Browsing by Author "Brahm, Rafael"

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    Author correction: An ultrahot Neptune in the Neptune desert
    (2020) Jenkins, James S.; Díaz, Matías R.; Kurtovic, Nicolás T.; Espinoza, Néstor; Vines, Jose I.; Peña Rojas, Pablo A.; Brahm, Rafael; Torres, Pascal; Cortés Zuleta, Pía ; Soto, Maritza G.; López, Eric D.; King, George W.; Wheatley, Peter J.; Winn, Joshua N.; Ciardi, David R.; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Jenkins, Jon M.; Beichman, Charles A.; Bieryla, Allyson; Burke, Christopher J.; Christiansen , Jessie L.; Henze, Christopher E.; Klaus, Todd C.; McCaulif, Sean; Mori, Mayuko; Narita, Norio; Nishiumi, Taku; Tamura, Motohide; Pitogo de Leon, Jerome; Quinn, Samuel N.; Villaseñor, Jesus Noel; Vezie, Michael; Lissauer, Jack J.; Collins, Karen A.; Collins, Kevin I.; Isopi, Giovanni; Mallia, Franco; Ercolino, Andrea; Petrovich, Cristobal; Jordán, Andrés; Acton, Jack S.; Armstrong, David J.; Bayliss, Daniel; Bouchy, François; Belardi, Claudia; Bryant, Edward M.; Burleigh, Matthew R.; Cabrera, Juan; Casewell, Sarah L.; Chaushev, Alexander; Cooke, Benjamin F.; Eigmüller, Philipp; Erikson, Anders; Foxell, Emma; Gänsicke, Boris T.; Gill, Samuel; Gillen, Edward; Günther, Maximilian N.; Goad, Michael R.; Hooton, Matthew J.; Jackman, James A. G.; Louden, Tom; McCormac, James; Moyano, Maximiliano; Nielsen, Louise D.; Pollacco, Don; Queloz, Didier; Rauer, Heike; Raynard, Liam; Smith, Alexis M. S.; Tilbrook, Rosanna H.; Titz Weider, Ruth; Turner, Oliver; Udry, Stéphane; Walker, Simon R.; Watson, Christopher A.; West, Richard G.; Palle, Enric; Ziegler, Carl; Law, Nicholas; Mann, Andrew W.
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    Early optical spectra of nova V1369 Cen show the presence of lithium
    (2015) Izzo, Luca; Della Valle, Massimo; Mason, Elena; Matteucci, F.; Romano, Donatella; Pasquini, Luca; Vanzi, Leonardo; Jordán Colzani, Andrés Cristóbal; Fernandez, José Miguel; Bluhm, Paz; Brahm, Rafael; Espinoza, Nestor; Williams, Robert
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    Hats-3b: An inflated hot jupiter transiting an F-type star*
    (2013) Bayliss, D.; Zhou, Guangyuan; Penev, Kaloyan; Bakos, G. Á.; Hartman, J. D.; Jordán Colzani, Andrés Cristóbal; Mancini, Luigi; Mohler-Fischer, Maren; Suc, Vincent; Rabus, Markus; Béky, Bence; Csubry, Zoltan; Buchhave, L.; Henning, T.; Nikolov, Nikolay; Csák, B.; Brahm, Rafael; Espinoza Pérez, Néstor
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    Resolving the planetesimal belt of HR 8799 with ALMA
    (2016) Haworth-Booth, Mark; Jordán Colzani, Andrés Cristóbal; Casassus, Simon; Hales, Antonio S.; Dent, William R. F.; Faramaz, Virginie; Matrà, Luca; Barkats, Denis; Brahm, Rafael; Cuadra Stipetich, Jorge Rodrigo
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    The Aligned Orbit of the Eccentric Proto Hot Jupiter TOI-3362b
    (2023) Espinoza Retamal, Juan; Brahm, Rafael; Petrovich, Cristobal; Jordán, Andrés; Stefánsson, Guðmundur; Sedaghati, Elyar; Hobson, Melissa J.; Muñoz, Diego J.; Boyle, Gavin; Leiva, Rodrigo; Suc, Vincent
    High-eccentricity tidal migration predicts the existence of highly eccentric proto-hot Jupiters on the "tidal circularization track," meaning that they might eventually become hot Jupiters, but that their migratory journey remains incomplete. Having experienced moderate amounts of the tidal reprocessing of their orbital elements, proto-hot Jupiters systems can be powerful test-beds for the underlying mechanisms of eccentricity growth. Notably, they may be used for discriminating between variants of high-eccentricity migration, each predicting a distinct evolution of misalignment between the star and the planet's orbit. We constrain the spin-orbit misalignment of the proto-hot Jupiter TOI-3362b with high-precision radial velocity observations using ESPRESSO at VLT. The observations reveal a sky-projected obliquity $\lambda = 1.2_{-2.7}^{+2.8}$ deg and constrain the orbital eccentricity to $e=0.720 \pm 0.016$, making it one of the most eccentric gas giants for which the obliquity has been measured. The large eccentricity and the striking orbit alignment of the planet suggest that ongoing coplanar high-eccentricity migration driven by a distant companion is a likely explanation for the system's architecture. This distant companion would need to reside beyond 5 au at 95% confidence to be compatible with the available radial velocity observations....