KELT-25b and KELT-26b: A Hot Jupiter and a Substellar Companion Transiting Young A-stars Observed by TESS

Creators: Rodríguez Martínez, Romy; Gaudi, B. Scott; Rodriguez, Joseph E.; Zhou, George; Labadie-Bartz, Jonathan; Quinn, Samuel N.; Penev, Kaloyan Minev; Tan, Thiam-Guan; Latham, David W.; Paredes, Leonardo A.; Kielkopf, John; Addison, Brett C.; Wright, Duncan J.; Teske, Johanna K.; Howell, Steve B.; Ciardi, David R.; Ziegler, Carl; Stassun, Keivan G.; Johnson, Marshall C.; Eastman, Jason D.; Siverd, Robert J.; Beatty, Thomas G.; Bouma, Luke G.; Pepper, Joshua; Lund, Michael B.; Villanueva, Steven; Stevens, Daniel J.; Jensen, Eric L. N.; Kilby, Coleman; Cohen, David H.; Bayliss, Daniel; Bieryla, Allyson; Cargile, Phillip A.; Collins, Karen A.; Conti, Dennis M.; Colón, Knicole D.; Curtis, Ivan A.; DePoy, Darren L.; Evans, Phil A.; Feliz, Dax; Gregorio, Joao; Rothenberg, Jason; James, David J.; Penny, Matthew T.; Reed, Phillip A.; Relles, Howard M.; Stephens, Denise C.; Joner, Michael D.; Kuhn, Rudolf B.; Stockdale, Chris; Trueblood, Mark; Trueblood, Patricia; Yao, Xinyu; Zambelli, Roberto; Vanderspek, Roland; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Henry, Todd J.; James, Hodari-Sadiki; Jao, Wei-Chun; Wang, Sharon X.; Butler, R. Paul; Crane, Jeffrey D.; Thompson, Ian B.; Schectman, Stephen; Wittenmyer, Robert A.; Bedding, Timothy R.; Okumura, Jack; Plavchan, Peter; Bowler, Brendan P.; Horner, Jonathan; Kane, Stephen R.; Mengel, Matthew W.; Morton, Timothy D.; Tinney, C. G.; Zhang, Hui; Scott, Nicholas J.; Matson, Rachel A.; Everett, Mark E.; Tokovinin, Andrei; Mann, Andrew W.; Dragomir, Diana; Guenther, Maximilian N.; Ting, Eric B.; Fausnaugh, Michael; Glidden, Ana; Quintana, Elisa V.; Manner, Mark; Marshall, Jennifer L.; McLeod, Kim K.; Khakpash, Somayeh

Abstract

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 (T_(eff) = 8280⁺⁴⁴⁰₋₁₈₀ K, M⋆ = 2.18^(+0.12)_(−0.11) M⊙), while KELT-26 b is on a 3.34 day orbit around the V = 9.95 star HD 134004 (T_(eff) =8640⁺⁵⁰⁰₋₂₄₀ = K, M⋆ = 1.93^(+0.14)_(−0.16) M⊙), 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^(+0.039)_(−0.043) 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^(+0.43)_(−0.51) M_J and R_P = 1.940^(+0.060)_(−0.058) 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.

Additional Information

© 2020 The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2019 December 2; revised 2020 June 16; accepted 2020 June 17; published 2020 August 14. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. The authors thank the anonymous referee for providing useful comments that improved the quality of this paper. J.E.R. was supported by the Harvard Future Faculty Leaders Postdoctoral fellowship. Work by G.Z. is provided by NASA through Hubble Fellowship grant HST-HF2-51402.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA under contract NAS 5-26555. D.J.S. is supported by Penn State University's Eberly Research Fellowship. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Support for this work was provided by NASA through Hubble Fellowship grant HST-HF2-51399.001 awarded to J.K.T. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA under contract NAS5-26555. M.N.G. acknowledges support from MIT's Kavli Institute as a Juan Carlos Torres Fellow. C.Z. is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. K.G.S. acknowledges support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. T.N. and A.Y. are also grateful to Mizuki Isogai, Akira Arai, and Hideyo Kawakita for their technical support on observations at Koyama Astronomical Observatory. C.D.K. was supported by the Swarthmore College Provost's Office. J.L.-B. acknowledges support from FAPESP (grant 2017/23731-1). K.P. acknowledges support from NASA grants 80NSSC18K1009 and NNX17AB94G. Funding for the TESS mission is provided by NASA's Science Mission directorate. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), Ministério da Ciência, Tecnologia e Inovação (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Some of the observations in the paper made use of the High-Resolution Imaging instrument Zorro at Gemini-South. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration, 2018). MINERVA-Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grant DP180100972, the Mount Cuba Astronomical Foundation, and institutional partners the University of Southern Queensland, UNSW Australia, MIT, Nanjing University, George Mason University, the University of Louisville, the University of California Riverside, the University of Florida, and the University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all elders, ancestors, and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt. Kent is situated. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Facilities: FLWO 1.5 m (Tillinghast Reflector Echelle Spectrograph - , TRES); Kilodegree Extremely Little Telescope (KELT); MINiature Exoplanet Radial Velocity Array (MINERVA); Las Cumbres Observatory at Tenerife (LCO TFN); University of Louisville Manner Telescope (ULMT - , Mt. Lemmon); KeplerCam (FLWO 1.2 m); Stacja Obserwacji Tranzytów Egzoplanet w Suwałkach (SOTES); CROW Observatory; Koyama Astronomical Observatory (KAO); Gemini-South Zorro - . Software: EXOFASTv2 (Eastman et al. 2013; Eastman 2017), AstroImageJ (Collins et al. 2017), SPC (Buchhave et al. 2010).

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