K2-237 b and K2-238 b: discovery and characterization of two new transiting hot Jupiters from K2

Creators: Soto, M. G.; Díaz, M. R.; Jenkins, J. S.; Rojas, F.; Espinoza, N.; Brahm, R.; Drass, H.; Jones, M. I.; Rabus, M.; Hartman, J.; Sarkis, P.; Jordán, A.; Lachaume, R.; Pantoja, B.; Vučković, M.; Ciardi, D. R.; Crossfield, I.; Dressing, C.; Gonzales, E.; Hirsch, L.

Abstract

We report the discovery of two hot Jupiters orbiting the stars K2-237 and K2-238. We used photometric data from Campaigns 11 and 12 of the Kepler K2mission and radial velocity data obtained using the HARPS, FEROS, and CORALIE spectrographs. K2-237 b and K2-238 b have masses of 1.60^(+0.11)_(−0.11) and 0.86^(+0.13)_(−0.12) M_(Jup), radii of 1.65^(+0.07)_(−0.08) and 1.30^(+0.15)_(−0.14) R_(Jup), and are orbiting their host stars in 2.18- and 3.20-d orbits, respectively. The large radius of K2-237 b leads us to conclude that this candidate corresponds to a highly inflated hot Jupiter. K2-238 b has a radius consistent with theoretical models, considering the high incident flux falling on the planet. We consider K2-237 b to be an excellent system for follow-up studies, since not only is it very inflated, but it also orbits a relatively bright star (V = 11.6).

Additional Information

© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices). Accepted 2018 May 17. Received 2018 May 16; in original form 2018 January 23. Published: 18 May 2018. MGS acknowledges the support of CONICYT-PFCHA/Doctorado Nacional-21141037, Chile. MRD is supported by CONICYT-PFCHA/Doctorado Nacional-21140646, Chile. JSJ acknowledges support by FONDECYT grant 1161218 and partial support by CATA-Basal (PB06, CONICYT). AJ acknowledges support from FONDECYT project 1171208, BASAL CATA PFB-06, and by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). HD acknowledges support from FONDECYT Postdoctorado 3150314 and FONDECYT Regular 1171364, from Fondo Nacional de Desarrollo Científico y Tecnológico. RL acknowledges support from BASAL CATA PFB-06. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS 143, 23.

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