Exoplanetas y Astrobiología

    General
    Descripción

    La búsqueda de vida en el Universo se ha visto impulsada por los recientes descubrimientos de planetas alrededor de otras estrellas (los llamados exoplanetas), convirtiéndose en uno de los campos más activos dentro de la Astrofísica moderna. En los últimos años los descubrimientos cada vez más numerosos de nuevos exoplanetas y los últimos avances en el estudio de sus atmósferas no sólo están dándonos valiosa nueva información sobre sus propiedades físicas, sino que nos están permitiendo además poner las propiedades de los planetas de nuestro Sistema Solar dentro un contexto más global. El campo esta acercándose al importante descubrimiento de los primeros planetas potencialmente habitables, impulsando estudios más detallados de estos planetas. Con el lanzamiento de las nuevas misiones como JWST, CHEOPS, TESS, ARIEL o PLATO, al campo de exoplanetas se le plantea un futuro muy excitante.

    Es por esta razon que este campo se ayuda de y, a su vez motiva, el desarrollo de instrumentación cada vez más sensible y estable tanto para telescopios de tierra como para las misiones espaciales. Dos frentes para los que nuestro grupo esta especialmente preparado. Por un lado, durante los ultimos años hemos desarrollado tecnicas de observacion y reduccion de transitos de exoplanetas para los telescopios del ORM, siendo el nuestro uno de los grupos mas productivos en la explotacion de GTC. Por otro lado, todas las misiones espaciales ESA (presentes y futuras) relacionadas con exoplanetas cuentan con uno o varios de los componentes del proyecto como CoIs.

    En el marco de este proyecto, pretendemos que los investigadores del IAC mantengan una situación aventajada con la explotación de OSIRIS y EMIR, instrumentos de primera luz de GTC, y participen en la construcción, comisionado y operación de nuevos instrumentos, como el espectrografo óptico de alta resolución HORUS en el GTC. La explotacion de la fotometria y espectroscopia de transitos con LIRIS en el WHT es tambien uno de nuestros principales intereses, especialmente en preparacion de la instalacion en 2015 del instrumento EMIR en el GTC.

    En resumen, el proyecto "Exoplanetas y Astrobiologia" se centrará entorno a estas cuatro lineas principales de actuacion:

    1) Caracterización de las propiedades fisicas y atmosfericas de exoplanetas (GTC, WHT, HARPSN, CARMENES, ESPRESSO, ARIEL etc.)

    2) Búsquedas y confirmacion de exoplanetas por transitos (CoRoT, Kepler, K2, CHEOPS, XO, LCOGT, WFC, PLATO, etc.)

    3) Busquedas/ confirmacion de exoplanetas por velocidad radial (HARPSN, HORUS, LCOGT, SONG, CARMENES)

    4) Astrobiología

    Investigador principal
    Personal del proyecto
    1. Deteccion de He en la atmosfera de un exoplaneta por primera vez, publicado en Science.
    2. Deteccion de un planeta entorno a la estrella de Barnard, publicado en Nature
    3. Deteccion de los primeros planetas del la mision TESS, con varios articulos de impacto
    4. Descubrimiento de rasgos de Na y Halpha en el espectro de KELT-20b con el TNG
    5. Publicación del Handbook of Exoplanets, la obra de referencia más extenso en el campo de los exoplanetas. Este Manual fue editado por miembros de nuestro grupo e incluye contribuciones de unos 300 expertos en todo el mundo, incluidos 12 miembros de IAC.

    Publicaciones relacionadas

    • A Radial Velocity Study of the Planetary System of π Mensae: Improved Planet Parameters for π Mensae c and a Third Planet on a 125 Day Orbit
      π Men hosts a transiting planet detected by the Transiting Exoplanet Survey Satellite space mission and an outer planet in a 5.7 yr orbit discovered by radial velocity (RV) surveys. We studied this system using new RV measurements taken with the HARPS spectrograph on ESO's 3.6 m telescope, as well as archival data. We constrain the stellar RV
      Hatzes, Artie P. et al.

      Fecha de publicación:

      5
      2022
      Número de citas
      12
    • Radio emission in a nearby, ultra-cool dwarf binary: A multifrequency study
      Context. The substellar triple system VHS J125601.92−125723.9 (hereafter VHS 1256−1257) is composed of an equal-mass M7.5 brown dwarf binary and an L7 low-mass substellar object. In Guirado et al. (2018, A&A, 610, A23) we published the detection of radio emission at 8.4 GHz coming from the central binary and making it an excellent target for
      Climent, J. B. et al.

      Fecha de publicación:

      4
      2022
      Número de citas
      7
    • A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
      Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting
      Christian, Sam et al.

      Fecha de publicación:

      5
      2022
      Número de citas
      26
    • CaRM: Exploring the chromatic Rossiter-McLaughlin effect. The cases of HD 189733b and WASP-127b
      Aims: In this paper we introduce CaRM, a semi-automatic code for the retrieval of broadband transmission spectra of transiting planets through the chromatic Rossiter-McLaughlin method. We applied it to HARPS and ESPRESSO observations of two exoplanets to retrieve the transmission spectrum and we analyze its fitting transmission models. Methods: We
      Cristo, E. et al.

      Fecha de publicación:

      4
      2022
      Número de citas
      5
    • Investigation of the upper atmosphere in ultra-hot Jupiter WASP-76 b with high-resolution spectroscopy
      Alkali metal lines are one of the most important key opacity sources for understanding exoplanetary atmospheres because the Na I resonance doublets are thought to be the cause of low albedo, as the alkali metal's wide line wings absorb almost all of the incoming stellar irradiation. High-resolution transmission spectroscopy of Na absorption lines
      Kawauchi, Kiyoe et al.

      Fecha de publicación:

      4
      2022
      Número de citas
      9
    • Nodal precession of WASP-33b for 11 yr by Doppler tomographic and transit photometric observations
      WASP-33b, a hot Jupiter around a hot star, is a rare system in which nodal precession has been discovered. We updated the model for the nodal precession of WASP-33b by adding new observational points. Consequently, we found a motion of the nodal precession spanning 11 yr. We present homogenous Doppler tomographic analyses of eight data sets
      Watanabe, Noriharu et al.

      Fecha de publicación:

      5
      2022
      Número de citas
      10
    • Black Mirror: The impact of rotational broadening on the search for reflected light from 51 Pegasi b with high resolution spectroscopy
      Context. The extreme contrast ratios between stars and their planets at optical wavelengths make it challenging to isolate the light reflected by exoplanet atmospheres. Yet, these reflective properties reveal key processes occurring in the atmospheres, and they also span wavelengths that include the potential O 2 biosignature. High resolution cross
      Spring, E. F. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      16
    • A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds
      LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M ⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using Transiting
      Winters, Jennifer G. et al.

      Fecha de publicación:

      4
      2022
      Número de citas
      34
    • Moderately misaligned orbit of the warm sub-Saturn HD 332231 b
      Measurements of exoplanetary orbital obliquity angles for different classes of planets are an essential tool in testing various planet formation theories. Measurements for those transiting planets on relatively large orbital periods (P > 10 d) present a rather difficult observational challenge. Here we present the obliquity measurement for the warm
      Sedaghati, E. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      5
    • Transit timing variations of AU Microscopii b and c
      Here we report large-amplitude transit timing variations (TTVs) for AU Microcopii b and c as detected in combined TESS (2018, 2020) and CHEOPS (2020, 2021) transit observations. AU Mic is a young planetary system with a debris disk and two transiting warm Neptunes. A TTV on the order of several minutes was previously reported for AU Mic b, which
      Szabó, Gy. M. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      11
    • The atmosphere and architecture of WASP-189 b probed by its CHEOPS phase curve
      Context. Gas giants orbiting close to hot and massive early-type stars can reach dayside temperatures that are comparable to those of the coldest stars. These `ultra-hot Jupiters' have atmospheres made of ions and atomic species from molecular dissociation and feature strong day-to-night temperature gradients. Photometric observations at different
      Deline, A. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      40
    • A tentative detection of He I in the atmosphere of GJ 1214 b
      The He I λ10833 Å triplet is a powerful tool for characterising the upper atmosphere of exoplanets and tracing possible mass loss. Here, we analysed one transit of GJ 1214 b observed with the CARMENES high-resolution spectrograph to study its atmosphere via transmission spectroscopy around the He I triplet. Although previous studies using lower
      Orell-Miquel, J. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      43
    • Metallicities in M dwarfs: Investigating different determination techniques
      Deriving metallicities for solar-like stars follows well-established methods, but for cooler stars such as M dwarfs, the determination is much more complicated due to forests of molecular lines that are present. Several methods have been developed in recent years to determine accurate stellar parameters for these cool stars (T eff ≲ 4000 K)
      Passegger, V. M. et al.

      Fecha de publicación:

      2
      2022
      Número de citas
      29
    • CHEOPS geometric albedo of the hot Jupiter HD 209458 b
      We report the detection of the secondary eclipse of the hot Jupiter HD 209458 b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4 −3.3 +3.2 parts per million translates into a geometric albedo of A g = 0.096 ± 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo
      Brandeker, A. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      22
    • Detection of iron emission lines and a temperature inversion on the dayside of the ultra-hot Jupiter KELT-20b
      Ultra-hot Jupiters (UHJs) are gas giants with very high equilibrium temperatures. In recent years, multiple chemical species, including various atoms and ions, have been discovered in their atmospheres. Most of these observations have been performed with transmission spectroscopy, although UHJs are also ideal targets for emission spectroscopy due
      Yan, F. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      25
    • HD 207897 b: A dense sub-Neptune transiting a nearby and bright K-type star
      We present the discovery and characterization of a transiting sub-Neptune that orbits the nearby (28 pc) and bright (V = 8.37) K0V star HD 207897 (TOI-1611) with a 16.20-day period. This discovery is based on photometric measurements from the Transiting Exoplanet Survey Satellite mission and radial velocity (RV) observations from the SOPHIE
      Heidari, N. et al.

      Fecha de publicación:

      2
      2022
      Número de citas
      11
    • Discovery and mass measurement of the hot, transiting, Earth-sized planet, GJ 3929 b
      We report the discovery of GJ 3929 b, a hot Earth-sized planet orbiting the nearby M3.5 V dwarf star, GJ 3929 (G 180-18, TOI-2013). Joint modelling of photometric observations from TESS sectors 24 and 25 together with 73 spectroscopic observations from CARMENES and follow-up transit observations from SAINT-EX, LCOGT, and OSN yields a planet radius
      Kemmer, J. et al.

      Fecha de publicación:

      3
      2022
      Número de citas
      11
    • Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
      We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R ⊕, M = 2.0 M ⊕), c (P = 10.78 d, R =
      Lacedelli, G. et al.

      Fecha de publicación:

      4
      2022
      Número de citas
      28
    • NEID Rossiter-McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star
      Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other
      Dong, Jiayin et al.

      Fecha de publicación:

      2
      2022
      Número de citas
      13
    • A multi-planetary system orbiting the early-M dwarf TOI-1238
      Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an
      González-Álvarez, E. et al.

      Fecha de publicación:

      2
      2022
      Número de citas
      9

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