Psaridi, Angelica and Bouchy, François and Lendl, Monika and Grieves, Nolan and Stassun, Keivan G. and Carmichael, Theron W. and Gill, Samuel and Peña Rojas, Pablo A. and Gan, Tianjun and Shporer, Avi and Bieryla, Allyson and Brahm, Rafael and Christiansen, Jessie L. and Crossfield, Ian J. M. and Galland, Franck and Hooton, Matthew J. and Jenkins, Jon M. and Jenkins, James S. and Latham, David W. and Lund, Michael B. and Rodriguez, Joseph E. and Ting, Eric B. and Udry, Stéphane and Ulmer-Moll, Solène and Wittenmyer, Robert A. and Zhang, Yanzhe and Zhou, George and Addison, Brett and Cointepas, Marion and Collins, Karen A. and Collins, Kevin I. and Deline, Adrien and Dressing, Courtney D. and Evans, Phil and Giacalone, Steven and Heitzmann, Alexis and Mireles, Ismael and Mounzer, Dany and Otegi, Jon and Radford, Don J. and Rudat, Alexander and Schlieder, Joshua E. and Schwarz, Richard P. and Srdoc, Gregor and Stockdale, Chris and Suarez, Olga and Wright, Duncan J. and Zhao, Yinan (2022) Three new brown dwarfs and a massive hot Jupiter revealed by TESS around early-type stars. Astronomy and Astrophysics, 664 . Art. No. A94. ISSN 0004-6361. doi:10.1051/0004-6361/202243454. https://resolver.caltech.edu/CaltechAUTHORS:20220815-504703000
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Abstract
Context. The detection and characterization of exoplanets and brown dwarfs around massive AF-type stars is essential to investigate and constrain the impact of stellar mass on planet properties. However, such targets are still poorly explored in radial velocity (RV) surveys because they only feature a small number of stellar lines and those are usually broadened and blended by stellar rotation as well as stellar jitter. As a result, the available information about the formation and evolution of planets and brown dwarfs around hot stars is limited. Aims. We aim to increase the sample and precisely measure the masses and eccentricities of giant planets and brown dwarfs transiting early-type stars detected by the Transiting Exoplanet Survey Satellite (TESS). Methods. We followed bright (V < 12 mag) stars with T_(eff) > 6200 K that host giant companions (R > 7 R_⊕) using ground-based photometric observations as well as high precision radial velocity measurements from the CORALIE, CHIRON, TRES, FEROS, and MINERVA-Australis spectrographs. Results. In the context of the search for exoplanets and brown dwarfs around early-type stars, we present the discovery of three brown dwarf companions, TOI-629b, TOI-1982b, and TOI-2543b, and one massive planet, TOI-1107b. From the joint analysis of TESS and ground-based photometry in combination with high precision radial velocity measurements, we find the brown dwarfs have masses between 66 and 68 M_(Jup), periods between 7.54 and 17.17 days, and radii between 0.95 and 1.11 R_(Jup). The hot Jupiter TOI-1107b has an orbital period of 4.08 days, a radius of 1.30 R_(Jup), and a mass of 3.35 M_(Jup). As a by-product of this program, we identified four low-mass eclipsing components (TOI-288b, TOI-446b, TOI-478b, and TOI-764b). Conclusions. Both TOI-1107b and TOI-1982b present an anomalously inflated radius with respect to the age of these systems. TOI-629 is among the hottest stars with a known transiting brown dwarf. TOI-629b and TOI-1982b are among the most eccentric brown dwarfs. The massive planet and the three brown dwarfs add to the growing population of well-characterized giant planets and brown dwarfs transiting AF-type stars and they reduce the apparent paucity.
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| Additional Information: | © A. Psaridi et al. 2022. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received: 2 March 2022 Accepted: 25 April 2022. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support. This work was carried out in the frame of the Swiss National Centre for Competence in Research (NCCR) PlanetS supported by the Swiss National Science Foundation (SNSF). This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planet data visualization, exchange, and analysis. DACE is a platform of NCCR PlanetS and is available at https://dace.unige.ch. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. JSJ gratefully acknowledges support by FONDECYT grant 1201371 and from the ANID BASAL projects ACE210002 and FB210003. 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. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. We acknowledge the efforts of Michael Calkin, Perry Berlind, and Gil Esquerdo for their diligent observations using the TRES spectrograph at Mount Hopkins, Arizona. Data presented herein were obtained at the MINERVA-Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognise 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. | ||||||||||||||||||||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | brown dwarfs / planetary systems / techniques: photometric / techniques: radial velocities / stars: early-type / binaries: eclipsing | ||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202243454 | ||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20220815-504703000 | ||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20220815-504703000 | ||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Three new brown dwarfs and a massive hot Jupiter revealed by TESS around early-type stars Angelica Psaridi, François Bouchy, Monika Lendl, Nolan Grieves, Keivan G. Stassun, Theron Carmichael, Samuel Gill, Pablo A. Peña Rojas, Tianjun Gan, Avi Shporer, Allyson Bieryla, Rafael Brahm, Jessie L. Christiansen, Ian J. M. Crossfield, Franck Galland, Matthew J. Hooton, Jon M. Jenkins, James S. Jenkins, David W. Latham, Michael B. Lund, Joseph E. Rodriguez, Eric B. Ting, Stéphane Udry, Solène Ulmer-Moll, Robert A. Wittenmyer, Yanzhe Zhang, George Zhou, Brett Addison, Marion Cointepas, Karen A. Collins, Kevin I. Collins, Adrien Deline, Courtney D. Dressing, Phil Evans, Steven Giacalone, Alexis Heitzmann, Ismael Mireles, Dany Mounzer, Jon Otegi, Don J. Radford, Alexander Rudat, Joshua E. Schlieder, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Olga Suarez, Duncan J. Wright and Yinan Zhao A&A, 664 (2022) A94 DOI: https://doi.org/10.1051/0004-6361/202243454 | ||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||
| ID Code: | 116286 | ||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 16 Aug 2022 14:32 | ||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 16 Aug 2022 14:32 |
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