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1. The CARMENES search for exoplanets around M dwarfs. Guaranteed time observations Data Release 1 (2016-2020)

Author

I. Ribas, A. Reiners, M. Zechmeister, J. A. Caballero, J. C. Morales, S. Sabotta, D. Baroch, P. J. Amado, A. Quirrenbach, M. Abril, J. Aceituno, G. Anglada-Escudé, M. Azzaro, D. Barrado, V. J. S. Béjar, D. Benítez de Haro, G. Bergond, P. Bluhm, R. Calvo Ortega, C. Cardona Guillén, P. Chaturvedi, C. Cifuentes, J. Colomé, D. Cont, M. Cortés-Contreras, S. Czesla, E. Díez-Alonso, S. Dreizler, C. Duque-Arribas, N. Espinoza, M. Fernández, B. Fuhrmeister, D. Galadí-Enríquez, A. García-López, E. González-Álvarez, J. I. González Hernández, E. W. Guenther, E. de Guindos, A. P. Hatzes, Th. Henning, E. Herrero, D. Hintz, Á. L. Huelmo, S. V. Jeffers, E. N. Johnson, E. de Juan, A. Kaminski, J. Kemmer, J. Khaimova, S. Khalafinejad, D. Kossakowski, M. Kürster, F. Labarga, M. Lafarga, S. Lalitha, M. Lampón, J. Lillo-Box, N. Lodieu, M. J. López González, M. López-Puertas, R. Luque, H. Magán, L. Mancini, E. Marfil, E. L. Martín, S. Martín-Ruiz, K. Molaverdikhani, D. Montes, E. Nagel, L. Nortmann, G. Nowak, E. Pallé, V. M. Passegger, A. Pavlov, S. Pedraz, V. Perdelwitz, M. Perger, A. Ramón-Ballesta, S. Reffert, D. Revilla, E. Rodríguez, C. Rodríguez-López, S. Sadegi, M. Á. Sánchez Carrasco, A. Sánchez-López, J. Sanz-Forcada, S. Schäfer, M. Schlecker, J. H. M. M. Schmitt, P. Schöfer, A. Schweitzer, W. Seifert, Y. Shan, S. L. Skrzypinski, E. Solano, O. Stahl, M. Stangret, S. Stock, J. Stürmer, H. M. Tabernero, L. Tal-Or, T. Trifonov, S. Vanaverbeke, F. Yan, and M. R. Zapatero Osorio

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

The CARMENES instrument was conceived to deliver high-accuracy radial velocity (RV) measurements with long-term stability to search for temperate rocky planets around a sample of nearby cool stars. The broad wavelength coverage was designed to provide a range of stellar activity indicators to assess the nature of potential RV signals and to provide valuable spectral information to help characterise the stellar targets. The CARMENES Data Release 1 (DR1) makes public all observations obtained during the CARMENES guaranteed time observations, which ran from 2016 to 2020 and collected 19,633 spectra for a sample of 362 targets. The CARMENES survey target selection was aimed at minimising biases, and about 70% of all known M dwarfs within 10 pc and accessible from Calar Alto were included. The data were pipeline-processed, and high-level data products, including 18,642 precise RVs for 345 targets, were derived. Time series data of spectroscopic activity indicators were also obtained. We discuss the characteristics of the CARMENES data, the statistical properties of the stellar sample, and the spectroscopic measurements. We show examples of the use of CARMENES data and provide a contextual view of the exoplanet population revealed by the survey, including 33 new planets, 17 re-analysed planets, and 26 confirmed planets from transiting candidate follow-up. A subsample of 238 targets was used to derive updated planet occurrence rates, yielding an overall average of 1.44+/-0.20 planets with 1 M_Earth < M sin i < 1000 M_Earth and 1 d < P_orb < 1000 d per star, and indicating that nearly every M dwarf hosts at least one planet. CARMENES data have proven very useful for identifying and measuring planetary companions as well as for additional applications, such as the determination of stellar properties, the characterisation of stellar activity, and the study of exoplanet atmospheres., Published in A&A (https://www.aanda.org/10.1051/0004-6361/202244879), 25 pages, 12 figures, Tables 1 and 2 only available online

Published
2023

2. The CARMENES search for exoplanets around M dwarfs. Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star

Author

D. Kossakowski, M. Kürster, T. Trifonov, Th. Henning, J. Kemmer, J. A. Caballero, R. Burn, S. Sabotta, J. S. Crouse, T. J. Fauchez, E. Nagel, A. Kaminski, E. Herrero, E. Rodríguez, E. González-Álvarez, A. Quirrenbach, P. J. Amado, I. Ribas, A. Reiners, J. Aceituno, V. J. S. Béjar, D. Baroch, S. T. Bastelberger, P. Chaturvedi, C. Cifuentes, S. Dreizler, S. V. Jeffers, R. Kopparapu, M. Lafarga, M. J. López-González, S. Martín-Ruiz, D. Montes, J. C. Morales, E. Pallé, A. Pavlov, S. Pedraz, V. Perdelwitz, M. Pérez-Torres, M. Perger, S. Reffert, C. Rodríguez López, M. Schlecker, P. Schöfer, A. Schweitzer, Y. Shan, A. Shields, S. Stock, E. Wolf, M. R. Zapatero Osorio, and M. Zechmeister

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery of an Earth-mass planet ($M_b\sin i = 1.26\pm0.21M_\oplus$) on a 15.6d orbit of a relatively nearby ($d\sim$9.6pc) and low-mass ($0.167\pm0.011 M_\odot$) M5.0V star, Wolf 1069. Sitting at a separation of $0.0672\pm0.0014$au away from the host star puts Wolf 1069b in the habitable zone (HZ), receiving an incident flux of $S=0.652\pm0.029S_\oplus$. The planetary signal was detected using telluric-corrected radial-velocity (RV) data from the CARMENES spectrograph, amounting to a total of 262 spectroscopic observations covering almost four years. There are additional long-period signals in the RVs, one of which we attribute to the stellar rotation period. This is possible thanks to our photometric analysis including new, well-sampled monitoring campaigns undergone with the OSN and TJO facilities that supplement archival photometry (i.e., from MEarth and SuperWASP), and this yielded an updated rotational period range of $P_{rot}=150-170$d, with a likely value at $169.3^{+3.7}_{-3.6}$d. The stellar activity indicators provided by the CARMENES spectra likewise demonstrate evidence for the slow rotation period, though not as accurately due to possible factors such as signal aliasing or spot evolution. Our detectability limits indicate that additional planets more massive than one Earth mass with orbital periods of less than 10 days can be ruled out, suggesting that perhaps Wolf 1069 b had a violent formation history. This planet is also the 6th closest Earth-mass planet situated in the conservative HZ, after Proxima Centauri b, GJ 1061d, Teegarden's Star c, and GJ 1002 b and c. Despite not transiting, Wolf 1069b is nonetheless a very promising target for future three-dimensional climate models to investigate various habitability cases as well as for sub-ms$^{-1}$ RV campaigns to search for potential inner sub-Earth-mass planets in order to test planet formation theories., 26 pages, 15 figures

Published
2023

3. TOI-220 b: a warm sub-Neptune discovered by TESS

Author

Petr Kabath, K. I. Collins, Florian Rodler, Christopher Stockdale, Sara Seager, T. Lopez, S. Hojjatpanah, Steve B. Howell, S. Sabotta, Nuno C. Santos, David Barrado, Enric Palle, Jan Subjak, M. Esposito, John P. Doty, Rafael Luque, Artyom Aguichine, Karen A. Collins, Olivier Demangeon, Vincent Van Eylen, J. R. De Medeiros, M. Fridlund, N. Scott, Susan E. Mullally, E. Goffo, J. F. Otegi, D. W. Latham, Oscar Barragán, Jon M. Jenkins, Rodrigo F. Díaz, L. M. Serrano, Stéphane Udry, P. Figueira, A. P. Hatzes, Vardan Adibekyan, Davide Gandolfi, P. Cortés-Zuleta, W. Fong, J. Cabrera, Peter J. Wheatley, Seth Redfield, Sascha Grziwa, A. Santerne, Benjamin F. Cooke, Sergio Hoyer, L. Acuña, Daniel Bayliss, J. D. Twicken, S. G. Sousa, A. Osborn, Joshua N. Winn, P. A. Strøm, Hans J. Deeg, E. Delgado Mena, H. P. Osborn, William D. Cochran, Rachel A. Matson, Elise Furlan, Jorge Lillo-Box, P. T. Boyd, John H. Livingston, I. C. Leão, James A. G. Jackman, Edward M. Bryant, François Bouchy, Magali Deleuil, O. Mousis, Jose-Manuel Almenara, Carina M. Persson, Judith Korth, Roland Vanderspek, Louise D. Nielsen, B. L. Canto Martins, David J. Armstrong, Eric L. N. Jensen, Emil Knudstrup, D. A. Yahalomi, Jeffrey C. Smith, S. C. C. Barros, Xavier Dumusque, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Department of Brain and Behavioural Sciences, University of Pavia, European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Astronomie et Astrophysique du Languedoc (GRAAL), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), Institut Néel (NEEL), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Department of Geosciences and Natural Resource Management [Copenhagen] (IGN), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), University of Warwick [Coventry], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics [Coventry], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Marine and Antarctic Studies [Horbat] (IMAS), University of Tasmania [Hobart, Australia] (UTAS), PSE-ENV/SEDRE/LETIS, Institut de Radioprotection et de Sûreté Nucléaire (IRSN), European Southern Observatory [Santiago] (ESO), Thüringer Landessternwarte Tautenburg (TLS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Universidad de Córdoba [Cordoba], Instituto de Astrofisica de Canarias (IAC), Wesleyan University, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Pavia = University of Pavia (UNIPV), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Universidade do Porto = University of Porto, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université de Genève = University of Geneva (UNIGE), Institute for Marine and Antarctic Studies [Hobart] (IMAS), Laboratoire d'étude et de recherche sur les transferts et les interactions dans les sous-sols (IRSN/PSE-ENV/SEDRE/LETIS), Service des déchets radioactifs et des transferts dans la géosphère (IRSN/PSE-ENV/SEDRE), Institut de Radioprotection et de Sûreté Nucléaire (IRSN)-Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Universidad de Córdoba = University of Córdoba [Córdoba], and Universidade do Porto = University of Porto-Universidade do Porto = University of Porto

Subjects
Dwarf star, Fundamental Parameters, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Individual, Astrophysics, Photometric, planets and satellites: individual: TYC 8897-01263-1, 01 natural sciences, techniques: photometric, Planet, Neptune, 0103 physical sciences, techniques: radial velocities, Radial Velocities, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, TYC 8897-01263-1, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Planets and Satellites, Radius, Planetary system, Stars, Exoplanet, Techniques, Radial velocity, 13. Climate action, Space and Planetary Science, echniques: photometric, stars: fundamental parameters, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.03 $\pm$ 0.15 R$_{Earth}$, implying a bulk density of 2.73 $\pm$ 0.47 $\textrm{g cm}^{-3}$. TOI-220 $b$ orbits a relative bright (V=10.4) and old (10.1$\pm$1.4 Gyr) K dwarf star with a period of $\sim$10.69 d. Thus, TOI-220 $b$ is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 $b$ internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core., Comment: Accepted for publication in MNRAS

Published
2021
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4. Lack of close-in, massive planets of main-sequence A-type stars from Kepler

Author

S. Sabotta, Eike W. Guenther, Sascha Grziwa, Daniel Dupkala, Marek Skarka, Judith Korth, Petr Kabath, and Tereza Klocova

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary system, Light curve, A-type main-sequence star, 01 natural sciences, Radial velocity, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Some theories of planet formation and evolution predict that intermediate-mass stars host more hot Jupiters than Sun-like stars, others reach the conclusion that such objects are very rare. By determining the frequencies of those planets we can test those theories. Based on the analysis of Kepler light curves it has been suggested that about 8 per cent of the intermediate-mass stars could have a close-in substellar companion. This would indicate a very high frequency of such objects. Up to now, there was no satisfactory proof or test of this hypothesis. We studied a previously reported sample of 166 planet candidates around main-sequence A-type stars in the Kepler field. We selected six of them for which we obtained extensive long-term radial velocity measurements with the Alfred Jensch 2-m telescope in Tautenburg and the Perek 2-m telescope in Ondřejov. We derive upper limits of the masses of the planet candidates. We show that we are able to detect this kind of planet with our telescopes and their instrumentation using the example of MASCARA-1 b. With the transit finding pipeline Extrans we confirm that there is no single transit event from a Jupiter-like planet in the light curves of those 166 stars. We furthermore determine that the upper limit for the occurrence rate of close-in, massive planets for A-type stars in the Kepler sample is around 0.75 per cent. We argue that there is currently little evidence for a very high frequency of close-in, massive planets of intermediate-mass stars.

Published
2019
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5. The CARMENES search for exoplanets around M dwarfs -- Planet occurrence rates from a subsample of 71 stars

Author

M. Kürster, P. J. Amado, I. Muñoz Rodríguez, Artie P. Hatzes, Priyanka Chaturvedi, M. Lafarga, M. Perger, M. Azzaro, E. W. Guenther, Th. Henning, Andreas Quirrenbach, Sandra V. Jeffers, Y. Shan, Ignasi Ribas, Mathias Zechmeister, D. Montes, A. Kaminski, Martin Schlecker, Ansgar Reiners, J. A. Caballero, Hubert Klahr, Juan Carlos Morales, Stefan Dreizler, Enric Palle, S. Sabotta, Sabine Reffert, V. M. Passegger, J. C. Muñoz Sánchez, German Research Foundation, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, and National Aeronautics and Space Administration (US)

Subjects
Astrofísica, Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, Methods: data analysis, low-mass [Stars], Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Stars: low-mass, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, Orbital period, Exoplanet, Planetary systems, Stars, 13. Climate action, Space and Planetary Science, Techniques: radial velocities, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. The CARMENES exoplanet survey of M dwarfs has obtained more than 18 000 spectra of 329 nearby M dwarfs over the past five years as part of its guaranteed time observations (GTO) program. Aims. We determine planet occurrence rates with the 71 stars from the GTO program for which we have more than 50 observations. Methods. We use injection-and-retrieval experiments on the radial-velocity time series to measure detection probabilities. We include 27 planets in 21 planetary systems in our analysis. Results. We find 0.06-0.03+0.04 giant planets (100 Mpdbl < Mpl sin i < 1000 Mpdbl) per star in periods of up to 1000 d, but due to a selection bias this number could be up to a factor of five lower in the whole 329-star sample. The upper limit for hot Jupiters (orbital period of less than 10 d) is 0.03 planets per star, while the occurrence rate of planets with intermediate masses (10 Mpdbl < Mpl sin i < 100 Mpdbl) is 0.18-0.05+0.07 planets per star. Less massive planets with 1 Mpdbl < Mpl sin i < 10 Mpdbl are very abundant, with an estimated rate of 1.32-0.31+0.33 planets per star for periods of up to 100 d. When considering only late M dwarfs with masses M- < 0.34 M⊙ , planets more massive than 10 Mpdbl become rare. Instead, low-mass planets with periods shorter than 10 d are significantly overabundant. Conclusions. For orbital periods shorter than 100 d, our results confirm the known stellar mass dependences from the Kepler survey: M dwarfs host fewer giant planets and at least two times more planets with Mpl sin i < 10 Mpdbl than G-type stars. In contrast to previous results, planets around our sample of very low-mass stars have a higher occurrence rate in short-period orbits of less than 10 d. Our results demonstrate the need to take into account host star masses in planet formation models. © ESO 2021., This work was supported by the Thuringer Ministerium fur Wirtschaft, Wissenschaft und Digitale Gesellschaft, and the Deutsche Forschungsgemeinschaft (DFG) under the DFG Research Unit FOR2544 "Blue Planets around Red Stars" (RE 2694/8-1) and the project GU 464/20-1. CARMENES is an instrument at the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto (Almeria, Spain), operated jointly by the Junta de Andalucia and the Instituto de Astrofisica de Andalucia (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Cientificas (CSIC), the Ministerio de Economia y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut fur Astronomie, Instituto de Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de Ciencies de l'Espai, Institut fur Astrophysik Gottingen, Universidad Complutense de Madrid, Thuringer Landessternwarte Tautenburg, Instituto de Astrofisica de Canarias, Hamburger Sternwarte, Centro de Astrobiologia and Centro Astronomico Hispano-Aleman), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and Research Unit FOR2544 "Blue Planets around Red Stars", the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia. We acknowledge financial support from the Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the ERDF through projects PID2019-109522GB-C5[1:4]/AEI/10.13039/501100011033 and the Centre of Excellence "Severo Ochoa" and "Maria de Maeztu" awards to the Instituto de Astrofisica de Canarias (SEV-2015-0548), Instituto de Astrofisica de Andalucia (SEV-2017-0709), and Centro de Astrobiologia (MDM-2017-0737), the Generalitat de Catalunya/CERCA programme, the DFG program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (JE 701/5-1), and NASA (NNX17AG24G).

Published
2021
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6. Mass determinations of the three mini-Neptunes transiting TOI-125

Author

Farzana Meru, Matías R. Díaz, John H. Livingston, Florian Rodler, Samuel N. Quinn, Pablo Rojas, Heike Rauer, Diana Kossakowski, Isabelle Boisse, George R. Ricker, P. T. Boyd, Ravit Helled, Judith Korth, S. C. C. Barros, L. A. dos Santos, A. P. Hatzes, S. Sabotta, Rafael Luque, M. Stalport, Andrew Vanderburg, Jason H. Steffen, Vincent Van Eylen, Edward M. Bryant, Jon M. Jenkins, David J. Armstrong, L. González-Cuesta, S. Hojjatpanah, Norio Narita, Felipe Murgas, Savita Mathur, J. F. Otegi, Paul Wilson, Iskra Georgieva, Nicolás T. Kurtovic, Sara Seager, Emeline Bolmont, Xavier Dumusque, Jose I. Vines, M. Esposito, Z. M. Berdinas, Sascha Grziwa, Olivier Demangeon, J. M. Almenara, O. Mousis, Julia V. Seidel, D. J. A. Brown, T. Lopez, A. Santerne, S. G. Sousa, Benjamin F. Cooke, Davide Gandolfi, R. A. Garcia, Eric B. Ting, Fei Dai, David W. Latham, Daniel Bayliss, Romain Allart, Peter J. Wheatley, François Bouchy, Christopher J. Burke, Vardan Adibekyan, Seth Redfield, Hugh P. Osborn, Natalia Guerrero, Joshua N. Winn, Malcolm Fridlund, Martin Turbet, Louise D. Nielsen, Chris Henze, Caroline Dorn, J. Dittman, K. W. F. Lam, Carina M. Persson, William D. Cochran, Jorge Lillo-Box, Rodrigo F. Díaz, Stéphane Udry, Nuno C. Santos, David Barrado, Enric Palle, James S. Jenkins, Roland Vanderspek, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Vanderburg, A. [0000-0001-7246-5438], Dos Santos, L. [0000-0002-2248-3838], Barrado, D. [0000-0002-5971-9242], Cochran, W. [0000-0001-9662-3496], Lillo Box, J. [0000-0003-3742-1987], Barros, S. [0000-0003-2434-3625], Stalport, M. [0000-0003-0996-6402], Dorn, C. [0000-0001-6110-4610], Nielsen, L. D. [0000-0002-5254-2499], Seidel, J. V. [0000-0002-7990-9596], Diaz, M. R. [0000-0002-2100-3257], Bolmont, E. [0000-0001-5657-4503], Adibekyan, V. [0000-0002-0601-6199], Van Eylen, V. [0000-0001-5542-8870], Armstrong, D. [0000-0002-5080-4117], Korth, J. [0000-0002-0076-6239], Díaz, R. [0000-0001-9289-5160], Santos, N. [0000-0003-4422-2919], Luque, R. [0000-0002-4671-2957], Turbet, M. [0000-0003-2260-9856], Mathur, S. [0000-0002-0129-0316], Strom, P. A. [0000-0002-7823-1090], Sabotta, S. [0000-0001-9078-5574], Wheatley, P. [0000-0003-1452-2240], Hojjatpanah, S. [0000-0002-0417-1902], Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Swiss National Science Foundation (SNSF), Deutsche Forschungsgemeinschaft (DFG), Agencia Estatal de Investigación (AEI), European Southern Observatory (ESO), Swiss National Centre of Competence inResearch (NCCR), National Aeronautics and Space Administration (NASA), Fundacao para a Ciencia e a Tecnologia (FCT), European Research Council (ERC), European Southern Observatory, STFC via an Ernest Rutherford Fellowship, FEDER -Fundo Europeu de Desenvolvimento Regional through COMPETE2020-Programa Operacional Competitividade e Internacionalizacao, Portuguese Foundation for Science and Technology, CONICYT-PFCHA/Doctorado Nacional, Comision Nacional de Investigacion Cientifica y Tecnologica CONICYT FONDECYT, German Research Foundation (DFG), Spanish State Research Agency (AEI), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, and Spanish Ministry under the Ramon y Cajal fellowship

Subjects
010504 meteorology & atmospheric sciences, Planets and satellites: detection, Planets and satellites: individual: (TOI-125, TIC 52368076), FOS: Physical sciences, 01 natural sciences, Neptune, Planet, TIC 52368076), 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], individual: TOI-125, TIC 52368076 [Planets and satellites], Ecliptic, Astronomy, Astronomy and Astrophysics, Radius, Planets and satellites: detection, Orbital period, Exoplanet, Radial velocity, detection [Planets and satellites], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - Earth and Planetary Astrophysics, Planets and satellites: individual: (TOI-125
Abstract

The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, steady progress was made in achieving the mission's primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, TESS's observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V=11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c and TOI-125d. TOI-125b has an orbital period of 4.65 days, a radius of $2.726 \pm 0.075 ~\mathrm{R_{\rm E}}$, a mass of $ 9.50 \pm 0.88 ~\mathrm{M_{\rm E}}$ and is near the 2:1 mean motion resonance with TOI-125c at 9.15 days. TOI-125c has a similar radius of $2.759 \pm 0.10 ~\mathrm{R_{\rm E}}$ and a mass of $ 6.63 \pm 0.99 ~\mathrm{M_{\rm E}}$, being the puffiest of the three planets. TOI-125d, has an orbital period of 19.98 days and a radius of $2.93 \pm 0.17~\mathrm{R_{\rm E}}$ and mass $13.6 \pm 1.2 ~\mathrm{M_{\rm E}}$. For TOI-125b and TOI-125d we find unusual high eccentricities of $0.19\pm 0.04$ and $0.17^{+0.08}_{-0.06}$, respectively. Our analysis also provides upper mass limits for the two low-SNR planet candidates in the system; for TOI-125.04 ($R_P=1.36 ~\mathrm{R_{\rm E}}$, $P=$0.53 days) we find a $2\sigma$ upper mass limit of $1.6~\mathrm{M_{\rm E}}$, whereas TOI-125.05 ( $R_P=4.2^{+2.4}_{-1.4} ~\mathrm{R_{\rm E}}$, $P=$ 13.28 days) is unlikely a viable planet candidate with upper mass limit $2.7~\mathrm{M_{\rm E}}$. We discuss the internal structure of the three confirmed planets, as well as dynamical stability and system architecture for this intriguing exoplanet system., Comment: Accepted for publication in MNRAS

Published
2020
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7. A possibly inflated planet around the bright, young star DS Tuc A

Author

M. Esposito, S. Sabotta, Riccardo Claudi, Valentina D'Orazi, Domenico Nardiello, Andrea Bignamini, L. Borsato, Silvano Desidera, Valerio Nascimbeni, Serena Benatti, Dino Mesa, Sergio Messina, C. Lovis, Luca Malavolta, Mario Damasso, Elvira Covino, and ITA

Subjects
planets and satellites: fundamental parameters, techniques: photometric, techniques: spectroscopic, techniques: radial velocities, techniques: imaging spectroscopy, stars: individual: DS Tuc A, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, Light curve, Orbital period, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

The origin of the observed diversity of planetary system architectures is one of the main topic of the exoplanetary research. The detection of a statistically significant sample of planets around young stars allows us to study the early stages of planet formation and evolution, but only a handful of them is known so far. In this regard, a considerable contribution is expected from the NASA TESS satellite, which is now performing a survey of $\sim 85 \%$ of the sky to search for short-period transiting planets In its first month of operations, TESS found a planet candidate with an orbital period of 8.14 days around a member of the Tuc-Hor young association ($\sim$ 40 Myr), the G6V main component of the binary system DS\,Tuc. If confirmed, it would be the first transiting planet around a young star suitable for radial velocity and/or atmospheric characterization. We aim to validate the planetary nature of this companion and to measure its orbital and physical parameters. We obtain accurate planet parameters by coupling an independent reprocessing of the TESS light curve with improved stellar parameters and the dilution caused by the binary companion; we analyse high precision archival radial velocities to impose an upper limit of about 0.1 M$_{\rm Jup}$ on the planet mass; we finally rule out the presence of external companions beyond 40 au with adaptive optics images. We confirm the presence of a young, giant (${\rm R} = 0.50$ R$_{\rm Jup}$) planet having a not negligible possibility to be inflated (theoretical mass $\lesssim 20$ M$_{\oplus}$) around DS\,Tuc~A. We discuss the feasibility of mass determination, Rossiter-McLaughlin analysis and atmosphere characterization, allowed by the brightness of the star., Comment: 12 pages, 11 figures. Accepted for publication in A&A

Published
2019
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8. K2-106, a system containing a metal-rich planet and a planet of lower density

Author

David Nespral, Ph. Eigmüller, Alexis M. S. Smith, Eike W. Guenther, Davide Gandolfi, Pamela Arriagada, Heike Rauer, R. P. Butler, S. Sabotta, Martin Pätzold, Jeffrey D. Crane, Bun'ei Sato, A. Chau, Robert A. Wittenmyer, S. Shectman, A. P. Hatzes, Grzegorz Nowak, Teruyuki Hirano, Enric Palle, Carina M. Persson, Judith Korth, Ravit Helled, Jennifer Burt, Juan Cabrera, Fei Dai, Andrew Vanderburg, G. Antoniciello, Oscar Barragán, M. Hjorth, Anders Erikson, Malcolm Fridlund, John Asher Johnson, Norio Narita, Luca Fossati, V. Van Eylen, Sz. Csizmadia, Jorge Prieto-Arranz, Sascha Grziwa, Johanna Teske, D. Kubyshkina, Amanda Kiilerich, Ian B. Thompson, Hans J. Deeg, William D. Cochran, Simon Albrecht, and Joshua N. Winn

Subjects
EXOPLANET, TELESCOPE, 010504 meteorology & atmospheric sciences, Period (periodic table), SHORT-PERIOD PLANETS, Planetary systems, Stars: Abundances, Stars: individual: TYC 608-458-1, Techniques: photometric, Techniques: Radial velocities, Astronomy and Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astrophysics, MASS, 01 natural sciences, PARAMETERS, photometric [techniques], Atmosphere, Planet, 0103 physical sciences, SPECTROGRAPH, planetary systems, 010303 astronomy & astrophysics, MISSION, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Range (particle radiation), Atmospheric escape, radial velocities [techniques], Radius, Planetary system, abundances [stars], SUPER-EARTHS, RADIAL-VELOCITY MEASUREMENTS, individual: TYC 608-458-1 [stars], STARS, Earth (classical element), Astrophysics - Earth and Planetary Astrophysics
Abstract

Planets in the mass range from 2 to 15 MEarth are very diverse. Some of them have low densities, while others are very dense. By measuring the masses and radii, the mean densities, structure, and composition of the planets are constrained. These parameters also give us important information about their formation and evolution, and about possible processes for atmospheric loss.We determined the masses, radii, and mean densities for the two transiting planets orbiting K2-106. The inner planet has an ultra-short period of 0.57 days. The period of the outer planet is 13.3 days.Although the two planets have similar masses, their densities are very different. For K2-106b we derive Mb=8.36-0.94+0.96 MEarh, Rb=1.52+/-0.16 REarth, and a high density of 13.1-3.6+5.4 gcm-3. For K2-106c, we find Mc=5.8-3.0+3.3 MEarth, Rc=2.50-0.26+0.27 REarth and a relatively low density of 2.0-1.1+1.6 gcm-3.Since the system contains two planets of almost the same mass, but different distances from the host star, it is an excellent laboratory to study atmospheric escape. In agreement with the theory of atmospheric-loss processes, it is likely that the outer planet has a hydrogen-dominated atmosphere. The mass and radius of the inner planet is in agreement with theoretical models predicting an iron core containing 80+20-30% of its mass. Such a high metal content is surprising, particularly given that the star has an ordinary (solar) metal abundance. We discuss various possible formation scenarios for this unusual planet., 11 pages with 9 figures, accepted by A&A, Sep 8, 2017

Published
2017
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9. A giant exoplanet orbiting a very-low-mass star challenges planet formation models

Author

Jesus M. Carro, A. Guijarro, F. Hernández Otero, Javier López-Santiago, E. Mirabet, Eduardo L. Martín, Hugo M. Tabernero, H. Martínez-Rodríguez, Antonio Claret, Martin Kürster, Florian Rodler, Birgit Fuhrmeister, M. Llamas, Z. M. Berdiñas, Thomas Henning, A. Rosich, Otmar Stahl, Guillem Anglada-Escudé, Luigi Mancini, E. W. Guenther, P. Huke, L. González-Cuesta, Ralf Launhardt, F. F. Bauer, Ignasi Ribas, D. Baroch, E. N. Johnson, M. Lafarga, Grzegorz Nowak, Priyanka Chaturvedi, M. Ammler-von Eiff, M. R. Zapatero Osorio, V. Wolthoff, E. Rodriguez, L. F. Sarmiento, E. Sánchez-Blanco, Luisa Lara, C. del Burgo, M. López del Fresno, Artie P. Hatzes, S. Lalitha, M. Kehr, Simon Tulloch, F. J. Lázaro, D. Montes, J. Klüter, Melvyn B. Davies, F. J. Aceituno, S. Martin-Ruiz, R. González-Peinado, Juan Luis Cano, Francesc Vilardell, Aviv Ofir, F. J. Abellán, J. Colomé, C. Cardona Guillén, Mathias Zechmeister, Urs Mall, D. Hintz, Richard P. Nelson, I. M. Ferro, V. M. Passegger, M. Cortés-Contreras, P. Martín-Fernández, M. Brinkmöller, Evangelos Nagel, Michael Perryman, Ovidio Rabaza, Jose Antonio Pascual, A. Kaminski, M. Perger, Gilles Bergond, D. Pérez Medialdea, Remo Burn, J. I. González Hernández, B. Arroyo-Torres, Rafael Luque, Martin Schlecker, Armin Huber, A. Fernández-Martín, M. J. López-González, S. Sabotta, G. Veredas, A. Ramón Ballesta, E. González-Álvarez, Fei Yan, Holger Mandel, J. Kemmer, J. I. Vico-Linares, S. Becerril-Jarque, Jorge Sanz-Forcada, Paula Sarkis, R. P. Hedrosa, Rafael Rebolo, J. Stürmer, A. Sánchez-López, Trifon Trifonov, F. Labarga, Jürgen H. M. M. Schmitt, Núria Casasayas-Barris, Alexandre Emsenhuber, Sebastian Schafer, J. A. Marín Molina, Alexander J. Mustill, Anders Johansen, H. Magán Madinabeitia, Hubert Klahr, F. J. Alonso-Floriano, S. V. Jeffers, I. Gallardo Cava, E. de Juan, Andreas Schweitzer, Peter H. Hauschildt, Ricardo Dorda, P. Redondo, M. Azzaro, M. Salz, M. Abril, Juan Carlos Suárez, Hans-Walter Rix, Carlos Cifuentes, Walter Seifert, M. L. García Vargas, Pedro J. Amado, J. Winkler, R. Hernández Arabí, S. Sadegi, I. Hermelo, A. Rodríguez Trinidad, G. Holgado, Karl Wagner, Vianak Naranjo, S. Czesla, M. Kim, D. Benítez, Sabine Reffert, A. Pavlov, Lluis Gesa, Nicolas Lodieu, Lisa Nortmann, D. Galadí-Enríquez, A. Moya, Andreas Quirrenbach, Jose A. Caballero, J. Aceituno, Enrique Herrero, Juan Carlos Morales, E. Casal, Emilio Marfil, Enrique Solano, Diana Kossakowski, E. Díez-Alonso, J.-L. Lizon, J. F. López Salas, M. Lampón, M. C. Cárdenas, P. Schöfer, Ansgar Reiners, R. Calvo-Ortega, T. Stuber, R. Antona, A. Garcia-Piquer, Lev Tal-Or, N. Labiche, Alfredo Sota, Ana Pérez-Calpena, David Barrado, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, S. Stock, M. Fernandez, Chris Mordasini, E. de Guindos, S. Pedraz, H.-J. Hagen, Jaime Guardia, A. Klutsch, M. A. Sánchez Carrasco, Christopher Marvin, V. Casanova, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Morales, J. C. [0000-0003-0061-518X], Mustill, A. J. [0000-0002-2086-3642], Ribas, I. [0000-0002-6689-0312], Davies, M. B. [0000-0001-6080-1190], Bauer, F. F. [0000-0003-1212-5225], Herrrero, E. [0000-0001-8602-6639], Rodríguez, E. [0000-0001-6827-9077], López González, M. J. [0000-0001-8104-5128], Rodríguez López, C. [0000-0001-5559-7850], Guenther, E. W. [0000-0002-9130-6747], López Santiago, J. [0000-0003-2402-8166], Kaminski, A. [0000-0003-0203-8208], Montes, D. [0000-0002-7779-238X], Baroch, D. [0000-0001-7568-5161], Alonso Floriano, F. J. [0000-0003-1202-5734], Ammler-von Eiff, M. [0000-0001-9565-1698], Anglada Escudé, G. [0000-0002-3645-5977], Barrado, D. [0000-0002-5971-9242], Becerril Jarque, S. [0000-0001-9009-1150], Díez Alonso, E. [0000-0002-5826-9892], Passegger, V. M. [0000-0002-8569-7243], Bergond, G. [0000-0003-3132-9215], Burn, R. [0000-0002-9020-7309], García Vargas, M. L. [0000-0002-2058-3528], Amado, P. J. [0000-0002-8388-6040], Cano, J. [0000-0003-1984-5401], Cardona Guillén, C. [0000-0002-2198-4200], Carro, J. [0000-0002-0838-3603], Abellán, F. J. [0000-0002-5724-1636], Chaturvedi, P. [0000-0002-1887-1192], Sabotta, S. [0000-0001-9078-5574], Cifuentes, C. [0000-0003-1715-5087], Colomé, J. [0000-0002-1678-2241], Arroyo Torres, B. [0000-0002-3392-4694], Emsenhuber, A. [0000-0002-8811-1914], Fuhrmeister, B. [0000-0001-8321-5514], Berdiñas, Z. M. [0000-0002-6057-6461], González Álvarez, E. [0000-0002-4820-2053], González Hernández, J. I. [0000-0002-0264-7356], Calvo Ortega, R. [0000-0003-3693-6030], Guàrdia, J. [0000-0002-7191-9001], Guijarro, A. [0000-0001-5518-1759], Lara, L. M. [0000-0002-7184-920X], Casasayas Barris, N. [0000-0002-2891-8222], Hermelo, I. [0000-0001-9178-694X], Hintz, D. [0000-0002-5274-2589], López del Fresno, M. [0000-0002-9479-7780], Czesla, S. [0000-0002-4203-4773], Johnson, E. [0000-0003-2260-5134], De Juan Fernández, E. [0000-0002-9382-4505], Kehr, M. [0000-0002-7420-7368], Galadí Enríquez, D. [0000-0003-4946-5653], Klüter, J. [0000-0002-3469-5133], González Cuesta, L. [0000-0002-1241-5508], Klutsch, A. [0000-0001-7869-3888], Labarga, F. [0000-0002-7143-0206], González Peinado, R. [0000-0002-6658-8930], Launhardt, R. [0000-0002-8298-2663], Lizon, J. L. [0000-0001-8928-2566], De Guindos, E. [0000-0002-8124-9101], Magan Madinabeitia, H. [0000-0003-1243-4597], Manici, L. [0000-0002-9428-8732], Huke, P. [0000-0001-5913-2743], Marín Molina, J. A. [0000-0002-3525-0806], Martín, E. [0000-0002-1208-4833], Rabaza, O. [0000-0003-2766-2103], Kim, M. [0000-0001-6218-2004], Martínez Rodríguez, H. [0000-0002-1919-228X], Marvin, C. J. [0000-0002-2249-2611], Rodríguez Trinidad, A. [0000-0002-3356-8634], Lampón, M. [0000-0002-0183-7158], Naranjo, V. [0000-0003-0097-1061], Nelson, R. [0000-0002-9687-8779], Nortmann, L. [0000-0001-8419-8760], Lodieu, N. [0000-0002-3612-8968], Ofir, A. [0000-0002-9152-5042], Aceituno, F. J. [0000-0001-8074-4760], Pascual Granado, J. [0000-0003-0139-6951], Pedraz, S. [0000-0003-1346-208X], Marfil, E. [0000-0001-8907-4775], Ramón Ballesta, A. [0000-0002-4323-0610], Redondo, P. G. [0000-0001-5992-5778], Martín Ruiz, S. [0000-0002-9006-7182], Sadegi, S. [0000-0001-9897-6121], Sánchez Carrasco, M. A. [0000-0001-5533-3660], Moya, A. [0000-0003-1665-5389], Sanz Forcada, J. [0000-0002-1600-7835], Sarkis, P. [0000-0001-8128-3126], Vilardell, F. [0000-0003-0441-1504], Nowak, G. [0000-0002-7031-7754], Schäfer, S. [0000-0001-8597-8048], Schlecker, M. [0000-0001-8355-2107], Béjar, V. J. S. [0000-0002-5086-4232], Pérez Calpena, A. [0000-0001-7361-9240], Schöfer, P. [0000-0002-5969-3708], Solano, E. [0000-0003-1885-5130], Sota, A. [https://orcid.org/0000-0002-9404-6952], Rodler, F. [0000-0003-0650-5723], Stuber, T. [0000-0003-2185-0525], García Piquer, A. [0000-0002-6872-4262], Suárez, J. C. [0000-0003-3649-8384], Tabernero, H. [0000-0002-8087-4298], Sánchez López, A. [0000-0002-0516-7956], Winkler, J. [0000-0003-0568-8820], Yan, F. [0000-0001-9585-9034], Sarmiento, L. F. [0000-0002-8475-9705], Luque, R. [0000-0002-4671-2957], Perger, M. [0000-0001-7098-0372], Schmitt, J. H. M. M. [0000-0003-2554-9916], Klahr, H. [0000-0002-8227-5467], Mordasini, C. [0000-0002-1013-2811], Aceituno, J. [0000-0003-0487-1105], Stock, S. [0000-0002-1166-9338], Cortés Contreras, M. [0000-0003-3734-9866], Lafarga, M. [0000-0002-8815-9416], Nagel, E. [0000-0002-4019-3631], Tulloch, S. [0000-0003-0840-8521], Reffert, S. [0000-0002-0460-8289], Rosich, A. [0000-0002-9141-3067], Trifonov, T. [0000-0002-0236-775X], Zapatero Osorio, M. R. [0000-0001-5664-2852], Israel Science Foundation (ISF), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), Swiss National Science Foundation (SNSF), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR), European Research Council (ERC), Generalitat de Catalunya, Deutsche Forschungsgemeinschaft (DFG), Queen Mary University of London, Consejo Nacional de Ciencia y Tecnología (CONACYT), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), German Centre for Air and Space Travel, European Research Council, German Research Foundation, National Science Foundation (US), Swiss National Science Foundation, Science and Technology Facilities Council (UK), Knut and Alice Wallenberg Foundation, Spanish Ministry for Science, Ramón y Cajal programa, Israel Science Foundation grant, CONICYT-FONDECYT/Chile Postdoctorado, Deutsches Zentrum fur Luft-un Raumfahrt (DLR), Italian Minister of Instruction, Mexican national council for science and technology, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, German Science Foundation (DFG) Research Unit, Priority Programs SPP, Exploring the Diversity of Extrasolar Planets, Swiss National Science Foundation under grant, Queen Mary University of London Scholarship and STFC, Spanish MCIU FPI-SO predoctoral contract, and European Research Council under the European Union Horizon 2020 research and innovation program

Subjects
010504 meteorology & atmospheric sciences, Gas giant, 530 Physics, FOS: Physical sciences, Minimum mass, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Multidisciplinary, 520 Astronomy, Giant planet, Astronomy, Planetary system, 620 Engineering, Accretion (astrophysics), Exoplanet, Orbit, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.Copyright © 2019 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science, This research was supported by the following programs, grants, and fellowships: Spanish Ministry for Science, Innovation and Universities (MCIU) ESP2014-54062-R, ESP2014-54362P, AYA2015-69350-C3-2-P, BES-2015-074542, AYA2016-79425-C3-1/2/3-P, ESP2016-76076-R, ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87143-R, ESP2017-87676-C05-02-R, ESP-2017-87676-2-2, RYC-2012-09913 (>Ramon y Cajal> program), and FPU15/01476; Israel Science Foundation grant 848/16, CONICYT-FONDECYT/Chile Postdoctorado 3180405; Deutsches Zentrum fur Luft-un Raumfahrt (DLR) 50OW0204 and 50OO1501; Italian Minister of Instruction, University and Research (MIUR), FFABR 2017; University of Rome Tor Vergata, >Mission: Sustainability 2016> fund; European Research Council under the European Union Horizon 2020 research and innovation program 694513; Mexican national council for science and technology CONACYT, CVU 448248; the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709); Generalitat de Catalunya/CERCA program; Fondo Europeo de Desarollo Regional (FEDER); German Science Foundation (DFG) Research Unit FOR2544 >Blue Planets around Red Stars> and Priority Programs SPP 1833, >Building a Habitable Earth> and SPP 1992, >Exploring the Diversity of Extrasolar Planets> NSF grants PHY17-48958 and PHY-1607761; Swiss National Science Foundation under grant BSGIO_155816 >PlaneltsInTime' and within the framework of the NCCR PlanetS; Queen Mary University of London Scholarship and STFC Consolidated Grant ST/P000592/1; Spanish MCIU FPI-SO predoctoral contract BES-2017-082610 and the Knut and Alice Wallenberg Foundation.

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