K2-295 b and K2-237 b: two transiting hot Jupiters. (arXiv:1807.05865v2 [astro-ph.EP] UPDATED)
<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:+Csizmadia_S/0/1/0/all/0/1">Sz. Csizmadia</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:+Albrecht_S/0/1/0/all/0/1">S. Albrecht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_R/0/1/0/all/0/1">R. Alonso</a>, <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:+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:+Dai_F/0/1/0/all/0/1">F. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deeg_H/0/1/0/all/0/1">H. Deeg</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:+Endl_M/0/1/0/all/0/1">M. Endl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erikson_A/0/1/0/all/0/1">A. Erikson</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:+Fukui_A/0/1/0/all/0/1">A. Fukui</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. 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:+Hidalgo_D/0/1/0/all/0/1">D. Hidalgo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirano_T/0/1/0/all/0/1">T. Hirano</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:+Kuzuhara_M/0/1/0/all/0/1">M. Kuzuhara</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:+Narita_N/0/1/0/all/0/1">N. Narita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nespral_D/0/1/0/all/0/1">D. Nespral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niraula_P/0/1/0/all/0/1">P. Niraula</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:+Palle_E/0/1/0/all/0/1">E. Palle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patzold_M/0/1/0/all/0/1">M. P&#xe4;tzold</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:+Prieto_Arranz_J/0/1/0/all/0/1">J. Prieto-Arranz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauer_H/0/1/0/all/0/1">H. Rauer</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:+Ribas_I/0/1/0/all/0/1">I. Ribas</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 the discovery from K2 of two transiting hot Jupiter systems. K2-295
(observed in Campaign 8) is a K5 dwarf which hosts a planet slightly smaller
than Jupiter, orbiting with a period of 4.0 d. We have made an independent
discovery of K2-237 b (Campaign 11), which orbits an F6 dwarf every 2.2 d and
has an inflated radius 50 – 60 per cent larger than that of Jupiter. We use
high-precision radial velocity measurements, obtained using the HARPS and FIES
spectrographs, to measure the planetary masses. We find that K2-295 b has a
similar mass to Saturn, while K2-237 b is a little more massive than Jupiter.

We report the discovery from K2 of two transiting hot Jupiter systems. K2-295
(observed in Campaign 8) is a K5 dwarf which hosts a planet slightly smaller
than Jupiter, orbiting with a period of 4.0 d. We have made an independent
discovery of K2-237 b (Campaign 11), which orbits an F6 dwarf every 2.2 d and
has an inflated radius 50 – 60 per cent larger than that of Jupiter. We use
high-precision radial velocity measurements, obtained using the HARPS and FIES
spectrographs, to measure the planetary masses. We find that K2-295 b has a
similar mass to Saturn, while K2-237 b is a little more massive than Jupiter.

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