EChO

Tinetti, Giovanna; Beaulieu, J. P.; Henning, Thomas; Meyer, Michael; Micela, G.; Ribas, I.; Stam, Daphné; Swain, Mark R.; Krause, O.; Ollivier, M.; Pace, E.; Swinyard, B.; Aylward, A. D.; Boekel, R. van; Coradini, A.; Encrenaz, Th.; Snellen, I. A. G.; Osorio, M. R. Zapatero; Bouwman, J.; Cho, J. Y.K.; Foresto, V. Coudé de; Guillot, T.; López-Morales, M.; Mueller-Wodarg, Ingo; Πάλλη, Ε.; Selsis, F.; Sozzetti, A.; Ade, Peter A. R.; Achilleos, N.; Adriani, A.; Agnor, C. B.; Afonso, C.; Prieto, C. Allende; Bakos, G. Á.; Barber, R. J.; Barlow, M. J.; Batista, V.; Bernath, Peter F.; Bézard, Bruno; Bordé, P.; Brown, Linda R.; Cassan, A.; Cavarroc, C.; Ciaravella, A.; Cockell, C.; Coustenis, A.; Danielski, Camilla; Decin, L.; Kok, Remco de; Demangeon, O.; Deroo, P.; Doel, P.; Drossart, P.; Fletcher, Leigh N.; Focardi, M.; Forget, F.; Fossey, S. J.; Fouqué, P.; Frith, J.; Galand, M.; Gaulme, P.; Hernández, J. I. González; Grasset, O.; Grassi, D.; Grenfell, John Lee; Griffin, M. J.; Griffith, C. A.; Grözinger, U.; Guêdel, M.; Guio, P.; Hainaut, Olivier; Hargreaves, Robert J.; Hauschildt, P. H.; Heng, Kevin; Heyrovsky, David; Hueso, R.; Irwin, Patrick; Kaltenegger, Lisa; Kervella, P.; Kipping, David; Koskinen, Tommi; Kovács, G.; Barbera, A. La; Lämmer, H.; Lellouch, E.; Leto, G.; Morales, M.; López‐Valverde, M. A.; López‐Puertas, M.; Lovis, C.; Maggio, A.; Maillard, J. P.; Maldonado, J.; Marquette, J. B.; Martín‐Torres, Javier; Maxted, P. F. L.; Miller, Steve; Molinari, S.; Montes, D.; Moro‐Martín, Amaya; Moses, J. I.; Mousis, O.; Tuong, Napoléon Nguyen; Nelson, Richard P.; Orton, Glenn S.; Pantin, E.; Pascale, Enzo; Pezzuto, S.; Pinfield, D. J.; Poretti, E.; Prinja, R. K.; Prisinzano, L.; Rees, Jon M.; Reiners, A.; Samuel, B.; Sánchez‐Lavega, A.; Sanz-Forcada, J.; Sasselov, Dimitar; Savini, G.; Sicardy, B.; Smith, Alan M.; Stixrude, Lars; Strazzulla, G.; Tennyson, Jonathan; Tessenyi, Marcell; Vasisht, Gautam; Vinatier, S.; Viti, S.; Waldmann, I. P.; White, G. J.; Widemann, Thomas; Wordsworth, R.; Yelle, R. V.; Yung, Yuk L.; Yurchenko, Sergei N.

doi:10.1007/s10686-012-9303-4

Cited by 111 publications

(45 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…4 (b), for instance, we assumed a 3 m telescope with a diffraction limited wavefront error of λ = 20 µm, and defocusing corresponding to a diffraction limited PSF size of λ = 20 µm and λ = 40 µm for X and Y direction at the geometric optics approximation, respectively. It should be noted that a 1 m class telescope has the potential to gather photons to detect O3 features in exoplanetary atmospheres [9,10] . So a 3 m class telescope can do it more efficiently.…”

Section: Discussion: Future Work In Development and Application To Anmentioning

confidence: 99%

Development of a Fine Grating on ZnS for a Wideband Spectral Disperser in Characterizing Exoplanets Using Space-Borne Telescopes

Enya

Sukegawa

Sugiyama

et al. 2014

AMR

View full text Add to dashboard Cite

We present the fabrication and optical testing of a fine grating on a ZnS substrate to be used as a wideband infrared spectral disperser and for which the primary application is measurement of the composition of the atmospheres of transiting exoplanets using space-borne infrared astronomical telescopes. A grating with a blaze angle of 2.1 deg. and pitch of 166.667 µm was constructed on a roughly flat 10 mm × 10 mm substrate with a maximum thickness of 1 mm. To obtain high accuracy, the sample was fabricated on a ZnS monocrystal using a high performance processing machine at Canon Inc. The surface roughness measured with a microscope interferometer was 2.6 nm rms. The shape of the fabricated grating edges was examined with a scanning electron microscope. The diffraction efficiency was evaluated by optical experiments at λ = 633 nm, 980 nm, and 1550 nm, and compared with the efficiencies calculated using a Fourier Modal Method. The results showed that the differences between the diffraction efficiencies obtained from experiment and by calculation were between just 0.9 % and 2.4 %. We concluded that the quality of the fabricated ZnS grating was sufficiently high to provide excellent diffraction efficiency for use in the infrared wavelength region. We also present the design of a spectral disperser in CdTe for future more advanced performance.

show abstract

Section: Discussion: Future Work In Development and Application To Anmentioning

confidence: 99%

Development of a Fine Grating on ZnS for a Wideband Spectral Disperser in Characterizing Exoplanets Using Space-Borne Telescopes

Enya

Sukegawa

Sugiyama

et al. 2014

AMR

View full text Add to dashboard Cite

show abstract

“…It also requires spectroscopy that is both accurate and sufficiently broadband to (i) determine the continuum formed by atmospheric temperatures and hazes and (ii) unambiguously detect the presence of molecular species. Space-borne spectroscopy from the UV to the infrared, potentially from the James Webb Space Telescope or the Exoplanet Characterisation Observatory (EChO) [96], could begin to validate some of the early findings on irradiated EGPs and extend coverage to planets with longer orbital periods and smaller stellar influences (see figure 3 for the range of T eq within reach of such transit studies). Based on the current statistics of targets suitable for EChO, up to 50% of the mission time could be devoted to the Jupiter class [96].…”

Section: Conclusion: An Ensemble Of Jupitersmentioning

confidence: 97%

“…Space-borne spectroscopy from the UV to the infrared, potentially from the James Webb Space Telescope or the Exoplanet Characterisation Observatory (EChO) [96], could begin to validate some of the early findings on irradiated EGPs and extend coverage to planets with longer orbital periods and smaller stellar influences (see figure 3 for the range of T eq within reach of such transit studies). Based on the current statistics of targets suitable for EChO, up to 50% of the mission time could be devoted to the Jupiter class [96]. Hot metallic Jupiters and silicate cloud Jupiters will be well sampled across all stellar types (the hot sample, T eq > 1800 K), but sulfide cloud Jupiters, cloud-free Jupiters with strong alkali lines (700 < T eq < 1800, the temperate sample) and water-cloud jovians (the cool sample) could also be targeted.…”

Section: Conclusion: An Ensemble Of Jupitersmentioning

confidence: 97%

Exploring the diversity of Jupiter-class planets

Fletcher

Irwin

Barstow

et al. 2014

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Of the 900+ confirmed exoplanets discovered since 1995 for which we have constraints on their mass (i.e. not including Kepler candidates), 75% have masses larger than Saturn (0.3 M J ), 53% are more massive than Jupiter and 67% are within 1 AU of their host stars. When Kepler candidates are included, Neptunesized giant planets could form the majority of the planetary population. And yet the term 'hot Jupiter' fails to account for the incredible diversity of this class of astrophysical object, which exists on a continuum of giant planets from the cool jovians of our own Solar System to the highly irradiated, tidally locked hot roasters. We review theoretical expectations for the temperatures, molecular composition and cloud properties of hydrogen-dominated Jupiterclass objects under a variety of different conditions. We discuss the classification schemes for these Jupiter-class planets proposed to date, including the implications for our own Solar System giant planets and the pitfalls associated with compositional classification at this early stage of exoplanetary spectroscopy. We discuss the range of planetary types described by previous authors, accounting for (i) thermochemical equilibrium expectations for cloud condensation and favoured chemical stability fields; (ii) the metallicity and formation mechanism for these giant planets; (iii) the importance of

show abstract

“…A more comprehensive review of this mission concept can be found in the EChO assessment study report, the "yellow book" 1 , and in [9]. The telescope has a 1.2 m aperture diameter which is passively cooled to less than 50 K. The radiation collected by the primary aperture feeds five spectroscopic channels covering continuously the required spectral band from 0.55 to 11 μm.…”

Section: Echo Instrument Designmentioning

confidence: 99%

“…A dedicated space mission addresses both problems. The Exoplanet Characterisation Observatory [9], EChO, was a proposed space mission for the ESA science programme (M3) which underwent a two year long study phase. EChO was designed for photometric stability over a spectral band spanning from the visible to the mid-IR part of the electromagnetic spectrum and EChOSim is the end-to-end software simulator developed to aid the instrument definition and to validate the mission concept.…”

Section: Introductionmentioning

confidence: 99%

EChOSim: The Exoplanet Characterisation Observatory software simulator

et al. 2015

Self Cite

View full text Add to dashboard Cite

EChOSim is the end-to-end time-domain simulator of the Exoplanet Characterisation Observatory (EChO) space mission. EChOSim has been developed to assess the capability of the EChO mission concept to detect and characterise the atmospheres of transiting exoplanets. Here we discuss the details of the EChOSim implementation and describe the models used to represent the instrument and to simulate the detection. Software simulators have assumed a central role in the design of new instrumentation and in assessing the level of systematics affecting the measurements of existing experiments. Thanks to its high modularity, EChOSim can simulate basic aspects of several existing and proposed spectrometers including instruments on the Hubble Space Telescope and Spitzer, ground-based and balloon-borne experiments . A discussion of different uses of EChOSim is given, including examples of simulations performed to assess the EChO mission.

show abstract

EChO

Cited by 111 publications

References 76 publications

Development of a Fine Grating on ZnS for a Wideband Spectral Disperser in Characterizing Exoplanets Using Space-Borne Telescopes

Development of a Fine Grating on ZnS for a Wideband Spectral Disperser in Characterizing Exoplanets Using Space-Borne Telescopes

Exploring the diversity of Jupiter-class planets

EChOSim: The Exoplanet Characterisation Observatory software simulator

Contact Info

Product

Resources

About