EChO

Research areas:

Intérieurs planétaires (2011 - 2016)

Year:

2012

Authors:

G. Tinetti
J. P. Beaulieu
T. Henning
M. Meyer
G. Micela
I. Ribas
D. Stam
M. Swain
O. Krause
M. Ollivier
E. Pace
B. Swinyard
A. Aylward
R. van Boekel
A. Coradini
T. Encrenaz
I. Snellen
M. R. Zapatero-Osorio
J. Bouwman
J. Y-K. Cho
V. Coude du Foresto
T. Guillot
M. Lopez-Morales
I. Mueller-Wodarg
E. Palle
F. Selsis
A. Sozzetti
P. A. R. Ade
N. Achilleos
A. Adriani
C. B. Agnor
C. Afonso
C. Allende Prieto
G. Bakos
R. J. Barber
M. Barlow
V. Batista
P. Bernath
B. Bezard
P. Borde
L. R. Brown
A. Cassan
C. Cavarroc
A. Ciaravella
C. Cockell
A. Coustenis
C. Danielski
L. Decin
R. De Kok
O. Demangeon
P. Deroo
P. Doel
P. Drossart
L. N. Fletcher
M. Focardi
F. Forget
S. Fossey
P. Fouque
J. Frith
M. Galand
P. Gaulme
J. I. Gonzalez Hernandez
Olivier Grasset
D. Grassi
J. L. Grenfell
M. J. Griffin
C. A. Griffith
U. Groezinger
M. Guedel
P. Guio
O. Hainaut
R. Hargreaves
P. H. Hauschildt
K. Heng
D. Heyrovsky
R. Hueso
P. Irwin
L. Kaltenegger
P. Kervella
D. Kipping
T. T. Koskinen
G. Kovacs
A. La Barbera
H. Lammer
E. Lellouch
G. Leto
M. A. Lopez Valverde
M. Lopez-Puertas
C. Lovis
A. Maggio
J. P. Maillard
J. Maldonado Prado
J. B. Marquette
F. J. Martin-Torres
P. Maxted
S. Miller
S. Molinari
D. Montes
A. Moro-Martin
J. I. Moses
O. Mousis
N. Nguyen Tuong
R. Nelson
G. S. Orton
E. Pantin
E. Pascale
S. Pezzuto
D. Pinfield
E. Poretti
R. Prinja
L. Prisinzano
J. M. Rees
A. Reiners
B. Samuel
A. Sanchez-Lavega
J. Sanz Forcada
D. Sasselov
G. Savini
B. Sicardy
A. Smith
L. Stixrude
J. Tennyson
G. Strazzulla
M. Tessenyi
G. Vasisht
S. Vinatier
S. Viti
I. Waldmann
G. J. White
T. Widemann
R. Wordsworth
R. Yelle
Y. Yung
S. N. Yurchenko

Journal:

EXPERIMENTAL ASTRONOMY

Volume:

Number:

2, SI

Pages:

311-353

Month:

October

ISSN:

0922-6435

BibTex:

@article{WOS:000309230600007,
author = "G. Tinetti and J. P. Beaulieu and T. Henning and M. Meyer and G. Micela and I. Ribas and D. Stam and M. Swain and O. Krause and M. Ollivier and E. Pace and B. Swinyard and A. Aylward and van Boekel, R. and A. Coradini and T. Encrenaz and I. Snellen and M. R. Zapatero-Osorio and J. Bouwman and J. Y-K. Cho and du Foresto, V. Coude and T. Guillot and M. Lopez-Morales and I. Mueller-Wodarg and E. Palle and F. Selsis and A. Sozzetti and P. A. R. Ade and N. Achilleos and A. Adriani and C. B. Agnor and C. Afonso and C. Allende Prieto and G. Bakos and R. J. Barber and M. Barlow and V. Batista and P. Bernath and B. Bezard and P. Borde and L. R. Brown and A. Cassan and C. Cavarroc and A. Ciaravella and C. Cockell and A. Coustenis and C. Danielski and L. Decin and R. De Kok and O. Demangeon and P. Deroo and P. Doel and P. Drossart and L. N. Fletcher and M. Focardi and F. Forget and S. Fossey and P. Fouque and J. Frith and M. Galand and P. Gaulme and J. I. Gonzalez Hernandez and Olivier Grasset and D. Grassi and J. L. Grenfell and M. J. Griffin and C. A. Griffith and U. Groezinger and M. Guedel and P. Guio and O. Hainaut and R. Hargreaves and P. H. Hauschildt and K. Heng and D. Heyrovsky and R. Hueso and P. Irwin and L. Kaltenegger and P. Kervella and D. Kipping and T. T. Koskinen and G. Kovacs and A. La Barbera and H. Lammer and E. Lellouch and G. Leto and M. A. Lopez Valverde and M. Lopez-Puertas and C. Lovis and A. Maggio and J. P. Maillard and J. Maldonado Prado and J. B. Marquette and F. J. Martin-Torres and P. Maxted and S. Miller and S. Molinari and D. Montes and A. Moro-Martin and J. I. Moses and O. Mousis and N. Nguyen Tuong and R. Nelson and G. S. Orton and E. Pantin and E. Pascale and S. Pezzuto and D. Pinfield and E. Poretti and R. Prinja and L. Prisinzano and J. M. Rees and A. Reiners and B. Samuel and A. Sanchez-Lavega and J. Sanz Forcada and D. Sasselov and G. Savini and B. Sicardy and A. Smith and L. Stixrude and J. Tennyson and G. Strazzulla and M. Tessenyi and G. Vasisht and S. Vinatier and S. Viti and I. Waldmann and G. J. White and T. Widemann and R. Wordsworth and R. Yelle and Y. Yung and S. N. Yurchenko",
abstract = "A dedicated mission to investigate exoplanetary atmospheres represents a
   major milestone in our quest to understand our place in the universe by
   placing our Solar System in context and by addressing the suitability of
   planets for the presence of life. EChO-the Exoplanet Characterisation
   Observatory-is a mission concept specifically geared for this purpose.
   EChO will provide simultaneous, multi-wavelength spectroscopic
   observations on a stable platform that will allow very long exposures.
   The use of passive cooling, few moving parts and well established
   technology gives a low-risk and potentially long-lived mission. EChO
   will build on observations by Hubble, Spitzer and ground-based
   telescopes, which discovered the first molecules and atoms in
   exoplanetary atmospheres. However, EChO{\&}#039;s configuration and
   specifications are designed to study a number of systems in a consistent
   manner that will eliminate the ambiguities affecting prior observations.
   EChO will simultaneously observe a broad enough spectral region-from the
   visible to the mid-infrared-to constrain from one single spectrum the
   temperature structure of the atmosphere, the abundances of the major
   carbon and oxygen bearing species, the expected photochemically-produced
   species and magnetospheric signatures. The spectral range and resolution
   are tailored to separate bands belonging to up to 30 molecules and
   retrieve the composition and temperature structure of planetary
   atmospheres. The target list for EChO includes planets ranging from
   Jupiter-sized with equilibrium temperatures T (eq) up to 2,000 K, to
   those of a few Earth masses, with T (eq) \textbackslash{}u223c 300 K.
   The list will include planets with no Solar System analog, such as the
   recently discovered planets GJ1214b, whose density lies between that of
   terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with
   day-side temperature close to 3,000 K. As the number of detected
   exoplanets is growing rapidly each year, and the mass and radius of
   those detected steadily decreases, the target list will be constantly
   adjusted to include the most interesting systems. We have baselined a
   dispersive spectrograph design covering continuously the 0.4-16 mu m
   spectral range in 6 channels (1 in the visible, 5 in the InfraRed),
   which allows the spectral resolution to be adapted from several tens to
   several hundreds, depending on the target brightness. The instrument
   will be mounted behind a 1.5 m class telescope, passively cooled to 50
   K, with the instrument structure and optics passively cooled to
   \textbackslash{}u223c45 K. EChO will be placed in a grand halo orbit
   around L2. This orbit, in combination with an optimised thermal shield
   design, provides a highly stable thermal environment and a high degree
   of visibility of the sky to observe repeatedly several tens of targets
   over the year. Both the baseline and alternative designs have been
   evaluated and no critical items with Technology Readiness Level (TRL)
   less than 4-5 have been identified. We have also undertaken a
   first-order cost and development plan analysis and find that EChO is
   easily compatible with the ESA M-class mission framework.",
doi = "10.1007/s10686-012-9303-4",
extra = "PICL",
issn = "0922-6435",
journal = "EXPERIMENTAL ASTRONOMY",
month = "OCT",
number = "2, SI",
pages = "311-353",
title = "{EC}h{O}",
volume = "34",
year = "2012",
}

Abstract:

A dedicated mission to investigate exoplanetary atmospheres represents a
major milestone in our quest to understand our place in the universe by
placing our Solar System in context and by addressing the suitability of
planets for the presence of life. EChO-the Exoplanet Characterisation
Observatory-is a mission concept specifically geared for this purpose.
EChO will provide simultaneous, multi-wavelength spectroscopic
observations on a stable platform that will allow very long exposures.
The use of passive cooling, few moving parts and well established
technology gives a low-risk and potentially long-lived mission. EChO
will build on observations by Hubble, Spitzer and ground-based
telescopes, which discovered the first molecules and atoms in
exoplanetary atmospheres. However, EChO's configuration and
specifications are designed to study a number of systems in a consistent
manner that will eliminate the ambiguities affecting prior observations.
EChO will simultaneously observe a broad enough spectral region-from the
visible to the mid-infrared-to constrain from one single spectrum the
temperature structure of the atmosphere, the abundances of the major
carbon and oxygen bearing species, the expected photochemically-produced
species and magnetospheric signatures. The spectral range and resolution
are tailored to separate bands belonging to up to 30 molecules and
retrieve the composition and temperature structure of planetary
atmospheres. The target list for EChO includes planets ranging from
Jupiter-sized with equilibrium temperatures T (eq) up to 2,000 K, to
those of a few Earth masses, with T (eq) \textbackslash{}u223c 300 K.
The list will include planets with no Solar System analog, such as the
recently discovered planets GJ1214b, whose density lies between that of
terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with
day-side temperature close to 3,000 K. As the number of detected
exoplanets is growing rapidly each year, and the mass and radius of
those detected steadily decreases, the target list will be constantly
adjusted to include the most interesting systems. We have baselined a
dispersive spectrograph design covering continuously the 0.4-16 mu m
spectral range in 6 channels (1 in the visible, 5 in the InfraRed),
which allows the spectral resolution to be adapted from several tens to
several hundreds, depending on the target brightness. The instrument
will be mounted behind a 1.5 m class telescope, passively cooled to 50
K, with the instrument structure and optics passively cooled to
\textbackslash{}u223c45 K. EChO will be placed in a grand halo orbit
around L2. This orbit, in combination with an optimised thermal shield
design, provides a highly stable thermal environment and a high degree
of visibility of the sky to observe repeatedly several tens of targets
over the year. Both the baseline and alternative designs have been
evaluated and no critical items with Technology Readiness Level (TRL)
less than 4-5 have been identified. We have also undertaken a
first-order cost and development plan analysis and find that EChO is
easily compatible with the ESA M-class mission framework.

EChO

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