Persona: Caballero, Jose A.
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Centro de Astrobiologia
El Centro de Astrobiología (CAB) es un centro mixto de investigación en astrobiología, dependiente tanto del Instituto Nacional de Técnica Aeroespacial (INTA) como del Consejo Superior de Investigaciones Científicas (CSIC).
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Caballero
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Jose A.
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Publicación Acceso Abierto The 10 parsec sample in the Gaia era(EDP Sciences, 2021-06-30) Reylé, C.; Jardine, K.; Fouqué, P.; Caballero, Jose A.; Smart, R. L.; Sozzetti, A.; Agencia Estatal de Investigación (AEI); Agenzia Spaziale Italiana (ASI); Istituto Nazionale di Astrofisica (INAF); Reylé, C. [0000-0003-2258-2403]; Jardine, K. [0000-0001-6068-2734]; Fouqué, P. [0000-0002-1436-7351]; Caballero, J. A. [0000-0002-7349-1387]; Sozzetti, A. [0000-0002-7504-365X]Context. The nearest stars provide a fundamental constraint for our understanding of stellar physics and the Galaxy. The nearby sample serves as an anchor where all objects can be seen and understood with precise data. This work is triggered by the most recent data release of the astrometric space mission Gaia and uses its unprecedented high precision parallax measurements to review the census of objects within 10 pc. Aims. The first aim of this work was to compile all stars and brown dwarfs within 10 pc observable by Gaia and compare it with the Gaia Catalogue of Nearby Stars as a quality assurance test. We complement the list to get a full 10 pc census, including bright stars, brown dwarfs, and exoplanets. Methods. We started our compilation from a query on all objects with a parallax larger than 100 mas using the Set of Identifications, Measurements, and Bibliography for Astronomical Data database (SIMBAD). We completed the census by adding companions, brown dwarfs with recent parallax measurements not in SIMBAD yet, and vetted exoplanets. The compilation combines astrometry and photometry from the recent Gaia Early Data Release 3 with literature magnitudes, spectral types, and line-of-sight velocities. Results. We give a description of the astrophysical content of the 10 pc sample. We find a multiplicity frequency of around 27%. Among the stars and brown dwarfs, we estimate that around 61% are M stars and more than half of the M stars are within the range from M3.0 V to M5.0 V. We give an overview of the brown dwarfs and exoplanets that should be detected in the next Gaia data releases along with future developments. Conclusions. We provide a catalogue of 540 stars, brown dwarfs, and exoplanets in 339 systems, within 10 pc from the Sun. This list is as volume-complete as possible from current knowledge and it provides benchmark stars that can be used, for instance, to define calibration samples and to test the quality of the forthcoming Gaia releases. It also has a strong outreach potential.Publicación Acceso Abierto A super-Earth on a close-in orbit around the M1V star GJ 740 A HADES and CARMENES collaboration(EDP Sciences, 2021-04-07) Toledo Padrón, B.; Suárez Mascareño, A.; González Hernández, J. I.; Rebolo, R.; Pinamonti, M.; Perger, M.; Scandariato, G.; Damasso, M.; Sozzetti, A.; Moldonado, J.; Desidera, S.; Ribas, I.; Micela, G.; Affer, L.; González Álvarez, E.; Leto, G.; Pagano, I.; Zanmar Sánchez, R.; Giacobbe, P.; Herrero, Enrique; Morales, J. C.; Amado, P. J.; Caballero, Jose A.; Quirrenbach, A.; Reiners, A.; Zechmeister, M.; Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Generalitat de CatalunyaContext. M-dwarfs have proven to be ideal targets for planetary radial velocity (RV) searches due to their higher planet-star mass contrast, which favors the detection of low-mass planets. The abundance of super-Earth and Earth-like planets detected around this type of star motivates further such research on hosts without reported planetary companions. Aims. The HADES and CARMENES programs are aimed at carrying out extensive searches of exoplanetary systems around M-type stars in the northern hemisphere, allowing us to address, in a statistical sense, the properties of the planets orbiting these objects. In this work, we perform a spectroscopic and photometric study of one of the program stars (GJ 740), which exhibits a short-period RV signal that is compatible with a planetary companion. Methods. We carried out a spectroscopic analysis based on 129 HARPS-N spectra taken over a time span of 6 yr combined with 57 HARPS spectra taken over 4 yr, as well as 32 CARMENES spectra taken during more than 1 yr, resulting in a dataset with a time coverage of 10 yr. We also relied on 459 measurements from the public ASAS survey with a time-coverage of 8 yr, along with 5 yr of photometric magnitudes from the EXORAP project taken in the V, B, R, and I filters to carry out a photometric study. Both analyses were made using Markov chain Monte Carlo simulations and Gaussian process regression to model the activity of the star. Results. We present the discovery of a short-period super-Earth with an orbital period of 2.37756−0.00011+0.00013 d and a minimum mass of 2.96−0.48+0.50 M⊕. We offer an update to the previously reported characterization of the magnetic cycle and rotation period of the star, obtaining values of Prot = 35.563 ± 0.071 d and Pcycle = 2800 ± 150 d. Furthermore, the RV time series exhibits a possibly periodic long-term signal, which might be related to a Saturn-mass planet of ~100 M⊕.Publicación Acceso Abierto The PLATO mission(Springer Nature Link, 2025-04-21) Rauer, Heike; Aerts, Conny; Cabrera, Juán; Deleuil, Magali; Erikson, Anders; Gizon, Laurent; Goupil, Mariejo; Heras, Ana; Walloschek, Thomas; Lorénzo Álvarez, José; Marliani, Filippo; Martín García, César; Mas Hesse, José Miguel; O´Rourke, Laurence; Osborn, Hugh P.; Pagano, Isabella; Piotto, Giampaolo; Pollacco, Don; Ragazzoni, Roberto; Ramsay, Gavin; Udry, Stéphane; Appourchaux, Thierry; Benz, Willy; Brandeker, Alexis; Güdel, Manuel; Janot Pacheco, Eduardo; Kabath, Petr; Kjeldsen, Hans; Min, Michiel; Santos, Nuno C.; Smith, Alan; Suarez, Juan Carlos; Werner, Stephanie; Aboudan, Alessio; Abreu, Manuel; Acuña, Lorena; Adams, Moritz; Adibekyan, Vardan; Affer, Laura; Agneray, François; Agnor, Craig; Aguirre Børsen Koch, Victor; Ahmed, Saad; Aigrain, Suzanne; Al Bahlawan, Ashraf; De los Angeles Alcacera Gil, Ma; Alei, Eleonora; Alencar, Silvia; Alexander, Richard; Alfonso Garzón, Julia; Alibert, Yann; Alende Prieto, Carlos; Almeida, Leonardo; Alonso Sobrino, Roi; Altavilla, Giuseppe; Althaus, Christian; Álvarez Trujillo, Luis Alonso; Amarsi, Anish; Von Eiff, Matthias Ammler; Amôres, Eduardo; Andrade, Laerte; Antoniadis Karnavas, Alexandros; Antonio, Carlos; Aparico del Moral, Beatriz; Appolloni, Mateo; Arena, Claudio; Armstrong, David; Aroca Aliaga, José; Asplund, Martín; Audenaert, Jeoen; Auricchio, Natalia; Avelino, Pedro; Baeke, Ann; Baillié, Kevin; Balado, Ana; Ballber Balagueró, Pau; Balestra, Andrea; Ball, Warrick; Ballans, Herve; Ballot, Jerome; Barban, Caroline; Barbary, Gaële; Barbieri, Mauro; Barceló Fortaleza, Sebastià; Barker, Adrian; Barklem, Paul; Barnes, Sydney; Barrado, David; Barragan, Oscar; Baruteau, Clément; Basu, Sarbani; Baudin, Frederic; Baumeister, Philipp; Bayliss, Daniel; Bazot, Michael; Beck, Paul; Belkacem, Kevin; Bellinger, Earl; Benatti, Serena; Benomar, Othman; Bérard, Diae; Bergemann, María; Bergomi, María; Bernardo, Pierre; Biazzo, Katia; Bignamini, Andrea; Bigot, Lionel; Billot, Nicolas; Binet, Martín; Biondi, David; Biondi, Federico; Birch, Aaron; Bisch, Bertram; Bluhm Ceballos, Paz Victoria; Bódi, Attila; Bognár, Zsófia; Boisse, Isabelle; Bolmont, Emeline; Bonanno, Alfio; Bonavita, Mariangela; Bonfanti, Andrea; Bonfils, Xavier; Bonito, Rosaria; Bonomo, Aldo Stefano; Börner, Anko; Boro Saikia, Sudeshna; Borreguero Martín, Elisa; Borsa, Francesco; Borsato, Luca; Bossini, Diego; Bouchy, F.; Boué, Gwenaël; Boufleur, Rodrigo; Boumier, Patrick; Bourrier, V.; Bowman, Dominic; Bozzo, Enrico; Bradley, Louisa; Bray, John; Bressan, Aessandro; Breton, Sylvain; Brienza, Daniele; Brito, Ana; Brogi, Matteo; Brown, Beverly; Brown, David; Sacha Brun, Allan; Bruno, Giovanni; Bruns, Michael; Buchhave, Lars; Bugnet, Lisa; Buldgen, Gaël; Burgess, Patrick; Busatta, Andrea; Busso, Giogia; Buzasi, Derek; Caballero, Jose A.; Cabral, Alexandre; Cabrero Gómez, Juan Francisco; Calderone, Flavia; Cameron, Robert; Cameron, Andrew; Campante, Tiago; Campos Gestal, Néstor; Canto Martins, Bruno Leonardo; Cara, Christophe; Carone, Ludmila; Carrasco, Josep Manuel; Casagrande, Luca; Casewell, Sarah; Cassisi, Santi; Castellani, Marco; Castro, Matthieu; Catala, Claude; Catalán Fernández, Irene; Catelan, Márcio; Cegla, Heather; Cerruti, Chiara; Cessa, Virginie; Chadid, Merieme; Chaplin, William; Charpinet, Stephane; Chiappini, Cristina; Chiarucci, Simone; Chiavassa, Andrea; Chinellato, Simonetta; Chirulli, Giovanni; Christensen Dalsgaard, Jørgen; Church, Ross; Claret, Antonio; Clarke, Cathie; Claudi, Riccardo; Clermont, Lionel; et., al.; European Commission (EC); European Research Council (ERC); Agencia Estatal de Investigación (AEI)PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2R) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.Publicación Acceso Abierto A giant exoplanet orbiting a very-low-mass star challenges planet formation models(American Association for the Advancement of Science, 2019-09-27) Morales, J. C.; Mustill, A. J.; Ribas, I.; Davies, M. B.; Reiners, A.; Bauer, F. F.; Kossakowski, D.; Herrero, Enrique; Rodríguez, E.; López González, M. J.; Rodríguez López, C.; Stock, S.; Zechmeister, M.; Luque, R. ; Gesa, L.; Pedraz, S.; Baroch, D.; Sarkis, P.; Lafarga, M.; Johnson, E. N.; Anglada Escudé, G.; González Álvarez, E.; Perryman, M. A. C.; Dreizler, S.; Sarmiento, L. F.; Tal Or, L.; Labarga, F.; Reffert, S.; Rebolo, R.; Schweitzer, A.; Schäfer, S.; Hagen, H. J.; Lázaro, F. J.; Quirrenbach, A.; Perger, M.; Guenther, E. W.; Schlecker, M.; Montes, D.; Jeffers, S. V.; Cortés Contreras, M.; Kürster, M.; Schmitt, J. H. M. M.; Aceituno, Francisco José; Abellán, F. J.; Rosich, A.; Aceituno, J.; Schöfer, P.; Arroyo Torres, B.; Amado, P. J.; Antona, R.; Solano, Enrique; Benítez, D.; Kaminski, A.; Becerril Jarque, S.; Sota, A.; Kehr, M.; Abril, M.; Brinkmöller, M.; Béjar, V. J. S.; Ammler von Eiff, M.; Calvo Ortega, R.; Zapatero Osorio, María Rosa; Barrado, David; Cardona Guillén, C.; Yan, F.; Bergond, G.; Casanova, V.; Klahr, H.; Chaturvedi, P.; Nagel, E.; Claret, A.; Trifonov, T.; Czesla, S.; Henning, T.; Dorda, R.; Seifert, W.; Fernández Hernández, Maite; Alonso Floriano, F. J.; Azzaro, M.; Berdiñas, Z. M.; Del Burgo, C.; Cano, J.; Carro, J.; Casasayas Barris, N.; Carlos, Cifuentes; Colomé, J.; Díez Alonso, E.; Emsenhuber, A.; Guàrdia, J.; Guijarro, A.; De Guindos, E.; Hatzes, Artie ; Hauschildt, P. H.; Hedrosa, R. P.; Hermelo, I.; Hernández Arabi, R.; Hernández Otero, F.; Hintz, D.; Klüter, J.; González Peinado, R.; González Hernández, J. I.; González Cuesta, L.; De Juan, E.; Stahl, O.; Burn, R.; Kim, M.; Fernández Martín, A.; Lara, L. M.; Mordasini, C.; Labiche, N.; Cárdenas, M. C.; Lampón, M.; Ferro, I. M.; López del Fresno, M.; Passegger, V. M.; Lizon, Jean Louis; Casal, E.; Lodieu, N.; Fuhrmeister, B.; Mancini, L.; López Santiago, J.; Kemmer, J.; Mall, U.; Galadí Enríquez, D.; Martín Fernández, P.; Marfil, E.; Lalitha, S.; Martín, Eduardo L.; Gallardo Cava, I.; Mirabet, E.; Llamas, M.; Marvin, E. L.; García Vargas, M. L.; Nortmann, L.; Magán Madinabeitia, H.; Nelson, Richard; García Piquer, A.; Pallé, E. ; Marín Molina, J. A.; Pascual Granado, J.; Caballero, Jose A.; Martínez Rodríguez, H.; Pérez Medialdea, D.; Huke, P.; Naranjo, V.; Rabaza, O.; Huber, A.; Ofir, A.; Redondo, P.; Holgado, G.; Rodler, F.; Klutsch, A.; Sabotta, S.; Launhardt, R.; Salz, M.; López Salas, F. J.; Sánchez Carrasco, M. A.; Mandel, H.; Sanz-Forcada, Jorge; Martín Ruiz, S.; Moya, A.; Nowak, G.; Pavlov, Alexander; Pérez Calpena, A.; Ramón Ballesta, A.; Rix, H. W.; Rodríguez Trinidad, A.; Sadegi, S.; Sánchez Blanco, E.; Sánchez López, A.; Stürmer, J.; Suárez, J. C.; Tabernero, H. M. ; Tulloch, S. M.; Veredas, G.; Vico Linares, J. I.; Vilardell, F.; Wagner, K.; Winkler, J.; Wolthoff, V.; Johansen, A.; Stuber, T.; 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); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; 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]; López González, M. J. [0000-0001-8104-5128]; Rodríguez López, C. [0000-0001-5559-7850]; Sarkis, P. [0000-0001-8128-3126]; López Santiago, J. [0000-0003-2402-8166]; Vilardell, F. [0000-0003-0441-1504]; Winkler, J. [0000-0003-0568-8820]; Nowak, G. [0000-0002-7031-7754]; Béjar, V. J. S. [0000-0002-5086-4232]; Luque, R. [0000-0002-4671-2957]; Pérez Calpena, A. [0000-0001-7361-9240]; Sota, A. [https://orcid.org/0000-0002-9404-6952]; Klahr, H. [0000-0002-8227-5467]; Mordasini, C. [0000-0002-1013-2811]; Rodler, F. [0000-0003-0650-5723]; Tabernero, H. [0000-0002-8087-4298]; Cortés Contreras, M. [0000-0003-3734-9866]; Lafarga, M. [0000-0002-8815-9416]; Sánchez López, A. [0000-0002-0516-7956]; Yan, F. [0000-0001-9585-9034]; Reffert, S. [0000-0002-0460-8289]; Rosich, A. [0000-0002-9141-3067]; Sarmiento, L. F. [0000-0002-8475-9705]; Perger, M. [0000-0001-7098-0372]; Sabotta, S. [0000-0001-9078-5574]; Guenther, E. W. [0000-0002-9130-6747]; Kaminski, A. [0000-0003-0203-8208]; Schmitt, J. H. M. M. [0000-0003-2554-9916]; Aceituno, J. [0000-0003-0487-1105]; Alonso Floriano, F. J. [0000-0003-1202-5734]; Stock, S. [0000-0002-1166-9338]; Nagel, E. [0000-0002-4019-3631]; Barrado, D. [0000-0002-5971-9242]; Tulloch, S. [0000-0003-0840-8521]; Trifonov, T. [0000-0002-0236-775X]; Bergond, G. [0000-0003-3132-9215]; Burn, R. [0000-0002-9020-7309]; Zapatero Osorio, M. R. [0000-0001-5664-2852]; Montes, D. [0000-0002-7779-238X]; Cano, J. [0000-0003-1984-5401]; Cardona Guillén, C. [0000-0002-2198-4200]; Baroch, D. [0000-0001-7568-5161]; Ammler-von Eiff, M. [0000-0001-9565-1698]; Chaturvedi, P. [0000-0002-1887-1192]; Cifuentes, C. [0000-0003-1715-5087]; Anglada Escudé, G. [0000-0002-3645-5977]; Becerril Jarque, S. [0000-0001-9009-1150]; González Cuesta, L. [0000-0002-1241-5508]; Díez Alonso, E. [0000-0002-5826-9892]; Emsenhuber, A. [0000-0002-8811-1914]; Passegger, V. M. [0000-0002-8569-7243]; García Vargas, M. L. [0000-0002-2058-3528]; González Álvarez, E. [0000-0002-4820-2053]; Amado, P. J. [0000-0002-8388-6040]; Carro, J. [0000-0002-0838-3603]; Guàrdia, J. [0000-0002-7191-9001]; Abellán, F. J. [0000-0002-5724-1636]; Colomé, J. [0000-0002-1678-2241]; Hermelo, I. [0000-0001-9178-694X]; Hintz, D. [0000-0002-5274-2589]; Arroyo Torres, B. [0000-0002-3392-4694]; Fuhrmeister, B. [0000-0001-8321-5514]; Johnson, E. [0000-0003-2260-5134]; De Juan Fernández, E. [0000-0002-9382-4505]; Berdiñas, Z. M. [0000-0002-6057-6461]; González Hernández, J. I. [0000-0002-0264-7356]; Klüter, J. [0000-0002-3469-5133]; Klutsch, A. [0000-0001-7869-3888]; Calvo Ortega, R. [0000-0003-3693-6030]; Guijarro, A. [0000-0001-5518-1759]; Aceituno, F. J. [0000-0001-8074-4760]; Lara, L. M. [0000-0002-7184-920X]; Launhardt, R. [0000-0002-8298-2663]; Casasayas Barris, N. [0000-0002-2891-8222]; López del Fresno, M. [0000-0002-9479-7780]; Magan Madinabeitia, H. [0000-0003-1243-4597]; Czesla, S. [0000-0002-4203-4773]; Kehr, M. [0000-0002-7420-7368]; Marín Molina, J. A. [0000-0002-3525-0806]; Galadí Enríquez, D. [0000-0003-4946-5653]; Labarga, F. [0000-0002-7143-0206]; Martínez Rodríguez, H. [0000-0002-1919-228X]; Marvin, C. J. [0000-0002-2249-2611]; González Peinado, R. [0000-0002-6658-8930]; Lizon, J. L. [0000-0001-8928-2566]; Naranjo, V. [0000-0003-0097-1061]; Nelson, R. [0000-0002-9687-8779]; De Guindos, E. [0000-0002-8124-9101]; Manici, L. [0000-0002-9428-8732]; Ofir, A. [0000-0002-9152-5042]; Pascual Granado, J. [0000-0003-0139-6951]; Huke, P. [0000-0001-5913-2743]; Martín, E. [0000-0002-1208-4833]; García Piquer, A. [0000-0002-6872-4262]; Rabaza, O. [0000-0003-2766-2103]; Ramón Ballesta, A. [0000-0002-4323-0610]; Kim, M. [0000-0001-6218-2004]; Rodríguez Trinidad, A. [0000-0002-3356-8634]; Sadegi, S. [0000-0001-9897-6121]; Lampón, M. [0000-0002-0183-7158]; Nortmann, L. [0000-0001-8419-8760]; Sanz Forcada, J. [0000-0002-1600-7835]; Lodieu, N. [0000-0002-3612-8968]; Pedraz, S. [0000-0003-1346-208X]; Schäfer, S. [0000-0001-8597-8048]; Schlecker, M. [0000-0001-8355-2107]; Marfil, E. [0000-0001-8907-4775]; Redondo, P. G. [0000-0001-5992-5778]; Schöfer, P. [0000-0002-5969-3708]; Solano, E. [0000-0003-1885-5130]; Martín Ruiz, S. [0000-0002-9006-7182]; Sánchez Carrasco, M. A. [0000-0001-5533-3660]; Stuber, T. [0000-0003-2185-0525]; Suárez, J. C. [0000-0003-3649-8384]; Moya, A. [0000-0003-1665-5389]; 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-2017-0709Surveys 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 SciencePublicación Acceso Abierto Galactic extinction laws – II. Hidden in plain sight, a new interstellar absorption band at 7700 Å broader than any known DIB(Oxford Academics: Oxford University Press, 2021-02-12) Maíz Apellániz, J.; Barbá, R. H.; Caballero, Jose A.; Bohlin, R. C.; Fariña, C.; Agencia Estatal de Investigación (AEI)We have detected a broad interstellar absorption band centred close to 7700 Å and with a full width at half-maximum (FWHM) of 176.6 ± 3.9 Å. This is the first such absorption band detected in the optical range and is significantly wider than the numerous diffuse interstellar bands (DIBs). It remained undiscovered until now because it is partially hidden behind the A telluric band produced by O2. The band was discovered using STIS@HST spectra and later detected in a large sample of stars of diverse type (OB stars, BA supergiants, red giants), using further STIS and ground-based spectroscopy. The EW of the band is measured and compared with our extinction and K I λλ7667.021, 7701.093 measurements for the same sample. The carrier is ubiquitous in the diffuse and translucent Galactic interstellar medium (ISM) but is depleted in the environment around OB stars. In particular, it appears to be absent or nearly so in sightlines rich in molecular carbon. This behaviour is similar to that of the σ-type DIBs, which originate in the low/intermediate-density UV-exposed ISM but are depleted in the high-density UV-shielded molecular clouds. We also present an update on our previous work on the relationship between E(4405–5495) and R5495 and incorporate our results into a general model of the ISM.Publicación Acceso Abierto CARMENES input catalog of M dwarfs VI. A time-resolved Ca II H&K catalog from archival data(EDP Sciences, 2021-08-20) Perdelwitz, V.; Mittag, M.; Tal Or, L.; Schmitt, J. H. M. M.; Caballero, Jose A.; Jeffers, S. V.; Reiners, A.; Schweitzer, A.; Trifonov, T.; Ribas, I.; Quirrenbach, A.; Amado, P. J.; Seifert, W.; Cifuentes, C.; Cortés Contreras, M.; Montes, D.; Revilla, D.; Skrzypinski, S. L.; Agencia Estatal de Investigación (AEI); Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC; Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Canarias; Perdelwitz, V. [0000-0002-6859-0882]; Tal Or, L. [0000-0003-3757-1440]; Caballero, J. A. [0000-0002-7349-1387]; Reiners, A. [0000-0003-1242-5922]; Schweitzer, A. [0000-0002-1624-0389]; Ribas, I. [0000-0002-6689-0312]; Amado, P. J. [0000-0001-8012-3788]; Cifuentes, C. [0000-0003-1715-5087]; Cortés Contreras, M. [0000-0003-3734-9866]; Skrzypinski, S. L. [0000-0002-0926-9888]; 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-2017-0709Context. Radial-velocity (RV) jitter caused by stellar magnetic activity is an important factor in state-of-the-art exoplanet discovery surveys such as CARMENES. Stellar rotation, along with heterogeneities in the photosphere and chromosphere caused by activity, can result in false-positive planet detections. Hence, it is necessary to determine the stellar rotation period and compare it to any putative planetary RV signature. Long-term measurements of activity indicators such as the chromospheric emission in the Ca II H&K lines (RHK′) enable the identification of magnetic activity cycles. Aims. In order to determine stellar rotation periods and study the long-term behavior of magnetic activity of the CARMENES guaranteed time observations (GTO) sample, it is advantageous to extract RHK′ time series from archival data, since the CARMENES spectrograph does not cover the blue range of the stellar spectrum containing the Ca II H&K lines. Methods. We have assembled a catalog of 11 634 archival spectra of 186 M dwarfs acquired by seven different instruments covering the Ca II H&K regime: ESPaDOnS, FEROS, HARPS, HIRES, NARVAL, TIGRE, and UVES. The relative chromospheric flux in these lines, RHK′, was directly extracted from the spectra by rectification with PHOENIX synthetic spectra via narrow passbands around the Ca II H&K line cores. Results. The combination of archival spectra from various instruments results in time series for 186 stars from the CARMENES GTO sample. As an example of the use of the catalog, we report the tentative discovery of three previously unknown activity cycles of M dwarfs. Conclusions. We conclude that the method of extracting with the use of model spectra yields consistent results for different instruments and that the compilation of this catalog will enable the analysis of long-term activity time series for a large number of M dwarfs.Publicación Acceso Abierto CARMENES input catalogue of M dwarfs: V. Luminosities, colours, and spectral energy distributions(EDP Sciences, 2020-10-12) Carlos, Cifuentes; Caballero, Jose A.; Cortés Contreras, M.; Montes, D.; Abellán, F. J.; Dorda, R.; Holgado, G.; Zapatero Osorio, María Rosa; Morales, J. C.; Amado, P. J.; Passegger, V. M.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sanz-Forcada, Jorge; Schweitzer, A.; Seifert, W.; Solano, Enrique; Agencia Estatal de Investigación (AEI); National Aeronautics and Space Administration (NASA); 0000-0003-1715-5087; 0000-0003-3734-9866; 0000-0002-7779-238X; 0000-0001-5664-2852; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Context. The relevance of M dwarfs in the search for potentially habitable Earth-sized planets has grown significantly in the last years. Aims. In our on-going effort to comprehensively and accurately characterise confirmed and potential planet-hosting M dwarfs, in particular for the CARMENES survey, we have carried out a comprehensive multi-band photometric analysis involving spectral energy distributions, luminosities, absolute magnitudes, colours, and spectral types, from which we have derived basic astrophysical parameters. Methods. We have carefully compiled photometry in 20 passbands from the ultraviolet to the mid-infrared, and combined it with the latest parallactic distances and close-multiplicity information, mostly from Gaia DR2, of a sample of 2479 K5 V to L8 stars and ultracool dwarfs, including 2210 nearby, bright M dwarfs. For this, we made extensive use of Virtual Observatory tools. Results. We have homogeneously computed accurate bolometric luminosities and effective temperatures of 1843 single stars, derived their radii and masses, studied the impact of metallicity, and compared our results with the literature. The over 40 000 individually inspected magnitudes, together with the basic data and derived parameters of the stars, individual and averaged by spectral type, have been made public to the astronomical community. In addition, we have reported 40 new close multiple systems and candidates (ρ < 3.3 arcsec) and 36 overluminous stars that are assigned to young Galactic populations. Conclusions. In the new era of exoplanet searches around M dwarfs via transit (e.g. TESS, PLATO) and radial velocity (e.g. CARMENES, NIRPS+HARPS), this work is of fundamental importance for stellar and therefore planetary parameter determination. © ESO 2020.Publicación Restringido A nearby transiting rocky exoplanet that is suitable for atmospheric investigation(Science, 2021-03-05) Trifonov, T.; Caballero, Jose A.; Morales, J. C.; Seifahrt, A.; Reiners, A.; Bean, J. L.; Luque, R. ; Parviainen, H.; Pallé, E. ; Stock, S.; Zechmeister, M.; Amado, P. J.; Anglada Escudé, G.; Azzaro, M.; Barclay, T.; Béjar, V. J. S.; Bluhm, P.; Casasayas Barris, N.; Carlos, Cifuentes; Collins, K. A.; Collins, K. I.; Cortés Contreras, M.; De Leon, J. P.; Dreizler, S.; Dressing, C. D.; Esparza Borges, E.; Espinoza, N.; Fausnaugh, M.; Fukui, A.; Hatzes, Artie ; Hellier, C.; Henning, T.; Henze, C. E.; Herrero, Enrique; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kaminski, A.; Kasper, D.; Kossakowski, D.; Kürster, M.; Lafarga, M.; Latham, D. W.; Mann, A. W.; Molaverdikhani, K.; Montes, D.; Montet, B. T.; Murgas Alcaino, F. ; Narita, N.; Oshagh, M.; Passegger, V. M.; Pollacco, D.; Quinn, S. N.; Quirrenbach, A.; Ricker, George; Rodríguez López, C.; Sanz-Forcada, Jorge; Schwarz, R. P.; Schweitzer, A.; Seager, S.; Shporer, A.; Stangret, M.; Stürmer, J.; Tan, T. G.; Tenenbaum, P.; Twicken, J. D.; Vanderspek, R.; Winn, J. N.; Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); National Aeronautics and Space Administration (NASA); European Research Council (ERC); Japan Society for the Promotion of Science (JSPS); La Caixa; Japan Science and Technology Agency (JST); Trifonov, T. [0000-0002-0236-775X]; Caballero, J. A. [0000-0002-7349-1387]; Morales, J. C. [0000-0003-0061-518X]; Seifahrt, A. [0000-0003-4526-3747]; Ribas, I. [0000-0002-6689-0312]; Bean, J. [0000-0003-4733-6532]; Luque, R. [0000-0002-4671-2957]; Parviainen, H. [0000-0001-5519-1391]; Pallé, E. [0000-0003-0987-1593]; Stock, S. [0000-0002-1166-9338]; Zechmeister, M. [0000-0002-6532-4378]; Amado, P. J. [0000-0002-8388-6040]; Anglada Escudé, G. [0000-0002-3645-5977]; Azzaro, M. [0000-0002-1317-0661]; Barclay, T. [0000-0001-7139-2724]; Béjar, V. J. S. [0000-0002-5086-4232]; Bluhm, P. [0000-0002-0374-8466]; Casasayas Barris, N. [0000-0002-2891-8222]; Cifuentes, C. [0000-0003-1715-5087]; Collins, K. A. [0000-0001-6588-9574]; Collins, K. I. [0000-0003-2781-3207]; Cortés Contreras, M. [0000-0003-3734-9866]; Dreizler, S. [0000-0001-6187-5941]; Dressing, C. D. [0000-0001-8189-0233]; Esparza Borges, E. [0000-0002-2341-3233]; Espinoza, N. [0000-0001-9513-1449]; Fausnaugh, M. [0000-0002-9113-7162]; Fukui, A. [0000-0002-4909-5763]; Hatzes, A. P. [0000-0002-3404-8358]; Hellier, C. [0000-0002-3439-1439]; Henning, T. [0000-0002-1493-300X]; Herrero, E. [0000-0001-8602-6639]; Jeffers, S. V. [0000-0003-2490-4779]; Jenkins, J. M. [0000-0002-4715-9460]; Jensen, E. L. N. [0000-0002-4625-7333]; Kaminski, A. [0000-0003-0203-8208]; Kasper, D. [0000-0003-0534-6388]; Kossakowski, D. [0000-0002-0436-7833]; Lafarga, M. [0000-0002-8815-9416]; Latham, D. W. [0000-0001-9911-7388]; Mann, A. W. [0000-0003-3654-1602]; Molaverdikhani, K. [0000-0002-0502-0428]; Montes, D. [0000-0002-7779-238X]; Montet, B. T. [0000-0001-7516-8308]; Murgas, F. [0000-0001-9087-1245]; Narita, N. [0000-0001-8511-2981]; Oshagh, M. [0000-0002-0715-8789]; Passegger, V. M. [0000-0002-8569-7243]; Pollacco, D. [0000-0001-9850-9697]; Quinn, S. N. [0000-0002-8964-8377]; Rodríguez López, C. [0000-0001-5559-7850]; Sanz Forcada, J. [0000-0002-1600-7835]; Schwarz, R. P. [0000-0001-8227-1020]; Schweitzer, A. [0000-0002-1624-0389]; Seager, S. [0000-0002-6892-6948]; Stangret, M. [0000-0002-1812-8024]; Stürmer, J. [0000-0002-4410-4712]; Tan, T. G. [0000-0001-5603-6895]; Tenenbaum, P. [0000-0002-1949-4720]; Twicken, J. D. [0000-0002-6778-7552]; Vanderspek, R. [0000-0001-6763-6562]; Winn, J. N. [0000-0002-4265-047X]; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet’s short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy.Publicación Acceso Abierto He I λ 10 830 Å in the transmission spectrum of HD209458 b(EDP Sciences, 2019-09-12) Alonso Floriano, F. J.; Snellen, Ignas; Czesla, S.; Bauer, F. F.; Salz, M.; Lampón, M.; Lara, L. M.; Nagel, E.; López Puertas, M.; Nortmann, L.; Sánchez López, A.; Sanz-Forcada, Jorge; Caballero, Jose A.; Reiners, A.; Ribas, I.; Quirrenbach, A.; Amado, P. J.; Aceituno, J.; Anglada Escudé, G.; Béjar, V. J. S.; Brinkmöller, M.; Hatzes, Artie ; Henning, T.; Kaminski, A.; Kürster, M.; Labarga, F.; Montes, D.; Pallé, E. ; Schmitt, J. H. M. M.; Zapatero Osorio, María Rosa; Ministerio de Economía y Competitividad (MINECO); Max-Planck-Gesellschaft (MPG); European Research Council (ERC); Comunidad de Madrid; Agencia Estatal de Investigación (AEI); Alonso Floriano, F. J. [0000-0003-1202-5734]; 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-2017-0709Context. 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.Publicación Acceso Abierto All-sky visible and near infrared space astrometry(Springer Link, 2021-03-11) Hobbs, D.; Brown, Anthony; Hog, E.; Jordi, C.; Kawata, D.; Tanga, P.; Klioner, S. A.; Sozzetti, A.; Wyrzykowski, L.; Walton, N.; Vallenari, A.; Makarov, V.; Rybizki, J.; Jiménez Esteban, F. M.; Caballero, Jose A.; McMillan, P. J.; Secrest, N.; Mor, R.; Andrews, Jeff J.; Zwitter, T.; Chiappini, C.; Fynbo, J. P. U.; Ting, Y. S.; Hestroffer, D.; Lindegren, L.; McArthur, B.; Gouda, N.; Moore, A.; González, O. A.; Vaccari, M.; Hobbs, D. [0000-0002-2696-1366]; Brown, A. [0000-0002-7419-9679]; Sozzetti, A. [0000-0002-7504-365X]; Secrest, N. [0000-0002-4902-8077]The era of all-sky space astrometry began with the Hipparcos mission in 1989 and provided the first very accurate catalogue of apparent magnitudes, positions, parallaxes and proper motions of 120 000 bright stars at the milliarcsec (or milliarcsec per year) accuracy level. Hipparcos has now been superseded by the results of the Gaia mission. The second Gaia data release contained astrometric data for almost 1.7 billion sources with tens of microarcsec (or microarcsec per year) accuracy in a vast volume of the Milky Way and future data releases will further improve on this. Gaia has just completed its nominal 5-year mission (July 2019), but is expected to continue in operations for an extended period of an additional 5 years through to mid 2024. Its final catalogue to be released ∼ 2027, will provide astrometry for ∼ 2 billion sources, with astrometric precisions reaching 10 microarcsec. Why is accurate astrometry so important? The answer is that it provides fundamental data which underpin much of modern observational astronomy as will be detailed in this White Paper. All-sky visible and Near-InfraRed (NIR) astrometry with a wavelength cutoff in the K-band is not just focused on a single or small number of key science cases. Instead, it is extremely broad, answering key science questions in nearly every branch of astronomy while also providing a dense and accurate visible-NIR reference frame needed for future astronomy facilities.
