Romy Rodríguez Martínez, The Ohio State University
B. Scott Gaudi, The Ohio State University
Joseph E. Rodriguez, Harvard-Smithsonian Center for Astrophysics
George Zhou, Harvard-Smithsonian Center for Astrophysics
Jonathan Labadie-Bartz, Universidade de São Paulo
Samuel N. Quinn, Harvard-Smithsonian Center for Astrophysics
Kaloyan Penev, The University of Texas at Dallas
Thiam Guan Tan, Perth Exoplanet Survey Telescope
David W. Latham, Harvard-Smithsonian Center for Astrophysics
Leonardo A. Paredes, Georgia State University
John F. Kielkopf, University of Louisville
Brett Addison, University of Southern Queensland
Duncan J. Wright, University of Southern Queensland
Johanna Teske, Carnegie Observatories
Steve B. Howell, NASA Ames Research Center
David Ciardi, California Institute of Technology
Carl Ziegler, Dunlap Institute for Astronomy & Astrophysics
Keivan G. Stassun, Vanderbilt University
Marshall C. Johnson, Las Cumbres Observatory Global Telescope Network, Inc
Jason D. Eastman, Harvard-Smithsonian Center for Astrophysics
Robert J. Siverd, Gemini Observatory
Thomas G. Beatty, The University of Arizona
Luke Bouma, Princeton University
Timothy Bedding, The University of Sydney
Joshua Pepper, Lehigh University
Joshua Winn, Princeton University
Michael B. Lund, California Institute of Technology
Steven Villanueva, MIT Kavli Institute for Astrophysics and Space Research
Daniel J. Stevens, Pennsylvania State University
Eric L.N. Jensen, Swarthmore College
Coleman Kilby, Swarthmore College
Jeffrey D. Crane, Carnegie Observatories
Andrei Tokovinin, Cerro Tololo Inter American Observatory

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We present the discoveries of KELT-25 b (TIC 65412605, TOI-626.01) and KELT-26 b (TIC 160708862, TOI-1337.01), two transiting companions orbiting relatively bright, early A stars. The transit signals were initially detected by the KELT survey and subsequently confirmed by Transiting Exoplanet Survey Satellite (TESS) photometry. KELT-25 b is on a 4.40 day orbit around the V = 9.66 star CD-24 5016 (Teff=8280-180+440 K, M ∗ = 2.18-0.11+0.12 M o˙), while KELT-26 b is on a 3.34 day orbit around the V = 9.95 star HD 134004 (Teff = 8640-240+500 K, M ∗ = 1.93-0.16+0.14 M o˙), which is likely an Am star. We have confirmed the substellar nature of both companions through detailed characterization of each system using ground-based and TESS photometry, radial velocity measurements, Doppler tomography, and high-resolution imaging. For KELT-25, we determine a companion radius of R P = 1.64-0.043+0.039 R J and a 3σ upper limit on the companion's mass of ∼64 M J. For KELT-26 b, we infer a planetary mass and radius of M P = 1.41-0.51+0.43MJ and R P = 1.94-0.058+0.060 R J. From Doppler tomographic observations, we find KELT-26 b to reside in a highly misaligned orbit. This conclusion is weakly corroborated by a subtle asymmetry in the transit light curve from the TESS data. KELT-25 b appears to be in a well-aligned, prograde orbit, and the system is likely a member of the cluster Theia 449.

Publication Source (Journal or Book title)

Astronomical Journal