TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS

Medientyp: E-Artikel
Titel: TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS
Beteiligte: Davis, Allen B.; Wang, Songhu; Jones, Matias; Eastman, Jason D.; Günther, Maximilian N.; Stassun, Keivan G.; Addison, Brett C.; Collins, Karen A.; Quinn, Samuel N.; Latham, David W.; Trifonov, Trifon; Shahaf, Sahar; Mazeh, Tsevi; Kane, Stephen R.; Narita, Norio; Wang, Xian-Yu; Tan, Thiam-Guan; Ciardi, David R.; Tokovinin, Andrei; Ziegler, Carl; Tronsgaard, René; Millholland, Sarah; Cruz, Bryndis; Berlind, Perry; [...]
Erschienen: American Astronomical Society, 2020
Erschienen in: The Astronomical Journal
Sprache: Nicht zu entscheiden
DOI: 10.3847/1538-3881/aba49d
ISSN: 0004-6256; 1538-3881
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Beschreibung: <jats:title>Abstract</jats:title> <jats:p>We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${1.463}_{-0.096}^{+0.10}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="ajaba49dieqn1.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>M</jats:italic> <jats:sub>J</jats:sub> and a radius of <jats:inline-formula> <jats:tex-math> <?CDATA ${1.02}_{-0.29}^{+0.71}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="ajaba49dieqn2.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>R</jats:italic> <jats:sub>J</jats:sub>. Also a classical hot Jupiter, TOI 905 b has a mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${0.667}_{-0.041}^{+0.042}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="ajaba49dieqn3.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>M</jats:italic> <jats:sub>J</jats:sub> and radius of <jats:inline-formula> <jats:tex-math> <?CDATA ${1.171}_{-0.051}^{+0.053}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="ajaba49dieqn4.gif" xlink:type="simple" /> </jats:inline-formula> <jats:italic>R</jats:italic> <jats:sub>J</jats:sub>. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with <jats:italic>V</jats:italic> ∼ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of <jats:inline-formula> <jats:tex-math> <?CDATA ${0.994}_{-0.049}^{+0.083}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="ajaba49dieqn5.gif" xlink:type="simple" /> </jats:inline-formula>, making it one of only ∼20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.</jats:p>
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