Search

Your search keyword '"Ryan Cloutier"' showing total 4 results
Start Over Author "Ryan Cloutier" Journal astronomy & astrophysics
4 results on '"Ryan Cloutier"'

1. A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776

Author

Enric Palle, Eric L. N. Jensen, David Charbonneau, Iskra Georgieva, Priyanka Chaturvedi, Juan Cabrera, E. Goffo, Christopher E. Henze, Ian J. M. Crossfield, Davide Gandolfi, Massimiliano Esposito, Carina M. Persson, Ana Glidden, Karen A. Collins, R. C. Kidwell, Florian Rodler, C. Ziegler, Jack J. Lissauer, Vincent Van Eylen, Grzegorz Nowak, E. W. Guenther, George R. Ricker, Oscar Barragán, Martin Paegert, Emil Knudstrup, Artie P. Hatzes, Thiam-Guan Tan, Malcolm Fridlund, M. C. Nixon, Hans J. Deeg, David W. Latham, Nikku Madhusudhan, S. Grziwa, Seth Redfield, John F. Kielkopf, Teruyuki Hirano, Luisa M. Serrano, Sz. Csizmadia, Sara Seager, John H. Livingston, Jon M. Jenkins, Judith Korth, Petr Kabath, Kevin I. Collins, Cesar Briceno, Eric B. Ting, Knicole D. Colón, K. W. F. Lam, Karan Molaverdikhani, Robert F. Goeke, Joshua E. Schlieder, Joshua N. Winn, Nicholas J. Scott, Jonathan Irwin, Elisabeth Matthews, S. Albrecht, J. Šubjak, Fei Dai, Steve B. Howell, Rafael Luque, Roland Vanderspek, Ismael Mireles, Ryan Cloutier, Norio Narita, William D. Cochran, Andrew W. Mann, Nikku, Madhusudhan [0000-0002-4869-000X], and Apollo - University of Cambridge Repository

Subjects
Extrasolare Planeten und Atmosphären, Rotation period, 010504 meteorology & atmospheric sciences, Stellar mass, FOS: Physical sciences, Individual, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometric, individual: LP 961-53 [Stars], 01 natural sciences, Spectral line, techniques: photometric, Planet, low-mass [Stars], stars: low-mass, 0103 physical sciences, techniques: radial velocities, Radial Velocities, Astrophysics::Solar and Stellar Astrophysics, Planetary Systems, Low-Mass, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], photometric [Techniques], stars: individual: LP 961-53, Astronomy and Astrophysics, Radius, Planetary system, Stars, Exoplanet, Techniques, Planetary systems, 13. Climate action, Space and Planetary Science, LP 961-53, lanetary systems – techniques: photometric – techniques: radial velocities – stars: individual: LP 961-53 – stars: low-mass, Astrophysics::Earth and Planetary Astrophysics, Stars: individual: LP 961-53, Stars: low-mass, Techniques: photometric, Techniques: radial velocities, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776, J = 8.5 mag, M = 0.54+-0.03 Msun) detected during Sector 10 observations of the Transiting Exoplanet Survey Satellite (TESS). Combining the TESS photometry with HARPS radial velocities, as well as ground-based follow-up transit observations from MEarth and LCOGT telescopes, we measured for the inner planet, TOI-776 b, a period of 8.25 d, a radius of 1.85+-0.13 Re, and a mass of 4.0+-0.9 Me; and for the outer planet, TOI-776 c, a period of 15.66 d, a radius of 2.02+-0.14 Re, and a mass of 5.3+-1.8 Me. The Doppler data shows one additional signal, with a period of 34 d, associated with the rotational period of the star. The analysis of fifteen years of ground-based photometric monitoring data and the inspection of different spectral line indicators confirm this assumption. The bulk densities of TOI-776 b and c allow for a wide range of possible interior and atmospheric compositions. However, both planets have retained a significant atmosphere, with slightly different envelope mass fractions. Thanks to their location near the radius gap for M dwarfs, we can start to explore the mechanism(s) responsible for the radius valley emergence around low-mass stars as compared to solar-like stars. While a larger sample of well-characterized planets in this parameter space is still needed to draw firm conclusions, we tentatively estimate that the stellar mass below which thermally-driven mass loss is no longer the main formation pathway for sculpting the radius valley is between 0.63 and 0.54 Msun. Due to the brightness of the star, the TOI-776 system is also an excellent target for the James Webb Space Telescope, providing a remarkable laboratory to break the degeneracy in planetary interior models and to test formation and evolution theories of small planets around low-mass stars., Comment: 26 pages, 15 figures, 8 tables. Accepted for publication in Astronomy & Astrophysics

Published
2021
Full Text
View/download PDF

2. Characterization of the L 98-59 multi-planetary system with HARPS

Author

Guillermo Torres, George R. Ricker, Nicolás T. Kurtovic, Francesco Pepe, Sara Seager, Rodrigo F. Díaz, Philip S. Muirhead, Z. M. Berdinas, Ryan Cloutier, Stéphane Udry, Matías R. Díaz, Nuno C. Santos, C. Lovis, Damien Ségransan, Robert L. Morris, Michael Vezie, Eric R. Morgan, M. Mayor, Kristen Menou, X. Delfosse, D. W. Latham, James S. Jenkins, P. Figueira, Jon M. Jenkins, Roland Vanderspek, François Bouchy, Peter Tenenbaum, T. Forveille, Nicola Astudillo-Defru, Felipe Murgas, J. Villasenor, Joshua N. Winn, Jose-Manuel Almenara, René Doyon, Xavier Bonfils, and Jeffrey C. Smith

Subjects
Physics, Super-Earth, Outer planets, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Radial velocity, Planetary science, 13. Climate action, Space and Planetary Science, Planet, Neptune, 0103 physical sciences, Terrestrial planet, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Aims.L 98-59 (TIC 307210830, TOI-175) is a nearby M3 dwarf around which TESS revealed three small transiting planets (0.80, 1.35, 1.57 Earth radii) in a compact configuration with orbital periods shorter than 7.5 days. Here we aim to measure the masses of the known transiting planets in this system using precise radial velocity (RV) measurements taken with the HARPS spectrograph.Methods.We considered both trained and untrained Gaussian process regression models of stellar activity, which are modeled simultaneously with the planetary signals. Our RV analysis was then supplemented with dynamical simulations to provide strong constraints on the planets’ orbital eccentricities by requiring long-term stability.Results.We measure the planet masses of the two outermost planets to be 2.42 ± 0.35 and 2.31 ± 0.46 Earth masses, which confirms the bulk terrestrial composition of the former and eludes to a significant radius fraction in an extended gaseous envelope for the latter. We are able to place an upper limit on the mass of the smallest, innermost planet of e< 0.1.Conclusions.L 98-59 is likely a compact system of two rocky planets plus a third outer planet with a lower bulk density possibly indicative of the planet having retained a modest atmosphere. The system offers a unique laboratory for studies of planet formation, dynamical stability, and comparative atmospheric planetology as the two outer planets are attractive targets for atmospheric characterization through transmission spectroscopy. Continued RV monitoring will help refine the characterization of the innermost planet and potentially reveal additional planets in the system at wider separations.

Published
2019
Full Text
View/download PDF

3. Confirmation of the radial velocity super-Earth K2-18c with HARPS and CARMENES

Author

A. Wünsche, Francesco Pepe, Michel Mayor, Nuno C. Santos, Nicola Astudillo-Defru, Xavier Bonfils, Stéphane Udry, Felipe Murgas, François Bouchy, René Doyon, T. Forveille, Kristen Menou, X. Delfosse, C. Lovis, Ryan Cloutier, Jose-Manuel Almenara, Université du Québec à Rimouski (UQAR), Institut de Recherche sur les Exoplanètes (iREX), Université de Montréal (UdeM), Universidad de Concepción [Chile], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto [Porto], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Universidade do Porto

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Signal, fundamental parameters -planets and satellites, Planet, radial velocities -planets and satellites, techniques: radial velocities, 0103 physical sciences, individual, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, Spectrograph, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, K2-18, Super-Earth, Astronomy and Astrophysics, planets and satellites: individual: K2-18, Planetary system, data analysis -planets and satellites, methods: data analysis, Radial velocity, detectionmethods, Wavelength, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, techniques, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

In an earlier campaign to characterize the mass of the transiting temperate super-Earth K2-18b with HARPS, a second, non-transiting planet was posited to exist in the system at $\sim 9$ days. Further radial velocity follow-up with the CARMENES spectrograph visible channel revealed a much weaker signal at 9 days which also appeared to vary chromatically and temporally leading to the conclusion that the origin of the 9 day signal was more likely to be related to stellar activity than to being planetary. Here we conduct a detailed re-analysis of all available RV time-series, including a set of 31 previously unpublished HARPS measurements, to investigate the effects of time-sampling and of simultaneous modelling of planetary + activity signals on the existence and origin of the curious 9 day signal. We conclude that the 9 day signal is real and was initially seen to be suppressed in the CARMENES data due to a small number of anomalous measurements, although the exact cause of these anomalies remains unknown. Investigation of the signal's evolution in time, with wavelength, and detailed model comparison reveals that the 9 day signal is most likely planetary in nature. By this analysis, we reconcile the conflicting HARPS and CARMENES results and measure precise and self-consistent planet masses of $m_{p,b} = 8.63 \pm 1.35$ and $m_{p,c}\sin{i_c}=5.62 \pm 0.84$ M$_{\oplus}$. This work, along with the previously published RV papers on the K2-18 planetary system, highlight the importance of understanding one's time-sampling and of simultaneous planet + stochastic activity modelling, particularly when searching for sub-Neptune-sized planets with radial velocities., 19 pages, 10 figures (including 9 interactive figures when viewed in Adobe Acrobat), accepted for publication in Astronomy & Astrophysics

Published
2019
Full Text
View/download PDF

4. Radial velocity follow-up of GJ1132 with HARPS

Author

Jonathan Irwin, Kristen Menou, Stéphane Udry, René Doyon, Ryan Cloutier, Elisabeth R. Newton, T. Forveille, Francesco Pepe, Rodrigo F. Díaz, François Bouchy, David Charbonneau, X. Delfosse, C. Lovis, Jose-Manuel Almenara, Zachory K. Berta-Thompson, Felipe Murgas, Xavier Bonfils, Nuno C. Santos, Jason A. Dittmann, Michel Mayor, A. Wünsche, Nicola Astudillo-Defru, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université du Québec à Rimouski (UQAR), Universidad de Concepción [Chile], Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Montréal (UdeM), Université du Texas, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Centro de Astrofísica da Universidade do Porto (CAUP), and Universidade do Porto

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Orbital elements, 010504 meteorology & atmospheric sciences, Red dwarf, Stellar rotation, stars: late-type, FOS: Physical sciences, Minimum mass, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Radial velocity, 13. Climate action, Space and Planetary Science, Planet, techniques: radial velocities, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], planetary systems, 010303 astronomy & astrophysics, Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

GJ1132 is a nearby red dwarf known to host a transiting Earth-size planet. After its initial detection, we pursued an intense follow-up with the HARPS velocimeter. We now confirm the detection of GJ1132b with radial velocities only. We refined its orbital parameters and, in particular, its mass ($m_b = 1.66\pm0.23 M_\oplus$), density ($��_b = 6.3\pm1.3$ g.cm$^{-3}$) and eccentricity ($e_b < 0.22 $; 95\%). We also detect at least one more planet in the system. GJ1132c is a super-Earth with period $P_c = 8.93\pm0.01$ days and minimum mass $m_c \sin i_c = 2.64\pm0.44~M_\oplus$. Receiving about 1.9 times more flux than Earth in our solar system, its equilibrium temperature is that of a temperate planet ($T_{eq}=230-300$ K for albedos $A=0.75-0.00$) and places GJ1132c near the inner edge of the so-called habitable zone. Despite an a priori favourable orientation for the system, $Spitzer$ observations reject most transit configurations, leaving a posterior probability $, accepted in Astronomy and Astrophysics

Published
2018
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results