Browsing by Author "Tala Pinto, Marcelo"

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    A long-period transiting substellar companion in the super-Jupiters to brown dwarfs mass regime and a prototypical warm-Jupiter detected by TESS
    (2024) Jones, Matias I.; Reinarz, Yared; Brahm, Rafael; Tala Pinto, Marcelo; Eberhardt, Jan; Rojas, Felipe; Triaud, Amaury H. M. J.; Gupta, Arvind F.; Ziegler, Carl; Hobson, Melissa J.; Jordan, Andres; Henning, Thomas; Trifonov, Trifon; Schlecker, Martin; Espinoza, Nestor; Torres-Miranda, Pascal; Sarkis, Paula; Ulmer-Moll, Solene; Lendl, Monika; Uzundag, Murat; Moyano, Maximiliano; Hesse, Katharine; Caldwell, Douglas A.; Shporer, Avi; Lund, Michael B.; Jenkins, Jon M.; Seager, Sara; Winn, Joshua N.; Ricker, George R.; Burke, Christopher J.; Figueira, Pedro; Psaridi, Angelica; Al Moulla, Khaled; Mounzer, Dany; Standing, Matthew R.; Martin, David V.; Dransfield, Georgina; Baycroft, Thomas; Dragomir, Diana; Boyle, Gavin; Suc, Vincent; Mann, Andrew W.; Timmermans, Mathilde; Ducrot, Elsa; Hooton, Matthew J.; Zuniga-Fernandez, Sebastian; Sebastian, Daniel; Gillon, Michael; Queloz, Didier; Carson, Joe; Lissauer, Jack J.
    We report on the confirmation and follow-up characterization of two long-period transiting substellar companions on low-eccentricity orbits around TIC 4672985 and TOI-2529, whose transit events were detected by the TESS space mission. Ground-based photometric and spectroscopic follow-up from different facilities, confirmed the substellar nature of TIC 4672985 b, a massive gas giant in the transition between the super-Jupiters and brown dwarfs mass regime. From the joint analysis we derived the following orbital parameters: P = 69.0480(-0.0005)(+0.0004) d, M-p = 12.74(-1.01)(+1.01) M-J, R-p = 1.026(-0.067)(+0.065) R-J and e = 0.018(-0.004)(+0.004). In addition, the RV time series revealed a significant trend at the similar to 350 m s(-1) yr(-1) level, which is indicative of the presence of a massive outer companion in the system. TIC 4672985 b is a unique example of a transiting substellar companion with a mass above the deuterium-burning limit, located beyond 0.1 AU and in a nearly circular orbit. These planetary properties are difficult to reproduce from canonical planet formation and evolution models. For TOI-2529 b, we obtained the following orbital parameters: P = 64.5949(-0.0003)(+0.0003) d, M-p = 2.340(-0.195)(+0.197) M-J, R-p = 1.030(-0.050)(+0.050) R-J and e = 0.021(-0.015)(+0.024), making this object a new example of a growing population of transiting warm giant planets.
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    Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b
    (2024) Carleo, Ilaria; Barragan, Oscar; Persson, Carina M.; Fridlund, Malcolm; Lam, Kristine W. F.; Messina, Sergio; Gandolfi, Davide; Smith, Alexis M. S.; Johnson, Marshall C.; Cochran, William; Osborne, Hannah L. M.; Brahm, Rafael; Ciardi, David R.; Collins, Karen A.; Everett, Mark E.; Giacalone, Steven; Guenther, Eike W.; Hatzes, Artie; Hellier, Coel; Horner, Jonathan; Kabath, Petr; Korth, Judith; MacQueen, Phillip; Masseron, Thomas; Murgas, Felipe; Nowak, Grzegorz; Rodriguez, Joseph E.; Watkins, Cristilyn N.; Wittenmyer, Rob; Zhou, George; Ziegler, Carl; Bieryla, Allyson; Boyd, Patricia T.; Clark, Catherine A.; Dressing, Courtney D.; Eastman, Jason D.; Eberhardt, Jan; Endl, Michael; Espinoza, Nestor; Fausnaugh, Michael; Guerrero, Natalia M.; Henning, Thomas; Hesse, Katharine; Hobson, Melissa J.; Howell, Steve B.; Jordan, Andres; Latham, David W.; Lund, Michael B.; Mireles, Ismael; Narita, Norio; Tala Pinto, Marcelo; Pugh, Teznie; Quinn, Samuel N.; Ricker, George; Rodriguez, David R.; Rojas, Felipe I.; Rose, Mark E.; Rudat, Alexander; Sarkis, Paula; Savel, Arjun B.; Schlecker, Martin; Schwarz, Richard P.; Seager, Sara; Shporer, Avi; Smith, Jeffrey C.; Stassun, Keivan G.; Stockdale, Chris; Trifonov, Trifon; Vanderspek, Roland; Winn, Joshua N.; Wright, Duncan
    Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of P-b=5.8 days, a mass of M-b=0.9 M-J, and a radius of R-b=1.3 R-J, with a planetary density of 0.477 g cm(-3). TOI-2485 b has an orbital period of P-b=11.2 days, a mass of M-b=2.4 M-J, and a radius of R-b=1.1 R-J with a density of 2.36 g cm(-3). Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario.