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1. TOI-269 b: an eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author

Sara Seager, Eric B. Ting, Felipe Murgas, Nicholas M. Law, D. Maurel, S. Curaba, Tianjun Gan, S. Rochat, Richard G. West, George R. Ricker, Francesco Pepe, René Doyon, P. Kern, Coel Hellier, Jon M. Jenkins, Thibaut Moulin, I. C. Leão, G. Gaisne, Caroline Dorn, Xavier Bonfils, Laurent Jocou, Yves Magnard, J.-J. Correia, Eric Stadler, P. Rabou, C. Melo, Joshua N. Winn, C. Ziegler, J. D. Twicken, C. Lovis, Karen A. Collins, Nicola Astudillo-Defru, B. L. Canto Martins, Aurélien Wyttenbach, X. Delfosse, Alain Roux, Kevin I. Collins, Alain Delboulbé, J. F. Otegi, David R. Anderson, Jose-Manuel Almenara, William Waalkes, Ravit Helled, Marion Cointepas, François Bouchy, J. R. De Medeiros, Roland Vanderspek, Étienne Artigau, David Charbonneau, Pedro Figueira, T. Forveille, David W. Latham, L. Gluck, David R. Rodriguez, Andrew W. Mann, A. Wunsche, S. Lafrasse, Nuno C. Santos, Damien Ségransan, Rodrigo F. Díaz, Stéphane Udry, Philippe Feautrier, 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), 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]), and Université de Montréal (UdeM)

Subjects
010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, 01 natural sciences, Transmission spectroscopy, Photometry (optics), Neptune, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Radius, Orbital period, Exoplanet, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC 220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d = 57 pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P = 3.6977104 +- 0.0000037 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8 +- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions., Comment: 23 pages, 16 figures, Accepted for publication in A&A

Published
2021
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2. MASCARA-4 b/bRing-1 b: A retrograde hot Jupiter around a bright A-type star

Author

Andrés Jordán, Aurélien Wyttenbach, R. Hinojosa, David J. Osip, Eric E. Mamajek, B. Lomberg, Pascal Torres, Gilles Otten, Gáspár Á. Bakos, Matthew A. Kenworthy, Michael J. Ireland, Rafael Brahm, Rudi B. Kuhn, John I. Bailey, Remko Stuik, G. J. J. Talens, Steven M. Crawford, Ignas Snellen, Waqas Bhatti, Hodari-Sadiki James, L. Vanzi, A. Zapata, L. A. Paredes, Wei-Chun Jao, Todd J. Henry, Samuel N. Mellon, Vincent Suc, Patrick Dorval, Z. Csubry, Laboratoire d'Astrophysique de Marseille (LAM), and 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)

Subjects
Proper motion, 010504 meteorology & atmospheric sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Retrograde motion, stars: individual: bRing-1b, stars: individual: MASCARA-4b, Astronomy and Astrophysics, Planetary system, stars: individual: HD 85628, Radial velocity, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. The Multi-site All-Sky CAmeRA (MASCARA) and bRing are both photometric ground-based instruments with multiple stations that rely on interline charge-coupled devices with wide-field lenses to monitor bright stars in the local sky for variability. MASCARA has already discovered several planets in the northern sky, which are among the brightest known transiting hot Jupiter systems. Aims. In this paper, we aim to characterize a transiting planetary candidate in the southern skies found in the combined MASCARA and bRing data sets of HD 85628, an A7V star of V = 8.2 mag at a distance 172 pc, to establish its planetary nature. Methods. The candidate was originally detected in data obtained jointly with the MASCARA and bRing instruments using a Box Least-Square search for transit events. Further photometry was taken by the 0.7 m Chilean-Hungarian Automated Telescope (CHAT), and radial velocity measurements with the Fiber Dual Echelle Optical Spectrograph on the European Southern Observatory 1.0 m Telescope. High-resolution spectra during a transit were taken with the CTIO high-resolution spectrometer (CHIRON) on the Small and Moderate Aperture Research Telescope System 1.5 m telescope to target the Doppler shadow of the candidate. Results. We confirm the existence of a hot Jupiter transiting the bright A7V star HD 85628, which we co-designate as MASCARA-4b and bRing-1b. It is in an orbit of 2.824 days, with an estimated planet radius of 1.53−0.04+0.07 RJup and an estimated planet mass of 3.1 ± 0.9 MJup, putting it well within the planetary regime. The CHAT observations show a partial transit, reducing the probability that the transit was around a faint background star. The CHIRON observations show a clear Doppler shadow, implying that the transiting object is in a retrograde orbit with |λ| =244.9−3.6+2.7°. The planet orbits at a distance of 0.047 ± 0.004 AU from the star and has a zero-albedo equilibrium temperature of 2100 ± 100 K. In addition, we find that HD 85628 has a previously unreported stellar companion star in the Gaia DR2 data demonstrating common proper motion and parallax at 4.3′′ separation (projected separation ~740 AU), and with absolute magnitude consistent with being a K/M dwarf. Conclusions. MASCARA-4 b/bRing-1 b is the brightest transiting hot Jupiter known to date in a retrograde orbit. It further confirms that planets in near-polar and retrograde orbits are more common around early-type stars. Due to its high apparent brightness and short orbital period, the system is particularly well suited for further atmospheric characterization.

Published
2020
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3. Precise masses for the transiting planetary system HD 106315 with HARPS

Author

Isabelle Boisse, James A. G. Jackman, William D. Cochran, Don Pollacco, S. G. Sousa, Francesca Faedi, R. Ligi, Pedro Figueira, David J. Armstrong, Néstor Espinoza, C. Melo, J. Bento, Olivier Demangeon, Arthur Vigan, Xavier Dumusque, Monika Lendl, V. Adibekyan, H. P. Osborn, E. Foxell, Aurélien Wyttenbach, C. Lovis, S. C. C. Barros, Daniel Bayliss, Magali Deleuil, O. Mousis, Avi Shporer, Aldo S. Bonomo, H. Gosselin, James D. Armstrong, E. Delgado Mena, Amanda P. Doyle, Amaury H. M. J. Triaud, João P. Faria, A. Collier Cameron, Alexandre Santerne, David Ehrenreich, S. Hojjatpanah, Ramotholo Sefako, Guillaume Hébrard, B. Brugger, Duncan A. Brown, Rodrigo F. Díaz, Stéphane Udry, Nuno C. Santos, David Barrado, François Bouchy, J. J. Neal, Jorge Lillo-Box, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
010504 meteorology & atmospheric sciences, Ciencias Físicas, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Spectral line, COMPOSITION [PLANETS AND SATELLITES], purl.org/becyt/ford/1 [https], Planet, 0103 physical sciences, DETECTION [PLANETS AND SATELLITES], fundamental parameters [Planetary systems], QB Astronomy, Transit (astronomy), 010303 astronomy & astrophysics, QC, 0105 earth and related environmental sciences, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], detection [Planetary systems], photometric [Techniques], Astronomy and Astrophysics, Radius, purl.org/becyt/ford/1.3 [https], 3rd-DAS, Planetary system, individual HD 106315, EPIC 201437844 [Stars], Radial velocity, Astronomía, Photometry (astronomy), QC Physics, 13. Climate action, Space and Planetary Science, composition [Planetary systems], FUNDAMENTAL PARAMETERS [PLANETS AND SATELLITES], CIENCIAS NATURALES Y EXACTAS, INDIVIDUAL: HD 106315 [STARS], Astrophysics - Earth and Planetary Astrophysics
Abstract

The multi-planetary system HD 106315 was recently found in K2 data . The planets have periods of $P_b \sim9.55$ and $P_c \sim 21.06\,$days, and radii of $ r_b = 2.44 \pm 0.17\, $ and $r_c = 4.35 \pm 0.23\, $ $R_{\oplus}$. The brightness of the host star (V=9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. We obtained high precision radial velocities for HD~106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. We estimate the mass of HD 106315b to be 12.6 $\pm$ 3.2 $M_{\oplus}$ and the density to be $4.7 \pm 1.7\, g\,cm^{-3}$, while for HD 106315c we estimate a mass of 15.2 $\pm$ 3.7 $M_{\oplus}$ and a density of $1.01 \pm 0.29\, $g\,cm$^{-3}$. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5-29\%, and the water mass fraction to be 10-50\%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H-He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions., 16 pages, 9 figures, A\&A accepted

Published
2017
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4. Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) I. Detection of hot neutral sodium at high altitudes on WASP‐49b

Author

C. Lovis, David Ehrenreich, Damien Ségransan, Lorenzo Pino, Stéphane Udry, Alexandre Santerne, Francesco Pepe, Kevin Heng, Nicola Astudillo-Defru, Aurélien Wyttenbach, C. Melo, Heather M. Cegla, Baptiste Lavie, Felipe Murgas, Vincent Bourrier, Romain Allart, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and 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)

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Atmosphere, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Radius, Exoplanet, 3. Good health, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

High-resolution optical spectroscopy during the transit of HD 189733b, a prototypical hot Jupiter, allowed the resolution of the Na I D sodium lines in the planet, giving access to the extreme conditions of the planet upper atmosphere. We have undertaken HEARTS, a spectroscopic survey of exoplanet upper atmospheres, to perform a comparative study of hot gas giants and determine how stellar irradiation affect them. Here, we report on the first HEARTS observations of the hot Saturn-mass planet WASP-49b. We observed the planet with the HARPS high-resolution spectrograph at ESO 3.6m telescope. We collected 126 spectra of WASP-49, covering three transits of WASP-49b. We analyzed and modeled the planet transit spectrum, while paying particular attention to the treatment of potentially spurious signals of stellar origin. We spectrally resolve the Na I D lines in the planet atmosphere and show that these signatures are unlikely to arise from stellar contamination. The large contrasts of $2.0\pm0.5\%$ (D$_2$) and $1.8\pm0.7\%$ (D$_1$) require the presence of hot neutral sodium ($2,950^{+400}_{-500}$ K) at high altitudes ($\sim$1.5 planet radius or $\sim$45,000 km). From estimating the cloudiness index of WASP-49b, we determine its atmosphere to be cloud free at the altitudes probed by the sodium lines. WASP-49b is close to the border of the evaporation desert and exhibits an enhanced thermospheric signature with respect to a farther-away planet such as HD 189733b., Accepted for publication in A&A. 14 pages

Published
2017
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5. The HARPS search for southern extra-solar planets XXXVIII. Bayesian re-analysis of three systems. New super-Earths, unconfirmed signals, and magnetic cycles

Author

F. Bouchy, Willy Benz, Pedro Figueira, Nuno C. Santos, Damien Ségransan, Michel Mayor, Francesco Pepe, G. Lo Curto, Christoph Mordasini, Aurélien Wyttenbach, E. Pompei, Roi Alonso, Rodrigo F. Díaz, Stéphane Udry, A. Collier Cameron, Michaël Gillon, Maxime Marmier, Didier Queloz, Fatemeh Motalebi, Xavier Dumusque, A. Coffinet, C. Moutou, Christophe Lovis, Magali Deleuil, Don Pollacco, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Departamento de Matemàtica, PUC RIO, Physikalisches Institut [Bern], Universität Bern [Bern], Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-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), University of St Andrews [Scotland], 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), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto [Porto], Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, European Southern Observatory (ESO), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Canada-France-Hawaii Telescope Corporation, Université de Genève = University of Geneva (UNIGE), Universität Bern [Bern] (UNIBE), Universidade do Porto = University of Porto, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universidade do Porto, European Commission, Science & Technology Facilities Council, PPARC - Now STFC, and University of St Andrews. School of Physics and Astronomy

Subjects
statistical [Methods], Bayesian probability, NDAS, FOS: Physical sciences, Astrophysics, Bayesian inference, 01 natural sciences, Data modeling, Planet, 0103 physical sciences, QB Astronomy, data analysis [Methods], 010303 astronomy & astrophysics, QC, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 010308 nuclear & particles physics, Model selection, Astronomy and Astrophysics, Planetary system, Exoplanet, Stars, Planetary systems, QC Physics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the analysis of the entire HARPS observations of three stars that host planetary systems: HD1461, HD40307, and HD204313. The data set spans eight years and contains more than 200 nightly averaged velocity measurements for each star. This means that it is sensitive to both long-period and low-mass planets and also to the effects induced by stellar activity cycles. We modelled the data using Keplerian functions that correspond to planetary candidates and included the short- and long-term effects of magnetic activity. A Bayesian approach was taken both for the data modelling, which allowed us to include information from activity proxies such as $\log{(R'_{\rm HK})}$ in the velocity modelling, and for the model selection, which permitted determining the number of significant signals in the system. The Bayesian model comparison overcomes the limitations inherent to the traditional periodogram analysis. We report an additional super-Earth planet in the HD1461 system. Four out of the six planets previously reported for HD40307 are confirmed and characterised. We discuss the remaining two proposed signals. In particular, we show that when the systematic uncertainty associated with the techniques for estimating model probabilities are taken into account, the current data are not conclusive concerning the existence of the habitable-zone candidate HD40307 g. We also fully characterise the Neptune-mass planet that orbits HD204313 in 34.9 days., Comment: 23 pages + online material, 23 figures. Accepted for publication in A&A. Small typos and series numbering corrected

Published
2016
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