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:
CreatorsEmailORCIDORCID Put Code
Johnson, M. C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Dai, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Justesen, A. B.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gandolfi, D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hatzes, A. P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Nowak, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Endl, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Cochran, W. D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hidalgo, D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Watanabe, N.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Parviainen, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hirano, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Villanueva, S., Jr.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Prieto-Arranz, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Narita, N.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Palle, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Guenther, E. W.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Barragan, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Trifonov, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Niraula, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
MacQueen, P. J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Cabrera, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Csizmadia, Sz.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eigmueller, Ph.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Grziwa, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Korth, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Paetzold, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Smith, A. M. S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Albrecht, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Alonso, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Deeg, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Erikson, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Esposito, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Fridlund, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Fukui, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kusakabe, N.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kuzuhara, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Livingston, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Montanes Rodriguez, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Nespral, D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Persson, C. M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Purismo, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Raimundo, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rauer, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ribas, I.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Tamura, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Van Eylen, V.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Winn, J. N.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
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:
KeywordsLanguage
SECONDARY ECLIPSE; SIZED PLANET; SUPER-EARTHS; ORBIT; SPECTROGRAPH; COMPANIONS; VELOCITIES; PHOTOMETRY; EXOPLANETS; EVOLUTIONMultiple languages
Astronomy & AstrophysicsMultiple languages
Refereed: Yes
URI: http://kups.ub.uni-koeln.de/id/eprint/16716

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