Persona: Sanz-Forcada, Jorge
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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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Sanz-Forcada
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Jorge
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Publicación Acceso Abierto Evidence of energy-, recombination-, and photon-limited escape regimes in giant planet H/He atmospheres(EDP Sciences, 2021-04-23) Lampón, M.; López Puertas, M.; Czesla, S.; Sánchez López, A.; Lara, L. M.; Salz, M.; Sanz-Forcada, Jorge; Molaverdikhani, K.; Quirrenbach, A.; Pallé, E. ; Caballero, J. A.; Henning, T.; Nortmann, L.; Amado, P. J.; Montes, D.; Reiners, A.; Ribas, I.; Consejo Superior de Investigaciones Científicas (CSIC); Junta de Andalucía; European Regional Development Fund (ERDF); Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Generalitat de Catalunya; European Research Council (ERC); Lampón, M. [0000-0002-0183-7158]; López Puertas, M. [0000-0003-2941-7734]; Sánchez López, A. [0000-0002-0516-7956]; Lara, L. M. [0000-0002-7184-920X]; Sanz Forcada, J. [0000-0002-1600-7835]; Molaverdikhani, K. [0000-0002-0502-0428]; Caballero, J. A. [0000-0002-7349-1387]; Nortmann, L. [0000-0001-8419-8760]; Amado, P. J. [0000-0001-8012-3788]; Montes, D. [0000-0002-7779-238X]; Ribas, I. [0000-0002-6689-0312]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía , SEV-2017-0709; Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Canarias, SEV-2015-0548Hydrodynamic escape is the most efficient atmospheric mechanism of planetary mass loss and has a large impact on planetary evolution. Three hydrodynamic escape regimes have been identified theoretically: energy-limited, recombination-limited, and photon-limited. However, no evidence of these regimes had been reported until now. Here, we report evidence of these three regimes via an analysis of a helium I triplet at 10 830 Å and Lyα absorption involving a 1D hydrodynamic model that allows us to estimate hydrogen recombination and advection rates. In particular, we show that HD 209458 b is in the energy-limited regime, HD 189733 b is in the recombination-limited regime, and GJ 3470 b is in the photon-limited regime. These exoplanets can be considered as benchmark cases for their respective regimes.Publicación Acceso Abierto HST PanCET program: non-detection of atmospheric escape in the warm Saturn-sized planet WASP-29 b(EDP Sciences, 2021-05-07) Dos Santos, L. A.; Bourrier, V.; Ehrenreich, D.; Sanz-Forcada, Jorge; López Morales, M.; Sing, D. K.; García Muñoz, Antonio; Henry, G. W.; Lavvas, P.; Lecavelier des Etangs, A.; Mikal Evans, T.; Vidal Madjar, A.; Wakeford, H. R.; Centre National D'Etudes Spatiales (CNES); European Research Council (ERC); Agencia Estatal de Investigación (AEI); Dos Santos, L. A. [0000-0002-2248-3838]; Sanz Forcada, J. [0000-0002-1600-7835]; López Morales, M. [0000-0003-3204-8183]; Sing, D. K. [0000-0001-6050-7645]; García Muñoz, A. [0000-0003-1756-4825]; Henry, G. W. [0000-0003-4155-8513]; Lecavelier des Etangs, A. [0000-0002-5637-5253]; Mikal Evans, T. [0000-0001-5442-1300]Short-period gas giant exoplanets are susceptible to intense atmospheric escape due to their large scale heights and strong high-energy irradiation. This process is thought to occur ubiquitously, but to date we have only detected direct evidence of atmospheric escape in hot Jupiters and warm Neptunes. The latter planets are particularly more sensitive to escape-driven evolution as a result of their lower gravities with respect to Jupiter-sized planets. But the paucity of cases for intermediate, Saturn-sized exoplanets at varying levels of irradiation precludes a detailed understanding of the underlying physics in atmospheric escape of hot gas giants. Aiming to address this issue, our objectives here are to assess the high-energy environment of the warm (Teq = 970 K) Saturn WASP-29 b and search for signatures of atmospheric escape. We used far-ultraviolet observations from the Hubble Space Telescope to analyze the flux time series of H I, C II, Si III, Si IV, and N V during the transit of WASP-29 b. At 88 pc, a large portion of the Lyman-α core of the K4V-type host WASP-29 is attenuated by interstellar medium absorption, limiting our ability to probe the escape of H at velocities between −84 and +35 km s−1. At 3σ confidence, we rule out any in-transit absorption of H I larger than 92% in the Lyman-α blue wing and 19% in the red wing. We found an in-transit flux decrease of 39%−11%+12% in the ground-state C II emission line at 1334.5 Å. But due to this signal being significantly present in only one visit, it is difficult to attribute a planetary or stellar origin to the ground-state C II signal. We place 3σ absorption upper limits of 40, 49, and 24% on Si III, Si IV, and for excited-state C II at 1335.7 Å, respectively. Low activity levels and the faint X-ray luminosity suggest that WASP-29 is an old, inactive star. Nonetheless, an energy-limited approximation combined with the reconstructed EUV spectrum of the host suggests that the planet is losing its atmosphere at a relatively large rate of 4 × 109 g s−1. The non-detection at Lyman-α could be partly explained by a low fraction of escaping neutral hydrogen, or by the state of fast radiative blow-out we infer from the reconstructed Lyman-α line.Publicación Acceso Abierto The EChO science case(Springer Link, 2015-11-29) Tinetti, G.; Drossart, P.; Eccleston, P.; Hartogh, P.; Isaak, K.; Linder, M.; Lovis, C.; Micela, G.; Olliver, M.; Puig, L.; Ribas, I.; Sicardy, B.; Kehoe, T.; Deeg, H.; Petrov, R.; Doel, P.; Tennyson, J.; Filacchione, G.; Varley, R.; Temple, J.; Lahav, O.; MacTavish, C.; Wisniowski, T.; Piccioni, G.; Guàrdia, J.; Cavarroc, C.; Jones, G.; Ade, P.; Sanromá, E.; Frith, J.; Lognonné, P.; Pantin, E.; Crook, J.; Colomé, J.; Allard, F.; Azzollini, R.; Burston, R.; Parviainen, H.; Malaguti, G.; Gerard, J. C.; Stamper, R.; Barrado, David; Maldonado, J.; Morales, J. C.; Yurchenko, S. N.; Lagage, P. O.; Prinja, R.; Koskinen, T.; Waldmann, I.; Venot, O.; Heiter, U.; Lim, T.; Pace, E.; Moya Bedon, A.; Irwin, P.; Michaut, C.; Monteiro, M.; Jones, H.; Wawer, P.; Fouqué, P.; Widemann, T.; Alonso Floriano, F. J.; Eiroa, C.; Savini, G.; Stixrude, L.; Damasso, M.; Rataj, M.; Glasse, A.; Koskinen, T.; Bulgarelli, A.; Ciaravella, A.; Hollis, M.; Schmider, F. X.; Kerschbaum, F.; Licandro Goldaracena, J.; Claret, A.; Rocchetto, M.; López Valverde, Miguel Ángel; Fossey, S.; Leto, G.; Ramos Zapata, G.; Beaulieu, J. P.; Balado, A.; Luzzi, D.; Rebordao, J.; Encrenaz, T.; Adriani, A.; Alcala, J.; Guedel, M.; Morales Calderón, M.; Peña Ramírez, K. Y.; Herrero, Enrique; Focardi, M.; Montalto, M.; Wright, G.; Danielski, C.; Burleigh, M. R.; Medvedev, A.; Murgas Alcaino, F. ; Chadney, J.; Bowles, N.; Maxted, Pierre; Kerschbaum, F.; Ward Thompson, D.; Laken, B.; Börne, P.; Christian Jessen, N.; Dominic, C.; López Morales, M.; Miles Paez, P.; Achilleos, N.; Biondi, D.; White, G.; López Heredero, Raquel; De Kok, R.; Frith, J.; Grodent, D.; Rank Lüftinger, T.; Scholz, A.; Villaver, E.; Dobrijévic, M.; Alard, C.; Demangeon, O. D. S.; De Witt, J.; Machado, P.; Cordier, D.; Charnoz, S.; Rodler, F.; Gerard, J. C.; Sousa, S. G.; Viti, S.; Cole, R.; Blecka, M.; Barber, R. J.; Middleton, K.; Griffin, M.; Giro, E.; Cho, J.; Covino, E.; Turrini, D.; Moro Martín, A.; Decin, L.; Ramos, A. A.; Schrader, J. R.; Massi, F.; Abe, L.; Mauskopf, P.; Batista, V.; Agnor, C.; Bordé, P.; Fabrizio, N.; Bakos, G.; Rengel, M.; Gustin, J.; Hueso, R.; Fernández Hernández, Maite; Ray, T.; Claudi, R.; Femenía Castella, B.; Rebolo, R.; Sethenadh, J.; Luntzer, A.; Mueller Wodarg, I.; Delgado Mena, E.; Brown, L.; De Sio, A.; González Hernández, J.; Selsis, F.; Leconte, J.; Del Vecchio, C.; Budaj, J.; Scandariato, G.; Pagano, I.; García Piquer, A.; Guillot, T.; Terenzi, L.; Tabernero, H. M. ; Forget, F.; Hargrave, P.; North, C.; Heyrovsky, D.; Cerulli, R.; Adybekian, V.; Read, P.; Pinsard, Frederic; Parmentier, V.; Collura, A.; Hubert, B.; Lanza, N.; Graczyk, R.; Fouqué, P.; Giuranna, M.; Valdivieso, M. L.; Pérez Hoyos, S.; Andersen, A.; Mall, U.; Buchhave, L. A.; Yelle, R.; Rickman, H.; Ballerini, P.; Affer, L.; Maruquette, J. B.; Sánchez Béjar, V. J.; Nelson, Richard; Fletcher, L.; Radioti, A.; Turrini, D.; Montes, D.; Gizon, L.; Galand, M.; Gómez, H.; Eymet, V.; Esposito, M.; Smith, A.; Morello, G.; Allende Prieto, C.; Justtanot, K.; Bryson, I.; Pallé, E. ; Amado, P. J.; Figueira, P.; Shore, Steven; Focardi, M.; Strazzulla, G.; Giani, E.; Pietrzak, R.; González Merino, B.; Lo Cicero, Ugo; Gaulme, P.; Sozzetti, A.; Femenía Castella, B.; Maillard, J. P.; Cabral, A.; Iro, N.; Magnes, W.; Pinfield, David J.; Swain, M.; Showman, A.; Bellucci, G.; Kerins, E.; Maurin, A. S.; Poretti, E.; Boisse, I.; Barton, E. J.; Kervella, P.; Guio, P.; Norgaard Nielsen, H. U.; Bézard, B.; Montañés Rodríguez, P.; Banaszkiewicz, M.; Kovács, G.; Baffa, C.; Del Val Borro, M.; Belmonte Avilés, J. A.; Palla, F.; Hersant, F.; Correira, A.; Yung, Y.; Cockell, Charles S.; Vinatier, S.; Pilat Lohinger, E.; Krupp, N.; Orton, G.; Vakili, F.; Pezzuto, S.; Di Giorgio, A.; Waltham, D.; Testi, L.; Stiepen, A.; Deroo, P.; Capria, M. T.; Eales, S.; Irshad, R.; Stolarski, M.; Zapatero Osorio, María Rosa; Swinyard, B.; Griffith, C.; Winek, W.; Bouy, H.; Thompson, S.; Maggio, A.; Moses, J.; Liu, S. J.; Lithgow Bertelloni, C.; Coudé du Foresto, V.; Martín Torres, Javier; Fletcher, L.; Barlow, M.; Coustenis, A.; Berry, D.; López Puertas, M.; Banaszkiewicz, M.; Lundgaard Rasmussen, I.; Hoogeveen, Ruud; Morais, H.; Watkins, C.; Oliva, E.; Scuderi, S.; Aylward, A.; Bonford, B.; Sitek, P.; Haigh, J.; Prisinzano, L.; Soret, Lauriane; Wawrzaszk, A.; Lammer, H.; Figueira, P.; Gianotti, F.; Readorn, K.; Tanga, P.; Israelian, G.; Gesa, L.; Peralta, J.; Gómez Leal, I.; Cassan, A.; Tecsa, M.; Tessenyi, M.; Pancrazzi, M.; Coates, A.; Gambicorti, L.; Gear, W.; Winter, B.; Piskunov, N.; Álvarez Iglesias, C. A.; Polichtchouk, I.; Altieri, F.; Ottensamer, R.; Watson, D.; Rezac, L.; Vandenbussche, B.; Waters, R.; Dorfi, E.; Morgante, G.; Pascale, E.; Hornstrup, A.; Snellen, Ignas; Lodieu, N.; Lellouch, E.; Espinoza Contreras, M.; Jarchow, C.; Agúndez, Marcelino ; Filacchione, G.; Abreu, M.; Grassi, D.; Tingley, B. W.; Sánchez Lavega, Agustín; Tozzi, A.; Sanz-Forcada, Jorge; Kipping, D.; Chamberlain, S.; Trifoglio, M.; Barstow, J. K.; Santos, Nuno C. ; Gillon, M.; Hébrard, E.; Cecchi Pestellini, C.; Fossey, S.; García López, Ramón ; Thrastarson, H.; Rees, J. M.; Selig, A.; Galand, M.; Jacquemoud, S.; Branduardi Raymont, Graziella; Rebordao, J. [0000-0002-7418-0345]; Kerschbaum, F. [0000-0001-6320-0980]; Abreu, M. [0000-0002-0716-9568]; Tabernero, H. [0000-0002-8087-4298]; López Puertas, M. [0000-0003-2941-7734]; Jacquemoud, S. [0000-0002-1500-5256]; Tennyson, J. [0000-0002-4994-5238]; Focardi, M. [0000-0002-3806-4283]; Leto, G. [0000-0002-0040-5011]; Lodieu, N. [0000-0002-3612-8968]; Tinetti, G. [0000-0001-6058-6654]; Danielski, C. [0000-0002-3729-2663]; Hornstrup, A. [0000-0002-3363-0936]; Kervella, P. [0000-0003-0626-1749]; Sánchez Bejar, V. [0000-0002-5086-4232]; López Heredero, R. [0000-0002-2197-8388]; Sanz Forcada, J. [0000-0002-1600-7835]; Rickman, H. [0000-0002-9603-6619]; Maggio, A. [0000-0001-5154-6108]; Medved, A. [0000-0003-2713-8977]; Tinetti, G. [0000-0001-6058-6654]; Fletcher, L. [0000-0001-5834-9588]; Haigh, J. [0000-0001-5504-4754]; Bakos, G. [0000-0001-7204-6727]; Stixrude, L. [0000-0003-3778-2432]; Amado, P. J. [0000-0002-8388-6040]; Martín Torres, J. [0000-0001-6479-2236]; Correira, A. [0000-0002-8946-8579]; Yurchenko, S. [0000-0001-9286-9501]; Rataj, M. [0000-0002-2978-9629]; Guedel, M. [0000-0001-9818-0588]; Piskunov, N. [0000-0001-5742-7767]; Filacchione, G. [0000-0001-9567-0055]; Adibekyan, V. [0000-0002-0601-6199]; Budaj, J. [0000-0002-9125-7340]; Poretti, E. [0000-0003-1200-0473]; Pascale, E. [0000-0002-3242-8154]; Claudi, R. [0000-0001-7707-5105]; Piccioni, G. [0000-0002-7893-6808]; Ribas, I. [0000-0002-6689-0312]; Sanroma, E. [0000-0001-8859-7937]; Agundez, M. [0000-0003-3248-3564]; Montes, D. [0000-0002-7779-238X]; Lognonne, P. [0000-0002-1014-920X]; Abreu, M. [0000-0002-0716-9568]; Montes, D. [0000-0002-7779-238X]; Morais, M. H. [0000-0001-5333-2736]; Tanga, P. [0000-0002-2718-997X]; Peralta, J. [0000-0002-6823-1695]; Hueso, R. [0000-0003-0169-123X]; Leto, G. [0000-0002-0040-5011]; Morales, J. C. [0000-0003-0061-518X]; Pérez Hoyos, S. [0000-0002-2587-4682]; Santos, N. [0000-0003-4422-2919]; Lithgow Bertelloni, C. [0000-0003-0924-6587]; Delgado, M. E. [0000-0003-4434-2195]; Barlow, M. [0000-0002-3875-1171]; Deeg, H. [0000-0003-0047-4241]; Bouy, H. [0000-0002-7084-487X[; Grassi, D. [0000-0003-1653-3066]; Figueira, P. [0000-0001-8504-283X]; Barton, E. [0000-0001-5945-9244]; Coates, A. [0000-0002-6185-3125]; García Ramón, J. [0000-0002-8204-6832]; Watson, D. [0000-0002-4465-8264]; Morales Calderon, M. [0000-0001-9526-9499]; Demangeon, O. [0000-0001-7918-0355]; Ray, T. [0000-0002-2110-1068]; Guio, P. [0000-0002-1607-5862]; Gillon, M. [0000-0003-1462-7739]; Bulgarelli, A. [0000-0001-6347-0649]; Prisinzano, L. [0000-0002-8893-2210]; Barstow, J. [0000-0003-3726-5419]; Pancrazzi, M. [0000-0002-3789-2482]; Barrado Navascues, D. [0000-0002-5971-9242]; Balado, A. [0000-0003-4268-2516]; Malaguti, G. [0000-0001-9872-3378]; Zapatero Osorio, M. R. [0000-0001-5664-2852]; Affer, L. [0000-0001-5600-3778]; Ciaravella, A. [0000-0002-3127-8078]; Guillot, T. [0000-0002-7188-8428]; Altieri, F. [0000-0002-6338-8300]; Covino, E. [0000-0002-6187-6685]; Venot, O. [0000-0003-2854-765X]; López Valverde, M. A. [0000-0002-7989-4267]; Cabral, A. [0000-0002-9433-871X]; Selsis, F. [0000-0001-9619-5356]; Turrini, D. [0000-0002-1923-7740]; Ward Thompson, D. [0000-0003-1140-2761]; Rebolo, R. [0000-0003-3767-7085]; Damasso, M. [0000-0001-9984-4278]; Tizzi, A. [0000-0002-6725-3825]; Morgante, G. [0000-0001-9234-7412]; Pena Ramírez, K. [0000-0002-5855-401X]; Galand, M. [0000-0001-5797-914X]; Pace, E. [0000-0001-5870-1772]; Pilat Lohinger, E. [0000-0002-5292-1923]; Sánchez Lavega, A. [0000-0001-7234-7634]; Waldmann, I. [0000-0002-4205-5267]; Claret, A. [0000-0002-4045-8134]; Olivia, E. [0000-0002-9123-0412]; Kovacs, G. [0000-0002-2365-2330]; Gómez, H. [0000-0003-3398-0052]; Monteiro, M. [0000-0001-5644-0898]; Bellucci, G. [0000-0003-0867-8679]; Baffa, C. [0000-0002-4935-100X]; Scholz, A. [0000-0001-8993-5053]; Bezard, B. [0000-0002-5433-5661]; Scuderi, Salvatore [0000-0002-8637-2109]; Hersant, F. [0000-0002-2687-7500]; Maldonado, J. [0000-0002-4282-1072]; Gear, W. [0000-0001-6789-6196]; Sousa, S. [0000-0001-9047-2965]; Irwin, P. [0000-0002-6772-384X]; Pinfield, D. [0000-0002-7804-4260]; Kipping, D. [0000-0002-4365-7366]; Ade, P. [0000-0002-5127-0401]; Vandenbussche, B. [0000-0002-1368-3109]; Burleigh, M. [0000-0003-0684-7803]; Chadney, J. [0000-0002-5174-2114]; Moro Martín, A. [0000-0001-9504-8426]; Scandariato, G. [0000-0003-2029-0626]; Rodríguez, P. [0000-0002-6855-9682]; Maldonado, J. [0000-0002-2218-5689]; Michaut, C. [0000-0002-2578-0117]; Pérez Hoyos, S. [0000-0001-9797-4917]The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune—all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10−4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R ~ 300 for wavelengths less than 5 μm and R ~ 30 for wavelengths greater than this. The transit spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate than current observations. This would enable the detection of molecular abundances three orders of magnitude lower than currently possible and a fourfold increase from the handful of molecules detected to date. Combining these data with estimates of planetary bulk compositions from accurate measurements of their radii and masses would allow degeneracies associated with planetary interior modelling to be broken, giving unique insight into the interior structure and elemental abundances of these alien worlds. EChO would allow scientists to study exoplanets both as a population and as individuals. The mission can target super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300–3000 K) of F to M-type host stars. The EChO core science would be delivered by a three-tier survey. The EChO Chemical Census: This is a broad survey of a few-hundred exoplanets, which allows us to explore the spectroscopic and chemical diversity of the exoplanet population as a whole. The EChO Origin: This is a deep survey of a subsample of tens of exoplanets for which significantly higher signal to noise and spectral resolution spectra can be obtained to explain the origin of the exoplanet diversity (such as formation mechanisms, chemical processes, atmospheric escape). The EChO Rosetta Stones: This is an ultra-high accuracy survey targeting a subsample of select exoplanets. These will be the bright “benchmark” cases for which a large number of measurements would be taken to explore temporal variations, and to obtain two and three dimensional spatial information on the atmospheric conditions through eclipse-mapping techniques. If EChO were launched today, the exoplanets currently observed are sufficient to provide a large and diverse sample. The Chemical Census survey would consist of > 160 exoplanets with a range of planetary sizes, temperatures, orbital parameters and stellar host properties. Additionally, over the next 10 years, several new ground- and space-based transit photometric surveys and missions will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO’s launch and enable the atmospheric characterisation of hundreds of planets.Publicación Acceso Abierto The CARMENES search for exoplanets around M dwarfs: A super-Earth planet orbiting HD 79211 (GJ 338 B)(EDP Sciences, 2020-05-27) González Álvarez, E.; Zapatero Osorio, María Rosa; Caballero, J. A.; Sanz-Forcada, Jorge; Béjar, V. J. S.; González Cuesta, L.; Dreizler, S.; Bauer, F. F.; Rodríguez, E.; Tal Or, L.; Zechmeister, M.; Montes, D.; López González, M. J.; Ribas, I.; Reiners, A.; Quirrenbach, A.; Amado, P. J.; Anglada Escudé, G.; Azzaro, M.; Cortés Contreras, M.; Hatzes, Artie ; Henning, T.; Jeffers, S. V.; Kaminski, A.; Kürster, M.; Lafarga, M.; Morales, J. C.; Pallé, E. ; Perger, M.; Schmitt, H. M. M.; Agencia Estatal de Investigación (AEI); González Álvarez, E. https://orcid.org/0000-0002-4820-2053; Zapatero Osorio, M. R.https://orcid.org/0000-0001-5664-2852; Caballero, J. A. https://orcid.org/0000-0002-7349-1387; López González, M. J. https://orcid.org/0000-0002-0011-3086; 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-2017-0709Aims. We report on radial velocity time series for two M0.0 V stars, GJ 338 B and GJ 338 A, using the CARMENES spectrograph, complemented by ground-telescope photometry from Las Cumbres and Sierra Nevada observatories. We aim to explore the presence of small planets in tight orbits using the spectroscopic radial velocity technique. Methods. We obtained 159 and 70 radial velocity measurements of GJ 338 B and A, respectively, with the CARMENES visible channel between 2016 January and 2018 October. We also compiled additional relative radial velocity measurements from the literature and a collection of astrometric data that cover 200 a of observations to solve for the binary orbit. Results. We found dynamical masses of 0.64 ± 0.07 M° for GJ 338 B and 0.69 ± 0.07 M° for GJ 338 A. The CARMENES radial velocity periodograms show significant peaks at 16.61 ± 0.04 d (GJ 338 B) and 16.3-1.3+3.5 d (GJ 338 A), which have counterparts at the same frequencies in CARMENES activity indicators and photometric light curves. We attribute these to stellar rotation. GJ 338 B shows two additional, significant signals at 8.27 ± 0.01 and 24.45 ± 0.02 d, with no obvious counterparts in the stellar activity indices. The former is likely the first harmonic of the star's rotation, while we ascribe the latter to the existence of a super-Earth planet with a minimum mass of 10.27-1.38+1.47 M⊕ orbiting GJ 338 B. We have not detected signals of likely planetary origin around GJ 338 A. Conclusions. GJ 338 Bb lies inside the inner boundary of the habitable zone around its parent star. It is one of the least massive planets ever found around any member of stellar binaries. The masses, spectral types, brightnesses, and even the rotational periods are very similar for both stars, which are likely coeval and formed from the same molecular cloud, yet they differ in the architecture of their planetary systems. © ESO 2020.Publicación Acceso Abierto Modelling the He i triplet absorption at 10 830 A in the atmosphere of HD 209458 b(EDP Sciences, 2020-04-07) Lampón, M.; López Puertas, M.; Lara, L. M.; Sánchez López, A.; Salz, M.; Czesla, S.; Sanz-Forcada, Jorge; Molaverdikhani, K.; Alonso Floriano, F. J.; Nortmann, L.; Caballero, J. A.; Bauer, F. F.; Pallé, E. ; Montes, D.; Quirrenbach, A.; Nagel, E.; Ribas, I.; Reiners, A.; Amado, P. J.; Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); Ministerio de Economía y Competitividad (MINECO); Junta de Andalucía; 0000-0002-0183-7158; 0000-0003-2941-7734; 0000-0002-7184-920X; 0000-0002-0516-7956; 0000-0002-0502-0428; 0000-0002-7349-1387; 0000-0003-1212-5225; 0000-0003-0987-1593; 0000-0002-7779-238X; 0000-0002-4019-3631; 0000-0002-6689-0312; 0000-0002-8388-6040; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709Context. HD 209458 b is an exoplanet with an upper atmosphere undergoing blow-off escape that has mainly been studied using measurements of the Lyα absorption. Recently, high-resolution measurements of absorption in the He I triplet line at 10 830 A of several exoplanets (including HD 209458 b) have been reported, creating a new opportunity to probe escaping atmospheres. Aims. We aim to better understand the atmospheric regions of HD 209458 b from where the escape originates. Methods. We developed a 1D hydrodynamic model with spherical symmetry for the HD 209458 b thermosphere coupled with a non-local thermodynamic model for the population of the He I triplet state. In addition, we performed high-resolution radiative transfer calculations of synthetic spectra for the helium triplet lines and compared them with the measured absorption spectrum in order to retrieve information about the atmospheric parameters. Results. We find that the measured spectrum constrains the [H]/[H+] transition altitude occurring in the range of 1.2 RP-1.9 RP. Hydrogen is almost fully ionised at altitudes above 2.9 RP. We also find that the X-ray and extreme ultraviolet absorption takes place at effective radii from 1.16 to 1.30 RP, and that the He I triplet peak density occurs at altitudes from 1.04 to 1.60 RP. Additionally, the averaged mean molecular weight is confined to the 0.61-0.73 g mole-1 interval, and the thermospheric H/He ratio should be larger than 90/10, and most likely approximately 98/2. We also provide a one-to-one relationship between mass-loss rate and temperature. Based on the energy-limited escape approach and assuming heating efficiencies of 0.1-0.2, we find a mass-loss rate in the range of (0.42-1.00) ×1011 g s-1 and a corresponding temperature range of 7125-8125 K. Conclusions. The analysis of the measured He I triplet absorption spectrum significantly constrains the thermospheric structure of HD 209458 b and advances our knowledge of its escaping atmosphere. © ESO 2020.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 The Hubble PanCET program: long-term chromospheric evolution and flaring activity of the M dwarf host GJ 3470(EDP Sciences, 2021-06-08) Bourrier, V.; Dos Santos, L. A.; Sanz-Forcada, Jorge; García Muñoz, Antonio; Henry, G. W.; Lavvas, P.; Lecavelier des Etangs, A.; López Morales, M.; Mikal Evans, T.; Sing, D. K.; Wakeford, H. R.; Ehrenreich, D.; European Research Council (ERC)Neptune-size exoplanets seem particularly sensitive to atmospheric evaporation, making it essential to characterize the stellar high-energy radiation that drives this mechanism. This is particularly important with M dwarfs, which emit a large and variable fraction of their luminosity in the ultraviolet and can display strong flaring behavior. The warm Neptune GJ 3470b, hosted by an M2 dwarf, was found to harbor a giant exosphere of neutral hydrogen thanks to three transits observed with the Hubble Space Telescope Imaging Spectrograph (HST/STIS). Here we report on three additional transit observations from the Panchromatic Comparative Exoplanet Treasury program, obtained with the HST Cosmic Origin Spectrograph. These data confirm the absorption signature from GJ 3470b’s exosphere in the stellar Lyman-α line and demonstrate its stability over time. No planetary signatures are detected in other stellar lines, setting a 3σ limit on GJ 3470b’s far-ultraviolet (FUV) radius at 1.3 times its Roche lobe radius. We detect three flares from GJ 3470. They show different spectral energy distributions but peak consistently in the Si III line, which traces intermediate-temperature layers in the transition region. These layers appear to play a particular role in GJ 3470’s activity as emission lines that form at lower or higher temperatures than Si III evolved differently over the long term. Based on the measured emission lines, we derive synthetic X-ray and extreme-ultraviolet (X+EUV, or XUV) spectra for the six observed quiescent phases, covering one year, as well as for the three flaring episodes. Our results suggest that most of GJ 3470’s quiescent high-energy emission comes from the EUV domain, with flares amplifying the FUV emission more strongly. The neutral hydrogen photoionization lifetimes and mass loss derived for GJ 3470b show little variation over the epochs, in agreement with the stability of the exosphere. Simulations informed by our XUV spectra are required to understand the atmospheric structure and evolution of GJ 3470b and the role played by evaporation in the formation of the hot-Neptune desert.Publicación Acceso Abierto Modelling the He I triplet absorption at 10 830 Å in the atmospheres of HD 189733 b and GJ 3470 b(EDP Sciences, 2021-03-23) Lampón, M.; López Puertas, M.; Sanz-Forcada, Jorge; Sánchez López, A.; Molaverdikhani, K. ; Czesla, S.; Quirrenbach, A.; Pallé, E. ; Caballero, J. A.; Henning, T.; Salz, M.; Nortmann, L.; Aceituno, J.; Amado, P. J.; Bauer, F. F.; Montes, D.; Nagel, E.; Reiners, A.; Ribas, I.; European Regional Development Fund (ERDF); Deutsche Forschungsgemeinschaft (DFG); Agencia Estatal de Investigación (AEI); Generalitat de Catalunya; European Research Council (ERC); 0000-0002-0183-7158; 0000-0003-2941-7734; 0000-0002-1600-7835; 0000-0002-0516-7956; 0000-0002-7349-1387; 0000-0001-8419-8760; 0000-0001-8012-3788; 0000-0002-4019-3631; 0000-0002-6689-0312; 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 ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709Characterising the atmospheres of exoplanets is key to understanding their nature and provides hints about their formation and evolution. High resolution measurements of the helium triplet absorption of highly irradiated planets have been recently reported, which provide a new means of studying their atmospheric escape. In this work we study the escape of the upper atmospheres of HD 189733 b and GJ 3470 b by analysing high resolution He I triplet absorption measurements and using a 1D hydrodynamic spherically symmetric model coupled with a non-local thermodynamic model for the He I triplet state. We also use the H density derived from Lyα observations to further constrain their temperatures, mass-loss rates, and H/He ratios. We have significantly improved our knowledge of the upper atmospheres of these planets. While HD 189733 b has a rather compressed atmosphere and small gas radial velocities, GJ 3470 b, on the other hand with a gravitational potential ten times smaller, exhibits a very extended atmosphere and large radial outflow velocities. Hence, although GJ 3470 b is much less irradiated in the X-ray and extreme ultraviolet radiation, and its upper atmosphere is much cooler, it evaporates at a comparable rate. In particular, we find that the upper atmosphere of HD 189733 b is compact and hot, with a maximum temperature of 12 400−300+400 K, with a very low mean molecular mass (H/He = (99.2/0.8) ± 0.1), which is almost fully ionised above 1.1 RP, and with a mass-loss rate of (1.1 ± 0.1) × 1011 g s−1. In contrast, the upper atmosphere of GJ 3470 b is highly extended and relatively cold, with a maximum temperature of 5100 ± 900 K, also with a very low mean molecular mass (H/He = (98.5/1.5)−1.5+1.0), which is not strongly ionised, and with a mass-loss rate of (1.9 ± 1.1) × 1011 g s−1. Furthermore, our results suggest that upper atmospheres of giant planets undergoing hydrodynamic escape tend to have a very low mean molecular mass (H/He ≳ 97/3).Publicación Acceso Abierto The CARMENES search for exoplanets around M dwarfs The He I triplet at 10830 Å across the M dwarf sequence(EDP Sciences, 2019-11-25) Fuhrmeister, B.; Czesla, S.; Hildebrandt, L.; Nagel, E.; Schmitt, H. M. M.; Hintz, D.; Johnson, E. N.; Sanz-Forcada, Jorge; Schöfer, P.; Jeffers, S. V.; Caballero, J. A.; Zechmeister, M.; Reiners, A.; Ribas, I.; Amado, P. J.; Quirrenbach, A.; Bauer, F. F.; Béjar, V. J. S.; Cortés Contreras, M.; Díez Alonso, E.; Dreizler, S.; Galadí Enríquez, D.; Guenther, E. W.; Kaminski, A.; Kürster, M.; Lafarga, M.; Montes, D.; Deutsche Forschungsgemeinschaft (DFG); Ministerio de Economía y Competitividad (MINECO); Agencia Estatal de Investigación (AEI); Ribas, I. [0000-0002-6689-0312]; Montes, D. [0000-0002-7779-238X]; Lafarga, M. [0000-0002-8815-9416]; Amado, P. [0000-0001-8012-3788]; Nagel, E. [0000-0002-4019-3631]; 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; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548The He I infrared (IR) triplet at 10 830 Å is an important activity indicator for the Sun and in solar-type stars, however, it has rarely been studied in relation to M dwarfs to date. In this study, we use the time-averaged spectra of 319 single stars with spectral types ranging from M0.0 V to M9.0 V obtained with the CARMENES high resolution optical and near-infrared spectrograph at Calar Alto to study the properties of the He I IR triplet lines. In quiescence, we find the triplet in absorption with a decrease of the measured pseudo equivalent width (pEW) towards later sub-types. For stars later than M5.0 V, the He I triplet becomes undetectable in our study. This dependence on effective temperature may be related to a change in chromospheric conditions along the M dwarf sequence. When an emission in the triplet is observed, we attribute it to flaring. The absence of emission during quiescence is consistent with line formation by photo-ionisation and recombination, while flare emission may be caused by collisions within dense material. The He I triplet tends to increase in depth according to increasing activity levels, ultimately becoming filled in; however, we do not find a correlation between the pEW(He IR) and X-ray properties. This behaviour may be attributed to the absence of very inactive stars (LX∕Lbol < −5.5) in our sample or to the complex behaviour with regard to increasing depth and filling in.Publicación Acceso Abierto Evidence of a Clear Atmosphere for WASP-62b: The Only Known Transiting Gas Giant in the JWST Continuous Viewing Zone(IOP Science Publishing, 2021-01-11) Alam, M. K.; López Morales, M.; MacDonald, R. J.; Nikolov, N.; Kirk, J.; Goyal, J. M.; Sing, D. K.; Wakeford, H. R.; Rathcke, A. D.; Deming, D. L.; Sanz-Forcada, Jorge; Lewis, N. K.; Barstow, J. K.; Mikal Evans, T.; Buchhave, L. A.; National Aeronautics and Space Administration (NASA); National Science Foundation (NSF); Agencia Estatal de Investigación (AEI); Alam, M. K. [0000-0003-4157-832X]; López Morales, M. [0000-0003-3204-8183]; MacDonald, R. J. [0000-0003-4816-3469]; Nikolov, N. [0000-0002-6500-3574]; Kirk, J. [0000-0002-4207-6615]; Goyal, J. M. [0000-0002-8515-7204]; Sing, D. K. [0000-0001-6050-7645]; Wakeford, H. R. [0000-0003-4328-3867]; Rathcke, A. D. [0000-0002-4227-4953]; Deming, D. L. [0000-0001-5727-4094]; Sanz Forcada, J. [0000-0002-1600-7835]; Lewis, N. K. [0000-0002-8507-1304]; Barstow, J. K. [0000-0003-3726-5419]; Mikal Evans, T. [0000-0001-5442-1300]; Buchhave, L. A. [0000-0003-1605-5666]Exoplanets with cloud-free, haze-free atmospheres at the pressures probed by transmission spectroscopy represent a valuable opportunity for detailed atmospheric characterization and precise chemical abundance constraints. We present the first optical to infrared (0.3−5 μm) transmission spectrum of the hot Jupiter WASP-62b, measured with Hubble/STIS and Spitzer/IRAC. The spectrum is characterized by a 5.1σ detection of Na i absorption at 0.59 μm, in which the pressure-broadened wings of the Na D-lines are observed from space for the first time. A spectral feature at 0.4 μm is tentatively attributed to SiH at 2.1σ confidence. Our retrieval analyses are consistent with a cloud-free atmosphere without significant contamination from stellar heterogeneities. We simulate James Webb Space Telescope (JWST) observations, for a combination of instrument modes, to assess the atmospheric characterization potential of WASP-62b. We demonstrate that JWST can conclusively detect Na, H2O, FeH, NH3, CO, CO2, CH4, and SiH within the scope of its Early Release Science (ERS) program. As the only transiting giant planet currently known in the JWST Continuous Viewing Zone, WASP-62b could prove a benchmark giant exoplanet for detailed atmospheric characterization in the James Webb era.
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