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1. The nebula around the binary post-AGB star 89 Herculis

Author

I. Gallardo Cava, J. Alcolea, V. Bujarrabal, M. Gómez-Garrido, and A. Castro-Carrizo

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

There is a class of binary post-asymptotic giant branch (post-AGB) stars that exhibit remarkable near-infrared (NIR) excess. These stars are surrounded by disks with Keplerian or quasi-Keplerian dynamics and outflows composed of gas escaping from the rotating disk. Depending on the dominance of these components, there are two subclasses of binary post-AGB stars: disk-dominated and outflow-dominated. We aim to properly study the hourglass-like structure that surrounds the Keplerian disk around 89 Her. We present total-power on-the-fly maps of $^{12}$CO and $^{13}$CO $J$=2-1 emission lines in 89 Her. Previous studies are known to suffer from flux losses in the most extended components. We merge these total-power maps with previous NOEMA maps. The resulting combined maps are expected to detect the whole nebula extent of the source. Our new combined maps contain the entirety of the detectable flux of the source and at the same time are of high spatial resolution thanks to the interferometric observations. We find that the hourglass-like extended outflow around the rotating disk is larger and more massive than suggested by previous works. The total nebular mass of this very extended nebula is 1.8E-2 solar masses, of which 65% comes from the outflow. The observational data and model results lead us to classify the envelope around 89 Her as an outflow-dominated nebula, together with R Sct and IRAS 19125+0343 (and very probably AI CMi, IRAS 20056+1834, and IRAS 18123+0511). The updated statistics on the masses of the two post-AGB main components reveal that there are two distinct subclasses of nebulae around binary post-AGB stars depending on which component is the dominant one. We speculate that the absence of an intermediate subclass of sources is due to the different initial conditions of the stellar system and not because both subclasses are in different stages of the post-AGB evolution., Accepted 5 January 2023 in Astronomy & Astrophysics. 17 pages

Published
2023

2. Chemistry of nebulae around binary post-AGB stars: A molecular survey of mm-wave lines

Author

I. Gallardo Cava, V. Bujarrabal, J. Alcolea, M. Gómez-Garrido, and M. Santander-García

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

Context. There is a class of binary post-asymptotic giant branch (post-AGB) stars that exhibit remarkable near-infrared excess. Such stars are surrounded by Keplerian or quasi-Keplerian disks, as well as extended outflows composed of gas escaping from the disk. This class can be subdivided into disk- and outflow-dominated sources, depending on whether it is the disk or the outflow that represents most of the nebular mass, respectively. The chemistry of this type of source has been practically unknown thus far. Aims. Our objective is to study the molecular content of nebulae around binary post-AGB stars that show disks with Keplerian dynamics, including molecular line intensities, chemistry, and abundances. Methods. We focused our observations on the 1.3, 2, 3 mm bands of the 30mIRAM telescope and on the 7 and 13 mm bands of the 40 m Yebes telescope. Our observations add up ~600 h of telescope time. We investigated the integrated intensities of pairs of molecular transitions for CO, other molecular species, and IRAS fluxes at 12, 25, and 60 μm. Additionally, we studied isotopic ratios, in particular 17O/18O, to analyze the initial stellar mass, as well as 12CO/13CO, to study the line and abundance ratios. Results. We present the first single-dish molecular survey of mm-wave lines in nebulae around binary post-AGB stars. We conclude that the molecular content is relatively low in nebulae around binary post-AGB stars, as their molecular lines and abundances are especially weaker compared with AGB stars. This fact is very significant in those sources where the Keplerian disk is the dominant component of the nebula. The study of their chemistry allows us to classify nebulae around AC Her, the Red Rectangle, AI CMi, R Sct, and IRAS 20056+1834 as O-rich, while that of 89 Her is probably C-rich. The calculated abundances of the detected species other than CO are particularly low compared with AGB stars. The initial stellar mass derived from the 17O/18O ratio for the Red Rectangle and 89 Her is compatible with the central total stellar mass derived from previous mm-wave interferometric maps. The very low 12CO/13CO ratios found in binary post-AGB stars reveal a high 13CO abundance compared to AGB and other post-AGB stars.

Published
2022

3. The CARMENES search for exoplanets around M dwarfs Two temperate Earth-mass planet candidates around Teegarden's Star

Author

A. Claret, E. Casal, Jorge Sanz-Forcada, D. Montes, Juan Luis Cano, N. Casasayas-Barris, M. Lampón, C. Rodríguez López, E. de Guindos, Michael Perryman, N. Lodieu, S. Pedraz, Johana Panduro, Otmar Stahl, Guillem Anglada-Escudé, Peter H. Hauschildt, E. Solano, A. López-Comazzi, Ralf Launhardt, J. I. Vico Linares, E. Herrero, M. J. López-González, J. Kemmer, P. Schöfer, T. Stuber, A. Klutsch, J. H. M. M. Schmitt, S. Reinhardt, Manuel López-Puertas, M. Ammler-von Eiff, M. Lafarga, Manuel Perger, R. Hernández Arabí, M. R. Zapatero Osorio, J. Garcia de la Fuente, Hugo M. Tabernero, Priyanka Chaturvedi, Ulrich Grözinger, M. López del Fresno, Grzegorz Nowak, F. J. Alonso-Floriano, M. Brinkmöller, F. Labarga, Lluis Gesa, R. Calvo Ortega, L. M. Lara, Juan Pablo Pascual, Francesc Vilardell, M. C. Cárdenas Vázquez, Andreas Schweitzer, Denis Shulyak, Aviv Ofir, A. Rosich, J. Klüter, Alfredo Sota, Ernesto Sánchez-Blanco, Ignasi Ribas, M. Tala Pinto, A. Fernández-Martín, V. Casanova, Sebastian Schafer, Vianak Naranjo, P. Martín-Fernández, S. Czesla, I. Hermelo, P. Rhode, Hannu Parviainen, Karl Wagner, M. Kürster, Hubert Klahr, Juan Carlos Suárez, Florian Rodler, V. Wolthoff, P. Bluhm, Birgit Fuhrmeister, M. Llamas, Emilio Marfil, S. V. Jeffers, Philipp Huke, H. Magán Madinabeitia, Jose A. Caballero, R. Antona Jiménez, Fei Yan, S. Lalitha, C. del Burgo, E. Díez-Alonso, A. Rodríguez Trinidad, A. Pavlov, F. F. Bauer, J. Góngora Rueda, M. Azzaro, Jesus M. Carro, I. Gallardo Cava, L. F. Sarmiento, M. Kim, A. Guijarro, Susana Martín-Ruiz, M. L. García Vargas, M. A. Sánchez Carrasco, Sabine Reffert, Lisa Nortmann, Andreas Quirrenbach, A. Fukui, M. Cortés-Contreras, Pedro J. Amado, H. Anwand-Heerwart, Ricardo Dorda, F. J. Lázaro, A. P. Hatzes, F. Hernández Otero, Javier López-Santiago, Jesús Aceituno, E. Mirabet, D. Baroch, Mahmoudreza Oshagh, Ana Pérez-Calpena, J. B. P. Strachan, Juan Carlos Morales, Evangelos Nagel, Th. Henning, R. González-Peinado, J. Helmling, David Barrado, E. N. Johnson, S. Dreizler, Lev Tal-Or, Enric Palle, Víctor J. S. Béjar, M. Fernandez, J. Guàrdia, S. Stock, E. L. Martin, S. Becerril, D. Pérez Medialdea, Armin Huber, D. Hintz, L. Hernández Castaño, I. M. Ferro, M. Zechmeister, H. W. Rix, C. Cardona Guillén, Gilles Bergond, S. Sadegi, W. Xu, G. Veredas, A. Ramón Ballesta, B. Arroyo-Torres, R. P. Hedrosa, Rafael Rebolo, J. A. Marín Molina, A. Sánchez-López, Norio Narita, F. J. Aceituno, Ovidio Rabaza, J. I. González Hernández, A. Garcia-Piquer, M. E. Moreno-Raya, Rafael Luque, Paula Sarkis, J. Stürmer, Trifon Trifonov, P. Redondo, E. Gonzalez-Alvarez, E. Rodriguez, Ralf Klein, L. Mancini, Diana Kossakowski, D. Benítez, J. F. López Salas, D. Galadí-Enríquez, Josep Colomé, C. J. Marvin, E. de Juan, Z. M. Berdinas, D. Maroto Fernández, Ansgar Reiners, Carlos Cifuentes, Walter Seifert, Pilar Montañés-Rodríguez, Ulrich Mall, V. M. Passegger, A. Kaminski, L. Gonzalez-Cuesta, Holger Mandel, Miguel Abril, Max Planck Institute for Astronomy, CSIC - Instituto de Astrofísica de Andalucía (IAA), Landessternwarte Königstuhl, CSIC - Instituto de Ciencias del Espacio (ICE), Institute for Astrophysics in Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg Karl Schwarzschild-Observatorium, Instituto de Astrofísica de Canarias, Hamburg Observatory, Max Planck Society, Observatorio de Calar Alto, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Junta de Andalucía, German Research Foundation, German Centre for Air and Space Travel, European Research Council, CSIC-INTA - Centro de Astrobiología (CAB), Consejo Superior de Investigaciones Científicas (España), European Commission, Ministero dell'Istruzione, dell'Università e della Ricerca, Science and Technology Facilities Council (UK), Israel Science Foundation, Consejo Nacional de Ciencia y Tecnología (México), and Japan Society for the Promotion of Science

Subjects
Astrofísica, Brightness, 010504 meteorology & atmospheric sciences, individual: Teegarden’s Star [Stars], methods: data analysis, planetary systems, stars: late-type, stars: individual: Teegarden's Star, FOS: Physical sciences, Minimum mass, Stars: late-type, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, individual: Teegarden's Star [Stars], 0105 earth and related environmental sciences, Stars: individual: Teegarden's Star, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy, Astronomy and Astrophysics, Earth mass, Exoplanet, Radial velocity, Planetary systems, Slow rotation, 13. Climate action, Space and Planetary Science, late-type [Stars], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Teegarden's Star is the brightest and one of the nearest ultra-cool dwarfs in the solar neighbourhood. For its late spectral type (M7.0 V), the star shows relatively little activity and is a prime target for near-infrared radial velocity surveys such as CARMENES. Aims. As part of the CARMENES search for exoplanets around M dwarfs, we obtained more than 200 radial-velocity measurements of Teegarden's Star and analysed them for planetary signals. Methods. We find periodic variability in the radial velocities of Teegarden's Star. We also studied photometric measurements to rule out stellar brightness variations mimicking planetary signals. Results. We find evidence for two planet candidates, each with 1.1 M minimum mass, orbiting at periods of 4.91 and 11.4 d, respectively. No evidence for planetary transits could be found in archival and follow-up photometry. Small photometric variability is suggestive of slow rotation and old age. Conclusions. The two planets are among the lowest-mass planets discovered so far, and they are the first Earth-mass planets around an ultra-cool dwarf for which the masses have been determined using radial velocities.© ESO 2019., M.Z. acknowledges support from the Deutsche Forschungsgemeinschaft under DFG RE 1664/12-1 and Research Unit FOR2544 >Blue Planets around Red Stars>, project no. RE 1664/14-1. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain). CARMENES is funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, 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 Spanish Ministry of Economy, the German Science Foundation through the Major Research Instrumentation Programme and DFG 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. Based on data from the CARMENES data archive at CAB (INTA-CSIC). This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sanchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. Data were partly collected with the 150-cm and 90-cm telescopes at the Sierra Nevada Observatory (SNO) operated by the Instituto de Astrofisica de Andalucia (IAA-CSIC). Data were partly obtained with the MONET/South telescope of the MOnitoring NEtwork of Telescopes, funded by the Alfried Krupp von Bohlen und Halbach Foundation, Essen, and operated by the Georg-August-Universitat Gottingen, the McDonald Observatory of the University of Texas at Austin, and the South African Astronomical Observatory. We acknowledge financial support from the Spanish Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades and the European FEDER/ERF funds through projects AYA2015-69350-C3-2-P, AYA2016-79425-C3-1/2/3-P, AYA2018-84089, BES-2017-080769, BES-2017-082610, ESP2015-65712-C5-5-R, ESP2016-80435-C2-1/2-R, ESP2017-87143-R, ESP2017-87676-2-2, ESP2017-87676-C5-1/2/5-R, FPU15/01476, RYC-2012-09913, 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 through CERCA programme>, the Deutsches Zentrum fur Luft-und Raumfahrt through grants 50OW0204 and 50OO1501, the European Research Council through grant 6 94 513, the Italian Ministero dell'instruzione, dell'universita de della ricerca and Universita degli Studi di Roma Tor Vergata through FFABR 2017 and >Mission: Sustainability 2016>, the UK Science and Technology Facilities Council through grant ST/P000592/1, the Israel Science Foundation through grant 848/16, the Chilean CONICYT-FONDECYT through grant 31 80 405, the Mexican CONACYT through grant CVU 4 48 248, the JSPS KAKENHI through grants JP18H01265 and 18H05439, and the JST PRESTO through grant JPMJPR1775.

Published
2019

4. Keplerian disks and outflows in post-AGB stars: AC Herculis, 89 Herculis, IRAS 19125+0343, and R Scuti

Author

M. Gómez-Garrido, Javier Alcolea, Valentin Bujarrabal, H. Van Winckel, A. Castro-Carrizo, and I. Gallardo Cava

Subjects
FOS: Physical sciences, Binary number, Model fitting, Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, circumstellar matter, 01 natural sciences, general [binaries], 0103 physical sciences, general [planetary nebulae], 010303 astronomy & astrophysics, stars [radio lines], Solar and Stellar Astrophysics (astro-ph.SR), Physics, Nebula, Science & Technology, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, AGB and post-AGB [stars], Physics::History of Physics, interferometric [techniques], Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physical Sciences, Outflow, Mass fraction
Abstract

There is a class of binary post-AGB stars with a remarkable near-infrared excess that are surrounded by Keplerian or quasi-Keplerian disks and extended outflows composed of gas escaping from the disk. The Keplerian dynamics had been well identified in four cases, namely the Red Rectangle, AC Her, IW Car, and IRAS 08544-4431. In these objects, the mass of the outflow represents ~ 10 % of the nebular mass, the disk being the dominant component of the nebula. We present interferometric NOEMA maps of 12CO and 13CO J=2-1 in 89 Her and 12CO J=2-1 in AC Her, IRAS 19125+0343, and R Sct. Several properties of the nebula are obtained from the data and model fitting, including the structure, density, and temperature distributions, as well as the dynamics. We also discuss the uncertainties on the derived values. The presence of an expanding component in AC Her is doubtful, but thanks to new maps and models, we estimate an upper limit to the mass of this outflow of < 3 10^-5 Mo, that is, the mass of the outflow is < 5 % of the total nebular mass. For 89 Her, we find a total nebular mass of 1.4 10^-2 Mo, of which ~ 50 % comes from an hourglass-shaped extended outflow. In the case of IRAS 19125+0343, the nebular mass is 1.1 10^-2 Mo, where the outflow contributes ~ 70 % of the total mass. The nebular mass of R Sct is 3.2 10^-2 Mo, of which ~ 75 % corresponds to a very extended outflow that surrounds the disk. Our results for IRAS 19125+0343 and R Sct lead us to introduce a new subclass of binary post-AGB stars, for which the outflow is the dominant component of the nebula. Moreover, the outflow mass fraction found in AC Her is smaller than those found in other disk-dominated binary post-AGB stars. 89 Her would represent an intermediate case between both subclasses., Accepted 4 March 2021 in Astronomy & Astrophysics. 26 pages

Published
2021

5. 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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