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1. 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

2. He I λ 10 830 Å in the transmission spectrum of HD209458 b

Author

Th. Henning, S. Czesla, M. Lampón, F. J. Alonso-Floriano, Jorge Sanz-Forcada, Pedro J. Amado, Enric Palle, Jose A. Caballero, Víctor J. S. Béjar, A. Sánchez-López, F. F. Bauer, Lisa Nortmann, Andreas Quirrenbach, D. Montes, Manuel López-Puertas, M. R. Zapatero Osorio, Ansgar Reiners, J. H. M. M. Schmitt, L. M. Lara, M. Brinkmöller, M. Salz, A. P. Hatzes, Jesús Aceituno, Evangelos Nagel, Martin Kürster, Ignas Snellen, Guillem Anglada-Escudé, Adrian Kaminski, F. Labarga, Ignasi Ribas, 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, Alonso Floriano, F. J. [0000-0003-1202-5734], Ministerio de Economía y Competitividad (MINECO), Max-Planck-Gesellschaft (MPG), European Research Council (ERC), Comunidad de Madrid, Agencia Estatal de Investigación (AEI), Science & Technology Facility Council, ST/P000592/1, Spanish MCIU, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía CSIC, and European Commission (EC)

Subjects
Physics, Astrofísica, individual: HD 209458b [Planets and satellites], 010504 meteorology & atmospheric sciences, Absorption spectroscopy, Astronomy and Astrophysics, Astrophysics, planetary systems [Infrared], 01 natural sciences, Spectral line, spectroscopic [Techniques], Radial velocity, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, atmospheres [Planets and satellites], Transit (astronomy), Emission spectrum, Astrophysics::Earth and Planetary Astrophysics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

The error is an approximation obtained from the average transmission spectrum provided by Allart et al. (2018). Program H18-3.5-022, P.I: S. Czesla. After one year from the observation date, the reduced spectra can be downloaded from the Calar Alto archive, http://caha.sdc.cab.inta-csic.es/calto/ https://www.nist.gov/pml/atomic-spectra-database Context. Recently, the He I triplet at 10 830 Å was rediscovered as an excellent probe of the extended and possibly evaporating atmospheres of close-in transiting planets. This has already resulted in detections of this triplet in the atmospheres of a handful of planets, both from space and from the ground. However, while a strong signal is expected for the hot Jupiter HD 209458 b, only upper limits have been obtained so far. Aims. Our goal is to measure the helium excess absorption from HD 209458 b and assess the extended atmosphere of the planet and possible evaporation. Methods. We obtained new high-resolution spectral transit time-series of HD 209458 b using CARMENES at the 3.5 m Calar Alto telescope, targeting the He I triplet at 10 830 Å at a spectral resolving power of 80 400. The observed spectra were corrected for stellar absorption lines using out-of-transit data, for telluric absorption using the MOLECFIT software, and for the sky emission lines using simultaneous sky measurements through a second fibre. Results. We detect He I absorption at a level of 0.91 ± 0.10% (9 σ) at mid-transit. The absorption follows the radial velocity change of the planet during transit, unambiguously identifying the planet as the source of the absorption. The core of the absorption exhibits a net blueshift of 1.8 ± 1.3 km s−1. Possible low-level excess absorption is seen further blueward from the main absorption near the centre of the transit, which could be caused by an extended tail. However, this needs to be confirmed. Conclusions. Our results further support a close relation between the strength of planetary absorption in the helium triplet lines and the level of ionising, stellar X-ray, and extreme-UV irradiation. We thank P. Molliere and A. Wyttenbach for the nice scientific discussions during the preparation of this publication. F.J.A.-F. and I.S. acknowledge funding from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation programme under grant agreement No 694 513. 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 (MaxPlanck-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. Financial support was also provided by the Universidad Complutense de Madrid, the Comunidad Autonoma de Madrid, the Spanish Ministerios de Ciencia e Innovacion and of Economia y Competitividad, the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> and Science & Technology Facility Council Consolidated, and the Fondo Social Europeo. The corresponding funding grants are: ESP2014-54 362-P, ESP2014-54 062-R, AYA2015-69 350-C3-2-P, BES-2015-074542, AYA2016-79 425-C3-1/2/3-P, ESP2016-76 076-R, ESP2017-87 143-R, SEV-2017-0709, ST/P000592/1. Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia. We thank the anonymous referee for their insightful comments, which contributed to improve the quality of the manuscript; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). Peer review

Published
2019

3. The CARMENES search for exoplanets around M dwarfs: High-resolution optical and near-infrared spectroscopy of 324 survey stars

Author

S. Becerril, S. Reinhart, I. M. Ferro, Philipp Huke, E. Díez-Alonso, R. González-Peinado, M. Azzaro, Richard J. Mathar, Jose Antonio Pascual, A. Lamert, Javier López-Santiago, E. Mirabet, M. A. Sánchez Carrasco, Gilles Bergond, Ulrich Mall, D. Pérez Medialdea, Armin Huber, E. Herrero, E. Casal, S. V. Jeffers, Grzegorz Nowak, Sebastian Schafer, J. Helmling, S. Sadegi, H. Magán Madinabeitia, G. Veredas, M. Lampón, E. N. Johnson, W. Xu, Karl Wagner, M. L. García Vargas, David Barrado, J. H. M. M. Schmitt, Enric Palle, R. Oreiro, D. Baroch, B. Arroyo-Torres, Pedro J. Amado, C. Cifuentes, J. A. Marín Molina, D. Galadí-Enríquez, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, A. Rodríguez Trinidad, M. Lafarga, I. Hermelo, V. M. Passegger, H. W. Rix, H. Anwand-Heerwart, Juan Carlos Suárez, Florian Rodler, Martin Kürster, M. Kim, P. Schöfer, J. Klüter, M. Tala, R.-R. Rohloff, D. Benítez, Johana Panduro, Lisa Nortmann, Andreas Quirrenbach, Z. M. Berdiñas, J. Schiller, J. López-González, S. Czesla, P. Rhode, Adrian Kaminski, A. Pavlov, Holger Mandel, L. Hernández Castaño, J. I. Vico Linares, C. Feiz, Guillem Anglada-Escudé, L. F. Sarmiento, Susana Martín-Ruiz, Simon Tulloch, A. P. Hatzes, Jesús Aceituno, Eike W. Guenther, M. Pluto, Juan Carlos Morales, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, R. G. Ulbrich, Otmar Stahl, M. López del Fresno, Emilio Marfil, Reinhard Mundt, Lluis Gesa, Evangelos Nagel, Werner Laun, Josep Colomé, Francesc Vilardell, M. C. Cárdenas Vázquez, J. F. López Salas, Jose A. Caballero, M. Blümcke, A. Ramón, Aviv Ofir, E. de Guindos, Ana Pérez-Calpena, S. Pedraz, Ralf Launhardt, Rainer Lenzen, A. Claret, Sabine Reffert, U. Lemke, Luigi Mancini, J. B. P. Strachan, F. J. Alonso-Floriano, M. A. C. Perryman, Fei Yan, Mathias Zechmeister, Ernesto Sánchez-Blanco, Vianak Naranjo, A. Klutsch, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Ulrich Grözinger, Walter Seifert, V. Gómez Galera, Luisa Lara, R. P. Hedrosa, Rafael Rebolo, A. Guijarro, E. de Juan, A. Sánchez-López, Rafael Luque, M. Brinkmöller, Paula Sarkis, J. Stürmer, Ovidio Rabaza, J. I. González Hernández, C. del Burgo, A. Rosich, Andreas Schweitzer, D. Montes, Miguel Abril, M. E. Moreno-Raya, H. J. Hagen, S. Grohnert, Birgit Fuhrmeister, P. Redondo, F. F. Bauer, E. Rodriguez, Ralf Klein, R. Antona, A. Garcia-Piquer, J. Cano, Trifon Trifonov, A. Moya, Ansgar Reiners, Jorge Sanz-Forcada, Peter H. Hauschildt, E. Solano, J. Winkler, Manuel Perger, R. Hernández Arabí, Ignasi Ribas, C. J. Marvin, Th. Henning, V. Wolthoff, D. Maroto Fernández, Juan Gutiérrez-Soto, M. Cortés-Contreras, Eduardo L. Martín, Hugo M. Tabernero, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), German Centre for Air and Space Travel, European Research Council, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, and Astrofísica Estelar (AE)

Subjects
Astrofísica, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Stars: late-type, Astrophysics::Cosmology and Extragalactic Astrophysics, Stellar classification, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Settore FIS/05 - Astronomia e Astrofisica, Planet, law, low-mass [Stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Stars: low-mass, 010303 astronomy & astrophysics, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astronomía y Astrofísica, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Near-infrared spectroscopy, Stars: rotation, Astronomy and Astrophysics, Atlases, Catalogues, Exoplanet, Infrared: stars, Radial velocity, Astronomía, rotation [Stars], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, late-type [Stars], stars [Infrared], Astrophysics::Earth and Planetary Astrophysics, Catalogs, Astrophysics - Earth and Planetary Astrophysics
Abstract

The CARMENES radial velocity (RV) survey is observing 324 M dwarfs to search for any orbiting planets. In this paper, we present the survey sample by publishing one CARMENES spectrum for each M dwarf. These spectra cover the wavelength range 520¿1710 nm at a resolution of at least R >80 000, and we measure its RV, H¿ emission, and projected rotation velocity. We present an atlas of high-resolution M-dwarf spectra and compare the spectra to atmospheric models. To quantify the RV precision that can be achieved in low-mass stars over the CARMENES wavelength range, we analyze our empirical information on the RV precision from more than 6500 observations. We compare our high-resolution M-dwarf spectra to atmospheric models where we determine the spectroscopic RV information content, Q, and signal-to-noise ratio. We find that for all M-type dwarfs, the highest RV precision can be reached in the wavelength range 700¿900 nm. Observations at longer wavelengths are equally precise only at the very latest spectral types (M8 and M9). We demonstrate that in this spectroscopic range, the large amount of absorption features compensates for the intrinsic faintness of an M7 star. To reach an RV precision of 1 m s¿1 in very low mass M dwarfs at longer wavelengths likely requires the use of a 10 m class telescope. For spectral types M6 and earlier, the combination of a red visual and a near-infrared spectrograph is ideal to search for low-mass planets and to distinguish between planets and stellar variability. At a 4 m class telescope, an instrument like CARMENES has the potential to push the RV precision well below the typical jitter level of 3-4 m s-1. © ESO 2018., We thank an anonymous referee for prompt attention and helpful comments that helped to improve the quality of this paper. 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, Insitut 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. This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. We acknowledge the following funding programs: European Research Council (ERC-279347), Deutsche Forschungsgemeinschaft (RE 1664/12-1, RE 2694/4-1), Bundesministerium fur Bildung und Forschung (BMBF-05A14MG3, BMBF-05A17MG3), Spanish Ministry of Economy and Competitiveness (MINECO, grants AYA2015-68012-C2-2-P, AYA2016-79425-C3-1,2,3-P, AYA2015-69350-C3-2-P, AYA2014-54348-C03-01, AYA2014-56359-P, AYA2014-54348-C3-2R, AYA2016-79425-C3-3-P and 2013 Ramon y Cajal program RYC-2013-14875), Fondo Europeo de Desarrollo Regional (FEDER, grant ESP2016-80435-C2-1-R, ESP2015-65712-C5-5-R), Generalitat de Catalunya/CERCA programme, Spanish Ministerio de Educacion, Cultura y Deporte, programa de Formacion de Profesorado Universitario (grant FPU15/01476), Deutsches Zentrum fur Luft- und Raumfahrt (grants 50OW0204 and 50OO1501), Office of Naval Research Global (award no. N62909-15-1-2011), Mexican CONACyT grant CB-2012-183007.

Published
2018

4. CARMENES: high-resolution spectra and precise radial velocities in the red and infrared

Author

R. Gonzalez Peinado, Ralf Launhardt, Lluis Gesa, C. del Burgo, F. F. Bauer, M. Doellinger, R. P. Hedrosa, J. Carro, Jose A. Caballero, Z. M. Berdiñas, D. Montes, Ulrich Mall, M. Blümcke, M. Kehr, S. Schäfer, D. Pérez-Medialdea, M. Salz, Mercedes López-Morales, E. N. Johnson, V. Wolthoff, A. Rosich, Mathias Zechmeister, P. Redondo, E. Mirabet, E. Díez-Alonso, Johana Panduro, L. Hernández Castaño, P. Rhode, I. Hermelo, David Barrado, Enric Palle, Walter Seifert, Manuel Perger, Javier López-Santiago, D. Benítez, E. Herrero, S. Sabotta, Víctor J. S. Béjar, M. L. García-Vargas, S. Becerril, M. J. López González, Rainer Lenzen, Luigi Mancini, M. Lafarga, A. Kaminski, P. Schöfer, M. E. Moreno-Raya, R.-R. Rohloff, H. W. Rix, C. J. Marvin, Ignasi Ribas, R. Garrido, J. A. Marín Molina, D. Hermann, Emilio Marfil, J. H. M. M. Schmitt, M. Pluto, M. Cortés-Contreras, Reinhard Mundt, M. A. Sánchez Carrasco, L. González-Cuesta, Th. Henning, J. Klüter, M. Tala Pinto, D. Galadí-Enríquez, P. Huke, J. Pascual, M. López del Fresno, Grzegorz Nowak, Trifon Trifonov, M. Llamas, P. H. Hauschildt, G. Veredas, N. Lodieu, E. de Juan, J. B. P. Strachan, S. Sadegi, W. Xu, O. Herbort, E. de Guindos, J. Sanz-Forcada, M. Lampón, Michael Perryman, K. F. Huber, Josep Colomé, Denis Shulyak, M. Kim, J. Aceituno, Lisa Nortmann, Andreas Quirrenbach, Juan Carlos Suárez, C. Cardona Guillén, Ana Pérez-Calpena, A. Claret, Martin Kürster, Werner Laun, J. Cano, Lev Tal-Or, A. Garcia-Piquer, F. J. Alonso-Floriano, B. Arroyo-Torres, A. Klutsch, Hubert Klahr, H. Martínez-Rodríguez, Ulrich Grözinger, O. Stahl, S. Pedraz, S. Martin-Ruiz, M. Azzaro, J. L. Lizon, C. Feiz, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, Rafael Luque, I. Gallardo, Guillem Anglada-Escudé, L. Sairam, J. F. López Salas, H. Mandel, A. Ramón, D. Hidalgo, N. Labiche, J. Guàrdia, F. Hernández Hernando, U. Lemke, Francesc Vilardell, E. González-Álvarez, J. Stürmer, Hugo M. Tabernero, G. Bergondy, R. Hernández Arabí, Vianak Naranjo, J. Winkler, Armin Huber, Fei Yan, B. Fuhrmeister, Rafael Rebolo, Simon Tulloch, Ansgar Reiners, F. J. Lázaro, A. P. Hatzes, H. Magán Madinabeitia, Paula Sarkis, J. Helmling, Z. Zhao, Sabine Reffert, E. Casal, A. Sánchez-López, M. C. Gálvez-Ortiz, J. I. González Hernández, D. Hintz, D. Baroch, A. Lamert, E. L. Martín, A. Schweitzer, Evangelos Nagel, V. Gómez Galera, M. Fernández, A. Guijarro, C. Cifuentes, E. Sánchez-Blanco, R. G. Ulbrich, Carlo Schmidt, F. Labarga, Pedro J. Amado, V. M. Passegger, F. J. Abellán, S. Grohnert, F. Rodler, Ricardo Dorda, Clemens Storz, G. Gaisné, K. Frölich, A. Moya, Juan Carlos Morales, E. W. Guenther, E. Rodriguez, H. J. Hagen, Ralf Klein, D. Maroto Fernández, I. M. Ferro, Karl Wagner, L. M. Lara, S. Dreizler, S. Czesla, M. Brinkmöller, M. C. Cardenas, Enrique Solano, M. Vidal-Dasilva, C. Rodríguez López, M. Abril, G. Holgado, J. Schiller, L. F. Sarmiento, A. Pavlov, H. Anwand-Heerwart, S. V. Jeffers, S. Reinhart, J. L. Vico Linares, and Richard J. Mathar

Subjects
Astrofísica, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 010309 optics, Planet, Spectrographs, Cool Stars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), M Dwarfs, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Optical Instrumentation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Extrasolar Planets, Exoplanet, Radial velocity, Stars, 13. Climate action, Terrestrial planet, Spectral atlas, Astrophysics::Earth and Planetary Astrophysics, Circumstellar habitable zone, Near-Infrared Instrumentation
Abstract

The design and construction of CARMENES has been presented at previous SPIE conferences. It is a next-generation radial-velocity instrument at the 3.5m telescope of the Calar Alto Observatory, which was built by a consortium of eleven Spanish and German institutions. CARMENES consists of two separate échelle spectrographs covering the wavelength range from 0.52 to 1.71¿m at a spec-tral resolution of R < 80,000, fed by fibers from the Cassegrain focus of the telescope. CARMENES saw ¿First Light¿ on Nov 9, 2015. During the commissioning and initial operation phases, we established basic performance data such as throughput and spectral resolution. We found that our hollow-cathode lamps are suitable for precise wavelength calibration, but their spectra contain a number of lines of neon or argon that are so bright that the lamps cannot be used in simultaneous exposures with stars. We have therefore adopted a calibration procedure that uses simultaneous star / Fabry Pérot etalon exposures in combination with a cross-calibration between the etalons and hollow-cathode lamps during daytime. With this strategy it has been possible to achieve 1-2 m/s precision in the visible and 5-10 m/s precision in the near-IR; further improvements are expected from ongoing work on temperature control, calibration procedures and data reduction. Comparing the RV precision achieved in different wavelength bands, we find a ¿sweet spot¿ between 0.7 and 0.8¿m, where deep TiO bands provide rich RV information in mid-M dwarfs. This is in contrast to our pre-survey models, which predicted comparatively better performance in the near-IR around 1¿m, and explains in part why our near-IR RVs do not reach the same precision level as those taken with the visible spectrograph. We are now conducting a large survey of 340 nearby M dwarfs (with an average distance of only 12pc), with the goal of finding terrestrial planets in their habitable zones. We have detected the signatures of several previously known or suspected planets and also discovered several new planets. We find that the radial velocity periodograms of many M dwarfs show several significant peaks. The development of robust methods to distinguish planet signatures from activity-induced radial velocity jitter is therefore among our priorities. Due to its large wavelength coverage, the CARMENES survey is generating a unique data set for studies of M star atmospheres, rotation, and activity. The spectra cover important diagnostic lines for activity (H alpha, Na I D1 and D2, and the Ca II infrared triplet), as well as FeH lines, from which the magnetic field can be inferred. Correlating the time series of these features with each other, and with wavelength-dependent radial velocities, provides excellent handles for the discrimination between planetary companions and stellar radial velocity jitter. These data are also generating new insight into the physical properties of M dwarf atmospheres, and the impact of activity and flares on the habitability of M star planets. © 2018 SPIE., 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, Insitut 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 Science, the German Science Foundation through the Major Research Instrumentation Program 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.

Published
2018

5. CARMENES: an overview six months after first light

Author

E. de Juan, Ignasi Ribas, R.-R. Rohloff, D. Benítez, A. Lamert, Th. Henning, P. Rhode, Karl Wagner, Josep Colomé, Sebastian Schafer, M. Cortés-Contreras, R. G. Ulbrich, F. J. Alonso-Floriano, R. Gonzalez Peinado, Simon Tulloch, H. Anwand-Heerwart, Juan Carlos Suárez, Florian Rodler, M. C. Gálvez-Ortiz, Hugo M. Tabernero, A. P. Hatzes, Jesús Aceituno, Birgit Fuhrmeister, Clemens Storz, R. Morales Muñoz, Ana Pérez-Calpena, J. Schiller, M. Llamas, Evangelos Nagel, Mercedes Lopez-Morales, Sabine Reffert, A. Garcia-Piquer, F. F. Bauer, E. Rodriguez, Ulrich Mall, Eike W. Guenther, Holger Mandel, A. Claret, Ralf Klein, Ralf Launhardt, A. Quirrenbach, P. Schöfer, David Barrado, Javier López-Santiago, E. Mirabet, Jorge Sanz-Forcada, Enric Palle, U. Lemke, V. M. Passegger, Stefan Dreizler, Víctor J. S. Béjar, J. Stürmer, C. Rodríguez López, Werner Laun, Grzegorz Nowak, M. Lafarga, Peter H. Hauschildt, E. Solano, J. Winkler, K. F. Huber, Rafael Rebolo, M. Kehr, M. C. Cardenas, D. Galadí, J. F. López Salas, A. Ramón, Manuel Perger, R. Hernández Arabí, E. de Guindos, J. Klüter, M. Tala, A. Rosich, Armin Huber, Paula Sarkis, Miguel Abril, S. Pedraz, V. Gómez Galera, Susana Martín-Ruiz, C. Feiz, C. del Burgo, M. Doellinger, Adrian Kaminski, M. L. García-Vargas, P. Redondo, M. Pluto, D. Montes, Ansgar Reiners, S. Becerril, C. J. Marvin, C. Schmidt, Mathias Zechmeister, Philipp Huke, J. I. González Hernández, I. M. Ferro, D. Maroto Fernández, Walter Seifert, H. W. Rix, Martin Kürster, M. Azzaro, Trifon Trifonov, I. Gallardo, Guillem Anglada-Escudé, Z. M. Berdiñas, M. A. Sánchez Carrasco, A. Pavlov, Sandra V. Jeffers, M. Brinkmöller, J. Helmling, L. F. Sarmiento, W. Xu, Andreas Schweitzer, A. Klutsch, Ulrich Grözinger, J. H. M. M. Schmitt, R. Garrido, H. J. Hagen, H. Magán Madinabeitia, S. Reinhart, L. M. Lara, Richard J. Mathar, Pedro J. Amado, Juan Carlos Morales, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Johana Panduro, D. Hermann, Otmar Stahl, Luigi Mancini, E. L. Martin, L. Hernández Castaño, Denis Shulyak, M. A. C. Perryman, J. B. P. Strachan, J. L. Lizon, Manuel López-Puertas, M. Ammler-von Eiff, S. Czesla, M. R. Zapatero Osorio, Ernesto Sánchez-Blanco, J. I. Vico Linares, Lluis Gesa, Vianak Naranjo, Jose A. Caballero, M. López del Fresno, Reinhard Mundt, Francesc Vilardell, Aviv Ofir, D. Pérez-Medialdea, E. Herrero, E. Casal, G. Veredas, J. A. Marín Molina, M. Kim, Rainer Lenzen, and Enrique Pérez

Subjects
Astrofísica, Physics, Instrument control, Astronomy, First light, 01 natural sciences, Exoplanet, law.invention, Astronomía, 010309 optics, Telescope, Observatory, law, 0103 physical sciences, Interlock, 010303 astronomy & astrophysics, Spectrograph, Data reduction, Remote sensing
Abstract

The CARMENES instrument is a pair of high-resolution (R greater than or similar to 80, 000) spectrographs covering the wavelength range from 0.52 to 1.71 mu m, optimized for precise radial velocity measurements. It was installed and commissioned at the 3.5 m telescope of the Calar Alto observatory in Southern Spain in 2015. The first large science program of CARMENES is a survey of similar to 300 M dwarfs, which started on Jan 1, 2016. We present an overview of all subsystems of CARMENES (front end, fiber system, visible-light spectrograph, near-infrared spectrograph, calibration units, etalons, facility control, interlock system, instrument control system, data reduction pipeline, data flow, and archive), and give an overview of the assembly, integration, verification, and commissioning phases of the project. We show initial results and discuss further plans for the scientific use of CARMENES.

Published
2016

6. 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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7. The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems

Author

E. de Juan, Ralf Launhardt, M. Zechmeister, P. Rhode, Birgit Fuhrmeister, E. Díez-Alonso, Rafael Luque, H. J. Hagen, David Barrado, H. W. Rix, Ignasi Ribas, J. F. López Salas, L. M. Lara, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, F. F. Bauer, Paula Sarkis, J. Stürmer, C. J. Marvin, Ovidio Rabaza, J. I. González Hernández, V. Wolthoff, Grzegorz Nowak, Jose Antonio Pascual, P. Schöfer, D. Maroto Fernández, Richard J. Mathar, Juan Gutiérrez-Soto, M. Cortés-Contreras, A. Claret, A. Kaminski, S. Grohnert, M. Lafarga, Walter Seifert, A. Guijarro, Susana Martín-Ruiz, I. Hermelo, A. Rosich, S. Sadegi, W. Xu, Holger Mandel, C. del Burgo, S. V. Jeffers, H. Magán Madinabeitia, Jorge Sanz-Forcada, M. Pluto, R.-R. Rohloff, D. Benítez, J. Klüter, M. Tala, Eike W. Guenther, D. Galadí-Enríquez, D. Montes, Ana Pérez-Calpena, Josep Colomé, Peter H. Hauschildt, M. Brinkmöller, Werner Laun, C. Feiz, A. Pavlov, E. Solano, J. Winkler, Eduardo L. Martín, Hugo M. Tabernero, U. Lemke, Ulrich Mall, Andreas Schweitzer, Manuel Perger, R. Hernández Arabí, Miguel Abril, A. Ramón, E. de Guindos, L. F. Sarmiento, Simon Tulloch, Karl Wagner, S. Pedraz, Fei Yan, J. B. P. Strachan, R. P. Hedrosa, A. P. Hatzes, Jesús Aceituno, P. Redondo, Guillem Anglada-Escudé, Johana Panduro, Rafael Rebolo, R. Oreiro, Philipp Huke, A. Sánchez-López, E. Rodriguez, E. Herrero, Evangelos Nagel, V. Gómez Galera, V. M. Passegger, Ralf Klein, M. E. Moreno-Raya, Otmar Stahl, H. Anwand-Heerwart, M. Azzaro, E. Casal, Luigi Mancini, M. A. C. Perryman, M. A. Sánchez Carrasco, J. Schiller, J. H. M. M. Schmitt, S. Reinhardt, M. Lampón, Z. M. Berdiñas, B. Arroyo-Torres, A. Klutsch, Ulrich Grözinger, S. Czesla, J. I. Vico Linares, M. J. López-González, M. López del Fresno, Reinhard Mundt, Sebastian Schafer, L. Hernández Castaño, Juan Carlos Suárez, Florian Rodler, D. Baroch, Lluis Gesa, Jose A. Caballero, M. Kürster, M. Blümcke, Emilio Marfil, Gilles Bergond, G. Veredas, C. Cifuentes, J. A. Marín Molina, F. J. Alonso-Floriano, Ernesto Sánchez-Blanco, S. Becerril, I. M. Ferro, Vianak Naranjo, Javier López-Santiago, E. Mirabet, J. Helmling, E. N. Johnson, Ansgar Reiners, R. Antona, M. L. García Vargas, A. Garcia-Piquer, Pedro J. Amado, A. Rodríguez Trinidad, J. Cano, M. Kim, Juan Carlos Morales, Trifon Trifonov, Lisa Nortmann, Andreas Quirrenbach, A. Moya, Th. Henning, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, Manuel López-Puertas, M. Ammler-von Eiff, M. R. Zapatero Osorio, Francesc Vilardell, M. C. Cárdenas Vázquez, Aviv Ofir, Rainer Lenzen, R. González-Peinado, Sabine Reffert, D. Pérez Medialdea, Armin Huber, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, German Research Foundation, Junta de Andalucía, Universidad Complutense de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), Comisión Nacional de Investigación Científica y Tecnológica (Chile), and German Centre for Air and Space Travel

Subjects
Astrofísica, FOS: Physical sciences, Context (language use), Stars: late-type, Astrophysics, 7. Clean energy, 01 natural sciences, Settore FIS/05 - Astronomia e Astrofisica, low-mass [Stars], Planet, 0103 physical sciences, Stars: low-mass, 010303 astronomy & astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Orbital elements, Physics, Planets and satellites: dynamical evolution and stability, 010308 nuclear & particles physics, Astronomy and Astrophysics, Planetary system, dynamical evolution and stability [Planets and satellites], Exoplanet, Radial velocity, Astronomía, Planetary systems, Stars, 13. Climate action, Space and Planetary Science, late-type [Stars], Terrestrial planet, Astrophysics - Earth and Planetary Astrophysics
Abstract

The appendix tables are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/609/A117, Context. The main goal of the CARMENES survey is to find Earth-mass planets around nearby M-dwarf stars. Seven M dwarfs included in the CARMENES sample had been observed before with HIRES and HARPS and either were reported to have one short period planetary companion (GJ 15 A, GJ 176, GJ 436, GJ 536 and GJ 1148) or are multiple planetary systems (GJ 581 and GJ 876). Aims. We aim to report new precise optical radial velocity measurements for these planet hosts and test the overall capabilities of CARMENES. Methods. We combined our CARMENES precise Doppler measurements with those available from HIRES and HARPS and derived new orbital parameters for the systems. Bona-fide single planet systems were fitted with a Keplerian model. The multiple planet systems were analyzed using a self-consistent dynamical model and their best fit orbits were tested for long-term stability. Results. We confirm or provide supportive arguments for planets around all the investigated stars except for GJ 15 A, for which we find that the post-discovery HIRES data and our CARMENES data do not show a signal at 11.4 days. Although we cannot confirm the super-Earth planet GJ 15 Ab, we show evidence for a possible long-period (P = 7030 d) Saturn-mass (msini = 51.8M) planet around GJ 15 A. In addition, based on our CARMENES and HIRES data we discover a second planet around GJ 1148, for which we estimate a period P = 532.6 days, eccentricity e = 0.342 and minimum mass msini = 68.1M. Conclusions. The CARMENES optical radial velocities have similar precision and overall scatter when compared to the Doppler measurements conducted with HARPS and HIRES. We conclude that CARMENES is an instrument that is up to the challenge of discovering rocky planets around low-mass stars.© ESO, 2018., 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, Insitut 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 (DFG), the Klaus Tschira Stiftung, the states of Baden-Wurttemberg and Niedersachsen, the DFG Research Unit FOR2544 >Blue Planets around Red Stars>, and by the Junta de Andalucia. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work used the Systemic Console package (Meschiari et al. 2009) for cross-checking our Keplerian and Dynamical fits and the python package astroML (VanderPlas et al. 2012) for the calculation of the GLS periodogram. The IEEC-CSIC team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grant ESP2016-80435-C2-1-R, as well as the support of the Generalitat de Catalunya/CERCA programme. The IAA-CSIC team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) through grants AYA2014-54348-C03-01 and AYA2016-79425-C3-3-P as well as FEDER funds. The UCM team acknowledges support by the Spanish Ministry of Economy and Competitiveness (MINECO) from projects AYA2015-68012-C2-2-P and AYA2016-79425- C3-1,2,3-P and the Spanish Ministerio de Educacion, Cultura y Deporte, programa de Formacion de Profesorado Universitario, under grant FPU15/01476. T. T. and M.K. thank to Jan Rybizki for the very helpful discussion in the early phases of this work. V.J.S.B. is supported by grant AYA2015-69350-C3-2-P from the Spanish Ministry of Economy and Competiveness (MINECO). J.C.S. acknowledges funding support from Spanish public funds for research under project ESP2015-65712-C5-5-R (MINECO/FEDER), and under Research Fellowship program >Ramon y Cajal> with reference RYC2012-09913 (MINECO/FEDER). The contributions of M.A. were supported by DLR (Deutsches Zentrum fur Luft- und Raumfahrt) through the grants 50OW0204 and 50OO1501. J.L.-S. acknowledges the Office of Naval Research Global (award No. N62909-15- 1-2011) for support. C.d.B. acknowledges that this work has been supported by Mexican CONACyT research grant CB-2012-183007 and the Spanish Ministry of Economy and Competitivity through projects AYA2014-54348-C3-2-R. J.I.G.H., and R.R. acknowledge financial support from the Spanish Ministry project MINECO AYA2014-56359-P. J.I.G.H. also acknowledges financial support from the Spanish MINECO under the 2013 Ramon y Cajal program MINECO RYC-2013-14875. V. Wolthoff acknowledges funding from the DFG Research Unit FOR2544 >Blue Planets around Red Stars>, project No. RE 2694/4-1.We thank the anonymous referee for the excellent comments that helped to improve the quality of this paper.

8. The CARMENES search for exoplanets around M dwarfs - HD 147379b: A nearby Neptune in the temperate zone of an early-M dwarf

Author

Lluis Gesa, A. Lamert, Jose A. Caballero, Fei Yan, M. Blümcke, Karl Wagner, J. H. M. M. Schmitt, E. de Juan, E. Casal, V. Gómez Galera, Simon Tulloch, R. Oreiro, David Barrado, P. Schöfer, M. Lampón, Eike W. Guenther, A. P. Hatzes, Jesús Aceituno, A. Rosich, Rainer Lenzen, Enric Palle, Stefan Dreizler, Cristina Rodríguez-López, Víctor J. S. Béjar, B. Arroyo-Torres, H. Anwand-Heerwart, U. Lemke, J. B. P. Strachan, Miguel Abril, J. Schiller, J. Helmling, Evangelos Nagel, M. Lafarga, E. N. Johnson, Walter Seifert, R. P. Hedrosa, Rafael Rebolo, A. Guijarro, Sebastian Schafer, C. del Burgo, J. Klüter, M. Tala, S. Czesla, M. E. Moreno-Raya, A. Sánchez-López, Grzegorz Nowak, D. Montes, F. Labarga, L. Hernández Castaño, Juan Carlos Suárez, A. Claret, Ulrich Mall, J. F. López Salas, J. I. Vico Linares, E. Herrero, Florian Rodler, Manuel López-Puertas, M. Ammler-von Eiff, D. Baroch, Philipp Huke, R. González-Peinado, C. Feiz, M. J. López-González, S. V. Jeffers, S. Becerril, H. Magán Madinabeitia, I. M. Ferro, M. Brinkmöller, P. Rhode, M. R. Zapatero Osorio, I. Hermelo, Francesc Vilardell, C. J. Marvin, Ralf Launhardt, Gilles Bergond, M. López del Fresno, Reinhard Mundt, M. Zechmeister, Jorge Sanz-Forcada, M. C. Cárdenas Vázquez, G. Veredas, D. Pérez Medialdea, Aviv Ofir, Andreas Schweitzer, Armin Huber, Ansgar Reiners, R. Antona, A. Garcia-Piquer, Ana Pérez-Calpena, D. Maroto Fernández, D. Galadí-Enríquez, S. Reinhart, R. G. Ulbrich, H. W. Rix, Javier López-Santiago, E. Mirabet, C. Cifuentes, Johana Panduro, L. M. Lara, J. A. Marín Molina, A. Pavlov, M. Azzaro, M. A. Sánchez Carrasco, Susana Martín-Ruiz, Birgit Fuhrmeister, V. M. Passegger, A. Kaminski, M. Pluto, Richard J. Mathar, F. F. Bauer, Otmar Stahl, L. F. Sarmiento, Z. M. Berdiñas, Eduardo L. Martín, Hugo M. Tabernero, A. Rodríguez Trinidad, M. Kim, Peter H. Hauschildt, E. Solano, J. Winkler, Manuel Perger, R. Hernández Arabí, J. Cano, Lisa Nortmann, Andreas Quirrenbach, Trifon Trifonov, A. Klutsch, Ulrich Grözinger, S. Sadegi, Luigi Mancini, A. Moya, Holger Mandel, Ovidio Rabaza, Werner Laun, M. A. C. Perryman, J. I. González Hernández, W. Xu, F. J. Alonso-Floriano, A. Ramón, Ignasi Ribas, Ernesto Sánchez-Blanco, E. de Guindos, S. Pedraz, Vianak Naranjo, Sabine Reffert, M. Kürster, V. Wolthoff, H. J. Hagen, Emilio Marfil, Juan Gutiérrez-Soto, E. Díez-Alonso, M. Cortés-Contreras, Jose Antonio Pascual, Guillem Anglada-Escudé, Rafael Luque, Paula Sarkis, J. Stürmer, P. Redondo, S. Grohnert, E. Rodriguez, Ralf Klein, R.-R. Rohloff, D. Benítez, Josep Colomé, Th. Henning, Lev Tal-Or, M. Fernandez, J. Guàrdia, F. Hernández Hernando, M. L. García Vargas, Pedro J. Amado, Juan Carlos Morales, Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), Ministry of Science, Research and Art Baden-Württemberg, Comisión Nacional de Investigación Científica y Tecnológica (Chile), German Centre for Air and Space Travel, European Research Council, and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
Rotation period, Stars: activity, Astrofísica, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Stars: late-type, 01 natural sciences, Planets and satellites: individual: HD 147379 b, Settore FIS/05 - Astronomia e Astrofisica, Neptune, Planet, low-mass [Stars], 0103 physical sciences, Stars: low-mass, Eccentricity (behavior), individual: HD 147379 [Stars], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stars: rotation, Stars: individual: HD 147379, Astronomy and Astrophysics, Exoplanet, individual: HD147379 [Stars], Radial velocity, Astronomía, rotation [Stars], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], individual: HD147379 b [Planets and satellites], individual: HD 147379 b [Planets and satellites], activity [Stars], Astrophysics - Earth and Planetary Astrophysics
Abstract

We report on the first star discovered to host a planet detected by radial velocity (RV) observations obtained within the CARMENES survey for exoplanets around M dwarfs. HD 147379 (V = 8.9 mag, M = 0.58 ± 0.08 M⊙), a bright M0.0 V star at a distance of 10.7 pc, is found to undergo periodic RV variations with a semi-amplitude of K = 5.1 ± 0.4 m s−1 and a period of P = 86.54 ± 0.06 d. The RV signal is found in our CARMENES data, which were taken between 2016 and 2017, and is supported by HIRES/Keck observations that were obtained since 2000. The RV variations are interpreted as resulting from a planet of minimum mass mP sin i = 25 ± 2 M⊕, 1.5 times the mass of Neptune, with an orbital semi-major axis a = 0.32 au and low eccentricity (e < 0.13). HD 147379 b is orbiting inside the temperate zone around the star, where water could exist in liquid form. The RV time-series and various spectroscopic indicators show additional hints of variations at an approximate period of 21.1 d (and its first harmonic), which we attribute to the rotation period of the star., FEDER/ERF FICTS-2011-02 funds, Major Research Instrumentation Programme and DFG Research Unit FOR2544 “Blue Planets around Red Stars, European Research Council (ERC-279347), Deutsche Forschungsgemeinschaft (RE 1664/12-1, RE 2694/4-1), Bundesministerium für Bildung und Forschung (BMBF-05A14MG3, BMBF-05A17MG3), Spanish Ministry of Economy and Competitiveness (MINECO, grants AYA2015-68012-C2-2-P, AYA2016-79425-C3-1,2,3-P, AYA2015-69350-C3-2-P, AYA2014-54348-C03- 01, AYA2014-56359-P, AYA2014-54348-C3-2-R, AYA2016-79425-C3-3-P and 2013 Ramòn y Cajal program RYC-2013-14875), Fondo Europeo de Desarrollo Regional (FEDER, grant ESP2016-80435-C2-1-R, ESP2015-65712-C5- 5-R), Generalitat de Catalunya/CERCA programme, Spanish Ministerio de Educación, Cultura y Deporte, programa de Formación de Profesorado Universitario (grant FPU15/01476), Deutsches Zentrum für Luft- und Raumfahrt (grants 50OW0204 and 50OO1501), Office of Naval Research Global (award no. N62909-15-1-2011), Mexican CONACyT grant CB-2012-183007.

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

Author

Morales JC, Mustill AJ, Ribas I, Davies MB, Reiners A, Bauer FF, Kossakowski D, Herrero E, Rodríguez E, López-González MJ, Rodríguez-López C, Béjar VJS, González-Cuesta L, Luque R, Pallé E, Perger M, Baroch D, Johansen A, Klahr H, Mordasini C, Anglada-Escudé G, Caballero JA, Cortés-Contreras M, Dreizler S, Lafarga M, Nagel E, Passegger VM, Reffert S, Rosich A, Schweitzer A, Tal-Or L, Trifonov T, Zechmeister M, Quirrenbach A, Amado PJ, Guenther EW, Hagen HJ, Henning T, Jeffers SV, Kaminski A, Kürster M, Montes D, Seifert W, Abellán FJ, Abril M, Aceituno J, Aceituno FJ, Alonso-Floriano FJ, Ammler-von Eiff M, Antona R, Arroyo-Torres B, Azzaro M, Barrado D, Becerril-Jarque S, Benítez D, Berdiñas ZM, Bergond G, Brinkmöller M, Del Burgo C, Burn R, Calvo-Ortega R, Cano J, Cárdenas MC, Guillén CC, Carro J, Casal E, Casanova V, Casasayas-Barris N, Chaturvedi P, Cifuentes C, Claret A, Colomé J, Czesla S, Díez-Alonso E, Dorda R, Emsenhuber A, Fernández M, Fernández-Martín A, Ferro IM, Fuhrmeister B, Galadí-Enríquez D, Cava IG, Vargas MLG, Garcia-Piquer A, Gesa L, González-Álvarez E, Hernández JIG, González-Peinado R, Guàrdia J, Guijarro A, de Guindos E, Hatzes AP, Hauschildt PH, Hedrosa RP, Hermelo I, Arabi RH, Otero FH, Hintz D, Holgado G, Huber A, Huke P, Johnson EN, de Juan E, Kehr M, Kemmer J, Kim M, Klüter J, Klutsch A, Labarga F, Labiche N, Lalitha S, Lampón M, Lara LM, Launhardt R, Lázaro FJ, Lizon JL, Llamas M, Lodieu N, López Del Fresno M, Salas JFL, López-Santiago J, Madinabeitia HM, Mall U, Mancini L, Mandel H, Marfil E, Molina JAM, Martín EL, Martín-Fernández P, Martín-Ruiz S, Martínez-Rodríguez H, Marvin CJ, Mirabet E, Moya A, Naranjo V, Nelson RP, Nortmann L, Nowak G, Ofir A, Pascual J, Pavlov A, Pedraz S, Medialdea DP, Pérez-Calpena A, Perryman MAC, Rabaza O, Ballesta AR, Rebolo R, Redondo P, Rix HW, Rodler F, Trinidad AR, Sabotta S, Sadegi S, Salz M, Sánchez-Blanco E, Carrasco MAS, Sánchez-López A, Sanz-Forcada J, Sarkis P, Sarmiento LF, Schäfer S, Schlecker M, Schmitt JHMM, Schöfer P, Solano E, Sota A, Stahl O, Stock S, Stuber T, Stürmer J, Suárez JC, Tabernero HM, Tulloch SM, Veredas G, Vico-Linares JI, Vilardell F, Wagner K, Winkler J, Wolthoff V, Yan F, and Osorio MRZ

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. No claim to original U.S. Government Works.)

Published
2019
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