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Dr. Rabus, Markus
Research Outputs
TOI-1842b: A Transiting Warm Saturn Undergoing Reinflation around an Evolving Subgiant
2022, Wittenmyer, Robert, Clark, Jake, Trifonov, Trifon, Addison, Brett, Wright, Duncan, Stassun, Keivan, Horner, Jonathan, Lowson, Nataliea, Kielkopf, John, Kane, Stephen, Plavchan, Peter, Shporer, Avi, Zhang, Hui, Bowler, Brendan, Mengel, Matthew, Okumura, Jack, Rabus, Markus, Johnson, Marshall, Harbeck, Daniel, Tronsgaard, René, Buchhave, Lars, Collins, Karen, Collins, Kevin, Gan, Tianjun, Jensen, Eric, Howell, Steve, Furlan, E., Gnilka, Crystal, Lester, Kathryn, Matson, Rachel, Scott, Nicholas, Ricker, George, Vanderspek, Roland, Latham, David, Seager, S., Winn, Joshua, Jenkins, Jon, Rudat, Alexander, Quintana, Elisa, Rodriguez, David, Caldwell, Douglas, Quinn, Samuel, Essack, Zahra, Bouma, Luke
The imminent launch of space telescopes designed to probe the atmospheres of exoplanets has prompted new efforts to prioritize the thousands of transiting planet candidates for follow-up characterization. We report the detection and confirmation of TOI-1842b, a warm Saturn identified by TESS and confirmed with ground-based observations from Minerva-Australis, NRES, and the Las Cumbres Observatory Global Telescope. This planet has a radius of R J, a mass of M J, an orbital period of days, and an extremely low density (? = 0.252 0.091 g cm-3). TOI-1842b has among the best known combinations of large atmospheric scale height (893 km) and host-star brightness (J = 8.747 mag), making it an attractive target for atmospheric characterization. As the host star is beginning to evolve off the main sequence, TOI-1842b presents an excellent opportunity to test models of gas giant reinflation. The primary transit duration of only 4.3 hr also makes TOI-1842b an easily-schedulable target for further ground-based atmospheric characterization. © 2022. The American Astronomical Society. All rights reserved.
TOI-1431b/MASCARA-5b: A highly irradiated Ultrahot Jupiter orbiting one of the hottest and brightest known exoplanet host stars
2021, Dr. Rabus, Markus, Addison, Brett, Knudstrup, Emil, Wong, Ian, Hébrard, Guillaume, Dorval, Patrick, Snellen, Ignas, Albrecht, Simon, Bello-Arufe, Aaron, Almenara, Jose-Manuel, Boisse, Isabelle, Bonfils, Xavier, Dalal, Shweta, Demangeon, Olivier, Hoyer, Sergio, Kiefer, Flavien, Santos, N. C., Nowak, Grzegorz, Luque, Rafael, Stangret, Monika, Palle, Enric, Tronsgaard, René, Antoci, Victoria, Buchhave, Lars A., Günther, Maximilian N., Daylan, Tansu, Murgas, Felipe, Parviainen, Hannu, Esparza-Borges, Emma, Crouzet, Nicolas, Narita, Norio, Fukui, Akihiko, Kawauchi, Kiyoe, Watanabe, Noriharu, Johnson, Marshall, Otten, Gilles, Jan-Talens, Geert, Cabot, Samuel, Fischer, Debra, Grundahl, Frank, Fredslun-Andersen, Mads, Jessen-Hansen, Jens, Pallé, Pere, Shporer, Avi, Ciardi, David, Clark, Jake, Wittenmyer, Robert, Wright, Duncan, Horner, Jonathan, Collins, Karen, Jensen, Eric, Kielkopf, John, Schwarz, Richard, Srdoc, Gregor, Yilmaz, Mesut, Senavci, Hakan, Diamond, Brendan, Harbeck, Daniel, Komacek, Thaddeus, Smith, Jeffrey, Wang, Songhu, Eastman, Jason, Stassun, Keivan, Latham, David, Vanderspek, Roland, Seager, Sara, Winn, Joshua, Jenkins, Jon, Louie, Dana, Bouma, Luke, Twicken, Joseph, Levine, Alan, McLean, Brian
We present the discovery of a highly irradiated and moderately inflated ultrahot Jupiter, TOI-1431b/MASCARA5 b (HD 201033b), first detected by NASA’s Transiting Exoplanet Survey Satellite mission (TESS) and the Multisite 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 Mp = 3.12 ± 0.18 MJ (990 ± 60 M⊕), an inflated radius of Rp = 1.49 ± 0.05 RJ (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 ( -+ 0.29 0.19 0.32 Gyr) Am type star with = -+ Teff 7690 250 400 K, resulting in a highly irradiated planet with an incident flux of á ñ= ´ - + F 7.24 0.64 0.68 109 erg s−1 cm−2 ( - + 5300 470 SÅ 500 ) and an equilibrium temperature of Teq = 2370 ± 70 K. TESS photometry also reveals a secondary eclipse with a depth of - + 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 Tday = 3004 ± 64 K and Tnight = 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.