@article{fdca454493c24ea7bb3ee4d016bc9824,
title = "K2-260 b: A hot Jupiter transiting an F star, and K2-261 b: A warm Saturn around a bright G star",
abstract = "We present the discovery and confirmation of two new transiting giant planets from the Kepler extended mission K2. K2-260 b is a hot Jupiter transiting a V = 12.7 F6V star in K2 Field 13, with a mass and radius of M = 1.39-0.06 +0.05 M⊙ and R = 1.69 ± 0.03 R. The planet has an orbital period of P = 2.627 d, and a mass and radius of MP = 1.42-0.32 +0.31 MJ and RP = 1.552-0.057 +0.048 RJ. This is the first K2 hot Jupiter with a detected secondary eclipse in the Kepler bandpass, with a depth of 71 ± 15 ppm, which we use to estimate a geometric albedo of Ag ~ 0.2. We also detected a candidate stellar companion at 0.6 arcsec from K2-260; we find that it is very likely physically associated with the system, in which case it would be an M5-6V star at a projected separation of ~400 au. K2-261 b is a warm Saturn transiting a bright (V = 10.5) G7IV/V star in K2 Field 14. The host star is a metal rich ([Fe/H] = 0.36 ± 0.06), mildly evolved 1.10-0.02 +0.01 M⊙ star with R = 1.65 ± 0.04 R. Thanks to its location near the main-sequence turn-off, we can measure a relatively precise age of 8.8-0.3 +0.4 Gyr. The planet has P = 11.633 d, MP = 0.223 ± 0.031 MJ, and RP = 0.850-0.022 +0.026 RJ, and its orbit is eccentric (e = 0.39 ± 0.15). Its brightness and relatively large transit depth make this one of the best-known warm Saturns for follow-up observations to further characterize the planetary system.",
keywords = "K2-261 b, Planets and satellites: detection, Planets and satellites: individual: K2-260 b",
author = "Johnson, {M. C.} and F. Dai and Justesen, {A. B.} and D. Gandolfi and Hatzes, {A. P.} and G. Nowak and M. Endl and Cochran, {W. D.} and D. Hidalgo and N. Watanabe and H. Parviainen and T. Hirano and S. Villanueva and J. Prieto-Arranz and N. Narita and E. Palle and Guenther, {E. W.} and O. Barrag{\'a}n and T. Trifonov and P. Niraula and MacQueen, {P. J.} and J. Cabrera and Sz Csizmadia and Ph Eigm{\"u}ller and S. Grziwa and J. Korth and M. P{\"a}tzold and Smith, {A. M.S.} and S. Albrecht and R. Alonso and H. Deeg and A. Erikson and M. Esposito and M. Fridlund and A. Fukui and N. Kusakabe and M. Kuzuhara and J. Livingston and {Monta{\~n}es Rodriguez}, P. and D. Nespral and Persson, {C. M.} and T. Purismo and S. Raimundo and H. Rauer and I. Ribas and M. Tamura and {Van Eylen}, V. and Winn, {J. N.}",
note = "Funding Information: We thank the anonymous referee for helpful comments that improved the quality of the paper. FD and JNW thank the Heising-Simons Foundation for financial support. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). This research was partly supported by JSPS (Japan Society for the Promotion of Science) KAKENHI Grant Number JP18H01265 and JST (Japan Science and Technology Agency) PRESTO (Precursory Research for Embryonic Science and Technology) Grant Number JPMJPR1775, Japan. APH, SzCs, SG, JK, MP, and HR acknowledge support by DFG (Deutsche Forschungsgemeinschaft) grants HA 3279/12-1, PA525/18-1, PA525/19-1, PA525/20-1, and RA 714/14-1 within the DFG Schwerpunkt SPP 1992, 'Exploring the Diversity of Extrasolar Planets'. WDC, ME, and PJM acknowledge support from NASA (National Aeronautics and Space Administration) grants NNX16AJ11G and 80NSSC18K0447 to The University of Texas at Austin. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement no. 730890. This material reflects only the authors views, and the Commission is not liable for any use that may be made of the information contained therein. We are very grateful to the McDonald, NOT, TNG, and ESO staffmembers for their support during the observations. This paper includes data taken at the McDonald Observatory of the University of Texas at Austin. Based on observations obtained (a) with the NOT, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos (ORM) of the Instituto de Astrofisica de Canarias (IAC), under programmes 56-010, 56-112, and 56-209; (b) with the Italian Telescopio Nazionale Galileo (TNG) also operated at the ORM (IAC) on the island of La Palma by the INAF (Istituto Nazionale di Astrofisica)-Fundacion Galileo Galilei, under Spanish CAT (Comisi{\'o}n de Asignaci{\'o}n de Tiempos) programmeCAT17B 99, OPTICON (Optical InfraredCoordination Network for Astronomy) programme OPT17B 59, and programme A36TAC 12, (c) with the 3.6 m ESO telescope at La Silla Observatory under programme 0100.C-0808 and 0101.C-0829. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This article is partly based on observations made with the MuSCAT2 instrument, developed by ABC (Astrobiology Center), at Telescopio Carlos S{\'a}nchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publicationmakes use of data products from theWide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research made use of NASA's Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013). Publisher Copyright: {\textcopyright} 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.",
year = "2018",
month = nov,
day = "21",
doi = "10.1093/mnras/sty2238",
language = "English (US)",
volume = "481",
pages = "596--612",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "1",
}