no code implementations • 20 Sep 2017 • Robert J. Siverd, Karen A. Collins, George Zhou, Samuel N. Quinn, B. Scott Gaudi, Keivan G. Stassun, Marshall C. Johnson, Allyson Bieryla, David W. Latham, David R. Ciardi, Joseph E. Rodriguez, Kaloyan Penev, Marc Pinsonneault, Joshua Pepper, Jason D. Eastman, Howard Relles, John F. Kielkopf, Joao Gregorio, Thomas E. Oberst, Giulio Francesco Aldi, Gilbert A. Esquerdo, Michael L. Calkins, Perry Berlind, Courtney D. Dressing, Rahul Patel, Daniel J. Stevens, Thomas G. Beatty, Michael B. Lund, Jonathan Labadie-Bartz, Rudolf B. Kuhn, Knicole D. Colón, David James, Xinyu Yao, John A. Johnson, Jason T. Wright, Nate McCrady, Robert A. Wittenmyer, Samson A. Johnson, David H. Sliski, Eric L. N. Jensen, David H. Cohen, Kim K. McLeod, Matthew T. Penny, Michael D. Joner, Denise C. Stephens, Steven Villanueva Jr., Roberto Zambelli, Christopher Stockdale, Phil Evans, Thiam-Guan Tan, Ivan A. Curtis, Phillip A. Reed, Mark Trueblood, Patricia Trueblood
We confirm the planetary nature of the companion via a combination of radial velocities, which limit the mass to $< 4. 1\,\mathrm{M_J}$ $(3\sigma)$, and a clear Doppler tomography signal, which indicates a retrograde projected spin-orbit misalignment of $\lambda = -179. 7^{+3. 7}_{-3. 8}$ degrees.
Earth and Planetary Astrophysics