133 results on '"Vincent Bourrier"'
Search Results
2. Hydrodynamic Atmospheric Escape in HD 189733 b: Signatures of Carbon and Hydrogen Measured with the Hubble Space Telescope
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Leonardo A. Dos Santos, Antonio García Muñoz, David K. Sing, Mercedes López-Morales, Munazza K. Alam, Vincent Bourrier, David Ehrenreich, Gregory W. Henry, Alain Lecavelier des Etangs, Thomas Mikal-Evans, Nikolay K. Nikolov, Jorge Sanz-Forcada, and Hannah R. Wakeford
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Exoplanet atmospheres ,Hot Jupiters ,Planet hosting stars ,Ultraviolet astronomy ,Astronomy ,QB1-991 - Abstract
One of the most well-studied exoplanets to date, HD 189733 b, stands out as an archetypal hot Jupiter with many observations and theoretical models aimed at characterizing its atmosphere, interior, host star, and environment. We report here on the results of an extensive campaign to observe atmospheric escape signatures in HD 189733 b using the Hubble Space Telescope and its unique ultraviolet capabilities. We have found a tentative, but repeatable in-transit absorption of singlyionized carbon (C ii , 5.2% ± 1.4%) in the epoch of June–July/2017, as well as a neutral hydrogen (H i ) absorption consistent with previous observations. We model the hydrodynamic outflow of HD 189733 b using an isothermal Parker wind formulation to interpret the observations of escaping C and O nuclei at the altitudes probed by our observations. Our forward models indicate that the outflow of HD 189733 b is mostly neutral within an altitude of ∼2 R _p and singly ionized beyond that point. The measured in-transit absorption of C ii at 1335.7 Å is consistent with an escape rate of ∼1.1 × 10 ^11 g s ^−1 , assuming solar C abundance and an outflow temperature of 12,100 K. Although we find marginal neutral oxygen (O i ) in-transit absorption, our models predict an in-transit depth that is only comparable to the size of measurement uncertainties. A comparison between the observed Ly α transit depths and hydrodynamics models suggests that the exosphere of this planet interacts with a stellar wind at least 1 order of magnitude stronger than solar.
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- 2023
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3. Disentangling Stellar and Airglow Emission Lines from Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) Spectra
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Fernando Cruz Aguirre, Allison Youngblood, Kevin France, and Vincent Bourrier
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Dwarf stars ,Main sequence stars ,Hubble Space Telescope ,Ultraviolet spectroscopy ,Stellar activity ,Astrophysics ,QB460-466 - Abstract
H i Ly α (1215.67 Å) and the O i triplet (1302.17, 1304.86, and 1306.03 Å) are bright far-ultraviolet (FUV) emission lines that trace the stellar chromosphere. Observations of stellar Ly α and O i using the Hubble Space Telescope's (HST) most sensitive FUV spectrograph, the Cosmic Origins Spectrograph (COS), are contaminated with geocoronal emission, or airglow. This study demonstrates that airglow emission profiles as observed by COS are sufficiently stable to create airglow templates that can be reliably subtracted from the data, recovering the underlying stellar flux. We developed a graphical user interface to implement the airglow subtraction on a sample of 171 main-sequence F-, G-, K-, and M-type dwarfs from the COS data archive. Correlations between recovered stellar emission and measures of stellar activity were investigated. Several power-law relationships are presented for predicting the stellar Ly α and O i emission. The apparent brightness of the stellar emission relative to the airglow is a critical factor in the success or failure of an airglow subtraction. We developed a predictor for the success of an airglow subtraction using the signal-to-noise ratio of the nearby chromospheric emission line Si iii (1206.51 Å). The minimum attenuated Ly α flux that was successfully recovered is 1.39 × 10 ^−14 erg cm ^−2 s ^−1 , and we recommend this as a minimum flux for COS Ly α recoveries.
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- 2023
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4. CHEOPS’s hunt for exocomets: photometric observations of 5 Vul
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Isabel Rebollido, Sebastian Zieba, Daniela Iglesias, Vincent Bourrier, Flavien Kiefer, and Alain Lecavelier Des Etangs
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Earth and Planetary Astrophysics (astro-ph.EP) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The presence of minor bodies in exoplanetary systems is in most cases inferred through infra-red excesses, with the exception of exocomets. Even if over 35 years have passed since the first detection of exocomets around beta Pic, only ~ 25 systems are known to show evidence of evaporating bodies, and most of them have only been observed in spectroscopy. With the appearance of new high-precision photometric missions designed to search for exoplanets, such as CHEOPS, a new opportunity to detect exocomets is available. Combining data from CHEOPS and TESS we investigate the lightcurve of 5 Vul, an A-type star with detected variability in spectroscopy, to search for non periodic transits that could indicate the presence of dusty cometary tails in the system. While we did not find any evidence of minor bodies, the high precision of the data, along with the combination with previous spectroscopic results and models, allows for an estimation of the sizes and spatial distribution of the exocomets., Comment: Accepted for publication in MNRAS
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- 2023
5. Transmission spectroscopy of the aligned hot Jupiter KELT-10b using HARPS
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Michal Steiner, Omar Attia, David Ehrenreich, and Vincent Bourrier
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Context High-resolution spectrographs provide an excellent opportunity for probing exoplanetary atmospheres, utilizing the transmission spectroscopy method (among others). This method allows us to explore deep into the atmosphere, detecting multiple atomic and molecular species. We can also study the atmospheric wind patterns by characterizing the line profile. So far, dozens of exoplanets, mainly hot Jupiters and warm Neptunes, have their atmosphere successfully observed with this method. Most studies so far have focussed on exoplanets showcasing easily detectable signatures (in particular, sodium); however, it is important, not to bias the sample of studied planets, to enquire about more challenging cases, which could feature different atmospheric conditions. KELT-10b Using the HARPS spectrograph, I will show my work on transmission spectroscopy of KELT-10b, a standard hot Jupiter-type planet, utilizing data from two transit nights. We used spectra from the HEARTS survey, which aims to study exoplanetary atmospheres using transmission spectroscopy with HARPS. I have been mainly focusing on the sodium lines and Balmer lines in the transmission spectrum of KELT-10b. Sodium has not been detected in KELT-10b with HARPS, although recently detected by UVES. I will discuss how high-quality non-detections can further strengthen our confidence in detected signals and how precise rectification of stellar effects is necessary for detections. Two photometric light curves have been observed complementary to the two transit night observations with HARPS. This allows us to monitor the star for potential stellar variation, and, by including the already public dataset, improve the ephemeris of this system. Rossiter-McLaughlin effect Since HARPS allows for precise observations of radial velocities, we analyzed the Rossiter-McLaughlin effect during the transits. We measured the obliquity and stellar projected equatorial velocity, finding the system to be aligned. Transmission spectroscopy Searching for sodium in the transmission spectroscopy has been unsuccessful, as KELT-10b is quite a faint target. However, due to the characteristics of the system, the effect of the Rossiter-McLaughlin effect is significant, possibly explaining the signature previously detected in UVES data.
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- 2022
6. An orbital stability-driven approach for the refinement of multi-planet systems’ architectures
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Manu Stalport, Jean-Baptiste Delisle, Stéphane Udry, Elisabeth Matthews, Vincent Bourrier, and Adrien Leleu
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The formation and evolution of planetary systems has been, and remains, one of the big questions of Science. With more than 800 multi-planet systems discovered so far, as many outcomes of these formation and evolution processes are in reach of characterization. These represent precious pieces of the big puzzle. In order to obtain the most from these constraints, a precise knowledge of each system's architecture is crucial: it is key to identify the leading processes in shaping those systems, and hence relate their present state to their formation stage. In this presentation, I will introduce a technique aiming at refining the planetary orbital parameters and masses (Stalport et al. 2022). This technique uses orbital stability arguments on top of a bayesian approach for the parameters' estimation. The estimation of orbital stability is based on short N-body numerical integrations together with the Numerical Analysis of Fundamental Frequencies (NAFF) fast chaos indicator (Laskar 1990), for which we propose a calibration strategy to scale chaos. The stability information is finally included a posteriori in the planetary parameters' posterior through importance sampling, after which new distributions of stable-only solutions are built. This stability-driven refinement technique can be applied on any type of multi-planet systems, and notably in the context of planets in binaries. Besides the advantage of reducing the uncertainties on the dynamical parameters (orbital elements and planetary masses), such an approach can also provide additional insights into the dynamical states of the studied systems. I will present the revision of a few multi-planet systems in light of our approach, and particularly, I will describe a comprehensive dynamical analysis of the Kepler-444 planetary system (Stalport et al. submitted to A&A). Approaches such as the one presented here are timely. They represent a way of getting the best constraints on planetary systems' architectures within limited observational datasets. I will stress for the importance of carrying a systematic revision of multi-planet systems under the loop of orbital stability.
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- 2022
7. A journey to the Interior of (ultra-short-period) Earths
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Mathilde Kervazo, Vincent Bourrier, Jo Ann Egger, and Yann Alibert
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Half of known exoplanets orbit close to their star, featuring a desert of hot Neptunes whose origins remain uncertain. The lower border of the desert ends in a population of small rocky planets (≤ 2 R⊕) on ultra-short periods (≤ 1 day) called USPs. These USPs are central to study planetary evolution around the desert, as they might be the exposed rocky cores of evaporated gaseous planets. Due to their proximity to the star, the surface temperature of USPs are expected to be higher than the melting point of most rock-forming minerals. Their likely molten unstable surface, which could lead to significant outgassing from magma oceans or active volcanoes, and the formation of a dust- and metal-rich envelope, would significantly affect the composition of the outer enveloppe. There is thus a need in characterising the internal structure of planets subjected to such extreme conditions. Most studies concerned with interior characterization have generally concentrated on computing mass-radius relations based on terrestrial-type interior structures and compositions. Such “forward” approaches, however, allow for different core sizes and mantle compositions, affecting the mass-radius relationship, and do not quantify the inherent degeneracy of interior structure models. In the light of this inherent ambiguity, some studies propose a complete Bayesian inverse analysis by employing a Markov chain Monte Carlo method to provide full probability distributions for the model parameters of interest. Moreover, a layered structure is classically considered, with, from the centrer to the surface, a metallic core, a rocky mantle, a water layer and an outer enveloppe composed of hydrogen and helium. This classical composition might be questioned in the particular case of the USPs, especially for their enveloppe part, for which the metallicity might vary due to compositional differences. In this context, the goal of our study is to develop a coherent internal structure model for the specific USP population and to derive samples of properties on their internal structure, by performing a statistical method which allows to characterize an exoplanet’s interior given its mass and radius. For that purpose, we use the simulation code call the Bayesian Interior Characterisation of ExoPlanetS (BICEPS) model, and adapt it to USPs in order to better understand the formation and evolution of short-period planets, in particular the atmospheric erosion, under strong stellar irradiation, characteristics of USPs. Acknowledgements: This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Spice Dune, grant agreement No 947634).
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- 2022
8. Transit detection of the long-period volatile-rich super-Earth ν2 Lupi d with CHEOPS
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Sergio Hoyer, Vardan Adibekyan, J.-B. Delisle, Nuno C. Santos, David Barrado, Enric Palle, Damien Ségransan, Isabella Pagano, Malcolm Fridlund, Antonio García Muñoz, M. Steller, A. Deline, Guillem Anglada-Escudé, A. Bekkelien, Nicolas Billot, Ignasi Ribas, Don Pollacco, Roberto Ragazzoni, Yann Alibert, T. Bárczy, Gaetano Scandariato, H. P. Osborn, L. Borsato, Alain Lecavelier des Etangs, Heike Rauer, Thomas G. Wilson, M. Beck, Mahmoudreza Oshagh, L. Delrez, Nicholas A. Walton, Roi Alonso, S. G. Sousa, Stéphane Udry, M. J. Hooton, Kevin Heng, S. Sulis, Manuel Guedel, Göran Olofsson, Vincent Bourrier, Michaël Gillon, Anders Erikson, Monika Lendl, Didier Queloz, Davide Gandolfi, Olivier Demangeon, Luca Fossati, Nicolas Thomas, Wolfgang Baumjohann, Pierre F. L. Maxted, Brice-Olivier Demory, S. C. C. Barros, Alexis M. S. Smith, Willy Benz, Andrea Bonfanti, Sébastien Charnoz, Melvyn B. Davies, Juan Cabrera, Magali Deleuil, Alexis Brandeker, J. Haldemann, László L. Kiss, Giampaolo Piotto, Valerio Nascimbeni, Christopher Broeg, Andrea Fortier, Jacques Laskar, Christophe Lovis, D. Futyan, Valérie Van Grootel, Pascal Guterman, Gyula M. Szabó, A. E. Simon, Francisco J. Pozuelos, Andrew Collier Cameron, David Ehrenreich, S. Salmon, Xavier Bonfils, Nathan Hara, Fundação para a Ciência e a Tecnologia (Portugal), European Commission, Swiss National Science Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Belgian Science Policy Office, Université de Liège, Austrian Research Promotion Agency, Hungarian Scientific Research Fund, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Cavendish Laboratory, University of Cambridge [UK] (CAM), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Laboratoire d'astrophysique de l'observatoire de Besançon (UMR 6091) (LAOB), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Université de Technologie de Belfort-Montbeliard (UTBM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), Université de Genève (UNIGE), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)
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010504 meteorology & atmospheric sciences ,530 Physics ,FOS: Physical sciences ,Astrophysics - Earth and planetary astrophysics ,Q1 ,01 natural sciences ,Planet ,QB460 ,0103 physical sciences ,Transit (astronomy) ,010303 astronomy & astrophysics ,QB600 ,QB ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Super-Earth ,520 Astronomy ,Astronomy ,Astronomy and Astrophysics ,Radius ,620 Engineering ,Exoplanet ,Orbit ,Stars ,13. Climate action ,Satellite ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,QB799 - Abstract
Delrez, L., et al., Exoplanets transiting bright nearby stars are key objects for advancing our knowledge of planetary formation and evolution. The wealth of photons from the host star gives detailed access to the atmospheric, interior and orbital properties of the planetary companions. ν Lupi (HD 136352) is a naked-eye (V = 5.78) Sun-like star that was discovered to host three low-mass planets with orbital periods of 11.6, 27.6 and 107.6 d via radial-velocity monitoring. The two inner planets (b and c) were recently found to transit, prompting a photometric follow-up by the brand new Characterising Exoplanets Satellite (CHEOPS). Here, we report that the outer planet d is also transiting, and measure its radius and mass to be 2.56 ± 0.09 R and 8.82 ± 0.94 M, respectively. With its bright Sun-like star, long period and mild irradiation (~5.7 times the irradiation of Earth), ν Lupi d unlocks a completely new region in the parameter space of exoplanets amenable to detailed characterization. We refine the properties of all three planets: planet b probably has a rocky mostly dry composition, while planets c and d seem to have retained small hydrogen–helium envelopes and a possibly large water fraction. This diversity of planetary compositions makes the ν Lupi system an excellent laboratory for testing formation and evolution models of low-mass planets., The MOC activities have been supported by ESA contract 4000124370. S.C. acknowledges financial support by LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001). This work was supported by FCT (Fundação para a Ciência e a Tecnologia) through national funds and by FEDER (Fundo Europeu de Desenvolvimento Regional) through COMPETE2020—Programa Operacional Competitividade e Internacionalização with these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B., S.G.S. and V.A. acknowledge support from FCT through contracts IF/01312/2014/CP1215/CT0004, CEECIND/00826/2018, POPH/FSE (EC) and IF/00650/2015/CP1273/CT0001. O.D.S.D. is supported in the form of a work contract (DL 57/2016/CP1364/CT0004) with national funds through FCT. M.J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. A.D. and D.E. acknowledge support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement 724427). S.H. acknowledges CNES funding through grant 837319. The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33 and MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The Belgian participation in CHEOPS has been supported by the Belgian Federal Science Policy Office in the framework of the PRODEX Programme of the ESA under contract PEA 4000131343, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia–Brussels Federation. L.D. is an FRS-FNRS Postdoctoral Researcher. M. Gillon is an FRS–FNRS Senior Research Associate. V.V.G. is an FRS–FNRS Research Associate. M.L. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 ‘GRAPPA’. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). S. Salmon has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement 833925, project STAREX). G.M.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS activities have been supported by the Italian Space Agency, under the programmes ASI-INAF 2013-016-R.0 and ASI-INAF 2019-29-HH.0. L.B., G.P., I.P., G.S. and V.N. acknowledge funding support from the Italian Space Agency (ASI) regulated by ‘Accordo ASI-INAF 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015’. A.C.C. and T.G.W. acknowledge support from STFC consolidated grant ST/M001296/1. D.G., X.B., S.C., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. We thank S. R. Kane for sharing some RV data before their publication and L. D. Nielsen for helping to plan the CHEOPS observations on the basis of her analysis of the TESS data. We also thank M. Cretignier for his independent analysis of the HARPS RV data.
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- 2021
9. Extreme-ultraviolet Stellar Characterization for Atmospheric Physics and Evolution mission: motivation and overview
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Kevin France, Brian Fleming, Allison Youngblood, James Mason, Jeremy J. Drake, Ute V. Amerstorfer, Martin Barstow, Vincent Bourrier, Patrick Champey, Luca Fossati, Cynthia S. Froning, James C. Green, Fabien Grisé, Guillaume Gronoff, Timothy Hellickson, Meng Jin, Tommi T. Koskinen, Adam F. Kowalski, Nicholas Kruczek, Jeffrey L. Linsky, Sarah J. Lipscy, Randall L. McEntaffer, David E. McKenzie, Drew M. Miles, Tom Patton, Sabrina Savage, Oswald Siegmund, Constance Spittler, Bryce W. Unruh, and Máire Volz
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Space and Planetary Science ,Control and Systems Engineering ,Mechanical Engineering ,Astronomy and Astrophysics ,Instrumentation ,Electronic, Optical and Magnetic Materials - Published
- 2022
10. Titanium oxide and chemical inhomogeneity in the atmosphere of the exoplanet WASP-189 b
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Bibiana Prinoth, H. Jens Hoeijmakers, Daniel Kitzmann, Elin Sandvik, Julia V. Seidel, Monika Lendl, Nicholas W. Borsato, Brian Thorsbro, David R. Anderson, David Barrado, Kateryna Kravchenko, Romain Allart, Vincent Bourrier, Heather M. Cegla, David Ehrenreich, Chloe Fisher, Christophe Lovis, Andrea Guzmán-Mesa, Simon Grimm, Matthew Hooton, Brett M. Morris, Maria Oreshenko, Lorenzo Pino, and Kevin Heng
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Earth and Planetary Astrophysics (astro-ph.EP) ,Atmospheres ,530 Physics ,Exoplanets ,520 Astronomy ,Cross-correlation ,FOS: Physical sciences ,High-resolution spectroscopy ,Astronomy and Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,620 Engineering ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The temperature of an atmosphere decreases with increasing altitude, unless a shortwave absorber exists that causes a temperature inversion. Ozone plays this role in the Earth`s atmosphere. In the atmospheres of highly irradiated exoplanets, shortwave absorbers are predicted to be titanium oxide (TiO) and vanadium oxide (VO). Detections of TiO and VO have been claimed using both low and high spectral resolution observations, but later observations have failed to confirm these claims or overturned them. Here we report the unambiguous detection of TiO in the ultra-hot Jupiter WASP-189b using high-resolution transmission spectroscopy. This detection is based on applying the cross-correlation technique to many spectral lines of TiO from 460 to 690 nm. Moreover, we report detections of metals, including neutral and singly ionised iron and titanium, as well as chromium, magnesium, vanadium and manganese (Fe, Fe+, Ti, Ti+, Cr, Mg, V, Mn). The line positions of the detected species differ, which we interpret as a consequence of spatial gradients in their chemical abundances, such that they exist in different regions or dynamical regimes. This is direct observational evidence for the three-dimensional thermo-chemical stratification of an exoplanet atmosphere derived from high-resolution ground-based spectroscopy., Published in Nature Astronomy on 27 January 2022, accepted on 1 December 2021 (32 pages, 21 figures, 3 tables)
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- 2022
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11. p-winds: an open-source Python code to model planetary outflows and upper atmospheres
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Leonardo A. Dos Santos, Aline A. Vidotto, Shreyas Vissapragada, Munazza K. Alam, Romain Allart, Vincent Bourrier, James Kirk, Julia V. Seidel, and David Ehrenreich
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Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites ,FOS: Physical sciences ,Astronomy and Astrophysics ,methods ,atmospheres, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics ,numerical, planets and satellites ,numerical ,Space and Planetary Science ,atmospheres ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Atmospheric escape is considered to be one of the main channels for evolution in sub-Jovian planets, particularly in their early lives. While there are several hypotheses proposed to explain escape in exoplanets, testing them with atmospheric observations remains a challenge. In this context, high-resolution transmission spectroscopy of transiting exoplanets for the metastable helium triplet (He 2$^3$S) at $1\,083$ nm has emerged as a reliable technique to observe and measure escape. To aid in the prediction and interpretation of metastable He transmission spectroscopy observations, we developed the code p-winds. This is an open-source, fully documented, scalable Python implementation of the one-dimensional, purely H+He Parker wind model for upper atmospheres coupled with ionization balance, ray-tracing, and radiative transfer routines. We demonstrate an atmospheric retrieval by fitting p-winds models to the observed metastable He transmission spectrum of the warm Neptune HAT-P-11 b, and take into account the variation of the in-transit absorption caused by transit geometry. For this planet, our best fit yields a total atmospheric escape rate of approximately $2.5 \times 10^{10}$ g s$^{-1}$ and wind temperature of $7200$ K. The range of retrieved mass loss rates increases significantly when we let the H atom fraction be a free parameter, but the posterior distribution of the latter remains unconstrained by He observations alone. The stellar host limb darkening does not have a significant impact in the retrieved escape rate or outflow temperature for HAT-P-11 b. Based on the non-detection of escaping He for GJ 436 b, we are able to rule out total escape rates higher than $3.4 \times 10^{10}$ g s$^{-1}$ at 99.7% (3$\sigma$) confidence., Comment: 13 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics. We encourage the community to send comments and test the code, which is openly available at https://github.com/ladsantos/p-winds
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- 2022
12. Other Worlds in the Cosmos: From Philosophy to Scientific Reality
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Michel Mayor, Emeline Bolmont, Vincent Bourrier, David Ehrenreich, and Christoph Mordasini
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- 2022
13. Characterizing Exoplanetary Atmospheres at High Resolution with SPIRou: Detection of Water on HD 189733 b
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Ray Jayawardhana, Pascal Fouqué, Romain Allart, Claire Moutou, Antoine Darveau-Bernier, Michael Radica, David Lafrenière, Baptiste Klein, J. H. C. Martins, Nuno C. Santos, Ryan Cloutier, João Gomes da Silva, Emily Deibert, Vincent Bourrier, Christophe Lovis, Étienne Artigau, Pedro Figueira, Jean-François Donati, Anne Boucher, Xavier Bonfils, Björn Benneke, Eder Martioli, René Doyon, Xavier Delfosse, Thierry Forveille, Jonathan Gagné, Stefan Pelletier, Guillaume Hébrard, Luc Arnold, Eric Gaidos, David Ehrenreich, Neil Cook, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ANR-18-CE31-0019,SPlaSH,Recherche de planètes habitables avec SPIRou(2018), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
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FOS: Physical sciences ,Astrophysics ,01 natural sciences ,law.invention ,Atmosphere ,Telescope ,Planet ,law ,0103 physical sciences ,Hot Jupiter ,Mixing ratio ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,010303 astronomy & astrophysics ,ComputingMilieux_MISCELLANEOUS ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Exoplanet ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Bar (unit) - Abstract
We present the first exoplanet atmosphere detection made as part of the SPIRou Legacy Survey, a Large Observing Program of 300 nights exploiting the capabilities of SPIRou, the new near-infrared high-resolution (R ~ 70 000) spectro-polarimeter installed on the Canada-France-Hawaii Telescope (CFHT; 3.6-m). We observed two transits of HD 189733, an extensively studied hot Jupiter that is known to show prominent water vapor absorption in its transmission spectrum. When combining the two transits, we successfully detect the planet's water vapor absorption at 5.9 sigma using a cross-correlation t-test, or with a Delta BIC >10 using a log-likelihood calculation. Using a Bayesian retrieval framework assuming a parametrized T-P profile atmosphere models, we constrain the planet atmosphere parameters, in the region probed by our transmission spectrum, to the following values: VMR[H2O] = -4.4^{+0.4}_{-0.4}, and P_cloud >~ 0.2 bar (grey clouds), both of which are consistent with previous studies of this planet. Our retrieved water volume mixing ratio is slightly sub-solar although, combining it with the previously retrieved super-solar CO abundances from other studies would imply super-solar C/O ratio. We furthermore measure a net blue shift of the planet signal of -4.62^{+0.46}_{-0.44} km s-1, which is somewhat larger than many previous measurements and unlikely to result solely from winds in the planet's atmosphere, although it could possibly be explained by a transit signal dominated by the trailing limb of the planet. This large blue shift is observed in all the different detection/retrieval methods that were performed and in each of the two transits independently., 24 pages, 12 figures; accepted for publication in The Astronomical Journal
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- 2021
14. The Hubble PanCET program: Transit and Eclipse Spectroscopy of the Hot Jupiter WASP-74b
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Gregory W. Henry, Guangwei Fu, Vincent Bourrier, Thomas Mikal-Evans, Hannah R. Wakeford, Kevin B. Stevenson, Mercedes Lopez-Morales, Leonardo A. dos Santos, Antonio García Muñoz, David K. Sing, Joshua D. Lothringer, Munazza Alam, E. M. May, Nikolay Nikolov, and Drake Deming
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Space and Planetary Science ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,Astrophysics::Earth and Planetary Astrophysics ,Spectroscopy ,Astrophysics::Galaxy Astrophysics ,Eclipse ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Planets are like children with each one being unique and special. A better understanding of their collective properties requires a deeper understanding of each planet. Here we add the transit and eclipse spectra of hot Jupiter WASP-74b into the ever growing dataset of exoplanet atmosphere spectral library. With six transits and three eclipses using the Hubble Space Telescope (HST) and Spitzer Space Telescope (\textit{Spitzer}), we present the most complete and precise atmospheric spectra of WASP-74b. We found no evidence for TiO/VO nor super-Rayleigh scattering reported in previous studies. The transit shows a muted water feature with strong Rayleigh scattering extending into the infrared. The eclipse shows a featureless blackbody-like WFC3/G141 spectrum and a weak methane absorption feature in the Spitzer 3.6 $\mu m$ band. Future James Webb Space Telescope (JWST) follow up observations are needed to confirm these results., Comment: 23 pages, 18 figures, accepted to AJ
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- 2021
15. A Lyman-alpha transit left undetected: the environment and atmospheric behavior of K2-25b
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Vincent Bourrier, Keighley Rockcliffe, Zachory K. Berta-Thompson, Allison Youngblood, David Charbonneau, Marcel A. Agüeros, Alejandro Núñez, Andrew W. Mann, and Elisabeth R. Newton
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Atmospheric escape ,010308 nuclear & particles physics ,Flux ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Light curve ,01 natural sciences ,Exoplanet ,Earth radius ,Atmosphere ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Transit (astronomy) ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
K2-25b is a Neptune-sized exoplanet (3.45 Earth radii) that orbits its M4.5 host with a period of 3.48 days. Due to its membership in the Hyades Cluster, the system has a known age (727 +/- 75 Myr). K2-25b's youth and its similarities with Gl 436b suggested that K2-25b could be undergoing strong atmospheric escape. We observed two transits of K2-25b at Lyman-alpha using HST/STIS in order to search for escaping neutral hydrogen. We were unable to detect an exospheric signature, but placed an upper limit of (R_p/R_s) < 0.56 at 95% confidence by fitting the light curve of the Lyman-alpha red-wing, or < 1.20 in the blue-wing. We reconstructed the intrinsic Lyman-alpha profile of K2-25 to determine its Lyman-alpha flux, and analyzed XMM-Newton observations to determined its X-ray flux. Based on the total X-ray and extreme ultraviolet irradiation of the planet (8763 +/- 1049 erg/s/cm^2), we estimated the maximum energy-limited mass loss rate of K2-25b to be 10.6 x 10^10 g/s (0.56 Earth masses per 1 Gyr), five times larger than the similarly estimated mass loss rate of Gl 436b (2.2 x 10^10 g/s). The photoionization time is about 3 hours, significantly shorter than Gl 436b's 14 hours. A non-detection of a Lyman-alpha transit could suggest K2-25b is not significantly losing its atmosphere, or factors of the system are resulting in the mass loss being unobservable (e.g., atmosphere composition or the system's large high energy flux). Further observations could provide more stringent constraints.
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- 2021
16. Coupling the Atmospheric and Dynamical Evolution of Close-in Exoplanets
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Omar Attia and Vincent Bourrier
- Abstract
The vast majority of the detected exoplanets orbit in less than a month around their star, in extreme conditions unmet in the Solar System. The demographics of these close-in planets exhibit a striking feature: the lack of Neptune-size worlds on very short orbits, also dubbed the "Neptunian desert", which challenges our understanding of planetary formation and evolution. Two classes of mechanisms thought to play a predominant role in shaping the desert are orbital migration, which brings such planets close to their star, and atmospheric escape under the resulting increased irradiation. Yet, their relative roles remain poorly assessed, in part because we lack numerical models that couple the two processes with high precision and on secular timescales. To address this need, we developed a state-of-the-art model, the JADE code, which allows to self-consistently simulate the complete lifetime of a planet around its host star. On the dynamical side, the most impactful processes for close-in planets are implemented. The three-dimensional evolution of the orbit is modeled under stellar and planetary tidal forces, a relativistic correction, and the action of a distant perturbing body. On the atmospheric side, the vertical structure of the atmosphere is integrated over time based on its thermodynamical properties, composition, inner heating, and the evolving stellar irradiation, which results, in particular, in high-energy-induced photo-evaporation. We bench-marked the JADE code on the intriguing case of GJ436 b, an evaporating Neptune at the fringes of the desert whose eccentric and misaligned orbit despite an advanced age is still a puzzle. We showed that its exciting properties can be naturally explained by a strong interplay between eventful orbital and atmospheric histories. Particularly, a hidden companion on a wide orbit is able to trigger a Kozai—Lidov resonance, trapping the inner planet in high-eccentricity cycles for secular periods of time. During this resonance phase, the atmosphere pulsates in tune with the Kozai—Lidov cycles, which leads to stronger tides and an earlier migration than predicted from pure dynamical simulations. Nonetheless, the planet still starts to evaporate upon migrating billions of years after its formation, refining the paradigm that mass loss is dominant in the early age of close-in planets. Precise measurements of orbital and atmospheric tracers are crucial to constrain our models. Our joined approach to the understanding of past dynamical and atmospheric history, combined with the servicing of next-generation instruments, offers the best chance to shed light on the origins of the desert and the processes that forge the close-in planet population. Article: “The JADE code: Coupling secular exoplanetary dynamics and photo-evaporation” O. Attia, V. Bourrier, P. Eggenberger, C. Mordasini, H. Beust, D. Ehrenreich March 2021 Astronomy & Astrophysics, Volume 647, id.A40 DOI: 10.1051/0004-6361/202039452 Figure 1: Illustration of how the JADE code works. The evolution of the inner planet’s orbit as well as its atmospheric structure is monitored. The figure depicts the configuration of the system at two different secular time steps. It illustrates a typical case where the inner orbit shrank, circularized, and changed inclination, and where the envelope substantially eroded. Figure 2: Possible interplay between secular dynamics and atmospheric evolution of GJ436 b, as unveiled by the JADE code. Top: a Kozai—Lidov resonance induced by a distant perturber generates large eccentricity oscillations. Middle: the periodic rise in eccentricity translates into shorter mean planet–star distance and higher stellar irradiation. This causes the atmosphere to heat up and pulsate in tune with Kozai—Lidov cycles (blue), as opposed to the case where this dynamical feedback is not taken into account (orange). Bottom: the increases in radius lead to stronger tidal effects and thus a faster migration (blue), as compared to the case where the atmosphere is not modeled (orange).
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- 2021
17. The SOPHIE search for northern extrasolar planets. XVII. A wealth of new objects: Six cool Jupiters, three brown dwarfs, and 16 low-mass binary stars
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J. Rey, M. J. Hobson, C. Lovis, Vincent Bourrier, Magali Deleuil, N. Heidari, O. Mousis, Flavien Kiefer, S. Dalal, C. Moutou, Eder Martioli, P. Cortés-Zuleta, Nicola Astudillo-Defru, Johannes Sahlmann, Luc Arnold, Isabelle Boisse, L. Mignon, François Bouchy, Olivier Demangeon, Alexandre Santerne, Xavier Bonfils, Nathan Hara, Guillaume Hébrard, Rodrigo F. Díaz, Stéphane Udry, Nuno C. Santos, Damien Ségransan, X. Delfosse, T. Forveille, T. Lopez, S. G. Sousa, B. Brugger, P. A. Strøm, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and ANR-18-CE31-0019,SPlaSH,Recherche de planètes habitables avec SPIRou(2018)
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010504 meteorology & atmospheric sciences ,BROWN DWARFS ,SPECTROGRAPHS [INSTRUMENTATION] ,Brown dwarf ,FOS: Physical sciences ,RADIAL VELOCITIES [TECHNIQUES] ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,purl.org/becyt/ford/1 [https] ,ASTROMETRY ,Planet ,0103 physical sciences ,Binary star ,PLANETARY SYSTEMS ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Giant planet ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Planetary system ,Exoplanet ,Radial velocity ,Stars ,Astrophysics - Solar and Stellar Astrophysics ,LOW-MASS [STARS] ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Distinguishing classes within substellar objects and understanding their formation and evolution need larger samples of substellar companions such as exoplanets, brown dwarfs, and low-mass stars. In this paper, we look for substellar companions using radial velocity surveys of FGK stars with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We assign here the radial velocity variations of 27 stars to their orbital motion induced by low-mass companions. We also constrained their plane-of-the-sky motion using HIPPARCOS and Gaia Data Release 1 measurements, which constrain the true masses of some of these companions. We report the detection and characterization of six cool Jupiters, three brown dwarf candidates, and 16 low-mass stellar companions. We additionally update the orbital parameters of the low-mass star HD 8291 B, and we conclude that the radial velocity variations of HD 204277 are likely due to stellar activity despite resembling the signal of a giant planet. One of the new giant planets, BD+631405 b, adds to the population of highly eccentric cool Jupiters, and it is presently the most massive member. Two of the cool Jupiter systems also exhibit signatures of an additional outer companion. The orbital periods of the new companions span 30 days to 11.5 years, their masses 0.72 Jupiter mass to 0.61 Solar mass, and their eccentricities 0.04 to 0.88. These discoveries probe the diversity of substellar objects and low-mass stars, which will help constrain the models of their formation and evolution., Comment: 27 pages, 14 figures, 13 tables, Accepted in A&A
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- 2021
18. The Hubble PanCET program: Long-term chromospheric evolution and flaring activity of the M dwarf host GJ 3470
- Author
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Mercedes López-Morales, A. García Muñoz, David K. Sing, Panayotis Lavvas, Hannah R. Wakeford, Vincent Bourrier, A. Lecavelier, Gregory W. Henry, Jorge Sanz-Forcada, Thomas Mikal-Evans, L. A. dos Santos, David Ehrenreich, Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), and European Research Council (ERC)
- Subjects
individual: GJ 3470 [Planets and satellites] ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,Spectral line ,spectroscopic [Techniques] ,Luminosity ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Roche lobe ,Emission spectrum ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Line (formation) ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Radius ,Exoplanet ,star [Ultraviolet] ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,chromospheres [Stars] ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Exosphere - Abstract
Neptune-size exoplanets seem particularly sensitive to atmospheric evaporation, making it essential to characterize the stellar high-energy radiation that drives this mechanism. This is particularly important with M dwarfs, which emit a large and variable fraction of their luminosity in the UV and can display strong flaring behavior. The warm Neptune GJ3470b, hosted by an M2 dwarf, was found to harbor a giant hydrogen exosphere thanks to 3 transits observed with the HST/STIS. Here we report on 3 additional transit observations from the PanCET program, obtained with the HST/COS. These data confirm the absorption signature from GJ3470b's exosphere in the stellar Ly-alpha line and demonstrate its stability over time. No planetary signatures are detected in other lines, setting a 3sigma limit on GJ3470b's FUV radius at 1.3x its Roche lobe radius. We detect 3 flares from GJ3470. They show different spectral energy distributions but peak consistently in the Si III line, which traces intermediate-temperature layers in the transition region. These layers appear to play a particular role in GJ3470's activity as emission lines that form at lower or higher temperatures than Si III evolved differently over the long term. Based on the measured emission lines, we derive synthetic XUV spectra for the 6 observed quiescent phases, covering one year, as well as for the 3 flaring episodes. Our results suggest that most of GJ3470's quiescent high-energy emission comes from the EUV domain, with flares amplifying the FUV emission more strongly. The hydrogen photoionization lifetimes and mass loss derived for GJ3470b show little variation over the epochs, in agreement with the stability of the exosphere. Simulations informed by our XUV spectra are required to understand the atmospheric structure and evolution of GJ3470b and the role played by evaporation in the formation of the hot-Neptune desert., Comment: 21 pages, 18 figures, accepted in A&A
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- 2021
19. HST PanCET program: non-detection of atmospheric escape in the warm Saturn-sized planet WASP-29 b
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David K. Sing, Hannah R. Wakeford, Mercedes López-Morales, Alfred Vidal-Madjar, Panayotis Lavvas, A. Lecavelier des Etangs, Gregory W. Henry, L. A. dos Santos, Thomas Mikal-Evans, Vincent Bourrier, David Ehrenreich, A. García Muñoz, Jorge Sanz-Forcada, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dos Santos, L. A. [0000-0002-2248-3838], Sanz Forcada, J. [0000-0002-1600-7835], López Morales, M. [0000-0003-3204-8183], Sing, D. K. [0000-0001-6050-7645], García Muñoz, A. [0000-0003-1756-4825], Henry, G. W. [0000-0003-4155-8513], Lecavelier des Etangs, A. [0000-0002-5637-5253], Mikal Evans, T. [0000-0001-5442-1300], Centre National D'Etudes Spatiales (CNES), European Research Council (ERC), and Agencia Estatal de Investigación (AEI)
- Subjects
010504 meteorology & atmospheric sciences ,Gas giant ,kinematics and dynamics ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Luminosity ,Planet ,individual: Wasp-29 [Stars] ,Saturn ,Kinematics and dynamics [ISM] ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,individual ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Atmospheric escape ,atmospheres -ISM ,Astronomy and Astrophysics ,Stars ,Exoplanet ,Interstellar medium ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,chromospheres [Stars] ,atmospheres [Planets and satellites] ,chromospheres -planets and satellites ,Astrophysics::Earth and Planetary Astrophysics ,WASP-29 -stars ,Astrophysics - Earth and Planetary Astrophysics - Abstract
(Abridged) Short-period gas giant exoplanets are susceptible to intense atmospheric escape due to their large scale heights and strong high-energy irradiation. This process is thought to occur ubiquitously, but to date we have only detected direct evidence of atmospheric escape in hot Jupiters and warm Neptunes. The paucity of cases for intermediate, Saturn-sized exoplanets at varying levels of irradiation precludes a detailed understanding of the underlying physics in atmospheric escape of hot gas giants. Our objectives here are to assess the high-energy environment of the warm ($T_\mathrm{eq} = 970$ K) Saturn WASP-29 b and search for signatures of atmospheric escape. We used far-ultraviolet (FUV) observations from the Hubble Space Telescope to analyze the flux time series of H I, C II, Si III, Si IV, and N V during the transit of WASP-29 b. At 3$\sigma$ confidence, we rule out any in-transit absorption of H Ilarger than 92% in the Lyman-$\alpha$ blue wing and 19% in the red wing. We found an in-transit flux decrease of $39\%^{+12\%}_{-11\%}$ in the ground-state C II emission line at 133.45 nm. But due to this signal being significantly present in only one visit, it is difficult to attribute a planetary or stellar origin for the ground-state C II signal. We place 3$\sigma$ absorption upper limits of 40%, 49% and 24% for Si III, Si IV, and for excited-state C II at 133.57 nm, respectively. Low activity levels and the faint X-ray luminosity suggest that WASP-29 is an old, inactive star. An energy-limited approximation combined with the reconstructed EUV spectrum of the host suggests that the planet is losing its atmosphere at a rate of $4 \times 10^9$ g s$^{-1}$. The non-detection at Lyman-$\alpha$ could be partly explained by a low fraction of escaping neutral hydrogen, or by the state of fast radiative blow-out we infer from the reconstructed stellar Lyman-$\alpha$ line., Comment: 10 pages, 8 figures, accepted for publication in Astronomy & Astrophysics. v2 with a few text changes for consistency
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- 2021
20. Tuning in to the radio environment of HD189733b
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Vincent Bourrier, Robert D. Kavanagh, Joe Llama, Aline A. Vidotto, Christiane Helling, D. Ó Fionnagáin, Rim Fares, C. Moutou, Moira Jardine, and Peter J. Wheatley
- Subjects
010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Planet ,Primary (astronomy) ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,Absorption (electromagnetic radiation) ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Attenuation ,Stellar magnetic field ,Astronomy and Astrophysics ,LOFAR ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The hot Jupiter HD189733b is expected to be a source of strong radio emission, due to its close proximity to its magnetically active host star. Here, we model the stellar wind of its host star, based on reconstructed surface stellar magnetic field maps. We use the local stellar wind properties at the planetary orbit obtained from our models to compute the expected radio emission from the planet. Our findings show that the planet emits with a peak flux density within the detection capabilities of LOFAR. However, due to absorption by the stellar wind itself, this emission may be attenuated significantly. We show that the best time to observe the system is when the planet is near primary transit of the host star, as the attenuation from the stellar wind is lowest in this region., Comment: 4 pages, 4 figures. Proceedings of the IAU Symposium 354, "Solar and Stellar Magnetic Fields: Origins and Manifestations", June 2019
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- 2019
21. Spectrally resolved helium absorption from the extended atmosphere of a warm Neptune-mass exoplanet
- Author
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Jessica Spake, Vincent Bourrier, Francesco Pepe, A. Lecavelier des Etangs, David K. Sing, David Ehrenreich, Lorenzo Pino, Romain Allart, Aurélien Wyttenbach, C. Lovis, and Low Energy Astrophysics (API, FNWI)
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Multidisciplinary ,chemistry.chemical_element ,FOS: Physical sciences ,Scale height ,Astrophysics ,01 natural sciences ,Exoplanet ,Interstellar medium ,Atmosphere ,chemistry ,13. Climate action ,Planet ,Neptune ,0103 physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,010306 general physics ,Absorption (electromagnetic radiation) ,010303 astronomy & astrophysics ,Helium ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Stellar heating causes atmospheres of close-in exoplanets to expand and escape. These extended atmospheres are difficult to observe because their main spectral signature - neutral hydrogen at ultraviolet wavelengths - is strongly absorbed by interstellar medium. We report the detection of the near-infrared triplet of neutral helium in the transiting warm Neptune-mass exoplanet HAT-P-11b using ground-based, high-resolution observations. The helium feature is repeatable over two independent transits, with an average absorption depth of 1.08+/-0.05%. Interpreting absorption spectra with 3D simulations of the planet's upper atmosphere suggests it extends beyond 5 planetary radii, with a large scale height and a helium mass loss rate =< 3x10^5 g/s. A net blue-shift of the absorption might be explained by high-altitude winds flowing at 3 km/s from day to night-side., Submitted to Science: 14 March 2018; Accepted by Science: 8 November 2018; Published by Science: 6 December 2018 - This is the author's version of the work. It is posted here by permission of the AAAS for personal use, not for redistribution. The definitive version was published by Science on 6 December 2018 - Report: 17 pages; 4 figures - Supplementary material: 26 pages; 6 figures, 2 tables
- Published
- 2018
22. Star-planet interactions VI. Tides, stellar activity and planet evaporation
- Author
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Patrick Eggenberger, Vincent Bourrier, Gaël Buldgen, Cyril Georgy, Christoph Mordasini, Suvrat Rao, C. Pezzotti, Sylvia Ekström, and Georges Meynet
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Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010504 meteorology & atmospheric sciences ,Computer Science::Information Retrieval ,Evaporation ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,01 natural sciences ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Tidal interactions and planet evaporation processes impact the evolution of close-in star-planet systems. We study the impact of stellar rotation on these processes. We compute the time evolution of star-planet systems consisting of a planet with initial mass between 0.02 and 2.5 M$_{ Jup}$ (6 and 800 M$_{ Earth}$), in a quasi-circular orbit with an initial orbital distance between 0.01 and 0.10 au, around a solar-type star evolving from the Pre-Main-Sequence (PMS) until the end of the Main-Sequence (MS) phase. We account for the evolution of: the stellar structure, the stellar angular momentum due to tides and magnetic braking, the tidal interactions (equilibrium and dynamical tides in stellar convective zones), the mass-evaporation of the planet, and the secular evolution of the planetary orbit. We consider that at the beginning of the evolution, the proto-planetary disk has fully dissipated and planet formation is complete. Both a rapid initial stellar rotation, and a more efficient angular momentum transport inside the star, in general, contribute toward the enlargement of the domain which is devoid of planets after the PMS phase, in the plane of planet mass vs. orbital distance. Comparisons with the observed distribution of exoplanets orbiting solar mass stars, in the plane of planet mass vs. orbital distance (addressing the "Neptunian desert" feature), show an encouraging agreement with the present simulations, especially since no attempts have been made to fine-tune initial parameters of the models to fit the observations. We also obtain an upper limit for the orbital period of bare-core planets, that agrees with observations of the "radius valley" feature in the plane of planet radius vs. orbital period. The two effects, tides and planet evaporation, should be accounted for simultaneously and in a consistent way, with a detailed model for the evolution of the star., 15 pages, 13 figures. This manuscript has been accepted for publication in Astronomy & Astrophysics section 10. Planets and planetary systems
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- 2021
23. Modelling the influence of high-energy radiation on the atmospheric composition of the hot Jupiter HD 189733b
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Patrick Barth, Moira Jardine, Vincent Bourrier, Nathan J. Mayne, Paul B. Rimmer, Rim Fares, Peter J. Wheatley, Christiane Helling, Eva E. Stüeken, and Aline A. Vidotto
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Atmospheric composition ,Hot Jupiter ,Environmental science ,Atmospheric sciences ,Radiofrequency radiation - Abstract
Hot Jupiters provide valuable natural laboratories for studying potential contributions of high-energy radiation to prebiotic synthesis in the atmospheres of exoplanets. HD 189733b, a hot Jupiter orbiting a K star, is one of the most studied and best observed exoplanets. We combine XUV observations and 3D climate simulations to model the atmospheric composition and kinetic chemistry with the STAND2019 network. We show how XUV radiation, cosmic rays (CR), and stellar energetic particles (SEP) influence the chemistry of the atmosphere. We explore the effect that the change in the XUV radiation has over time, and we identify key atmospheric signatures of an XUV, CR, and SEP influx. 3D simulations of HD 189733b's atmosphere with the 3D Met Office Unified Model provide a fine grid of pressure-temperature profiles, consistently taking into account kinetic cloud formation. We apply HST and XMM-Newton/Swift observations obtained by the MOVES programmewhich provide combined X-ray and ultraviolet (XUV) spectra of the host star HD 189733 at 4 different points in time. We find that the differences in the radiation field between the irradiated dayside and the shadowed nightside lead to stronger changes in the chemical abundances than the variability of the host star's XUV emission. We identify ammonium (NH4+) and oxonium (H3O+) as fingerprint ions for the ionization of the atmosphere by both galactic cosmic rays and stellar particles. All considered types of high-energy radiation have an enhancing effect on the abundance of key organic molecules such as hydrogen cyanide (HCN), formaldehyde (CH2O), and ethylene (C2H4). The latter two are intermediates in the production pathway of the amino acid glycine (C2H5NO2) and abundant enough to be potentially detectable by JWST. Ultimately, we show that high energy processes potentially play an important role in prebiotic chemistry.P Barth et al., MOVES IV. Modelling the influence of stellar XUV-flux, cosmic rays, and stellar energetic particles on the atmospheric composition of the hot Jupiter HD 189733b, Monthly Notices of the Royal Astronomical Society, in press, DOI:10.1093/mnras/staa3989
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- 2021
24. The JADE code: Coupling secular exoplanetary dynamics and photo-evaporation
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O. Attia, Vincent Bourrier, Christoph Mordasini, Hervé Beust, Patrick Eggenberger, and David Ehrenreich
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010504 meteorology & atmospheric sciences ,530 Physics ,FOS: Physical sciences ,Perturbation (astronomy) ,01 natural sciences ,Atmosphere ,Planet ,0103 physical sciences ,Tidal force ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Atmospheric escape ,520 Astronomy ,Desert (particle physics) ,Astronomy ,Astronomy and Astrophysics ,JADE (particle detector) ,13. Climate action ,Space and Planetary Science ,Orbit (dynamics) ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Close-in planets evolve under extreme conditions, raising questions about their origins and current nature. Two predominant mechanisms are orbital migration, which brings them close to their star, and atmospheric escape under the resulting increased irradiation. Yet, their relative roles remain unclear because we lack models that couple the two mechanisms with high precision on secular timescales. To address this need, we developed the JADE code, which simulates the secular atmospheric and dynamical evolution of a planet around its star, and can include the perturbation induced by a distant third body. On the dynamical side, the 3D evolution of the orbit is modeled under stellar and planetary tidal forces, a relativistic correction, and the action of the distant perturber. On the atmospheric side, the vertical structure of the atmosphere is integrated over time based on its thermodynamical properties, inner heating, and the evolving stellar irradiation, which results, in particular, in photo-evaporation. The JADE code is benchmarked on GJ436 b, prototype of evaporating giants on eccentric, misaligned orbits at the edge of the hot Neptunes desert. We confirm that its orbital architecture is well explained by Kozai migration and unveil a strong interplay between its atmospheric and orbital evolution. During the resonance phase, the atmosphere pulsates in tune with the Kozai cycles, which leads to stronger tides and an earlier migration. This triggers a strong evaporation several Gyr after the planet formed, refining the paradigm that mass loss is dominant in the early age of close-in planets. This suggests that the edge of the desert could be formed of warm Neptunes whose evaporation was delayed by migration. It strengthens the importance of coupling atmospheric and dynamical evolution over secular timescales, which the JADE code will allow simulating for a wide range of systems., 20 pages, 2 figures, accepted in A&A
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- 2021
25. Six transiting planets and a chain of Laplace resonances in TOI-178
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A. Leleu, Nathan Hara, Rosanna H. Tilbrook, Matthew J. Hooton, Jack S. Acton, Giuseppina Micela, Heike Rauer, Francisco J. Pozuelos, Xavier Dumusque, Michael R. Goad, T. Bárczy, Andrew Collier Cameron, Francesco Pepe, G. Lo Curto, Rafael Rebolo, Juan Cabrera, Pedro Figueira, M. Buder, Willy Benz, Romain Allart, Oliver Turner, Enric Palle, Alexis M. S. Smith, Ignasi Ribas, F. Ratti, M. Steller, Richard G. West, James McCormac, A. Lecavelier des Etangs, Alexandre C. M. Correia, Daniel Sebastian, S. G. Sousa, Emmanuel Jehin, Mathias Beck, J. Schneider, François Bouchy, Baptiste Lavie, J.-B. Delisle, Liam Raynard, Roberto Ragazzoni, K. Lam, H. Venus, Kate Gudrun Isaak, Roi Alonso, C. Murray, Laetitia Delrez, Martti H. Kristiansen, Mario Damasso, A. Bonfanti, David Ehrenreich, Stéphane Udry, Samuel Gill, Sergio Hoyer, Lionel Garcia, V. Adibekyan, Carina M. Persson, Maximiliano Moyano, Beth A. Henderson, Giampaolo Piotto, Andrés Jordán, Samantha Thompson, Alexis Brandeker, Elsa Ducrot, Daniel Angerhausen, Nuno C. Santos, David Barrado, Xavier Bonfils, Vincent Bourrier, F. Verrecchia, Monika Lendl, Andrea Mehner, C. Broeg, M. R. Zapatero Osorio, Matthew R. Burleigh, D. Futyan, Damien Ségransan, Amaury H. M. J. Triaud, Mahmoudreza Oshagh, C. Allende Prieto, J. Asquier, B. O. Demory, Philippe Robutel, C. Corral Van Damme, Nicola Rando, Malcolm Fridlund, Gisbert Peter, Roland Ottensamer, Alessandro Sozzetti, Paolo Molaro, James S. Jenkins, Melvyn B. Davies, Jorge Lillo-Box, S. Chamberlain, Thomas Beck, P. Di Marcantonio, Carlos Martins, Maximilian N. Günther, Daniel Bayliss, Jacques Laskar, Peter J. Wheatley, P. P. Pedersen, Nicolas Thomas, Nicholas A. Walton, Göran Olofsson, Marko Sestovic, David R. Anderson, Artem Burdanov, Kevin Heng, Manuel Guedel, Jose I. Vines, A. García Muñoz, Edward Gillen, Valérie Van Grootel, T. G. Wilson, Michaël Gillon, Olivier Demangeon, D. Wolter, Demetrio Magrin, G. Polenta, G. Anglada Escudé, Stefano Cristiani, J. Haldemann, László L. Kiss, H. P. Osborn, Valerio Nascimbeni, Aleisha Hogan, Ennio Poretti, Pierre F. L. Maxted, S. C. C. Barros, G. Boué, Sébastien Charnoz, Benjamin F. Cooke, Nicolas Billot, C. Reimers, Don Pollacco, Gaetano Scandariato, Luca Fossati, Douglas R. Alves, J. I. González Hernández, Edward M. Bryant, Anders Erikson, Nelson J. Nunes, Wolfgang Baumjohann, Yann Alibert, A. Suárez Mascareño, Antoine Simon, Gy. M. Szabó, C. Lovis, Magali Deleuil, Andrea Fortier, Isabella Pagano, A. Bekkelien, G. Di Persio, Didier Queloz, Davide Gandolfi, Centre Hospitalier Régional Universitaire [Lille] (CHRU Lille), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, ITA, USA, GBR, FRA, DEU, AUT, BEL, CHL, DNK, NLD, PRT, SWE, CHE, HUN, 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), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Genève (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Swiss National Science Foundation, Agence Nationale de la Recherche (France), Science and Technology Facilities Council (UK), Belgian Science Policy Office, Université de Liège, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Alvarez, M. [0000-0002-6786-2620], Carrasco Martínez, J. M. [0000-0002-3029-5853], Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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Brightness ,planets and satellites: detection ,Laplace resonance ,010504 meteorology & atmospheric sciences ,spectroscopic techniques ,planets and satellites: dynamical evolution and stability ,Astrophysics ,01 natural sciences ,Transits ,spectroscopic [Techniques] ,techniques: photometric ,Planet ,QB460 ,QB Astronomy ,010303 astronomy & astrophysics ,planets and satellites dynamical evolution and stability ,QC ,Institut für Optische Sensorsysteme ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Laplace transform ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,520 Astronomy ,photmetric [Techniques] ,3rd-DAS ,dynamical evolution and stability [Planets and satellites] ,planets and satellites detection ,Astrophysics::Earth and Planetary Astrophysics ,Extrasolare Planeten und Atmosphären ,Techniques: photmetric ,FOS: Physical sciences ,Context (language use) ,SPECULOOS ,Earth radius ,Mean-motion resonance ,0103 physical sciences ,Celestial mechanics ,CHEOPS ,QB600 ,0105 earth and related environmental sciences ,photometric techniques ,TESS ,Scattering ,Leitungsbereich PF ,photometric [Techniques] ,Astronomy and Astrophysics ,celestial mechanics ,620 Engineering ,detection [Planets and satellites] ,QC Physics ,13. Climate action ,Space and Planetary Science ,NGTS ,Planetare Sensorsysteme ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Event (particle physics) ,techniques: spectroscopic ,QB799 ,Planets and satellites: Detection ,Planets and satellites: Dynamical evolution and stability ,Techniques: Photometric ,Techniques: Spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Leleu, A., et al., Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152to 2.87Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02to 0.177times the Earth's density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes., The authors acknowledge support from the Swiss NCCR PlanetS and the Swiss National Science Foundation. Y.A. and M.J.H. acknowledge the support of the Swiss National Fund under grant 200020_172746. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/M001296/1. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. SH acknowledges CNES funding through the grant 837319. Based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) project ST/M001962/1. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. V.A. acknowledges the support from FCT through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. ABr was supported by the SNSA. A.C. acknowledges support by CFisUC projects (UIDB/04564/2020 and UIDP/04564/2020), GRAVITY (PTDC/FIS-AST/7002/2020), ENGAGE SKA (POCI-01-0145-FEDER-022217), and PHOBOS (POCI-01-0145-FEDER-029932), funded by COMPETE 2020 and FCT, Portugal. This work was supported by FCT - Fundaçãopara a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa OperacionalCompetitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER- 032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). M.F. and C.M.P. gratefully acknowledgethe support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. E.G. gratefully acknowledges support from the David and Claudia Harding Foundation in the form of a WintonExoplanet Fellowship. M.G. is an F.R.S.-FNRS Senior Research Associate. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal programme RYC-2013-14875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. MNG ackowledges support from the MIT Kavli Institute as a Juan Carlos Torres Fellow. J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme.She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection forthe programme. J.S.J. acknowledges support by FONDECYT grant 1201371, and partial support from CONICYT project Basal AFB-170002. A.J. acknowledges support from ANID - Millennium Science Initiative - ICN12_009 and from FONDECYT project 1171208. P.M. acknowledges support from STFC research grant number ST/M001040/1. N.J.N is supported by the contract and exploratory project IF/00852/2015, and projects UID/FIS/04434/2019, PTDC/FIS-OUT/29048/2017, COMPETE2020: POCI-01-0145-FEDER-028987 & FCT: PTDC/FIS-AST/28987/2017. N.J.N is supported by the contract and exploratory project IF/00852/2015, and project PTDC/FIS-OUT/29048/2017. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). Acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This project has been supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grants GINOP-2.3.2-15-2016-00003, K-119517, K-125015, and the City of Szombathely under Agreement No. 67.177-21/2016. This research received funding from the MERAC foundation, from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no 803193/ BEBOP, and from the Science and Technology Facilites Council (STFC, grant no ST/S00193X/1). V.V.G. is an F.R.S-FNRS Research Associate. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. M. R. Z. O. acknowledges financial support from projects AYA2016-79425-C3-2-P and PID2019-109522GB-C51 from the Spanish Ministry of Science, Innovation and Universities.
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- 2021
26. The atmosphere of HD 209458b seen with ESPRESSO. No detectable planetary absorptions at high resolution
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Vardan Adibekyan, M. R. Zapatero Osorio, Yann Alibert, P. Di Marcantonio, François Bouchy, Cristina Martins, N. Casasayas-Barris, Francesco Borsa, Andrea Mehner, Giuseppina Micela, Paolo Molaro, S. Cristiani, Francesco Pepe, Nuno C. Santos, J. Lillo-Box, C. Lovis, Enric Palle, Vincent Bourrier, G. Lo Curto, Gang Chen, Rafael Rebolo, Fei Yan, O. D. S. Demangeon, J. I. González Hernández, V. D Odorico, Stéphane Udry, M. Stangret, S. G. Sousa, Mahmoudreza Oshagh, C. Allende Prieto, B. Lavie, A. Suárez Mascareño, P. Figueira, Alessandro Sozzetti, David Ehrenreich, R. Génova Santos, Romain Allart, Nelson J. Nunes, Hugo M. Tabernero, E. Poretti, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Yan, F. [0000-0001-9585-9034], Sozzetti, A. [0000-0002-7504-365X], Nunes, N. [0000-0002-3837-6914], Santos, N. [0000-0003-4422-2919], National Natural Science Foundation of China (NSFC), Deutsche Forschungsgemeinschaft (DFG), European Research Council (ERC), Fundacao para a Ciencia e a Tecnologia (FCT), Istituto Nazionale di Astrofisica (INAF), Agencia Estatal de Investigación (AEI), Swiss National Science Foundation (SNSF), ITA, ESP, PRT, and CHE
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individual: HD 209458b [Planets and satellites] ,Absorption spectroscopy ,Gas giant ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Astronomical spectroscopy ,spectroscopic [Techniques] ,Atmosphere ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,observational [Methods] ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,Line (formation) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Atmospheric models ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Light curve ,Wavelength ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We observed two transits of the iconic gas giant HD 209458b between 380 and 780 nm, using the high-resolution ESPRESSO spectrograph. The derived planetary transmission spectrum exhibits features at all wavelengths where the parent star shows strong absorption lines, for example, NaI, MgI, FeI, FeII, CaI, VI, H$\alpha$, and KI. We interpreted these features as the signature of the deformation of the stellar line profiles due to the Rossiter-McLaughlin effect, combined with the centre-to-limb effects on the stellar surface, which is in agreement with similar reports recently presented in the literature. We also searched for species that might be present in the planetary atmosphere but not in the stellar spectra, such as TiO and VO, and obtained a negative result. Thus, we find no evidence of any planetary absorption, including previously reported NaI, in the atmosphere of HD 209458b. The high signal-to-noise ratio in the transmission spectrum allows us to compare the modelled deformation of the stellar lines in assuming different one-dimensional stellar atmospheric models. We conclude that the differences among various models and observations remain within the precision limits of the data. However, the transmission light curves are better explained when the centre-to-limb variation is not included in the computation and only the Rossiter-McLaughlin deformation is considered. This demonstrates that ESPRESSO is currently the best facility for spatially resolving the stellar surface spectrum in the optical range using transit observations and carrying out empirical validations of stellar models., Comment: 21 pages, 19 figures. Accepted
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- 2021
27. ESPRESSO high-resolution transmission spectroscopy of WASP-76 b
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S. Hojjatpanah, L. Genolet, Matteo Genoni, Paolo Molaro, Edoardo Maria Alberto Redaelli, T. Bandy, A. Segovia, Jorge Lillo-Box, Diogo Alves, A. Suárez Mascareño, Olivier Demangeon, Vincent Bourrier, João P. Faria, Julia V. Seidel, F. Tenegi, P. Figueira, Yann Alibert, Danuta Sosnowska, Giorgio Pariani, Matteo Aliverti, Antonino Bianco, M. Moschetti, J. Knudstrup, B. Delabre, M. Amate, Romain Allart, Olaf Iwert, Valentina D'Odorico, Francesco Borsa, Hugo M. Tabernero, J. L. Lizon, M. R. Zapatero Osorio, G. Avila, Paolo Conconi, Vardan Adibekyan, Alexandre Cabral, Ennio Poretti, Mário J. P. F. G. Monteiro, J. L. Rasilla, Andrea Mehner, Antonio Gouveia Oliveira, Filippo Maria Zerbi, Alessandro Sozzetti, François Bouchy, Luca Pasquini, Baptiste Lavie, Marco Landoni, E. Mueller, S. Deiries, Luca Oggioni, Nelson J. Nunes, R. Génova Santos, Claudio Cumani, João Coelho, S. C. C. Barros, Denis Mégevand, J. I. González Hernández, S. Santana-Tschudi, Paolo Santin, M. Affolter, Giuseppina Micela, Alessio Zanutta, G. Lo Curto, A. Fragoso, C. Allende Prieto, Pedro Santos, J. H. C. Martins, Antonio Manescau, Florian Kerber, Willy Benz, Hans Dekker, David Ehrenreich, Paolo Spanò, Rafael Rebolo, Xavier Dumusque, Cristina Martins, Núria Casasayas-Barris, Francesco Pepe, S. G. Sousa, Stefano Cristiani, C. Broeg, C. Maire, Andrea Modigliani, Stéphane Udry, Nuno C. Santos, Marco Riva, C. Lovis, Enric Palle, I. Hughes, P. Di Marcantonio, ITA, ESP, PRT, and CHE
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530 Physics ,Continuum (design consultancy) ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Molecular physics ,Spectral line ,Atmosphere ,Espresso ,Planet ,0103 physical sciences ,Irradiation ,010303 astronomy & astrophysics ,Spectrograph ,Solar and Stellar Astrophysics (astro-ph.SR) ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,520 Astronomy ,Astronomy and Astrophysics ,500 Science ,620 Engineering ,Transmission (telecommunications) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Aims. We report on ESPRESSO high-resolution transmission spectroscopic observations of two primary transits of the highly-irradiated, ultra-hot Jupiter-size planet WASP-76b. We investigate the presence of several key atomic and molecular features of interest that may reveal the atmospheric properties of the planet. Methods. We extracted two transmission spectra of WASP-76b with R approx 140,000 using a procedure that allowed us to process the full ESPRESSO wavelength range (3800-7880 A) simultaneously. We observed that at a high signal-to-noise ratio, the continuum of ESPRESSO spectra shows wiggles that are likely caused by an interference pattern outside the spectrograph. To search for the planetary features, we visually analysed the extracted transmission spectra and cross-correlated the observations against theoretical spectra of different atomic and molecular species. Results. The following atomic features are detected: Li I, Na I, Mg I, Ca II, Mn I, K I, and Fe I. All are detected with a confidence level between 9.2 sigma (Na I) and 2.8 sigma (Mg I). We did not detect the following species: Ti I, Cr I, Ni I, TiO, VO, and ZrO. We impose the following 1 sigma upper limits on their detectability: 60, 77, 122, 6, 8, and 8 ppm, respectively. Conclusions. We report the detection of Li I on WASP-76b for the first time. In addition, we found the presence of Na I and Fe I as previously reported in the literature. We show that the procedure employed in this work can detect features down to the level of ~ 0.1 % in the transmission spectrum and ~ 10 ppm by means of a cross-correlation method. We discuss the presence of neutral and singly ionised features in the atmosphere of WASP-76b., 20 pages, 19 figures, accepted for publication in Astronomy and Astrophysics
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28. The SOPHIE search for northern extrasolar planets: XVIII. Six new cold jupiters including one of the most eccentric exoplanet orbits
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Nathan Hara, M. J. Hobson, João P. Faria, Alexandre Santerne, Stéphane Udry, Vincent Bourrier, X. Delfosse, François Bouchy, Rodrigo F. Díaz, J. D. Camacho, Guillaume Hébrard, Olivier Demangeon, Xavier Bonfils, Tiago L. Campante, T. Lopez, Isabelle Boisse, S. Dalal, Flavien Kiefer, Susana Sousa, Nuno C. Santos, C. Moutou, T. Forveille, Luc Arnold, J. Rey, Benard Nsamba, Maria Tsantaki, P. A. Strøm, Johannes Sahlmann, Magali Deleuil, Nicola Astudillo-Defru, and N. Heidari
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010504 meteorology & atmospheric sciences ,Gas giant ,Population ,FOS: Physical sciences ,Context (language use) ,RADIAL VELOCITIES [TECHNIQUES] ,Astrophysics ,01 natural sciences ,Jupiter ,purl.org/becyt/ford/1 [https] ,Planet ,0103 physical sciences ,DETECTION [PLANETS AND SATELLITES] ,Transit (astronomy) ,education ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,education.field_of_study ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Exoplanet ,Radial velocity ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Context. Due to their low transit probability, the long-period planets are, as a population, only partially probed by transit surveys. Radial velocity surveys thus have a key role to play, in particular for giant planets. Cold Jupiters induce a typical radial velocity semi-amplitude of 10m.s^{-1}, which is well within the reach of multiple instruments that have now been in operation for more than a decade. Aims. We take advantage of the ongoing radial velocity survey with the sophie high-resolution spectrograph, which continues the search started by its predecessor elodie to further characterize the cold Jupiter population. Methods. Analyzing the radial velocity data from six bright solar-like stars taken over a period of up to 15 years, we attempt the detection and confirmation of Keplerian signals. Results. We announce the discovery of six planets, one per system, with minimum masses in the range 2.99-8.3 Mjup and orbital periods between 200 days and 10 years. The data do not provide enough evidence to support the presence of additional planets in any of these systems. The analysis of stellar activity indicators confirms the planetary nature of the detected signals. Conclusions. These six planets belong to the cold and massive Jupiter population, and four of them populate its eccentric tail. In this respect, HD 80869 b stands out as having one of the most eccentric orbits, with an eccentricity of 0.862^{+0.028}_{-0.018}. These planets can thus help to better constrain the migration and evolution processes at play in the gas giant population. Furthermore, recent works presenting the correlation between small planets and cold Jupiters indicate that these systems are good candidates to search for small inner planets., 24 pages, 12 figures, Accepted for publication in Astronomy & Astrophysics
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29. The near-UV transit of HD 189733b with the XMM-Newton optical monitor
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Vincent Bourrier, Maria Steinrueck, Alain Lecavelier des Etangs, David Ehrenreich, George King, Tom Louden, Lia Corrales, Panayotis Lavvas, Peter J. Wheatley, University of Michigan [Ann Arbor], University of Michigan System, University of Warwick [Coventry], Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), University of Arizona, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites: atmospheres ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,ultraviolet: planetary systems ,FOS: Physical sciences ,Astronomy and Astrophysics ,Radius ,Astrophysics ,01 natural sciences ,3. Good health ,planets and satellites: individual: HD 189733b ,Wavelength ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Hot Jupiter ,Roche lobe ,Absorption (logic) ,Transit (astronomy) ,Spectral resolution ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present analysis of XMM-Newton Optical Monitor observations in the near-ultraviolet of HD 189733, covering twenty primary transits of its hot Jupiter planet. The transit is clearly detected with both the UVW2 and UVM2 filters, and our fits to the data reveal transit depths in agreement with that observed optically. The measured depths correspond to radii of $1.059^{+0.046}_{-0.050}$ and $0.94^{+0.15}_{-0.17}$ times the optically-measured radius (1.187 R$_{\rm J}$ at 4950 \r{A}) in the UVW2 and UVM2 bandpasses, respectively. We also find no statistically significant variation in the transit depth across the 8 year baseline of the observations. We rule out extended broadband absorption towards or beyond the Roche lobe at the wavelengths investigated, although observations with higher spectral resolution are required to determine if absorption out to those distances from the planet is present in individual near-UV lines., Comment: 7 pages, 7 figures, 3 tables; accepted for publication in MNRAS
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30. The key impact of the host star's rotational history on the evolution of TOI-849b
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C. Pezzotti, Vincent Bourrier, O. Attia, Gaël Buldgen, and Patrick Eggenberger
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Star (game theory) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Rotation ,Omega ,Atmosphere ,Orbit ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Planet ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Planetary migration ,Envelope (waves) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Context. TOI-849b is one of the few planets populating the hot-Neptune desert and it is the densest Neptune-sized one discovered so far. Its extraordinary proximity to the host star, together with the absence of a massive H/He envelope on top of the 40.8 M⊕ rocky core, calls into question the role played by the host star in the evolution of the system. Aims. We aim to study the impact of the host star’s rotational history on the evolution of TOI-849b, particularly focussing on the planetary migration due to dynamical tides dissipated in the stellar convective envelope, and on the high-energy stellar emission. Methods. Rotating stellar models of TOI-849 are coupled to our orbital evolution code to study the evolution of the planetary orbit. The evolution of the planetary atmosphere is studied by means of the JADE code, which uses realistic X-ray and extreme-ultraviolet (XUV) fluxes provided by our rotating stellar models. Results. Assuming that the planet was at its present-day position (ain = 0.01598 AU) at the protoplanetary disc dispersal, with mass 40.8 M⊕, and considering a broad range of host star initial surface rotation rates (Ωin ∈ [3.2, 18] Ω⊙), we find that only for Ωin ≤ 5 Ω⊙ do we reproduce the current position of the planet, given that for Ωin > 5 Ω⊙ its orbit is efficiently deflected by dynamical tides within the first ∼40 Myr of evolution. We also simulated the evolution of the orbit for values of ain ≠ 0.01598 AU for each of the considered rotational histories, confirming that the only combination suited to reproduce the current position of the planet is given by ain = 0.01598 AU and Ωin ≤ 5 Ω⊙. We tested the impact of increasing the initial mass of the planet on the efficiency of tides, finding that a higher initial mass (Min = 1 MJup) does not change the results reported above. Based on these results we computed the evolution of the planetary atmospheres with the JADE code for a large range of initial masses above a core mass of 40.8 M⊕, finding that the strong XUV-flux received by the planet is able to remove the entirety of the envelope within the first 50 Myr, even if it formed as a Jupiter-mass planet.
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31. Revisiting Kepler-444. II. Rotational, orbital and high-energy fluxes evolution of the system
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C. Pezzotti, Georges Meynet, Patrick Eggenberger, Christoph Mordasini, Gaël Buldgen, and Vincent Bourrier
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics ,Planetary system ,Rotation ,01 natural sciences ,Luminosity ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Planetary mass ,Stellar evolution ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics ,0105 earth and related environmental sciences ,Line (formation) - Abstract
Context.Kepler-444 is one of the oldest planetary systems known thus far. Its peculiar configuration consisting of five sub-Earth-sized planets orbiting the companion to a binary stellar system makes its early history puzzling. Moreover, observations of HI-Lyαvariations raise many questions about the potential presence of escaping atmospheres today.Aims.We aim to study the orbital evolution of Kepler-444-d and Kepler-444-e and the impact of atmospheric evaporation on Kepler-444-e.Methods.Rotating stellar models of Kepler-444-A were computed with the Geneva stellar evolution code and coupled to an orbital evolution code, accounting for the effects of dynamical, equilibrium tides and atmospheric evaporation. The impacts of multiple stellar rotational histories and X-ray and extreme ultraviolet (XUV) luminosity evolutionary tracks are explored.Results.Using detailed rotating stellar models able to reproduce the rotation rate of Kepler-444-A, we find that its observed rotation rate is perfectly in line with what is expected for this old K0-type star, indicating that there is no reason for it to be exceptionally active as would be required to explain the observed HI-Lyαvariations from a stellar origin. We show that given the low planetary mass (~0.03 M⊕) and relatively large orbital distance (~0.06 AU) of Kepler-444-d and e, dynamical tides negligibly affect their orbits, regardless of the stellar rotational history considered. We point out instead how remarkable the impact is of the stellar rotational history on the estimation of the lifetime mass loss for Kepler-444-e. We show that, even in the case of an extremely slow rotating star, it seems unlikely that such a planet could retain a fraction of the initial water-ice content if we assume that it formed with a Ganymede-like composition.
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32. Spi-OPS: Spitzer and CHEOPS confirm the near-polar orbit of MASCARA-1 b and reveal a hint of dayside reflection
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T. Bárczy, Willy Benz, Sz. Csizmadia, Sergio Hoyer, David Ehrenreich, Nicholas A. Walton, Carina M. Persson, T. G. Wilson, Anders Erikson, Kevin Heng, H. Parviainen, M. Deleuil, Michaël Gillon, Yann Alibert, Ignasi Ribas, Olivier Demangeon, Don Pollacco, Demetrio Magrin, Juan Cabrera, Gy. M. Szabó, F. Ratti, Gaetano Scandariato, Luca Fossati, Mahmoudreza Oshagh, A. Bonfanti, Giampaolo Piotto, Nicolas Billot, G. Anglada Escudé, Alexis Brandeker, Gisbert Peter, Roberto Ragazzoni, Matthew J. Hooton, Heike Rauer, X. Bonfils, Nicola Rando, Malcolm Fridlund, Antoine Simon, C. Lovis, László L. Kiss, Göran Olofsson, Roi Alonso, Stéphane Udry, Enric Palle, S. G. Sousa, Andrea Fortier, M.-D. Busch, C. Broeg, Nuno C. Santos, David Barrado, Damien Ségransan, Roland Ottensamer, M. Steller, A. Luntzer, A. Deline, B. Ulmer, B. O. Demory, Brett M. Morris, Thomas Beck, Nicolas Thomas, Valerio Nascimbeni, Pierre F. L. Maxted, S. C. C. Barros, Sébastien Charnoz, Wolfgang Baumjohann, Isabella Pagano, Valérie Van Grootel, D. Futyan, Jacques Laskar, K. Jones, A. Lecavelier des Etangs, Mathias Beck, Alexis M. S. Smith, Laetitia Delrez, Vincent Bourrier, A. Collier Cameron, Melvyn B. Davies, Manuel Güdel, Kate Gudrun Isaak, Monika Lendl, Davide Gandolfi, Jacopo Farinato, S. Sulis, Didier Queloz, D. Kitzmann, Sébastien Salmon, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Swiss National Science Foundation, Science and Technology Facilities Council (UK), Fundação para a Ciência e a Tecnologia (Portugal), European Research Council, European Commission, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Space Agency, and Generalitat de Catalunya
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Astrophysics ,01 natural sciences ,Geometric albedo ,QB460 ,Planets and satellites: atmospheres ,QB Astronomy ,610 Medicine & health ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,520 Astronomy ,3rd-DAS ,techniques photometric ,symbols ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,individual: MASCARA-1 b [Planets and satellites] ,Photometry (optics) ,symbols.namesake ,Bond albedo ,planets and satellites individual ,0103 physical sciences ,Hot Jupiter ,planets and satellites physical evolution ,MASCARA-1 b ,Gravity darkening ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,QB600 ,physical evolution [Planets and satellites] ,MCC ,010308 nuclear & particles physics ,Stellar rotation ,photometric [Techniques] ,Planets and satellites: individual: MASCARA-1 b ,Astronomy and Astrophysics ,620 Engineering ,Light curve ,Stars ,QC Physics ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,planets and satellites atmospheres ,Planets and satellites: physical evolution ,Techniques: photometric ,570 Life sciences ,biology ,Astrophysics - Earth and Planetary Astrophysics - Abstract
M. J. Hooton et al., [Context] The light curves of tidally locked hot Jupiters transiting fast-rotating, early-type stars are a rich source of information about both the planet and star, with full-phase coverage enabling a detailed atmospheric characterisation of the planet. Although it is possible to determine the true spin–orbit angle Ψ – a notoriously difficult parameter to measure – from any transit asymmetry resulting from gravity darkening induced by the stellar rotation, the correlations that exist between the transit parameters have led to large disagreements in published values of Ψ for some systems., [Aims] We aimed to study these phenomena in the light curves of the ultra-hot Jupiter MASCARA-1 b, which is characteristically similar to well-studied contemporaries such as KELT-9 b and WASP-33 b., [Methods] We obtained optical CHaracterising ExOPlanet Satellite (CHEOPS) transit and occultation light curves of MASCARA-1 b, and analysed them jointly with a Spitzer/IRAC 4.5 μm full-phase curve to model the asymmetric transits, occultations, and phase-dependent flux modulation. For the latter, we employed a novel physics-driven approach to jointly fit the phase modulation by generating a single 2D temperature map and integrating it over the two bandpasses as a function of phase to account for the differing planet–star flux contrasts. The reflected light component was modelled using the general ab initio solution for a semi-infinite atmosphere., [Results] When fitting the CHEOPS and Spitzer transits together, the degeneracies are greatly diminished and return results consistent with previously published Doppler tomography. Placing priors informed by the tomography achieves even better precision, allowing a determination of Ψ = 72.1−2.4+2.5 deg. From the occultations and phase variations, we derived dayside and nightside temperatures of 3062−68+66 K and 1720 ± 330 K, respectively.Our retrieval suggests that the dayside emission spectrum closely follows that of a blackbody. As the CHEOPS occultation is too deep to be attributed to blackbody flux alone, we could separately derive geometric albedo Ag = 0.171−0.068+0.066 and spherical albedo As = 0.266−0.100+0.097 from the CHEOPS data, and Bond albedoAB = 0.057−0.101+0.083 from the Spitzer phase curve.Although small, the Ag and As indicate that MASCARA-1 b is more reflective than most other ultra-hot Jupiters, where H− absorption is expected to dominate., [Conclusions] Where possible, priors informed by Doppler tomography should be used when fitting transits of fast-rotating stars, though multi-colour photometry may also unlock an accurate measurement of Ψ. Our approach to modelling the phase variations at different wavelengths provides a template for how to separate thermal emission from reflected light in spectrally resolved James Webb Space Telescope phase curve data., Y.A. acknowledge the support of the Swiss National Fund under grant 200020_172746. S.H. gratefully acknowledges CNES funding through the grant 837319. D.K. acknowledges partial financial support from the Center for Space and Habitability (CSH), the PlanetS National Center of Competence in Research (NCCR), and the Swiss National Science Foundation and the Swiss-based MERAC Foundation. A.C.C. and T.G.W. acknowledge support from STFC consolidated grant number ST/M001296/1. P.M. acknowledges support from STFC research grant number ST/M001040/1. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX). A.Br. was supported by the SNSA. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizacão by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER- 032113, PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiologí a (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F., and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES. grant agreement no. 724427). D.E. acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. C.M.P. and M.F. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 ‘Gaseousor rocky? Unveiling the nature of small worlds’. M.G. is an F.R.S.-FNRS Senior Research Associate. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. Acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This project has been supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grants GINOP-2.3.2-15-2016-00003, K-119517, K-125015, and the City of Szombathely under Agreement No. 67.177-21/2016., , , ,
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33. CHEOPS precision phase curve of the Super-Earth 55 Cancri e
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Luca Fossati, M. Fridlund, Giampaolo Piotto, M. Beck, D. L. Pollacco, G. Olofsson, M. Deleuil, K. G. Isaak, Alexis Brandeker, P. Guterman, A. Lecavelier des Etangs, Nicolas Billot, Heike Rauer, Michaël Gillon, Anders Erikson, N. C. Santos, Laetitia Delrez, Andrew Collier Cameron, T. G. Wilson, Wolfgang Baumjohann, D. Segransan, Yann Alibert, C. Lovis, Kevin Heng, C. Broeg, Gisbert Peter, B. Ulmer, Manuel Guedel, B. O. Demory, Sergio Hoyer, Monika Lendl, Mahmoudreza Oshagh, Melvyn B. Davies, Brett M. Morris, J. Cabrera, Roberto Ragazzoni, Gy. M. Szabó, D. Queloz, Vincent Bourrier, S. G. Sousa, A. García Muñoz, Davide Gandolfi, Jacques Laskar, Willy Benz, S. Charnoz, Francisco J. Pozuelos, T. Bárczy, Nicola Rando, Thomas Beck, D. De Miguel Ferreras, David Ehrenreich, Pierre F. L. Maxted, G. Anglada Escudé, S. C. C. Barros, H. G. Floren, A. Deline, László L. Kiss, A. Bekkelien, M. Steller, D. Futyan, G. Scandariato, A. M. Smith, S. Sulis, I. Pagano, O. D. S. Demangeon, I. Ribas, M. Lieder, A. E. Simon, X. Bonfils, Andrea Fortier, Maria Bergomi, Roland Ottensamer, V. Nascimbeni, Demetrio Magrin, N. Thomas, David Barrado, Enric Palle, A. Pizarro Rubio, Roi Alonso, Stéphane Udry, N. A. Walton, Valérie Van Grootel, Cavendish Laboratory, University of Cambridge [UK] (CAM), Stockholm University, Institut für Festkörper- und Materialphysik, Technische Universität Dresden, Technische Universität Dresden = Dresden University of Technology (TU Dresden), 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), Center for Space and Habitability (CSH), University of Bern, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Swiss Space Office, Swiss National Science Foundation, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Queloz, Didier [0000-0002-3012-0316], Walton, Nicholas [0000-0003-3983-8778], and Apollo - University of Cambridge Repository
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Atmospheres ,010504 meteorology & atmospheric sciences ,55 Cnc ,individual: 55 Cnc e [Planets and satellites] ,Astrophysics ,01 natural sciences ,techniques: photometric ,Spitzer Space Telescope ,Planet ,QB460 ,Methods ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Observational ,Instrumentation ,QC ,planets and satellites: individual: 55 Cnc e ,Eclipse ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,planets and satellites: atmospheres ,Super-Earth ,520 Astronomy ,Planets and Satellites ,Exoplanet ,instrumentation: photometers ,Amplitude ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,methods: observational ,individual: 55 Cnc [Stars] ,FOS: Physical sciences ,Individual ,Photometric ,Photometry (optics) ,stars: individual: 55 Cnc ,0103 physical sciences ,observational [Methods] ,invidual: 55 Cnc [Stars] ,QB600 ,0105 earth and related environmental sciences ,MCC ,Photometers ,Stars: invidual: 55 Cnc ,photometric [Techniques] ,Astronomy and Astrophysics ,DAS ,Phase curve ,620 Engineering ,Stars ,Techniques ,photometers [Instrumentation] ,QC Physics ,13. Climate action ,Space and Planetary Science ,Instrumentation: photometers ,Methods: observational ,Planets and satellites: atmospheres ,Planets and satellites: individual: 55 Cnc e ,Stars: individual: 55 Cnc ,Techniques: photometric ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,55 Cnc e ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Morris, B. M. et al., [Context] 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. [Aims] We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. [Methods] We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. [Results] We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. [Conclusions] This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time., Centre of Competence in Research (NCCR) supported by the Swiss National Science Foundation (SNSF). CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The Swiss participation to CHEOPS has been supported by the Swiss Space Office (SSO) in the framework of the Prodex programme and the Activités Nationales Complémentaires (ANC), the Universities of Bern and Geneva as well as of the NCCR PlanetS and the Swiss National Science Foundation. This work benefited from support from the Swiss National Science Foundation (PP00P2-163967 and PP00P2-190080). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). X.B., S.C., D.G., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/R000824/1. This project was supported by the CNES. S.H. gratefully acknowledges CNES funding through the grant 837319. P.M. acknowledges support from STFC consolidated grant number ST/M001040/1. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme.
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- 2021
34. ESPRESSO at VLT. On-sky performance and first results
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G. Avila, Alexandre Cabral, Andrea Mehner, S. Deiries, C. Allende Prieto, Vardan Adibekyan, Roberto Cirami, Manuel Abreu, Luca Pasquini, M. Affolter, Luca Oggioni, Igor Coretti, Nelson J. Nunes, J. Knudstrup, G. Lo Curto, Nuno C. Santos, C. Lovis, Enric Palle, Damien Ségransan, Filippo Maria Zerbi, Yann Alibert, Jose Luis Rasilla, I. Hughes, A. Fragoso, S. Santana Tschudi, T. M. Schmidt, Romain Allart, Florian Kerber, Antonino Bianco, R. Génova Santos, Mahmoudreza Oshagh, Matteo Genoni, A. Segovia, João P. Faria, Rafael Rebolo, Vincent Bourrier, M. Moschetti, Olivier Demangeon, M. A. Monteiro, Marco Landoni, Danuta Sosnowska, Valentina D'Odorico, Willy Benz, P. Figueira, François Bouchy, Baptiste Lavie, Andrea Modigliani, Marco Riva, L. Genolet, Matteo Aliverti, Paolo Santin, B. Delabre, Paolo Molaro, J. L. Lizon, F. Tenegi, M. R. Zapatero Osorio, Antonio Gouveia Oliveira, Francesco Pepe, Paolo Conconi, Stéphane Udry, Guido Cupani, Hugo M. Tabernero, S. G. Sousa, José Manuel Rebordão, Hans Dekker, T. Bandy, Ennio Poretti, S. C. C. Barros, D. Álvarez, A. Suárez Mascareño, Stefano Cristiani, C. Maire, J. I. González Hernández, Giuseppina Micela, Giorgio Calderone, V. Baldini, Xavier Dumusque, Alessandro Sozzetti, Claudio Cumani, João Coelho, M. Amate, Francesco Borsa, Olaf Iwert, Denis Mégevand, Cristina Martins, Antonio Manescau, Alessio Zanutta, Michael T. Murphy, C. Broeg, Mario Damasso, M. Mayor, Jorge Lillo-Box, Pedro Santos, P. Di Marcantonio, P. Spano, Edoardo Maria Alberto Redaelli, Diogo Alves, Giorgio Pariani, Mário J. P. F. G. Monteiro, David Ehrenreich, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Swiss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), European Research Council (ERC), Agencia Estatal de Investigación (AEI), and Australian Research Council
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Accuracy and precision ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,01 natural sciences ,7. Clean energy ,law.invention ,010309 optics ,Telescope ,Espresso ,Observatory ,law ,0103 physical sciences ,miscellaneous [Cosmology] ,spectrographs [Instrumentation] ,010303 astronomy & astrophysics ,Spectrograph ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Very Large Telescope ,radial velocities [Techniques] ,Asteroseismology ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,detection [Planets and satellites] ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
ESPRESSO is the new high-resolution spectrograph of ESO's Very-Large Telescope (VLT). It was designed for ultra-high radial-velocity precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UT) of the VLT at a spectral resolving power of 140,000 or 190,000 over the 378.2 to 788.7 nm wavelength range, or with all UTs together, turning the VLT into a 16-m diameter equivalent telescope in terms of collecting area, while still providing a resolving power of 70,000. We provide a general description of the ESPRESSO instrument, report on the actual on-sky performance, and present our Guaranteed-Time Observation (GTO) program with its first results. ESPRESSO was installed on the Paranal Observatory in fall 2017. Commissioning (on-sky testing) was conducted between December 2017 and September 2018. The instrument saw its official start of operations on October 1st, 2018, but improvements to the instrument and re-commissioning runs were conducted until July 2019. The measured overall optical throughput of ESPRESSO at 550 nm and a seeing of 0.65 arcsec exceeds the 10% mark under nominal astro-climatic conditions. We demonstrate a radial-velocity precision of better than 25 cm/s during one night and 50 cm/s over several months. These values being limited by photon noise and stellar jitter show that the performanceis compatible with an instrumental precision of 10 cm/s. No difference has been measured across the UTs neither in throughput nor RV precision. The combination of the large collecting telescope area with the efficiency and the exquisite spectral fidelity of ESPRESSO opens a new parameter space in RV measurements, the study of planetary atmospheres, fundamental constants, stellar characterisation and many other fields., 26 pages, 28 figures
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- 2021
35. Into the storm
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Yann Alibert, Olivier Demangeon, Andrea Mehner, Aurélien Wyttenbach, Nuno C. Santos, H. J. Hoeijmakers, C. Lovis, Enric Palle, Hugo M. Tabernero, S. G. Sousa, M. R. Zapatero Osorio, Vincent Bourrier, N. Casasayas-Barris, Paolo Molaro, Francesco Borsa, P. Di Marcantonio, J. I. González Hernández, N. J. Nunes, Stefano Cristiani, Julia V. Seidel, P. Figueira, Vardan Adibekyan, Alessandro Sozzetti, Francesco Pepe, Romain Allart, Jorge Lillo-Box, Cristina Martins, David Ehrenreich, and L. Pino
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530 Physics ,Gas giant ,Line: profiles ,FOS: Physical sciences ,Techniques: spectroscopic ,Astrophysics ,Astrophysics - Earth and planetary astrophysics ,01 natural sciences ,Atmosphere ,Planet ,Methods: data analysis ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,Planets and satellites: atmospheres ,010303 astronomy & astrophysics ,Physics::Atmospheric and Oceanic Physics ,Planets and satellites: individual: WASP-76 b ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Atmospheric models ,010308 nuclear & particles physics ,520 Astronomy ,Astronomy and Astrophysics ,500 Science ,620 Engineering ,Exoplanet ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Thermosphere ,Exosphere - Abstract
Despite swift progress in the characterisation of exoplanet atmospheres in composition and structure, the study of atmospheric dynamics has not progressed at the same speed. While theoretical models have been developed to describe the lower layers of the atmosphere and, disconnected, the exosphere, little is known about the intermediate layers up to the thermosphere. We aim to provide a clearer picture of atmospheric dynamics for the class of ultra hot Jupiters, highly-irradiated gas giants, on the example of WASP-76~b. We analysed two datasets jointly, obtained with the HARPS and ESPRESSO spectrographs, to interpret the resolved planetary sodium doublet. We then applied an updated version of the MERC code, with added planetary rotation, also provides the possibility to model the latitude dependence of the wind patterns. We retrieve the highest Bayesian evidence for an isothermal atmosphere, interpreted as a mean temperature of $3389\pm227$ K, a uniform day-to-night side wind of $5.5^{+1.4}_{-2.0}\,$ km/s in the lower atmosphere with a vertical wind in the upper atmosphere of $22.7^{+4.9}_{-4.1}\,$ km/s, switching atmospheric wind patterns at $10^{-3}$ bar above the reference surface pressure ($10$ bar). Our results for WASP-76~b are compatible with previous studies of the lower atmospheric dynamics of WASP-76~b and other ultra hot Jupiters. They highlight the need for vertical winds in the intermediate atmosphere above the layers probed by global circulation model studies to explain the line broadening of the sodium doublet in this planet. This work demonstrates the capability of exploiting the resolved spectral line shapes to observationally constrain possible wind patterns in exoplanet atmospheres, an invaluable input to more sophisticated 3D atmospheric models in the future., 17 pages, 20 figures, submitted to A&A 15.Feb.2021, accepted for publication in A&A 20.Jul.2021
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- 2021
36. EUV spectroscopy with the ESCAPE mission: exploring the stellar drivers of exoplanet habitability
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Kevin C. France, Brian T. Fleming, Allison Youngblood, James P. Mason, Tom Patton, Nicholas E. Kruczek, Timothy Hellickson, Luca Fossati, Randall L. McEntaffer, Drew M. Miles, Martin A. Barstow, James C. Green, Guillaume Gronoff, Cynthia S. Froning, Ute Amerstorfer, Meng Jin, Vincent Bourrier, Jeffrey Linsky, Oswald Siegmund, and Jeremy J. Drake
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Planetary habitability ,Atmospheric escape ,Habitability ,Extreme ultraviolet lithography ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Exoplanet ,law.invention ,Astrobiology ,Telescope ,Heliophysics ,law ,Physics::Space Physics ,Astrophysics::Solar and Stellar Astrophysics ,Environmental science ,Astrophysics::Earth and Planetary Astrophysics ,Circumstellar habitable zone - Abstract
The Extreme-ultraviolet Stellar Characterization for Atmospheric Physics and Evolution (ESCAPE) mission is an astrophysics Small Explorer employing ultraviolet spectroscopy (EUV: 80 – 825 A and FUV: 1280 – 1650 A) to explore the high-energy radiation environment in the habitable zones around nearby stars. ESCAPE provides the first comprehensive study of the stellar EUV and coronal mass ejection environments which directly impact the habitability of rocky exoplanets. In a 21 month science mission, ESCAPE will provide the essential stellar characterization to identify exoplanetary systems most conducive to habitability and provide a roadmap for future life-finder missions. ESCAPE accomplishes this goal with roughly two-order-of-magnitude gains in EUV efficiency over previous missions. ESCAPE employs a grazing incidence telescope that feeds an EUV and FUV spectrograph, building on experience with ultraviolet and X-ray instrumentation, grazing incidence optical systems, and photon-counting ultraviolet detectors. The instrument builds on design and hardware heritage from numerous NASA UV astrophysics, heliophysics, and planetary science missions. The ESCAPE spacecraft bus is the versatile and high-heritage Ball Aerospace BCP-Smallspacecraft. Data archives are housed at the Mikulski Archive for Space Telescopes (MAST).
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- 2020
37. Wind of Change: Atmospheric wind retrieval and its implications for hot Jupiters
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Julia Seidel, David Ehrenreich, Vincent Bourrier, Lorenzo Pino, Aurelien Wyttenbach, Romain Allart, Baptiste Lavie, Dany Mounzer, and Christophe Lovis
- Abstract
The sodium doublet is one of the most powerful probes of exoplanet atmospheric properties when observed in transmission spectroscopy during transits. Recent high-spectral resolution observations of the sodium doublet in hot gas giants allowed us to resolve the line shape, opening the way for extracting atmospheric properties using line-profile fitting. Using the MERC code (Seidel et al. 2020a), a retrieval tool to determine temperature-pressure profiles and high-altitude winds in exoplanet thermospheres, we have studied the curiously broadened sodium signatures of various hot Jupiters. We have updated the MERC code to a quasi 3D treatment of the atmosphere (Seidel et al. 2020c, in prep.) and analysed three hot Jupiters, spanning a wide range of this class of exoplanets (see figure). Using the sodium signature of three examples - WASP-76b (a highly irradiated ultra-hot Jupiter, Seidel et al. 2019), KELT-11b (a puffy hot Jupiter, Mounzer et al. 2020, in prep.), and lastly HD189733b (one of the most studied hot Jupiters to date, Wyttenbach et al. 2015) - we explore possible trends in the atmospheric structure of hot Jupiters.We will first introduce the new quasi 3D retrieval of MERC, and proceed to show that high-velocity winds in the thermosphere are one possible explanation of the broadened sodium features seen in hot Jupiters. We plan to highlight various caveats and present likely origin scenarios for the observed wind patterns. We will then put these results in the context of past studies using global circulation models (GCMs) on hot Jupiters.
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- 2020
38. Measuring and modeling the Balmer series in hot gaseous giant exoplanets
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Aurélien Wyttenbach, Heather M. Cegla, Ignas Snellen, Louise D. Nielsen, David Ehrenreich, Vincent Bourrier, Christophe Lovis, Julia V. Seidel, Xavier Bonfils, Paul Mollière, Lorenzo Pino, Jens Hoeijmakers, Baptiste Lavie, Francesco Pepe, and Romain Allart
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Physics ,symbols.namesake ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Balmer series ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics ,Exoplanet - Abstract
Atmospheric escape rate is a key parameter to measure in order to understand the evolution of exoplanets. In this presentation, we will show that the Balmer series, observed with high-resolution transmission spectroscopy, is a precise probe to measure exoplanet evaporation, especially for ultra hot Jupiters orbiting early-type star. These hot gaseous giant exoplanets (such as KELT-9 b) are presumed to have an atmosphere dominated by neutral and ionized atomic species. In particular, hydrogen Balmer lines have been detected in some of their upper atmospheres, suggesting that hydrogen is filling the planetary Roche lobe and escaping from these planets. Here, we will present new significant absorptions of the Balmer series in the KELT-9b atmosphere obtained with HARPS-N. The precise line shapes of the Hα, Hβ, and Hγ absorptions allow us to put constraints on the thermospheric temperature. Moreover, the mass loss rate, and the excited hydrogen population of KELT-9 b are also constrained, thanks to a retrieval analysis performed with a new atmospheric model (the PAWN model). We retrieved a thermospheric temperature of T = 13 200+800-720 K and a mass loss rate of log10(MLR) = 10^(12.8+-0.3) g/s when the atmosphere was assumed to be in hydrodynamical expansion and in local thermodynamic equilibrium (LTE). Since the thermospheres of hot Jupiters are not expected to be in LTE, we explored atmospheric structures with non-Boltzmann equilibrium for the population of the excited hydrogen. We do not find strong statistical evidence in favor of a departure from LTE. However, our non-LTE scenario suggests that a departure from the Boltzmann equilibrium may not be sufficient to explain the retrieved low number densities of the excited hydrogen. In non-LTE, Saha equilibrium departure via photo-ionization, is also likely to be necessary to explain the data.
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- 2020
39. Search for helium in the upper atmosphere of the hot Jupiter WASP-127 b using Phoenix/Gemini
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Leonardo A. dos Santos, David Ehrenreich, Vincent Bourrier, Romain Allart, George King, Monika Lendl, Christophe Lovis, Steve Margheim, Jorge Meléndez, Julia V. Seidel, and Sérgio G. Sousa
- Abstract
Large-scale exoplanet search surveys have shown evidence that atmospheric escape is a ubiquitous process that shapes the evolution and demographics of planets. However, we lack a detailed understanding of this process because very few exoplanets discovered to date could be probed for signatures of atmospheric escape. Recently, the metastable helium triplet at 1.083 μm has been shown to be a viable window for the presence of He-rich escaping envelopes around short-period exoplanets. Our objective is to use, for the first time, the Phoenix spectrograph to search for helium in the upper atmosphere of the inflated hot Jupiter WASP-127 b. We observed one transit and reduced the data manually since there is no pipeline available. We did not find a significant in-transit absorption signal indicative of the presence of helium around WASP-127 b, and set a 90% confidence upper limit for excess absorption at 0.87% in a 0.75 Å passband covering the He triplet. Given the large scale height of this planet, the lack of a detectable feature is likely due to unfavorable photoionization conditions to populate the metastable He I triplet. This conclusion is supported by the inferred low coronal and chromospheric activity of the host star and the old age of the system, which result in a relatively mild high-energy environment around the planet.
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- 2020
40. The GAPS programme at TNG: XXII. The GIARPS view of the extended helium atmosphere of HD 189733 b accounting for stellar activity
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Andrea Bignamini, Katia Biazzo, N. Hernandez, Giampaolo Piotto, G. Falcini, Jesus Maldonado, Antonio Maggio, Vincent Bourrier, Massimo Cecconi, Giuseppina Micela, Emilio Molinari, A. F. Lanza, Gaetano Scandariato, Riccardo Claudi, G. Frustagli, Marco Pedani, José Guerra, Andrea Baruffolo, A. F. Martinez Fiorenzano, Avet Harutyunyan, Carlo Baffa, Rosario Cosentino, Laura Affer, Silvano Desidera, Walter Boschin, Monica Rainer, Lorenzo Pino, Valerio Nascimbeni, Ennio Poretti, Serena Benatti, Alessandro Sozzetti, M. Esposito, E. González-Álvarez, Isabella Pagano, Ilaria Carleo, Matteo Brogi, Adriano Ghedina, Paolo Giacobbe, Luca Malavolta, Giuseppe Leto, Aldo S. Bonomo, Ansgar Reiners, Luigi Mancini, Luca Fossati, M. S. Giampapa, Elvira Covino, Vincenzo Andretta, Mario Damasso, G. Bruno, G. Guilluy, Francesco Borsa, Guilluy, G, Andretta, V, Borsa, F, Giacobbe, P, Sozzetti, A, Covino, E, Bourrier, V, Fossati, L, Bonomo, A, Esposito, M, Giampapa, M, Harutyunyan, A, Rainer, M, Brogi, M, Bruno, G, Claudi, R, Frustagli, G, Lanza, A, Mancini, L, Pino, L, Poretti, E, Scandariato, G, Affer, L, Baffa, C, Baruffolo, A, Benatti, S, Biazzo, K, Bignamini, A, Boschin, W, Carleo, I, Cecconi, M, Cosentino, R, Damasso, M, Desidera, S, Falcini, G, Martinez Fiorenzano, A, Ghedina, A, Gonzalez-Alvarez, E, Guerra, J, Hernandez, N, Leto, G, Maggio, A, Malavolta, L, Maldonado, J, Micela, G, Molinari, E, Nascimbeni, V, Pagano, I, Pedani, M, Piotto, G, Reiners, A, Claudi, R. [orcid.org/0000-0001-7707-5105], Leto, G. [orcid.org/0000-0002-0040-5011], Ghedina, A. [orcid.org/0000-0003-4702-5152], Pino, L. [orcid.org/0000-0002-1321-8856], Damaso, M. [orcid.org/0000-0001-9984-4278], Cosentino, R. [orcid.org/0000-0003-1784-1431], Agenzia Spaziale Italiana (ASI), 2018-24-HH.0, German Research Foundation (DFG), SPP 1992 HA 3279/12-1, INAF through the ASI-INAF, 2015-019-R0, Agenzia Spaziale Italiana (ASI), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Istituto Nazionale di Astrofisica (INAF), Swiss National Science Foundation (SNSF), European Research Council (ERC), and Deutsche Forschungsgemeinschaft (DFG)
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astro-ph.SR ,Absorption spectroscopy ,fundamental parameters [Planets and satellites] ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Spectral line ,Planets and satellites: fundamental parameter ,spectroscopic [Techniques] ,Planet ,0103 physical sciences ,Hot Jupiter ,stars: activity ,Astrophysics::Solar and Stellar Astrophysics ,Absorption (electromagnetic radiation) ,planets and satellites: fundamental parameters ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,planets and satellites: atmospheres ,Planets and satellites: atmosphere ,010308 nuclear & particles physics ,Settore FIS/05 ,individual: HD 189733 b [Planets and satellites] ,Astronomy and Astrophysics ,Exoplanet ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,astro-ph.EP ,planets and satellites: individual: HD 189733 b ,atmospheres [Planets and satellites] ,H-alpha ,Astrophysics::Earth and Planetary Astrophysics ,Equivalent width ,Planets and satellites: atmospheres ,Planets and satellites: fundamental parameters ,Planets and satellites: individual: HD 189733 b ,Stars: activity ,Techniques: spectroscopic ,activity [Stars] ,techniques: spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Exoplanets orbiting very close to their host star are strongly irradiated. This can lead the upper atmospheric layers to expand and evaporate into space. The metastable helium (HeI) triplet at 1083.3nm has recently been shown to be a powerful diagnostic to probe extended and escaping exoplanetary atmosphere. We perform high-resolution transmission spectroscopy of the transiting hot Jupiter HD189733b with the GIARPS (GIANO-B + HARPS-N) observing mode of the Telescopio Nazionale Galileo, taking advantage of the simultaneous optical+near infrared spectral coverage to detect HeI in the planet's extended atmosphere and to gauge the impact of stellar magnetic activity on the planetary absorption signal. Observations were performed during five transit events of HD189733b. By comparison of the in- and out-of-transit GIANO-B observations we compute high-resolution transmission spectra, on which we perform equivalent width measurements and light-curves analyses to gauge the excess in-transit absorption in the HeI triplet. We detect an absorption signal during all five transits. The mean in-transit absorption depth amounts to 0.75+/-0.03%. We detect night-to-night variations in the HeI absorption signal likely due to the transit events occurring in presence of stellar surface inhomogeneities. We evaluate the impact of stellar-activity pseudo-signals on the true planetary absorption using a comparative analysis of the HeI and the H$\alpha$ lines. We interpret the time-series of the HeI absorption lines in the three nights not affected by stellar contamination -exhibiting a mean in-transit absorption depth of 0.77+/-0.04%- using a 3-d atmospheric code. Our simulations suggest that the helium layers only fill part of the Roche lobe. Observations can be explained with a thermosphere heated to $\sim$12000 K, expanding up to $\sim$1.2 planetary radii, and losing $\sim$1 g/s of metastable helium., Comment: 17 pages, 17 figures, accepted for publication in A&A
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- 2020
41. High-resolution transmission spectroscopy of MASCARA-2 b with EXPRES
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René Tronsgaard, David Ehrenreich, Lily Zhao, Samuel H. C. Cabot, Daniel Kitzmann, Debra A. Fischer, Allen B. Davis, Heather M. Cegla, Kevin Heng, Lars A. Buchhave, Vincent Bourrier, Christophe Lovis, H. Jens Hoeijmakers, and Simon L. Grimm
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High resolution ,FOS: Physical sciences ,Astrophysics ,Mascara ,01 natural sciences ,spectroscopic [Techniques] ,Transmission spectroscopy ,Optics ,0103 physical sciences ,spectrographs [Instrumentation] ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,business.industry ,Astronomy and Astrophysics ,3. Good health ,gaseous planets [Planets and satellites] ,13. Climate action ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,business ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report detections of atomic species in the atmosphere of MASCARA-2 b, using the first transit observations obtained with the newly commissioned EXPRES spectrograph. EXPRES is a highly stabilised optical echelle spectrograph, designed to detect stellar reflex motions with amplitudes down to 30 cm/s, and was recently deployed at the Lowell Discovery Telescope. By analysing the transmission spectrum of the ultra-hot Jupiter MASCARA-2 b using the cross-correlation method, we confirm previous detections of Fe I, Fe II and Na I, which likely originate in the upper regions of the inflated atmosphere. In addition, we report significant detections of Mg I and Cr II. The absorption strengths change slightly with time, possibly indicating different temperatures and chemistry in the day-side and night-side terminators. Using the effective stellar line-shape variation induced by the transiting planet, we constrain the projected spin-orbit misalignment of the system to $1.6\pm3.1$ degrees, consistent with an aligned orbit. We demonstrate that EXPRES joins a suite of instruments capable of phase-resolved spectroscopy of exoplanet atmospheres., Accepted for publication in A&A, 20 pages, 22 figures
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- 2020
42. Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS). V. Detection of sodium on the bloated super-Neptune WASP-166b
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Vincent Bourrier, David Ehrenreich, Stéphane Udry, E. Linder, Damien Ségransan, Monika Lendl, Aurélien Wyttenbach, O. Attia, Heather M. Cegla, Baptiste Lavie, Francesco Pepe, C. H. F. Melo, H. J. Hoeijmakers, C. Lovis, Kevin Heng, Julia V. Seidel, Daniel Bayliss, Nicola Astudillo-Defru, L. A. dos Santos, and Romain Allart
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics ,Planetary system ,01 natural sciences ,Exoplanet ,Radial velocity ,Space and Planetary Science ,Neptune ,Planet ,0103 physical sciences ,Transit (astronomy) ,Hot Neptune ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Planet formation processes or evolution mechanisms are surmised to be at the origin of the hot Neptune desert. Studying exoplanets currently living within or at the edge of this desert could allow disentangling the respective roles of formation and evolution. We present the HARPS transmission spectrum of the bloated super-Neptune WASP-166b, located at the outer rim of the Neptune desert. Neutral sodium is detected at the 3.4 $\sigma$ level ($0.455 \pm 0.135 \%$), with a tentative indication of line broadening, which could be caused by winds blowing sodium farther into space, a possible manifestation of the bloated character of these highly irradiated worlds. We put this detection into context with previous work claiming a non-detection of sodium in the same observations and show that the high noise in the trace of the discarded stellar sodium lines was responsible for the non-detection. We highlight the impact of this low signal-to-noise remnant on detections for exoplanets similar to WASP-166b., Comment: 7 pages, 7 figures, accepted for publication in A&A
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- 2020
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43. The high-energy environment and atmospheric escape of the mini-Neptune K2-18 b
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David Ehrenreich, Nicola Astudillo-Defru, Stéphane Udry, Xavier Bonfils, Vincent Bourrier, Christophe Lovis, Leonardo A. dos Santos, Francesco Pepe, François Forget, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Universidad Católica de la Santísima Concepción (UCSC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (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), Université de Genève = University of Geneva (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut Pierre-Simon-Laplace (IPSL (FR_636)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
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stars ,stars: chromospheres ,010504 meteorology & atmospheric sciences ,kinematics and dynamics ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,Atmosphere ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,K2-18 -stars ,Transit (astronomy) ,individual ,010303 astronomy & astrophysics ,Space Telescope Imaging Spectrograph ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,ISM: kinematics and dynamics ,planets and satellites: atmospheres ,[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph] ,Atmospheric escape ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,atmospheres -ISM ,Astronomy and Astrophysics ,stars: individual: K2-18 ,Redshift ,Radiation pressure ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,chromospheres -planets and satellites ,Mini-Neptune ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
K2-18 b is a transiting mini-Neptune that orbits a nearby (38 pc) cool M3 dwarf and is located inside its region of temperate irradiation. We report on the search for hydrogen escape from the atmosphere K2-18 b using Lyman-$\alpha$ transit spectroscopy with the Space Telescope Imaging Spectrograph (STIS) instrument installed on the Hubble Space Telescope (HST). We analyzed the time-series of the fluxes of the stellar Lyman-$\alpha$ emission of K2-18 in both its blue- and redshifted wings. We found that the average blueshifted emission of K2-18 decreases by $67\% \pm 18\%$ during the transit of the planet compared to the pre-transit emission, tentatively indicating the presence of H atoms escaping vigorously and being blown away by radiation pressure. This interpretation is not definitive because it relies on one partial transit. Based on the reconstructed Lyman-$\alpha$ emission of K2-18, we estimate an EUV irradiation between $10^1-10^2$ erg s$^{-1}$ cm$^{-2}$ and a total escape rate in the order of $10^8$ g s$^{-1}$. The inferred escape rate suggests that the planet will lose only a small fraction (< 1%) of its mass and retain its volatile-rich atmosphere during its lifetime. More observations are needed to rule out stellar variability effects, confirm the in-transit absorption and better assess the atmospheric escape and high-energy environment of K2-18 b., Comment: 5 pages, 4 figures, accepted for publication in A&A Letters, V2 with editorial corrections
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- 2020
44. Broadband transmission spectroscopy of HD 209458b with ESPRESSO: evidence for Na, TiO, or both
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Cristina Martins, Marco Riva, C. Lovis, Enric Palle, E. Poretti, O. D. S. Demangeon, S. G. Sousa, S. C. C. Barros, P. Figueira, G. Lo Curto, Xavier Dumusque, Nelson J. Nunes, Romain Allart, J. I. González Hernández, Vardan Adibekyan, Rafael Rebolo, François Bouchy, S. Cristiani, Yann Alibert, Stéphane Udry, Andrea Mehner, M. R. Zapatero Osorio, C. Allende Prieto, B. Lavie, David Ehrenreich, Alessandro Sozzetti, A. Suárez Mascareño, Paolo Molaro, Francesco Pepe, E. Cristo, N. C. Santos, Denis Mégevand, Giuseppina Micela, J. H. C. Martins, Vincent Bourrier, P. Di Marcantonio, Hugo M. Tabernero, A. Cabral, N. Casasayas-Barris, Francesco Borsa, Antonio Manescau, M. Oshagh, Hans Dekker, J. P. Faria, V. D'Odorico, Fundacao para a Ciencia e a Tecnologia (FCT), Istituto Nazionale di Astrofisica (INAF), European Research Council (ERC), Agencia Estatal de Investigación (AEI), Santos, N. C. [0000-0003-4422-2919], Cristo, E. [0000-0001-5992-7589], Demangeon, O. D. S. [0000-0001-7918-0355], Oshagh, M. [0000-0002-0715-8789], Palle, E. [0000-0003-0987-1593], Portuguese Foundation for Science and Technology, FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao, Italian Ministry of Education University, and Research, European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project Four Aces grant), and Spanish Ministry of Science Innovation and Universities (MICIU)
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FOS: Physical sciences ,Context (language use) ,01 natural sciences ,7. Clean energy ,Spectral line ,spectroscopic [Techniques] ,Espresso ,Planet ,0103 physical sciences ,HD 209458b ,Chromatic scale ,Spectroscopy ,010303 astronomy & astrophysics ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Exoplanet ,3. Good health ,Computational physics ,Planetary systems ,Transmission (telecommunications) ,13. Climate action ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Context. The detection and characterization of exoplanet atmospheres is currently one of the main drivers pushing the development of new observing facilities. In this context, high-resolution spectrographs are proving their potential and showing that high-resolution spectroscopy will be paramount in this field. Aims. We aim to make use of ESPRESSO high-resolution spectra, which cover two transits of HD 209458b, to probe the broadband transmission optical spectrum of the planet. Methods. We applied the chromatic Rossiter-McLaughin method to derive the transmission spectrum of HD 209458b. We compared the results with previous HST observations and with synthetic spectra. Results. We recover a transmission spectrum of HD 209458b similar to the one obtained with HST data. The models suggest that the observed signal can be explained by only Na, only TiO, or both Na and TiO, even though none is fully capable of explaining our observed transmission spectrum. Extra absorbers may be needed to explain the full dataset, though modeling approximations and observational errors can also be responsible for the observed mismatch. Conclusions. Using the chromatic Rossiter-McLaughlin technique, ESPRESSO is able to provide broadband transmission spectra of exoplanets from the ground, in conjunction with space-based facilities, opening good perspectives for similar studies of other planets., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
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- 2020
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45. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS
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H. Ottacher, T. Kuntzer, M. Steller, Xavier Bonfils, A. García Muñoz, Don Pollacco, Ingo Walter, Gaetano Scandariato, A. Deline, Ignasi Ribas, J. Hasiba, T. Bandy, Bruno Chazelas, Yann Alibert, Luca Marafatto, Maria Bergomi, E. Hernandez, Michaël Gillon, Anders Erikson, O. Demangeon, Valerio Nascimbeni, Heike Rauer, N. Thomas, Virginie Cessa, G. Olofsson, F. Safa, R. Rohlfs, N. A. Walton, C. Broeg, Didier Queloz, C. Corral Van Damme, D. Futyan, Nicola Rando, Malcolm Fridlund, Federico Biondi, Roi Alonso, David Ehrenreich, T. Lüftinger, Stéphane Udry, László L. Kiss, K. G. Isaak, Wolfgang Baumjohann, Alexis M. S. Smith, Monika Lendl, D. Wolter, A. E. Simon, Thomas Beck, L. Malvasio, Nuno C. Santos, David Barrado, Demetrio Magrin, J. Asquier, V. Singh, Enric Palle, Damien Ségransan, Pierre F. L. Maxted, Roland Ottensamer, Gisbert Peter, M.-D. Busch, S. C. C. Barros, D. Kitzmann, Willy Benz, S. Hoyer, B. M. Morris, C. Lovis, Kevin Heng, Isabella Pagano, S. Salmon, Davide Gandolfi, Jacopo Farinato, Gy. M. Szabó, Sébastien Charnoz, Giampaolo Piotto, A. Bekkelien, Andrea Fortier, M. Sordet, A. Bonfanti, Nicolas Billot, Luca Fossati, Jacques Laskar, Francois Wildi, Szilard Csizmadia, Martin Rieder, M. Tschentscher, Valérie Van Grootel, Valentina Viotto, Vincent Bourrier, Roberto Ragazzoni, M. Beck, M. J. Hooton, F. Ratti, T. G. Wilson, T. Bárczy, L. Delrez, Daniele Piazza, A. Collier Cameron, Melvyn B. Davies, S. G. Sousa, B. O. Demory, Juan Cabrera, Alexis Brandeker, P. Guterman, M. Deleuil, A. Lecavelier des Etangs, Harald Michaelis, Matteo Munari, Swiss Space Office, University of Bern, Swiss National Science Foundation, Austrian Research Promotion Agency, German Research Foundation, European Commission, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Fédération Wallonie-Bruxelles, Hungarian Scientific Research Fund, Agenzia Spaziale Italiana, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Wilson, T. G. [0000-0001-8749-1962], Cameron, A. [0000-0002-8863-7828], Fridlund, M. [0000-0002-0855-8426], Cabrera, J. [0000-0001-6653-5487], Barros, S. [0000-0003-2434-3625], Santos, N. [0000-0003-4422-2919], Piotto, G. [0000-0002-9937-6387], Austrian Research Promotion Agency (FFG), Deutsche Forschungsgemeinschaft (DFG), European Research Council (ERC), Swiss National Science Foundation (SNSF), Agencia Estatal de Investigación (AEI), Fundação para a Ciência e a Tecnologia (FCT), National Research Development and Innovation Office, Hungarian (NKFIH), Agenzia Spaziale Italiana (ASI), European Space Agency (ESA), Fundacao para a Ciencia e a Tecnologia (FCT), Belgian Federal Science Policy Office (BELSPO), Istituto Nazionale di Astrofisica (INAF), University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Physikalisches Institut [Bern], Universität Bern [Bern], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Research Council (ERC) under European Union, European Commission (EU), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, European Space Agency, FEDER through COMPETE2020 Programa Operacional Competitividade e Internacionalizacao, Hungarian National Research, and Centre National D'etudes Spatiales
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010504 meteorology & atmospheric sciences ,Astrophysics ,atmospheres -planets and satellites ,01 natural sciences ,7. Clean energy ,Occultation ,Planet ,Planets and satellites: atmospheres ,QB Astronomy ,photometric -planets and satellites ,individual ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,16. Peace & justice ,Exoplanet ,Astrophysics - Solar and Stellar Astrophysics ,individual: WASP- 189 b [Planets and satellites] ,atmospheres [Planets and satellites] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Extrasolare Planeten und Atmosphären ,Weltrauminstrumente ,FOS: Physical sciences ,WASP-189 b ,Photometry (optics) ,0103 physical sciences ,Hot Jupiter ,individual: WASP-189 b [Planets and satellites] ,Planets and satellites: individual: WASP-189 b ,Techniques: photometric ,Gravity darkening ,planetary systems ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,abundance pattern ,photometric [Techniques] ,Astronomy and Astrophysics ,DAS ,Light curve ,Stars ,QC Physics ,Space and Planetary Science ,exoplanet occultation ,Planetare Sensorsysteme ,techniques ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Earth and Planetary Astrophysics ,QB799 - Abstract
Full author list: Lendl, M., Csizmadia, S., Deline, A., Fossati, L., Kitzmann, D., Heng, K., Hoyer, S., Salmon, S., Benz, W., Broeg, C., Ehrenreich, D., Fortier, A., Queloz, D., Bonfanti, A., Brandeker, A., Collier Cameron, A., Delrez, L.a,g,l, Garcia Muñoz, A.m, Hooton, M.J.f, Maxted, P.F.L.i, Morris, B.M., Van Grootel, V., Wilson, T.G., Alibert, Y., Alonso, R., Asquier, J., Bandy, T.f, Bárczy, T.q, Barrado, D.r, Barros, S.C.C.s,t, Baumjohann, W.b, Beck, M., Beck, T., Bekkelien, A., Bergomi, M., Billot, N., Biondi, F., Bonfils, X., Bourrier, V., Busch, M.-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Corral Van Damme, C., Davies, M.B., Deleuil, M., Demangeon, O.D.S., Demory, B.-O., Erikson, A., Farinato, J., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M.l, Guterman, P., Hasiba, J., Hernandez, E., Isaak, K., Kiss, L., Kuntzer, T., Lecavelier Des Etangs, A., Lüftinger, T., Laskar, J., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ratti, F., Rauer, H., Ragazzoni, R., Rando, N., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Santos, N.C., Scandariato, G., Ségransan, D., Simon, A.E., Singh, V., Smith, A.M.S., Sordet, M., Sousa, S.G., Steller, M., Szabó, G.M., Thomas, N., Tschentscher, M., Udry, S., Viotto, V., Walter, I., Walton, N.A., Wildi, F., Wolter, D., The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189 b, a MP ≈ 2MJ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of dF = 87.9 ± 4.3 ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of 3435 ± 27 K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189 b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a ~25% deeper transit compared to the discovery paper and updating the radius of WASP-189 b to 1.619 ± 0.021RJ. We further measured the projected orbital obliquity to be λ = 86.4-4.4+2.9°, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of ψ = 85.4 ± 4.3°. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V = 6.6 mag star, and using a 1-h binning, we obtain a residual RMS between 10 and 17 ppm on the individual light curves, and 5.7 ppm when combining the four visits., with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The Swiss participation to CHEOPS has been supported by the Swiss Space Office (SSO) in the framework of the Prodex Programme and the Activités Nationales Complémentaires (ANC), the Universities of Bern and Geneva as well as well as of the NCCR PlanetS and the Swiss National Science Foundation. M.L.E. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 “GRAPPA”. Sz. Cs. thanks DFG Research Unit 2440: ‘Matter Under Planetary Interior Conditions: High Pressure, Planetary, and Plasma Physics’ for support. Sz. Cs. acknowledges support by DFG grants RA 714/14-1 within the DFG Schwerpunkt SPP 1992: “Exploring the Diversity of Extrasolar Planets”. A.D.E. and D.E.H. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement no. 724427). M.J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33, and MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liege through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. M.G. is F.R.S.-FNRS Senior Research Associate. S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). Gy.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS activities have been supported by the Italian Space Agency, under the programs: ASI-INAF n. 2013-016-R.0 and ASI-INAF n. 2019-29-HH.0. The team at LAM acknowledges CNES funding for the development of the CHEOPS DRP, including grants 124378 for O.D. and 837319 for S.H. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as an ESA-appointed CHEOPS science team members.
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46. Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS). III. Atmospheric structure of the misaligned ultra-hot Jupiter WASP-121b
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C. Melo, Francesco Pepe, A. Suarez-Mascareno, Nicola Astudillo-Defru, M. Cretignier, Damien Ségransan, T. Kuntzer, Valerio Nascimbeni, Monika Lendl, Aurélien Wyttenbach, C. Lovis, Kevin Heng, Heather M. Cegla, H. Giles, Stéphane Udry, Romain Allart, Lorenzo Pino, H. J. Hoeijmakers, Felipe Murgas, Xavier Dumusque, Baptiste Lavie, David Ehrenreich, Daniel Kitzmann, and Vincent Bourrier
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Planetary system ,01 natural sciences ,Exoplanet ,Tidal locking ,Jupiter ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Hot Jupiter ,Differential rotation ,Transit (astronomy) ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Ultra-hot Jupiters offer interesting prospects for expanding our theories on dynamical evolution and the properties of extremely irradiated atmospheres. In this context, we present the analysis of new optical spectroscopy for the transiting ultra-hot Jupiter WASP-121b. We first refine the orbital properties of WASP-121b, which is on a nearly polar (obliquity $\psi^{\rm North}$=88.1$\pm$0.25$^{\circ}$ or $\psi^{\rm South}$=91.11$\pm$0.20$^{\circ}$) orbit, and exclude a high differential rotation for its fast-rotating (P$, Comment: 20 pages, 15 figures, accepted for publication in A&A on 19 December 2019
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47. Expected performances of the Characterising Exoplanet Satellite (CHEOPS) (II) The CHEOPS simulator
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M. Beck, Vincent Bourrier, A. Deline, Monika Lendl, A. Collier Cameron, T. Kuntzer, Andrea Fortier, Willy Benz, D. Queloz, A. Bekkelien, C. Broeg, David Ehrenreich, Nicolas Billot, Francois Wildi, R. Rohlfs, A. E. Simon, D. Futyan, Queloz, Didier [0000-0002-3012-0316], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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planets and satellites ,detection ,FOS: Physical sciences ,Image processing ,01 natural sciences ,7. Clean energy ,law.invention ,methods ,Photometry (optics) ,Telescope ,numerical ,Planet ,law ,0103 physical sciences ,QB Astronomy ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,QC ,Simulation ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,instrumentation ,numerical [Methods] ,010308 nuclear & particles physics ,Exoplanets ,Astrophysics::Instrumentation and Methods for Astrophysics ,CCDs ,Astronomy and Astrophysics ,3rd-DAS ,Orbital period ,Light curve ,Exoplanet ,detection [Planets and satellites] ,photometers [Instrumentation] ,QC Physics ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,photometers ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Data reduction - Abstract
The CHaracterising ExOPlanet Satellite (CHEOPS) is a mission dedicated to the search for exoplanetary transits through high precision photometry of bright stars already known to host planets. The telescope will provide the unique capability of determining accurate radii for planets whose masses have already been measured from ground-based spectroscopic surveys. This will allow a first-order characterisation of the planets' internal structure through the determination of the bulk density, providing direct insight into their composition. The CHEOPS simulator has been developed to perform detailed simulations of the data which is to be received from the CHEOPS satellite. It generates accurately simulated images that can be used to explore design options and to test the on-ground data processing, in particular, the pipeline producing the photometric time series. It is, thus, a critical tool for estimating the photometric performance expected in flight and to guide photometric analysis. It can be used to prepare observations, consolidate the noise budget, and asses the performance of CHEOPS in realistic astrophysical fields that are difficult to reproduce in the laboratory. Images generated by CHEOPSim take account of many detailed effects, including variations of the incident signal flux and backgrounds, and detailed modelling of the satellite orbit, pointing jitter and telescope optics, as well as the CCD response, noise and readout. The simulator results presented in this paper have been used in the context of validating the data reduction processing chain, in which image time series generated by CHEOPSim were used to generate light curves for simulated planetary transits across real and simulated targets. Independent analysts were successfully able to detect the planets and measure their radii to an accuracy within the science requirements of the mission., Comment: Accepted for publication in A&A. 16 pages, 18 figures
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48. Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS). IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b
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Damien Ségransan, Daniel Kitzmann, Julia V. Seidel, Valerio Nascimbeni, Monika Lendl, Aurélien Wyttenbach, Daniel Bayliss, Sergei N. Yurchenko, Heather M. Cegla, David Ehrenreich, Lorenzo Pino, Andrea Gebek, Kevin Heng, C. H. F. Melo, C. Lovis, Baptiste Lavie, Romain Allart, H. J. Hoeijmakers, Apurva Oza, Jan Philip Sindel, Vincent Bourrier, Francesco Pepe, Felipe Murgas, Nicola Astudillo-Defru, and Stéphane Udry
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gaseous planets [planets and satellites] ,010504 meteorology & atmospheric sciences ,EXTRASOLAR PLANET ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,MASS ,01 natural sciences ,Computer Science::Digital Libraries ,Spectral line ,Jupiter ,0103 physical sciences ,Hot Jupiter ,ABSORPTION ,Spectral resolution ,Spectroscopy ,SOLAR ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Science & Technology ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,atmospheres [planets and satellites] ,Exoplanet ,Physics::History of Physics ,3. Good health ,LINE LISTS ,Chemical species ,INFRARED LASER SPECTROSCOPY ,TIS ,Space and Planetary Science ,TITANIUM ,GIANT PLANET ,Physical Sciences ,HD 189733B ,spectroscopic [techniques] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Aims: We survey the transmission spectrum of WASP-121 b for line-absorption by metals and molecules at high spectral resolution, and elaborate on existing interpretations of the optical transmission spectrum observed with HST/STIS and WFC3. Methods: We use the cross-correlation technique and direct differential spectroscopy to search for sodium and other neutral and ionised atoms, TiO, VO and SH in high-resolution transit spectra obtained with the HARPS spectrograph. We inject models assuming chemical and hydrostatic equilibrium with varying temperature and composition to enable model comparison, and employ two bootstrap methods to test the robustness of our detections. Results: We detect neutral Mg, Na, Ca, Cr, Fe, Ni and V, which we predict exists in equilibrium with a significant quantity of VO, supporting earlier observations by HST/WFC3. Non-detections of Ti and TiO support the hypothesis that Ti is depleted via a cold-trap mechanism as has been proposed in the literature. Atomic line depths are under-predicted by hydrostatic models by a factor of 1.5 to 8, confirming recent findings that the atmosphere is extended. We predict the existence of significant concentrations of gas-phase TiO$_2$, VO$_2$ and TiS, which could be important absorbers at optical and NIR wavelengths in hot Jupiter atmospheres, but for which accurate line-list data is currently not available. We find no evidence for absorption by SH, and find that inflated atomic lines can plausibly explain the slope of the transmission spectrum observed in the NUV with HST/STIS. The Na D lines are significantly broadened and show a difference in their respective depths of 15 scale heights, which is not expected from isothermal hydrostatic theory., Comment: Accepted for publication in A&A - June 19, 2020
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49. MOVES III. Simultaneous X-ray and ultraviolet observations unveiling the variable environment of the hot Jupiter HD 189733b
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Rim Fares, Vincent Bourrier, Peter J. Wheatley, David Ehrenreich, Joe Llama, A. Lecavelier des Etangs, Moira Jardine, Tom Louden, Christiane Helling, George W. King, Aline A. Vidotto, Science & Technology Facilities Council, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. School of Physics and Astronomy, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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Planet-star interactions ,stars: chromospheres ,chromospheres, coronae [Stars] ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,individual: HD 189733 [Stars] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,ISM: clouds ,spectroscopic [Techniques] ,0103 physical sciences ,Hot Jupiter ,planet-star interactions ,media_common.cataloged_instance ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,European union ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,media_common ,coronae ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Horizon (archaeology) ,010308 nuclear & particles physics ,individual: HD189733b [Planets and satellites] ,European research ,stars: individual: HD 189733 ,planets and satellites: individual: HD189733b ,Astronomy ,Astronomy and Astrophysics ,DAS ,Variable (computer science) ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - High Energy Astrophysical Phenomena ,clouds [ISM] ,techniques: spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
In this third paper of the MOVES (Multiwavelength Observations of an eVaporating Exoplanet and its Star) programme, we combine Hubble Space Telescope far-ultraviolet observations with XMM-Newton/Swift X-ray observations to measure the emission of HD 189733 in various FUV lines, and its soft X-ray spectrum. Based on these measurements we characterise the interstellar medium toward HD 189733 and derive semi-synthetic XUV spectra of the star, which are used to study the evolution of its high-energy emission at five different epochs. Two flares from HD 189733 are observed, but we propose that the long-term variations in its spectral energy distribution have the most important consequences for the environment of HD 189733b. Reduced coronal and wind activity could favour the formation of a dense population of Si$^{2+}$ atoms in a bow-shock ahead of the planet, responsible for pre- and in-transit absorption measured in the first two epochs. In-transit absorption signatures are detected in the Lyman-$\alpha$ line in the second, third and fifth epochs, which could arise from the extended planetary thermosphere and a tail of stellar wind protons neutralised via charge-exchange with the planetary exosphere. We propose that increases in the X-ray irradiation of the planet, and decreases in its EUV irradiation causing lower photoionisation rates of neutral hydrogen, favour the detection of these signatures by sustaining larger densities of H$^{0}$ atoms in the upper atmosphere and boosting charge-exchanges with the stellar wind. Deeper and broader absorption signatures in the last epoch suggest that the planet entered a different evaporation regime, providing clues as to the link between stellar activity and the structure of the planetary environment., Comment: 22 pages, 21 figures, accepted for publication in MNRAS on 23 January 2020
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50. The Hubble Space Telescope PanCET Program: An Optical to Infrared Transmission Spectrum of HAT-P-32Ab
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Vincent Bourrier, David K. Sing, Mercedes Lopez-Morales, Hannah R. Wakeford, Jorge Sanz-Forcada, Gregory W. Henry, Antonio García Muñoz, Claire Baxter, Ofer Cohen, Panayotis Lavvas, Lars A. Buchhave, Joanna K. Barstow, Nikolay Nikolov, Munazza Alam, Thomas Mikal-Evans, Michael H. Williamson, Jean-Michel Desert, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Space Telescope Science Institute (STSci), Department of Physics [Baltimore], University of Maryland [Baltimore County] (UMBC), University of Maryland System-University of Maryland System, Center of Excellence in Information Systems, Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Berlin (TU), Alam, M. K. [0000-0003-4157-832X], López Morales, M. [0000-0003-3204-8183], Nikolov, N. [0000-0002-6500-3574], Sing, D. K. [0000-0001-6050-7645], Henry, G. W. [0000-0003-4155-8513], Baxter, C. [0000-0003-3438-843X], Désert, J. M. [0000-0002-0875-8401], Barstow, J. K. [0000-0003-3726-5419], Mikal Evans, T. [0000-0001-5442-1300], Bourrier, V. [0000-0002-9148-034X], Lavvas, P. [0000-0002-5360-3660], Wakeford, H. R. [0000-0003-4328-3867], Forcada, J. S. [0000-0002-1600-7835], Buchhave, L. A. [0000-0003-1605-5666], Cohen, O. [0000-0003-3721-0215], García Muñoz, A. [0000-0003-1756-4825], National Aeronautics & Space Administration (NASA), NAS 5-26555, HST GO programs, 14767 14260, Space Telescope Science Institute, HST-GO-14767, Agencia Estatal de Investigación (AEI), National Aeronautics and Space Administration (NASA), European Research Council (ERC), and Low Energy Astrophysics (API, FNWI)
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010504 meteorology & atmospheric sciences ,Infrared ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Hot Jupiters ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Planet ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Space Telescope Imaging Spectrograph ,ComputingMilieux_MISCELLANEOUS ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Eclipse ,Physics ,planets and satellites: atmospheres ,[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph] ,planets and satellites: individual (HAT-P-32Ab) ,Exoplanets ,planets and satellites: composition ,Astronomy and Astrophysics ,Exoplanet ,Photometry (astronomy) ,Exoplanet atmospheric composition ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics::Earth and Planetary Astrophysics ,Wide Field Camera 3 ,Exoplanet atmospheres - Abstract
We present a 0.3-5 μm transmission spectrum of the hot Jupiter HAT-P-32Ab observed with the Space Telescope Imaging Spectrograph and Wide Field Camera 3 instruments mounted on the Hubble Space Telescope, combined with Spitzer Infrared Array Camera photometry. The spectrum is composed of 51 spectrophotometric bins with widths ranging between 150 and 400 Å, measured to a median precision of 215 ppm. Comparisons of the observed transmission spectrum to a grid of 1D radiative-convective equilibrium models indicate the presence of clouds/hazes, consistent with previous transit observations and secondary eclipse measurements. To provide more robust constraints on the planet's atmospheric properties, we perform the first full optical to infrared retrieval analysis for this planet. The retrieved spectrum is consistent with a limb temperature of 1248+9292 K, a thick cloud deck, enhanced Rayleigh scattering, and ∼10× solar H2O abundance. We find log(Z/Z o˙) =2.41+0.06-0.07, and compare this measurement with the mass-metallicity relation derived for the solar system., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
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- 2020
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