A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Morales, J. C.; Mustill, Alexander J.; Ribas, I.; Davies, Melvyn B.; Reiners, A.; Bauer, F. F.; Kossakowski, D.; Herrero, E.; Rodrı́guez, E.; López-González, M. J.; Rodríguez‐López, C.; Béjar, V. J. S.; González-Cuesta, L.; Luque, R.; Πάλλη, Ε.; Perger, M.; Baroch, D.; Johansen, Anders; Klahr, Hubert; Mordasini, Christoph; Anglada-Escudé, G.; Caballero, J. A.; Cortés-Contreras, M.; Dreizler, S.; Lafarga, M.; Nagel, E.; Passegger, V. M.; Reffert, S.; Rosich, A.; Schweitzer, A.; Tal-Or, L.; Trifonov, T.; Zechmeister, M.; Quirrenbach, A.; Amado, P. J.; Guenther, E. W.; Hagen, Hans; Henning, Th.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Montes, D.; Seifert, W.; Abellán, F. J.; Abril, Miguel; Aceituno, J.; Aceituno, F. J.; Alonso-Floriano, F. J.; Eiff, M. Ammler‐von; Antona, R.; Arroyo-Torres, B.; Azzaro, M.; Barrado, D.; Becerril-Jarque, S.; Benítez, D.; Berdiñas, Z. M.; Bergond, G.; Brinkmöller, M.; Burgo, C. del; Burn, Remo; Calvo-Ortega, R.; Cano, J.; Cárdenas, M. C.; Guillén, C. Cardona; Carro, Joseph; Casal, E.; Casanova, V.; Casasayas-Barris, N.; Chaturvedi, P.; Cifuentes, C.; Claret, A.; Colomé, J.; Czesla, S.; Díez-Alonso, E.; Dorda, R.; Emsenhuber, Alexandre; Fernández, M.; Fernández-Martín, A.; Ferro, I. M.; Fuhrmeister, B.; Galadí-Enríquez, D.; Cava, I. Gallardo; Vargas, M.; García-Piquer, Á.; Gesa, L.; González-Álvarez, E.; Hernández, J. I. González; González-Peinado, R.; Guàrdia, J.; Guijarro, A.; Guindos, E. de; Hatzes, A. P.; Hauschildt, P. H.; Hedrosa, R. P.; Hermelo, I.; Arabí, R. Hernández; Otero, Federico; Hintz, D.; Holgado, G.; Huber, Armin; Huke, P.; Johnson, E. N.; Juan, E. de; Kehr, M.; Kemmer, J.; Kim, M.; Klüter, J.; Klutsch, A.; Labarga, F.; Labiche, N.; Lalitha, S.; Lampón, M.; Lara, L. M.; Launhardt, R.; Lázaro, Francisco J.; Lizon, J. L.; Llamas, María Concepción Castrillo; Lodieu, N.; Fresno, M. López del; Salas, J. F. López; López‐Santiago, J.; Madinabeitia, H. Magán; Mall, U.; Mancini, L.; Mandel, H.; Marfil, E.; Molina, Juan; Martı́n, E. L.; Martín-Fernández, P.; Mart́ın-Rúız, S.; Martínez-Rodríguez, Héctor; Marvin, C. J.; Mirabet, E.; Moya, A.; Naranjo, V.; Nelson, Richard P.; Nortmann, L.; Nowak, G.; Ofir, A.; Pascual, Juan Pablo; Pavlov, A.; Pedraz, S.; Medialdea, D. Pérez; Pérez-Calpena, A.; Perryman, M. A. C.; Rabaza, O.; Ramón-Ballesta, A.; Rebolo, R.; Redondo, Pablo Quinzá; Rix, Hans─Walter; Rodler, F.; Trinidad, A. Rodríguez; Sabotta, S.; Sadegi, S.; Salz, M.; Sánchez-Blanco, E.; Carrasco, M. Á. Sánchez; Sánchez-López, A.; Sanz-Forcada, J.; Sarkis, P.; Sarmiento, L. F.; Schäfer, Sebastian; Schlecker, Martin; Schmitt, J. H. M. M.; Schöfer, P.; Solano, E.; Sota, A.; Stahl, O.; Stock, S.; Stuber, T.; Stürmer, Julian; Suárez, J. C.; Tabernero, H. M.; Tulloch, Simon; Veredas, G.; Vico-Linares, J. I.; Vilardell, F.; Wagner, K.; Winkler, Johannes; Wolthoff, V.; Yan, F.; Osorio, M. R. Zapatero

doi:10.1126/science.aax3198

Cited by 101 publications

(72 citation statements)

References 71 publications

(50 reference statements)

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“…The recent bulk of multi-planetary discoveries around M dwarfs opens a great opportunity to study their orbital architecture in detail. Understanding the dynamics of multi-planet systems around M dwarfs provides an important clue to planet formation around these low-mass stars (Lissauer 2007;Raymond et al 2007;Zhu et al 2012;Anglada-Escudé et al 2013;Coleman et al 2017;Morales et al 2019). Furthermore, the planetary dynamics affect the evolution of any natural satellites; these exomoons can provide critical information on the formation and evolution of a planetary system (see Heller et al 2014), and may 1 See also http://exoplanet.eu even be habitable themselves (Williams et al 1997;Heller & Barnes 2013;Forgan & Dobos 2016).…”

Section: Introductionmentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Trifonov

Lee²,

Kürster

et al. 2020

A&A

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Context. GJ 1148 is an M-dwarf star hosting a planetary system composed of two Saturn-mass planets in eccentric orbits with periods of 41.38 and 532.02 days. Aims. We reanalyze the orbital configuration and dynamics of the GJ 1148 multi-planetary system based on new precise radial velocity (RV) measurements taken with CARMENES. Methods. We combined new and archival precise Doppler measurements from CARMENES with those available from HIRES for GJ 1148 and modeled these data with a self-consistent dynamical model. We studied the orbital dynamics of the system using the secular theory and direct N-body integrations. The prospects of potentially habitable moons around GJ 1148 b were examined. Results. The refined dynamical analyses show that the GJ 1148 system is long-term stable in a large phase-space of orbital parameters with an orbital configuration suggesting apsidal alignment, but not in any particular high-order mean-motion resonant commensurability. GJ 1148 b orbits inside the optimistic habitable zone (HZ). We find only a narrow stability region around the planet where exomoons can exist. However, in this stable region exomoons exhibit quick orbital decay due to tidal interaction with the planet. Conclusions. The GJ 1148 planetary system is a very rare M-dwarf planetary system consisting of a pair of gas giants, the inner of which resides in the HZ. We conclude that habitable exomoons around GJ 1148 b are very unlikely to exist.

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Section: Introductionmentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

Trifonov

Lee²,

Kürster

et al. 2020

A&A

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“…The main goal of CARMENES is to discover and characterize Earth-like planets around an initial sample of about 300 M dwarfs (Reiners et al 2018b). To date, the program has already confirmed eight planet candidates from large-scale photometric and spectroscopic surveys (e.g., Trifonov et al 2018;Sarkis et al 2018) and detected more than ten new planets (e.g., Reiners et al 2018a;Kaminski et al 2018;Luque et al 2018Luque et al , 2019Ribas et al 2018;Nagel et al 2019;Perger et al 2019;Zechmeister et al 2019;Morales et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The CARMENES search for exoplanets around M dwarfs

González-Álvarez

Osorio

Caballero

et al. 2020

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Aims. We report on radial velocity time series for two M0.0 V stars, GJ 338 B and GJ 338 A, using the CARMENES spectrograph, complemented by ground-telescope photometry from Las Cumbres and Sierra Nevada observatories. We aim to explore the presence of small planets in tight orbits using the spectroscopic radial velocity technique. Methods. We obtained 159 and 70 radial velocity measurements of GJ 338 B and A, respectively, with the CARMENES visible channel between 2016 January and 2018 October. We also compiled additional relative radial velocity measurements from the literature and a collection of astrometric data that cover 200 a of observations to solve for the binary orbit. Results. We found dynamical masses of 0.64 ± 0.07 M for GJ 338 B and 0.69 ± 0.07 M for GJ 338 A. The CARMENES radial velocity periodograms show significant peaks at 16.61 ± 0.04 d (GJ 338 B) and 16.3 +3.5 −1.3 d (GJ 338 A), which have counterparts at the same frequencies in CARMENES activity indicators and photometric light curves. We attribute these to stellar rotation. GJ 338 B shows two additional, significant signals at 8.27 ± 0.01 and 24.45 ± 0.02 d, with no obvious counterparts in the stellar activity indices. The former is likely the first harmonic of the star's rotation, while we ascribe the latter to the existence of a super-Earth planet with a minimum mass of 10.27 +1.47 −1.38 M ⊕ orbiting GJ 338 B. We have not detected signals of likely planetary origin around GJ 338 A. Conclusions. GJ 338 Bb lies inside the inner boundary of the habitable zone around its parent star. It is one of the least massive planets ever found around any member of stellar binaries. The masses, spectral types, brightnesses, and even the rotational periods are very similar for both stars, which are likely coeval and formed from the same molecular cloud, yet they differ in the architecture of their planetary systems.

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“…EDEN has unique capabilities to target these stars and any planet our survey may detect will serve as a valuable addition to this small sample. The examples of TRAPPIST-1 (Gillon et al 2017) and GJ 3512b (Morales et al 2019) showed how individual discoveries can challenge our current understanding of planet formation and inform tests of competing formation theories. To assess such discoveries in terms of the actual underlying population of exoplanets, it is crucial to be aware of and able to quantify the relevant selection biases.…”

Section: Constraints On Planet Formation Theorymentioning

confidence: 99%

EDEN: Sensitivity Analysis and Transiting Planet Detection Limits for Nearby Late Red Dwarfs

Gibbs

Bixel

Rackham

et al. 2020

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Small planets are common around late-M dwarfs and can be detected through highly precise photometry by the transit method. Planets orbiting nearby stars are particularly important as they are often the best-suited for future follow-up studies. We present observations of three nearby M-dwarfs referred to as EIC-1, EIC-2, and EIC-3, and use them to search for transits and set limits on the presence of planets. On most nights our observations are sensitive to Earth-sized transiting planets, and photometric precision is similar to or better than TESS for faint late-M dwarfs of the same magnitude (I ≈ 15 mag). We present our photometry and transit search pipeline, which utilizes simple median detrending in combination with transit least squares based transit detection (Hippke & Heller 2019). For these targets, and transiting planets between one and two Earth radii, we achieve an average transit detection probability of∼60% between periods of 0.5 and 2 days, ∼30% between 2 and 5 days, and ∼10% between 5 and 10 days. These sensitivities are conservative compared to visual searches.

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A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Cited by 101 publications

References 71 publications

The CARMENES search for exoplanets around M dwarfs

The CARMENES search for exoplanets around M dwarfs

The CARMENES search for exoplanets around M dwarfs

EDEN: Sensitivity Analysis and Transiting Planet Detection Limits for Nearby Late Red Dwarfs

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