Dr. Astudillo-Defru, Nicola

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Dr. Astudillo-Defru, Nicola
Nombre completo
Astudillo Defru, Nicola
Facultad
Email
nastudillo@ucsc.cl
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20202
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Author: Anderson, David R. × Has files: false ×

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  • 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.
  • No Thumbnail Available
    Publication
    GJ 1252 b: A 1.2 R⊕ Planet Transiting an M3 Dwarf at 20.4 pc
    (IOP, 2020)
    Shporer, Avi
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    Collins, Karen A.
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    Astudillo-Defru, Nicola 
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    Irwin, Jonathan
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    Bonfils, Xavier
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    Collins, Kevin I.
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    Matthews, Elisabeth
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    Winters, Jennifer G.
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    Anderson, David R.
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    Armstrong, James D.
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    Charbonneau, David
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    Cloutier, Ryan
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    Daylan, Tansu
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    Gan, Tianjun
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    Günther, Maximilian N.
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    Hellier, Coel
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    Horne, Keith
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    Huang, Chelsea X.
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    Jensen, Eric L. N.
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    Kielkopf, John
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    Palle, Enric
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    Sefako, Ramotholo
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    Stassun, Keivan G.
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    Tan, Thiam-Guan
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    Vanderburg, Andrew
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    Ricker, George R.
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    Latham, David W.
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    Vanderspek, Roland
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    Seager, Sara
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    Winn, Joshua N.
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    Jenkins, Jon M.
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    Colon, Knicole
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    Dressing, Courtney D.
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    Léepine, Sébastien
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    Muirhead, Philip S.
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    Rose, Mark E.
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    Twicken, Joseph D.
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    Villaseñor, Jesús Noel
    We report the discovery of GJ 1252 b, a planet with a radius of 1.193 ± 0.074 ${R}_{\oplus }$ and an orbital period of 0.52 days around an M3-type star (0.381 ± 0.019 ${M}_{\odot }$, 0.391 ± 0.020 ${R}_{\odot }$) located 20.385 ± 0.019 pc away. We use Transiting Exoplanet Survey Satellite (TESS) data, ground-based photometry and spectroscopy, Gaia astrometry, and high angular resolution imaging to show that the transit signal seen in the TESS data must originate from a transiting planet. We do so by ruling out all false-positive scenarios that attempt to explain the transit signal as originating from an eclipsing stellar binary. Precise Doppler monitoring also leads to a tentative mass measurement of 2.09 ± 0.56 M⊕. The host star proximity, brightness (V = 12.19 mag, K = 7.92 mag), low stellar activity, and the system's short orbital period make this planet an attractive target for detailed characterization, including precise mass measurement, looking for other objects in the system, and planet atmosphere characterization.