Universität zu Köln

Johnson, M. C., Dai, F., Justesen, A. B., Gandolfi, D., Hatzes, A. P., Nowak, G., Endl, M., Cochran, W. D., Hidalgo, D., Watanabe, N., Parviainen, H., Hirano, T., Villanueva, S., Jr., Prieto-Arranz, J., Narita, N., Palle, E., Guenther, E. W., Barragan, O., Trifonov, T., Niraula, P., MacQueen, P. J., Cabrera, J., Csizmadia, Sz., Eigmueller, Ph., Grziwa, S., Korth, J., Paetzold, M., Smith, A. M. S., Albrecht, S., Alonso, R., Deeg, H., Erikson, A., Esposito, M., Fridlund, M., Fukui, A., Kusakabe, N., Kuzuhara, M., Livingston, J., Montanes Rodriguez, P., Nespral, D., Persson, C. M., Purismo, T., Raimundo, S., Rauer, H., Ribas, I., Tamura, M., Van Eylen, V. and Winn, J. N. (2018). K2-260 b: a hot Jupiter transiting an F star, and K2-261 b: a warm Saturn around a bright G star. Mon. Not. Roy. Astron. Soc., 481 (1). S. 596 - 613. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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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-star = 1.39(-0.06)(+0.05) M-circle dot and R-star = 1.69 +/- 0.03 R-circle dot. The planet has an orbital period of P = 2.627 d, and a mass and radius of M-P = 1.42(-0.32)(+0.31) M-J and R-P = 1.552(-0.057)(+0.048) R-J. 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 A(g) similar to 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 similar to 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-circle dot star with R-star = 1.65 +/- 0.04 R-circle dot. 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, M-P = 0.223 +/- 0.031 M-J, and R-P = 0.850(-0.022)(+0.026) R-J, 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.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Johnson, M. C. UNSPECIFIED UNSPECIFIED UNSPECIFIED Dai, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Justesen, A. B. UNSPECIFIED UNSPECIFIED UNSPECIFIED Gandolfi, D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Hatzes, A. P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Nowak, G. UNSPECIFIED UNSPECIFIED UNSPECIFIED Endl, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Cochran, W. D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Hidalgo, D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Watanabe, N. UNSPECIFIED UNSPECIFIED UNSPECIFIED Parviainen, H. UNSPECIFIED UNSPECIFIED UNSPECIFIED Hirano, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Villanueva, S., Jr. UNSPECIFIED UNSPECIFIED UNSPECIFIED Prieto-Arranz, J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Narita, N. UNSPECIFIED UNSPECIFIED UNSPECIFIED Palle, E. UNSPECIFIED UNSPECIFIED UNSPECIFIED Guenther, E. W. UNSPECIFIED UNSPECIFIED UNSPECIFIED Barragan, O. UNSPECIFIED UNSPECIFIED UNSPECIFIED Trifonov, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Niraula, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED MacQueen, P. J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Cabrera, J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Csizmadia, Sz. UNSPECIFIED UNSPECIFIED UNSPECIFIED Eigmueller, Ph. UNSPECIFIED UNSPECIFIED UNSPECIFIED Grziwa, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Korth, J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Paetzold, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Smith, A. M. S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Albrecht, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Alonso, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Deeg, H. UNSPECIFIED UNSPECIFIED UNSPECIFIED Erikson, A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Esposito, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Fridlund, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Fukui, A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Kusakabe, N. UNSPECIFIED UNSPECIFIED UNSPECIFIED Kuzuhara, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Livingston, J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Montanes Rodriguez, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Nespral, D. UNSPECIFIED UNSPECIFIED UNSPECIFIED Persson, C. M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Purismo, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Raimundo, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Rauer, H. UNSPECIFIED UNSPECIFIED UNSPECIFIED Ribas, I. UNSPECIFIED UNSPECIFIED UNSPECIFIED Tamura, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Van Eylen, V. UNSPECIFIED UNSPECIFIED UNSPECIFIED Winn, J. N. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-167162
DOI:	10.1093/mnras/sty2238
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	481
Number:	1
Page Range:	S. 596 - 613
Date:	2018
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language SECONDARY ECLIPSE; SIZED PLANET; SUPER-EARTHS; ORBIT; SPECTROGRAPH; COMPANIONS; VELOCITIES; PHOTOMETRY; EXOPLANETS; EVOLUTION Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/16716