TESS spots a hot Jupiter with an inner transiting Neptune

Chelsea X. Huang, Samuel N. Quinn, Andrew Vanderburg, Juliette Becker, Joseph E. Rodriguez, Francisco J. Pozuelos, Davide Gandolfi, George Zhou, Andrew W. Mann, Karen A. Collins, Ian Crossfield, Khalid Barkaoui, Kevin I. Collins, Malcolm Fridlund, Michaël Gillon, Erica J. Gonzales, Maximilian N. Günther, Todd J. Henry, Steve B. Howell, Hodari-Sadiki James, Wei-Chun Jao, Emmanuël Jehin, Eric L. N. Jensen, Stephen R. Kane, Jack J. Lissauer, Elisabeth Matthews, Rachel A. Matson, Leonardo A. Paredes, Joshua E. Schlieder, Keivan G. Stassun, Avi Shporer, Lizhou Sha, Thiam-Guan Tan, Iskra Georgieva, Savita Mathur, Enric Palle, Carina M. Persson, Vincent Van Eylen, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Christopher J. Burke, Robert F. Goeke, Stephen Rinehart, Mark E. Rose, Eric B. Ting, Guillermo Torres, Ian Wong

Published 2020-03-24Version 1

Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an 11th magnitude K-dwarf in the Gaia G band. It has two transiting planets: a Neptune-sized planet ($3.65\pm 0.10$ $R_E$) with a 4.1-day period, and a hot Jupiter ($1.50^{+0.27}_{-0.22}$ $R_J$) with an 8.4-day period. Precise radial-velocity observations show that the mass of the hot Jupiter is $0.974^{+0.043}_{-0.044}$ $M_J$. For the inner Neptune, the data provide only an upper limit on the mass of 0.17 $M_J$ (3$\sigma$). Nevertheless, we are confident the inner planet is real, based on follow-up ground-based photometry and adaptive optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.