The EChO science case
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- 作者：Giovanna Tinetti ; Pierre Drossart ; Paul Eccleston ; Paul Hartogh…
- 关键词：Exoplanets ; Spectroscopy ; Atmospheric science ; IR astronomy ; Space missions
- 刊名：Experimental Astronomy
- 出版年：2015
- 出版时间：December 2015
- 年：2015
- 卷：40
- 期：2-3
- 页码：329-391
- 全文大小：8,414 KB
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196.Zhu, Z., et al.: ApJL 758, L42 (2012)CrossRef ADS - 作者单位：Giovanna Tinetti (1)
Pierre Drossart (2)
Paul Eccleston (3)
Paul Hartogh (4)
Kate Isaak (5)
Martin Linder (5)
Christophe Lovis (6)
Giusi Micela (7)
Marc Ollivier (2) (8)
Ludovic Puig (5)
Ignasi Ribas (9)
Ignas Snellen (10)
Bruce Swinyard (1) (3)
France Allard (11)
Joanna Barstow (12)
James Cho (13)
Athena Coustenis (2)
Charles Cockell (14)
Alexandre Correia (15)
Leen Decin (16)
Remco de Kok (17)
Pieter Deroo (18)
Therese Encrenaz (2)
Francois Forget (19)
Alistair Glasse (20)
Caitlin Griffith (21)
Tristan Guillot (22)
Tommi Koskinen (21)
Helmut Lammer (23)
Jeremy Leconte (19) (24)
Pierre Maxted (25)
Ingo Mueller-Wodarg (26)
Richard Nelson (13)
Chris North (27)
Enric Pallé (28)
Isabella Pagano (29)
Guseppe Piccioni (30)
David Pinfield (31)
Franck Selsis (32)
Alessandro Sozzetti (33)
Lars Stixrude (1)
Jonathan Tennyson (1)
Diego Turrini (30)
Mariarosa Zapatero-Osorio (34)
Jean-Philippe Beaulieu (35)
Denis Grodent (36)
Manuel Guedel (37)
David Luz (38)
Hans Ulrik Nørgaard-Nielsen (39)
Tom Ray (40)
Hans Rickman (41) (42)
Avri Selig (17)
Mark Swain (18)
Marek Banaszkiewicz (41)
Mike Barlow (1)
Neil Bowles (12)
Graziella Branduardi-Raymont (43)
Vincent Coudé du Foresto (2)
Jean-Claude Gerard (36)
Laurent Gizon (4)
Allan Hornstrup (45)
Christopher Jarchow (4)
Franz Kerschbaum (37)
Géza Kovacs (45)
Pierre-Olivier Lagage (46)
Tanya Lim (3)
Mercedes Lopez-Morales (9)
Giuseppe Malaguti (47)
Emanuele Pace (48)
Enzo Pascale (27)
Bart Vandenbussche (16)
Gillian Wright (20)
Gonzalo Ramos Zapata (49)
Alberto Adriani (30)
Ruymán Azzollini (40)
Ana Balado (49)
Ian Bryson (20)
Raymond Burston (4)
Josep Colomé (9)
Martin Crook (3)
Anna Di Giorgio (30)
Matt Griffin (27)
Ruud Hoogeveen (17)
Roland Ottensamer (37)
Ranah Irshad (3)
Kevin Middleton (3)
Gianluca Morgante (47)
Frederic Pinsard (46)
Mirek Rataj (41)
Jean-Michel Reess (2)
Giorgio Savini (1)
Jan-Rutger Schrader (17)
Richard Stamper (3)
Berend Winter (43)
L. Abe (22)
M. Abreu (63)
N. Achilleos (1)
P. Ade (27)
V. Adybekian (62)
L. Affer (7)
C. Agnor (13)
M. Agundez (32)
C. Alard (35)
J. Alcala (58)
C. Allende Prieto (28)
F. J. Alonso Floriano (68)
F. Altieri (30)
C. A. Alvarez Iglesias (28)
P. Amado (66)
A. Andersen (51)
A. Aylward (1)
C. Baffa (56)
G. Bakos (79)
P. Ballerini (29)
M. Banaszkiewicz (41)
R. J. Barber (1)
D. Barrado (34) (49)
E. J. Barton (1)
V. Batista (35)
G. Bellucci (30)
J. A. Belmonte Avilés (28)
D. Berry (63)
B. Bézard (2)
D. Biondi (30)
M. Błęcka (41)
I. Boisse (62)
B. Bonfond (36)
P. Bordé (8)
P. Börner (4)
H. Bouy (34) (49)
L. Brown (18)
L. Buchhave (51)
J. Budaj (65)
A. Bulgarelli (47)
M. Burleigh (74)
A. Cabral (63)
M. T. Capria (30)
A. Cassan (35)
C. Cavarroc (46)
C. Cecchi-Pestellini (7)
R. Cerulli (30)
J. Chadney (26)
S. Chamberlain (63)
S. Charnoz (46)
N. Christian Jessen (44)
A. Ciaravella (7)
A. Claret (66)
R. Claudi (59)
A. Coates (43)
R. Cole (43)
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1. Department of Physics & Astronomy, University College London, WC1E6BT, London, UK
2. LESIA, Observatoire de Paris, Meudon, France
3. STFC Rutherford Appleton Laboratory, Harwell Campus, Didcot, OX11 0QX, UK
4. Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, Germany
5. European Space Agency-ESTEC, Noordwijk, The Netherlands
6. Geneva Observatory, Geneva, Switzerland
7. INAF: Osservatorio Astronomico di Palermo G.S. Vaiana, Palermo, Italy
8. Institut d’Astrophysique Spatiale, Orsay, France
9. Institut d’Estudis Espacials de Catalunya (ICE-CSIC), Barcelona, Spain
10. Leiden University, Leiden, The Netherlands
11. Ecole Normale Superieure, Lyon, France
12. Oxford University, Oxford, UK
13. Queen Mary University London, London, UK
14. Royal Observatory Edinburgh, Edinburgh, UK
15. Aveiro University, Aveiro, Portugal
16. University of Leuven, Leuven, Belgium
17. SRON, Institute for Space Research, Utrecht, The Netherlands
18. NASA Jet Propulsion Laboratory, Pasadena, CA, USA
19. LMD, Jussieu, Paris, France
20. STFC UK-ATC, Edinburgh, UK
21. University of Arizona, Tucson, AZ, USA
22. Observatoire de Nice, Nice, France
23. IWF, Graz, Austria
24. Canadian Institute of Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada
25. Keele University, Keele, UK
26. Imperial College, London, UK
27. Cardiff University, Cardiff, UK
28. Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain
29. INAF- OAT, Catania, Italy
30. INAF-IAPS, Rome, Italy
31. University of Hertfordshire, Hatfield, UK
32. Université de Bordeaux, Bordeaux, France
33. INAF, Torino, Italy
34. CAB, Madrid, Spain
35. Institut d’Astrophysique de Paris, Paris, France
36. Université de Liège, Liège, Belgium
37. University of Vienna, Vienna, Austria
38. Universidade de Lisboa, Lisbon, Portugal
39. DSRI, Lyngby, Denmark
40. Dublin Institute for Advanced Studies, Dublin, Ireland
41. Space Research Centre, Polish Academy of Science, Warsaw, Poland
42. Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
43. Mullard Space Science Laboratory, University College London, Surrey, RH5 6NT, UK
45. Konkoly Observatory, Budapest, Hungary
46. Centre Energie Atomique – Saclay, Gif-sur-Yvette, France
47. INAF – IASF – Bologna, Bologna, Italy
48. Università di Firenze, Florence, Italy
49. INTA, Águilas, Spain
63. CAAUL, Lisbon, Portugal
62. CAUP, Porto, Portugal
58. INAF – Capodimonte, Naples, Italy
68. UCM, Madrid, Spain
66. IAA, Madrid, Spain
51. DARK Cosmology Center, Copenhagen, Denmark
56. INAF – Arcetri, Florence, Italy
79. Princeton University, Princeton, NJ, USA
65. Slovak Academy of Sciences, Bratislava, Slovakia
74. University of Leicester, Leicester, UK
44. DTU Space, Kongens Lyngby, Denmark
59. INAF – Padova, Padova, Italy
52. Observatoire de Besancon, Besancon, France
78. Harvard Smithsonian Center for Astrophysics, Cambridge, MA, USA
61. University of Amsterdam, Amsterdam, The Netherlands
67. UAM, Madrid, Spain
54. LATT, Toulouse, France
50. Charles University, Prague, Czech Republic
69. UPV, Valencia, Spain
55. University of Hamburg, Hamburg, Germany
53. IPGP, Paris, France
70. Onsala Space Observatory, Onsala, Sweden
75. University of Manchester, Manchester, UK
71. Cambridge University, Cambridge, UK
80. Space Science Institute, Seabrook, TX, USA
57. INAF – Brera, Milan, Italy
60. Università di Pisa, Pisa, Italy
64. ESO, Garching, Germany
77. California Institute of Technology, Pasadena, CA, USA
81. Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain
82. Luleå Technical University, Kiruna, Sweden
73. Royal Holloway University of London, Surrey, UK
76. University of Lancaster, Lancaster, UK
72. Open University, Milton Keynes, UK - 刊物类别：Physics and Astronomy
- 刊物主题：Physics
Astronomy
Statistics for Engineering, Physics, Computer Science, Chemistry and Geosciences - 出版者：Springer Netherlands
- ISSN：1572-9508
文摘
The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune—all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10−4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R ~ 300 for wavelengths less than 5 μm and R ~ 30 for wavelengths greater than this. The transit spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate than current observations. This would enable the detection of molecular abundances three orders of magnitude lower than currently possible and a fourfold increase from the handful of molecules detected to date. Combining these data with estimates of planetary bulk compositions from accurate measurements of their radii and masses would allow degeneracies associated with planetary interior modelling to be broken, giving unique insight into the interior structure and elemental abundances of these alien worlds. EChO would allow scientists to study exoplanets both as a population and as individuals. The mission can target super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300–3000 K) of F to M-type host stars. The EChO core science would be delivered by a three-tier survey. The EChO Chemical Census: This is a broad survey of a few-hundred exoplanets, which allows us to explore the spectroscopic and chemical diversity of the exoplanet population as a whole. The EChO Origin: This is a deep survey of a subsample of tens of exoplanets for which significantly higher signal to noise and spectral resolution spectra can be obtained to explain the origin of the exoplanet diversity (such as formation mechanisms, chemical processes, atmospheric escape). The EChO Rosetta Stones: This is an ultra-high accuracy survey targeting a subsample of select exoplanets. These will be the bright “benchmark” cases for which a large number of measurements would be taken to explore temporal variations, and to obtain two and three dimensional spatial information on the atmospheric conditions through eclipse-mapping techniques. If EChO were launched today, the exoplanets currently observed are sufficient to provide a large and diverse sample. The Chemical Census survey would consist of > 160 exoplanets with a range of planetary sizes, temperatures, orbital parameters and stellar host properties. Additionally, over the next 10 years, several new ground- and space-based transit photometric surveys and missions will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO’s launch and enable the atmospheric characterisation of hundreds of planets. Keywords Exoplanets Spectroscopy Atmospheric science IR astronomy Space missions