S. Mathur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nowak_G/0/1/0/all/0/1">G. Nowak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_F/0/1/0/all/0/1">F. Pérez Hernández</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Persson_C/0/1/0/all/0/1">C. M. Persson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albrecht_S/0/1/0/all/0/1">S. H. Albrecht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barragan_O/0/1/0/all/0/1">O. Barragán</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrera_J/0/1/0/all/0/1">J. Cabrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cochran_W/0/1/0/all/0/1">W. D. Cochran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deeg_H/0/1/0/all/0/1">H.J. Deeg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fridlund_M/0/1/0/all/0/1">M. Fridlund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Georgieva_I/0/1/0/all/0/1">I. Y. Georgieva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goffo_E/0/1/0/all/0/1">E. Goffo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guenther_E/0/1/0/all/0/1">E. W. Guenther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatzes_A/0/1/0/all/0/1">A. P. Hatzes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kabath_P/0/1/0/all/0/1">P. Kabath</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Livingston_J/0/1/0/all/0/1">J. H. Livingston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luque_R/0/1/0/all/0/1">R. Luque</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palle_E/0/1/0/all/0/1">E. Palle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Redfield_S/0/1/0/all/0/1">S. Redfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodler_F/0/1/0/all/0/1">F. Rodler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serrano_L/0/1/0/all/0/1">L. M. Serrano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eylen_V/0/1/0/all/0/1">V. Van Eylen</a>
We report new photometric and spectroscopic observations of the K2-99
planetary system. Asteroseismic analysis of the short-cadence light curve from
K2’s Campaign 17 allows us to refine the stellar properties. We find K2-99 to
be significantly smaller than previously thought, with $R_{star} =
2.55pm0.02$ $mathrm{R_odot}$. The new light curve also contains four
transits of K2-99b, which we use to improve our knowledge of the planetary
properties. We find the planet to be a non-inflated warm Jupiter, with
$R_mathrm{b} = 1.06 pm 0.01$ $mathrm{R_{Jup}}$. Sixty new radial velocity
measurements from HARPS, HARPS-N, and HIRES enable the determination of the
orbital parameters of K2-99c, which were previously poorly constrained. We find
that this outer planet has a minimum mass $M_mathrm{c} sin i_mathrm{c} =
8.4pm0.2$ $mathrm{M_{Jup}}$, and an eccentric orbit ($e_mathrm{c} = 0.210
pm 0.009$) with a period of $522.2pm1.4$ d. Upcoming TESS observations in
2022 have a good chance of detecting the transit of this planet, if the mutual
inclination between the two planetary orbits is small.
We report new photometric and spectroscopic observations of the K2-99
planetary system. Asteroseismic analysis of the short-cadence light curve from
K2’s Campaign 17 allows us to refine the stellar properties. We find K2-99 to
be significantly smaller than previously thought, with $R_{star} =
2.55pm0.02$ $mathrm{R_odot}$. The new light curve also contains four
transits of K2-99b, which we use to improve our knowledge of the planetary
properties. We find the planet to be a non-inflated warm Jupiter, with
$R_mathrm{b} = 1.06 pm 0.01$ $mathrm{R_{Jup}}$. Sixty new radial velocity
measurements from HARPS, HARPS-N, and HIRES enable the determination of the
orbital parameters of K2-99c, which were previously poorly constrained. We find
that this outer planet has a minimum mass $M_mathrm{c} sin i_mathrm{c} =
8.4pm0.2$ $mathrm{M_{Jup}}$, and an eccentric orbit ($e_mathrm{c} = 0.210
pm 0.009$) with a period of $522.2pm1.4$ d. Upcoming TESS observations in
2022 have a good chance of detecting the transit of this planet, if the mutual
inclination between the two planetary orbits is small.
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