The EChO science case

Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Tinetti, Giovanna [verfasserIn] Drossart, Pierre [verfasserIn] Eccleston, Paul [verfasserIn] Hartogh, Paul [verfasserIn] Isaak, Kate [verfasserIn] Linder, Martin [verfasserIn] Lovis, Christophe [verfasserIn] Micela, Giusi [verfasserIn] Ollivier, Marc [verfasserIn] Puig, Ludovic [verfasserIn] Ribas, Ignasi [verfasserIn] Snellen, Ignas [verfasserIn] Swinyard, Bruce [verfasserIn] Allard, France [verfasserIn] Barstow, Joanna [verfasserIn] Cho, James [verfasserIn] Coustenis, Athena [verfasserIn] Cockell, Charles [verfasserIn] Correia, Alexandre [verfasserIn] Decin, Leen [verfasserIn] de Kok, Remco [verfasserIn] Deroo, Pieter [verfasserIn] Encrenaz, Therese [verfasserIn] Forget, Francois [verfasserIn] Glasse, Alistair [verfasserIn] Griffith, Caitlin [verfasserIn] Guillot, Tristan [verfasserIn] Koskinen, Tommi [verfasserIn] Lammer, Helmut [verfasserIn] Leconte, Jeremy [verfasserIn] Maxted, Pierre [verfasserIn] Mueller-Wodarg, Ingo [verfasserIn] Nelson, Richard [verfasserIn] North, Chris [verfasserIn] Pallé, Enric [verfasserIn] Pagano, Isabella [verfasserIn] Piccioni, Guseppe [verfasserIn] Pinfield, David [verfasserIn] Selsis, Franck [verfasserIn] Sozzetti, Alessandro [verfasserIn] Stixrude, Lars [verfasserIn] Tennyson, Jonathan [verfasserIn] Turrini, Diego [verfasserIn] Zapatero-Osorio, Mariarosa [verfasserIn] Beaulieu, Jean-Philippe [verfasserIn] Grodent, Denis [verfasserIn] Guedel, Manuel [verfasserIn] Luz, David [verfasserIn] Nørgaard-Nielsen, Hans Ulrik [verfasserIn] Ray, Tom [verfasserIn] Rickman, Hans [verfasserIn] Selig, Avri [verfasserIn] Swain, Mark [verfasserIn] Banaszkiewicz, Marek [verfasserIn] Barlow, Mike [verfasserIn] Bowles, Neil [verfasserIn] Branduardi-Raymont, Graziella [verfasserIn] du Foresto, Vincent Coudé [verfasserIn] Gerard, Jean-Claude [verfasserIn] Gizon, Laurent [verfasserIn] Hornstrup, Allan [verfasserIn] Jarchow, Christopher [verfasserIn] Kerschbaum, Franz [verfasserIn] Kovacs, Géza [verfasserIn] Lagage, Pierre-Olivier [verfasserIn] Lim, Tanya [verfasserIn] Lopez-Morales, Mercedes [verfasserIn] Malaguti, Giuseppe [verfasserIn] Pace, Emanuele [verfasserIn] Pascale, Enzo [verfasserIn] Vandenbussche, Bart [verfasserIn] Wright, Gillian [verfasserIn] Zapata, Gonzalo Ramos [verfasserIn] Adriani, Alberto [verfasserIn] Azzollini, Ruymán [verfasserIn] Balado, Ana [verfasserIn] Bryson, Ian [verfasserIn] Burston, Raymond [verfasserIn] Colomé, Josep [verfasserIn] Crook, Martin [verfasserIn] Di Giorgio, Anna [verfasserIn] Griffin, Matt [verfasserIn] Hoogeveen, Ruud [verfasserIn] Ottensamer, Roland [verfasserIn] Irshad, Ranah [verfasserIn] Middleton, Kevin [verfasserIn] Morgante, Gianluca [verfasserIn] Pinsard, Frederic [verfasserIn] Rataj, Mirek [verfasserIn] Reess, Jean-Michel [verfasserIn] Savini, Giorgio [verfasserIn] Schrader, Jan-Rutger [verfasserIn] Stamper, Richard [verfasserIn] Winter, Berend [verfasserIn] Abe, L. [verfasserIn] Abreu, M. [verfasserIn] Achilleos, N. [verfasserIn] Ade, P. [verfasserIn] Adybekian, V. [verfasserIn] Affer, L. [verfasserIn] Agnor, C. [verfasserIn] Agundez, M. [verfasserIn] Alard, C. [verfasserIn] Alcala, J. [verfasserIn] Allende Prieto, C. [verfasserIn] Alonso Floriano, F. J. [verfasserIn] Altieri, F. [verfasserIn] Alvarez Iglesias, C. A. [verfasserIn] Amado, P. [verfasserIn] Andersen, A. [verfasserIn] Aylward, A. [verfasserIn] Baffa, C. [verfasserIn] Bakos, G. [verfasserIn] Ballerini, P. [verfasserIn] Banaszkiewicz, M. [verfasserIn] Barber, R. J. [verfasserIn] Barrado, D. [verfasserIn] Barton, E. J. [verfasserIn] Batista, V. [verfasserIn] Bellucci, G. [verfasserIn] Belmonte Avilés, J. A. [verfasserIn] Berry, D. [verfasserIn] Bézard, B. [verfasserIn] Biondi, D. [verfasserIn] Błęcka, M. [verfasserIn] Boisse, I. [verfasserIn] Bonfond, B. [verfasserIn] Bordé, P. [verfasserIn] Börner, P. [verfasserIn] Bouy, H. [verfasserIn] Brown, L. [verfasserIn] Buchhave, L. [verfasserIn] Budaj, J. [verfasserIn] Bulgarelli, A. [verfasserIn] Burleigh, M. [verfasserIn] Cabral, A. [verfasserIn] Capria, M. T. [verfasserIn] Cassan, A. [verfasserIn] Cavarroc, C. [verfasserIn] Cecchi-Pestellini, C. [verfasserIn] Cerulli, R. [verfasserIn] Chadney, J. [verfasserIn] Chamberlain, S. [verfasserIn] Charnoz, S. [verfasserIn] Christian Jessen, N. [verfasserIn] Ciaravella, A. [verfasserIn] Claret, A. [verfasserIn] Claudi, R. [verfasserIn] Coates, A. [verfasserIn] Cole, R. [verfasserIn] Collura, A. [verfasserIn] Cordier, D. [verfasserIn] Covino, E. [verfasserIn] Danielski, C. [verfasserIn] Damasso, M. [verfasserIn] Deeg, H. J. [verfasserIn] Delgado-Mena, E. [verfasserIn] Del Vecchio, C. [verfasserIn] Demangeon, O. [verfasserIn] De Sio, A. [verfasserIn] De Wit, J. [verfasserIn] Dobrijévic, M. [verfasserIn] Doel, P. [verfasserIn] Dominic, C. [verfasserIn] Dorfi, E. [verfasserIn] Eales, S. [verfasserIn] Eiroa, C. [verfasserIn] Espinoza Contreras, M. [verfasserIn] Esposito, M. [verfasserIn] Eymet, V. [verfasserIn] Fabrizio, N. [verfasserIn] Fernández, M. [verfasserIn] Femenía Castella, B. [verfasserIn] Figueira, P. [verfasserIn] Filacchione, G. [verfasserIn] Fletcher, L. [verfasserIn] Focardi, M. [verfasserIn] Fossey, S. [verfasserIn] Fouqué, P. [verfasserIn] Frith, J. [verfasserIn] Galand, M. [verfasserIn] Gambicorti, L. [verfasserIn] Gaulme, P. [verfasserIn] García López, R. J. [verfasserIn] Garcia-Piquer, A. [verfasserIn] Gear, W. [verfasserIn] Gerard, J.-C. [verfasserIn] Gesa, L. [verfasserIn] Giani, E. [verfasserIn] Gianotti, F. [verfasserIn] Gillon, M. [verfasserIn] Giro, E. [verfasserIn] Giuranna, M. [verfasserIn] Gomez, H. [verfasserIn] Gomez-Leal, I. [verfasserIn] Gonzalez Hernandez, J. [verfasserIn] González Merino, B. [verfasserIn] Graczyk, R. [verfasserIn] Grassi, D. [verfasserIn] Guardia, J. [verfasserIn] Guio, P. [verfasserIn] Gustin, J. [verfasserIn] Hargrave, P. [verfasserIn] Haigh, J. [verfasserIn] Hébrard, E. [verfasserIn] Heiter, U. [verfasserIn] Heredero, R. L. [verfasserIn] Herrero, E. [verfasserIn] Hersant, F. [verfasserIn] Heyrovsky, D. [verfasserIn] Hollis, M. [verfasserIn] Hubert, B. [verfasserIn] Hueso, R. [verfasserIn] Israelian, G. [verfasserIn] Iro, N. [verfasserIn] Irwin, P. [verfasserIn] Jacquemoud, S. [verfasserIn] Jones, G. [verfasserIn] Jones, H. [verfasserIn] Justtanont, K. [verfasserIn] Kehoe, T. [verfasserIn] Kerschbaum, F. [verfasserIn] Kerins, E. [verfasserIn] Kervella, P. [verfasserIn] Kipping, D. [verfasserIn] Koskinen, T. [verfasserIn] Krupp, N. [verfasserIn] Lahav, O. [verfasserIn] Laken, B. [verfasserIn] Lanza, N. [verfasserIn] Lellouch, E. [verfasserIn] Leto, G. [verfasserIn] Licandro Goldaracena, J. [verfasserIn] Lithgow-Bertelloni, C. [verfasserIn] Liu, S. J. [verfasserIn] Lo Cicero, U. [verfasserIn] Lodieu, N. [verfasserIn] Lognonné, P. [verfasserIn] Lopez-Puertas, M. [verfasserIn] Lopez-Valverde, M. A. [verfasserIn] Lundgaard Rasmussen, I. [verfasserIn] Luntzer, A. [verfasserIn] Machado, P. [verfasserIn] MacTavish, C. [verfasserIn] Maggio, A. [verfasserIn] Maillard, J.-P. [verfasserIn] Magnes, W. [verfasserIn] Maldonado, J. [verfasserIn] Mall, U. [verfasserIn] Marquette, J.-B. [verfasserIn] Mauskopf, P. [verfasserIn] Massi, F. [verfasserIn] Maurin, A.-S. [verfasserIn] Medvedev, A. [verfasserIn] Michaut, C. [verfasserIn] Miles-Paez, P. [verfasserIn] Montalto, M. [verfasserIn] Montañés Rodríguez, P. [verfasserIn] Monteiro, M. [verfasserIn] Montes, D. [verfasserIn] Morais, H. [verfasserIn] Morales, J. C. [verfasserIn] Morales-Calderón, M. [verfasserIn] Morello, G. [verfasserIn] Moro Martín, A. [verfasserIn] Moses, J. [verfasserIn] Moya Bedon, A. [verfasserIn] Murgas Alcaino, F. [verfasserIn] Oliva, E. [verfasserIn] Orton, G. [verfasserIn] Palla, F. [verfasserIn] Pancrazzi, M. [verfasserIn] Pantin, E. [verfasserIn] Parmentier, V. [verfasserIn] Parviainen, H. [verfasserIn] Peña Ramírez, K. Y. [verfasserIn] Peralta, J. [verfasserIn] Perez-Hoyos, S. [verfasserIn] Petrov, R. [verfasserIn] Pezzuto, S. [verfasserIn] Pietrzak, R. [verfasserIn] Pilat-Lohinger, E. [verfasserIn] Piskunov, N. [verfasserIn] Prinja, R. [verfasserIn] Prisinzano, L. [verfasserIn] Polichtchouk, I. [verfasserIn] Poretti, E. [verfasserIn] Radioti, A. [verfasserIn] Ramos, A. A. [verfasserIn] Rank-Lüftinger, T. [verfasserIn] Read, P. [verfasserIn] Readorn, K. [verfasserIn] Rebolo López, R. [verfasserIn] Rebordão, J. [verfasserIn] Rengel, M. [verfasserIn] Rezac, L. [verfasserIn] Rocchetto, M. [verfasserIn] Rodler, F. [verfasserIn] Sánchez Béjar, V. J. [verfasserIn] Sanchez Lavega, A. [verfasserIn] Sanromá, E. [verfasserIn] Santos, N. [verfasserIn] Sanz Forcada, J. [verfasserIn] Scandariato, G. [verfasserIn] Schmider, F.-X. [verfasserIn] Scholz, A. [verfasserIn] Scuderi, S. [verfasserIn] Sethenadh, J. [verfasserIn] Shore, S. [verfasserIn] Showman, A. [verfasserIn] Sicardy, B. [verfasserIn] Sitek, P. [verfasserIn] Smith, A. [verfasserIn] Soret, L. [verfasserIn] Sousa, S. [verfasserIn] Stiepen, A. [verfasserIn] Stolarski, M. [verfasserIn] Strazzulla, G. [verfasserIn] Tabernero, H. M. [verfasserIn] Tanga, P. [verfasserIn] Tecsa, M. [verfasserIn] Temple, J. [verfasserIn] Terenzi, L. [verfasserIn] Tessenyi, M. [verfasserIn] Testi, L. [verfasserIn] Thompson, S. [verfasserIn] Thrastarson, H. [verfasserIn] Tingley, B. W. [verfasserIn] Trifoglio, M. [verfasserIn] Martín Torres, J. [verfasserIn] Tozzi, A. [verfasserIn] Turrini, D. [verfasserIn] Varley, R. [verfasserIn] Vakili, F. [verfasserIn] de Val-Borro, M. [verfasserIn] Valdivieso, M. L. [verfasserIn] Venot, O. [verfasserIn] Villaver, E. [verfasserIn] Vinatier, S. [verfasserIn] Viti, S. [verfasserIn] Waldmann, I. [verfasserIn] Waltham, D. [verfasserIn] Ward-Thompson, D. [verfasserIn] Waters, R. [verfasserIn] Watkins, C. [verfasserIn] Watson, D. [verfasserIn] Wawer, P. [verfasserIn] Wawrzaszk, A. [verfasserIn] White, G. [verfasserIn] Widemann, T. [verfasserIn] Winek, W. [verfasserIn] Wiśniowski, T. [verfasserIn] Yelle, R. [verfasserIn] Yung, Y. [verfasserIn] Yurchenko, S. N. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2015

Schlagwörter:	Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions

Übergeordnetes Werk:	Enthalten in: Experimental astronomy - Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989, 40(2015), 2-3 vom: 29. Nov., Seite 329-391
Übergeordnetes Werk:	volume:40 ; year:2015 ; number:2-3 ; day:29 ; month:11 ; pages:329-391

Links:	Volltext

DOI / URN:	10.1007/s10686-015-9484-8

Katalog-ID:	SPR012459186

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100	1		\|a Tinetti, Giovanna \|e verfasserin \|4 aut
245	1	4	\|a The EChO science case
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520			\|a Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.
650		4	\|a Exoplanets \|7 (dpeaa)DE-He213
650		4	\|a Spectroscopy \|7 (dpeaa)DE-He213
650		4	\|a Atmospheric science \|7 (dpeaa)DE-He213
650		4	\|a IR astronomy \|7 (dpeaa)DE-He213
650		4	\|a Space missions \|7 (dpeaa)DE-He213
700	1		\|a Drossart, Pierre \|e verfasserin \|4 aut
700	1		\|a Eccleston, Paul \|e verfasserin \|4 aut
700	1		\|a Hartogh, Paul \|e verfasserin \|4 aut
700	1		\|a Isaak, Kate \|e verfasserin \|4 aut
700	1		\|a Linder, Martin \|e verfasserin \|4 aut
700	1		\|a Lovis, Christophe \|e verfasserin \|4 aut
700	1		\|a Micela, Giusi \|e verfasserin \|4 aut
700	1		\|a Ollivier, Marc \|e verfasserin \|4 aut
700	1		\|a Puig, Ludovic \|e verfasserin \|4 aut
700	1		\|a Ribas, Ignasi \|e verfasserin \|4 aut
700	1		\|a Snellen, Ignas \|e verfasserin \|4 aut
700	1		\|a Swinyard, Bruce \|e verfasserin \|4 aut
700	1		\|a Allard, France \|e verfasserin \|4 aut
700	1		\|a Barstow, Joanna \|e verfasserin \|4 aut
700	1		\|a Cho, James \|e verfasserin \|4 aut
700	1		\|a Coustenis, Athena \|e verfasserin \|4 aut
700	1		\|a Cockell, Charles \|e verfasserin \|4 aut
700	1		\|a Correia, Alexandre \|e verfasserin \|4 aut
700	1		\|a Decin, Leen \|e verfasserin \|4 aut
700	1		\|a de Kok, Remco \|e verfasserin \|4 aut
700	1		\|a Deroo, Pieter \|e verfasserin \|4 aut
700	1		\|a Encrenaz, Therese \|e verfasserin \|4 aut
700	1		\|a Forget, Francois \|e verfasserin \|4 aut
700	1		\|a Glasse, Alistair \|e verfasserin \|4 aut
700	1		\|a Griffith, Caitlin \|e verfasserin \|4 aut
700	1		\|a Guillot, Tristan \|e verfasserin \|4 aut
700	1		\|a Koskinen, Tommi \|e verfasserin \|4 aut
700	1		\|a Lammer, Helmut \|e verfasserin \|4 aut
700	1		\|a Leconte, Jeremy \|e verfasserin \|4 aut
700	1		\|a Maxted, Pierre \|e verfasserin \|4 aut
700	1		\|a Mueller-Wodarg, Ingo \|e verfasserin \|4 aut
700	1		\|a Nelson, Richard \|e verfasserin \|4 aut
700	1		\|a North, Chris \|e verfasserin \|4 aut
700	1		\|a Pallé, Enric \|e verfasserin \|4 aut
700	1		\|a Pagano, Isabella \|e verfasserin \|4 aut
700	1		\|a Piccioni, Guseppe \|e verfasserin \|4 aut
700	1		\|a Pinfield, David \|e verfasserin \|4 aut
700	1		\|a Selsis, Franck \|e verfasserin \|4 aut
700	1		\|a Sozzetti, Alessandro \|e verfasserin \|4 aut
700	1		\|a Stixrude, Lars \|e verfasserin \|4 aut
700	1		\|a Tennyson, Jonathan \|e verfasserin \|4 aut
700	1		\|a Turrini, Diego \|e verfasserin \|4 aut
700	1		\|a Zapatero-Osorio, Mariarosa \|e verfasserin \|4 aut
700	1		\|a Beaulieu, Jean-Philippe \|e verfasserin \|4 aut
700	1		\|a Grodent, Denis \|e verfasserin \|4 aut
700	1		\|a Guedel, Manuel \|e verfasserin \|4 aut
700	1		\|a Luz, David \|e verfasserin \|4 aut
700	1		\|a Nørgaard-Nielsen, Hans Ulrik \|e verfasserin \|4 aut
700	1		\|a Ray, Tom \|e verfasserin \|4 aut
700	1		\|a Rickman, Hans \|e verfasserin \|4 aut
700	1		\|a Selig, Avri \|e verfasserin \|4 aut
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700	1		\|a Banaszkiewicz, Marek \|e verfasserin \|4 aut
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700	1		\|a Bowles, Neil \|e verfasserin \|4 aut
700	1		\|a Branduardi-Raymont, Graziella \|e verfasserin \|4 aut
700	1		\|a du Foresto, Vincent Coudé \|e verfasserin \|4 aut
700	1		\|a Gerard, Jean-Claude \|e verfasserin \|4 aut
700	1		\|a Gizon, Laurent \|e verfasserin \|4 aut
700	1		\|a Hornstrup, Allan \|e verfasserin \|4 aut
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700	1		\|a Kovacs, Géza \|e verfasserin \|4 aut
700	1		\|a Lagage, Pierre-Olivier \|e verfasserin \|4 aut
700	1		\|a Lim, Tanya \|e verfasserin \|4 aut
700	1		\|a Lopez-Morales, Mercedes \|e verfasserin \|4 aut
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700	1		\|a Pace, Emanuele \|e verfasserin \|4 aut
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700	1		\|a Vandenbussche, Bart \|e verfasserin \|4 aut
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700	1		\|a Adriani, Alberto \|e verfasserin \|4 aut
700	1		\|a Azzollini, Ruymán \|e verfasserin \|4 aut
700	1		\|a Balado, Ana \|e verfasserin \|4 aut
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700	1		\|a Colomé, Josep \|e verfasserin \|4 aut
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700	1		\|a Di Giorgio, Anna \|e verfasserin \|4 aut
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700	1		\|a Hoogeveen, Ruud \|e verfasserin \|4 aut
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700	1		\|a Cecchi-Pestellini, C. \|e verfasserin \|4 aut
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700	1		\|a Christian Jessen, N. \|e verfasserin \|4 aut
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700	1		\|a Danielski, C. \|e verfasserin \|4 aut
700	1		\|a Damasso, M. \|e verfasserin \|4 aut
700	1		\|a Deeg, H. J. \|e verfasserin \|4 aut
700	1		\|a Delgado-Mena, E. \|e verfasserin \|4 aut
700	1		\|a Del Vecchio, C. \|e verfasserin \|4 aut
700	1		\|a Demangeon, O. \|e verfasserin \|4 aut
700	1		\|a De Sio, A. \|e verfasserin \|4 aut
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700	1		\|a Eales, S. \|e verfasserin \|4 aut
700	1		\|a Eiroa, C. \|e verfasserin \|4 aut
700	1		\|a Espinoza Contreras, M. \|e verfasserin \|4 aut
700	1		\|a Esposito, M. \|e verfasserin \|4 aut
700	1		\|a Eymet, V. \|e verfasserin \|4 aut
700	1		\|a Fabrizio, N. \|e verfasserin \|4 aut
700	1		\|a Fernández, M. \|e verfasserin \|4 aut
700	1		\|a Femenía Castella, B. \|e verfasserin \|4 aut
700	1		\|a Figueira, P. \|e verfasserin \|4 aut
700	1		\|a Filacchione, G. \|e verfasserin \|4 aut
700	1		\|a Fletcher, L. \|e verfasserin \|4 aut
700	1		\|a Focardi, M. \|e verfasserin \|4 aut
700	1		\|a Fossey, S. \|e verfasserin \|4 aut
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700	1		\|a Frith, J. \|e verfasserin \|4 aut
700	1		\|a Galand, M. \|e verfasserin \|4 aut
700	1		\|a Gambicorti, L. \|e verfasserin \|4 aut
700	1		\|a Gaulme, P. \|e verfasserin \|4 aut
700	1		\|a García López, R. J. \|e verfasserin \|4 aut
700	1		\|a Garcia-Piquer, A. \|e verfasserin \|4 aut
700	1		\|a Gear, W. \|e verfasserin \|4 aut
700	1		\|a Gerard, J.-C. \|e verfasserin \|4 aut
700	1		\|a Gesa, L. \|e verfasserin \|4 aut
700	1		\|a Giani, E. \|e verfasserin \|4 aut
700	1		\|a Gianotti, F. \|e verfasserin \|4 aut
700	1		\|a Gillon, M. \|e verfasserin \|4 aut
700	1		\|a Giro, E. \|e verfasserin \|4 aut
700	1		\|a Giuranna, M. \|e verfasserin \|4 aut
700	1		\|a Gomez, H. \|e verfasserin \|4 aut
700	1		\|a Gomez-Leal, I. \|e verfasserin \|4 aut
700	1		\|a Gonzalez Hernandez, J. \|e verfasserin \|4 aut
700	1		\|a González Merino, B. \|e verfasserin \|4 aut
700	1		\|a Graczyk, R. \|e verfasserin \|4 aut
700	1		\|a Grassi, D. \|e verfasserin \|4 aut
700	1		\|a Guardia, J. \|e verfasserin \|4 aut
700	1		\|a Guio, P. \|e verfasserin \|4 aut
700	1		\|a Gustin, J. \|e verfasserin \|4 aut
700	1		\|a Hargrave, P. \|e verfasserin \|4 aut
700	1		\|a Haigh, J. \|e verfasserin \|4 aut
700	1		\|a Hébrard, E. \|e verfasserin \|4 aut
700	1		\|a Heiter, U. \|e verfasserin \|4 aut
700	1		\|a Heredero, R. L. \|e verfasserin \|4 aut
700	1		\|a Herrero, E. \|e verfasserin \|4 aut
700	1		\|a Hersant, F. \|e verfasserin \|4 aut
700	1		\|a Heyrovsky, D. \|e verfasserin \|4 aut
700	1		\|a Hollis, M. \|e verfasserin \|4 aut
700	1		\|a Hubert, B. \|e verfasserin \|4 aut
700	1		\|a Hueso, R. \|e verfasserin \|4 aut
700	1		\|a Israelian, G. \|e verfasserin \|4 aut
700	1		\|a Iro, N. \|e verfasserin \|4 aut
700	1		\|a Irwin, P. \|e verfasserin \|4 aut
700	1		\|a Jacquemoud, S. \|e verfasserin \|4 aut
700	1		\|a Jones, G. \|e verfasserin \|4 aut
700	1		\|a Jones, H. \|e verfasserin \|4 aut
700	1		\|a Justtanont, K. \|e verfasserin \|4 aut
700	1		\|a Kehoe, T. \|e verfasserin \|4 aut
700	1		\|a Kerschbaum, F. \|e verfasserin \|4 aut
700	1		\|a Kerins, E. \|e verfasserin \|4 aut
700	1		\|a Kervella, P. \|e verfasserin \|4 aut
700	1		\|a Kipping, D. \|e verfasserin \|4 aut
700	1		\|a Koskinen, T. \|e verfasserin \|4 aut
700	1		\|a Krupp, N. \|e verfasserin \|4 aut
700	1		\|a Lahav, O. \|e verfasserin \|4 aut
700	1		\|a Laken, B. \|e verfasserin \|4 aut
700	1		\|a Lanza, N. \|e verfasserin \|4 aut
700	1		\|a Lellouch, E. \|e verfasserin \|4 aut
700	1		\|a Leto, G. \|e verfasserin \|4 aut
700	1		\|a Licandro Goldaracena, J. \|e verfasserin \|4 aut
700	1		\|a Lithgow-Bertelloni, C. \|e verfasserin \|4 aut
700	1		\|a Liu, S. J. \|e verfasserin \|4 aut
700	1		\|a Lo Cicero, U. \|e verfasserin \|4 aut
700	1		\|a Lodieu, N. \|e verfasserin \|4 aut
700	1		\|a Lognonné, P. \|e verfasserin \|4 aut
700	1		\|a Lopez-Puertas, M. \|e verfasserin \|4 aut
700	1		\|a Lopez-Valverde, M. A. \|e verfasserin \|4 aut
700	1		\|a Lundgaard Rasmussen, I. \|e verfasserin \|4 aut
700	1		\|a Luntzer, A. \|e verfasserin \|4 aut
700	1		\|a Machado, P. \|e verfasserin \|4 aut
700	1		\|a MacTavish, C. \|e verfasserin \|4 aut
700	1		\|a Maggio, A. \|e verfasserin \|4 aut
700	1		\|a Maillard, J.-P. \|e verfasserin \|4 aut
700	1		\|a Magnes, W. \|e verfasserin \|4 aut
700	1		\|a Maldonado, J. \|e verfasserin \|4 aut
700	1		\|a Mall, U. \|e verfasserin \|4 aut
700	1		\|a Marquette, J.-B. \|e verfasserin \|4 aut
700	1		\|a Mauskopf, P. \|e verfasserin \|4 aut
700	1		\|a Massi, F. \|e verfasserin \|4 aut
700	1		\|a Maurin, A.-S. \|e verfasserin \|4 aut
700	1		\|a Medvedev, A. \|e verfasserin \|4 aut
700	1		\|a Michaut, C. \|e verfasserin \|4 aut
700	1		\|a Miles-Paez, P. \|e verfasserin \|4 aut
700	1		\|a Montalto, M. \|e verfasserin \|4 aut
700	1		\|a Montañés Rodríguez, P. \|e verfasserin \|4 aut
700	1		\|a Monteiro, M. \|e verfasserin \|4 aut
700	1		\|a Montes, D. \|e verfasserin \|4 aut
700	1		\|a Morais, H. \|e verfasserin \|4 aut
700	1		\|a Morales, J. C. \|e verfasserin \|4 aut
700	1		\|a Morales-Calderón, M. \|e verfasserin \|4 aut
700	1		\|a Morello, G. \|e verfasserin \|4 aut
700	1		\|a Moro Martín, A. \|e verfasserin \|4 aut
700	1		\|a Moses, J. \|e verfasserin \|4 aut
700	1		\|a Moya Bedon, A. \|e verfasserin \|4 aut
700	1		\|a Murgas Alcaino, F. \|e verfasserin \|4 aut
700	1		\|a Oliva, E. \|e verfasserin \|4 aut
700	1		\|a Orton, G. \|e verfasserin \|4 aut
700	1		\|a Palla, F. \|e verfasserin \|4 aut
700	1		\|a Pancrazzi, M. \|e verfasserin \|4 aut
700	1		\|a Pantin, E. \|e verfasserin \|4 aut
700	1		\|a Parmentier, V. \|e verfasserin \|4 aut
700	1		\|a Parviainen, H. \|e verfasserin \|4 aut
700	1		\|a Peña Ramírez, K. Y. \|e verfasserin \|4 aut
700	1		\|a Peralta, J. \|e verfasserin \|4 aut
700	1		\|a Perez-Hoyos, S. \|e verfasserin \|4 aut
700	1		\|a Petrov, R. \|e verfasserin \|4 aut
700	1		\|a Pezzuto, S. \|e verfasserin \|4 aut
700	1		\|a Pietrzak, R. \|e verfasserin \|4 aut
700	1		\|a Pilat-Lohinger, E. \|e verfasserin \|4 aut
700	1		\|a Piskunov, N. \|e verfasserin \|4 aut
700	1		\|a Prinja, R. \|e verfasserin \|4 aut
700	1		\|a Prisinzano, L. \|e verfasserin \|4 aut
700	1		\|a Polichtchouk, I. \|e verfasserin \|4 aut
700	1		\|a Poretti, E. \|e verfasserin \|4 aut
700	1		\|a Radioti, A. \|e verfasserin \|4 aut
700	1		\|a Ramos, A. A. \|e verfasserin \|4 aut
700	1		\|a Rank-Lüftinger, T. \|e verfasserin \|4 aut
700	1		\|a Read, P. \|e verfasserin \|4 aut
700	1		\|a Readorn, K. \|e verfasserin \|4 aut
700	1		\|a Rebolo López, R. \|e verfasserin \|4 aut
700	1		\|a Rebordão, J. \|e verfasserin \|4 aut
700	1		\|a Rengel, M. \|e verfasserin \|4 aut
700	1		\|a Rezac, L. \|e verfasserin \|4 aut
700	1		\|a Rocchetto, M. \|e verfasserin \|4 aut
700	1		\|a Rodler, F. \|e verfasserin \|4 aut
700	1		\|a Sánchez Béjar, V. J. \|e verfasserin \|4 aut
700	1		\|a Sanchez Lavega, A. \|e verfasserin \|4 aut
700	1		\|a Sanromá, E. \|e verfasserin \|4 aut
700	1		\|a Santos, N. \|e verfasserin \|4 aut
700	1		\|a Sanz Forcada, J. \|e verfasserin \|4 aut
700	1		\|a Scandariato, G. \|e verfasserin \|4 aut
700	1		\|a Schmider, F.-X. \|e verfasserin \|4 aut
700	1		\|a Scholz, A. \|e verfasserin \|4 aut
700	1		\|a Scuderi, S. \|e verfasserin \|4 aut
700	1		\|a Sethenadh, J. \|e verfasserin \|4 aut
700	1		\|a Shore, S. \|e verfasserin \|4 aut
700	1		\|a Showman, A. \|e verfasserin \|4 aut
700	1		\|a Sicardy, B. \|e verfasserin \|4 aut
700	1		\|a Sitek, P. \|e verfasserin \|4 aut
700	1		\|a Smith, A. \|e verfasserin \|4 aut
700	1		\|a Soret, L. \|e verfasserin \|4 aut
700	1		\|a Sousa, S. \|e verfasserin \|4 aut
700	1		\|a Stiepen, A. \|e verfasserin \|4 aut
700	1		\|a Stolarski, M. \|e verfasserin \|4 aut
700	1		\|a Strazzulla, G. \|e verfasserin \|4 aut
700	1		\|a Tabernero, H. M. \|e verfasserin \|4 aut
700	1		\|a Tanga, P. \|e verfasserin \|4 aut
700	1		\|a Tecsa, M. \|e verfasserin \|4 aut
700	1		\|a Temple, J. \|e verfasserin \|4 aut
700	1		\|a Terenzi, L. \|e verfasserin \|4 aut
700	1		\|a Tessenyi, M. \|e verfasserin \|4 aut
700	1		\|a Testi, L. \|e verfasserin \|4 aut
700	1		\|a Thompson, S. \|e verfasserin \|4 aut
700	1		\|a Thrastarson, H. \|e verfasserin \|4 aut
700	1		\|a Tingley, B. W. \|e verfasserin \|4 aut
700	1		\|a Trifoglio, M. \|e verfasserin \|4 aut
700	1		\|a Martín Torres, J. \|e verfasserin \|4 aut
700	1		\|a Tozzi, A. \|e verfasserin \|4 aut
700	1		\|a Turrini, D. \|e verfasserin \|4 aut
700	1		\|a Varley, R. \|e verfasserin \|4 aut
700	1		\|a Vakili, F. \|e verfasserin \|4 aut
700	1		\|a de Val-Borro, M. \|e verfasserin \|4 aut
700	1		\|a Valdivieso, M. L. \|e verfasserin \|4 aut
700	1		\|a Venot, O. \|e verfasserin \|4 aut
700	1		\|a Villaver, E. \|e verfasserin \|4 aut
700	1		\|a Vinatier, S. \|e verfasserin \|4 aut
700	1		\|a Viti, S. \|e verfasserin \|4 aut
700	1		\|a Waldmann, I. \|e verfasserin \|4 aut
700	1		\|a Waltham, D. \|e verfasserin \|4 aut
700	1		\|a Ward-Thompson, D. \|e verfasserin \|4 aut
700	1		\|a Waters, R. \|e verfasserin \|4 aut
700	1		\|a Watkins, C. \|e verfasserin \|4 aut
700	1		\|a Watson, D. \|e verfasserin \|4 aut
700	1		\|a Wawer, P. \|e verfasserin \|4 aut
700	1		\|a Wawrzaszk, A. \|e verfasserin \|4 aut
700	1		\|a White, G. \|e verfasserin \|4 aut
700	1		\|a Widemann, T. \|e verfasserin \|4 aut
700	1		\|a Winek, W. \|e verfasserin \|4 aut
700	1		\|a Wiśniowski, T. \|e verfasserin \|4 aut
700	1		\|a Yelle, R. \|e verfasserin \|4 aut
700	1		\|a Yung, Y. \|e verfasserin \|4 aut
700	1		\|a Yurchenko, S. N. \|e verfasserin \|4 aut
773	0	8	\|i Enthalten in \|t Experimental astronomy \|d Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 \|g 40(2015), 2-3 vom: 29. Nov., Seite 329-391 \|w (DE-627)312841116 \|w (DE-600)2012330-9 \|x 1572-9508 \|7 nnns
773	1	8	\|g volume:40 \|g year:2015 \|g number:2-3 \|g day:29 \|g month:11 \|g pages:329-391
856	4	0	\|u https://dx.doi.org/10.1007/s10686-015-9484-8 \|z kostenfrei \|3 Volltext
912			\|a GBV_USEFLAG_A
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912			\|a GBV_ILN_285
912			\|a GBV_ILN_293
912			\|a GBV_ILN_370
912			\|a GBV_ILN_602
912			\|a GBV_ILN_636
912			\|a GBV_ILN_702
912			\|a GBV_ILN_2001
912			\|a GBV_ILN_2003
912			\|a GBV_ILN_2004
912			\|a GBV_ILN_2005
912			\|a GBV_ILN_2006
912			\|a GBV_ILN_2007
912			\|a GBV_ILN_2008
912			\|a GBV_ILN_2009
912			\|a GBV_ILN_2010
912			\|a GBV_ILN_2011
912			\|a GBV_ILN_2014
912			\|a GBV_ILN_2015
912			\|a GBV_ILN_2020
912			\|a GBV_ILN_2021
912			\|a GBV_ILN_2025
912			\|a GBV_ILN_2026
912			\|a GBV_ILN_2027
912			\|a GBV_ILN_2031
912			\|a GBV_ILN_2034
912			\|a GBV_ILN_2037
912			\|a GBV_ILN_2038
912			\|a GBV_ILN_2039
912			\|a GBV_ILN_2044
912			\|a GBV_ILN_2048
912			\|a GBV_ILN_2049
912			\|a GBV_ILN_2050
912			\|a GBV_ILN_2055
912			\|a GBV_ILN_2057
912			\|a GBV_ILN_2059
912			\|a GBV_ILN_2061
912			\|a GBV_ILN_2064
912			\|a GBV_ILN_2065
912			\|a GBV_ILN_2068
912			\|a GBV_ILN_2070
912			\|a GBV_ILN_2086
912			\|a GBV_ILN_2088
912			\|a GBV_ILN_2093
912			\|a GBV_ILN_2106
912			\|a GBV_ILN_2107
912			\|a GBV_ILN_2108
912			\|a GBV_ILN_2110
912			\|a GBV_ILN_2111
912			\|a GBV_ILN_2112
912			\|a GBV_ILN_2113
912			\|a GBV_ILN_2116
912			\|a GBV_ILN_2118
912			\|a GBV_ILN_2119
912			\|a GBV_ILN_2122
912			\|a GBV_ILN_2129
912			\|a GBV_ILN_2143
912			\|a GBV_ILN_2144
912			\|a GBV_ILN_2147
912			\|a GBV_ILN_2148
912			\|a GBV_ILN_2152
912			\|a GBV_ILN_2153
912			\|a GBV_ILN_2188
912			\|a GBV_ILN_2190
912			\|a GBV_ILN_2232
912			\|a GBV_ILN_2336
912			\|a GBV_ILN_2446
912			\|a GBV_ILN_2470
912			\|a GBV_ILN_2472
912			\|a GBV_ILN_2507
912			\|a GBV_ILN_2522
912			\|a GBV_ILN_2548
912			\|a GBV_ILN_4012
912			\|a GBV_ILN_4035
912			\|a GBV_ILN_4037
912			\|a GBV_ILN_4046
912			\|a GBV_ILN_4112
912			\|a GBV_ILN_4125
912			\|a GBV_ILN_4126
912			\|a GBV_ILN_4242
912			\|a GBV_ILN_4246
912			\|a GBV_ILN_4249
912			\|a GBV_ILN_4251
912			\|a GBV_ILN_4305
912			\|a GBV_ILN_4306
912			\|a GBV_ILN_4307
912			\|a GBV_ILN_4313
912			\|a GBV_ILN_4322
912			\|a GBV_ILN_4323
912			\|a GBV_ILN_4324
912			\|a GBV_ILN_4325
912			\|a GBV_ILN_4326
912			\|a GBV_ILN_4333
912			\|a GBV_ILN_4334
912			\|a GBV_ILN_4335
912			\|a GBV_ILN_4336
912			\|a GBV_ILN_4338
912			\|a GBV_ILN_4393
912			\|a GBV_ILN_4700
936	b	k	\|a 39.00 \|q ASE
951			\|a AR
952			\|d 40 \|j 2015 \|e 2-3 \|b 29 \|c 11 \|h 329-391

Indexfelder

author_variant	g t gt p d pd p e pe p h ph k i ki m l ml c l cl g m gm m o mo l p lp i r ir i s is b s bs f a fa j b jb j c jc a c ac c c cc a c ac l d ld k r d kr krd p d pd t e te f f ff a g ag c g cg t g tg t k tk h l hl j l jl p m pm i m w imw r n rn c n cn e p ep i p ip g p gp d p dp f s fs a s as l s ls j t jt d t dt m z o mzo j p b jpb d g dg m g mg d l dl h u n n hun hunn t r tr h r hr a s as m s ms m b mb m b mb n b nb g b r gbr f v c d fvc fvcd j c g jcg l g lg a h ah c j cj f k fk g k gk p o l pol t l tl m l m mlm g m gm e p ep e p ep b v bv g w gw g r z gr grz a a aa r a ra a b ab i b ib r b rb j c jc m c mc g a d ga gad m g mg r h rh r o ro r i ri k m km g m gm f p fp m r mr j m r jmr g s gs j r s jrs r s rs b w bw l a la m a ma n a na p a pa v a va l a la c a ca m a ma c a ca j a ja p c a pc pca f f j a ffj ffja f a fa i c a a ica icaa p a pa a a aa a a aa c b cb g b gb p b pb m b mb r j b rj rjb d b db e j b ej ejb v b vb g b gb a j a b aja ajab d b db b b bb d b db m b mb i b ib b b bb p b pb p b pb h b hb l b lb l b lb j b jb a b ab m b mb a c ac m t c mt mtc a c ac c c cc c c p ccp r c rc j c jc s c sc s c sc j n c jn jnc a c ac a c ac r c rc a c ac r c rc a c ac d c dc e c ec c d cd m d md h j d hj hjd e d m edm v c d vc vcd o d od s a d sa sad w j d wj wjd m d md p d pd c d cd e d ed s e se c e ce c m e cm cme m e me v e ve n f nf m f mf c b f cb cbf p f pf g f gf l f lf m f mf s f sf p f pf j f jf m g mg l g lg p g pg l r j g lrj lrjg a g p agp w g wg j c g jcg l g lg e g eg f g fg m g mg e g eg m g mg h g hg i g l igl h j g hj hjg m b g mb mbg r g rg d g dg j g jg p g pg j g jg p h ph j h jh e h eh u h uh r l h rl rlh e h eh f h fh d h dh m h mh b h bh r h rh g i gi n i ni p i pi s j sj g j gj h j hj k j kj t k tk f k fk e k ek p k pk d k dk t k tk n k nk o l ol b l bl n l nl e l el g l gl g j l gj gjl c l b clb s j l sj sjl c u l cu cul n l nl p l pl m l p mlp m a l v mal malv r i l ri ril a l al p m pm c m cm a m am j p m jpm w m wm j m jm u m um j b m jbm p m pm f m fm a s m asm a m am c m cm p m p pmp m m mm r p m rp rpm m m mm d m dm h m hm j c m jc jcm m m c mmc g m gm m a m ma mam j m jm b a m ba bam a f m af afm e o eo g o go f p fp m p mp e p ep v p vp h p hp r k y p rky rkyp j p jp s p h sph r p rp s p sp r p rp e p l epl n p np r p rp l p lp i p ip e p ep a r ar a a r aa aar t r l trl p r pr k r kr l r r lr lrr j r jr m r mr l r lr m r mr f r fr b v j s bvj bvjs l a s la las e s es n s ns f j s fj fjs g s gs f x s fxs a s as s s ss j s js s s ss a s as b s bs p s ps a s as l s ls s s ss a s as m s ms g s gs h m t hm hmt p t pt m t mt j t jt l t lt m t mt l t lt s t st h t ht b w t bw bwt m t mt t j m tj tjm a t at d t dt r v rv f v fv v b m d vbm vbmd m l v ml mlv o v ov e v ev s v sv s v sv i w iw d w dw d w t dwt r w rw c w cw d w dw p w pw a w aw g w gw t w tw w w ww t w tw r y ry y y yy s n y sn sny
matchkey_str	article:15729508:2015----::hehsin
hierarchy_sort_str	2015
bklnumber	39.00
publishDate	2015
allfields	10.1007/s10686-015-9484-8 doi (DE-627)SPR012459186 (SPR)s10686-015-9484-8-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Tinetti, Giovanna verfasserin aut The EChO science case 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213 Drossart, Pierre verfasserin aut Eccleston, Paul verfasserin aut Hartogh, Paul verfasserin aut Isaak, Kate verfasserin aut Linder, Martin verfasserin aut Lovis, Christophe verfasserin aut Micela, Giusi verfasserin aut Ollivier, Marc verfasserin aut Puig, Ludovic verfasserin aut Ribas, Ignasi verfasserin aut Snellen, Ignas verfasserin aut Swinyard, Bruce verfasserin aut Allard, France verfasserin aut Barstow, Joanna verfasserin aut Cho, James verfasserin aut Coustenis, Athena verfasserin aut Cockell, Charles verfasserin aut Correia, Alexandre verfasserin aut Decin, Leen verfasserin aut de Kok, Remco verfasserin aut Deroo, Pieter verfasserin aut Encrenaz, Therese verfasserin aut Forget, Francois verfasserin aut Glasse, Alistair verfasserin aut Griffith, Caitlin verfasserin aut Guillot, Tristan verfasserin aut Koskinen, Tommi verfasserin aut Lammer, Helmut verfasserin aut Leconte, Jeremy verfasserin aut Maxted, Pierre verfasserin aut Mueller-Wodarg, Ingo verfasserin aut Nelson, Richard verfasserin aut North, Chris verfasserin aut Pallé, Enric verfasserin aut Pagano, Isabella verfasserin aut Piccioni, Guseppe verfasserin aut Pinfield, David verfasserin aut Selsis, Franck verfasserin aut Sozzetti, Alessandro verfasserin aut Stixrude, Lars verfasserin aut Tennyson, Jonathan verfasserin aut Turrini, Diego verfasserin aut Zapatero-Osorio, Mariarosa verfasserin aut Beaulieu, Jean-Philippe verfasserin aut Grodent, Denis verfasserin aut Guedel, Manuel verfasserin aut Luz, David verfasserin aut Nørgaard-Nielsen, Hans Ulrik verfasserin aut Ray, Tom verfasserin aut Rickman, Hans verfasserin aut Selig, Avri verfasserin aut Swain, Mark verfasserin aut Banaszkiewicz, Marek verfasserin aut Barlow, Mike verfasserin aut Bowles, Neil verfasserin aut Branduardi-Raymont, Graziella verfasserin aut du Foresto, Vincent Coudé verfasserin aut Gerard, Jean-Claude verfasserin aut Gizon, Laurent verfasserin aut Hornstrup, Allan verfasserin aut Jarchow, Christopher verfasserin aut Kerschbaum, Franz verfasserin aut Kovacs, Géza verfasserin aut Lagage, Pierre-Olivier verfasserin aut Lim, Tanya verfasserin aut Lopez-Morales, Mercedes verfasserin aut Malaguti, Giuseppe verfasserin aut Pace, Emanuele verfasserin aut Pascale, Enzo verfasserin aut Vandenbussche, Bart verfasserin aut Wright, Gillian verfasserin aut Zapata, Gonzalo Ramos verfasserin aut Adriani, Alberto verfasserin aut Azzollini, Ruymán verfasserin aut Balado, Ana verfasserin aut Bryson, Ian verfasserin aut Burston, Raymond verfasserin aut Colomé, Josep verfasserin aut Crook, Martin verfasserin aut Di Giorgio, Anna verfasserin aut Griffin, Matt verfasserin aut Hoogeveen, Ruud verfasserin aut Ottensamer, Roland verfasserin aut Irshad, Ranah verfasserin aut Middleton, Kevin verfasserin aut Morgante, Gianluca verfasserin aut Pinsard, Frederic verfasserin aut Rataj, Mirek verfasserin aut Reess, Jean-Michel verfasserin aut Savini, Giorgio verfasserin aut Schrader, Jan-Rutger verfasserin aut Stamper, Richard verfasserin aut Winter, Berend verfasserin aut Abe, L. verfasserin aut Abreu, M. verfasserin aut Achilleos, N. verfasserin aut Ade, P. verfasserin aut Adybekian, V. verfasserin aut Affer, L. verfasserin aut Agnor, C. verfasserin aut Agundez, M. verfasserin aut Alard, C. verfasserin aut Alcala, J. verfasserin aut Allende Prieto, C. verfasserin aut Alonso Floriano, F. J. verfasserin aut Altieri, F. verfasserin aut Alvarez Iglesias, C. A. verfasserin aut Amado, P. verfasserin aut Andersen, A. verfasserin aut Aylward, A. verfasserin aut Baffa, C. verfasserin aut Bakos, G. verfasserin aut Ballerini, P. verfasserin aut Banaszkiewicz, M. verfasserin aut Barber, R. J. verfasserin aut Barrado, D. verfasserin aut Barton, E. J. verfasserin aut Batista, V. verfasserin aut Bellucci, G. verfasserin aut Belmonte Avilés, J. A. verfasserin aut Berry, D. verfasserin aut Bézard, B. verfasserin aut Biondi, D. verfasserin aut Błęcka, M. verfasserin aut Boisse, I. verfasserin aut Bonfond, B. verfasserin aut Bordé, P. verfasserin aut Börner, P. verfasserin aut Bouy, H. verfasserin aut Brown, L. verfasserin aut Buchhave, L. verfasserin aut Budaj, J. verfasserin aut Bulgarelli, A. verfasserin aut Burleigh, M. verfasserin aut Cabral, A. verfasserin aut Capria, M. T. verfasserin aut Cassan, A. verfasserin aut Cavarroc, C. verfasserin aut Cecchi-Pestellini, C. verfasserin aut Cerulli, R. verfasserin aut Chadney, J. verfasserin aut Chamberlain, S. verfasserin aut Charnoz, S. verfasserin aut Christian Jessen, N. verfasserin aut Ciaravella, A. verfasserin aut Claret, A. verfasserin aut Claudi, R. verfasserin aut Coates, A. verfasserin aut Cole, R. verfasserin aut Collura, A. verfasserin aut Cordier, D. verfasserin aut Covino, E. verfasserin aut Danielski, C. verfasserin aut Damasso, M. verfasserin aut Deeg, H. J. verfasserin aut Delgado-Mena, E. verfasserin aut Del Vecchio, C. verfasserin aut Demangeon, O. verfasserin aut De Sio, A. verfasserin aut De Wit, J. verfasserin aut Dobrijévic, M. verfasserin aut Doel, P. verfasserin aut Dominic, C. verfasserin aut Dorfi, E. verfasserin aut Eales, S. verfasserin aut Eiroa, C. verfasserin aut Espinoza Contreras, M. verfasserin aut Esposito, M. verfasserin aut Eymet, V. verfasserin aut Fabrizio, N. verfasserin aut Fernández, M. verfasserin aut Femenía Castella, B. verfasserin aut Figueira, P. verfasserin aut Filacchione, G. verfasserin aut Fletcher, L. verfasserin aut Focardi, M. verfasserin aut Fossey, S. verfasserin aut Fouqué, P. verfasserin aut Frith, J. verfasserin aut Galand, M. verfasserin aut Gambicorti, L. verfasserin aut Gaulme, P. verfasserin aut García López, R. J. verfasserin aut Garcia-Piquer, A. verfasserin aut Gear, W. verfasserin aut Gerard, J.-C. verfasserin aut Gesa, L. verfasserin aut Giani, E. verfasserin aut Gianotti, F. verfasserin aut Gillon, M. verfasserin aut Giro, E. verfasserin aut Giuranna, M. verfasserin aut Gomez, H. verfasserin aut Gomez-Leal, I. verfasserin aut Gonzalez Hernandez, J. verfasserin aut González Merino, B. verfasserin aut Graczyk, R. verfasserin aut Grassi, D. verfasserin aut Guardia, J. verfasserin aut Guio, P. verfasserin aut Gustin, J. verfasserin aut Hargrave, P. verfasserin aut Haigh, J. verfasserin aut Hébrard, E. verfasserin aut Heiter, U. verfasserin aut Heredero, R. L. verfasserin aut Herrero, E. verfasserin aut Hersant, F. verfasserin aut Heyrovsky, D. verfasserin aut Hollis, M. verfasserin aut Hubert, B. verfasserin aut Hueso, R. verfasserin aut Israelian, G. verfasserin aut Iro, N. verfasserin aut Irwin, P. verfasserin aut Jacquemoud, S. verfasserin aut Jones, G. verfasserin aut Jones, H. verfasserin aut Justtanont, K. verfasserin aut Kehoe, T. verfasserin aut Kerschbaum, F. verfasserin aut Kerins, E. verfasserin aut Kervella, P. verfasserin aut Kipping, D. verfasserin aut Koskinen, T. verfasserin aut Krupp, N. verfasserin aut Lahav, O. verfasserin aut Laken, B. verfasserin aut Lanza, N. verfasserin aut Lellouch, E. verfasserin aut Leto, G. verfasserin aut Licandro Goldaracena, J. verfasserin aut Lithgow-Bertelloni, C. verfasserin aut Liu, S. J. verfasserin aut Lo Cicero, U. verfasserin aut Lodieu, N. verfasserin aut Lognonné, P. verfasserin aut Lopez-Puertas, M. verfasserin aut Lopez-Valverde, M. A. verfasserin aut Lundgaard Rasmussen, I. verfasserin aut Luntzer, A. verfasserin aut Machado, P. verfasserin aut MacTavish, C. verfasserin aut Maggio, A. verfasserin aut Maillard, J.-P. verfasserin aut Magnes, W. verfasserin aut Maldonado, J. verfasserin aut Mall, U. verfasserin aut Marquette, J.-B. verfasserin aut Mauskopf, P. verfasserin aut Massi, F. verfasserin aut Maurin, A.-S. verfasserin aut Medvedev, A. verfasserin aut Michaut, C. verfasserin aut Miles-Paez, P. verfasserin aut Montalto, M. verfasserin aut Montañés Rodríguez, P. verfasserin aut Monteiro, M. verfasserin aut Montes, D. verfasserin aut Morais, H. verfasserin aut Morales, J. C. verfasserin aut Morales-Calderón, M. verfasserin aut Morello, G. verfasserin aut Moro Martín, A. verfasserin aut Moses, J. verfasserin aut Moya Bedon, A. verfasserin aut Murgas Alcaino, F. verfasserin aut Oliva, E. verfasserin aut Orton, G. verfasserin aut Palla, F. verfasserin aut Pancrazzi, M. verfasserin aut Pantin, E. verfasserin aut Parmentier, V. verfasserin aut Parviainen, H. verfasserin aut Peña Ramírez, K. Y. verfasserin aut Peralta, J. verfasserin aut Perez-Hoyos, S. verfasserin aut Petrov, R. verfasserin aut Pezzuto, S. verfasserin aut Pietrzak, R. verfasserin aut Pilat-Lohinger, E. verfasserin aut Piskunov, N. verfasserin aut Prinja, R. verfasserin aut Prisinzano, L. verfasserin aut Polichtchouk, I. verfasserin aut Poretti, E. verfasserin aut Radioti, A. verfasserin aut Ramos, A. A. verfasserin aut Rank-Lüftinger, T. verfasserin aut Read, P. verfasserin aut Readorn, K. verfasserin aut Rebolo López, R. verfasserin aut Rebordão, J. verfasserin aut Rengel, M. verfasserin aut Rezac, L. verfasserin aut Rocchetto, M. verfasserin aut Rodler, F. verfasserin aut Sánchez Béjar, V. J. verfasserin aut Sanchez Lavega, A. verfasserin aut Sanromá, E. verfasserin aut Santos, N. verfasserin aut Sanz Forcada, J. verfasserin aut Scandariato, G. verfasserin aut Schmider, F.-X. verfasserin aut Scholz, A. verfasserin aut Scuderi, S. verfasserin aut Sethenadh, J. verfasserin aut Shore, S. verfasserin aut Showman, A. verfasserin aut Sicardy, B. verfasserin aut Sitek, P. verfasserin aut Smith, A. verfasserin aut Soret, L. verfasserin aut Sousa, S. verfasserin aut Stiepen, A. verfasserin aut Stolarski, M. verfasserin aut Strazzulla, G. verfasserin aut Tabernero, H. M. verfasserin aut Tanga, P. verfasserin aut Tecsa, M. verfasserin aut Temple, J. verfasserin aut Terenzi, L. verfasserin aut Tessenyi, M. verfasserin aut Testi, L. verfasserin aut Thompson, S. verfasserin aut Thrastarson, H. verfasserin aut Tingley, B. W. verfasserin aut Trifoglio, M. verfasserin aut Martín Torres, J. verfasserin aut Tozzi, A. verfasserin aut Turrini, D. verfasserin aut Varley, R. verfasserin aut Vakili, F. verfasserin aut de Val-Borro, M. verfasserin aut Valdivieso, M. L. verfasserin aut Venot, O. verfasserin aut Villaver, E. verfasserin aut Vinatier, S. verfasserin aut Viti, S. verfasserin aut Waldmann, I. verfasserin aut Waltham, D. verfasserin aut Ward-Thompson, D. verfasserin aut Waters, R. verfasserin aut Watkins, C. verfasserin aut Watson, D. verfasserin aut Wawer, P. verfasserin aut Wawrzaszk, A. verfasserin aut White, G. verfasserin aut Widemann, T. verfasserin aut Winek, W. verfasserin aut Wiśniowski, T. verfasserin aut Yelle, R. verfasserin aut Yung, Y. verfasserin aut Yurchenko, S. N. verfasserin aut Enthalten in Experimental astronomy Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 40(2015), 2-3 vom: 29. Nov., Seite 329-391 (DE-627)312841116 (DE-600)2012330-9 1572-9508 nnns volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391 https://dx.doi.org/10.1007/s10686-015-9484-8 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 40 2015 2-3 29 11 329-391
spelling	10.1007/s10686-015-9484-8 doi (DE-627)SPR012459186 (SPR)s10686-015-9484-8-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Tinetti, Giovanna verfasserin aut The EChO science case 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213 Drossart, Pierre verfasserin aut Eccleston, Paul verfasserin aut Hartogh, Paul verfasserin aut Isaak, Kate verfasserin aut Linder, Martin verfasserin aut Lovis, Christophe verfasserin aut Micela, Giusi verfasserin aut Ollivier, Marc verfasserin aut Puig, Ludovic verfasserin aut Ribas, Ignasi verfasserin aut Snellen, Ignas verfasserin aut Swinyard, Bruce verfasserin aut Allard, France verfasserin aut Barstow, Joanna verfasserin aut Cho, James verfasserin aut Coustenis, Athena verfasserin aut Cockell, Charles verfasserin aut Correia, Alexandre verfasserin aut Decin, Leen verfasserin aut de Kok, Remco verfasserin aut Deroo, Pieter verfasserin aut Encrenaz, Therese verfasserin aut Forget, Francois verfasserin aut Glasse, Alistair verfasserin aut Griffith, Caitlin verfasserin aut Guillot, Tristan verfasserin aut Koskinen, Tommi verfasserin aut Lammer, Helmut verfasserin aut Leconte, Jeremy verfasserin aut Maxted, Pierre verfasserin aut Mueller-Wodarg, Ingo verfasserin aut Nelson, Richard verfasserin aut North, Chris verfasserin aut Pallé, Enric verfasserin aut Pagano, Isabella verfasserin aut Piccioni, Guseppe verfasserin aut Pinfield, David verfasserin aut Selsis, Franck verfasserin aut Sozzetti, Alessandro verfasserin aut Stixrude, Lars verfasserin aut Tennyson, Jonathan verfasserin aut Turrini, Diego verfasserin aut Zapatero-Osorio, Mariarosa verfasserin aut Beaulieu, Jean-Philippe verfasserin aut Grodent, Denis verfasserin aut Guedel, Manuel verfasserin aut Luz, David verfasserin aut Nørgaard-Nielsen, Hans Ulrik verfasserin aut Ray, Tom verfasserin aut Rickman, Hans verfasserin aut Selig, Avri verfasserin aut Swain, Mark verfasserin aut Banaszkiewicz, Marek verfasserin aut Barlow, Mike verfasserin aut Bowles, Neil verfasserin aut Branduardi-Raymont, Graziella verfasserin aut du Foresto, Vincent Coudé verfasserin aut Gerard, Jean-Claude verfasserin aut Gizon, Laurent verfasserin aut Hornstrup, Allan verfasserin aut Jarchow, Christopher verfasserin aut Kerschbaum, Franz verfasserin aut Kovacs, Géza verfasserin aut Lagage, Pierre-Olivier verfasserin aut Lim, Tanya verfasserin aut Lopez-Morales, Mercedes verfasserin aut Malaguti, Giuseppe verfasserin aut Pace, Emanuele verfasserin aut Pascale, Enzo verfasserin aut Vandenbussche, Bart verfasserin aut Wright, Gillian verfasserin aut Zapata, Gonzalo Ramos verfasserin aut Adriani, Alberto verfasserin aut Azzollini, Ruymán verfasserin aut Balado, Ana verfasserin aut Bryson, Ian verfasserin aut Burston, Raymond verfasserin aut Colomé, Josep verfasserin aut Crook, Martin verfasserin aut Di Giorgio, Anna verfasserin aut Griffin, Matt verfasserin aut Hoogeveen, Ruud verfasserin aut Ottensamer, Roland verfasserin aut Irshad, Ranah verfasserin aut Middleton, Kevin verfasserin aut Morgante, Gianluca verfasserin aut Pinsard, Frederic verfasserin aut Rataj, Mirek verfasserin aut Reess, Jean-Michel verfasserin aut Savini, Giorgio verfasserin aut Schrader, Jan-Rutger verfasserin aut Stamper, Richard verfasserin aut Winter, Berend verfasserin aut Abe, L. verfasserin aut Abreu, M. verfasserin aut Achilleos, N. verfasserin aut Ade, P. verfasserin aut Adybekian, V. verfasserin aut Affer, L. verfasserin aut Agnor, C. verfasserin aut Agundez, M. verfasserin aut Alard, C. verfasserin aut Alcala, J. verfasserin aut Allende Prieto, C. verfasserin aut Alonso Floriano, F. J. verfasserin aut Altieri, F. verfasserin aut Alvarez Iglesias, C. A. verfasserin aut Amado, P. verfasserin aut Andersen, A. verfasserin aut Aylward, A. verfasserin aut Baffa, C. verfasserin aut Bakos, G. verfasserin aut Ballerini, P. verfasserin aut Banaszkiewicz, M. verfasserin aut Barber, R. J. verfasserin aut Barrado, D. verfasserin aut Barton, E. J. verfasserin aut Batista, V. verfasserin aut Bellucci, G. verfasserin aut Belmonte Avilés, J. A. verfasserin aut Berry, D. verfasserin aut Bézard, B. verfasserin aut Biondi, D. verfasserin aut Błęcka, M. verfasserin aut Boisse, I. verfasserin aut Bonfond, B. verfasserin aut Bordé, P. verfasserin aut Börner, P. verfasserin aut Bouy, H. verfasserin aut Brown, L. verfasserin aut Buchhave, L. verfasserin aut Budaj, J. verfasserin aut Bulgarelli, A. verfasserin aut Burleigh, M. verfasserin aut Cabral, A. verfasserin aut Capria, M. T. verfasserin aut Cassan, A. verfasserin aut Cavarroc, C. verfasserin aut Cecchi-Pestellini, C. verfasserin aut Cerulli, R. verfasserin aut Chadney, J. verfasserin aut Chamberlain, S. verfasserin aut Charnoz, S. verfasserin aut Christian Jessen, N. verfasserin aut Ciaravella, A. verfasserin aut Claret, A. verfasserin aut Claudi, R. verfasserin aut Coates, A. verfasserin aut Cole, R. verfasserin aut Collura, A. verfasserin aut Cordier, D. verfasserin aut Covino, E. verfasserin aut Danielski, C. verfasserin aut Damasso, M. verfasserin aut Deeg, H. J. verfasserin aut Delgado-Mena, E. verfasserin aut Del Vecchio, C. verfasserin aut Demangeon, O. verfasserin aut De Sio, A. verfasserin aut De Wit, J. verfasserin aut Dobrijévic, M. verfasserin aut Doel, P. verfasserin aut Dominic, C. verfasserin aut Dorfi, E. verfasserin aut Eales, S. verfasserin aut Eiroa, C. verfasserin aut Espinoza Contreras, M. verfasserin aut Esposito, M. verfasserin aut Eymet, V. verfasserin aut Fabrizio, N. verfasserin aut Fernández, M. verfasserin aut Femenía Castella, B. verfasserin aut Figueira, P. verfasserin aut Filacchione, G. verfasserin aut Fletcher, L. verfasserin aut Focardi, M. verfasserin aut Fossey, S. verfasserin aut Fouqué, P. verfasserin aut Frith, J. verfasserin aut Galand, M. verfasserin aut Gambicorti, L. verfasserin aut Gaulme, P. verfasserin aut García López, R. J. verfasserin aut Garcia-Piquer, A. verfasserin aut Gear, W. verfasserin aut Gerard, J.-C. verfasserin aut Gesa, L. verfasserin aut Giani, E. verfasserin aut Gianotti, F. verfasserin aut Gillon, M. verfasserin aut Giro, E. verfasserin aut Giuranna, M. verfasserin aut Gomez, H. verfasserin aut Gomez-Leal, I. verfasserin aut Gonzalez Hernandez, J. verfasserin aut González Merino, B. verfasserin aut Graczyk, R. verfasserin aut Grassi, D. verfasserin aut Guardia, J. verfasserin aut Guio, P. verfasserin aut Gustin, J. verfasserin aut Hargrave, P. verfasserin aut Haigh, J. verfasserin aut Hébrard, E. verfasserin aut Heiter, U. verfasserin aut Heredero, R. L. verfasserin aut Herrero, E. verfasserin aut Hersant, F. verfasserin aut Heyrovsky, D. verfasserin aut Hollis, M. verfasserin aut Hubert, B. verfasserin aut Hueso, R. verfasserin aut Israelian, G. verfasserin aut Iro, N. verfasserin aut Irwin, P. verfasserin aut Jacquemoud, S. verfasserin aut Jones, G. verfasserin aut Jones, H. verfasserin aut Justtanont, K. verfasserin aut Kehoe, T. verfasserin aut Kerschbaum, F. verfasserin aut Kerins, E. verfasserin aut Kervella, P. verfasserin aut Kipping, D. verfasserin aut Koskinen, T. verfasserin aut Krupp, N. verfasserin aut Lahav, O. verfasserin aut Laken, B. verfasserin aut Lanza, N. verfasserin aut Lellouch, E. verfasserin aut Leto, G. verfasserin aut Licandro Goldaracena, J. verfasserin aut Lithgow-Bertelloni, C. verfasserin aut Liu, S. J. verfasserin aut Lo Cicero, U. verfasserin aut Lodieu, N. verfasserin aut Lognonné, P. verfasserin aut Lopez-Puertas, M. verfasserin aut Lopez-Valverde, M. A. verfasserin aut Lundgaard Rasmussen, I. verfasserin aut Luntzer, A. verfasserin aut Machado, P. verfasserin aut MacTavish, C. verfasserin aut Maggio, A. verfasserin aut Maillard, J.-P. verfasserin aut Magnes, W. verfasserin aut Maldonado, J. verfasserin aut Mall, U. verfasserin aut Marquette, J.-B. verfasserin aut Mauskopf, P. verfasserin aut Massi, F. verfasserin aut Maurin, A.-S. verfasserin aut Medvedev, A. verfasserin aut Michaut, C. verfasserin aut Miles-Paez, P. verfasserin aut Montalto, M. verfasserin aut Montañés Rodríguez, P. verfasserin aut Monteiro, M. verfasserin aut Montes, D. verfasserin aut Morais, H. verfasserin aut Morales, J. C. verfasserin aut Morales-Calderón, M. verfasserin aut Morello, G. verfasserin aut Moro Martín, A. verfasserin aut Moses, J. verfasserin aut Moya Bedon, A. verfasserin aut Murgas Alcaino, F. verfasserin aut Oliva, E. verfasserin aut Orton, G. verfasserin aut Palla, F. verfasserin aut Pancrazzi, M. verfasserin aut Pantin, E. verfasserin aut Parmentier, V. verfasserin aut Parviainen, H. verfasserin aut Peña Ramírez, K. Y. verfasserin aut Peralta, J. verfasserin aut Perez-Hoyos, S. verfasserin aut Petrov, R. verfasserin aut Pezzuto, S. verfasserin aut Pietrzak, R. verfasserin aut Pilat-Lohinger, E. verfasserin aut Piskunov, N. verfasserin aut Prinja, R. verfasserin aut Prisinzano, L. verfasserin aut Polichtchouk, I. verfasserin aut Poretti, E. verfasserin aut Radioti, A. verfasserin aut Ramos, A. A. verfasserin aut Rank-Lüftinger, T. verfasserin aut Read, P. verfasserin aut Readorn, K. verfasserin aut Rebolo López, R. verfasserin aut Rebordão, J. verfasserin aut Rengel, M. verfasserin aut Rezac, L. verfasserin aut Rocchetto, M. verfasserin aut Rodler, F. verfasserin aut Sánchez Béjar, V. J. verfasserin aut Sanchez Lavega, A. verfasserin aut Sanromá, E. verfasserin aut Santos, N. verfasserin aut Sanz Forcada, J. verfasserin aut Scandariato, G. verfasserin aut Schmider, F.-X. verfasserin aut Scholz, A. verfasserin aut Scuderi, S. verfasserin aut Sethenadh, J. verfasserin aut Shore, S. verfasserin aut Showman, A. verfasserin aut Sicardy, B. verfasserin aut Sitek, P. verfasserin aut Smith, A. verfasserin aut Soret, L. verfasserin aut Sousa, S. verfasserin aut Stiepen, A. verfasserin aut Stolarski, M. verfasserin aut Strazzulla, G. verfasserin aut Tabernero, H. M. verfasserin aut Tanga, P. verfasserin aut Tecsa, M. verfasserin aut Temple, J. verfasserin aut Terenzi, L. verfasserin aut Tessenyi, M. verfasserin aut Testi, L. verfasserin aut Thompson, S. verfasserin aut Thrastarson, H. verfasserin aut Tingley, B. W. verfasserin aut Trifoglio, M. verfasserin aut Martín Torres, J. verfasserin aut Tozzi, A. verfasserin aut Turrini, D. verfasserin aut Varley, R. verfasserin aut Vakili, F. verfasserin aut de Val-Borro, M. verfasserin aut Valdivieso, M. L. verfasserin aut Venot, O. verfasserin aut Villaver, E. verfasserin aut Vinatier, S. verfasserin aut Viti, S. verfasserin aut Waldmann, I. verfasserin aut Waltham, D. verfasserin aut Ward-Thompson, D. verfasserin aut Waters, R. verfasserin aut Watkins, C. verfasserin aut Watson, D. verfasserin aut Wawer, P. verfasserin aut Wawrzaszk, A. verfasserin aut White, G. verfasserin aut Widemann, T. verfasserin aut Winek, W. verfasserin aut Wiśniowski, T. verfasserin aut Yelle, R. verfasserin aut Yung, Y. verfasserin aut Yurchenko, S. N. verfasserin aut Enthalten in Experimental astronomy Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 40(2015), 2-3 vom: 29. Nov., Seite 329-391 (DE-627)312841116 (DE-600)2012330-9 1572-9508 nnns volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391 https://dx.doi.org/10.1007/s10686-015-9484-8 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 40 2015 2-3 29 11 329-391
allfields_unstemmed	10.1007/s10686-015-9484-8 doi (DE-627)SPR012459186 (SPR)s10686-015-9484-8-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Tinetti, Giovanna verfasserin aut The EChO science case 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213 Drossart, Pierre verfasserin aut Eccleston, Paul verfasserin aut Hartogh, Paul verfasserin aut Isaak, Kate verfasserin aut Linder, Martin verfasserin aut Lovis, Christophe verfasserin aut Micela, Giusi verfasserin aut Ollivier, Marc verfasserin aut Puig, Ludovic verfasserin aut Ribas, Ignasi verfasserin aut Snellen, Ignas verfasserin aut Swinyard, Bruce verfasserin aut Allard, France verfasserin aut Barstow, Joanna verfasserin aut Cho, James verfasserin aut Coustenis, Athena verfasserin aut Cockell, Charles verfasserin aut Correia, Alexandre verfasserin aut Decin, Leen verfasserin aut de Kok, Remco verfasserin aut Deroo, Pieter verfasserin aut Encrenaz, Therese verfasserin aut Forget, Francois verfasserin aut Glasse, Alistair verfasserin aut Griffith, Caitlin verfasserin aut Guillot, Tristan verfasserin aut Koskinen, Tommi verfasserin aut Lammer, Helmut verfasserin aut Leconte, Jeremy verfasserin aut Maxted, Pierre verfasserin aut Mueller-Wodarg, Ingo verfasserin aut Nelson, Richard verfasserin aut North, Chris verfasserin aut Pallé, Enric verfasserin aut Pagano, Isabella verfasserin aut Piccioni, Guseppe verfasserin aut Pinfield, David verfasserin aut Selsis, Franck verfasserin aut Sozzetti, Alessandro verfasserin aut Stixrude, Lars verfasserin aut Tennyson, Jonathan verfasserin aut Turrini, Diego verfasserin aut Zapatero-Osorio, Mariarosa verfasserin aut Beaulieu, Jean-Philippe verfasserin aut Grodent, Denis verfasserin aut Guedel, Manuel verfasserin aut Luz, David verfasserin aut Nørgaard-Nielsen, Hans Ulrik verfasserin aut Ray, Tom verfasserin aut Rickman, Hans verfasserin aut Selig, Avri verfasserin aut Swain, Mark verfasserin aut Banaszkiewicz, Marek verfasserin aut Barlow, Mike verfasserin aut Bowles, Neil verfasserin aut Branduardi-Raymont, Graziella verfasserin aut du Foresto, Vincent Coudé verfasserin aut Gerard, Jean-Claude verfasserin aut Gizon, Laurent verfasserin aut Hornstrup, Allan verfasserin aut Jarchow, Christopher verfasserin aut Kerschbaum, Franz verfasserin aut Kovacs, Géza verfasserin aut Lagage, Pierre-Olivier verfasserin aut Lim, Tanya verfasserin aut Lopez-Morales, Mercedes verfasserin aut Malaguti, Giuseppe verfasserin aut Pace, Emanuele verfasserin aut Pascale, Enzo verfasserin aut Vandenbussche, Bart verfasserin aut Wright, Gillian verfasserin aut Zapata, Gonzalo Ramos verfasserin aut Adriani, Alberto verfasserin aut Azzollini, Ruymán verfasserin aut Balado, Ana verfasserin aut Bryson, Ian verfasserin aut Burston, Raymond verfasserin aut Colomé, Josep verfasserin aut Crook, Martin verfasserin aut Di Giorgio, Anna verfasserin aut Griffin, Matt verfasserin aut Hoogeveen, Ruud verfasserin aut Ottensamer, Roland verfasserin aut Irshad, Ranah verfasserin aut Middleton, Kevin verfasserin aut Morgante, Gianluca verfasserin aut Pinsard, Frederic verfasserin aut Rataj, Mirek verfasserin aut Reess, Jean-Michel verfasserin aut Savini, Giorgio verfasserin aut Schrader, Jan-Rutger verfasserin aut Stamper, Richard verfasserin aut Winter, Berend verfasserin aut Abe, L. verfasserin aut Abreu, M. verfasserin aut Achilleos, N. verfasserin aut Ade, P. verfasserin aut Adybekian, V. verfasserin aut Affer, L. verfasserin aut Agnor, C. verfasserin aut Agundez, M. verfasserin aut Alard, C. verfasserin aut Alcala, J. verfasserin aut Allende Prieto, C. verfasserin aut Alonso Floriano, F. J. verfasserin aut Altieri, F. verfasserin aut Alvarez Iglesias, C. A. verfasserin aut Amado, P. verfasserin aut Andersen, A. verfasserin aut Aylward, A. verfasserin aut Baffa, C. verfasserin aut Bakos, G. verfasserin aut Ballerini, P. verfasserin aut Banaszkiewicz, M. verfasserin aut Barber, R. J. verfasserin aut Barrado, D. verfasserin aut Barton, E. J. verfasserin aut Batista, V. verfasserin aut Bellucci, G. verfasserin aut Belmonte Avilés, J. A. verfasserin aut Berry, D. verfasserin aut Bézard, B. verfasserin aut Biondi, D. verfasserin aut Błęcka, M. verfasserin aut Boisse, I. verfasserin aut Bonfond, B. verfasserin aut Bordé, P. verfasserin aut Börner, P. verfasserin aut Bouy, H. verfasserin aut Brown, L. verfasserin aut Buchhave, L. verfasserin aut Budaj, J. verfasserin aut Bulgarelli, A. verfasserin aut Burleigh, M. verfasserin aut Cabral, A. verfasserin aut Capria, M. T. verfasserin aut Cassan, A. verfasserin aut Cavarroc, C. verfasserin aut Cecchi-Pestellini, C. verfasserin aut Cerulli, R. verfasserin aut Chadney, J. verfasserin aut Chamberlain, S. verfasserin aut Charnoz, S. verfasserin aut Christian Jessen, N. verfasserin aut Ciaravella, A. verfasserin aut Claret, A. verfasserin aut Claudi, R. verfasserin aut Coates, A. verfasserin aut Cole, R. verfasserin aut Collura, A. verfasserin aut Cordier, D. verfasserin aut Covino, E. verfasserin aut Danielski, C. verfasserin aut Damasso, M. verfasserin aut Deeg, H. J. verfasserin aut Delgado-Mena, E. verfasserin aut Del Vecchio, C. verfasserin aut Demangeon, O. verfasserin aut De Sio, A. verfasserin aut De Wit, J. verfasserin aut Dobrijévic, M. verfasserin aut Doel, P. verfasserin aut Dominic, C. verfasserin aut Dorfi, E. verfasserin aut Eales, S. verfasserin aut Eiroa, C. verfasserin aut Espinoza Contreras, M. verfasserin aut Esposito, M. verfasserin aut Eymet, V. verfasserin aut Fabrizio, N. verfasserin aut Fernández, M. verfasserin aut Femenía Castella, B. verfasserin aut Figueira, P. verfasserin aut Filacchione, G. verfasserin aut Fletcher, L. verfasserin aut Focardi, M. verfasserin aut Fossey, S. verfasserin aut Fouqué, P. verfasserin aut Frith, J. verfasserin aut Galand, M. verfasserin aut Gambicorti, L. verfasserin aut Gaulme, P. verfasserin aut García López, R. J. verfasserin aut Garcia-Piquer, A. verfasserin aut Gear, W. verfasserin aut Gerard, J.-C. verfasserin aut Gesa, L. verfasserin aut Giani, E. verfasserin aut Gianotti, F. verfasserin aut Gillon, M. verfasserin aut Giro, E. verfasserin aut Giuranna, M. verfasserin aut Gomez, H. verfasserin aut Gomez-Leal, I. verfasserin aut Gonzalez Hernandez, J. verfasserin aut González Merino, B. verfasserin aut Graczyk, R. verfasserin aut Grassi, D. verfasserin aut Guardia, J. verfasserin aut Guio, P. verfasserin aut Gustin, J. verfasserin aut Hargrave, P. verfasserin aut Haigh, J. verfasserin aut Hébrard, E. verfasserin aut Heiter, U. verfasserin aut Heredero, R. L. verfasserin aut Herrero, E. verfasserin aut Hersant, F. verfasserin aut Heyrovsky, D. verfasserin aut Hollis, M. verfasserin aut Hubert, B. verfasserin aut Hueso, R. verfasserin aut Israelian, G. verfasserin aut Iro, N. verfasserin aut Irwin, P. verfasserin aut Jacquemoud, S. verfasserin aut Jones, G. verfasserin aut Jones, H. verfasserin aut Justtanont, K. verfasserin aut Kehoe, T. verfasserin aut Kerschbaum, F. verfasserin aut Kerins, E. verfasserin aut Kervella, P. verfasserin aut Kipping, D. verfasserin aut Koskinen, T. verfasserin aut Krupp, N. verfasserin aut Lahav, O. verfasserin aut Laken, B. verfasserin aut Lanza, N. verfasserin aut Lellouch, E. verfasserin aut Leto, G. verfasserin aut Licandro Goldaracena, J. verfasserin aut Lithgow-Bertelloni, C. verfasserin aut Liu, S. J. verfasserin aut Lo Cicero, U. verfasserin aut Lodieu, N. verfasserin aut Lognonné, P. verfasserin aut Lopez-Puertas, M. verfasserin aut Lopez-Valverde, M. A. verfasserin aut Lundgaard Rasmussen, I. verfasserin aut Luntzer, A. verfasserin aut Machado, P. verfasserin aut MacTavish, C. verfasserin aut Maggio, A. verfasserin aut Maillard, J.-P. verfasserin aut Magnes, W. verfasserin aut Maldonado, J. verfasserin aut Mall, U. verfasserin aut Marquette, J.-B. verfasserin aut Mauskopf, P. verfasserin aut Massi, F. verfasserin aut Maurin, A.-S. verfasserin aut Medvedev, A. verfasserin aut Michaut, C. verfasserin aut Miles-Paez, P. verfasserin aut Montalto, M. verfasserin aut Montañés Rodríguez, P. verfasserin aut Monteiro, M. verfasserin aut Montes, D. verfasserin aut Morais, H. verfasserin aut Morales, J. C. verfasserin aut Morales-Calderón, M. verfasserin aut Morello, G. verfasserin aut Moro Martín, A. verfasserin aut Moses, J. verfasserin aut Moya Bedon, A. verfasserin aut Murgas Alcaino, F. verfasserin aut Oliva, E. verfasserin aut Orton, G. verfasserin aut Palla, F. verfasserin aut Pancrazzi, M. verfasserin aut Pantin, E. verfasserin aut Parmentier, V. verfasserin aut Parviainen, H. verfasserin aut Peña Ramírez, K. Y. verfasserin aut Peralta, J. verfasserin aut Perez-Hoyos, S. verfasserin aut Petrov, R. verfasserin aut Pezzuto, S. verfasserin aut Pietrzak, R. verfasserin aut Pilat-Lohinger, E. verfasserin aut Piskunov, N. verfasserin aut Prinja, R. verfasserin aut Prisinzano, L. verfasserin aut Polichtchouk, I. verfasserin aut Poretti, E. verfasserin aut Radioti, A. verfasserin aut Ramos, A. A. verfasserin aut Rank-Lüftinger, T. verfasserin aut Read, P. verfasserin aut Readorn, K. verfasserin aut Rebolo López, R. verfasserin aut Rebordão, J. verfasserin aut Rengel, M. verfasserin aut Rezac, L. verfasserin aut Rocchetto, M. verfasserin aut Rodler, F. verfasserin aut Sánchez Béjar, V. J. verfasserin aut Sanchez Lavega, A. verfasserin aut Sanromá, E. verfasserin aut Santos, N. verfasserin aut Sanz Forcada, J. verfasserin aut Scandariato, G. verfasserin aut Schmider, F.-X. verfasserin aut Scholz, A. verfasserin aut Scuderi, S. verfasserin aut Sethenadh, J. verfasserin aut Shore, S. verfasserin aut Showman, A. verfasserin aut Sicardy, B. verfasserin aut Sitek, P. verfasserin aut Smith, A. verfasserin aut Soret, L. verfasserin aut Sousa, S. verfasserin aut Stiepen, A. verfasserin aut Stolarski, M. verfasserin aut Strazzulla, G. verfasserin aut Tabernero, H. M. verfasserin aut Tanga, P. verfasserin aut Tecsa, M. verfasserin aut Temple, J. verfasserin aut Terenzi, L. verfasserin aut Tessenyi, M. verfasserin aut Testi, L. verfasserin aut Thompson, S. verfasserin aut Thrastarson, H. verfasserin aut Tingley, B. W. verfasserin aut Trifoglio, M. verfasserin aut Martín Torres, J. verfasserin aut Tozzi, A. verfasserin aut Turrini, D. verfasserin aut Varley, R. verfasserin aut Vakili, F. verfasserin aut de Val-Borro, M. verfasserin aut Valdivieso, M. L. verfasserin aut Venot, O. verfasserin aut Villaver, E. verfasserin aut Vinatier, S. verfasserin aut Viti, S. verfasserin aut Waldmann, I. verfasserin aut Waltham, D. verfasserin aut Ward-Thompson, D. verfasserin aut Waters, R. verfasserin aut Watkins, C. verfasserin aut Watson, D. verfasserin aut Wawer, P. verfasserin aut Wawrzaszk, A. verfasserin aut White, G. verfasserin aut Widemann, T. verfasserin aut Winek, W. verfasserin aut Wiśniowski, T. verfasserin aut Yelle, R. verfasserin aut Yung, Y. verfasserin aut Yurchenko, S. N. verfasserin aut Enthalten in Experimental astronomy Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 40(2015), 2-3 vom: 29. Nov., Seite 329-391 (DE-627)312841116 (DE-600)2012330-9 1572-9508 nnns volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391 https://dx.doi.org/10.1007/s10686-015-9484-8 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 40 2015 2-3 29 11 329-391
allfieldsGer	10.1007/s10686-015-9484-8 doi (DE-627)SPR012459186 (SPR)s10686-015-9484-8-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Tinetti, Giovanna verfasserin aut The EChO science case 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213 Drossart, Pierre verfasserin aut Eccleston, Paul verfasserin aut Hartogh, Paul verfasserin aut Isaak, Kate verfasserin aut Linder, Martin verfasserin aut Lovis, Christophe verfasserin aut Micela, Giusi verfasserin aut Ollivier, Marc verfasserin aut Puig, Ludovic verfasserin aut Ribas, Ignasi verfasserin aut Snellen, Ignas verfasserin aut Swinyard, Bruce verfasserin aut Allard, France verfasserin aut Barstow, Joanna verfasserin aut Cho, James verfasserin aut Coustenis, Athena verfasserin aut Cockell, Charles verfasserin aut Correia, Alexandre verfasserin aut Decin, Leen verfasserin aut de Kok, Remco verfasserin aut Deroo, Pieter verfasserin aut Encrenaz, Therese verfasserin aut Forget, Francois verfasserin aut Glasse, Alistair verfasserin aut Griffith, Caitlin verfasserin aut Guillot, Tristan verfasserin aut Koskinen, Tommi verfasserin aut Lammer, Helmut verfasserin aut Leconte, Jeremy verfasserin aut Maxted, Pierre verfasserin aut Mueller-Wodarg, Ingo verfasserin aut Nelson, Richard verfasserin aut North, Chris verfasserin aut Pallé, Enric verfasserin aut Pagano, Isabella verfasserin aut Piccioni, Guseppe verfasserin aut Pinfield, David verfasserin aut Selsis, Franck verfasserin aut Sozzetti, Alessandro verfasserin aut Stixrude, Lars verfasserin aut Tennyson, Jonathan verfasserin aut Turrini, Diego verfasserin aut Zapatero-Osorio, Mariarosa verfasserin aut Beaulieu, Jean-Philippe verfasserin aut Grodent, Denis verfasserin aut Guedel, Manuel verfasserin aut Luz, David verfasserin aut Nørgaard-Nielsen, Hans Ulrik verfasserin aut Ray, Tom verfasserin aut Rickman, Hans verfasserin aut Selig, Avri verfasserin aut Swain, Mark verfasserin aut Banaszkiewicz, Marek verfasserin aut Barlow, Mike verfasserin aut Bowles, Neil verfasserin aut Branduardi-Raymont, Graziella verfasserin aut du Foresto, Vincent Coudé verfasserin aut Gerard, Jean-Claude verfasserin aut Gizon, Laurent verfasserin aut Hornstrup, Allan verfasserin aut Jarchow, Christopher verfasserin aut Kerschbaum, Franz verfasserin aut Kovacs, Géza verfasserin aut Lagage, Pierre-Olivier verfasserin aut Lim, Tanya verfasserin aut Lopez-Morales, Mercedes verfasserin aut Malaguti, Giuseppe verfasserin aut Pace, Emanuele verfasserin aut Pascale, Enzo verfasserin aut Vandenbussche, Bart verfasserin aut Wright, Gillian verfasserin aut Zapata, Gonzalo Ramos verfasserin aut Adriani, Alberto verfasserin aut Azzollini, Ruymán verfasserin aut Balado, Ana verfasserin aut Bryson, Ian verfasserin aut Burston, Raymond verfasserin aut Colomé, Josep verfasserin aut Crook, Martin verfasserin aut Di Giorgio, Anna verfasserin aut Griffin, Matt verfasserin aut Hoogeveen, Ruud verfasserin aut Ottensamer, Roland verfasserin aut Irshad, Ranah verfasserin aut Middleton, Kevin verfasserin aut Morgante, Gianluca verfasserin aut Pinsard, Frederic verfasserin aut Rataj, Mirek verfasserin aut Reess, Jean-Michel verfasserin aut Savini, Giorgio verfasserin aut Schrader, Jan-Rutger verfasserin aut Stamper, Richard verfasserin aut Winter, Berend verfasserin aut Abe, L. verfasserin aut Abreu, M. verfasserin aut Achilleos, N. verfasserin aut Ade, P. verfasserin aut Adybekian, V. verfasserin aut Affer, L. verfasserin aut Agnor, C. verfasserin aut Agundez, M. verfasserin aut Alard, C. verfasserin aut Alcala, J. verfasserin aut Allende Prieto, C. verfasserin aut Alonso Floriano, F. J. verfasserin aut Altieri, F. verfasserin aut Alvarez Iglesias, C. A. verfasserin aut Amado, P. verfasserin aut Andersen, A. verfasserin aut Aylward, A. verfasserin aut Baffa, C. verfasserin aut Bakos, G. verfasserin aut Ballerini, P. verfasserin aut Banaszkiewicz, M. verfasserin aut Barber, R. J. verfasserin aut Barrado, D. verfasserin aut Barton, E. J. verfasserin aut Batista, V. verfasserin aut Bellucci, G. verfasserin aut Belmonte Avilés, J. A. verfasserin aut Berry, D. verfasserin aut Bézard, B. verfasserin aut Biondi, D. verfasserin aut Błęcka, M. verfasserin aut Boisse, I. verfasserin aut Bonfond, B. verfasserin aut Bordé, P. verfasserin aut Börner, P. verfasserin aut Bouy, H. verfasserin aut Brown, L. verfasserin aut Buchhave, L. verfasserin aut Budaj, J. verfasserin aut Bulgarelli, A. verfasserin aut Burleigh, M. verfasserin aut Cabral, A. verfasserin aut Capria, M. T. verfasserin aut Cassan, A. verfasserin aut Cavarroc, C. verfasserin aut Cecchi-Pestellini, C. verfasserin aut Cerulli, R. verfasserin aut Chadney, J. verfasserin aut Chamberlain, S. verfasserin aut Charnoz, S. verfasserin aut Christian Jessen, N. verfasserin aut Ciaravella, A. verfasserin aut Claret, A. verfasserin aut Claudi, R. verfasserin aut Coates, A. verfasserin aut Cole, R. verfasserin aut Collura, A. verfasserin aut Cordier, D. verfasserin aut Covino, E. verfasserin aut Danielski, C. verfasserin aut Damasso, M. verfasserin aut Deeg, H. J. verfasserin aut Delgado-Mena, E. verfasserin aut Del Vecchio, C. verfasserin aut Demangeon, O. verfasserin aut De Sio, A. verfasserin aut De Wit, J. verfasserin aut Dobrijévic, M. verfasserin aut Doel, P. verfasserin aut Dominic, C. verfasserin aut Dorfi, E. verfasserin aut Eales, S. verfasserin aut Eiroa, C. verfasserin aut Espinoza Contreras, M. verfasserin aut Esposito, M. verfasserin aut Eymet, V. verfasserin aut Fabrizio, N. verfasserin aut Fernández, M. verfasserin aut Femenía Castella, B. verfasserin aut Figueira, P. verfasserin aut Filacchione, G. verfasserin aut Fletcher, L. verfasserin aut Focardi, M. verfasserin aut Fossey, S. verfasserin aut Fouqué, P. verfasserin aut Frith, J. verfasserin aut Galand, M. verfasserin aut Gambicorti, L. verfasserin aut Gaulme, P. verfasserin aut García López, R. J. verfasserin aut Garcia-Piquer, A. verfasserin aut Gear, W. verfasserin aut Gerard, J.-C. verfasserin aut Gesa, L. verfasserin aut Giani, E. verfasserin aut Gianotti, F. verfasserin aut Gillon, M. verfasserin aut Giro, E. verfasserin aut Giuranna, M. verfasserin aut Gomez, H. verfasserin aut Gomez-Leal, I. verfasserin aut Gonzalez Hernandez, J. verfasserin aut González Merino, B. verfasserin aut Graczyk, R. verfasserin aut Grassi, D. verfasserin aut Guardia, J. verfasserin aut Guio, P. verfasserin aut Gustin, J. verfasserin aut Hargrave, P. verfasserin aut Haigh, J. verfasserin aut Hébrard, E. verfasserin aut Heiter, U. verfasserin aut Heredero, R. L. verfasserin aut Herrero, E. verfasserin aut Hersant, F. verfasserin aut Heyrovsky, D. verfasserin aut Hollis, M. verfasserin aut Hubert, B. verfasserin aut Hueso, R. verfasserin aut Israelian, G. verfasserin aut Iro, N. verfasserin aut Irwin, P. verfasserin aut Jacquemoud, S. verfasserin aut Jones, G. verfasserin aut Jones, H. verfasserin aut Justtanont, K. verfasserin aut Kehoe, T. verfasserin aut Kerschbaum, F. verfasserin aut Kerins, E. verfasserin aut Kervella, P. verfasserin aut Kipping, D. verfasserin aut Koskinen, T. verfasserin aut Krupp, N. verfasserin aut Lahav, O. verfasserin aut Laken, B. verfasserin aut Lanza, N. verfasserin aut Lellouch, E. verfasserin aut Leto, G. verfasserin aut Licandro Goldaracena, J. verfasserin aut Lithgow-Bertelloni, C. verfasserin aut Liu, S. J. verfasserin aut Lo Cicero, U. verfasserin aut Lodieu, N. verfasserin aut Lognonné, P. verfasserin aut Lopez-Puertas, M. verfasserin aut Lopez-Valverde, M. A. verfasserin aut Lundgaard Rasmussen, I. verfasserin aut Luntzer, A. verfasserin aut Machado, P. verfasserin aut MacTavish, C. verfasserin aut Maggio, A. verfasserin aut Maillard, J.-P. verfasserin aut Magnes, W. verfasserin aut Maldonado, J. verfasserin aut Mall, U. verfasserin aut Marquette, J.-B. verfasserin aut Mauskopf, P. verfasserin aut Massi, F. verfasserin aut Maurin, A.-S. verfasserin aut Medvedev, A. verfasserin aut Michaut, C. verfasserin aut Miles-Paez, P. verfasserin aut Montalto, M. verfasserin aut Montañés Rodríguez, P. verfasserin aut Monteiro, M. verfasserin aut Montes, D. verfasserin aut Morais, H. verfasserin aut Morales, J. C. verfasserin aut Morales-Calderón, M. verfasserin aut Morello, G. verfasserin aut Moro Martín, A. verfasserin aut Moses, J. verfasserin aut Moya Bedon, A. verfasserin aut Murgas Alcaino, F. verfasserin aut Oliva, E. verfasserin aut Orton, G. verfasserin aut Palla, F. verfasserin aut Pancrazzi, M. verfasserin aut Pantin, E. verfasserin aut Parmentier, V. verfasserin aut Parviainen, H. verfasserin aut Peña Ramírez, K. Y. verfasserin aut Peralta, J. verfasserin aut Perez-Hoyos, S. verfasserin aut Petrov, R. verfasserin aut Pezzuto, S. verfasserin aut Pietrzak, R. verfasserin aut Pilat-Lohinger, E. verfasserin aut Piskunov, N. verfasserin aut Prinja, R. verfasserin aut Prisinzano, L. verfasserin aut Polichtchouk, I. verfasserin aut Poretti, E. verfasserin aut Radioti, A. verfasserin aut Ramos, A. A. verfasserin aut Rank-Lüftinger, T. verfasserin aut Read, P. verfasserin aut Readorn, K. verfasserin aut Rebolo López, R. verfasserin aut Rebordão, J. verfasserin aut Rengel, M. verfasserin aut Rezac, L. verfasserin aut Rocchetto, M. verfasserin aut Rodler, F. verfasserin aut Sánchez Béjar, V. J. verfasserin aut Sanchez Lavega, A. verfasserin aut Sanromá, E. verfasserin aut Santos, N. verfasserin aut Sanz Forcada, J. verfasserin aut Scandariato, G. verfasserin aut Schmider, F.-X. verfasserin aut Scholz, A. verfasserin aut Scuderi, S. verfasserin aut Sethenadh, J. verfasserin aut Shore, S. verfasserin aut Showman, A. verfasserin aut Sicardy, B. verfasserin aut Sitek, P. verfasserin aut Smith, A. verfasserin aut Soret, L. verfasserin aut Sousa, S. verfasserin aut Stiepen, A. verfasserin aut Stolarski, M. verfasserin aut Strazzulla, G. verfasserin aut Tabernero, H. M. verfasserin aut Tanga, P. verfasserin aut Tecsa, M. verfasserin aut Temple, J. verfasserin aut Terenzi, L. verfasserin aut Tessenyi, M. verfasserin aut Testi, L. verfasserin aut Thompson, S. verfasserin aut Thrastarson, H. verfasserin aut Tingley, B. W. verfasserin aut Trifoglio, M. verfasserin aut Martín Torres, J. verfasserin aut Tozzi, A. verfasserin aut Turrini, D. verfasserin aut Varley, R. verfasserin aut Vakili, F. verfasserin aut de Val-Borro, M. verfasserin aut Valdivieso, M. L. verfasserin aut Venot, O. verfasserin aut Villaver, E. verfasserin aut Vinatier, S. verfasserin aut Viti, S. verfasserin aut Waldmann, I. verfasserin aut Waltham, D. verfasserin aut Ward-Thompson, D. verfasserin aut Waters, R. verfasserin aut Watkins, C. verfasserin aut Watson, D. verfasserin aut Wawer, P. verfasserin aut Wawrzaszk, A. verfasserin aut White, G. verfasserin aut Widemann, T. verfasserin aut Winek, W. verfasserin aut Wiśniowski, T. verfasserin aut Yelle, R. verfasserin aut Yung, Y. verfasserin aut Yurchenko, S. N. verfasserin aut Enthalten in Experimental astronomy Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 40(2015), 2-3 vom: 29. Nov., Seite 329-391 (DE-627)312841116 (DE-600)2012330-9 1572-9508 nnns volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391 https://dx.doi.org/10.1007/s10686-015-9484-8 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 40 2015 2-3 29 11 329-391
allfieldsSound	10.1007/s10686-015-9484-8 doi (DE-627)SPR012459186 (SPR)s10686-015-9484-8-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Tinetti, Giovanna verfasserin aut The EChO science case 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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. Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213 Drossart, Pierre verfasserin aut Eccleston, Paul verfasserin aut Hartogh, Paul verfasserin aut Isaak, Kate verfasserin aut Linder, Martin verfasserin aut Lovis, Christophe verfasserin aut Micela, Giusi verfasserin aut Ollivier, Marc verfasserin aut Puig, Ludovic verfasserin aut Ribas, Ignasi verfasserin aut Snellen, Ignas verfasserin aut Swinyard, Bruce verfasserin aut Allard, France verfasserin aut Barstow, Joanna verfasserin aut Cho, James verfasserin aut Coustenis, Athena verfasserin aut Cockell, Charles verfasserin aut Correia, Alexandre verfasserin aut Decin, Leen verfasserin aut de Kok, Remco verfasserin aut Deroo, Pieter verfasserin aut Encrenaz, Therese verfasserin aut Forget, Francois verfasserin aut Glasse, Alistair verfasserin aut Griffith, Caitlin verfasserin aut Guillot, Tristan verfasserin aut Koskinen, Tommi verfasserin aut Lammer, Helmut verfasserin aut Leconte, Jeremy verfasserin aut Maxted, Pierre verfasserin aut Mueller-Wodarg, Ingo verfasserin aut Nelson, Richard verfasserin aut North, Chris verfasserin aut Pallé, Enric verfasserin aut Pagano, Isabella verfasserin aut Piccioni, Guseppe verfasserin aut Pinfield, David verfasserin aut Selsis, Franck verfasserin aut Sozzetti, Alessandro verfasserin aut Stixrude, Lars verfasserin aut Tennyson, Jonathan verfasserin aut Turrini, Diego verfasserin aut Zapatero-Osorio, Mariarosa verfasserin aut Beaulieu, Jean-Philippe verfasserin aut Grodent, Denis verfasserin aut Guedel, Manuel verfasserin aut Luz, David verfasserin aut Nørgaard-Nielsen, Hans Ulrik verfasserin aut Ray, Tom verfasserin aut Rickman, Hans verfasserin aut Selig, Avri verfasserin aut Swain, Mark verfasserin aut Banaszkiewicz, Marek verfasserin aut Barlow, Mike verfasserin aut Bowles, Neil verfasserin aut Branduardi-Raymont, Graziella verfasserin aut du Foresto, Vincent Coudé verfasserin aut Gerard, Jean-Claude verfasserin aut Gizon, Laurent verfasserin aut Hornstrup, Allan verfasserin aut Jarchow, Christopher verfasserin aut Kerschbaum, Franz verfasserin aut Kovacs, Géza verfasserin aut Lagage, Pierre-Olivier verfasserin aut Lim, Tanya verfasserin aut Lopez-Morales, Mercedes verfasserin aut Malaguti, Giuseppe verfasserin aut Pace, Emanuele verfasserin aut Pascale, Enzo verfasserin aut Vandenbussche, Bart verfasserin aut Wright, Gillian verfasserin aut Zapata, Gonzalo Ramos verfasserin aut Adriani, Alberto verfasserin aut Azzollini, Ruymán verfasserin aut Balado, Ana verfasserin aut Bryson, Ian verfasserin aut Burston, Raymond verfasserin aut Colomé, Josep verfasserin aut Crook, Martin verfasserin aut Di Giorgio, Anna verfasserin aut Griffin, Matt verfasserin aut Hoogeveen, Ruud verfasserin aut Ottensamer, Roland verfasserin aut Irshad, Ranah verfasserin aut Middleton, Kevin verfasserin aut Morgante, Gianluca verfasserin aut Pinsard, Frederic verfasserin aut Rataj, Mirek verfasserin aut Reess, Jean-Michel verfasserin aut Savini, Giorgio verfasserin aut Schrader, Jan-Rutger verfasserin aut Stamper, Richard verfasserin aut Winter, Berend verfasserin aut Abe, L. verfasserin aut Abreu, M. verfasserin aut Achilleos, N. verfasserin aut Ade, P. verfasserin aut Adybekian, V. verfasserin aut Affer, L. verfasserin aut Agnor, C. verfasserin aut Agundez, M. verfasserin aut Alard, C. verfasserin aut Alcala, J. verfasserin aut Allende Prieto, C. verfasserin aut Alonso Floriano, F. J. verfasserin aut Altieri, F. verfasserin aut Alvarez Iglesias, C. A. verfasserin aut Amado, P. verfasserin aut Andersen, A. verfasserin aut Aylward, A. verfasserin aut Baffa, C. verfasserin aut Bakos, G. verfasserin aut Ballerini, P. verfasserin aut Banaszkiewicz, M. verfasserin aut Barber, R. J. verfasserin aut Barrado, D. verfasserin aut Barton, E. J. verfasserin aut Batista, V. verfasserin aut Bellucci, G. verfasserin aut Belmonte Avilés, J. A. verfasserin aut Berry, D. verfasserin aut Bézard, B. verfasserin aut Biondi, D. verfasserin aut Błęcka, M. verfasserin aut Boisse, I. verfasserin aut Bonfond, B. verfasserin aut Bordé, P. verfasserin aut Börner, P. verfasserin aut Bouy, H. verfasserin aut Brown, L. verfasserin aut Buchhave, L. verfasserin aut Budaj, J. verfasserin aut Bulgarelli, A. verfasserin aut Burleigh, M. verfasserin aut Cabral, A. verfasserin aut Capria, M. T. verfasserin aut Cassan, A. verfasserin aut Cavarroc, C. verfasserin aut Cecchi-Pestellini, C. verfasserin aut Cerulli, R. verfasserin aut Chadney, J. verfasserin aut Chamberlain, S. verfasserin aut Charnoz, S. verfasserin aut Christian Jessen, N. verfasserin aut Ciaravella, A. verfasserin aut Claret, A. verfasserin aut Claudi, R. verfasserin aut Coates, A. verfasserin aut Cole, R. verfasserin aut Collura, A. verfasserin aut Cordier, D. verfasserin aut Covino, E. verfasserin aut Danielski, C. verfasserin aut Damasso, M. verfasserin aut Deeg, H. J. verfasserin aut Delgado-Mena, E. verfasserin aut Del Vecchio, C. verfasserin aut Demangeon, O. verfasserin aut De Sio, A. verfasserin aut De Wit, J. verfasserin aut Dobrijévic, M. verfasserin aut Doel, P. verfasserin aut Dominic, C. verfasserin aut Dorfi, E. verfasserin aut Eales, S. verfasserin aut Eiroa, C. verfasserin aut Espinoza Contreras, M. verfasserin aut Esposito, M. verfasserin aut Eymet, V. verfasserin aut Fabrizio, N. verfasserin aut Fernández, M. verfasserin aut Femenía Castella, B. verfasserin aut Figueira, P. verfasserin aut Filacchione, G. verfasserin aut Fletcher, L. verfasserin aut Focardi, M. verfasserin aut Fossey, S. verfasserin aut Fouqué, P. verfasserin aut Frith, J. verfasserin aut Galand, M. verfasserin aut Gambicorti, L. verfasserin aut Gaulme, P. verfasserin aut García López, R. J. verfasserin aut Garcia-Piquer, A. verfasserin aut Gear, W. verfasserin aut Gerard, J.-C. verfasserin aut Gesa, L. verfasserin aut Giani, E. verfasserin aut Gianotti, F. verfasserin aut Gillon, M. verfasserin aut Giro, E. verfasserin aut Giuranna, M. verfasserin aut Gomez, H. verfasserin aut Gomez-Leal, I. verfasserin aut Gonzalez Hernandez, J. verfasserin aut González Merino, B. verfasserin aut Graczyk, R. verfasserin aut Grassi, D. verfasserin aut Guardia, J. verfasserin aut Guio, P. verfasserin aut Gustin, J. verfasserin aut Hargrave, P. verfasserin aut Haigh, J. verfasserin aut Hébrard, E. verfasserin aut Heiter, U. verfasserin aut Heredero, R. L. verfasserin aut Herrero, E. verfasserin aut Hersant, F. verfasserin aut Heyrovsky, D. verfasserin aut Hollis, M. verfasserin aut Hubert, B. verfasserin aut Hueso, R. verfasserin aut Israelian, G. verfasserin aut Iro, N. verfasserin aut Irwin, P. verfasserin aut Jacquemoud, S. verfasserin aut Jones, G. verfasserin aut Jones, H. verfasserin aut Justtanont, K. verfasserin aut Kehoe, T. verfasserin aut Kerschbaum, F. verfasserin aut Kerins, E. verfasserin aut Kervella, P. verfasserin aut Kipping, D. verfasserin aut Koskinen, T. verfasserin aut Krupp, N. verfasserin aut Lahav, O. verfasserin aut Laken, B. verfasserin aut Lanza, N. verfasserin aut Lellouch, E. verfasserin aut Leto, G. verfasserin aut Licandro Goldaracena, J. verfasserin aut Lithgow-Bertelloni, C. verfasserin aut Liu, S. J. verfasserin aut Lo Cicero, U. verfasserin aut Lodieu, N. verfasserin aut Lognonné, P. verfasserin aut Lopez-Puertas, M. verfasserin aut Lopez-Valverde, M. A. verfasserin aut Lundgaard Rasmussen, I. verfasserin aut Luntzer, A. verfasserin aut Machado, P. verfasserin aut MacTavish, C. verfasserin aut Maggio, A. verfasserin aut Maillard, J.-P. verfasserin aut Magnes, W. verfasserin aut Maldonado, J. verfasserin aut Mall, U. verfasserin aut Marquette, J.-B. verfasserin aut Mauskopf, P. verfasserin aut Massi, F. verfasserin aut Maurin, A.-S. verfasserin aut Medvedev, A. verfasserin aut Michaut, C. verfasserin aut Miles-Paez, P. verfasserin aut Montalto, M. verfasserin aut Montañés Rodríguez, P. verfasserin aut Monteiro, M. verfasserin aut Montes, D. verfasserin aut Morais, H. verfasserin aut Morales, J. C. verfasserin aut Morales-Calderón, M. verfasserin aut Morello, G. verfasserin aut Moro Martín, A. verfasserin aut Moses, J. verfasserin aut Moya Bedon, A. verfasserin aut Murgas Alcaino, F. verfasserin aut Oliva, E. verfasserin aut Orton, G. verfasserin aut Palla, F. verfasserin aut Pancrazzi, M. verfasserin aut Pantin, E. verfasserin aut Parmentier, V. verfasserin aut Parviainen, H. verfasserin aut Peña Ramírez, K. Y. verfasserin aut Peralta, J. verfasserin aut Perez-Hoyos, S. verfasserin aut Petrov, R. verfasserin aut Pezzuto, S. verfasserin aut Pietrzak, R. verfasserin aut Pilat-Lohinger, E. verfasserin aut Piskunov, N. verfasserin aut Prinja, R. verfasserin aut Prisinzano, L. verfasserin aut Polichtchouk, I. verfasserin aut Poretti, E. verfasserin aut Radioti, A. verfasserin aut Ramos, A. A. verfasserin aut Rank-Lüftinger, T. verfasserin aut Read, P. verfasserin aut Readorn, K. verfasserin aut Rebolo López, R. verfasserin aut Rebordão, J. verfasserin aut Rengel, M. verfasserin aut Rezac, L. verfasserin aut Rocchetto, M. verfasserin aut Rodler, F. verfasserin aut Sánchez Béjar, V. J. verfasserin aut Sanchez Lavega, A. verfasserin aut Sanromá, E. verfasserin aut Santos, N. verfasserin aut Sanz Forcada, J. verfasserin aut Scandariato, G. verfasserin aut Schmider, F.-X. verfasserin aut Scholz, A. verfasserin aut Scuderi, S. verfasserin aut Sethenadh, J. verfasserin aut Shore, S. verfasserin aut Showman, A. verfasserin aut Sicardy, B. verfasserin aut Sitek, P. verfasserin aut Smith, A. verfasserin aut Soret, L. verfasserin aut Sousa, S. verfasserin aut Stiepen, A. verfasserin aut Stolarski, M. verfasserin aut Strazzulla, G. verfasserin aut Tabernero, H. M. verfasserin aut Tanga, P. verfasserin aut Tecsa, M. verfasserin aut Temple, J. verfasserin aut Terenzi, L. verfasserin aut Tessenyi, M. verfasserin aut Testi, L. verfasserin aut Thompson, S. verfasserin aut Thrastarson, H. verfasserin aut Tingley, B. W. verfasserin aut Trifoglio, M. verfasserin aut Martín Torres, J. verfasserin aut Tozzi, A. verfasserin aut Turrini, D. verfasserin aut Varley, R. verfasserin aut Vakili, F. verfasserin aut de Val-Borro, M. verfasserin aut Valdivieso, M. L. verfasserin aut Venot, O. verfasserin aut Villaver, E. verfasserin aut Vinatier, S. verfasserin aut Viti, S. verfasserin aut Waldmann, I. verfasserin aut Waltham, D. verfasserin aut Ward-Thompson, D. verfasserin aut Waters, R. verfasserin aut Watkins, C. verfasserin aut Watson, D. verfasserin aut Wawer, P. verfasserin aut Wawrzaszk, A. verfasserin aut White, G. verfasserin aut Widemann, T. verfasserin aut Winek, W. verfasserin aut Wiśniowski, T. verfasserin aut Yelle, R. verfasserin aut Yung, Y. verfasserin aut Yurchenko, S. N. verfasserin aut Enthalten in Experimental astronomy Dordrecht [u.a.] : Springer Science + Business Media B.V., 1989 40(2015), 2-3 vom: 29. Nov., Seite 329-391 (DE-627)312841116 (DE-600)2012330-9 1572-9508 nnns volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391 https://dx.doi.org/10.1007/s10686-015-9484-8 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 40 2015 2-3 29 11 329-391
language	English
source	Enthalten in Experimental astronomy 40(2015), 2-3 vom: 29. Nov., Seite 329-391 volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391
sourceStr	Enthalten in Experimental astronomy 40(2015), 2-3 vom: 29. Nov., Seite 329-391 volume:40 year:2015 number:2-3 day:29 month:11 pages:329-391
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions
dewey-raw	520
isfreeaccess_bool	true
container_title	Experimental astronomy
authorswithroles_txt_mv	Tinetti, Giovanna @@aut@@ Drossart, Pierre @@aut@@ Eccleston, Paul @@aut@@ Hartogh, Paul @@aut@@ Isaak, Kate @@aut@@ Linder, Martin @@aut@@ Lovis, Christophe @@aut@@ Micela, Giusi @@aut@@ Ollivier, Marc @@aut@@ Puig, Ludovic @@aut@@ Ribas, Ignasi @@aut@@ Snellen, Ignas @@aut@@ Swinyard, Bruce @@aut@@ Allard, France @@aut@@ Barstow, Joanna @@aut@@ Cho, James @@aut@@ Coustenis, Athena @@aut@@ Cockell, Charles @@aut@@ Correia, Alexandre @@aut@@ Decin, Leen @@aut@@ de Kok, Remco @@aut@@ Deroo, Pieter @@aut@@ Encrenaz, Therese @@aut@@ Forget, Francois @@aut@@ Glasse, Alistair @@aut@@ Griffith, Caitlin @@aut@@ Guillot, Tristan @@aut@@ Koskinen, Tommi @@aut@@ Lammer, Helmut @@aut@@ Leconte, Jeremy @@aut@@ Maxted, Pierre @@aut@@ Mueller-Wodarg, Ingo @@aut@@ Nelson, Richard @@aut@@ North, Chris @@aut@@ Pallé, Enric @@aut@@ Pagano, Isabella @@aut@@ Piccioni, Guseppe @@aut@@ Pinfield, David @@aut@@ Selsis, Franck @@aut@@ Sozzetti, Alessandro @@aut@@ Stixrude, Lars @@aut@@ Tennyson, Jonathan @@aut@@ Turrini, Diego @@aut@@ Zapatero-Osorio, Mariarosa @@aut@@ Beaulieu, Jean-Philippe @@aut@@ Grodent, Denis @@aut@@ Guedel, Manuel @@aut@@ Luz, David @@aut@@ Nørgaard-Nielsen, Hans Ulrik @@aut@@ Ray, Tom @@aut@@ Rickman, Hans @@aut@@ Selig, Avri @@aut@@ Swain, Mark @@aut@@ Banaszkiewicz, Marek @@aut@@ Barlow, Mike @@aut@@ Bowles, Neil @@aut@@ Branduardi-Raymont, Graziella @@aut@@ du Foresto, Vincent Coudé @@aut@@ Gerard, Jean-Claude @@aut@@ Gizon, Laurent @@aut@@ Hornstrup, Allan @@aut@@ Jarchow, Christopher @@aut@@ Kerschbaum, Franz @@aut@@ Kovacs, Géza @@aut@@ Lagage, Pierre-Olivier @@aut@@ Lim, Tanya @@aut@@ Lopez-Morales, Mercedes @@aut@@ Malaguti, Giuseppe @@aut@@ Pace, Emanuele @@aut@@ Pascale, Enzo @@aut@@ Vandenbussche, Bart @@aut@@ Wright, Gillian @@aut@@ Zapata, Gonzalo Ramos @@aut@@ Adriani, Alberto @@aut@@ Azzollini, Ruymán @@aut@@ Balado, Ana @@aut@@ Bryson, Ian @@aut@@ Burston, Raymond @@aut@@ Colomé, Josep @@aut@@ Crook, Martin @@aut@@ Di Giorgio, Anna @@aut@@ Griffin, Matt @@aut@@ Hoogeveen, Ruud @@aut@@ Ottensamer, Roland @@aut@@ Irshad, Ranah @@aut@@ Middleton, Kevin @@aut@@ Morgante, Gianluca @@aut@@ Pinsard, Frederic @@aut@@ Rataj, Mirek @@aut@@ Reess, Jean-Michel @@aut@@ Savini, Giorgio @@aut@@ Schrader, Jan-Rutger @@aut@@ Stamper, Richard @@aut@@ Winter, Berend @@aut@@ Abe, L. @@aut@@ Abreu, M. @@aut@@ Achilleos, N. @@aut@@ Ade, P. @@aut@@ Adybekian, V. @@aut@@ Affer, L. @@aut@@ Agnor, C. @@aut@@ Agundez, M. @@aut@@ Alard, C. @@aut@@ Alcala, J. @@aut@@ Allende Prieto, C. @@aut@@ Alonso Floriano, F. J. @@aut@@ Altieri, F. @@aut@@ Alvarez Iglesias, C. A. @@aut@@ Amado, P. @@aut@@ Andersen, A. @@aut@@ Aylward, A. @@aut@@ Baffa, C. @@aut@@ Bakos, G. @@aut@@ Ballerini, P. @@aut@@ Banaszkiewicz, M. @@aut@@ Barber, R. J. @@aut@@ Barrado, D. @@aut@@ Barton, E. J. @@aut@@ Batista, V. @@aut@@ Bellucci, G. @@aut@@ Belmonte Avilés, J. A. @@aut@@ Berry, D. @@aut@@ Bézard, B. @@aut@@ Biondi, D. @@aut@@ Błęcka, M. @@aut@@ Boisse, I. @@aut@@ Bonfond, B. @@aut@@ Bordé, P. @@aut@@ Börner, P. @@aut@@ Bouy, H. @@aut@@ Brown, L. @@aut@@ Buchhave, L. @@aut@@ Budaj, J. @@aut@@ Bulgarelli, A. @@aut@@ Burleigh, M. @@aut@@ Cabral, A. @@aut@@ Capria, M. T. @@aut@@ Cassan, A. @@aut@@ Cavarroc, C. @@aut@@ Cecchi-Pestellini, C. @@aut@@ Cerulli, R. @@aut@@ Chadney, J. @@aut@@ Chamberlain, S. @@aut@@ Charnoz, S. @@aut@@ Christian Jessen, N. @@aut@@ Ciaravella, A. @@aut@@ Claret, A. @@aut@@ Claudi, R. @@aut@@ Coates, A. @@aut@@ Cole, R. @@aut@@ Collura, A. @@aut@@ Cordier, D. @@aut@@ Covino, E. @@aut@@ Danielski, C. @@aut@@ Damasso, M. @@aut@@ Deeg, H. J. @@aut@@ Delgado-Mena, E. @@aut@@ Del Vecchio, C. @@aut@@ Demangeon, O. @@aut@@ De Sio, A. @@aut@@ De Wit, J. @@aut@@ Dobrijévic, M. @@aut@@ Doel, P. @@aut@@ Dominic, C. @@aut@@ Dorfi, E. @@aut@@ Eales, S. @@aut@@ Eiroa, C. @@aut@@ Espinoza Contreras, M. @@aut@@ Esposito, M. @@aut@@ Eymet, V. @@aut@@ Fabrizio, N. @@aut@@ Fernández, M. @@aut@@ Femenía Castella, B. @@aut@@ Figueira, P. @@aut@@ Filacchione, G. @@aut@@ Fletcher, L. @@aut@@ Focardi, M. @@aut@@ Fossey, S. @@aut@@ Fouqué, P. @@aut@@ Frith, J. @@aut@@ Galand, M. @@aut@@ Gambicorti, L. @@aut@@ Gaulme, P. @@aut@@ García López, R. J. @@aut@@ Garcia-Piquer, A. @@aut@@ Gear, W. @@aut@@ Gerard, J.-C. @@aut@@ Gesa, L. @@aut@@ Giani, E. @@aut@@ Gianotti, F. @@aut@@ Gillon, M. @@aut@@ Giro, E. @@aut@@ Giuranna, M. @@aut@@ Gomez, H. @@aut@@ Gomez-Leal, I. @@aut@@ Gonzalez Hernandez, J. @@aut@@ González Merino, B. @@aut@@ Graczyk, R. @@aut@@ Grassi, D. @@aut@@ Guardia, J. @@aut@@ Guio, P. @@aut@@ Gustin, J. @@aut@@ Hargrave, P. @@aut@@ Haigh, J. @@aut@@ Hébrard, E. @@aut@@ Heiter, U. @@aut@@ Heredero, R. L. @@aut@@ Herrero, E. @@aut@@ Hersant, F. @@aut@@ Heyrovsky, D. @@aut@@ Hollis, M. @@aut@@ Hubert, B. @@aut@@ Hueso, R. @@aut@@ Israelian, G. @@aut@@ Iro, N. @@aut@@ Irwin, P. @@aut@@ Jacquemoud, S. @@aut@@ Jones, G. @@aut@@ Jones, H. @@aut@@ Justtanont, K. @@aut@@ Kehoe, T. @@aut@@ Kerschbaum, F. @@aut@@ Kerins, E. @@aut@@ Kervella, P. @@aut@@ Kipping, D. @@aut@@ Koskinen, T. @@aut@@ Krupp, N. @@aut@@ Lahav, O. @@aut@@ Laken, B. @@aut@@ Lanza, N. @@aut@@ Lellouch, E. @@aut@@ Leto, G. @@aut@@ Licandro Goldaracena, J. @@aut@@ Lithgow-Bertelloni, C. @@aut@@ Liu, S. J. @@aut@@ Lo Cicero, U. @@aut@@ Lodieu, N. @@aut@@ Lognonné, P. @@aut@@ Lopez-Puertas, M. @@aut@@ Lopez-Valverde, M. A. @@aut@@ Lundgaard Rasmussen, I. @@aut@@ Luntzer, A. @@aut@@ Machado, P. @@aut@@ MacTavish, C. @@aut@@ Maggio, A. @@aut@@ Maillard, J.-P. @@aut@@ Magnes, W. @@aut@@ Maldonado, J. @@aut@@ Mall, U. @@aut@@ Marquette, J.-B. @@aut@@ Mauskopf, P. @@aut@@ Massi, F. @@aut@@ Maurin, A.-S. @@aut@@ Medvedev, A. @@aut@@ Michaut, C. @@aut@@ Miles-Paez, P. @@aut@@ Montalto, M. @@aut@@ Montañés Rodríguez, P. @@aut@@ Monteiro, M. @@aut@@ Montes, D. @@aut@@ Morais, H. @@aut@@ Morales, J. C. @@aut@@ Morales-Calderón, M. @@aut@@ Morello, G. @@aut@@ Moro Martín, A. @@aut@@ Moses, J. @@aut@@ Moya Bedon, A. @@aut@@ Murgas Alcaino, F. @@aut@@ Oliva, E. @@aut@@ Orton, G. @@aut@@ Palla, F. @@aut@@ Pancrazzi, M. @@aut@@ Pantin, E. @@aut@@ Parmentier, V. @@aut@@ Parviainen, H. @@aut@@ Peña Ramírez, K. Y. @@aut@@ Peralta, J. @@aut@@ Perez-Hoyos, S. @@aut@@ Petrov, R. @@aut@@ Pezzuto, S. @@aut@@ Pietrzak, R. @@aut@@ Pilat-Lohinger, E. @@aut@@ Piskunov, N. @@aut@@ Prinja, R. @@aut@@ Prisinzano, L. @@aut@@ Polichtchouk, I. @@aut@@ Poretti, E. @@aut@@ Radioti, A. @@aut@@ Ramos, A. A. @@aut@@ Rank-Lüftinger, T. @@aut@@ Read, P. @@aut@@ Readorn, K. @@aut@@ Rebolo López, R. @@aut@@ Rebordão, J. @@aut@@ Rengel, M. @@aut@@ Rezac, L. @@aut@@ Rocchetto, M. @@aut@@ Rodler, F. @@aut@@ Sánchez Béjar, V. J. @@aut@@ Sanchez Lavega, A. @@aut@@ Sanromá, E. @@aut@@ Santos, N. @@aut@@ Sanz Forcada, J. @@aut@@ Scandariato, G. @@aut@@ Schmider, F.-X. @@aut@@ Scholz, A. @@aut@@ Scuderi, S. @@aut@@ Sethenadh, J. @@aut@@ Shore, S. @@aut@@ Showman, A. @@aut@@ Sicardy, B. @@aut@@ Sitek, P. @@aut@@ Smith, A. @@aut@@ Soret, L. @@aut@@ Sousa, S. @@aut@@ Stiepen, A. @@aut@@ Stolarski, M. @@aut@@ Strazzulla, G. @@aut@@ Tabernero, H. M. @@aut@@ Tanga, P. @@aut@@ Tecsa, M. @@aut@@ Temple, J. @@aut@@ Terenzi, L. @@aut@@ Tessenyi, M. @@aut@@ Testi, L. @@aut@@ Thompson, S. @@aut@@ Thrastarson, H. @@aut@@ Tingley, B. W. @@aut@@ Trifoglio, M. @@aut@@ Martín Torres, J. @@aut@@ Tozzi, A. @@aut@@ Turrini, D. @@aut@@ Varley, R. @@aut@@ Vakili, F. @@aut@@ de Val-Borro, M. @@aut@@ Valdivieso, M. L. @@aut@@ Venot, O. @@aut@@ Villaver, E. @@aut@@ Vinatier, S. @@aut@@ Viti, S. @@aut@@ Waldmann, I. @@aut@@ Waltham, D. @@aut@@ Ward-Thompson, D. @@aut@@ Waters, R. @@aut@@ Watkins, C. @@aut@@ Watson, D. @@aut@@ Wawer, P. @@aut@@ Wawrzaszk, A. @@aut@@ White, G. @@aut@@ Widemann, T. @@aut@@ Winek, W. @@aut@@ Wiśniowski, T. @@aut@@ Yelle, R. @@aut@@ Yung, Y. @@aut@@ Yurchenko, S. N. @@aut@@
publishDateDaySort_date	2015-11-29T00:00:00Z
hierarchy_top_id	312841116
dewey-sort	3520
id	SPR012459186
language_de	englisch
fullrecord	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR012459186</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220110234001.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201005s2015 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s10686-015-9484-8</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR012459186</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)s10686-015-9484-8-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">520</subfield><subfield code="q">ASE</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.00</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Tinetti, Giovanna</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The EChO science case</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Exoplanets</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Spectroscopy</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Atmospheric science</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">IR astronomy</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Space missions</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Drossart, 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J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Garcia-Piquer, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gear, W.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gerard, J.-C.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gesa, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giani, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gianotti, F.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gillon, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giro, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giuranna, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gomez, H.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gomez-Leal, I.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gonzalez Hernandez, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">González Merino, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Graczyk, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Grassi, D.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Guardia, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Guio, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gustin, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hargrave, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Haigh, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hébrard, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Heiter, U.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Heredero, R. 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author	Tinetti, Giovanna
spellingShingle	Tinetti, Giovanna ddc 520 bkl 39.00 misc Exoplanets misc Spectroscopy misc Atmospheric science misc IR astronomy misc Space missions The EChO science case
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topic_title	520 ASE 39.00 bkl The EChO science case Exoplanets (dpeaa)DE-He213 Spectroscopy (dpeaa)DE-He213 Atmospheric science (dpeaa)DE-He213 IR astronomy (dpeaa)DE-He213 Space missions (dpeaa)DE-He213
topic	ddc 520 bkl 39.00 misc Exoplanets misc Spectroscopy misc Atmospheric science misc IR astronomy misc Space missions
topic_unstemmed	ddc 520 bkl 39.00 misc Exoplanets misc Spectroscopy misc Atmospheric science misc IR astronomy misc Space missions
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title	The EChO science case
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title_full	The EChO science case
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author_browse	Tinetti, Giovanna Drossart, Pierre Eccleston, Paul Hartogh, Paul Isaak, Kate Linder, Martin Lovis, Christophe Micela, Giusi Ollivier, Marc Puig, Ludovic Ribas, Ignasi Snellen, Ignas Swinyard, Bruce Allard, France Barstow, Joanna Cho, James Coustenis, Athena Cockell, Charles Correia, Alexandre Decin, Leen de Kok, Remco Deroo, Pieter Encrenaz, Therese Forget, Francois Glasse, Alistair Griffith, Caitlin Guillot, Tristan Koskinen, Tommi Lammer, Helmut Leconte, Jeremy Maxted, Pierre Mueller-Wodarg, Ingo Nelson, Richard North, Chris Pallé, Enric Pagano, Isabella Piccioni, Guseppe Pinfield, David Selsis, Franck Sozzetti, Alessandro Stixrude, Lars Tennyson, Jonathan Turrini, Diego Zapatero-Osorio, Mariarosa Beaulieu, Jean-Philippe Grodent, Denis Guedel, Manuel Luz, David Nørgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coudé Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Géza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Zapata, Gonzalo Ramos Adriani, Alberto Azzollini, Ruymán Balado, Ana Bryson, Ian Burston, Raymond Colomé, Josep Crook, Martin Di Giorgio, Anna Griffin, Matt Hoogeveen, Ruud Ottensamer, Roland Irshad, Ranah Middleton, Kevin Morgante, Gianluca Pinsard, Frederic Rataj, Mirek Reess, Jean-Michel Savini, Giorgio Schrader, Jan-Rutger Stamper, Richard Winter, Berend Abe, L. Abreu, M. Achilleos, N. Ade, P. Adybekian, V. Affer, L. Agnor, C. Agundez, M. Alard, C. Alcala, J. Allende Prieto, C. Alonso Floriano, F. J. Altieri, F. Alvarez Iglesias, C. A. Amado, P. Andersen, A. Aylward, A. Baffa, C. Bakos, G. Ballerini, P. Banaszkiewicz, M. Barber, R. J. Barrado, D. Barton, E. J. Batista, V. Bellucci, G. Belmonte Avilés, J. A. Berry, D. Bézard, B. Biondi, D. Błęcka, M. Boisse, I. Bonfond, B. Bordé, P. Börner, P. Bouy, H. Brown, L. Buchhave, L. Budaj, J. Bulgarelli, A. Burleigh, M. Cabral, A. Capria, M. T. Cassan, A. Cavarroc, C. Cecchi-Pestellini, C. Cerulli, R. Chadney, J. Chamberlain, S. Charnoz, S. Christian Jessen, N. Ciaravella, A. Claret, A. Claudi, R. Coates, A. Cole, R. Collura, A. Cordier, D. Covino, E. Danielski, C. Damasso, M. Deeg, H. J. Delgado-Mena, E. Del Vecchio, C. Demangeon, O. De Sio, A. De Wit, J. Dobrijévic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernández, M. Femenía Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouqué, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. García López, R. J. Garcia-Piquer, A. Gear, W. Gerard, J.-C. Gesa, L. Giani, E. Gianotti, F. Gillon, M. Giro, E. Giuranna, M. Gomez, H. Gomez-Leal, I. Gonzalez Hernandez, J. González Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hébrard, E. Heiter, U. Heredero, R. L. Herrero, E. Hersant, F. Heyrovsky, D. Hollis, M. Hubert, B. Hueso, R. Israelian, G. Iro, N. Irwin, P. Jacquemoud, S. Jones, G. Jones, H. Justtanont, K. Kehoe, T. Kerschbaum, F. Kerins, E. Kervella, P. Kipping, D. Koskinen, T. Krupp, N. Lahav, O. Laken, B. Lanza, N. Lellouch, E. Leto, G. Licandro Goldaracena, J. Lithgow-Bertelloni, C. Liu, S. J. Lo Cicero, U. Lodieu, N. Lognonné, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Lundgaard Rasmussen, I. Luntzer, A. Machado, P. MacTavish, C. Maggio, A. Maillard, J.-P. Magnes, W. Maldonado, J. Mall, U. Marquette, J.-B. Mauskopf, P. Massi, F. Maurin, A.-S. Medvedev, A. Michaut, C. Miles-Paez, P. Montalto, M. Montañés Rodríguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderón, M. Morello, G. Moro Martín, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Peña Ramírez, K. Y. Peralta, J. Perez-Hoyos, S. Petrov, R. Pezzuto, S. Pietrzak, R. Pilat-Lohinger, E. Piskunov, N. Prinja, R. Prisinzano, L. Polichtchouk, I. Poretti, E. Radioti, A. Ramos, A. A. Rank-Lüftinger, T. Read, P. Readorn, K. Rebolo López, R. Rebordão, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sánchez Béjar, V. J. Sanchez Lavega, A. Sanromá, E. Santos, N. Sanz Forcada, J. Scandariato, G. Schmider, F.-X. Scholz, A. Scuderi, S. Sethenadh, J. Shore, S. Showman, A. Sicardy, B. Sitek, P. Smith, A. Soret, L. Sousa, S. Stiepen, A. Stolarski, M. Strazzulla, G. Tabernero, H. M. Tanga, P. Tecsa, M. Temple, J. Terenzi, L. Tessenyi, M. Testi, L. Thompson, S. Thrastarson, H. Tingley, B. W. Trifoglio, M. Martín Torres, J. Tozzi, A. Turrini, D. Varley, R. Vakili, F. de Val-Borro, M. Valdivieso, M. L. Venot, O. Villaver, E. Vinatier, S. Viti, S. Waldmann, I. Waltham, D. Ward-Thompson, D. Waters, R. Watkins, C. Watson, D. Wawer, P. Wawrzaszk, A. White, G. Widemann, T. Winek, W. Wiśniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N.
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author-letter	Tinetti, Giovanna
doi_str_mv	10.1007/s10686-015-9484-8
dewey-full	520
author2-role	verfasserin
title_sort	echo science case
title_auth	The EChO science case
abstract	Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.
abstractGer	Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.
abstract_unstemmed	Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.
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container_issue	2-3
title_short	The EChO science case
url	https://dx.doi.org/10.1007/s10686-015-9484-8
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author2	Drossart, Pierre Eccleston, Paul Hartogh, Paul Isaak, Kate Linder, Martin Lovis, Christophe Micela, Giusi Ollivier, Marc Puig, Ludovic Ribas, Ignasi Snellen, Ignas Swinyard, Bruce Allard, France Barstow, Joanna Cho, James Coustenis, Athena Cockell, Charles Correia, Alexandre Decin, Leen de Kok, Remco Deroo, Pieter Encrenaz, Therese Forget, Francois Glasse, Alistair Griffith, Caitlin Guillot, Tristan Koskinen, Tommi Lammer, Helmut Leconte, Jeremy Maxted, Pierre Mueller-Wodarg, Ingo Nelson, Richard North, Chris Pallé, Enric Pagano, Isabella Piccioni, Guseppe Pinfield, David Selsis, Franck Sozzetti, Alessandro Stixrude, Lars Tennyson, Jonathan Turrini, Diego Zapatero-Osorio, Mariarosa Beaulieu, Jean-Philippe Grodent, Denis Guedel, Manuel Luz, David Nørgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coudé Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Géza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Zapata, Gonzalo Ramos Adriani, Alberto Azzollini, Ruymán Balado, Ana Bryson, Ian Burston, Raymond Colomé, Josep Crook, Martin Di Giorgio, Anna Griffin, Matt Hoogeveen, Ruud Ottensamer, Roland Irshad, Ranah Middleton, Kevin Morgante, Gianluca Pinsard, Frederic Rataj, Mirek Reess, Jean-Michel Savini, Giorgio Schrader, Jan-Rutger Stamper, Richard Winter, Berend Abe, L. Abreu, M. Achilleos, N. Ade, P. Adybekian, V. Affer, L. Agnor, C. Agundez, M. Alard, C. Alcala, J. Allende Prieto, C. Alonso Floriano, F. J. Altieri, F. Alvarez Iglesias, C. A. Amado, P. Andersen, A. Aylward, A. Baffa, C. Bakos, G. Ballerini, P. Banaszkiewicz, M. Barber, R. J. Barrado, D. Barton, E. J. Batista, V. Bellucci, G. Belmonte Avilés, J. A. Berry, D. Bézard, B. Biondi, D. Błęcka, M. Boisse, I. Bonfond, B. Bordé, P. Börner, P. Bouy, H. Brown, L. Buchhave, L. Budaj, J. Bulgarelli, A. Burleigh, M. Cabral, A. Capria, M. T. Cassan, A. Cavarroc, C. Cecchi-Pestellini, C. Cerulli, R. Chadney, J. Chamberlain, S. Charnoz, S. Christian Jessen, N. Ciaravella, A. Claret, A. Claudi, R. Coates, A. Cole, R. Collura, A. Cordier, D. Covino, E. Danielski, C. Damasso, M. Deeg, H. J. Delgado-Mena, E. Del Vecchio, C. Demangeon, O. De Sio, A. De Wit, J. Dobrijévic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernández, M. Femenía Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouqué, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. García López, R. J. Garcia-Piquer, A. Gear, W. Gerard, J.-C. Gesa, L. Giani, E. Gianotti, F. Gillon, M. Giro, E. Giuranna, M. Gomez, H. Gomez-Leal, I. Gonzalez Hernandez, J. González Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hébrard, E. Heiter, U. Heredero, R. L. Herrero, E. Hersant, F. Heyrovsky, D. Hollis, M. Hubert, B. Hueso, R. Israelian, G. Iro, N. Irwin, P. Jacquemoud, S. Jones, G. Jones, H. Justtanont, K. Kehoe, T. Kerschbaum, F. Kerins, E. Kervella, P. Kipping, D. Koskinen, T. Krupp, N. Lahav, O. Laken, B. Lanza, N. Lellouch, E. Leto, G. Licandro Goldaracena, J. Lithgow-Bertelloni, C. Liu, S. J. Lo Cicero, U. Lodieu, N. Lognonné, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Lundgaard Rasmussen, I. Luntzer, A. Machado, P. MacTavish, C. Maggio, A. Maillard, J.-P. Magnes, W. Maldonado, J. Mall, U. Marquette, J.-B. Mauskopf, P. Massi, F. Maurin, A.-S. Medvedev, A. Michaut, C. Miles-Paez, P. Montalto, M. Montañés Rodríguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderón, M. Morello, G. Moro Martín, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Peña Ramírez, K. Y. Peralta, J. Perez-Hoyos, S. Petrov, R. Pezzuto, S. Pietrzak, R. Pilat-Lohinger, E. Piskunov, N. Prinja, R. Prisinzano, L. Polichtchouk, I. Poretti, E. Radioti, A. Ramos, A. A. Rank-Lüftinger, T. Read, P. Readorn, K. Rebolo López, R. Rebordão, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sánchez Béjar, V. J. Sanchez Lavega, A. Sanromá, E. Santos, N. Sanz Forcada, J. Scandariato, G. Schmider, F.-X. Scholz, A. Scuderi, S. Sethenadh, J. Shore, S. Showman, A. Sicardy, B. Sitek, P. Smith, A. Soret, L. Sousa, S. Stiepen, A. Stolarski, M. Strazzulla, G. Tabernero, H. M. Tanga, P. Tecsa, M. Temple, J. Terenzi, L. Tessenyi, M. Testi, L. Thompson, S. Thrastarson, H. Tingley, B. W. Trifoglio, M. Martín Torres, J. Tozzi, A. Turrini, D. Varley, R. Vakili, F. de Val-Borro, M. Valdivieso, M. L. Venot, O. Villaver, E. Vinatier, S. Viti, S. Waldmann, I. Waltham, D. Ward-Thompson, D. Waters, R. Watkins, C. Watson, D. Wawer, P. Wawrzaszk, A. White, G. Widemann, T. Winek, W. Wiśniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N.
author2Str	Drossart, Pierre Eccleston, Paul Hartogh, Paul Isaak, Kate Linder, Martin Lovis, Christophe Micela, Giusi Ollivier, Marc Puig, Ludovic Ribas, Ignasi Snellen, Ignas Swinyard, Bruce Allard, France Barstow, Joanna Cho, James Coustenis, Athena Cockell, Charles Correia, Alexandre Decin, Leen de Kok, Remco Deroo, Pieter Encrenaz, Therese Forget, Francois Glasse, Alistair Griffith, Caitlin Guillot, Tristan Koskinen, Tommi Lammer, Helmut Leconte, Jeremy Maxted, Pierre Mueller-Wodarg, Ingo Nelson, Richard North, Chris Pallé, Enric Pagano, Isabella Piccioni, Guseppe Pinfield, David Selsis, Franck Sozzetti, Alessandro Stixrude, Lars Tennyson, Jonathan Turrini, Diego Zapatero-Osorio, Mariarosa Beaulieu, Jean-Philippe Grodent, Denis Guedel, Manuel Luz, David Nørgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coudé Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Géza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Zapata, Gonzalo Ramos Adriani, Alberto Azzollini, Ruymán Balado, Ana Bryson, Ian Burston, Raymond Colomé, Josep Crook, Martin Di Giorgio, Anna Griffin, Matt Hoogeveen, Ruud Ottensamer, Roland Irshad, Ranah Middleton, Kevin Morgante, Gianluca Pinsard, Frederic Rataj, Mirek Reess, Jean-Michel Savini, Giorgio Schrader, Jan-Rutger Stamper, Richard Winter, Berend Abe, L. Abreu, M. Achilleos, N. Ade, P. Adybekian, V. Affer, L. Agnor, C. Agundez, M. Alard, C. Alcala, J. Allende Prieto, C. Alonso Floriano, F. J. Altieri, F. Alvarez Iglesias, C. A. Amado, P. Andersen, A. Aylward, A. Baffa, C. Bakos, G. Ballerini, P. Banaszkiewicz, M. Barber, R. J. Barrado, D. Barton, E. J. Batista, V. Bellucci, G. Belmonte Avilés, J. A. Berry, D. Bézard, B. Biondi, D. Błęcka, M. Boisse, I. Bonfond, B. Bordé, P. Börner, P. Bouy, H. Brown, L. Buchhave, L. Budaj, J. Bulgarelli, A. Burleigh, M. Cabral, A. Capria, M. T. Cassan, A. Cavarroc, C. Cecchi-Pestellini, C. Cerulli, R. Chadney, J. Chamberlain, S. Charnoz, S. Christian Jessen, N. Ciaravella, A. Claret, A. Claudi, R. Coates, A. Cole, R. Collura, A. Cordier, D. Covino, E. Danielski, C. Damasso, M. Deeg, H. J. Delgado-Mena, E. Del Vecchio, C. Demangeon, O. De Sio, A. De Wit, J. Dobrijévic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernández, M. Femenía Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouqué, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. García López, R. J. Garcia-Piquer, A. Gear, W. Gerard, J.-C. Gesa, L. Giani, E. Gianotti, F. Gillon, M. Giro, E. Giuranna, M. Gomez, H. Gomez-Leal, I. Gonzalez Hernandez, J. González Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hébrard, E. Heiter, U. Heredero, R. L. Herrero, E. Hersant, F. Heyrovsky, D. Hollis, M. Hubert, B. Hueso, R. Israelian, G. Iro, N. Irwin, P. Jacquemoud, S. Jones, G. Jones, H. Justtanont, K. Kehoe, T. Kerschbaum, F. Kerins, E. Kervella, P. Kipping, D. Koskinen, T. Krupp, N. Lahav, O. Laken, B. Lanza, N. Lellouch, E. Leto, G. Licandro Goldaracena, J. Lithgow-Bertelloni, C. Liu, S. J. Lo Cicero, U. Lodieu, N. Lognonné, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Lundgaard Rasmussen, I. Luntzer, A. Machado, P. MacTavish, C. Maggio, A. Maillard, J.-P. Magnes, W. Maldonado, J. Mall, U. Marquette, J.-B. Mauskopf, P. Massi, F. Maurin, A.-S. Medvedev, A. Michaut, C. Miles-Paez, P. Montalto, M. Montañés Rodríguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderón, M. Morello, G. Moro Martín, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Peña Ramírez, K. Y. Peralta, J. Perez-Hoyos, S. Petrov, R. Pezzuto, S. Pietrzak, R. Pilat-Lohinger, E. Piskunov, N. Prinja, R. Prisinzano, L. Polichtchouk, I. Poretti, E. Radioti, A. Ramos, A. A. Rank-Lüftinger, T. Read, P. Readorn, K. Rebolo López, R. Rebordão, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sánchez Béjar, V. J. Sanchez Lavega, A. Sanromá, E. Santos, N. Sanz Forcada, J. Scandariato, G. Schmider, F.-X. Scholz, A. Scuderi, S. Sethenadh, J. Shore, S. Showman, A. Sicardy, B. Sitek, P. Smith, A. Soret, L. Sousa, S. Stiepen, A. Stolarski, M. Strazzulla, G. Tabernero, H. M. Tanga, P. Tecsa, M. Temple, J. Terenzi, L. Tessenyi, M. Testi, L. Thompson, S. Thrastarson, H. Tingley, B. W. Trifoglio, M. Martín Torres, J. Tozzi, A. Turrini, D. Varley, R. Vakili, F. de Val-Borro, M. Valdivieso, M. L. Venot, O. Villaver, E. Vinatier, S. Viti, S. Waldmann, I. Waltham, D. Ward-Thompson, D. Waters, R. Watkins, C. Watson, D. Wawer, P. Wawrzaszk, A. White, G. Widemann, T. Winek, W. Wiśniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N.
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doi_str	10.1007/s10686-015-9484-8
up_date	2024-07-04T03:10:48.782Z
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fullrecord_marcxml	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR012459186</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220110234001.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201005s2015 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s10686-015-9484-8</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR012459186</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)s10686-015-9484-8-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">520</subfield><subfield code="q">ASE</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.00</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Tinetti, Giovanna</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The EChO science case</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract 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 $ m^{2} $ is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 $ m^{2} $ 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.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Exoplanets</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Spectroscopy</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Atmospheric science</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">IR astronomy</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Space missions</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Drossart, 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J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Garcia-Piquer, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gear, W.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gerard, J.-C.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gesa, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giani, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gianotti, F.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gillon, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giro, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Giuranna, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gomez, H.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gomez-Leal, I.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gonzalez Hernandez, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">González Merino, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Graczyk, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Grassi, D.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Guardia, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Guio, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Gustin, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hargrave, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Haigh, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hébrard, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Heiter, U.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Heredero, R. L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Herrero, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hersant, F.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Heyrovsky, D.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hollis, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hubert, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Hueso, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Israelian, G.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Iro, N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Irwin, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Jacquemoud, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Jones, G.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Jones, H.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Justtanont, K.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kehoe, T.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kerschbaum, F.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kerins, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kervella, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kipping, D.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Koskinen, T.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Krupp, N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Lahav, O.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Laken, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Lanza, N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Lellouch, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Leto, G.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Licandro Goldaracena, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Lithgow-Bertelloni, C.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Liu, S. 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Y.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Peralta, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Perez-Hoyos, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Petrov, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Pezzuto, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Pietrzak, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Pilat-Lohinger, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Piskunov, N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Prinja, R.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Prisinzano, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Polichtchouk, I.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Poretti, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Radioti, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ramos, A. 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J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sanchez Lavega, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sanromá, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Santos, N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sanz Forcada, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Scandariato, G.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Schmider, F.-X.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Scholz, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Scuderi, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sethenadh, J.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Shore, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Showman, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sicardy, B.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sitek, P.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Smith, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Soret, L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sousa, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Stiepen, A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Stolarski, M.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Strazzulla, G.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Tabernero, H. 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