Dragomir, Diana2; Matthews, Jaymie M.3; Howard, Andrew W.4; Antoci, Victoria13; Henry, Gregory W.5; Guenther, David B.6; Johnson, John A.7; Kuschnig, Rainer8; Marcy, Geoffrey W.4; Moffat, Anthony F. J.9; Rowe, Jason F.10; Rucinski, Slavek M.11; Sasselov, Dimitar12; Weiss, Werner W.8
1 Department of Physics and Astronomy, Science and Technology, Aarhus University2 Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada firstname.lastname@example.org Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada4 Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA5 Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209, USA6 Department of Astronomy and Physics, St. Marys University Halifax, NS B3H 3C3, Canada7 Department of Astronomy, California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA8 Universität Wien, Institut für Astronomie, Türkenschanzstrasse 17, A1180 Wien, Austria9 Dépt de physique, Univ de Montréal C.P. 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, and Obs. du mont Mégantic, Canada10 NASA Ames Research Center, Moffett Field, CA 94035, USA11 Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada12 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA13 Department of Physics and Astronomy, Science and Technology, Aarhus University
The radial velocity-discovered exoplanet HD 97658b was recently announced to transit, with a derived planetary radius of 2.93 ± 0.28 R ⊕. As a transiting super-Earth orbiting a bright star, this planet would make an attractive candidate for additional observations, including studies of its atmospheric properties. We present and analyze follow-up photometric observations of the HD 97658 system acquired with the Microvariability and Oscillations of STars space telescope. Our results show no transit with the depth and ephemeris reported in the announcement paper. For the same ephemeris, we rule out transits for a planet with radius larger than 2.09 R ⊕, corresponding to the reported 3σ lower limit. We also report new radial velocity measurements which continue to support the existence of an exoplanet with a period of 9.5 days, and obtain improved orbital parameters.