WASP-167b/KELT-13b: Joint discovery of a hot Jupiter transiting a rapidly rotating F1V star

L. Y. Temple, C. Hellier, M. D. Albrow, D. R. Anderson, D. Bayliss, T. G. Beatty, A. Bieryla, D. J.A. Brown, P. A. Cargile, A. Collier Cameron, K. A. Collins, K. D. Colón, I. A. Curtis, G. D'Ago, L. Delrez, J. Eastman, B. S. Gaudi, M. Gillon, J. Gregorio, D. JamesE. Jehin, M. D. Joner, J. F. Kielkopf, R. B. Kuhn, J. Labadie-Bartz, D. W. Latham, M. Lendl, M. B. Lund, A. L. Malpas, P. F.L. Maxted, G. Myers, T. E. Oberst, F. Pepe, J. Pepper, D. Pollacco, D. Queloz, J. E. Rodriguez, D. Ségransan, R. J. Siverd, B. Smalley, K. G. Stassun, D. J. Stevens, C. Stockdale, T. G. Tan, A. H.M.J. Triaud, S. Udry, S. Villanueva, R. G. West, G. Zhou

Research output: Contribution to journalArticlepeer-review

41 Scopus citations


We report the jointWASP/KELT discovery ofWASP-167b/KELT-13b, a transiting hot Jupiter with a 2.02-d orbit around a V = 10.5, F1V star with [Fe/H] = 0.1 ± 0.1. The 1.5 RJup planet was confirmed by Doppler tomography of the stellar line profiles during transit. We place a limit of < 8 MJup on its mass. The planet is in a retrograde orbit with a sky-projected spin-orbit angle of λ=-165° ±5°. This is in agreement with the known tendency for orbits around hotter stars to be more likely to be misaligned. WASP-167/KELT-13 is one of the few systems where the stellar rotation period is less than the planetary orbital period. We find evidence of non-radial stellar pulsations in the host star, making it a δ-Scuti or γ -Dor variable. The similarity to WASP-33, a previously known hot-Jupiter host with pulsations, adds to the suggestion that close-in planets might be able to excite stellar pulsations.

Original languageEnglish (US)
Pages (from-to)2743-2752
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
StatePublished - Nov 1 2017

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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