Dr. Astudillo-Defru, Nicola

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Nombre de publicación
Dr. Astudillo-Defru, Nicola
Nombre completo
Astudillo Defru, Nicola
Facultad
Email
nastudillo@ucsc.cl
ORCID

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20202
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Research Outputs

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  • No Thumbnail Available
    Publication
    Optical phase curve of the ultra-hot Jupiter WASP-121b
    (EDP Sciences, 2020)
    Bourrier, V.
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    Kitzmann, D.
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    Kuntzer, T.
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    Nascimbeni, V.
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    Lendl, M.
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    Lavie, B.
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    Hoeijmakers, H. J.
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    Pino, L.
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    Ehrenreich, D.
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    Heng, K.
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    Allart, R.
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    Cegla, H. M.
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    Dumusque, X.
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    Melo, C.
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    Astudillo-Defru, Nicola 
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    Caldwell, Douglas A.
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    Cretignier, M.
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    Giles, H.
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    Henze, C. E.
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    Jenkins, J.
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    Lovis, C.
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    Murgas, F.
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    Pepe, F.
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    Ricker, G. R.
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    Rose, M. E.
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    Seager, S.
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    Segransan, D.
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    Suárez-Mascareño, A.
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    Udry, S.
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    Vanderspek, R.
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    Wyttenbach, A.
    We present the analysis of TESS optical photometry of WASP-121b, which reveals the phase curve of this transiting ultra-hot Jupiter. Its hotspot is located at the sub-stellar point, showing inefficient heat transport from the dayside (2870 ± 50 K) to the nightside (<2500 K at 3σ) at the altitudes probed by TESS. The TESS eclipse depth, measured at the shortest wavelength to date for WASP-121b, confirms the strong deviation from blackbody planetary emission. Our atmospheric retrieval on the complete emission spectrum supports the presence of a temperature inversion, which can be explained by the presence of VO and possibly TiO and FeH. The strong planetary emission at short wavelengths could arise from an H− continuum.
  • No Thumbnail Available
    Publication
    A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS
    (EDP Sciences, 2020)
    Astudillo-Defru, Nicola 
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    Cloutier, Ryan
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    Wang, S. X.
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    Teske, J.
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    Brahm, R.
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    Hellier, C.
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    Ricker, G.
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    Vanderspek, R.
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    Latham, D.
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    Seager, S.
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    Winn, J. N.
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    Jenkins, J. M.
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    Collins, Karen A.
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    Stassun, K. G.
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    Ziegler, C.
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    Almenara, José Manuel
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    Anderson, David R.
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    Artigau, Étienne
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    Bonfils, X.
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    Bouchy, F.
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    Briceño, C.
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    Butler, R. P.
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    Charbonneau, D.
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    Conti, Dennis M.
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    Crane, J.
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    Crossfield, Ian J. M.
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    Davies, M.
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    Delfosse, X.
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    Díaz, R. F.
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    Doyon, R.
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    Dragomir, D.
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    Eastman, J. D.
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    Espinoza, N.
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    Essack, Z.
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    Feng, F.
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    Figueira, P.
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    Forveille, T.
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    Gan, T.
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    Glidden, A.
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    Guerrero, N.
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    Hart, R.
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    Henning, Th.
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    Horch, E. P.
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    Isopi, G.
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    Jenkins, J. S.
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    Jordán, A.
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    Kielkopf, J. F.
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    Law, N.
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    Lovis, C.
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    Mallia, F.
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    Mann, A. W.
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    De Medeiros, J. R.
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    Melo, C.
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    Mennickent, R. E.
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    Mignon, L.
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    Murgas. F.
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    Nusdeo, D. A.
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    Pepe, F.
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    Relles, H. M.
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    Rose, M.
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    Santos, N. C.
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    Ségransan, D.
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    Shectman, S.
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    Shporer, A.
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    Smith, J. C.
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    Torres, P.
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    Udry, S.
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    Villaseñor, J.
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    Winters, J. G.
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    Zhou, G.
    We report the detection of a transiting super-Earth-sized planet (R = 1.39 ± 0.09 R⊕) in a 1.4-day orbit around L 168-9 (TOI-134), a bright M1V dwarf (V = 11, K = 7.1) located at 25.15 ± 0.02 pc. The host star was observed in the first sector of the Transiting Exoplanet Survey Satellite (TESS) mission. For confirmation and planet mass measurement purposes, this was followed up with ground-based photometry, seeing-limited and high-resolution imaging, and precise radial velocity (PRV) observations using the HARPS and Magellan/PFS spectrographs. By combining the TESS data and PRV observations, we find the mass of L 168-9 b to be 4.60 ± 0.56 M⊕ and thus the bulk density to be 1.74−0.33+0.44 times higher than that of the Earth. The orbital eccentricity is smaller than 0.21 (95% confidence). This planet is a level one candidate for the TESS mission’s scientific objective of measuring the masses of 50 small planets, and it is one of the most observationally accessible terrestrial planets for future atmospheric characterization.