Examinando por Autor "Isaak, K."

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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.; Ducrot, E.; Gillen, E.; Alonso, R.; Pepe, F. A.; Correia, A. C. M.; Alves, D.; Cooke, B. F.; Cristiani, S.; Damasso, M.; Simon, A. E.; Angerhausen, D.; Günther, M. N.; Beck, M.; Queloz, D.; Dumusque, X.; Beck, T.; Di Marcoantonio, P.; Ehrenreich, D.; Erikson, A.; Olofsson, G.; Bourrier, V.; Reimers, C.; Futyan, D.; Boué, G.; Fridlund, M.; Gandolfi, D.; García Muñoz, Antonio; Peter, G.; Burleigh, M. R.; Bárczy, T.; Guillon, M.; Goad, M. R.; Cabrera, J.; Chamberlain, S.; Moyaro, M.; Davies, M. B.; Thomas, N.; Isaak, K.; Deleuil, M.; Heng, K.; Jehin, E.; Jenkins, J. S.; Anglada Escudé, G.; Pedersen, P. P.; Figueira, P.; Verrecchia, F.; Lecavelier des Etangs, A.; Fortier, A.; Lam, K.; Lendl, M.; Lillo Box, J.; Sousa, S. G.; García, L. J.; Osborn, Hugh P.; Gill, S.; Maxted, P. F. L.; McCormac, J.; Mehner, A.; Tilbrook, R. H.; Guedel, M.; Nunes, N. J.; Oshagh, M.; Ottensamer, R.; Charnoz, S.; Haldemann, J.; Sebastian, D.; Jordán, A.; Bekkelien, A.; Piotto, G.; Kiss, L.; Persson, C. M.; Polenta, G.; Pollacco, D.; Acton, J. S.; Lo Curto, G.; Brandeker, A.; Rando, N.; Magrin, D.; Ragazzoni, R.; Ratti, F.; Rauer, H.; Barrado, D.; Micela, G.; Molaro, P.; Ribas, I.; Santos, N. C.; Scandariato, G.; Billot, N.; Murray, C. A.; Zapatero Osorio, M. R.; Pagano, I.; Demory, B. O.; Sozzetti, A.; Pallé, E.; Smith, A. M. S.; Steller, M.; Suárez Mascareño, A.; Henderson, B.; Anderson, D. R.; Poretti, E.; Fossati, L.; Triaud, A.; Pozuelos, F. J.; Thompson, S.; Turner, O.; Udry, S.; Corral Van Damme, C.; Raynard, L.; Adibekyan, V.; Rebolo, R.; Vines, J. I.; Walton, N. A.; West, R. G.; Di Persio, G.; Schneider, J.; Delrez, L.; Allart, R.; Allende Prieto, C.; Nascimbeni, V.; Sestovic, M.; Cameron, A. C.; Szabó, G. M.; Kristiansen, M. H.; Barros, S. C. C.; Ségransan, D.; Asquier, J.; Baumjohann, W.; Bayliss, D.; Demangeon, O. D. S.; Van Grootel, V.; Martins, C. J. A. P.; Bonfanti, A.; Venus, H.; Benz, W.; Bonfils, X.; Bouchy, F.; Hogan, A. E.; Wheatley, P. J.; Wolter, D.; Broeg, C.; Buder, M.; Burdanov, A.; Lavie, B.; 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-2017-0737
Determining 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.
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.; Schrader, J. R.; Scholz, A.; Watkins, C.; Maillard, J. P.; Abreu, M.; Glasse, A.; Testi, L.; Doel, P.; Magnes, W.; Licandro Goldaracena, J.; Wawer, P.; Zapatero Osorio, M. R.; Decin, L.; Sánz Forcada, J.; Vakili, F.; Aylward, A.; Swain, M.; Sozzetti, A.; Filacchione, G.; Delgado Mena, E.; Read, P.; Lognonné, P.; Irshad, R.; Coates, A.; Cecchi Pestellini, C.; Thrastarson, H.; Brown, L.; Guillot, T.; Strazzulla, G.; Barstow, J. K.; Budaj, J.; Morgante, G.; Pietrzak, R.; Leconte, J.; Hersant, F.; De Sio, A.; Grassi, D.; Selsis, F.; Jarchow, C.; Fouqué, P.; Del Vecchio, C.; Tennyson, J.; Cassan, A.; Fernández Hernández, Maite; Burleigh, M. R.; Cordier, D.; De Witt, J.; Pagano, I.; Ray, T.; Gambicorti, L.; Palla, F.; Maldonado, J.; Biondi, D.; Eiroa, C.; Winek, W.; Ade, P.; Villaver, E.; Temple, J.; Gear, W.; Thompson, S.; Dominic, C.; Galand, M.; Focardi, M.; Cockell, C.; Pace, E.; Dorfi, E.; Bryson, I.; Cavarroc, C.; Pilat Lohinger, E.; Smith, A.; Eymet, V.; MacTavish, C.; Morales, J. C.; Gómez, H.; Stamper, R.; Esposito, M.; Andersen, A.; Azzollini, R.; Maxted, P.; Allende Prieto, C.; Nelson, R.; Gillon, M.; Achilleos, N.; Buchhave, L. A.; Fabrizio, N.; Ciaravella, A.; Claudi, R.; Damasso, M.; Bordé, P.; Figueira, P.; Rickman, H.; Rees, J. M.; Sitek, P.; Fossey, S.; Bakos, G.; Pascale, E.; Laken, B.; Soret, L.; Femenía Castella, B.; Allard, F.; Amado, P. J.; Luzzi, D.; Colomé, J.; Galand, M.; Lammer, H.; Bonford, B.; López Valverde, M. A.; Kerins, E.; Yung, Y.; Espinoza Contreras, M.; Irwin, P.; Herrero, E.; Wright, G.; Guàrdia, J.; Banaszkiewicz, M.; Hoogeeven, R.; Alcala, J.; Guio, P.; Koskinen, T.; Barton, E. J.; Piskunov, N.; Maurin, A. S.; Leto, G.; Boisse, I.; Claret, A.; Massi, F.; Kervella, P.; Börne, P.; Heiter, U.; Hargrave, P.; Fletcher, L.; Sánchez Béjar, V. J.; Bézard, B.; Cabral, A.; Michaut, C.; Winter, B.; Sousa, S.; Giuranna, M.; Batista, V.; Frith, J.; Ballerini, P.; López Morales, M.; Monteiro, M.; Tingley, B. W.; Lanza, N.; Maggio, A.; Lundgaard Rasmussen, I.; Altieri, F.; Covino, E.; Coustenis, A.; Heredero, R. L.; Watson, D.; Coudé du Foresto, V.; Liu, S. J.; Sicardy, B.; Deeg, H. J.; Moses, J.; Rodler, F.; Lithgow Bertelloni, C.; Demangeon, O.; Adybekian, V.; Fletcher, L.; Swinyard, B.; Morales Calderón, M.; Fouqué, P.; Deroo, P.; Lo Cicero, Ugo; Hueso, R.; Iro, N.; González Merino, B.; López Puertas, M.; Capria, M. T.; Danielski, C.; Branduardi Raymont, G.; Luntzer, A.; Gaulme, P.; Bulgarelli, A.; Parmentier, V.; Gerard, J. C.; Alard, C.; Frith, J.; Dobrijévic, M.; Medvedev, A.; Barrado, D.; Jacquemoud, S.; Sethenadh, J.; Readorn, K.; Polichtchouk, I.; Petrov, R.; García Piquer, A.; Tabernero, H. M.; White, G.; Pancrazzi, M.; García López, Ramón; Filacchione, G.; Gómez Leal, I.; Rengel, M.; Gesa, L.; Tanga, P.; Mueller Wodarg, I.; Israelian, G.; Rebolo López, R.; Shore, S.; Peralta, J.; Collura, A.; Giro, E.; Del Val Borro, M.; Griffith, C.; Tecsa, M.; Haigh, J.; Moro Martín, A.; Jones, H.; Gizon, L.; Pezzuto, S.; Giani, E.; Mall, U.; Eales, S.; Graczyk, R.; Ramos Zapata, G.; Krupp, N.; Sánchez Lavega, A.; Fossey, S.; Alonso Floriano, F. J.; Justtanot, K.; Santos, N.; Pérez Hoyos, S.; Savini, G.; Chamberlain, S.; Bowles, N.; Kerschbaum, F.; Tozzi, A.; Turrini, D.; Kipping, D.; Maruquette, J. B.; Correira, A.; Trifoglio, M.; Agúndez, Marcelino; Scandaratio, G.; Snellen, I. A.; Scuderi, S.; Femenía Castella, B.; Prisinzano, L.; Oliva, E.; Hébrard, E.; Lodieu, N.; Forget, F.; Chadney, J.; Showman, A.; Gustin, J.; Vinatier, S.; Charnoz, S.; Affer, L.; Rank Lüftinger, T.; Poretti, E.; Lahav, O.; North, C.; Gerard, J. C.; Murgas Alcaino, F.; Yurchenko, S. N.; Widemann, T.; Ward Thompson, D.; Montañés Rodríguez, P.; Kovács, G.; Valdivieso, M. L.; Moya Bedon, A.; Montalto, M.; Christian Jessen, N.; Venot, O.; Koskinen, T.; Lagage, P. O.; Bellucci, G.; Prinja, R.; Pinfield, D.; Banaszkiewicz, M.; Waldmann, I.; Jones, G.; Morello, G.; Crook, J.; Lim, T.; Parviainen, H.; Pallé, E.; Ramos, A. A.; Sanromá, E.; Waters, R.; Morais, H.; Stiepen, A.; Lellouch, E.; Orton, G.; Rezac, L.; Beaulieu, J. P.; Focardi, M.; Mauskopf, P.; Barlow, M.; Guedel, M.; Waltham, D.; Agnor, C.; Encrenaz, T.; Cerulli, R.; Balado, A.; Bouy, H.; Rebordao, J.; Stolarski, M.; Álvarez Iglesias, C. A.; Adriani, A.; Rocchetto, M.; Norgaard Nielsen, H. U.; Hollis, M.; Selig, A.; Malaguti, G.; Burston, R.; Peña Ramírez, K. Y.; Schmider, F. X.; Baffa, C.; Heyrovsky, D.; Figueira, P.; Piccioni, G.; Ottensamer, R.; Radioti, A.; Yelle, R.; Pantin, E.; Miles Paez, P.; Belmonte Avilés, J. A.; Montes, D.; Varley, R.; Viti, S.; Abe, L.; Pinsard, F.; Tessenyi, M.; Di Giorgio, A.; Turrini, D.; Terenzi, L.; Hubert, B.; Griffin, M.; Barber, R. J.; Cole, R.; Gianotti, F.; Blecka, M.; Wawrzaszk, A.; Middleton, K.; De Kok, R.; Martín Torres, Javier; Kehoe, T.; Cho, J.; Machado, P.; Berry, D.; Wisniowski, T.; Grodent, D.; Rataj, M.; Hornstrup, A.; Kerschbaum, F.; Vandenbussche, B.; Stixrude, L.; González Hernández, Carmen; 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]; Bulgarelli, A. [0000-0001-6347-0649]; Morales Calderon, M. [0000-0001-9526-9499]; Ward Thompson, D. [0000-0003-1140-2761]; Rebolo, R. [0000-0003-3767-7085]; López Valverde, M. A. [0000-0002-7989-4267]; Gillon, M. [0000-0003-1462-7739]; Morgante, G. [0000-0001-9234-7412]; Pena Ramírez, K. [0000-0002-5855-401X]; Galand, M. [0000-0001-5797-914X]; Pancrazzi, M. [0000-0002-3789-2482]; Pilat Lohinger, E. [0000-0002-5292-1923]; Altieri, F. [0000-0002-6338-8300]; Malaguti, G. [0000-0001-9872-3378]; Sánchez Lavega, A. [0000-0001-7234-7634]; Waldmann, I. [0000-0002-4205-5267]; Kovacs, G. [0000-0002-2365-2330]; Guillot, T. [0000-0002-7188-8428]; Monteiro, M. [0000-0001-5644-0898]; Bellucci, G. [0000-0003-0867-8679]; Baffa, C. [0000-0002-4935-100X]; Olivia, E. [0000-0002-9123-0412]; Tizzi, A. [0000-0002-6725-3825]; Selsis, F. [0000-0001-9619-5356]; Scuderi, Salvatore [0000-0002-8637-2109]; Hersant, F. [0000-0002-2687-7500]; Gear, W. [0000-0001-6789-6196]; Damasso, M. [0000-0001-9984-4278]; Irwin, P. [0000-0002-6772-384X]; Pinfield, D. [0000-0002-7804-4260]; Kipping, D. [0000-0002-4365-7366]; Maldonado, J. [0000-0002-4282-1072]; Pace, E. [0000-0001-5870-1772]; Burleigh, M. [0000-0003-0684-7803]; Chadney, J. [0000-0002-5174-2114]; Moro Martín, A. [0000-0001-9504-8426]; Claret, A. [0000-0002-4045-8134]; Rodríguez, P. [0000-0002-6855-9682]; Bezard, B. [0000-0002-5433-5661]; Gómez, H. [0000-0003-3398-0052]; Maldonado, J. [0000-0002-2218-5689]; Michaut, C. [0000-0002-2578-0117]; Hornstrup, A. [0000-0002-3363-0936]; Scholz, A. [0000-0001-8993-5053]; Sánchez Bejar, V. [0000-0002-5086-4232]; López Heredero, R. [0000-0002-2197-8388]; Sanz Forcada, J. [0000-0002-1600-7835]; Danielski, C. [0000-0002-3729-2663]; Vandenbussche, B. [0000-0002-1368-3109]; Sousa, S. [0000-0001-9047-2965]; Medved, A. [0000-0003-2713-8977]; Tinetti, G. [0000-0001-6058-6654]; Bakos, G. [0000-0001-7204-6727]; Ade, P. [0000-0002-5127-0401]; Amado, P. J. [0000-0002-8388-6040]; Martín Torres, J. [0000-0001-6479-2236]; Correira, A. [0000-0002-8946-8579]; Haigh, J. [0000-0001-5504-4754]; Scandariato, G. [0000-0003-2029-0626]; Guedel, M. [0000-0001-9818-0588]; Piskunov, N. [0000-0001-5742-7767]; Adibekyan, V. [0000-0002-0601-6199]; Pérez Hoyos, S. [0000-0001-9797-4917]; Poretti, E. [0000-0003-1200-0473]; Maggio, A. [0000-0001-5154-6108]; Kervella, P. [0000-0003-0626-1749]; Pascale, E. [0000-0002-3242-8154]; Claudi, R. [0000-0001-7707-5105]; Filacchione, G. [0000-0001-9567-0055]; Rickman, H. [0000-0002-9603-6619]; Sanroma, E. [0000-0001-8859-7937]; Agundez, M. [0000-0003-3248-3564]; Montes, D. [0000-0002-7779-238X]; Fletcher, L. [0000-0001-5834-9588]; Rataj, M. [0000-0002-2978-9629]; Stixrude, L. [0000-0003-3778-2432]; Montes, D. [0000-0002-7779-238X]; Morais, M. H. [0000-0001-5333-2736]; Hueso, R. [0000-0003-0169-123X]; Yurchenko, S. [0000-0001-9286-9501]; Morales, J. C. [0000-0003-0061-518X]; Pérez Hoyos, S. [0000-0002-2587-4682]; Santos, N. [0000-0003-4422-2919]; Peralta, J. [0000-0002-6823-1695]; Budaj, J. [0000-0002-9125-7340]; Barlow, M. [0000-0002-3875-1171]; Deeg, H. [0000-0003-0047-4241]; Grassi, D. [0000-0003-1653-3066]; Piccioni, G. [0000-0002-7893-6808]; Barton, E. [0000-0001-5945-9244]; Abreu, M. [0000-0002-0716-9568]; Ribas, I. [0000-0002-6689-0312]; Coates, A. [0000-0002-6185-3125]; García Ramón, J. [0000-0002-8204-6832]; Bouy, H. [0000-0002-7084-487X[; Lognonne, P. [0000-0002-1014-920X]; Demangeon, O. [0000-0001-7918-0355]; Ray, T. [0000-0002-2110-1068]; Guio, P. [0000-0002-1607-5862]; Tanga, P. [0000-0002-2718-997X]; Delgado, M. E. [0000-0003-4434-2195]; Leto, G. [0000-0002-0040-5011]; Prisinzano, L. [0000-0002-8893-2210]; Barstow, J. [0000-0003-3726-5419]; Balado, A. [0000-0003-4268-2516]; Lithgow Bertelloni, C. [0000-0003-0924-6587]; Zapatero Osorio, M. R. [0000-0001-5664-2852]; Affer, L. [0000-0001-5600-3778]; Ciaravella, A. [0000-0002-3127-8078]; Barrado Navascues, D. [0000-0002-5971-9242]; Figueira, P. [0000-0001-8504-283X]; Covino, E. [0000-0002-6187-6685]; Venot, O. [0000-0003-2854-765X]; Cabral, A. [0000-0002-9433-871X]; Watson, D. [0000-0002-4465-8264]; Turrini, D. [0000-0002-1923-7740]
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.