Persona: González Hernández, Carmen
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González Hernández
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Publicación Acceso Abierto Broadband transmission spectroscopy of HD 209458b with ESPRESSO: evidence for Na, TiO, or both(EDP Sciences, 2020-12-01) Santos, Nuno C.; Cristo, E.; Demangeon, O. D. S.; Oshagh, M.; Allart, R.; Barros, S. C. C.; Borsa, F.; Bourrier, V.; Casasayas Barris, N.; Ehrenreich, D.; Faria, J. P.; Figueira, P.; Martins, J. H. C.; Micela, G.; Pallé, E.; Sozzetti, A.; Tabernero, H. M.; Zapatero Osorio, M. R.; Pepe, Francesco; Cristiani, S.; Rebolo, R.; Adibekyan, V.; Allende Prieto, C.; Alibert, Y.; Bouchy, F.; Cabral, A.; Dekker, H.; Di Marcantonio, P.; D´Odorico, V.; Dumusque, X.; González Hernández, J. I.; Lavie, B.; Lo Curto, G.; Lovis, C.; Manescau, A.; Martins, C. J. A. P.; Mégevand, D.; Mehner, A.; Molaro, P.; Nunes, Nelson J.; Poretti, E.; Rivas, M.; Sousa, S. G.; Suárez Mascareño, A.; Udry, S.; González Hernández, Carmen; Fundacao para a Ciencia e a Tecnologia (FCT); Istituto Nazionale di Astrofisica (INAF); European Research Council (ERC); Agencia Estatal de Investigación (AEI); 0000-0003-4422-2919; 0000-0001-5992-7589; 0000-0001-7918-0355; 0000-0002-0715-8789; 0000-0003-0987-1593Context. The detection and characterization of exoplanet atmospheres is currently one of the main drivers pushing the development of new observing facilities. In this context, high-resolution spectrographs are proving their potential and showing that high-resolution spectroscopy will be paramount in this field. Aims. We aim to make use of ESPRESSO high-resolution spectra, which cover two transits of HD 209458b, to probe the broadband transmission optical spectrum of the planet. Methods. We applied the chromatic Rossiter–McLaughin method to derive the transmission spectrum of HD 209458b. We compared the results with previous HST observations and with synthetic spectra. Results. We recover a transmission spectrum of HD 209458b similar to the one obtained with HST data. The models suggest that the observed signal can be explained by only Na, only TiO, or both Na and TiO, even though none is fully capable of explaining our observed transmission spectrum. Extra absorbers may be needed to explain the full dataset, though modeling approximations and observational errors can also be responsible for the observed mismatch. Conclusions. Using the chromatic Rossiter–McLaughlin technique, ESPRESSO is able to provide broadband transmission spectra of exoplanets from the ground, in conjunction with space-based facilities, opening good perspectives for similar studies of other planets.Publicación Acceso Abierto The GAPS Programme at TNG XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis b(EDP Sciences, 2020-05-29) Carleo, I.; Malavolta, L.; Lanza, A. F.; Damasso, M.; Desidera, S.; Borsa, F.; Mallonn, M.; Pinamonti, M.; Gratton, R.; Alei, E.; Benatti, S.; Mancini, L.; Maldonado, J.; Biazzo, K.; Esposito, M.; Frustagli, G.; González Álvarez, E.; Micela, G.; Scandariato, G.; Sozzetti, A.; Affer, L.; Bignamini, A.; Bonomo, A. S.; Claudi, R.; Cosentino, R.; Covino, E.; Fiorenzano, A. F. M.; Giacobbe, P.; Harutyunyan, A.; Leto, G.; Maggio, A.; Molinari, E.; Nascimbeni, V.; Pagano, I.; Pedani, M.; Piotto, G.; Poretti, E.; Rainer, M.; Redfield, S.; Baffa, C.; Baruffolo, A.; Buschschacher, N.; Billoti, V.; Cecconi, M.; Falcini, G.; Fantinel, D.; Fini, L.; Galli, A.; Ghedina, A.; Ghinassi, F.; Giani, E.; González, C.; González, M.; Guerra, J.; Hernández Díaz, M.; Hernández, N.; Luzzolino, M.; Lodi, M.; Oliva, E.; Origlia, L.; Pérez Ventura, H.; Puglisi, A.; Riverol, C.; Riverol, L.; San Juan, J.; Sanna, N.; Scuderi, S.; Seemann, U.; Sozzi, M.; Tozzi, P.; González Hernández, Carmen; Jimeno González, María; Agenzia Spaziale Italiana (ASI); European Commission (EC); Claudi, R. [0000-0001-7707-5105]; Leto, G. [0000-0002-0040-5011]; Piotto, G. [0000-0002-9937-6387]; Bonomo, A. S. [0000-0002-6177-198X]; Sozzetti, A. [0000-0002-7504-365X]; Biazzo, K. [0000-0002-1892-2180]; Ghedina, A. [0000-0003-4702-5152]; Damasso, M. [0000-0001-9984-4278]; Cosentino, R. [0000-0003-1784-1431]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Context. The existence of hot Jupiters is still not well understood. Two main channels are thought to be responsible for their current location: a smooth planet migration through the protoplanetary disk or the circularization of an initial highly eccentric orbit by tidal dissipation leading to a strong decrease in the semimajor axis. Different formation scenarios result in different observable effects, such as orbital parameters (obliquity and eccentricity) or frequency of planets at different stellar ages. Aims. In the context of the GAPS Young Objects project, we are carrying out a radial velocity survey with the aim of searching and characterizing young hot-Jupiter planets. Our purpose is to put constraints on evolutionary models and establish statistical properties, such as the frequency of these planets from a homogeneous sample. Methods. Since young stars are in general magnetically very active, we performed multi-band (visible and near-infrared) spectroscopy with simultaneous GIANO-B + HARPS-N (GIARPS) observing mode at TNG. This helps in dealing with stellar activity and distinguishing the nature of radial velocity variations: stellar activity will introduce a wavelength-dependent radial velocity amplitude, whereas a Keplerian signal is achromatic. As a pilot study, we present here the cases of two known hot Jupiters orbiting young stars: HD 285507 b and AD Leo b. Results. Our analysis of simultaneous high-precision GIARPS spectroscopic data confirms the Keplerian nature of the variation in the HD 285507 radial velocities and refines the orbital parameters of the hot Jupiter, obtaining an eccentricity consistent with a circular orbit. Instead, our analysis does not confirm the signal previously attributed to a planet orbiting AD Leo. This demonstrates the power of the multi-band spectroscopic technique when observing active stars.Publicación Acceso Abierto Stellar atmospheric parameters of FGK-type stars from high-resolution optical and near-infrared CARMENES spectra(Oxford Academics: Oxford University Press, 2020-01-10) Marfil, E.; Tabernero, H. M.; Montes, D.; Caballero, J. A.; Soto, M. G.; González Hernández, J. I.; Kaminski, A.; Nagel, E.; Jeffers, S. V.; Reiners, A.; Ribas, I.; Quirrenbach, A.; Amado, P. J.; González Hernández, Carmen; Fundacao para a Ciencia e a Tecnologia (FCT); Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); 0000-0001-8907-4775; 0000-0002-8087-4298; 0000-0002-7349-1387; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737With the purpose of assessing classic spectroscopic methods on high-resolution and high signal-to-noise ratio spectra in the near-infrared wavelength region, we selected a sample of 65 F-, G-, and K-type stars observed with CARMENES, the new, ultra-stable, double channel spectrograph at the 3.5 m Calar Alto telescope. We computed their stellar atmospheric parameters (Teti, log g, 4, and [Fell I]) by means of the STEPAR code, a PYTHON implementation of the equivalent width method that employs the 2017 version of the MOOG code and a grid of MARCS model atmospheres. We compiled four Fe 1 and Fe tl line lists suited to metal-rich dwarfs, metal-poor dwarfs, metal-rich giants, and metal-poor giants that cover the wavelength range from 5300 to 17 100 A, thus substantially increasing the number of identified Fe! and Felt lines up to 653 and 23, respectively, We examined the impact of the near-infrared Fe and Fen lines upon our parameter determinations after an exhaustive literature search, placing special emphasis on the 14 Gala benchmark stars contained in our sample, Even though our parameter determinations remain in good agreement with the literature values, the increase in the number of Fel and Feu lines when the near-infrared region is taken into account reveals a deeper Teff scale that might stem from a higher sensitivity of the near-infrared lines to Tff.C 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical SocietyPublicación 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, E.; 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, M. R.; Barrado, D.; 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.; Cifuentes, C.; 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, J. 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, J.; 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.; Solano, Enrique; González Hernández, Carmen; 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 K2-111: an old system with two planets in near-resonance.(Oxford Academics: Blackwell Publishing, 2020-10-27) Mortier, A.; Zapatero Osorio, M. R.; Malavolta, L.; Alibert, Y.; Rice, K.; Lillo Box, J.; Vanderburg, A.; Oshagh, M.; Buchhave, L. A.; Adibekyan, V.; Delgado Mena, E.; López Morales, M.; Charbonneau, D.; Sousa, S. G.; Lovis, C.; After, L.; Allende Prieto, C.; Barros, S. C. C.; Benatti, S.; Bonomo, A. S.; Boschin, W.; Bouchy, F.; Cabral, A.; Collier Cameron, A.; Cosentino, R.; Cristiani, S.; Demangeon, O. D. S.; Di Marcantonio, P.; D´Odorico, V.; Dumusque, X.; Ehrenreich, D.; Figueira, P.; Fiorenzano, A. F. M.; Ghedina, A.; González Hernández, J. I.; Haldemann, J.; Harutyunyan, A.; Haywood, R. D.; Latham, D. W.; Lavie, B.; Lo Curto, G.; Maldonado, J.; Menescau, A.; Martins, C. J. A. P.; Mayor, M.; Mégevand, D.; Mehner, A.; Micela, G.; Molaro, P.; Molinari, E.; Nunes, Nelson J.; Pepe, Francesco; Pallé, E.; Phillips, D.; Piotto, G.; Pinamonti, M.; Poretti, E.; Rivas, M.; Rebolo, R.; Santos, Nuno C.; Sasselov, D.; Sozzetti, A.; Suárez Mascareño, A.; Udry, S.; West, R. G.; Watson, C. A.; Wilson, T. G.; González Hernández, Carmen; Science and Technology Facilities Council (STFC); Istituto Nazionale di Astrofisica (INAF); Swiss National Science Foundation (SNSF); Fundação para a Ciência e a Tecnologia (FCT); National Aeronautics and Space Administration (NASA); European Research Council (ERC); 0000-0002-9433-871X; 0000-0002-3814-5323; 0000-0002-0571-4163; 0000-0003-4434-2195; 0000-0003-1605-5666; 0000-0001-7246-5438; 0000-0003-2434-3625; 0000-0003-1231-2389; 0000-0003-1784-1431; 0000-0002-7504-365X; 0000-0002-0601-6199; 0000-0001-8749-1962; 0000-0002-8863-7828; 0000-0003-4422-2919; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737This paper reports on the detailed characterization of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry, as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved (log g = 4.17), iron-poor ([Fe/H]=-0.46), but alpha-enhanced ([alpha/Fe]=0.27), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT, shows that the transiting planet, K2-111 b, orbits with a period P-b = 5.3518 +/- 0.0004 d and has a planet radius of 1.82(-0.09)(+0.11) R-circle plus and a mass of 5.29(-0.77)(+0.76) M-circle plus, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111 b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111 c, with an orbital period of 15.6785 +/- 0.0064 d, orbiting in near-3:1 mean motion resonance with the transiting planet, and a minimum planet mass of 11.3 +/- 1.1M(circle plus). Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters.Publicación Acceso Abierto ESPRESSO at VLT On-sky performance and first results(EDP Sciences, 2021-01-19) Pepe, Francesco; Cristiani, S.; Rebolo, R.; Santos, Nuno C.; Dekker, H.; Cabral, A.; Di Marcantonio, P.; Figueira, P.; Lo Curto, G.; Lovis, C.; Mayor, M.; Mégevand, D.; Molaro, P.; Riva, M.; Zapatero Osorio, M. R.; Amate, M.; Manescau, A.; Pasquini, L.; Zerbi, Filippo M.; Adibekyan, V.; Abreu, M.; Affolter, M.; Alibert, Y.; Aliverti, M.; Allart, R.; Allende Prieto, C.; Álvarez, D.; Alves, D.; Ávila, G.; Baldini, V.; Bandy, T.; Barros, S. C. C.; Benz, W.; Bianco, A.; Borsa, F.; Bourrier, V.; Bouchy, F.; Broeg, C.; Calderone, G.; Cirami, R.; Coelho, J.; Conconi, P.; Coretti, I.; Cumani, C.; Cupani, G.; D´Odorico, V.; Damasso, M.; Deiries, S.; Delabre, B.; Demangeon, O. D. S.; Dumusque, X.; Ehrenreich, D.; Faria, J. P.; Fragoso, A.; Genolet, L.; Genoni, M.; Génova Santos, R.; González Hernández, J. I.; Hughes, I.; Iwert, O.; Kerber, F.; Knudstrup, J.; Landoni, M.; Lavie, B.; Lillo Box, J.; Lizon, Jean Louis; Maire, C.; Martins, C. J. A. P.; Mehner, A.; Micela, G.; Modigliani, A.; Monteiro, M. A.; Monteiro, M. J. P. F. G.; Moschetti, M.; Murphy, M. T.; Nunes, Nelson J.; Oggioni, L.; Oliveira, António; Oshagh, M.; Pallé, E.; Pariani, G.; Poretti, E.; Rasilla, J. L.; Rebordao, J.; Redaelli, E.; Santana Tschudi, S.; Santin, P.; Santos, Pedro; Ségransan, D.; Schmidt, T. M.; Segovia, A.; Sosnowska, D.; Sozzetti, A.; Sousa, S. G.; Spanò, P.; Suárez Mascareño, A.; Tabernero, H. M.; Tenegi, F.; Udry, S.; Zanutta, A.; González Hernández, Carmen; Swiss National Science Foundation (SNSF); Fundacao para a Ciencia e a Tecnologia (FCT); European Research Council (ERC); Agencia Estatal de Investigación (AEI); Australian Research Council; 0000-0002-9433-871X; 0000-0003-0513-8116; 0000-0002-4339-0550; 0000-0002-6728-244X; 0000-0003-2434-3625; 0000-0002-7504-365X; 0000-0002-7040-5498; 0000-0003-4422-2919; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Context. ESPRESSO is the new high-resolution spectrograph of ESO’s Very Large Telescope (VLT). It was designed for ultra-high radial-velocity (RV) precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UTs) of the VLT at a spectral resolving power of 140 000 or 190 000 over the 378.2 to 788.7 nm wavelength range; it can also observe with all four UTs together, turning the VLT into a 16 m diameter equivalent telescope in terms of collecting area while still providing a resolving power of 70 000. Aims. We provide a general description of the ESPRESSO instrument, report on its on-sky performance, and present our Guaranteed Time Observation (GTO) program along with its first results. Methods. ESPRESSO was installed on the Paranal Observatory in fall 2017. Commissioning (on-sky testing) was conducted between December 2017 and September 2018. The instrument saw its official start of operations on October 1, 2018, but improvements to the instrument and recommissioning runs were conducted until July 2019. Results. The measured overall optical throughput of ESPRESSO at 550 nm and a seeing of 0.65″ exceeds the 10% mark under nominal astroclimatic conditions. We demonstrate an RV precision of better than 25 cm s−1 during a single night and 50 cm s−1 over several months. These values being limited by photon noise and stellar jitter shows that the performance is compatible with an instrumental precision of 10 cm s−1. No difference has been measured across the UTs, neither in throughput nor RV precision. Conclusions. The combination of the large collecting telescope area with the efficiency and the exquisite spectral fidelity of ESPRESSO opens a new parameter space in RV measurements, the study of planetary atmospheres, fundamental constants, stellar characterization, and many other fields.Publicación Acceso Abierto The Gaia -ESO Survey: Calibrating the lithium-age relation with open clusters and associations: I. Cluster age range and initial membership selections(EDP Sciences, 2020-11-05) Gutiérrez Albarrán, M. L.; Montes, D.; Gómez Garrido, M.; Tabernero, H. M.; González Hernández, J. I.; Marfil, E.; Frasca, A.; Lanzafame, A. C.; Klutsch, A.; Franciosini, E.; Randich, S.; Smiljanic, R.; Korn, A. J.; Gilmore, G.; Alfaro, Emilio J.; Baratella, M.; Bayo, A.; Bensby, T.; Bonito, R.; Carraro, G.; Delgado Mena, E.; Feltzing, S.; Gonneau, A.; Heiter, U.; Hourihane, A.; Jiménez Esteban, F. M.; Jofre, P.; Masseron, T.; Monaco, L.; Morbidelli, L.; Prisinzano, L.; Roccatagliata, V.; Sousa, S. G.; Van der Swaelmen, M.; Worley, Charlotte C.; Zaggia, S.; González Hernández, Carmen; Ministerio de Economía y Competitividad (MINECO); European Commission (EC); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); Agencia Estatal de Investigación (AEI); Fundação para a Ciência e a Tecnologia (FCT); Leverhulme Trust; 0000-0002-7569-3513; 0000-0002-7779-238X; 0000-0002-8087-4298; 0000-0002-0264-7356; 0000-0001-8907-4775; 0000-0002-0474-0896; 0000-0001-7869-3888; 0000-0003-3969-0232; 0000-0003-2438-0899; 0000-0003-0942-7855; 0000-0003-3978-1409; 0000-0001-9297-7748; 0000-0002-0155-9434; 0000-0002-3148-9836Context. Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. Aims. We perform a thorough membership analysis for a large number of stars observed within the Gaia-ESO survey (GES) in the field of 20 open clusters, ranging in age from young clusters and associations, to intermediate-age and old open clusters. Methods. Based on the parameters derived from the GES spectroscopic observations, we obtained lists of candidate members for each of the clusters in the sample by deriving radial velocity distributions and studying the position of the kinematic selections in the EW(Li)-versus-Teff plane to obtain lithium members. We used gravity indicators to discard field contaminants and studied [Fe/H] metallicity to further confirm the membership of the candidates. We also made use of studies using recent data from the Gaia DR1 and DR2 releases to assess our member selections. Results. We identified likely member candidates for the sample of 20 clusters observed in GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that allowed us to characterize the properties of these members as well as identify field contaminant stars, both lithium-rich giants and non-giant outliers. Conclusions. This work is the first step towards the calibration of the lithium-age relation and its dependence on other GES parameters. During this project we aim to use this relation to infer the ages of GES field stars, and identify their potential membership to young associations and stellar kinematic groups of different ages. © ESO 2020.Publicación Acceso Abierto Six transiting planets and a chain of Laplace resonances in TOI-178(EDP Sciences, 2021-05-06) Leleu, A.; Alibert, Y.; Hara, N. C.; Hooton, M. J.; Wilson, T. G.; Robutel, P.; Delisle, J. B.; Laskar, J.; Hoyer, S.; Lovis, C.; Bryant, E. M.; Angerhausen, D.; Simon, A. E.; Beck, T.; Sousa, S. G.; Futyan, D.; Di Marcantonio, P.; Ehrenreich, D.; Erikson, A.; Figueira, P.; Acton, J. S.; Haldemann, J.; Thomas, N.; Boué, G.; Tilbrook, R. H.; Isaak, K.; Fridlund, M.; Gandolfi, D.; García Muñoz, Antonio; García, L. J.; Verrecchia, F.; Bárczy, T.; Charnoz, S.; Lecavelier des Etangs, A.; Guillon, M.; Goad, M. R.; González Hernández, J. I.; Guedel, M.; Zapatero Osorio, M. R.; Heng, K.; Jehin, E.; Jenkins, J. S.; Jordán, A.; Kiss, L.; Anderson, D. R.; Murray, C. A.; Anglada Escudé, G.; Fortier, A.; Barrado, D.; Osborn, Hugh P.; Lam, K.; Lendl, M.; Lillo Box, J.; Lo Curto, G.; Corral Van Damme, C.; Bekkelien, A.; Gill, S.; Billot, N.; Piotto, G.; Maxted, P. F. L.; McCormac, J.; Mehner, A.; Micela, G.; Brandeker, A.; Nunes, Nelson J.; Rando, N.; Oshagh, M.; Ottensamer, R.; Pagano, I.; Pallé, E.; Cameron, A. C.; Persson, Carina; Polenta, G.; Pollacco, D.; Poretti, E.; Demangeon, O. D. S.; Sestovic, M.; Demory, B. O.; Magrin, D.; Di Persio, G.; Sozzetti, A.; Ragazzoni, R.; Ratti, F.; Rauer, H.; Raynard, L.; Fossati, L.; Molaro, P.; Nascimbeni, V.; Triaud, A.; Ribas, I.; Santos, Nuno C.; Scandariato, G.; Schneider, J.; Gillen, E.; Smith, A. M. S.; Steller, M.; Suárez Mascareño, A.; Szabó, Gy. M.; Ségransan, D.; Günther, M. N.; Ducrot, E.; Henderson, B.; Pozuelos, F. J.; Hogan, A. E.; Adibekyan, V.; Thompson, S.; Turner, O.; Udry, S.; Van Grootel, V.; Olofsson, G.; Kristiansen, M. H.; Rebolo, R.; Lavie, B.; Barros, S. C. C.; Vines, J. I.; Walton, N. A.; West, R. G.; Wheatley, Peter; Martins, C. J. A. P.; Delrez, L.; Bonfanti, A.; Allart, R.; Allende Prieto, C.; Alonso, R.; Alves, D.; Moyaro, M.; Asquier, J.; Baumjohann, W.; Bayliss, D.; Beck, M.; Pedersen, P. P.; Chamberlain, S.; Pepe, Francesco; Venus, H.; Peter, G.; Correia, A. C. M.; Benz, W.; Bonfils, X.; Bouchy, F.; Bourrier, V.; Queloz, D.; Wolter, D.; Cabrera, J.; Dumusque, X.; Broeg, C.; Buder, M.; Burdanov, A.; Burleigh, M. R.; Reimers, C.; Cooke, B. F.; Cristiani, S.; Damasso, M.; Davies, M. B.; Deleuil, M.; Sebastian, D.; González Hernández, Carmen; Alvarez, M. [0000-0002-6786-2620]; Carrasco Martínez, J. M. [0000-0002-3029-5853]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152−0.070+0.073 to 2.87−0.13+0.14 Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02−0.23+0.28 to 0.177−0.061+0.055 times the Earth’s density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.Publicación Acceso Abierto HADES RV Programme with HARPS-N at TNG XIII. A sub-Neptune around the M dwarf GJ 720 A(EDP Sciences, 2021-05-31) González Álvarez, E.; Petralia, A.; Micela, G.; Maldonado, J.; Affer, L.; Maggio, A.; Covino, E.; Damasso, M.; Lanza, A. F.; Perger, M.; Pinamonti, M.; Poretti, E.; Scandariato, G.; Sozzetti, A.; Bignamini, A.; Giacobbe, P.; Leto, G.; Pagano, I.; Zanmar Sánchez, R.; González Hernández, J. I.; Rebolo, R.; Ribas, I.; Suárez Mascareño, A.; Toledo Padrón, B.; González Hernández, Carmen; National Science Foundation (USA NSF); Agenzia Spaziale Italiana (ASI); Generalitat de Catalunya; Fundación Caixa; Agencia Estatal de Investigación (AEI); González Álvarez, E. [0000-0002-4820-2053]; Petralia, A. [0000-0002-9882-1020]; Maldonado, J. [0000-0002-2218-5689]; Affer, L. [0000-0001-5600-3778]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Context. The high number of super-Earth and Earth-like planets in the habitable zone detected around M-dwarf stars in recent years has revealed these stellar objects to be the key to planetary radial velocity (RV) searches. Aims. Using the HARPS-N spectrograph within The HArps-n red Dwarf Exoplanet Survey (HADES) we have reached the precision needed to detect small planets with a few Earth masses using the spectroscopic radial velocity technique. HADES is mainly focused on the M-dwarf population of the northern hemisphere. Methods. We obtained 138 HARPS-N RV measurements between 2013 May and 2020 September of GJ 720 A, classified as an M0.5 V star located at a distance of 15.56 pc. To characterize the stellar variability and to distinguish the periodic variation due to the Keplerian signals from those related to stellar activity, the HARPS-N spectroscopic activity indicators and the simultaneous photometric observations with the APACHE and EXORAP transit surveys were analyzed. We also took advantage of TESS, MEarth, and SuperWASP photometric surveys. The combined analysis of HARPS-N RVs and activity indicators let us address the nature of the periodic signals. The final model and the orbital planetary parameters were obtained by simultaneously fitting the stellar variability and the Keplerian signal using a Gaussian process regression and following a Bayesian criterion. Results. The HARPS-N RV periodic signals around 40 days and 100 days have counterparts at the same frequencies in HARPS-N activity indicators and photometric light curves. We thus attribute these periodicities to stellar activity; the first period is likely associated with the stellar rotation. GJ 720 A shows the most significant signal at 19.466 ± 0.005 days with no counterparts in any stellar activity indices. We hence ascribe this RV signal, having a semi-amplitude of 4.72 ± 0.27 m s−1, to the presence of a sub-Neptune mass planet. The planet GJ 720 Ab has a minimum mass of 13.64 ± 0.79 M⊕, it is in circular orbit at 0.119 ± 0.002 AU from its parent star, and lies inside the inner boundary of the habitable zone around its parent star.Publicación Acceso Abierto HADES RV programme with HARPS-N at TNG XIV. A candidate super-Earth orbiting the M-dwarf GJ 9689 with a period close to half the stellar rotation period(EDP Sciences, 2021-07-12) Maldonado, J.; Petralia, A.; Damasso, M.; Pinamonti, M.; Scandariato, G.; González Álvarez, E.; Affer, L.; Micela, G.; Lanza, A. F.; Leto, G.; Poretti, E.; Sozzetti, A.; Perger, M.; Giacobbe, P.; Zanmar Sánchez, R.; Maggio, A.; González Hernández, J. I.; Rebolo, R.; Ribas, I.; Suárez Mascareño, A.; Toledo Padrón, B.; Bignamini, A.; Molinari, E.; Covino, E.; Claudi, R.; Desidera, S.; Herrero, Enrique; Morales, J. C.; Pagano, I.; Piotto, G.; González Hernández, Carmen; Agencia Estatal de Investigación (AEI); Generalitat de Catalunya; Maldonado, J. [0000-0002-2218-5689]; Petralia, A. [0000-0002-9882-1020]; Damasso, M. [0000-0001-9984-4278]; Pinamonti, M. [0000-0002-4445-1845]; Affer, L. [0000-0001-5600-3778]; Lanza, A. F. [0000-0001-5928-7251]; Leto, G. [0000-0002-0040-5011]; Poretti, E. [0000-0003-1200-0473]; Sozzetti, A. [0000-0002-7504-365X]; Perger, M. [0000-0001-7098-0372]; Zanmar Sánchez, R. [0000-0002-6997-0887]; Maggio, A. [0000-0001-5154-6108]; González Hernández, J. I. [0000-0002-0264-7356]; Ribas, I. [0000-0002-6689-0312]; Toledo Padrón, B. [0000-0002-8194-215X]; Bignamini, A. [0000-0002-5606-6354]; Molinari, E. [0000-0002-1742-7735]; Covino, E. [0000-0002-7579-2298]; Claudi, R. [0000-0001-7707-5105]; Desidera, S. [0000-0001-8613-2589]Context. It is now well-established that small, rocky planets are common around low-mass stars. However, the detection of such planets is challenged by the short-term activity of host stars. Aims. The HARPS-N red Dwarf Exoplanet Survey programme is a long-term project at the Telescopio Nazionale Galileo aimed at monitoring nearby, early-type, M dwarfs, using the HARPS-N spectrograph to search for small, rocky planets. Methods. A total of 174 HARPS-N spectroscopic observations of the M0.5V-type star GJ 9689 taken over the past seven years have been analysed. We combined these data with photometric measurements to disentangle signals related to the stellar activity of the star from possible Keplerian signals in the radial velocity data. We ran an MCMC analysis, applying Gaussian process regression techniques to model the signals present in the data. Results. We identify two periodic signals in the radial velocity time series, with periods of 18.27 and 39.31 d. The analysis of the activity indexes, photometric data, and wavelength dependency of the signals reveals that the 39.31 d signal corresponds to the stellar rotation period. On the other hand, the 18.27 d signal shows no relation to any activity proxy or the first harmonic of the rotation period. We, therefore, identify it as a genuine Keplerian signal. The best-fit model describing the newly found planet, GJ 9689 b, corresponds to an orbital period of Pb = 18.27 ± 0.01 d and a minimum mass of MP sini = 9.65 ± 1.41 M⊕.
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