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TOI-1431b/MASCARA-5b: A Highly Irradiated Ultrahot Jupiter Orbiting One of the Hottest and Brightest Known Exoplanet Host Stars

2021; Institute of Physics; Volume: 162; Issue: 6 Linguagem: Inglês

10.3847/1538-3881/ac224e

1538-3881

Brett C. Addison, Emil Knudstrup, Ian Wong, G. Hébrard, Patrick Dorval, I. A. G. Snellen, Simon Albrecht, Aaron Bello-Arufe, José-Manuel Almenara, I. Boisse, X. Bonfıls, S. Dalal, O. D. S. Demangeon, S. Hoyer, F. Kiefer, N. C. Santos, G. Nowak, R. Luque, M. Stangret, Ε. Πάλλη, R. Tronsgaard, V. Antoci, Lars A. Buchhave, Maximilian N. Günther, Tansu Daylan, F. Murgas, H. Parviainen, E. Esparza-Borges, Nicolas Crouzet, Norio Narita, Akihiko Fukui, Kiyoe Kawauchi, Noriharu Watanabe, M. Rabus, Marshall C. Johnson, G. P. P. L. Otten, G. J. J. Talens, Samuel H. C. Cabot, Debra A. Fischer, F. Grundahl, M. F. Andersen, J. Jessen-Hansen, P. L. Pallé, Avi Shporer, David R. Ciardi, Jake T. Clark, Robert A. Wittenmyer, D. J. Wright, Jonathan Horner, Karen A. Collins, Eric L. N. Jensen, John F. Kielkopf, Richard P. Schwarz, Gregor Srdoč, M. Yılmaz, H. V. Şenavcı, B. Diamond, Daniel Harbeck, Thaddeus D. Komacek, Jeffrey C. Smith, Songhu Wang, Jason D. Eastman, Keivan G. Stassun, David W. Latham, R. Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Dana R. Louie, Luke G. Bouma, Joseph D. Twicken, Alan M. Levine, B. McLean,

Astro and Planetary Science

Abstract We present the discovery of a highly irradiated and moderately inflated ultrahot Jupiter, TOI-1431b/MASCARA-5 b (HD 201033b), first detected by NASA’s Transiting Exoplanet Survey Satellite mission (TESS) and the Multi-site All-Sky Camera (MASCARA). The signal was established to be of planetary origin through radial velocity measurements obtained using SONG, SOPHIE, FIES, NRES, and EXPRES, which show a reflex motion of K = 294.1 ± 1.1 m s −1 . A joint analysis of the TESS and ground-based photometry and radial velocity measurements reveals that TOI-1431b has a mass of M p = 3.12 ± 0.18 M J (990 ± 60 M ⊕ ), an inflated radius of R p = 1.49 ± 0.05 R J (16.7 ± 0.6 R ⊕ ), and an orbital period of P = 2.650237 ± 0.000003 days. Analysis of the spectral energy distribution of the host star reveals that the planet orbits a bright ( V = 8.049 mag) and young ( <?CDATA ${0.29}_{-0.19}^{+0.32}$?> 0.29 − 0.19 + 0.32 Gyr) Am type star with <?CDATA ${T}_{\mathrm{eff}}={7690}_{-250}^{+400}$?> T eff = 7690 − 250 + 400 K, resulting in a highly irradiated planet with an incident flux of <?CDATA $\langle F\rangle ={7.24}_{-0.64}^{+0.68}\times $?> 〈 F 〉 = 7.24 − 0.64 + 0.68 × 10 9 erg s −1 cm −2 ( <?CDATA ${5300}_{-470}^{+500}\,{S}_{\oplus }$?> 5300 − 470 + 500 S ⊕ ) and an equilibrium temperature of T eq = 2370 ± 70 K. TESS photometry also reveals a secondary eclipse with a depth of <?CDATA ${127}_{-5}^{+4}$?> 127 − 5 + 4 ppm as well as the full phase curve of the planet’s thermal emission in the red-optical. This has allowed us to measure the dayside and nightside temperature of its atmosphere as T day = 3004 ± 64 K and T night = 2583 ± 63 K, the second hottest measured nightside temperature. The planet’s low day/night temperature contrast (∼420 K) suggests very efficient heat transport between the dayside and nightside hemispheres. Given the host star brightness and estimated secondary eclipse depth of ∼1000 ppm in the K band, the secondary eclipse is potentially detectable at near-IR wavelengths with ground-based facilities, and the planet is ideal for intensive atmospheric characterization through transmission and emission spectroscopy from space missions such as the James Webb Space Telescope and the Atmospheric Remote-sensing Infrared Exoplanet Large-survey.