Radial velocity confirmation of K2-100b: a young, highly irradiated, and low density transiting hot Neptune. (arXiv:1909.05252v1 [astro-ph.EP])

Radial velocity confirmation of K2-100b: a young, highly irradiated, and low density transiting hot Neptune. (arXiv:1909.05252v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Barragan_O/0/1/0/all/0/1">O. Barrag&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aigrain_S/0/1/0/all/0/1">S. Aigrain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kubyshkina_D/0/1/0/all/0/1">D. Kubyshkina</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:+Livingston_J/0/1/0/all/0/1">J. Livingston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fridlund_M/0/1/0/all/0/1">M. C. V. Fridlund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_L/0/1/0/all/0/1">L. Fossati</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:+Parviainen_H/0/1/0/all/0/1">H. Parviainen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malavolta_L/0/1/0/all/0/1">L. Malavolta</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:+Deeg_H/0/1/0/all/0/1">H. J. Deeg</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:+Rajpaul_V/0/1/0/all/0/1">V. M. Rajpaul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zicher_N/0/1/0/all/0/1">N. Zicher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antoniciello_G/0/1/0/all/0/1">G. Antoniciello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narita_N/0/1/0/all/0/1">N. Narita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albrecht_S/0/1/0/all/0/1">S. Albrecht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedin_L/0/1/0/all/0/1">L. R. Bedin</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:+Leon_J/0/1/0/all/0/1">J. de Leon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eigmuller_P/0/1/0/all/0/1">Ph. Eigm&#xfc;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fukui_A/0/1/0/all/0/1">A. Fukui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Granata_V/0/1/0/all/0/1">V. Granata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grziwa_S/0/1/0/all/0/1">S. Grziwa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guenther_E/0/1/0/all/0/1">E. 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:+Kusakabe_N/0/1/0/all/0/1">N. Kusakabe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">D. W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Libralato_M/0/1/0/all/0/1">M. Libralato</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:+Montanes_Rodriguez_P/0/1/0/all/0/1">P. Monta&#xf1;&#xe9;s-Rodr&#xed;guez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murgas_F/0/1/0/all/0/1">F. Murgas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nardiello_D/0/1/0/all/0/1">D. Nardiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pagano_I/0/1/0/all/0/1">I. Pagano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piotto_G/0/1/0/all/0/1">G. Piotto</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:+Redfield_S/0/1/0/all/0/1">S. Redfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamura_M/0/1/0/all/0/1">M. Tamura</a>

We present a detailed analysis of HARPS-N radial velocity observations of
K2-100, a young and active star in the Praesepe cluster, which hosts a
transiting planet with a period of 1.7 days. We model the activity-induced
radial velocity variations of the host star with a multi-dimensional Gaussian
Process framework and detect a planetary signal of $10.6 pm 3.0 {rm
m,s^{-1}}$, which matches the transit ephemeris, and translates to a planet
mass of $21.8 pm 6.2 M_oplus$. We perform a suite of validation tests to
confirm that our detected signal is genuine. This is the first mass measurement
for a transiting planet in a young open cluster. The relatively low density of
the planet, $2.04^{+0.66}_{-0.61} {rm g,cm^{-3}}$, implies that K2-100b
retains a significant volatile envelope. We estimate that the planet is losing
its atmosphere at a rate of $10^{11}-10^{12},{rm g,s^{-1}}$ due to the high
level of radiation it receives from its host star.

We present a detailed analysis of HARPS-N radial velocity observations of
K2-100, a young and active star in the Praesepe cluster, which hosts a
transiting planet with a period of 1.7 days. We model the activity-induced
radial velocity variations of the host star with a multi-dimensional Gaussian
Process framework and detect a planetary signal of $10.6 pm 3.0 {rm
m,s^{-1}}$, which matches the transit ephemeris, and translates to a planet
mass of $21.8 pm 6.2 M_oplus$. We perform a suite of validation tests to
confirm that our detected signal is genuine. This is the first mass measurement
for a transiting planet in a young open cluster. The relatively low density of
the planet, $2.04^{+0.66}_{-0.61} {rm g,cm^{-3}}$, implies that K2-100b
retains a significant volatile envelope. We estimate that the planet is losing
its atmosphere at a rate of $10^{11}-10^{12},{rm g,s^{-1}}$ due to the high
level of radiation it receives from its host star.

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