Author: "Tinetti, G." / Publication Year Range: Last 10 years - Searchworks@Jio Institute Digital Library Search Results

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121 results on '"Tinetti, G."'

1. ExoClock Project III: 450 new exoplanet ephemerides from ground and space observations

Author: Kokori, A., Tsiaras, A., Edwards, B., Jones, A., Pantelidou, G., Tinetti, G., Bewersdorff, L., Iliadou, A., Jongen, Y., Lekkas, G., Nastasi, A., Poultourtzidis, E., Sidiropoulos, C., Walter, F., Wünsche, A., Abraham, R., Agnihotri, V. K., Albanesi, R., Arce-Mansego, E., Arnot, D., Audejean, M., Aumasson, C., Bachschmidt, M., Baj, G., Barroy, P. R., Belinski, A. A., Bennett, D., Benni, P., Bernacki, K., Betti, L., Biagini, A., Bosch, P., Brandebourg, P., Brát, L., Bretton, M., Brincat, S. M., Brouillard, S., Bruzas, A., Bruzzone, A., Buckland, R. A., Caló, M., Campos, F., Carreno, A., Rodrigo, J. -A. Carrion, Casali, R., Casalnuovo, G., Cataneo, M., Chang, C. -M., Changeat, L., Chowdhury, V., Ciantini, R., Cilluffo, M., Coliac, J. -F., Conzo, G., Correa, M., Coulon, G., Crouzet, N., Crow, M. V., Curtis, I., Daniel, D., Dawes, S., Dauchet, B., Deldem, M., Deligeorgopoulos, D., Dransfield, G., Dymock, R., Eenmäe, T., Evans, P., Esseiva, N., Falco, C., Farfán, R. G., Fernández-Lajús, E., Ferratfiat, S., Ferreira, S. L., Ferretti, A., Fiołka, J., Fowler, M., Futcher, S. R., Gabellini, D., Gainey, T., Gaitan, J., Gajdoš, P., García-Sánchez, A., Garlitz, J., Gillier, C., Gison, C., Horta, F. Grau, Grivas, G., Gonzales, J., Gorshanov, D., Guerra, P., Guillot, T., Haswell, C. A., Haymes, T., Hentunen, V. -P., Hills, K., Hose, K., Humbert, T., Hurter, F., Hynek, T., Irzyk, M., Jacobsen, J., Jannetta, A. L., Johnson, K., Jóźwik-Wabik, P., Kaeouach, A. E., Kang, W., Kiiskinen, H., Kim, T., Kivila, Ü., Koch, B., Kolb, U., Kučáková, H., Lai, S. -P., Laloum, D., Lasota, S., Lewis, L. A., Liakos, G. -I., Libotte, F., Lopresti, C., Lomoz, F., Majewski, R., Malcher, A., Mallonn, M., Mannucci, M., Marchini, A., Mari, J. -M., Marino, A., Marino, G., Mario, J. -C., Marquette, J. -B., Martínez-Bravo, F. A., Mašek, M., Matassa, P., Michel, P., Michelet, J., Miller, M., Miny, E., Mollier, T., Molina, D., Monteleone, B., Montigiani, N., Morales-Aimar, M., Mortari, F., Morvan, M., Mugnai, L. V., Murawski, G., Naponiello, L., Naves, R., Naudin, J. -L., Néel, D., Neito, R., Neveu, S., Noschese, A., Öğmen, Y., Ohshima, O., Orbanic, Z., Pace, E. P., Pantacchini, C., Paschalis, N. I., Pereira, C., Peretto, I., Perroud, V., Phillips, M., Pintr, P., Pioppa, J. -B., Plazas, J., Poelarends, A. J., Popowicz, A., Purcell, J., Quinn, N., Raetz, M., Rees, D., Regembal, F., Rocchetto, M., Rocci, P. -F., Rockenbauer, M., Roth, R., Rousselot, L., Rubia, X., Ruocco, N., Russo, E., Salisbury, M., Salvaggio, F., Santos, A., Savage, J., Scaggiante, F., Sedita, D., Shadick, S., Silva, A. F., Sioulas, N., Školník, V., Smith, M., Smolka, M., Solmaz, A., Stanbury, N., Stouraitis, D., Tan, T. -G., Theusner, M., Thurston, G., Tifner, F. -P., Tomacelli, A., Tomatis, A., Trnka, J., Tylšar, M., Valeau, P., Vignes, J. -P., Villa, A., Sureda, A. Vives, Vora, K., Vrašťák, M., Walliang, D., Wenzel, B., Wright, D. E., Zambelli, R., Zhang, M., and Zíbar, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The ExoClock project has been created with the aim of increasing the efficiency of the Ariel mission. It will achieve this by continuously monitoring and updating the ephemerides of Ariel candidates over an extended period, in order to produce a consistent catalogue of reliable and precise ephemerides. This work presents a homogenous catalogue of updated ephemerides for 450 planets, generated by the integration of $\sim$18000 data points from multiple sources. These sources include observations from ground-based telescopes (ExoClock network and ETD), mid-time values from the literature and light-curves from space telescopes (Kepler/K2 and TESS). With all the above, we manage to collect observations for half of the post-discovery years (median), with data that have a median uncertainty less than one minute. In comparison with literature, the ephemerides generated by the project are more precise and less biased. More than 40\% of the initial literature ephemerides had to be updated to reach the goals of the project, as they were either of low precision or drifting. Moreover, the integrated approach of the project enables both the monitoring of the majority of the Ariel candidates (95\%), and also the identification of missing data. The dedicated ExoClock network effectively supports this task by contributing additional observations when a gap in the data is identified. These results highlight the need for continuous monitoring to increase the observing coverage of the candidate planets. Finally, the extended observing coverage of planets allows us to detect trends (TTVs - Transit Timing Variations) for a sample of 19 planets. All products, data, and codes used in this work are open and accessible to the wider scientific community., Comment: Recommended for publication to ApJS (reviewer's comments implemented). Main body: 13 pages, total: 77 pages, 7 figures, 7 tables. Data available at http://doi.org/10.17605/OSF.IO/P298N
Published: 2022
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2. ExoClock project II: A large-scale integrated study with 180 updated exoplanet ephemerides

Author: Kokori, A., Tsiaras, A., Edwards, B., Rocchetto, M., Tinetti, G., Bewersdorff, L., Jongen, Y., Lekkas, G., Pantelidou, G., Poultourtzidis, E., Wünsche, A., Aggelis, C., Agnihotri, V. K., Arena, C., Bachschmidt, M., Bennett, D., Benni, P., Bernacki, K., Besson, E., Betti, L., Biagini, A., Brandebourg, P., Bretton, M., Brincat, S. M., Caló, M., Campos, F., Casali, R., Ciantini, R., Crow, M. V., Dauchet, B., Dawes, S., Deldem, M., Deligeorgopoulos, D., Dymock, R., Eenmäe, T., Evans, P., Esseiva, N., Falco, C., Ferratfiat, S., Fowler, M., Futcher, S. R., Gaitan, J., Horta, F. Grau, Guerra, P., Hurter, F., Jones, A., Kang, W., Kiiskinen, H., Kim, T., Laloum, D., Lee, R., Lomoz, F., Lopresti, C., Mallonn, M., Mannucci, M., Marino, A., Mario, J. -C., Marquette, J. -B., Michelet, J., Miller, M., Mollier, T., Molina, D., Montigiani, N., Mortari, F., Morvan, M., Mugnai, L. V., Naponiello, L., Nastasi, A., Neito, R., Pace, E., Papadeas, P., Paschalis, N., Pereira, C., Perroud, V., Phillips, M., Pintr, P., Pioppa, J. -B., Popowicz, A., Raetz, M., Regembal, F., Rickard, K., Roberts, M., Rousselot, L., Rubia, X., Savage, J., Sedita, D., Shave-Wall, D., Sioulas, N., Školník, V., Smith, M., St-Gelais, D., Stouraitis, D., Strikis, I., Thurston, G., Tomacelli, A., Tomatis, A., Trevan, B., Valeau, P., Vignes, J. -P., Vora, K., Vrašťák, M., Walter, F., Wenzel, B., Wright, D. E., and Zíbar, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The ExoClock project is an inclusive, integrated, and interactive platform that was developed to monitor the ephemerides of the Ariel targets to increase the mission efficiency. The project makes the best use of all available resources, i.e., observations from ground telescopes, mid-time values from the literature and finally, observations from space instruments. Currently, the ExoClock network includes 280 participants with telescopes capable of observing 85\% of the currently known Ariel candidate targets. This work includes the results of $\sim$1600 observations obtained up to the 31st of December 2020 from the ExoClock network. These data in combination with $\sim$2350 mid-time values collected from the literature are used to update the ephemerides of 180 planets. The analysis shows that 40\% of the updated ephemerides will have an impact on future scheduling as either they have a significantly improved precision, or they have revealed biases in the old ephemerides. With the new observations, the observing coverage and rate for half of the planets in the sample has been doubled or more. Finally, from a population perspective, we identify that the differences in the 2028 predictions between the old and the new ephemerides have an STD that is double what is expected from gaussian uncertainties. These findings have implications for planning future observations, where we will need to account for drifts potentially greater than the prediction uncertainties. The updated ephemerides are open and accessible to the wider exoplanet community both from our Open Science Framework (OSF) repository and our website., Comment: 9 pages (47 with appendices and references), 8 figures, 2 tables. Submitted to ApJS. Revised based on the reviewer's comments
Published: 2021
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3. A Principal Component Analysis-based method to analyse high-resolution spectroscopic data

Author: Damiano, M., Micela, G., and Tinetti, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: High-Resolution Spectroscopy (HRS) has been used to study the composition and dynamics of exoplanetary atmospheres. In particular, the spectrometer CRIRES installed on the ESO-VLT has been used to record high-resolution spectra in the Near-IR of gaseous exoplanets. Here we present a new automatic pipeline to analyze CRIRES data-sets. Said pipeline is based on a novel use of Principal Component Analysis (PCA) and Cross-Correlation Function (CCF). The exoplanetary atmosphere is modeled with the $\tau$-REx code using opacities at high temperature from the ExoMol project. In this work, we tested our analysis tools on the detection of CO and H$_2$O in the atmospheres of the hot-Jupiters HD209458b and HD189733b. The results of our pipeline are in agreement with previous results in the literature and other techniques., Comment: 14 pages, 12 figures, 2 tables, published in ApJ
Published: 2019
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4. Near-IR transmission spectrum of HAT-P-32 b using HST/WFC3

Author: Damiano, M., Morello, G., Tsiaras, A., Zingales, T., and Tinetti, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report here the analysis of the near-infrared transit spectrum of the hot-Jupiter HAT-P-32b which was recorded with the Wide Field Camera 3 (WFC3) on-board the Hubble Space Telescope (HST). HAT-P-32b is one of the most inflated exoplanets discovered, making it an excellent candidate for transit spectroscopic measurements. To obtain the transit spectrum, we have adopted different analysis methods, both parametric and non parametric (Independent Component Analysis, ICA), and compared the results. The final spectra are all consistent within 0.5$\sigma$. The uncertainties obtained with ICA are larger than those obtained with the parametric method by a factor $\sim$1.6 - 1.8. This difference is the trade-off for higher objectivity due to the lack of any assumption about the instrument systematics compared to the parametric approach. The ICA error-bars are therefore worst-case estimates. To interpret the spectrum of HAT-P-32b, we used T-Rex, our fully Bayesian spectral retrieval code. As for other hot-Jupiters, the results are consistent with the presence of water vapor ($\log{\text{H}_2\text{O}} = -3.45_{-1.65}^{+1.83}$), clouds (top pressure between 5.16 and 1.73 bar). Spectroscopic data over a broader wavelength range will be needed to de-correlate the mixing ratio of water vapor from clouds and identify other possible molecular species in the atmosphere of HAT-P-32b., Comment: 9 Pages, 5 Tables, 4 Figures, published in AJ
Published: 2018
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5. Observability of temperate exoplanets with Ariel

Author: Encrenaz, T., Coustenis, A., Gilli, G., Marcq, E., Molaverdikhani, K., Mugnai, L. V., Ollivier, M., and Tinetti, G.
Published: 2022
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6. The ARIEL Instrument Control Unit design for the M4 Mission Selection Review of the ESA's Cosmic Vision Program

Author: Focardi, M., Pace, E., Farina, M., Di Giorgio, A. M., Ferrer, J. Colome, Ribas, I., Roig, C. Sierra, Bote, L. Gesa, Morales, J. C., Amiaux, J., Cara, C., Augures, J. L., Pascale, E., Morgante, G., Da Deppo, V., Pancrazzi, M., Noce, V., Pezzuto, S., Freriks, M., Zwart, F., Bishop, G., Middleton, K., Eccleston, P., Micela, G., and Tinetti, G.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Atmospheric Remote-sensing Infrared Exoplanet Large-survey mission (ARIEL) is one of the three present candidates for the ESA M4 (the fourth medium mission) launch opportunity. The proposed Payload will perform a large unbiased spectroscopic survey from space concerning the nature of exoplanets atmospheres and their interiors to determine the key factors affecting the formation and evolution of planetary systems. ARIEL will observe a large number (>500) of warm and hot transiting gas giants, Neptunes and super-Earths around a wide range of host star types, targeting planets hotter than 600 K to take advantage of their well-mixed atmospheres. It will exploit primary and secondary transits spectroscopy in the 1.2-8 um spectral range and broad-band photometry in the optical and Near IR (NIR). The main instrument of the ARIEL Payload is the IR Spectrometer (AIRS) providing low-resolution spectroscopy in two IR channels: Channel 0 (CH0) for the 1.95-3.90 um band and Channel 1 (CH1) for the 3.90-7.80 um range. It is located at the intermediate focal plane of the telescope and common optical system and it hosts two IR sensors and two cold front-end electronics (CFEE) for detectors readout, a well defined process calibrated for the selected target brightness and driven by the Payload's Instrument Control Unit (ICU)., Comment: Experimental Astronomy, Special Issue on ARIEL, (2017)
Published: 2017
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7. A population study of gaseous exoplanets

Author: Tsiaras, A., Waldmann, I. P., Zingales, T., Rocchetto, M., Morello, G., Damiano, M., Karpouzas, K., Tinetti, G., McKemmish, L. K., Tennyson, J., and Yurchenko, S. N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present here the analysis of 30 gaseous extrasolar planets, with temperatures between 600 and 2400 K and radii between 0.35 and 1.9 $R_\mathrm{Jup}$. The quality of the HST/WFC3 spatially scanned data combined with our specialized analysis tools allow us to study the largest and most self-consistent sample of exoplanetary transmission spectra to date and examine the collective behavior of warm and hot gaseous planets rather than isolated case-studies. We define a new metric, the Atmospheric Detectability Index (ADI) to evaluate the statistical significance of an atmospheric detection and find statistically significant atmospheres around 16 planets out of the 30 analysed. For most of the Jupiters in our sample, we find the detectability of their atmospheres to be dependent on the planetary radius but not on the planetary mass. This indicates that planetary gravity plays a secondary role in the state of gaseous planetary atmospheres. We detect the presence of water vapour in all of the statistically detectable atmospheres, and we cannot rule out its presence in the atmospheres of the others. In addition, TiO and/or VO signatures are detected with 4$\sigma$ confidence in WASP-76 b, and they are most likely present in WASP-121 b. We find no correlation between expected signal-to-noise and atmospheric detectability for most targets. This has important implications for future large-scale surveys., Comment: 14 pages, 12 figures, 3 tables, published in AJ
Published: 2017
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8. Exploring Biases of Atmospheric Retrievals in Simulated JWST Transmission Spectra of Hot Jupiters

Author: Rocchetto, M., Waldmann, I. P., Venot, O., Lagage, P. -O., and Tinetti, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: With a scheduled launch in October 2018, the James Webb Space Telescope (JWST) is expected to revolutionise the field of atmospheric characterization of exoplanets. The broad wavelength coverage and high sensitivity of its instruments will allow us to extract far more information from exoplanet spectra than what has been possible with current observations. In this paper, we investigate whether current retrieval methods will still be valid in the era of JWST, exploring common approximations used when retrieving transmission spectra of hot Jupiters. To assess biases, we use 1D photochemical models to simulate typical hot Jupiter cloud-free atmospheres and generate synthetic observations for a range of carbon-to-oxygen ratios. Then, we retrieve these spectra using TauREx, a Bayesian retrieval tool, using two methodologies: one assuming an isothermal atmosphere, and one assuming a parametrized temperature profile. Both methods assume constant-with-altitude abundances. We found that the isothermal approximation biases the retrieved parameters considerably, overestimating the abundances by about one order of magnitude. The retrieved abundances using the parametrized profile are usually within one sigma of the true state, and we found the retrieved uncertainties to be generally larger compared to the isothermal approximation. Interestingly, we found that using the parametrized temperature profile we could place tight constraints on the temperature structure. This opens the possibility to characterize the temperature profile of the terminator region of hot Jupiters. Lastly, we found that assuming a constant-with-altitude mixing ratio profile is a good approximation for most of the atmospheres under study., Comment: 16 pages, 10 figures. Accepted for publication in The Astrophysical Journal
Published: 2016
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9. Detection of an atmosphere around the super-Earth 55 Cancri e

Author: Tsiaras, A., Rocchetto, M., Waldmann, I. P., Venot, O., Varley, R., Morello, G., Damiano, M., Tinetti, G., Barton, E. J., Yurchenko, S. N., and Tennyson, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the analysis of two new spectroscopic observations of the super-Earth 55 Cancri e, in the near infrared, obtained with the WFC3 camera onboard the HST. 55 Cancri e orbits so close to its parent star, that temperatures much higher than 2000 K are expected on its surface. Given the brightness of 55 Cancri, the observations were obtained in scanning mode, adopting a very long scanning length and a very high scanning speed. We use our specialized pipeline to take into account systematics introduced by these observational parameters when coupled with the geometrical distortions of the instrument. We measure the transit depth per wavelength channel with an average relative uncertainty of 22 ppm per visit and find modulations that depart from a straight line model with a 6$\sigma$ confidence level. These results suggest that 55 Cancri e is surrounded by an atmosphere, which is probably hydrogen-rich. Our fully Bayesian spectral retrieval code, T-REx, has identified HCN to be the most likely molecular candidate able to explain the features at 1.42 and 1.54 $\mu$m. While additional spectroscopic observations in a broader wavelength range in the infrared will be needed to confirm the HCN detection, we discuss here the implications of such result. Our chemical model, developed with combustion specialists, indicates that relatively high mixing ratios of HCN may be caused by a high C/O ratio. This result suggests this super-Earth is a carbon-rich environment even more exotic than previously thought., Comment: 10 pages, 10 figures, 4 tables, Accepted for publication in ApJ
Published: 2015
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10. A new approach to analysing HST spatial scans: the transmission spectrum of HD 209458 b

Author: Tsiaras, A., Waldmann, I. P., Rocchetto, M., Varley, R., Morello, G., Damiano, M., and Tinetti, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Wide Field Camera 3 (WFC3) on Hubble Space Telescope (HST) is currently one of the most widely used instruments for observing exoplanetary atmospheres, especially with the use of the spatial scanning technique. An increasing number of exoplanets have been studied using this technique as it enables the observation of bright targets without saturating the sensitive detectors. In this work we present a new pipeline for analyzing the data obtained with the spatial scanning technique, starting from the raw data provided by the instrument. In addition to commonly used correction techniques, we take into account the geometric distortions of the instrument, whose impact may become important when combined to the scanning process. Our approach can improve the photometric precision for existing data and also push further the limits of the spatial scanning technique, as it allows the analysis of even longer spatial scans. As an application of our method and pipeline, we present the results from a reanalysis of the spatially scanned transit spectrum of HD 209458 b. We calculate the transit depth per wavelength channel with an average relative uncertainty of 40 ppm. We interpret the final spectrum with T-Rex, our fully Bayesian spectral retrieval code, which confirms the presence of water vapor and clouds in the atmosphere of HD 209458 b. The narrow wavelength range limits our ability to disentangle the degeneracies between the fitted atmospheric parameters. Additional data over a broader spectral range are needed to address this issue., Comment: 13 pages, 15 figures, 7 tables, Accepted for publication in ApJ
Published: 2015
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11. ARIEL payload STOP analysis: a view on the in-flight operational cases for the telescope assembly

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Brucalassi, A., Araiza-Durán, J. A., Tozzi, A., Galy, C., Perez, A. G., Caldwell, A., Morgante, G., Bruzzi, D., Caldwell, M., Chioetto, P., Eccleston, P., Fernandez Soler, A. J., Ferruzzi, D., Gottini, D., Lilli, R., Micela, G., Pace, E., Pascale, E., Perez Alvarez, J., Piazzolla, R., Picchi, P., Preti, G., Salatti, M., Scippa, A., Tinetti, G., and Zuppella, P.
Published: 2024
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12. Aluminum based large telescopes: the ARIEL mission case

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Picchi, P., Tozzi, A., Brucalassi, A., Araiza, Antonio J., Pace, E., Chioetto, P., Zuppella, P., Scippa, A., Lilli, R., Gottini, D., Alvarez, J., García, A., Soler, Alejandro J., D'Anca, F., Guerriero, E., Del Vecchio, C., Falcini, G., Carbonaro, L., Eccleston, P., Caldwell, A., Ferruzzi, D., Malaguti, G., Micela, G., Pascale, E., Bocchieri, A., Preti, G., Piazzolla, R., Salatti, M., Brienza, D., Tommasi, E., Tinetti, G., Vernani, D., and Morgante, G.
Published: 2024
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13. Revisiting Spitzer transit observations with Independent Component Analysis: new results for the GJ436 system

Author: Morello, G., Waldmann, I. P., Tinetti, G., Howarth, I. D., Micela, G., and Allard, F.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We analyzed four Spitzer/IRAC observations at 3.6 and 4.5 {\mu}m of the primary transit of the exoplanet GJ436b, by using blind source separation techniques. These observations are important to investigate the atmospheric composition of the planet GJ436b. Previous analyses claimed strong inter-epoch variations of the transit parameters due to stellar variability, casting doubts on the possibility to extract conclusively an atmospheric signal; those analyses also reported discrepant results, hence the necessity of this reanalysis. The method we used has been proposed in Morello et al. (2014) to analyze 3.6 {\mu}m transit light-curves of the hot Jupiter HD189733b; it performes an Independent Component Analysis (ICA) on a set of pixel-light-curves, i.e. time series read by individual pixels, from the same photometric observation. Our method only assumes the independence of instrumental and astrophysical signals, and therefore guarantees a higher degree of objectivity compared to parametric detrending techniques published in the literature. The datasets we analyzed in this paper represent a more challenging test compared to the previous ones. Contrary to previous results reported in the literature, our results (1) do not support any detectable inter-epoch variations of orbital and stellar parameters, (2) are photometrically stable at the level 10e-4 in the IR, and (3) the transit depth measurements at the two wavelengths are consistent within 1{\sigma}. We also (4) detect a possible transit duration variation (TDV) of 80 s (2 {\sigma} significance level), that has not been pointed out in the literature, and (5) confirm no transit timing variations (TTVs) >30 s., Comment: accepted for publication in The Astrophysical Journal
Published: 2015
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14. Transit spectroscopy of temperate Jupiters with ARIEL: a feasibility study

Author: Encrenaz, Thérèse, Tinetti, G., and Coustenis, A.
Published: 2018
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15. The ARIEL Instrument Control Unit design: For the M4 Mission Selection Review of the ESA’s Cosmic Vision Program

Author: Focardi, M., Pace, E., Farina, M., Di Giorgio, A. M., Ferrer, J. Colomé, Ribas, I., Roig, C. Sierra, Bote, L. Gesa, Morales, J. C., Amiaux, J., Cara, C., Augurés, J. L., Pascale, E., Morgante, G., Da Deppo, V., Pancrazzi, M., Noce, V., Pezzuto, S., Frericks, M., Zwart, F., Bishop, G., Middleton, K., Eccleston, P., Micela, G., and Tinetti, G.
Published: 2018
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16. ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations

Author: Kokori, A., primary, Tsiaras, A., additional, Edwards, B., additional, Jones, A., additional, Pantelidou, G., additional, Tinetti, G., additional, Bewersdorff, L., additional, Iliadou, A., additional, Jongen, Y., additional, Lekkas, G., additional, Nastasi, A., additional, Poultourtzidis, E., additional, Sidiropoulos, C., additional, Walter, F., additional, Wünsche, A., additional, Abraham, R., additional, Agnihotri, V. K., additional, Albanesi, R., additional, Arce-Mansego, E., additional, Arnot, D., additional, Audejean, M., additional, Aumasson, C., additional, Bachschmidt, M., additional, Baj, G., additional, Barroy, P. R., additional, Belinski, A. A., additional, Bennett, D., additional, Benni, P., additional, Bernacki, K., additional, Betti, L., additional, Biagini, A., additional, Bosch, P., additional, Brandebourg, P., additional, Brát, L., additional, Bretton, M., additional, Brincat, S. M., additional, Brouillard, S., additional, Bruzas, A., additional, Bruzzone, A., additional, Buckland, R. A., additional, Caló, M., additional, Campos, F., additional, Carreño, A., additional, Carrion Rodrigo, J. A., additional, Casali, R., additional, Casalnuovo, G., additional, Cataneo, M., additional, Chang, C.-M., additional, Changeat, L., additional, Chowdhury, V., additional, Ciantini, R., additional, Cilluffo, M., additional, Coliac, J.-F., additional, Conzo, G., additional, Correa, M., additional, Coulon, G., additional, Crouzet, N., additional, Crow, M. V., additional, Curtis, I. A., additional, Daniel, D., additional, Dauchet, B., additional, Dawes, S., additional, Deldem, M., additional, Deligeorgopoulos, D., additional, Dransfield, G., additional, Dymock, R., additional, Eenmäe, T., additional, Esseiva, N., additional, Evans, P., additional, Falco, C., additional, Farfán, R. G., additional, Fernández-Lajús, E., additional, Ferratfiat, S., additional, Ferreira, S. L., additional, Ferretti, A., additional, Fiołka, J., additional, Fowler, M., additional, Futcher, S. R., additional, Gabellini, D., additional, Gainey, T., additional, Gaitan, J., additional, Gajdoš, P., additional, García-Sánchez, A., additional, Garlitz, J., additional, Gillier, C., additional, Gison, C., additional, Gonzales, J., additional, Gorshanov, D., additional, Grau Horta, F., additional, Grivas, G., additional, Guerra, P., additional, Guillot, T., additional, Haswell, C. A., additional, Haymes, T., additional, Hentunen, V.-P., additional, Hills, K., additional, Hose, K., additional, Humbert, T., additional, Hurter, F., additional, Hynek, T., additional, Irzyk, M., additional, Jacobsen, J., additional, Jannetta, A. L., additional, Johnson, K., additional, Jóźwik-Wabik, P., additional, Kaeouach, A. E., additional, Kang, W., additional, Kiiskinen, H., additional, Kim, T., additional, Kivila, Ü., additional, Koch, B., additional, Kolb, U., additional, Kučáková, H., additional, Lai, S.-P., additional, Laloum, D., additional, Lasota, S., additional, Lewis, L. A., additional, Liakos, G.-I., additional, Libotte, F., additional, Lomoz, F., additional, Lopresti, C., additional, Majewski, R., additional, Malcher, A., additional, Mallonn, M., additional, Mannucci, M., additional, Marchini, A., additional, Mari, J.-M., additional, Marino, A., additional, Marino, G., additional, Mario, J.-C., additional, Marquette, J.-B., additional, Martínez-Bravo, F. A., additional, Mašek, M., additional, Matassa, P., additional, Michel, P., additional, Michelet, J., additional, Miller, M., additional, Miny, E., additional, Molina, D., additional, Mollier, T., additional, Monteleone, B., additional, Montigiani, N., additional, Morales-Aimar, M., additional, Mortari, F., additional, Morvan, M., additional, Mugnai, L. V., additional, Murawski, G., additional, Naponiello, L., additional, Naudin, J.-L., additional, Naves, R., additional, Néel, D., additional, Neito, R., additional, Neveu, S., additional, Noschese, A., additional, Öğmen, Y., additional, Ohshima, O., additional, Orbanic, Z., additional, Pace, E. P., additional, Pantacchini, C., additional, Paschalis, N. I., additional, Pereira, C., additional, Peretto, I., additional, Perroud, V., additional, Phillips, M., additional, Pintr, P., additional, Pioppa, J.-B., additional, Plazas, J., additional, Poelarends, A. J., additional, Popowicz, A., additional, Purcell, J., additional, Quinn, N., additional, Raetz, M., additional, Rees, D., additional, Regembal, F., additional, Rocchetto, M., additional, Rocci, P.-F., additional, Rockenbauer, M., additional, Roth, R., additional, Rousselot, L., additional, Rubia, X., additional, Ruocco, N., additional, Russo, E., additional, Salisbury, M., additional, Salvaggio, F., additional, Santos, A., additional, Savage, J., additional, Scaggiante, F., additional, Sedita, D., additional, Shadick, S., additional, Silva, A. F., additional, Sioulas, N., additional, Školník, V., additional, Smith, M., additional, Smolka, M., additional, Solmaz, A., additional, Stanbury, N., additional, Stouraitis, D., additional, Tan, T.-G., additional, Theusner, M., additional, Thurston, G., additional, Tifner, F. P., additional, Tomacelli, A., additional, Tomatis, A., additional, Trnka, J., additional, Tylšar, M., additional, Valeau, P., additional, Vignes, J.-P., additional, Villa, A., additional, Sureda, A. Vives, additional, Vora, K., additional, Vrašt’ák, M., additional, Walliang, D., additional, Wenzel, B., additional, Wright, D. E., additional, Zambelli, R., additional, Zhang, M., additional, and Zíbar, M., additional
Published: 2023
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17. Thermal control system of the Exoplanet Characterisation Observatory Payload: design and predictions

Author: Morgante, G., Terenzi, L., Eccleston, P., Bradshaw, T., Crook, M., Linder, M., Hunt, T., Winter, B., Focardi, M., Malaguti, G., Micela, G., Pace, E., and Tinetti, G.
Published: 2015
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18. EChOSim: The Exoplanet Characterisation Observatory software simulator

Author: Pascale, E., Waldmann, I. P., MacTavish, C. J., Papageorgiou, A., Amaral-Rogers, A., Varley, R., Coudé du Foresto, V., Griffin, M. J., Ollivier, M., Sarkar, S., Spencer, L., Swinyard, B. M., Tessenyi, M., and Tinetti, G.
Published: 2015
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19. Brown dwarf characterization with EChO

Author: Morales, J. C., Beaulieu, J.-P., Coudé du Foresto, V., Drossart, P., and Tinetti, G.
Published: 2015
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20. Generation of an optimal target list for the exoplanet characterisation observatory (EChO)

Author: Varley, R., Waldmann, I., Pascale, E., Tessenyi, M., Hollis, M., Morales, J. C., Tinetti, G., Swinyard, B., Deroo, P., Ollivier, M., and Micela, G.
Published: 2015
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21. Transit spectroscopy of exoplanets from space: how to optimize the wavelength coverage and spectral resolving power

Author: Encrenaz, T., Tinetti, G., Tessenyi, M., Drossart, P., Hartogh, P., and Coustenis, A.
Published: 2015
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22. A Comparison of Chemical Models of Exoplanet Atmospheres Enabled by TauREx 3.1

Author: Al-Refaie, A. F., primary, Changeat, Q., additional, Venot, O., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2022
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23. Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse

Author: Changeat, Q., primary, Edwards, B., additional, Al-Refaie, A. F., additional, Tsiaras, A., additional, Skinner, J. W., additional, Cho, J. Y. K., additional, Yip, K. H., additional, Anisman, L., additional, Ikoma, M., additional, Bieger, M. F., additional, Venot, O., additional, Shibata, S., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2022
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24. ExoClock Project. II. A Large-scale Integrated Study with 180 Updated Exoplanet Ephemerides

Author: Kokori, A., primary, Tsiaras, A., additional, Edwards, B., additional, Rocchetto, M., additional, Tinetti, G., additional, Bewersdorff, L., additional, Jongen, Y., additional, Lekkas, G., additional, Pantelidou, G., additional, Poultourtzidis, E., additional, Wünsche, A., additional, Aggelis, C., additional, Agnihotri, V. K., additional, Arena, C., additional, Bachschmidt, M., additional, Bennett, D., additional, Benni, P., additional, Bernacki, K., additional, Besson, E., additional, Betti, L., additional, Biagini, A., additional, Brandebourg, P., additional, Bretton, M., additional, Brincat, S. M., additional, Caló, M., additional, Campos, F., additional, Casali, R., additional, Ciantini, R., additional, Crow, M. V., additional, Dauchet, B., additional, Dawes, S., additional, Deldem, M., additional, Deligeorgopoulos, D., additional, Dymock, R., additional, Eenmäe, T., additional, Evans, P., additional, Esseiva, N., additional, Falco, C., additional, Ferratfiat, S., additional, Fowler, M., additional, Futcher, S. R., additional, Gaitan, J., additional, Horta, F. Grau, additional, Guerra, P., additional, Hurter, F., additional, Jones, A., additional, Kang, W., additional, Kiiskinen, H., additional, Kim, T., additional, Laloum, D., additional, Lee, R., additional, Lomoz, F., additional, Lopresti, C., additional, Mallonn, M., additional, Mannucci, M., additional, Marino, A., additional, Mario, J.-C., additional, Marquette, J.-B., additional, Michelet, J., additional, Miller, M., additional, Mollier, T., additional, Molina, D., additional, Montigiani, N., additional, Mortari, F., additional, Morvan, M., additional, Mugnai, L. V., additional, Naponiello, L., additional, Nastasi, A., additional, Neito, R., additional, Pace, E., additional, Papadeas, P., additional, Paschalis, N., additional, Pereira, C., additional, Perroud, V., additional, Phillips, M., additional, Pintr, P., additional, Pioppa, J.-B., additional, Popowicz, A., additional, Raetz, M., additional, Regembal, F., additional, Rickard, K., additional, Roberts, M., additional, Rousselot, L., additional, Rubia, X., additional, Savage, J., additional, Sedita, D., additional, Shave-Wall, D., additional, Sioulas, N., additional, Školník, V., additional, Smith, M., additional, St-Gelais, D., additional, Stouraitis, D., additional, Strikis, I., additional, Thurston, G., additional, Tomacelli, A., additional, Tomatis, A., additional, Trevan, B., additional, Valeau, P., additional, Vignes, J.-P., additional, Vora, K., additional, Vrašťák, M., additional, Walter, F., additional, Wenzel, B., additional, Wright, D. E., additional, and Zíbar, M., additional
Published: 2022
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25. Thermal control system of the Exoplanet Characterisation Observatory Payload: design and predictions

Author: Morgante, G., primary, Terenzi, L., additional, Eccleston, P., additional, Bradshaw, T., additional, Crook, M., additional, Linder, M., additional, Hunt, T., additional, Winter, B., additional, Focardi, M., additional, Malaguti, G., additional, Micela, G., additional, Pace, E., additional, and Tinetti, G., additional
Published: 2015
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26. Generation of an optimal target list for the exoplanet characterisation observatory (EChO)

Author: Varley, R., primary, Waldmann, I., additional, Pascale, E., additional, Tessenyi, M., additional, Hollis, M., additional, Morales, J. C., additional, Tinetti, G., additional, Swinyard, B., additional, Deroo, P., additional, Ollivier, M., additional, and Micela, G., additional
Published: 2015
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27. Brown dwarf characterization with EChO

Author: Morales, J. C., primary, Beaulieu, J. P., additional, du Foresto, V. Coudé, additional, Drossart, P., additional, and Tinetti, G., additional
Published: 2015
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28. Observability of temperate exoplanets with Ariel

Author: Encrenaz, T., primary, Coustenis, A., additional, Gilli, G., additional, Marcq, E., additional, Molaverdikhani, K., additional, Mugnai, L. V., additional, Ollivier, M., additional, and Tinetti, G., additional
Published: 2021
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29. TauREx 3: A Fast, Dynamic, and Extendable Framework for Retrievals

Author: Al-Refaie, A. F., primary, Changeat, Q., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2021
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30. An Exploration of Model Degeneracies with a Unified Phase Curve Retrieval Analysis: The Light and Dark Sides of WASP-43 b

Author: Changeat, Q., primary, Al-Refaie, A. F., additional, Edwards, B., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2021
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31. Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

Author: Turrini, D., primary, Schisano, E., additional, Fonte, S., additional, Molinari, S., additional, Politi, R., additional, Fedele, D., additional, Panić, O., additional, Kama, M., additional, Changeat, Q., additional, and Tinetti, G., additional
Published: 2021
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32. Consolidation of surface charging analyses on the Ariel payload dielectrics in the early transfer orbit and L2 space environments

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Focardi, M., Michelagnoli, M., Pudney, M., Renouf, I., Merola, P., Carbonaro, L., Noce, V., Vela Nunez, M., Bolli, P., Nesti, R., Chiarucci, S., Dinuzzi, G., Tommasi, E., De Persio, F., Salatti, M., Brienza, D., Piazzolla, R., Morgante, G., Pace, E., Preti, G., Micela, G., Malaguti, G., Caldwell, A., Eccleston, P., and Tinetti, G.
Published: 2024
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33. The Ariel payload electrical and electronic architecture: a summary of the current design and implementation status

Author: Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Focardi, M., Noce, V., Merola, P., Di Giorgio, A., Ligori, S., Corcione, L., Capobianco, V., Bonino, D., V. Nunez, M., Chiarucci, S., Medinaceli, E., Auricchio, N., Farina, M., Giusi, G., Russi, A., Tortora, A., Serafini, L., Pannocchia, A., Giglio, G., Passerai, M., Verna, M., Del Vecchio Blanco, C., Morgante, G., Ateca, J., Bosch, J., Carmona, M., Casas, A., Gomez, J. M., Lopez, P., Marti, L., Royo, A., Ruiz, O., Serre, C., Skup, K. R., Rutkowski, K., Sobiecki, M., Ber, K., Sobolewski, M., Thernstrom, N., Winklera, M., Ciarka, M., Berthé, M., Cara, C., Fontignie, J., Martignac, J., Kaszubiak, G., Leguay, N., Grimoldi, R., Ober, G., Goullioud, R., Holmes, W., Swain, M., Vasisht, G., Cho, H., Mulder, J., Allen, G. D., Runkle, A., Guzman, E., Weilert, M., Weber, C., Tan, P., Morales, J., Hunacek, J., Rieck, A., Bolduc, A., Aaron, K., Turner, A., Krohn, B., Lew, M., Cillis, A., Foltz, R., Hewagama, T., Loose, M., Crook, M., Hills, M., Gilley, G., Mäkinen, S., Caldwell, A., Bishop, G., Desjonqueres, L., Drummond, R., Eccleston, P., Davidson, A., Umesh, P., Pace, E., Preti, G., Micela, G., Malaguti, G., and Tinetti, G.
Published: 2024
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34. MARVEL, a four-telescope array for high-precision radial-velocity monitoring

Author: Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Raskin, G., Schwab, C., Vandenbussche, B., de Ridder, J., Lanthermann, C., Padilla, J. Pérez, Tkachenko, A., Sana, H., Royer, P., Prins, S., Decin, L., Defrère, D., Pember, J., Atkinson, D., Glasse, A., Pollacco, D., Tinetti, G., Güdel, M., Stürmer, J., Ribas, I., Brandeker, A., Buchhave, L., Halverson, S., Avila, G., Morren, J., van Winckel, H., Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Raskin, G., Schwab, C., Vandenbussche, B., de Ridder, J., Lanthermann, C., Padilla, J. Pérez, Tkachenko, A., Sana, H., Royer, P., Prins, S., Decin, L., Defrère, D., Pember, J., Atkinson, D., Glasse, A., Pollacco, D., Tinetti, G., Güdel, M., Stürmer, J., Ribas, I., Brandeker, A., Buchhave, L., Halverson, S., Avila, G., Morren, J., and van Winckel, H.
Abstract: Since the first discovery of a planet outside of our Solar System in 1995, exoplanet research has shifted from detecting to characterizing worlds around other stars. The TESS (NASA, launched 2019) and PLATO mission (ESA, planned launch 2026) will find and constrain the size of thousands of exoplanets around bright stars all over the sky. Radial velocity measurements are needed to characterize the orbit and mass, and complete the picture of densities and composition of the exoplanet systems found. The Ariel mission (ESA, planned launch 2028) will characterize exoplanet atmospheres with infrared spectroscopy. Characterization of stellar activity using optical spectroscopy from the ground is key to retrieve the spectral footprint of the planetary atmosphere in Ariel's spectra. To enable the scientific harvest of the TESS, PLATO and Ariel space missions, we plan to install MARVEL as an extension of the existing Mercator Telescope at the Roque De Los Muchachos Observatory on La Palma (SPAIN). MARVEL consists of an array of four 80 cm telescopes linked through optical fibers to a single high-resolution echelle spectrograph, optimized for extreme-precision radial velocity measurements. It can observe the radial velocities of four different stars simultaneously or, alternatively, combine the flux from four telescopes pointing to a single faint target in one spectrum. MARVEL is constructed by a KU Leuven (Belgium) led collaboration, with contributions from the UK, Austria, Australia, Sweden, Denmark and Spain. In this paper, we present the MARVEL instrument with special focus on the optical design and expected performance of the spectrograph, and report on the status of the project.
Published: 2020

35. KELT-11 b: Abundances of Water and Constraints on Carbon-bearing Molecules from the Hubble Transmission Spectrum

Author: Changeat, Q., primary, Edwards, B., additional, Al-Refaie, A. F., additional, Morvan, M., additional, Tsiaras, A., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2020
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36. Integrating Light Curve and Atmospheric Modeling of Transiting Exoplanets

Author: Yip, K. H., primary, Tsiaras, A., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2020
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37. Alfnoor: A Retrieval Simulation of the Ariel Target List

Author: Changeat, Q., primary, Al-Refaie, A., additional, Mugnai, L. V., additional, Edwards, B., additional, Waldmann, I. P., additional, Pascale, E., additional, and Tinetti, G., additional
Published: 2020
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38. Impact of Planetary Mass Uncertainties on Exoplanet Atmospheric Retrievals

Author: Changeat, Q., primary, Keyte, L., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2020
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39. Toward a More Complex Description of Chemical Profiles in Exoplanet Retrievals: A Two-layer Parameterization

Author: Changeat, Q., primary, Edwards, B., additional, Waldmann, I. P., additional, and Tinetti, G., additional
Published: 2019
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40. The transiting exoplanet community early release science program for JWST

Author: Bean, JL, Stevenson, KB, Batalha, NM, Berta-Thompson, Z, Kreidberg, L, Crouzet, N, Benneke, B, Line, MR, Sing, DK, Wakeford, HR, Knutson, HA, Kempton, EMR, Désert, JM, Crossfield, I, Batalha, NE, De Wit, J, Parmentier, V, Harrington, J, Moses, JI, Lopez-Morales, M, Alam, MK, Blecic, J, Bruno, G, Carter, AL, Chapman, JW, Decin, L, Dragomir, D, Evans, TM, Fortney, JJ, Fraine, JD, Gao, P, Muñoz, AG, Gibson, NP, Goyal, JM, Heng, K, Hu, R, Kendrew, S, Kilpatrick, BM, Krick, J, Lagage, PO, Lendl, M, Louden, T, Madhusudhan, N, Mandell, AM, Mansfield, M, May, EM, Morello, G, Morley, CV, Nikolov, N, Redfield, S, Roberts, JE, Schlawin, E, Spake, JJ, Todorov, KO, Tsiaras, A, Venot, O, Waalkes, WC, Wheatley, PJ, Zellem, RT, Angerhausen, D, Barrado, D, Carone, L, Casewell, SL, Cubillos, PE, Damiano, M, Borro, MDV, Drummond, B, Edwards, B, Endl, M, Espinoza, N, France, K, Gizis, JE, Greene, TP, Henning, TK, Hong, Y, Ingalls, JG, Iro, N, Irwin, PGJ, Kataria, T, Lahuis, F, Leconte, J, Lillo-Box, J, Lines, S, Lothringer, JD, Mancini, L, Marchis, F, Mayne, N, Palle, E, Rauscher, E, Roudier, G, Shkolnik, EL, Southworth, J, Swain, MR, Taylor, J, Teske, J, Tinetti, G, Tremblin, P, Tucker, GS, Boekel, RV, Waldmann, IP, Bean, JL [0000-0003-4733-6532], and Apollo - University of Cambridge Repository
Subjects: planets and satellites: atmospheres, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, methods: observational, planets and satellites: individual (WASP-79b, WASP-43b, WASP-18b)
Abstract: The James Webb Space Telescope (JWST) presents the opportunity to transform our understanding of planets and the origins of life by revealing the atmospheric compositions, structures, and dynamics of transiting exoplanets in unprecedented detail. However, the high-precision, time-series observations required for such investigations have unique technical challenges, and prior experience with other facilities indicates that there will be a steep learning curve when JWST becomes operational. In this paper we describe the science objectives and detailed plans of the Transiting Exoplanet Community Early Release Science (ERS) Program, which is a recently approved program for JWST observations early in Cycle 1. The goal of this project, for which the obtained data will have no exclusive access period, is to accelerate the acquisition and diffusion of technical expertise for transiting exoplanet observations with JWST, while also providing a compelling set of representative datasets that will enable immediate scientific breakthroughs. The Transiting Exoplanet Community ERS Program will exercise the time-series modes of all four JWST instruments that have been identified as the consensus highest priorities, observe the full suite of transiting planet characterization geometries (transits, eclipses, and phase curves), and target planets with host stars that span an illustrative range of brightnesses. The observations in this program were defined through an inclusive and transparent process that had participation from JWST instrument experts and international leaders in transiting exoplanet studies. Community engagement in the project will be centered on a two-phase Data Challenge that culminates with the delivery of planetary spectra, time-series instrument performance reports, and open-source data analysis toolkits in time to inform the agenda for Cycle 2 of the JWST mission.
Published: 2018

41. A Principal Component Analysis-based Method to Analyze High-resolution Spectroscopic Data on Exoplanets

Author: Damiano, M., primary, Micela, G., additional, and Tinetti, G., additional
Published: 2019
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42. A Population Study of Gaseous Exoplanets

Author: Tsiaras, A, Waldmann, IP, Zingales, T, Rocchetto, M, Morello, G, Damiano, M, Karpouzas, K, Tinetti, G, McKemmish, LK, Tennyson, J, Yurchenko, SN, Tsiaras, A, Waldmann, IP, Zingales, T, Rocchetto, M, Morello, G, Damiano, M, Karpouzas, K, Tinetti, G, McKemmish, LK, Tennyson, J, and Yurchenko, SN
Abstract: We present here the analysis of 30 gaseous extrasolar planets, with temperatures between 600 and 2400 K and radii between 0.35 and 1.9 R Jup. The quality of the HST/WFC3 spatially scanned data combined with our specialized analysis tools allow us to study the largest and most self-consistent sample of exoplanetary transmission spectra to date and examine the collective behavior of warm and hot gaseous planets rather than isolated case studies. We define a new metric, the Atmospheric Detectability Index (ADI) to evaluate the statistical significance of an atmospheric detection and find statistically significant atmospheres in around 16 planets out of the 30 analyzed. For most of the Jupiters in our sample, we find the detectability of their atmospheres to be dependent on the planetary radius but not on the planetary mass. This indicates that planetary gravity plays a secondary role in the state of gaseous planetary atmospheres. We detect the presence of water vapour in all of the statistically detectable atmospheres, and we cannot rule out its presence in the atmospheres of the others. In addition, TiO and/or VO signatures are detected with 4σ confidence in WASP-76 b, and they are most likely present in WASP-121 b. We find no correlation between expected signal-to-noise and atmospheric detectability for most targets. This has important implications for future large-scale surveys.
Published: 2018

43. The science of ARIEL

Author: Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Leconte, J., Micela, G., Ollivier, M., Pilbratt, G., Puig, L., Heske, A., Turrini, D., Vandenbussche, B., Wolkenberg, P., University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, ECLIPSE 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo, Istituto Nazionale di Astrofisica (INAF), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), University of Valencia, Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Pomies, Marie-Paule, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics
Abstract: International audience; Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-size planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet's birth, and evolution. Progress with these science questions demands a large, unbiased spectroscopic survey of exoplanets. The ESA ARIEL M4 candidate mission has been conceived to conduct such a survey and to explore the nature of exoplanet atmospheres and interiors and, through this, the key factors affecting the formation and evolution of planetary systems.
Published: 2017

44. The ARIEL Mission Reference Sample

Author: Zingales, T., Tinetti, G., Pillitteri, I., Sarkar, S., Leconte, J., University College of London [London] (UCL), ECLIPSE 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics
Abstract: International audience; We present here an optimal list of targets observable by ARIEL (Atmospheric Remote-sensing Exoplanet Large survey), one of the three European Space Agency M4 mission candidates competing for a launch in 2026. In aprticular, we describe the assumptions made to estimate an optimal sample of exoplanets - including both the already known exoplanets and the "expected" ones yet to be discovered - observable by ARIEL and define a realistic mission scenario. The current ARIEL design enables the observation of 1000 planets during its four year mission lifetime. This nominal list of planets is expected to evolve over the years depending on the new exoplanet discoveries. Among the 1000 planets a good fraction of super-Earths and earth-sized planets will be included. While ARIEL will focus mainly on warm and hot planets, we briefly discuss its capability to study temperate planets around cool dwarfs like the ones orbiting TRAPPIST1.
Published: 2017

45. The EChO science case

Author: Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Isaak, K., Linder, M., Lovis, C., Micela, G., Olliver, M., Puig, L., Ribas, I., De Sio, A., Frith, J., Justtanot, K., Showman, A., Alard, C., Yurchenko, S. N., Parviainen, H., Fouqué, P., Oliva, E., Bordé, P., Balado, A., Varley, R., Di Giorgio, A., Griffin, M., Maillard, J. P., Maggio, A., Lellouch, E., Strazzulla, G., Villaver, E., Griffith, C., Stamper, R., Amado, P. J., Rezac, L., Laken, B., Hargrave, P., Orton, G., Thompson, S., Morales, J. C., Wright, G., Massi, F., Lundgaard Rasmussen, I., Altieri, F., Covino, E., Coustenis, A., Moses, J., Lithgow Bertelloni, C., Demangeon, O., Fletcher, L., Morales Calderón, M., Lo Cicero, U., López Puertas, M., Capria, M. T., Danielski, C., Luntzer, A., Bulgarelli, A., González Hernández, J., Jacquemoud, S., MacTavish, C., Mall, U., Christian Jessen, N., Sanromá, E., Femenía Castella, B., Rocchetto, M., Miles Paez, P., Allard, F., Aylward, A., Leconte, J., Palla, F., White, G., Malaguti, G., Cavarroc, C., Lammer, H., Leto, G., Batista, V., Adybekian, V., Readorn, K., Polichtchouk, I., Petrov, R., García Piquer, A., Pancrazzi, M., Gómez Leal, I., Israelian, G., Rebolo López, R., Peralta, J., Giro, E., Tecsa, M., Haigh, J., Moro Martín, A., Pezzuto, S., Piskunov, N., Agnor, C., Hollis, M., Radioti, A., De Kok, R., Gear, W., Eymet, V., Achilleos, N., Koskinen, T., Maurin, A. S., Rank Lüftinger, T., Barlow, M., Figueira, P., Affer, L., Viti, S., Machado, P., Vakili, F., Burston, R., González Merino, B., Dominic, C., Dorfi, E., Smith, A., Sitek, P., Sánchez Lavega, A., Kerschbaum, F., Hoogeeven, R., Ballerini, P., Filacchione, G., Rodler, F., Stixrude, L., Parmentier, V., Del Val Borro, M., Vandenbussche, B., Tingley, B. W., Deeg, H. J., Tabernero, H. M., Shore, S., Fossey, S., Alonso Floriano, F. J., Santos, N., Tozzi, A., Kipping, D., Maruquette, J. B., Trifoglio, M., Scandaratio, G., Scuderi, S., Hébrard, E., Lodieu, N., Forget, F., Gustin, J., Poretti, E., Murgas Alcaino, F., Sicardy, B., Stiepen, A., Hubert, B., Grodent, D., Magnes, W., Tennyson, J., Temple, J., Galand, M., Barton, E. J., Winter, B., Valdivieso, M. L., Cordier, D., Heredero, R. L., Barrado, D., Mueller Wodarg, I., Giani, E., Correira, A., Widemann, T., Ward Thompson, D., Montañés Rodríguez, P., Moya Bedon, A., Venot, O., Prinja, R., Pinfield, D., Waldmann, I., Morello, G., Lim, T., Pallé, E., Waters, R., Wawer, P., Lognonné, P., Pietrzak, R., Fernández Hernández, Maite, Winek, W., Andersen, A., Monteiro, M., Liu, S. J., Rengel, M., Tanga, P., Yelle, R., Barstow, J. K., Maldonado, J., Irshad, R., Nelson, R., Colomé, J., De Witt, J., Lanza, N., Glasse, A., Coudé du Foresto, V., Branduardi Raymont, G., Beaulieu, J. P., Claudi, R., García López, Ramón, Eales, S., López Valverde, M. A., Turrini, D., Vinatier, S., Crook, J., Damasso, M., Ramos Zapata, G., Kovács, G., Banaszkiewicz, M., Focardi, M., Mauskopf, P., Guedel, M., Rebordao, J., Stolarski, M., Adriani, A., Norgaard Nielsen, H. U., Selig, A., Peña Ramírez, K. Y., Schmider, F. X., Baffa, C., Piccioni, G., Pantin, E., Bowles, N., Hornstrup, A., Pilat Lohinger, E., Buchhave, L. A., Soret, L., Börne, P., López Morales, M., Medvedev, A., Gesa, L., Jones, H., Pérez Hoyos, S., Gerard, J. C., Bellucci, G., Morais, H., Álvarez Iglesias, C. A., Abe, L., Pinsard, F., Tessenyi, M., Blecka, M., Wawrzaszk, A., Middleton, K., Martín Torres, J., Cho, J., Berry, D., Rataj, M., Schrader, J. R., Scholz, A., Watkins, C., Abreu, M., Testi, L., Decin, L., Sánz Forcada, J., Sozzetti, A., Lagage, P. O., Ade, P., Alcala, J., Sousa, S., Espinoza Contreras, M., Swinyard, B., Dobrijévic, M., Sánchez Béjar, V. J., Krupp, N., Bakos, G., Chamberlain, S., Chadney, J., Brown, L., Iro, N., Montalto, M., Sethenadh, J., Bouy, H., Ottensamer, R., Kehoe, T., Doel, P., Delgado Mena, E., Read, P., Coates, A., Cecchi Pestellini, C., Guillot, T., Budaj, J., Selsis, F., Jarchow, C., Del Vecchio, C., Cassan, A., Burleigh, M. R., Pagano, I., Ray, T., Gambicorti, L., Biondi, D., Cerulli, R., Ciaravella, A., Watson, D., Deroo, P., Collura, A., Graczyk, R., North, C., Ramos, A. A., Waltham, D., Montes, D., Gianotti, F., Thrastarson, H., Cockell, C., Pace, E., Bryson, I., Gómez, H., Esposito, M., Azzollini, R., Allende Prieto, C., Gillon, M., Fabrizio, N., Rickman, H., Rees, J. M., Pascale, E., Luzzi, D., Bonford, B., Cole, R., Gizon, L., Licandro Goldaracena, J., Agundez, M., Lahav, O., Zapatero Osorio, M. R., Gaulme, P., Encrenaz, T., Heyrovsky, D., Guàrdia, J., Prisinzano, L., Terenzi, L., Swain, M., Grassi, D., Eiroa, C., Maxted, P., Kerins, E., Yung, Y., Irwin, P., Herrero, E., Guio, P., Boisse, I., Claret, A., Kervella, P., Heiter, U., Bézard, B., Cabral, A., Michaut, C., Giuranna, M., Hersant, F., Hueso, R., Savini, G., Snellen, I. A., Charnoz, S., Jones, G., Belmonte Avilés, J. A., Barber, R. J., Wisniowski, T., Morgante, G., University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, U.S. Army Research Laboratory [Adelphi, MD] (ARL), United States Army (U.S. Army), Royal Observatory Edinburgh (ROE), University of Edinburgh, Departamento de Fisica [Aveiro], Universidade de Aveiro, SRON Netherlands Institute for Space Research (SRON), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Planetary Sciences [Tucson], University of Arizona, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), The Samuel Roberts Noble Foundation, Center for Human-Computer Interaction (HCI), Virginia Tech [Blacksburg], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), ECLIPSE 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCL London], Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), University of Stuttgart, Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Mullard Space Science Laboratory (MSSL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Curie [Paris], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Centre for Behaviour and Evolution, Institute of Neuroscience, Newcastle University [Newcastle], foreign laboratories (FL), CERN [Genève], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Estrutura de Missão para a Extensão da Plataforma Continental, Estrutura de Missão para a Extensão para a Extensão da Plataforma Continental, Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Queen Mary University of London (QMUL), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Department of Geoscience, Nelson Mandela University [Port Elizabeth], African Earth Observatory Network - Earth Stewardship Science Research Institute (AEON-ESSRI), Animal Genetics, Teagasc - The Agriculture and Food Development Authority (Teagasc), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Instituto Nacional de Engenharia, Tecnologia e Inovacao (INETI), Université Pierre et Marie Curie - Paris 6 (UPMC), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università di Salerno - Dipartimento di Matematica, Università degli Studi di Salerno = University of Salerno (UNISA), Department of Genetics, University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC)-Carolina Center for the Genome Sciences, Institut de Recerca i Tecnologia Agroalimentàries = Institute of Agrifood Research and Technology (IRTA), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Department of Molecular Medicine, Università degli Studi di Padova = University of Padua (Unipd), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), ASP 2015, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de génétique et microbiologie [Orsay] (IGM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH = German Research Center for Artificial Intelligence (DFKI), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Dipartimento di Matematica 'Ulisse Dini', Università degli Studi di Firenze = University of Florence (UniFI), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Université de Rennes (UR), Imperial College London, Laboratoire Hippolyte Fizeau (FIZEAU), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Bradford, Instituto Universitario de Electroquimica, Universidad de Alicante, Centre de recherche en éducation de Nantes (CREN), Le Mans Université (UM)-Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN), Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), NASA Goddard Space Flight Center (GSFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Los Alamos National Laboratory (LANL), Osserv Astrofis Catania, Ist Nazl Astrofis, Centre d'Etude de l'Energie Nucléaire (SCK-CEN), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Super Invest Cient, Inst Astrofis Andalucia, ES-18080 Granada, Spain, Department of Rheumatology (LEIDEN - Rhumato), Leiden University Medical Center (LUMC), Universiteit Leiden-Universiteit Leiden, Department of Rheumatology (COIMBRA - Rhumato), Universidade de Coimbra [Coimbra], Centre Scientifique et Technique du Bâtiment (CSTB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Université de Bordeaux (UB), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des gaz et des plasmas (LPGP), Pontificia Universidad Católica de Chile (UC), Department of Computer Science [Verona] (UNIVR | DI), Università degli studi di Verona = University of Verona (UNIVR), IEB-UNIVERSITY OF BARCELONA, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Thüringer Landessternwarte Tautenburg (TLS), Bremer Institut für Produktion und Logistik GmbH (BIBA), Universität Bremen, INAF - Osservatorio Astrofisico di Catania (OACT), Plasmon Nano-optics, Institut de Ciencies Fotoniques [Castelldefels] (ICFO), Royal Holloway [University of London] (RHUL), Hong Kong Government Environmental Protection Department, Water Policy and Science Group, National Space Agencies, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max Planck Institute for Solar System Research (MPS), European Space Agency (ESA), European Space Agency, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Samuel Roberts Noble Foundation, Inc., Universidade de Lisboa (ULISBOA), Polska Akademia Nauk (PAN), University of Oxford [Oxford], Max-Planck-Institut für Sonnensystemforschung (MPS), Institut Curie, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], AEON-ESSRI African Earth Observatory Network — Earth Stewardship Science Research Institute, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Physiologie de la reproduction et des comportements [Nouzilly] (PRC), Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Institut Français du Cheval et de l'Equitation [Saumur]-Institut National de la Recherche Agronomique (INRA), Université Francois Rabelais [Tours], Institut Français du Cheval et de l'Equitation, Università degli Studi di Salerno (UNISA), IRTA, Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH (DFKI), Universidade do Porto [Porto], Università degli Studi di Firenze [Firenze], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Department of Earth Sciences, University College London, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre interdisciplinaire de recherche, culture, éducation, formation, travail (CIRCEFT), Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Station biologique, Centre National de la Recherche Scientifique (CNRS), Dipartimento di Informatica [Verona], Università degli Studi di Verona, Departamento de Física e Astronomia [Porto], UMR5116, Centre Émile Durkheim (CED), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Clinica Neurologica, Università degli Studi di Perugia (UNIPG), Rebordao, J. [0000-0002-7418-0345], Kerschbaum, F. [0000-0001-6320-0980], Abreu, M. [0000-0002-0716-9568], Tabernero, H. [0000-0002-8087-4298], López Puertas, M. [0000-0003-2941-7734], Jacquemoud, S. [0000-0002-1500-5256], Tennyson, J. [0000-0002-4994-5238], Focardi, M. [0000-0002-3806-4283], Leto, G. [0000-0002-0040-5011], Lodieu, N. [0000-0002-3612-8968], Tinetti, G. [0000-0001-6058-6654], Sanroma, E. [0000-0001-8859-7937], Poretti, E. [0000-0003-1200-0473], Deeg, H. [0000-0003-0047-4241], Grassi, D. [0000-0003-1653-3066], Piccioni, G. [0000-0002-7893-6808], Ribas, I. [0000-0002-6689-0312], Coates, A. [0000-0002-6185-3125], García Ramón, J. [0000-0002-8204-6832], Bouy, H. [0000-0002-7084-487X[, Lognonne, P. [0000-0002-1014-920X], Demangeon, O. [0000-0001-7918-0355], Morales, J. C. [0000-0003-0061-518X], Ray, T. [0000-0002-2110-1068], Guio, P. [0000-0002-1607-5862], Tanga, P. [0000-0002-2718-997X], Prisinzano, L. [0000-0002-8893-2210], Barstow, J. [0000-0003-3726-5419], Balado, A. [0000-0003-4268-2516], Lithgow Bertelloni, C. [0000-0003-0924-6587], Barton, E. [0000-0001-5945-9244], Delgado, M. E. [0000-0003-4434-2195], Affer, L. [0000-0001-5600-3778], Ciaravella, A. [0000-0002-3127-8078], Barrado Navascues, D. [0000-0002-5971-9242], Figueira, P. [0000-0001-8504-283X], Covino, E. [0000-0002-6187-6685], Venot, O. [0000-0003-2854-765X], Cabral, A. [0000-0002-9433-871X], Watson, D. [0000-0002-4465-8264], Morales Calderon, M. [0000-0001-9526-9499], Ward Thompson, D. [0000-0003-1140-2761], Rebolo, R. [0000-0003-3767-7085], López Valverde, M. A. [0000-0002-7989-4267], Gillon, M. [0000-0003-1462-7739], Morgante, G. [0000-0001-9234-7412], Zapatero Osorio, M. R. [0000-0001-5664-2852], Bulgarelli, A. [0000-0001-6347-0649], Pena Ramírez, K. [0000-0002-5855-401X], Galand, M. [0000-0001-5797-914X], Pancrazzi, M. [0000-0002-3789-2482], Malaguti, G. [0000-0001-9872-3378], Sánchez Lavega, A. [0000-0001-7234-7634], Waldmann, I. [0000-0002-4205-5267], Kovacs, G. [0000-0002-2365-2330], Guillot, T. [0000-0002-7188-8428], Turrini, D. [0000-0002-1923-7740], Altieri, F. [0000-0002-6338-8300], Bellucci, G. [0000-0003-0867-8679], Baffa, C. [0000-0002-4935-100X], Olivia, E. [0000-0002-9123-0412], Selsis, F. [0000-0001-9619-5356], Scuderi, Salvatore [0000-0002-8637-2109], Hersant, F. [0000-0002-2687-7500], Gear, W. [0000-0001-6789-6196], Damasso, M. [0000-0001-9984-4278], Tizzi, A. [0000-0002-6725-3825], Pinfield, D. [0000-0002-7804-4260], Kipping, D. [0000-0002-4365-7366], Maldonado, J. [0000-0002-4282-1072], Pace, E. [0000-0001-5870-1772], Burleigh, M. [0000-0003-0684-7803], Monteiro, M. [0000-0001-5644-0898], Pilat Lohinger, E. [0000-0002-5292-1923], Chadney, J. [0000-0002-5174-2114], Moro Martín, A. [0000-0001-9504-8426], Claret, A. [0000-0002-4045-8134], Gómez, H. [0000-0003-3398-0052], Maldonado, J. [0000-0002-2218-5689], Michaut, C. [0000-0002-2578-0117], Hornstrup, A. [0000-0002-3363-0936], Scholz, A. [0000-0001-8993-5053], Irwin, P. [0000-0002-6772-384X], Bezard, B. [0000-0002-5433-5661], López Heredero, R. [0000-0002-2197-8388], Sanz Forcada, J. [0000-0002-1600-7835], Danielski, C. [0000-0002-3729-2663], Sousa, S. [0000-0001-9047-2965], Medved, A. [0000-0003-2713-8977], Bakos, G. [0000-0001-7204-6727], Ade, P. [0000-0002-5127-0401], Vandenbussche, B. [0000-0002-1368-3109], Martín Torres, J. [0000-0001-6479-2236], Correira, A. [0000-0002-8946-8579], Haigh, J. [0000-0001-5504-4754], Scandariato, G. [0000-0003-2029-0626], Guedel, M. [0000-0001-9818-0588], Sánchez Bejar, V. [0000-0002-5086-4232], Rodríguez, P. [0000-0002-6855-9682], Piskunov, N. [0000-0001-5742-7767], Adibekyan, V. [0000-0002-0601-6199], Pérez Hoyos, S. [0000-0001-9797-4917], Kervella, P. [0000-0003-0626-1749], Pascale, E. [0000-0002-3242-8154], Claudi, R. [0000-0001-7707-5105], Filacchione, G. [0000-0001-9567-0055], Rickman, H. [0000-0002-9603-6619], Amado, P. J. [0000-0002-8388-6040], Maggio, A. [0000-0001-5154-6108], Agundez, M. [0000-0003-3248-3564], Montes, D. [0000-0002-7779-238X], Fletcher, L. [0000-0001-5834-9588], Stixrude, L. [0000-0003-3778-2432], Morais, M. H. [0000-0001-5333-2736], Hueso, R. [0000-0003-0169-123X], Yurchenko, S. [0000-0001-9286-9501], Rataj, M. [0000-0002-2978-9629], Pérez Hoyos, S. [0000-0002-2587-4682], Santos, N. [0000-0003-4422-2919], Peralta, J. [0000-0002-6823-1695], Budaj, J. [0000-0002-9125-7340], Barlow, M. [0000-0002-3875-1171], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto, Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), University of Verona (UNIVR), Universidade do Porto-Universidade do Porto, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN)-Le Mans Université (UM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Institut National de la Recherche Agronomique (INRA)-Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Firenze = University of Florence [Firenze], COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, University College of London [London] ( UCL ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Max Planck Institute for Solar System Research ( MPS ), School of Physics & Astronomy, European Space Agency ( ESA ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire des technologies de la microélectronique ( LTM ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Microélectronique, Electromagnétisme et Photonique - Laboratoire d'Hyperfréquences et Caractérisation ( IMEP-LAHC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National Polytechnique de Grenoble ( INPG ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Universidad Politécnica de Cataluña, U.S. Army Research Laboratory [Adelphi, MD] ( ARL ), United States Army ( U.S. Army ), Royal Observatory Edinburgh ( ROE ), SRON Netherlands Institute for Space Research ( SRON ), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Lunar and Planetary Laboratory [Tucson], Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Center for Human-Computer Interaction ( HCI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), University of Hertfordshire [Hatfield] ( UH ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), Centro de Astronomia e Astrofísica da Universidade de Lisboa ( CAAUL ), Universidade de Lisboa ( ULISBOA ), Space Research Centre [Warsaw] ( CBK ), Polska Akademia Nauk ( PAN ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Mullard Space Science Laboratory ( MSSL ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven ( KU Leuven ), foreign laboratories ( FL ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), Queen Mary University of London ( QMUL ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - 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Astrofísica, Centro de Astrobiología, Nelson Mandela Metropolitan University, Nelson Mandela Metropolitan University [Port Elizabeth, South Africa]-Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Teagasc, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Fraunhofer-Institute for Applied Solid-State Physics (IAF), Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Instituto Nacional de Engenharia, Tecnologia e Inovacco ( INETI ), INETI, Université Pierre et Marie Curie - Paris 6 ( UPMC ), Physiologie de la reproduction et des comportements [Nouzilly] ( PRC ), Institut National de la Recherche Agronomique ( INRA ) -Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique ( CNRS ), Università degli Studi di Salerno ( UNISA ), The University of North Carolina at Chapel Hill-Carolina Center for the Genome Sciences, Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Université de Franche-Comté ( UFC ), Universita degli Studi di Padova = University of Padua = Université de Padoue, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - 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Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH ( DFKI ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ), Laboratoire Hippolyte Fizeau ( FIZEAU ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Istituto di Fisica dello Spazio Interplanetario CNR (IFSI), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de recherche en éducation de Nantes ( CREN ), Université de Nantes ( UN ), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea ( UPV/EHU ), NASA Goddard Space Flight Center ( GSFC ), Onsala Space Observatory ( OSO ), Los Alamos National Laboratory ( LANL ), Centre d'Etude de l'Energie Nucléaire ( SCK-CEN ), Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Rheumatology ( LEIDEN - Rhumato ), Department of Rheumatology ( COIMBRA - Rhumato ), Centre Scientifique et Technique du Bâtiment ( CSTB ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Centre interdisciplinaire de recherche, culture, éducation, formation, travail ( CIRCEFT ), Université Paris 8 Vincennes-Saint-Denis ( UP8 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique des gaz et des plasmas ( LPGP ), Pontificia Universidad Católica de Chile, Thüringer Landessternwarte Tautenburg ( TLS ), BIBA Bremer Institut für Produktion und Logistik GmbH, Centre Émile Durkheim ( CED ), Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Institut de Ciencies Fotoniques [Castelldefels] ( ICFO ), Università di Perugia, Royal Holloway [University of London] ( RHUL ), and Low Energy Astrophysics (API, FNWI)
Subjects: Astrofísica, Solar System, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], HOT-JUPITER ATMOSPHERES, 7. Clean energy, Space missions, law.invention, Astronomi, astrofysik och kosmologi, Planet, law, Observatory, Astronomy, Astrophysics and Cosmology, Transit (astronomy), Atmospheric science, Exoplanets, IR astronomy, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, QC, QB, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, GIANT PLANETS, Physical Sciences, ENERGY-BALANCE, Astrophysics::Earth and Planetary Astrophysics, Population, MU-M, FOS: Physical sciences, F500, Astronomy & Astrophysics, Telescope, INFRARED-EMISSION-SPECTRUM, education, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], EXTRASOLAR PLANET ATMOSPHERE, Science & Technology, Astronomy, EXOPLANET HD 189733B, HUBBLE-SPACE-TELESCOPE, Astronomía, TRANSMISSION SPECTROSCOPY, 0201 Astronomical And Space Sciences, 13. Climate action, WATER-VAPOR, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract: The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. 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? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys 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. 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. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy
Published: 2015

46. A Population Study of Gaseous Exoplanets

Author: Tsiaras, A., primary, Waldmann, I. P., additional, Zingales, T., additional, Rocchetto, M., additional, Morello, G., additional, Damiano, M., additional, Karpouzas, K., additional, Tinetti, G., additional, McKemmish, L. K., additional, Tennyson, J., additional, and Yurchenko, S. N., additional
Published: 2018
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47. TWINKLE: a low earth orbit visible and infrared exoplanet spectroscopy observatory

Author: Savini, Giorgio, primary, Tinetti, G., primary, Arena, C., primary, Tennyson, J., primary, Pascale, En., primary, Ade, P. A. R., primary, Griffin, M. J., primary, Knowles, P., primary, Crook, M., primary, Saad, A., primary, Eccleston, P., primary, Shaughnessy, B., primary, Brooke, T., primary, Macleod, A., primary, Wright, G. S., primary, Jason, S., primary, Williams, J., primary, Winter, B., primary, Smith, A., primary, Tessenyi, M., primary, Zingales, T., primary, Sudiwala, R., primary, Papageorgiou, A., primary, Sarkar, S., primary, Barnes, K., primary, Hipwood, L., primary, Patel, M., primary, Leese, M., primary, Mason, J. P., primary, Tosh, I., primary, Wells, M., primary, Bryson, I., primary, Taylor, W., primary, Bezawada, N., primary, Friend, J., primary, Johnston, G., primary, Prasad, S., primary, Vora, A., primary, Saunders, C., primary, and Curry, P., primary
Published: 2018
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48. Transit spectroscopy of temperate Jupiters with ARIEL: a feasibility study

Author: Encrenaz, Thérèse, primary, Tinetti, G., additional, and Coustenis, A., additional
Published: 2017
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49. The ARIEL Instrument Control Unit design

Author: Focardi, M., primary, Pace, E., additional, Farina, M., additional, Di Giorgio, A. M., additional, Ferrer, J. Colomé, additional, Ribas, I., additional, Roig, C. Sierra, additional, Bote, L. Gesa, additional, Morales, J. C., additional, Amiaux, J., additional, Cara, C., additional, Augurés, J. L., additional, Pascale, E., additional, Morgante, G., additional, Da Deppo, V., additional, Pancrazzi, M., additional, Noce, V., additional, Pezzuto, S., additional, Frericks, M., additional, Zwart, F., additional, Bishop, G., additional, Middleton, K., additional, Eccleston, P., additional, Micela, G., additional, and Tinetti, G., additional
Published: 2017
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50. EChO

Author: Tinetti, G, Beaulieu, J, Henning, T, Meyer, M, Micela, G, Ribas, I, Stam, D, Swain, M, Krause, O, Ollivier, M, Pace, E, Swinyard, B, Aylward, A, van Boekel, R, Coradini, A, Encrenaz, T, Snellen, I, Zapatero-Osorio, MR, Bouwman, J, Cho, J, Foresto, d, Guillot, T, Lopez-Morales, M, Mueller-Wodarg, I, and Palle, E
Published: 2016

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