The EChO science case
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Data de Publicação: | 2015 |
Outros Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
Texto Completo: | http://hdl.handle.net/10773/15118 |
Resumo: | 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 mu m with a goal of covering from 0.4 to 16 mu m. Only modest spectral resolving power is needed, with R similar to 300 for wavelengths less than 5 mu m and R similar to 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 mu m 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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The EChO science caseExoplanetsSpectroscopyAtmospheric scienceIR astronomySpace missionsThe 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 mu m with a goal of covering from 0.4 to 16 mu m. Only modest spectral resolving power is needed, with R similar to 300 for wavelengths less than 5 mu m and R similar to 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 mu m 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.Springer2016-01-27T12:19:21Z2015-12-01T00:00:00Z2015-12info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10773/15118eng0922-643510.1007/s10686-015-9484-8Tinetti, GiovannaDrossart, PierreEccleston, PaulHartogh, PaulIsaak, KateLinder, MartinLovis, ChristopheMicela, GiusiOllivier, MarcPuig, LudovicRibas, IgnasiSnellen, IgnasSwinyard, BruceAllard, FranceBarstow, JoannaCho, JamesCoustenis, AthenaCockell, CharlesCorreia, AlexandreDecin, Leende Kok, RemcoDeroo, PieterEncrenaz, ThereseForget, FrancoisGlasse, AlistairGriffith, CaitlinGuillot, TristanKoskinen, TommiLammer, HelmutLeconte, JeremyMaxted, PierreMueller-Wodarg, IngoNelson, RichardNorth, ChrisPalle, EnricPagano, IsabellaPiccioni, GuseppePinfield, DavidSelsis, FranckSozzetti, AlessandroStixrude, LarsTennyson, JonathanTurrini, DiegoZapatero-Osorio, MariarosaBeaulieu, Jean-PhilippeGrodent, DenisGuedel, ManuelLuz, DavidNorgaard-Nielsen, Hans UlrikRay, TomRickman, HansSelig, AvriSwain, MarkBanaszkiewicz, MarekBarlow, MikeBowles, NeilBranduardi-Raymont, Grazielladu Foresto, Vincent CoudeGerard, Jean-ClaudeGizon, LaurentHornstrup, AllanJarchow, ChristopherKerschbaum, FranzKovacs, GezaLagage, Pierre-OlivierLim, TanyaLopez-Morales, MercedesMalaguti, GiuseppePace, EmanuelePascale, EnzoVandenbussche, BartWright, GillianRamos Zapata, GonzaloAdriani, AlbertoAzzollini, RuymanBalado, AnaBryson, IanBurston, RaymondColome, JosepCrook, MartinDi Giorgio, AnnaGriffin, MattHoogeveen, RuudOttensamer, RolandIrshad, RanahMiddleton, KevinMorgante, GianlucaPinsard, FredericRataj, MirekReess, Jean-MichelSavini, GiorgioSchrader, Jan-RutgerStamper, RichardWinter, BerendAbe, 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 Aviles, J. A.Berry, D.Bezard, B.Biondi, D.Blecka, M.Boisse, I.Bonfond, B.Borde, P.Boerner, 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.Jessen, N. ChristianCiaravella, 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.Dobrijevic, M.Doel, P.Dominic, C.Dorfi, E.Eales, S.Eiroa, C.Espinoza Contreras, M.Esposito, M.Eymet, V.Fabrizio, N.Fernandez, M.Femena Castella, B.Figueira, P.Filacchione, G.Fletcher, L.Focardi, M.Fossey, S.Fouque, P.Frith, J.Galand, M.Gambicorti, L.Gaulme, P.Garcia Lopez, 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.Gonzalez Merino, B.Graczyk, R.Grassi, D.Guardia, J.Guio, P.Gustin, J.Hargrave, P.Haigh, J.Hebrard, 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.Lognonne, P.Lopez-Puertas, M.Lopez-Valverde, M. A.Rasmussen, I. LundgaardLuntzer, 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.Montanes Rodriguez, P.Monteiro, M.Montes, D.Morais, H.Morales, J. C.Morales-Calderon, M.Morello, G.Moro Martin, A.Moses, J.Moya Bedon, A.Murgas Alcaino, F.Oliva, E.Orton, G.Palla, F.Pancrazzi, M.Pantin, E.Parmentier, V.Parviainen, H.Pena Ramirez, 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-Lueftinger, T.Read, P.Readorn, K.Rebolo Lopez, R.Rebordao, J.Rengel, M.Rezac, L.Rocchetto, M.Rodler, F.Sanchez Bejar, V. J.Lavega, A. SanchezSanroma, 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.Martin 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.Wisniowski, T.Yelle, R.Yung, Y.Yurchenko, S. N.info:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-02-22T11:27:53Zoai:ria.ua.pt:10773/15118Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T02:50:32.924423Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse |
dc.title.none.fl_str_mv |
The EChO science case |
title |
The EChO science case |
spellingShingle |
The EChO science case Tinetti, Giovanna Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions |
title_short |
The EChO science case |
title_full |
The EChO science case |
title_fullStr |
The EChO science case |
title_full_unstemmed |
The EChO science case |
title_sort |
The EChO science case |
author |
Tinetti, Giovanna |
author_facet |
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 Palle, 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 Norgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coude Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Geza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Ramos Zapata, Gonzalo Adriani, Alberto Azzollini, Ruyman Balado, Ana Bryson, Ian Burston, Raymond Colome, 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 Aviles, J. A. Berry, D. Bezard, B. Biondi, D. Blecka, M. Boisse, I. Bonfond, B. Borde, P. Boerner, 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. Jessen, N. Christian 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. Dobrijevic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernandez, M. Femena Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouque, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. Garcia Lopez, 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. Gonzalez Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hebrard, 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. Lognonne, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Rasmussen, I. Lundgaard 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. Montanes Rodriguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderon, M. Morello, G. Moro Martin, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Pena Ramirez, 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-Lueftinger, T. Read, P. Readorn, K. Rebolo Lopez, R. Rebordao, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sanchez Bejar, V. J. Lavega, A. Sanchez Sanroma, 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. Martin 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. Wisniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N. |
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author |
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 Palle, 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 Norgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coude Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Geza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Ramos Zapata, Gonzalo Adriani, Alberto Azzollini, Ruyman Balado, Ana Bryson, Ian Burston, Raymond Colome, 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 Aviles, J. A. Berry, D. Bezard, B. Biondi, D. Blecka, M. Boisse, I. Bonfond, B. Borde, P. Boerner, 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. Jessen, N. Christian 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. Dobrijevic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernandez, M. Femena Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouque, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. Garcia Lopez, 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. Gonzalez Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hebrard, 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. Lognonne, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Rasmussen, I. Lundgaard 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. Montanes Rodriguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderon, M. Morello, G. Moro Martin, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Pena Ramirez, 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-Lueftinger, T. Read, P. Readorn, K. Rebolo Lopez, R. Rebordao, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sanchez Bejar, V. J. Lavega, A. Sanchez Sanroma, 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. Martin 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. Wisniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N. |
author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
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 Palle, 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 Norgaard-Nielsen, Hans Ulrik Ray, Tom Rickman, Hans Selig, Avri Swain, Mark Banaszkiewicz, Marek Barlow, Mike Bowles, Neil Branduardi-Raymont, Graziella du Foresto, Vincent Coude Gerard, Jean-Claude Gizon, Laurent Hornstrup, Allan Jarchow, Christopher Kerschbaum, Franz Kovacs, Geza Lagage, Pierre-Olivier Lim, Tanya Lopez-Morales, Mercedes Malaguti, Giuseppe Pace, Emanuele Pascale, Enzo Vandenbussche, Bart Wright, Gillian Ramos Zapata, Gonzalo Adriani, Alberto Azzollini, Ruyman Balado, Ana Bryson, Ian Burston, Raymond Colome, 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 Aviles, J. A. Berry, D. Bezard, B. Biondi, D. Blecka, M. Boisse, I. Bonfond, B. Borde, P. Boerner, 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. Jessen, N. Christian 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. Dobrijevic, M. Doel, P. Dominic, C. Dorfi, E. Eales, S. Eiroa, C. Espinoza Contreras, M. Esposito, M. Eymet, V. Fabrizio, N. Fernandez, M. Femena Castella, B. Figueira, P. Filacchione, G. Fletcher, L. Focardi, M. Fossey, S. Fouque, P. Frith, J. Galand, M. Gambicorti, L. Gaulme, P. Garcia Lopez, 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. Gonzalez Merino, B. Graczyk, R. Grassi, D. Guardia, J. Guio, P. Gustin, J. Hargrave, P. Haigh, J. Hebrard, 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. Lognonne, P. Lopez-Puertas, M. Lopez-Valverde, M. A. Rasmussen, I. Lundgaard 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. Montanes Rodriguez, P. Monteiro, M. Montes, D. Morais, H. Morales, J. C. Morales-Calderon, M. Morello, G. Moro Martin, A. Moses, J. Moya Bedon, A. Murgas Alcaino, F. Oliva, E. Orton, G. Palla, F. Pancrazzi, M. Pantin, E. Parmentier, V. Parviainen, H. Pena Ramirez, 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-Lueftinger, T. Read, P. Readorn, K. Rebolo Lopez, R. Rebordao, J. Rengel, M. Rezac, L. Rocchetto, M. Rodler, F. Sanchez Bejar, V. J. Lavega, A. Sanchez Sanroma, 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. Martin 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. Wisniowski, T. Yelle, R. Yung, Y. Yurchenko, S. N. |
dc.subject.por.fl_str_mv |
Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions |
topic |
Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions |
description |
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 mu m with a goal of covering from 0.4 to 16 mu m. Only modest spectral resolving power is needed, with R similar to 300 for wavelengths less than 5 mu m and R similar to 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 mu m 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. |
publishDate |
2015 |
dc.date.none.fl_str_mv |
2015-12-01T00:00:00Z 2015-12 2016-01-27T12:19:21Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10773/15118 |
url |
http://hdl.handle.net/10773/15118 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
0922-6435 10.1007/s10686-015-9484-8 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
dc.publisher.none.fl_str_mv |
Springer |
publisher.none.fl_str_mv |
Springer |
dc.source.none.fl_str_mv |
reponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação instacron:RCAAP |
instname_str |
Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
instacron_str |
RCAAP |
institution |
RCAAP |
reponame_str |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
collection |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) |
repository.name.fl_str_mv |
Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informação |
repository.mail.fl_str_mv |
|
_version_ |
1799137555208208384 |