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1. HD207897 b: A dense sub-Neptune transiting a nearby and bright K-type star

Author

Heidari, N., Boisse, I., Orell-Mique, J., Hebrard, G., Acuna, L., Hara, N. C., Lillo-Box, J., Eastman, J. D., Arnold, L., Astudillo-Defru, N., Adibekyan, V., Bieryla, A., Bonfils, X., Bouchy, F., Barclay, T., Brasseur, C. E., Borgniet, S., Bourrier, V., Buchhave, L., Behmard, A., Beard, C., Batalha, N. M ., Courcol, B., Cortes-Zuleta, P., Collins, K., Carmona, A., Crossfield, I. J. M., Chontos, A., Delfosse, X., Dalal, S., Deleuil, M., Demangeon, O. D. S., Diaz, R. F., Dumusque, X., Daylan, T., Dragomir, D., Mena, E. Delgado, Dressing, C., Dai, F., Dalba, P. A., Ehrenreich, D., Forveille, T., Fulton, B., Fetherolf, T., Gaisne, G., Giacalone, S., Riazi, N., Hoyer, S., Hobson, M. J., Howard, A. W., Huber, D., Hill, M. L., Hirsch, L. A., Isaacson, H., Jenkins, J., Kane, S. R., Kiefer, F., Luque, R., Latham, D. W., Lubin, J., Lopez, T., Mousis, O., Moutou, C., Montagnier, G., Mignon, L., Mayo, A., Mocnik, T., Murphy, J. M. A., Palle, E., Pepe, F., Petigura, E. A., Rey, J., Ricker, G., Robertson, P., Roy, A., Rubenzahl, R. A., Rosenthal, L. J., Santerne, A., Santos, N. C., Sousa, S. G., Stassun, K. G., Stalport, M., Scarsdale, N., Strom, P. A., Seager, S., Segransan, D., Tenenbaum, P., Tronsgaard, R., Udry, S., Vanderspek, R., Vakili, F., Winn, J., and Weiss, L. M.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery and characterization of a transiting sub-Neptune orbiting with a 16.20 day period around a nearby (28 pc) and bright(V=8.37) K0V star HD207897 (TOI-1611). This discovery is based on photometric measurements from the Transiting Exoplanet Survey Satellite(TESS) mission and radial velocity (RV) observations from the SOPHIE, Automated Planet Finder (APF) and HIRES high precision spectrographs. We used EXOFASTv2 for simultaneously modeling the parameters of the planet and its host star, combining photometric and RV data to determine the planetary system parameters. We show that the planet has a radius of 2.50+/-0.08 RE and a mass of either 14.4+/-1.6 ME or 15.9+/-1.6 ME with nearly equal probability; the two solutions correspond to two possibilities for the stellar activity period. Hence, the density is either 5.1+/-0.7 g cm^-3 or 5.5^{+0.8}_{-0.7} g cm^-3, making it one of the relatively rare dense sub-Neptunes. The existence of such a dense planet at only 0.12 AU from its host star is unusual in the currently observed sub-Neptune (2

Published
2021
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2. The SOPHIE search for northern extrasolar planets. XVI. HD 158259: A compact planetary system in a near-3:2 mean motion resonance chain

Author

Hara, N. C., Bouchy, F., Stalport, M., Boisse, I., Rodrigues, J., Delisle, J-. B., Santerne, A., Henry, G. W., Arnold, L., Astudillo-Defru, N., Borgniet, S., Bonfils, X., Bourrier, V., Brugger, B., Courcol, B., Dalal, S., Deleuil, M., Delfosse, X., Demangeon, O., D'iaz, R. F., Dumusque, X., Forveille, T., Hébrard, G., Hobson, M., Kiefer, F., Lopez, T., Mignon, L., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santos, N. C., Ségransan, D., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Since 2011, the SOPHIE spectrograph has been used to search for Neptunes and super-Earths in the Northern Hemisphere. As part of this observational program, 290 radial velocity measurements of the 6.4 V magnitude star HD 158259 were obtained. Additionally, TESS photometric measurements of this target are available. We present an analysis of the SOPHIE data and compare our results with the output of the TESS pipeline. The radial velocity data, ancillary spectroscopic indices, and ground-based photometric measurements were analyzed with classical and $\ell_1$ periodograms. The stellar activity was modeled as a correlated Gaussian noise and its impact on the planet detection was measured with a new technique. The SOPHIE data support the detection of five planets, each with $m \sin i \approx 6 M_\oplus$, orbiting HD 158259 in 3.4, 5.2, 7.9, 12, and 17.4 days. Though a planetary origin is strongly favored, the 17.4 d signal is classified as a planet candidate due to a slightly lower statistical significance and to its proximity to the expected stellar rotation period. The data also present low frequency variations, most likely originating from a magnetic cycle and instrument systematics. Furthermore, the TESS pipeline reports a significant signal at 2.17 days corresponding to a planet of radius $\approx 1.2 R_\oplus$. A compatible signal is seen in the radial velocities, which confirms the detection of an additional planet and yields a $\approx 2 M_\oplus$ mass estimate. We find a system of five planets and a strong candidate near a 3:2 mean motion resonance chain orbiting HD 158259. The planets are found to be outside of the two and three body resonances., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2019
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3. The detection and characterisation of 54 massive companions with the SOPHIE spectrograph -- 7 new brown dwarfs and constraints on the BD desert

Author

Kiefer, F., Hébrard, G., Sahlmann, J., Sousa, S. G., Forveille, T., Santos, N., Mayor, M., Deleuil, M., Wilson, P. A., Dalal, S., Díaz, R. F., Henry, G. W., Hagelberg, J., Hobson, M. J., Demangeon, O., Bourrier, V., Delfosse, X., Arnold, L., Astudillo-Defru, N., Beuzit, J. -L., Boisse, I., Bonfils, X., Borgniet, S., Bouchy, F., Courcol, B., Ehrenreich, D., Hara, N., Lagrange, A. -M., Lovis, C., Montagnier, G., Moutou, C., Pepe, F., Perrier, C., Rey, J., Santerne, A., Ségransan, D., Udry, S., and Vidal-Madjar, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Brown-dwarfs are substellar objects with masses intermediate between planets and stars within about 13-80Mjup. While isolated BDs are most likely produced by gravitational collapse in molecular clouds down to masses of a few Mjup, a non-negligible fraction of low-mass companions might be formed through the planet formation channel in protoplanetary disks. The upper mass limit of objects formed within disks is still observationally unknown, the main reason being the strong dearth of BD companions at orbital periods shorter than 10 years, a.k.a. the BD desert. To address this question, we aim at determining the best statistics of secondary companions within the 10-100Mjup range and within 10 au from the primary star, while minimising observational bias. We made an extensive use of the RV surveys of FGK stars below 60pc distance to the Sun and in the northern hemisphere performed with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We derived the Keplerian solutions of the RV variations of 54 sources. Public astrometric data of the Hipparcos and Gaia missions allowed constraining the mass of the companion for most sources. We introduce GASTON, a new method to derive inclination combining RVs Keplerian and astrometric excess noise from Gaia DR1. We report the discovery of 12 new BD candidates. For 5 of them, additional astrometric data led to revise their mass in the M-dwarf regime. Among the 7 remaining objects, 4 are confirmed BD companions, and 3 others are likely in this mass regime. We also report the detection of 42 M-dwarfs within 90Mjup-0.52Msun. The resulting Msin(i)-P distribution of BD candidates shows a clear drop in the detection rate below 80-day orbital period. Above that limit, the BD desert reveals rather wet, with a uniform distribution of the Msin(i). We derive a minimum BD-detection frequency around Solar-like stars of 2.0+/-0.5%., Comment: 51 pages, 20 figures, 16 tables

Published
2019
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4. The SOPHIE search for northern extrasolar planets XV. A Warm Neptune around the M-dwarf Gl378

Author

Hobson, M. J., Delfosse, X., Astudillo-Defru, N., Boisse, I., Díaz, R. F., Bouchy, F., Bonfils, X., Forveille, T., Arnold, L., Borgniet, S., Bourrier, V., Brugger, B., Salazar, N. Cabrera, Courcol, B., Dalal, S., Deleuil, M., Demangeon, O., Dumusque, X., Hara, N., Hébrard, G., Kiefer, F., Lopez, T., Mignon, L., Montagnier, G., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santerne, A., Santos, N. C., Stalport, M., Ségransan, D., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the detection of a Warm Neptune orbiting the M-dwarf Gl378, using radial velocity measurements obtained with the SOPHIE spectrograph at the Observatoire de Haute-Provence. The star was observed in the context of the SOPHIE exoplanets consortium's subprogramme dedicated to finding planets around M-dwarfs. Gl378 is an M1 star, of solar metallicity, at a distance of 14.96 pc. The single planet detected, Gl378 b, has a minimum mass of 13.02 $\rm M_{Earth}$ and an orbital period of 3.82 days, which place it at the lower boundary of the Hot Neptune desert. As one of only a few such planets around M-dwarfs, Gl378 b provides important clues to the evolutionary history of these close-in planets. In particular, the eccentricity of 0.1 may point to a high-eccentricity migration. The planet may also have lost part of its envelope due to irradiation., Comment: 10 pages, 8 figures, accepted for publication in A&A

Published
2019
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5. SOPHIE velocimetry of Kepler transit candidates. XIX. The transiting temperate giant planet KOI-3680b

Author

Hebrard, G., Bonomo, A. S., Diaz, R. F., Santerne, A., Santos, N. C., Almenara, J. -M., Barros, S. C. C., Boisse, I., Bouchy, F., Bruno, G., Courcol, B., Deleuil, M., Demangeon, O., Guillot, T., Montagnier, G., Moutou, C., Rey, J., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Whereas thousands of transiting giant exoplanets are known today, only a few are well characterized with long orbital periods. Here we present KOI-3680b, a new planet in this category. First identified by the Kepler team as a promising candidate from the photometry of the Kepler spacecraft, we establish here its planetary nature from the radial velocity follow-up secured over two years with the SOPHIE spectrograph at Observatoire de Haute-Provence, France. The combined analysis of the whole dataset allows us to fully characterize this new planetary system. KOI-3680b has an orbital period of 141.2417 +/- 0.0001 days, a mass of 1.93 +/- 0.20 M_Jup, and a radius of 0.99 +/- 0.07 R_Jup. It exhibits a highly eccentric orbit (e = 0.50 +/- 0.03) around an early G dwarf. KOI-3680b is the transiting giant planet with the longest period characterized so far around a single star; it offers opportunities to extend studies which were mainly devoted to exoplanets close to their host stars, and to compare both exoplanet populations., Comment: 10 pages, 9 figures, 4 tables, accepted for publication in A&A

Published
2018
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6. The SOPHIE search for northern extrasolar planets XIII. Two planets around M-dwarfs Gl617A and Gl96

Author

Hobson, M. J., Díaz, R. F., Delfosse, X., Astudillo-Defru, N., Boisse, I., Bouchy, F., Bonfils, X., Forveille, T., Hara, N., Arnold, L., Borgniet, S., Bourrier, V., Brugger, B., Cabrera, N., Courcol, B., Dalal, S., Deleuil, M., Demangeon, O., Dumusque, X., Ehrenreich, D., Hébrard, G., Kiefer, F., Lopez, T., Mignon, L., Montagnier, G., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santerne, A., Santos, N., Stalport, M., Ségransan, D., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the detection of two exoplanets and a further tentative candidate around the M-dwarf stars Gl96 and Gl617A, based on radial velocity measurements obtained with the SOPHIE spectrograph at the Observatoire de Haute-Provence. Both stars were observed in the context of the SOPHIE exoplanet consortium's dedicated M-dwarf subprogramme, which aims to detect exoplanets around nearby M-dwarf stars through a systematic survey. For Gl96, we present the discovery of a new exoplanet at 73.9 d with a minimum mass of 19.66 earth masses. Gl96 b has an eccentricity of 0.44, placing it among the most eccentric planets orbiting M stars. For Gl617A we independently confirm a recently reported exoplanet at 86.7 d with a minimum mass of 31.29 earth masses. Both Gl96 b and Gl617A b are potentially within the habitable zone, though Gl96 b's high eccentricity may take it too close to the star at periapsis., Comment: 22 pages, 23 figures

Published
2018
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7. SOPHIE velocimetry of Kepler transit candidates XVIII. Radial velocity confirmation, absolute masses and radii, and origin of the Kepler-419 multiplanetary system

Author

Almenara, J. M., Díaz, R. F., Hébrard, G., Mardling, R., Damiani, C., Santerne, A., Bouchy, F., Barros, S. C. C., Boisse, I., Bonfils, X., Bonomo, A. S., Courcol, B., Demangeon, O., Deleuil, M., Rey, J., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Kepler-419 is a planetary system discovered by the Kepler photometry which is known to harbour two massive giant planets: [...] Here we present new radial velocity (RV) measurements secured over more than two years with the SOPHIE spectrograph, where both planets are clearly detected. The RV data is modelled together with the Kepler photometry using a photodynamical model. The inclusion of velocity information breaks the $MR^{-3}$ degeneracy inherent in timing data alone, allowing us to measure the absolute stellar and planetary radii and masses. With uncertainties of 12% and 13% for the stellar and inner planet radii, and 35%, 24%, and 35% for the masses of the star, planet b, and planet c respectively, these measurements are the most precise to date for a single host star system using this technique. The transiting planet mass is determined at better precision than the star mass. This shows that modelling the radial velocities and the light curve together in systems of dynamically interacting planets provides a way of characterising both the star and the planets without being limited by knowledge of the star. On the other hand, the period ratio and eccentricities place the Kepler-419 system in a sweet spot; had around twice as many transits been observed, the mass of the transiting planet could have been measured using its own TTVs. Finally, the origin of the Kepler-419 system is discussed. We show that the system is near a coplanar high-eccentricity secular fixed point, related to the alignment of the orbits, which has prevented the inner orbit from circularising. For most other relative apsidal orientations, planet b's orbit would be circular with a semi-major axis of 0.03 au. This suggests a mechanism for forming hot Jupiters in multiplanetary systems without the need of high mutual inclinations., Comment: 16 pages, 17 figures, accepted for publication in A&A

Published
2018
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8. Discovery of XO-6b: a hot Jupiter transiting a fast rotating F5 star on an oblique orbit

Author

Crouzet, N., McCullough, P. R., Long, D., Rodriguez, P. Montanes, Etangs, A. Lecavelier des, Ribas, I., Bourrier, V., Hébrard, G., Vilardell, F., Deleuil, M., Herrero, E., Garcia-Melendo, E., Akhenak, L., Foote, J., Gary, B., Benni, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., and Demangeon, O.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Only a few hot Jupiters are known to orbit around fast rotating stars. These exoplanets are harder to detect and characterize and may be less common than around slow rotators. Here, we report the discovery of the transiting hot Jupiter XO-6b, which orbits a bright, hot, and fast rotating star: V = 10.25, Teff = 6720 +/- 100 K, v sin i = 48 +/- 3 km/s. We detected the planet from its transits using the XO instruments and conducted a follow-up campaign. Because of the fast stellar rotation, radial velocities taken along the orbit do not yield the planet's mass with a high confidence level, but we secure a 3-sigma upper limit Mp < 4.4 MJup. We also obtain high resolution spectroscopic observations of the transit with the SOPHIE spectrograph at the 193-cm telescope of the Observatoire de Haute-Provence and analyze the stellar lines profile by Doppler tomography. The transit is clearly detected in the spectra. The radii measured independently from the tomographic analysis and from the photometric lightcurves are consistent, showing that the object detected by both methods is the same and indeed transits in front of XO-6. We find that XO-6b lies on a prograde and misaligned orbit with a sky-projected obliquity lambda = -20.7 +/- 2.3 deg. The rotation period of the star is shorter than the orbital period of the planet: Prot < 2.12 days, Porb = 3.77 days. Thus, this system stands in a largely unexplored regime of dynamical interactions between close-in giant planets and their host stars., Comment: 12 pages, 11 figures, Accepted for publication in AJ

Published
2016
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9. The SOPHIE search for northern extrasolar planets. XI. Three new companions and an orbit update: Giant planets in the habitable zone

Author

Díaz, R. F., Rey, J., Demangeon, O., Hébrard, G., Boisse, I., Arnold, L., Astudillo-Defru, N., Beuzit, J. -L., Bonfils, X., Borgniet, S., Bouchy, F., Bourrier, V., Courcol, B., Deleuil, M., Delfosse, X., Ehrenreich, D., Forveille, T., Lagrange, A. -M., Mayor, M., Moutou, C., Pepe, F., Queloz, D., Santerne, A., Santos, N. C., Sahlmann, J., Ségransan, D., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of three new substellar companions to solar-type stars, HD191806, HD214823, and HD221585, based on radial velocity measurements obtained at the Haute-Provence Observatory. Data from the SOPHIE spectrograph are combined with observations acquired with its predecessor, ELODIE, to detect and characterise the orbital parameters of three new gaseous giant and brown dwarf candidates. Additionally, we combine SOPHIE data with velocities obtained at the Lick Observatory to improve the parameters of an already known giant planet companion, HD16175 b. Thanks to the use of different instruments, the data sets of all four targets span more than ten years. Zero-point offsets between instruments are dealt with using Bayesian priors to incorporate the information we possess on the SOPHIE/ELODIE offset based on previous studies. The reported companions have orbital periods between three and five years and minimum masses between 1.6 Mjup and 19 Mjup. Additionally, we find that the star HD191806 is experiencing a secular acceleration of over 11 \ms\ per year, potentially due to an additional stellar or substellar companion. A search for the astrometric signature of these companions was carried out using Hipparcos data. No orbit was detected, but a significant upper limit to the companion mass can be set for HD221585, whose companion must be substellar. With the exception of HD191806 b, the companions are located within the habitable zone of their host star. Therefore, satellites orbiting these objects could be a propitious place for life to develop., Comment: 12 pages + tables, 7 figures. Accepted for publication in Astronomy & Astrophysics

Published
2016
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10. The SOPHIE search for northern extrasolar planets. X. Detection and characterization of giant planets by the dozen

Author

Hebrard, G., Arnold, L., Forveille, T., Correia, A. C. M., Laskar, J., Bonfils, X., Boisse, I., Diaz, R. F., Hagelberg, J., Sahlmann, J., Santos, N. C., Astudillo-Defru, N., Borgniet, S., Bouchy, F., Bourrier, V., Courcol, B., Delfosse, X., Deleuil, M., Demangeon, O., Ehrenreich, D., Gregorio, J., Jovanovic, N., Labrevoir, O., Lagrange, A. -M., Lovis, C., Lozi, J., Moutou, C., Montagnier, G., Pepe, F., Rey, J., Santerne, A., Segransan, D., Udry, S., Vanhuysse, M., Vigan, A., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new radial velocity measurements of eight stars secured with the spectrograph SOPHIE at the 193-cm telescope of the Haute-Provence Observatory allowing the detection and characterization of new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes between 6.7 and 9.6; the planets have minimum masses M_p sin i between 0.4 to 3.8 M_Jup and orbital periods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD143105, HIP109600, HD35759, HIP109384, HD220842, and HD12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP65407, allows the discovery of two giant planets, just outside the 12:5 resonance in weak mutual interaction. The last star, HD141399, was already known to host a four-planetary system; our additional data and analyses allow new constraints to be put on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planetary systems. HD143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted despite this is not a transiting system. The giant planets HIP109600b, HIP109384b, and HD141399c are located in the habitable zone of their host star., Comment: 20 pages, 19 figures, 5 tables, accepted for publication in A&A

Published
2016
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11. The SOPHIE search for northern extrasolar planets IX. Populating the brown dwarf desert

Author

Wilson, P. A., Hébrard, G., Santos, N. C., Sahlmann, J., Montagnier, G., Astudillo-Defru, N., Boisse, I., Bouchy, F., Rey, J., Arnold, L., Bonfils, X., Bourrier, V., Courcol, B., Deleuil, M., Delfosse, X., Díaz, R. F., Ehrenreich, D., Forveille, T., Moutou, C., Pepe, F., Santerne, A., Ségransan, D., and Udry, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Radial velocity planet search surveys of nearby Solar-type stars have shown a strong deficit of brown dwarf companions within $\sim5\,\mathrm{AU}$. There is presently no comprehensive explanation of this lack of brown dwarf companions, therefore, increasing the sample of such objects is crucial to understand their formation and evolution. Based on precise radial velocities obtained using the SOPHIE spectrograph at Observatoire de Haute-Provence we characterise the orbital parameters of $15$ companions to solar-type stars and constrain their true mass using astrometric data from the Hipparcos space mission. The nine companions not shown to be stellar in nature have minimum masses ranging from ~$13$ to $70\,\mathrm{M}_{\mathrm{Jup}}$, and are well distributed across the planet/brown dwarf mass regime, making them an important contribution to the known population of massive companions around solar-type stars. We characterise six companions as stellar in nature with masses ranging from a minimum mass of $76 \pm 4\,\mathrm{M}_{\mathrm{Jup}}$ to a mass of $0.35 \pm 0.03\,\mathrm{M_\odot}$. The orbital parameters of two previously known sub-stellar candidates are improved., Comment: 16 pages, 9 figures

Published
2016
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12. EPIC211089792 b: an aligned and inflated hot jupiter in a young visual binary

Author

Santerne, A., Hébrard, G., Lillo-Box, J., Armstrong, D. J., Barros, S. C. C., Demangeon, O., Barrado, D., Debackere, A., Deleuil, M., Mena, E. Delgado, Montalto, M., Pollacco, D., Osborn, H. P., Sousa, S. G., Abe, L., Adibekyan, V., Almenara, J. -M., André, P., Arlic, G., Barthe, G., Bendjoya, P., Behrend, R., Boisse, I., Bouchy, F., Boussier, H., Bretton, M., Brown, D. J. A., Carry, B., Cailleau, A., Conseil, E., Courcol, B., Dauchet, B., Dalouzy, J. -C., Deldem, M., Dubreuil, P., Fehrenbach, J. -M., Ferratfiat, S., Girelli, R., Gregorio, J., Jaecques, S., Kugel, F., Kirk, J., Labrevoir, O., Lachurié, J. -C., Lam, K. W. F., Guen, P. Le, Martinez, P., Maurin, L., McCormac, J., Pioppa, J-B., Quadri, U., Rajpurohit, A., Rey, J., Rivet, J. -P., Roy, R., Santos, N. C., Signoret, F., Strabla, L., Suarez, O., Toublanc, D., Tsantaki, M., Wilson, P. A., Bachschmidt, M., Colas, F., Gerteis, O., Louis, P., Mario, J. -C., Marlot, C., Montier, J., Perroud, V., Pic, V., Romeuf, D., Ubaud, S., and Verilhac, D.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In the present paper we report the discovery of a new hot Jupiter, EPIC211089792 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25d, a mass of 0.73 +/- 0.04 Mjup, and a radius of 1.19 +/- 0.02 Rjup. The host star is a relatively bright (V=12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of Lithium, we find that the system might be as young as about 450 Myr. The observation of the Rossiter-McLaughlin effect shows the planet is aligned with respect to the stellar spin. Given the deep transit (20mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where the both stars are relatively bright., Comment: Submitted to ApJ

Published
2016
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13. K2-30b and K2-34b: two inflated hot-Jupiters around Solar-type stars

Author

Lillo-Box, J., Demangeon, O., Santerne, A., Barros, S. C. C., Barrado, D., Hébrard, G., Osborn, H. P., Armstrong, D. J., Almenara, J. -M., Boisse, I., Bouchy, F., Brown, D. J. A., Courcol, B., Deleuil, M., Mena, E. Delgado, Díaz, R. F., Kirk, J., Lam, K. W. F., McCormac, J., Pollacco, D., Rajpurohit, A., Rey, J., Santos, N. C., Sousa, S. G., Tsantaki, M., and Wilson, P. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of the two hot-Jupiters K2-30b and K2-34b. The two planets were detected transiting their main-sequence star with periods $\sim$ 4.099 and $\sim$ 2.996 days, in campaigns 4 and 5 of the extension of the Kepler mission, K2. Subsequent ground-based radial velocity follow-up with SOPHIE, HARPS-N and CAFE, established the planetary nature of the transiting objects. We analyzed the transit signal, radial velocity and spectral energy distributions of the two systems to characterize their properties. Both planets (K2-30b and K2-34b) are bloated hot-Jupiters (1.25 $R_{\rm Jup}$ and 1.33 $R_{\rm Jup}$) around relatively bright (V =13.5 and V=11.5), slow rotating main-sequence (G8 and F9) stars. Thus, these systems are good candidates for detecting the Rossiter-MacLaughlin effect to measure their obliquity and for atmospheric studies., Comment: 7 pages, 3 figures, 7 tables, accepted for publication in A&A

Published
2016
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14. The SOPHIE search for northern extrasolar planets VIII. Follow-up of ELODIE candidates: long-period brown-dwarf companions

Author

Bouchy, F., Ségransan, D., Díaz, R. F., Forveille, T., Boisse, I., Arnold, L., Astudillo-Defru, N., Beuzit, J. -L., Bonfils, X., Borgniet, S., Bourrier, V., Courcol, B., Delfosse, X., Demangeon, O., Delorme, P., Ehrenreich, D., Hébrard, G., Lagrange, A. -M., Mayor, M., Montagnier, G., Moutou, C., Naef, D., Pepe, F., Perrier, C., Queloz, D., Rey, J., Sahlmann, J., Santerne, A., Santos, N. C., Sivan, J. -P., Udry, S., and Wilson, P. A.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Long-period brown dwarf companions detected in radial velocity surveys are important targets for direct imaging and astrometry to calibrate the mass-luminosity relation of substellar objects. Through a 20-year radial velocity monitoring of solar-type stars that began with ELODIE and was extended with SOPHIE spectrographs, giant exoplanets and brown dwarfs with orbital periods longer than ten years are discovered. We report the detection of five new potential brown dwarfs with minimum masses between 32 and 83 Jupiter mass orbiting solar-type stars with periods longer than ten years. An upper mass limit of these companions is provided using astrometric Hipparcos data, high-angular resolution imaging made with PUEO, and a deep analysis of the cross-correlation function of the main stellar spectra to search for blend effects or faint secondary components. These objects double the number of known brown dwarf companions with orbital periods longer than ten years and reinforce the conclusion that the occurrence of such objects increases with orbital separation. With a projected separation larger than 100 mas, all these brown dwarf candidates are appropriate targets for high-contrast and high angular resolution imaging., Comment: 17 pages, 9 figures, accepted in A&A

Published
2015
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15. SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period

Author

Santerne, A., Moutou, C., Tsantaki, M., Bouchy, F., Hébrard, G., Adibekyan, V., Almenara, J. -M., Amard, L., Barros, S. C. C., Boisse, I., Bonomo, A. S., Bruno, G., Courcol, B., Deleuil, M., Demangeon, O., Díaz, R. F., Guillot, T., Havel, M., Montagnier, G., Rajpurohit, A. S., Rey, J., and Santos, N. C.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

While giant extrasolar planets have been studied for more than two decades now, there are still some open questions such as their dominant formation and migration process, as well as their atmospheric evolution in different stellar environments. In this paper, we study a sample of giant transiting exoplanets detected by the Kepler telescope with orbital periods up to 400 days. We first defined a sample of 129 giant-planet candidates that we followed up with the SOPHIE spectrograph (OHP, France) in a 6-year radial velocity campaign. This allow us to unveil the nature of these candidates and to measure a false-positive rate of 54.6 +/- 6.5 % for giant-planet candidates orbiting within 400 days of period. Based on a sample of confirmed or likely planets, we then derive the occurrence rates of giant planets in different ranges of orbital periods. The overall occurrence rate of giant planets within 400 days is 4.6 +/- 0.6 %. We recover, for the first time in the Kepler data, the different populations of giant planets reported by radial velocity surveys. Comparing these rates with other yields, we find that the occurrence rate of giant planets is lower only for hot jupiters but not for the longer period planets. We also derive a first measurement on the occurrence rate of brown dwarfs in the brown-dwarf desert with a value of 0.29 +/- 0.17 %. Finally, we discuss the physical properties of the giant planets in our sample. We confirm that giant planets receiving a moderate irradiation are not inflated but we find that they are in average smaller than predicted by formation and evolution models. In this regime of low-irradiated giant planets, we find a possible correlation between their bulk density and the Iron abundance of the host star, which needs more detections to be confirmed., Comment: To appear in Astronomy and Astrophysics

Published
2015
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16. Photo-dynamical mass determination of the multi-planetary system K2-19

Author

Barros, S. C. C., Almenara, J. M., Demangeon, O., Tsantaki, M., Santerne, A., Armstrong, D. J., Barrado, D., Brown, D., Deleuil, M., Lillo-Box, J., Osborn, H., Pollacco, D., Abe, L., Andre, P., Bendjoya, P., Boisse, I., Bonomo, A. S., Bouchy, F., Bruno, G., Cerda, J. Rey, Courcol, B., Díaz, R. F., Hébrard, G., Kirk, J., Lachurié, J. C., Lam, K. W. F., Martinez, P., McCormac, J., Moutou, C., Rajpurohit, A., Rivet, J. -P., Spake, J., Suarez, O., Toublanc, D., and Walker, S. R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

K2-19 is the second multi-planetary system discovered with K2 observations. The system is composed of two Neptune size planets close to the 3:2 mean-motion resonance. To better characterise the system we obtained two additional transit observations of K2-19b and five additional radial velocity observations. These were combined with K2 data and fitted simultaneously with the system dynamics (photo-dynamical model) which increases the precision of the transit time measurements. The higher transit time precision allows us to detect the chopping signal of the dynamic interaction of the planets that in turn permits to uniquely characterise the system. Although the reflex motion of the star was not detected, dynamic modelling of the system allowed us to derive planetary masses of $M_b= 44 \pm 12\, M_{\oplus}$ and $M_c = 15.9 \pm 7.0\, M_{\oplus}$ for the inner and the outer planets respectively, leading to densities close to Uranus. We also show that our method allows the derivation of mass ratios using only the 80 days of observations during the first campaign of K2., Comment: 10 pages, 7 figures, 2 tables, MNRAS accepted

Published
2015
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17. The SOPHIE search for northern extrasolar planets VIII. A warm Neptune orbiting HD164595

Author

Courcol, B., Bouchy, F., Pepe, F., Santerne, A., Delfosse, X., Arnold, L., Astudillo-Defru, N., Boisse, I., Bonfils, X., Borgniet, S., Bourrier, V., Cabrera, N., Deleuil, M., Demangeon, O., Díaz, R. F., Ehrenreich, D., Forveille, T., Hébrard, G., Lagrange, A. M., Montagnier, G., Moutou, C., Rey, J., Santos, N. C., Ségransan, D., Udry, S., and Wilson, Paul A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

High-precision radial velocity surveys explore the population of low-mass exoplanets orbiting bright stars. This allows accurately deriving their orbital parameters such as their occurrence rate and the statistical distribution of their properties. Based on this, models of planetary formation and evolution can be constrained. The SOPHIE spectrograph has been continuously improved in past years, and thanks to an appropriate correction of systematic instrumental drift, it is now reaching 2 m/s precision in radial velocity measurements on all timescales. As part of a dedicated radial velocity survey devoted to search for low-mass planets around a sample of 190 bright solar-type stars in the northern hemisphere, we report the detection of a warm Neptune with a minimum mass of 16.1 +- 2.7 Mearth orbiting the solar analog HD164595 in 40 +- 0.24 days . We also revised the parameters of the multiplanetary system around HD190360. We discuss this new detection in the context of the upcoming space mission CHEOPS, which is devoted to a transit search of bright stars harboring known exoplanets., Comment: 11 pages, 9 figures

Published
2015
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18. WASP-135b : A Highly Irradiated, Inflated Hot Jupiter Orbiting a G5V Star

Author

Spake, J. J., Brown, D. J. A., Doyle, A. P., Hébrard, G., McCormac, J., Armstrong, D. J., Pollacco, D., Chew, Y. Gómez Maqueo, Anderson, D. R., Barros, S. C. C., Bouchy, F., Boumis, P., Bruno, G., Cameron, A. Collier, Courcol, B., Davies, G. R., Faedi, F., Hellier, C., Kirk, J., Lam, K. W. F., Liakos, A., Louden, T., Maxted, P. F. L., Osborn, H. P., Palle, E., Arranz, J. Prieto, Udry, S., Walker, S. R., West, R. G., and Wheatley, P. J.

Published
2016

19. HD 207897 b:A dense sub-Neptune transiting a nearby and bright K-type star

Author

Heidari, N., Boisse, I., Orell-Miquel, J., Hébrard, G., Acuña, L., Hara, N. C., Lillo-Box, J., Eastman, J. D., Arnold, L., Astudillo-Defru, N., Adibekyan, V., Bieryla, A., Bonfils, X., Bouchy, F., Barclay, T., Brasseur, C. E., Borgniet, S., Bourrier, V., Buchhave, L., Behmard, A., Beard, C., Batalha, N. M., Courcol, B., Cortés-Zuleta, P., Collins, K., Carmona, A., Crossfield, I. J.M., Chontos, A., Delfosse, X., Dalal, S., Deleuil, M., Demangeon, O. D.S., Diáz, R. F., Dumusque, X., Daylan, T., Dragomir, D., Delgado Mena, E., Dressing, C., Dai, F., Dalba, P. A., Ehrenreich, D., Forveille, T., Fulton, B., Fetherolf, T., Gaisné, G., Giacalone, S., Riazi, N., Hoyer, S., Hobson, M. J., Howard, A. W., Huber, D., Hill, M. L., Hirsch, L. A., Isaacson, H., Jenkins, J., Kane, S. R., Kiefer, F., Luque, R., Latham, D. W., Lubin, J., Lopez, T., Mousis, O., Moutou, C., Montagnier, G., Mignon, L., Mayo, A., Močnik, T., Murphy, J. M.A., Palle, E., Pepe, F., Petigura, E. A., Rey, J., Ricker, G., Robertson, P., Roy, A., Rubenzahl, R. A., Rosenthal, L. J., Santerne, A., Santos, N. C., Sousa, S. G., Stassun, K. G., Stalport, M., Scarsdale, N., Strøm, P. A., Seager, S., Segransan, D., Tenenbaum, P., Tronsgaard, R., Udry, S., Vanderspek, R., Vakili, F., Winn, J., Weiss, L. M., Heidari, N., Boisse, I., Orell-Miquel, J., Hébrard, G., Acuña, L., Hara, N. C., Lillo-Box, J., Eastman, J. D., Arnold, L., Astudillo-Defru, N., Adibekyan, V., Bieryla, A., Bonfils, X., Bouchy, F., Barclay, T., Brasseur, C. E., Borgniet, S., Bourrier, V., Buchhave, L., Behmard, A., Beard, C., Batalha, N. M., Courcol, B., Cortés-Zuleta, P., Collins, K., Carmona, A., Crossfield, I. J.M., Chontos, A., Delfosse, X., Dalal, S., Deleuil, M., Demangeon, O. D.S., Diáz, R. F., Dumusque, X., Daylan, T., Dragomir, D., Delgado Mena, E., Dressing, C., Dai, F., Dalba, P. A., Ehrenreich, D., Forveille, T., Fulton, B., Fetherolf, T., Gaisné, G., Giacalone, S., Riazi, N., Hoyer, S., Hobson, M. J., Howard, A. W., Huber, D., Hill, M. L., Hirsch, L. A., Isaacson, H., Jenkins, J., Kane, S. R., Kiefer, F., Luque, R., Latham, D. W., Lubin, J., Lopez, T., Mousis, O., Moutou, C., Montagnier, G., Mignon, L., Mayo, A., Močnik, T., Murphy, J. M.A., Palle, E., Pepe, F., Petigura, E. A., Rey, J., Ricker, G., Robertson, P., Roy, A., Rubenzahl, R. A., Rosenthal, L. J., Santerne, A., Santos, N. C., Sousa, S. G., Stassun, K. G., Stalport, M., Scarsdale, N., Strøm, P. A., Seager, S., Segransan, D., Tenenbaum, P., Tronsgaard, R., Udry, S., Vanderspek, R., Vakili, F., Winn, J., and Weiss, L. M.

Abstract

We present the discovery and characterization of a transiting sub-Neptune that orbits the nearby (28 pc) and bright (V = 8.37) K0V star HD 207897 (TOI-1611) with a 16.20-day period. This discovery is based on photometric measurements from the Transiting Exoplanet Survey Satellite mission and radial velocity (RV) observations from the SOPHIE, Automated Planet Finder, and HIRES high-precision spectrographs. We used EXOFASTv2 to model the parameters of the planet and its host star simultaneously, combining photometric and RV data to determine the planetary system parameters. We show that the planet has a radius of 2.50 ± 0.08 RE and a mass of either 14.4 ± 1.6 ME or 15.9 ± 1.6 ME with nearly equal probability. The two solutions correspond to two possibilities for the stellar activity period. The density accordingly is either 5.1 ± 0.7 g cm3 or 5.50.7+0.8 g cm3, making it one of the relatively rare dense sub-Neptunes. The existence of this dense planet at only 0.12 AU from its host star is unusual in the currently observed sub-Neptune (2 < RE < 4) population. The most likely scenario is that this planet has migrated to its current position.

Published
2022

20. HD 207897 b: A dense sub-Neptune transiting a nearby and bright K-type star

Author

Heidari, N., primary, Boisse, I., additional, Orell-Miquel, J., additional, Hébrard, G., additional, Acuña, L., additional, Hara, N. C., additional, Lillo-Box, J., additional, Eastman, J. D., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Adibekyan, V., additional, Bieryla, A., additional, Bonfils, X., additional, Bouchy, F., additional, Barclay, T., additional, Brasseur, C. E., additional, Borgniet, S., additional, Bourrier, V., additional, Buchhave, L., additional, Behmard, A., additional, Beard, C., additional, Batalha, N. M., additional, Courcol, B., additional, Cortés-Zuleta, P., additional, Collins, K., additional, Carmona, A., additional, Crossfield, I. J. M., additional, Chontos, A., additional, Delfosse, X., additional, Dalal, S., additional, Deleuil, M., additional, Demangeon, O. D. S., additional, Díaz, R. F., additional, Dumusque, X., additional, Daylan, T., additional, Dragomir, D., additional, Delgado Mena, E., additional, Dressing, C., additional, Dai, F., additional, Dalba, P. A., additional, Ehrenreich, D., additional, Forveille, T., additional, Fulton, B., additional, Fetherolf, T., additional, Gaisné, G., additional, Giacalone, S., additional, Riazi, N., additional, Hoyer, S., additional, Hobson, M. J., additional, Howard, A. W., additional, Huber, D., additional, Hill, M. L., additional, Hirsch, L. A., additional, Isaacson, H., additional, Jenkins, J., additional, Kane, S. R., additional, Kiefer, F., additional, Luque, R., additional, Latham, D. W., additional, Lubin, J., additional, Lopez, T., additional, Mousis, O., additional, Moutou, C., additional, Montagnier, G., additional, Mignon, L., additional, Mayo, A., additional, Močnik, T., additional, Murphy, J. M. A., additional, Palle, E., additional, Pepe, F., additional, Petigura, E. A., additional, Rey, J., additional, Ricker, G., additional, Robertson, P., additional, Roy, A., additional, Rubenzahl, R. A., additional, Rosenthal, L. J., additional, Santerne, A., additional, Santos, N. C., additional, Sousa, S. G., additional, Stassun, K. G., additional, Stalport, M., additional, Scarsdale, N., additional, Strøm, P. A., additional, Seager, S., additional, Segransan, D., additional, Tenenbaum, P., additional, Tronsgaard, R., additional, Udry, S., additional, Vanderspek, R., additional, Vakili, F., additional, Winn, J., additional, and Weiss, L. M., additional

Published
2022
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21. VizieR Online Data Catalog: HD 158259 SOPHIE radial velocities (Hara+, 2020)

Author

Hara, N. C., Bouchy, F., Stalport, M., Boisse, I., Rodrigues, J., Delisle, J. -B., Santerne, A., Henry, G. W., Arnold, L., Astudillo-Defru, N., Borgniet, S., Bonfils, X., Bourrier, V., Brugger, B., Courcol, B., Dalal, S., Deleuil, M., Delfosse, X., Demangeon, O., Diaz, R. F., Dumusque, X., Forveille, T., Hebrard, G., Hobson, M. J., Kiefer, F., Lopez, T., Mignon, L., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santos, N. C., Segransan, D., Udry, S., Wilson, P. A., Geneva Observatory, Université de Genève = University of Geneva (UNIGE), Observatoire Astronomique de l'Université de Genève (ObsGE), 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), Laboratório Nacional de Energia e Geologia (LNEG), Faculdade de Engenharia da Universidade do Porto (FEUP), Universidade do Porto = University of Porto, Center of Excellence in Information Systems, 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), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, 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 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 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, Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), 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), Centro de Astrofísica da Universidade do Porto (CAUP), Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, and University of Warwick [Coventry]

Subjects
Photometry, Radial velocities, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanets, Stars: G-type, ComputingMilieux_MISCELLANEOUS, Stars: double and multiple
Abstract

International audience

Published
2021

22. XIII. Two planets around M-dwarfs Gl617A and Gl96

Author

Hobson, M. J., Díaz, R. F., Delfosse, X., Astudillo-Defru, N., Boisse, I., Bouchy, F., Bonfils, X., Forveille, T., Hara, N., Arnold, L., Borgniet, S., Bourrier, V., Brugger, B., Cabrera, N., Courcol, B., Dalal, S., Deleuil, M., Demangeon, O., Dumusque, X., Ehrenreich, D., Hébrard, G., Kiefer, F., Lopez, T., Mignon, L., Montagnier, G., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santerne, A., Santos, N., Stalport, M., Ségransan, D., Udry, S., Wilson, P. A., 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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), Institut Pythéas (OSU PYTHEAS), 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), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), 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), 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 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]), Universidad de Concepción - University of Concepcion [Chile], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-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), 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 national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Université de Genève = University of Geneva (UNIGE), Laboratoire de Génie de la Conception (LGeco), Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, University of Warwick [Coventry], 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), Universidad de Concepción [Chile], Universidade do Porto [Porto], 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), 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, 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), and Universidade do Porto

Subjects
[SDU]Sciences of the Universe [physics], stars: late-type, techniques: radial velocities, stars: individual: Gl617A, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], planetary systems, stars: individual: Gl96
Abstract

International audience; Aims. Since 2011, the SOPHIE spectrograph has been used to search for Neptunes and super-Earths in the northern hemisphere. As part of this observational program, 290 radial velocity measurements of the 6.4 V magnitude star HD 158259 were obtained. Additionally, TESS photometric measurements of this target are available. We present an analysis of the SOPHIE data and compare our results with the output of the TESS pipeline.Methods. The radial velocity data, ancillary spectroscopic indices, and ground-based photometric measurements were analyzed with classical and ℓ1 periodograms. The stellar activity was modeled as a correlated Gaussian noise and its impact on the planet detection was measured with a new technique.Results. The SOPHIE data support the detection of five planets, each with m sin i ≈ 6 M⊕, orbiting HD 158259 in 3.4, 5.2, 7.9, 12, and 17.4 days. Though a planetary origin is strongly favored, the 17.4 d signal is classified as a planet candidate due to a slightly lower statistical significance and to its proximity to the expected stellar rotation period. The data also present low frequency variations, most likely originating from a magnetic cycle and instrument systematics. Furthermore, the TESS pipeline reports a significant signal at 2.17 days corresponding to a planet of radius ≈1.2 R⊕. A compatible signal is seen in the radial velocities, which confirms the detection of an additional planet and yields a ≈2 M⊕ mass estimate.Conclusions. We find a system of five planets and a strong candidate near a 3:2 mean motion resonance chain orbiting HD 158259. The planets are found to be outside of the two and three body resonances.

Published
2020
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23. The SOPHIE search for northern extrasolar planets

Author

Hara, N. C., primary, Bouchy, F., additional, Stalport, M., additional, Boisse, I., additional, Rodrigues, J., additional, Delisle, J.-B., additional, Santerne, A., additional, Henry, G. W., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Borgniet, S., additional, Bonfils, X., additional, Bourrier, V., additional, Brugger, B., additional, Courcol, B., additional, Dalal, S., additional, Deleuil, M., additional, Delfosse, X., additional, Demangeon, O., additional, Díaz, R. F., additional, Dumusque, X., additional, Forveille, T., additional, Hébrard, G., additional, Hobson, M. J., additional, Kiefer, F., additional, Lopez, T., additional, Mignon, L., additional, Mousis, O., additional, Moutou, C., additional, Pepe, F., additional, Rey, J., additional, Santos, N. C., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2020
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24. Seven new brown dwarfs and constraints on the brown dwarf desert

Author

Kiefer, F., Hébrard, G., Sahlmann, J., Sousa, S. G., Forveille, T., Santos, N., Mayor, M., Deleuil, M., Wilson, P. A., Dalal, S., Díaz, R. F., Henry, G. W., Hagelberg, J., Hobson, M. J., Demangeon, O., Bourrier, V., Delfosse, X., Arnold, L., Astudillo-Defru, N., Beuzit, J.-L., Boisse, I., Bonfils, X., Borgniet, S., Bouchy, F., Courcol, B., Ehrenreich, D., Hara, N., Lagrange, A.-M., Lovis, C., Montagnier, G., Moutou, C., Pepe, F., Perrier, C., Rey, J., Santerne, A., Ségransan, D., Udry, S., Vidal-Madjar, A., Laboratoire de Génie de la Conception (LGeco), Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), 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 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]), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), 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 d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universidade do Porto = University of Porto, Université de Genève = University of Geneva (UNIGE), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidade de Sao Paulo, Instituto Ocenografico, 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), Universidade do Porto [Porto], University of Warwick [Coventry], Center of Excellence in Information Systems, Université Paris-Sud - Paris 11 (UP11), 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), Universidad de Concepción [Chile], Tri ionique par les Systèmes Moléculaires auto-assemblés (LTSM), Institut de Chimie Séparative de Marcoule (ICSM - UMR 5257), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Université de Montpellier (UM)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Chimie de Montpellier (ENSCM)-Université de Montpellier (UM), 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)-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)

Subjects
[PHYS]Physics [physics], observational -methods, numerical, [SDU]Sciences of the Universe [physics], radial velocities -methods, techniques: radial velocities, brown dwarfs -binaries, methods: observational, spectroscopic -techniques, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], binaries: spectroscopic, methods: numerical, brown dwarfs
Abstract

International audience; Context. Brown dwarfs (BD) are substellar objects intermediate between planets and stars with masses of 13-80 MJ. While isolated BDs are most likely produced by gravitational collapse in molecular clouds down to masses of a few MJ, a non-negligible fraction of low-mass companions might be formed through the planet-formation channel in protoplanetary discs. The upper mass limit of objects formed within discs is still observationally unknown, the main reason being the strong dearth of BD companions at orbital periods shorter than 10 yr, also known as the BD desert. Aims: To address this question, we aim at determining the best statistics of companions within the 10-100 MJ mass regime and located closer than 10 au to the primary star, while minimising observation and selection bias. Methods: We made extensive use of the radial velocity (RV) surveys of northern hemisphere FGK stars within 60 pc of the Sun, performed with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We derived the Keplerian solutions of the RV variations of 54 sources. Public astrometric data of the HIPPARCOS and Gaia missions allowed us to constrain the masses of the companions for most sources. We introduce GASTON, a new method to derive inclination combining RVs and Keplerian and astrometric excess noise from Gaia DR1. Results: We report the discovery of 12 new BD candidates. For five of them, additional astrometric data led to a revision of their mass in the M-dwarf regime. Among the seven remaining objects, four are confirmed BD companions, and three others are likely also in this mass regime. Moreover, we report the detection of 42 M-dwarfs within the range of 90 MJ-0.52 M⊙. The resulting M sin i-P distribution of BD candidates shows a clear drop in the detection rate below 80-day orbital period. Above that limit, the BD desert appears rather wet, with a uniform distribution of the M sin i. We derive a minimum BD-detection frequency around Solar-like stars of 2.0 ± 0.5%. RV data are only available at the CDS and Tables B.1, B.3-B.7 are also available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/631/A125

Published
2019
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25. The SOPHIE search for northern extrasolar planets

Author

Cloutier, R., Berdiñas, Z., Ricker, G., Vanderspek, R., Latham, D., Seager, S., Winn, J., Jenkins, J., Almenara, J., Díaz, M., Doyon, R., Figueira, P., Kurtovic, N., Lovis, C., Mayor, M., Menou, K., Morgan, E., Morris, R., Muirhead, P., Murgas, F., Smith, J., Tenenbaum, P., Torres, G., Vezie, M., Villasenor, J., Hobson, M., Delfosse, X., Astudillo-Defru, N., Boisse, I., Díaz, R., Bouchy, F., Bonfils, Xavier, Forveille, T., Arnold, L., Borgniet, S., Bourrier, V., Brugger, B., Cabrera Salazar, N., Courcol, B., Dalal, S., Deleuil, M., Demangeon, O., Dumusque, X., Hara, N., Hébrard, G., Kiefer, F., Lopez, Téodolina, Mignon, L., Montagnier, G., Mousis, O., Moutou, C., Pepe, F., Rey, J., Santerne, A., Santos, N., Stalport, M., Ségransan, D., Udry, S., Wilson, P., Université du Québec à Rimouski (UQAR), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), 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]), 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), Universidad de Concepción [Chile], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), 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), Institut Pythéas (OSU PYTHEAS), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción - University of Concepcion [Chile], Université de Genève = University of Geneva (UNIGE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; We present the detection of a warm Neptune orbiting the M dwarf Gl 378, using radial velocity measurements obtained with the SOPHIE spectrograph at the Observatoire de Haute-Provence. The star was observed in the context of the SOPHIE exoplanet consortium’s sub-programme dedicated to finding planets around M dwarfs. Gl 378 is an M1 star, of solar metallicity, at a distance of 14.96 pc. The single planet detected, Gl 378 b, has a minimum mass of 13.02 MEarth and an orbital period of 3.82 days, which place it at the lower boundary of the hot Neptune desert. As one of only a few such planets around M dwarfs, Gl 378 b provides important clues to the evolutionary history of these close-in planets. In particular, the eccentricity of 0.1 may point to a high-eccentricity migration. The planet may also have lost part of its envelope due to irradiation.

Published
2019
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26. Detection and characterisation of 54 massive companions with the SOPHIE spectrograph Seven new brown dwarfs and constraints on the brown dwarf desert

Author

Kiefer, Flavien, Hebrard, G., Sahlmann, Johannes, Sousa, Sérgio G., Forveille, Thierry, Santos, Nuno, Mayor, Michel, Deleuil, Magali, Wilson, P.A., Dalal, S., Díaz, R.F., Henry, Gregory W., Hagelberg, Janis, Hobson, M.J., Demangeon, Olivier, Bourrier, V., Delfosse, Xavier, Arnold, Luc, Astudillo-Defru, Nicola, Beuzit, Jean-Luc, Boisse, Isabelle, Bonfils, Xavier, Borgniet, Simon, Bouchy, François, Courcol, B., Ehrenreich, David, Hara, N., Lagrange, Anne-Marie, Lovis, Christophe, Montagnier, Guillaume, Moutou, Claire, Pepe, Francesco, Perrier, C., Rey, J., Santerne, Alexandre, Ségransan, Damien, Udry, Stéphane, and Vidal-Madjar, Alfred

Subjects
spectroscopic, techniques: radial velocities, methods: observational, methods: numerical [brown dwarfs, binaries], binaries: spectroscopic, brown dwarfs, methods: numerical
Abstract

Context. Brown dwarfs (BD) are substellar objects intermediate between planets and stars with masses of ~13–80 MJ. While isolated BDs are most likely produced by gravitational collapse in molecular clouds down to masses of a few MJ, a non-negligible fraction of low-mass companions might be formed through the planet-formation channel in protoplanetary discs. The upper mass limit of objects formed within discs is still observationally unknown, the main reason being the strong dearth of BD companions at orbital periods shorter than 10 yr, also known as the BD desert. Aims. To address this question, we aim at determining the best statistics of companions within the 10–100 MJ mass regime and located closer than ~10 au to the primary star, while minimising observation and selection bias. Methods. We made extensive use of the radial velocity (RV) surveys of northern hemisphere FGK stars within 60 pc of the Sun, performed with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We derived the Keplerian solutions of the RV variations of 54 sources. Public astrometric data of the HIPPARCOS and Gaia missions allowed us to constrain the masses of the companions for most sources. We introduce GASTON, a new method to derive inclination combining RVs and Keplerian and astrometric excess noise from Gaia DR1. Results. We report the discovery of 12 new BD candidates. For five of them, additional astrometric data led to a revision of their mass in the M-dwarf regime. Among the seven remaining objects, four are confirmed BD companions, and three others are likely also in this mass regime. Moreover, we report the detection of 42 M-dwarfs within the range of 90 MJ–0.52 M⊙. The resulting M sin i-P distribution of BD candidates shows a clear drop in the detection rate below 80-day orbital period. Above that limit, the BD desert appears rather wet, with a uniform distribution of the M sin i. We derive a minimum BD-detection frequency around Solar-like stars of 2.0 ± 0.5%., Astronomy & Astrophysics, 631, ISSN:0004-6361, ISSN:1432-0746

Published
2019
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27. The SOPHIE search for northern extrasolar planets

Author

Hobson, M. J., primary, Delfosse, X., additional, Astudillo-Defru, N., additional, Boisse, I., additional, Díaz, R. F., additional, Bouchy, F., additional, Bonfils, X., additional, Forveille, T., additional, Arnold, L., additional, Borgniet, S., additional, Bourrier, V., additional, Brugger, B., additional, Cabrera Salazar, N., additional, Courcol, B., additional, Dalal, S., additional, Deleuil, M., additional, Demangeon, O., additional, Dumusque, X., additional, Hara, N., additional, Hébrard, G., additional, Kiefer, F., additional, Lopez, T., additional, Mignon, L., additional, Montagnier, G., additional, Mousis, O., additional, Moutou, C., additional, Pepe, F., additional, Rey, J., additional, Santerne, A., additional, Santos, N. C., additional, Stalport, M., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2019
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28. SOPHIE velocimetry ofKeplertransit candidates

Author

Hébrard, G., primary, Bonomo, A. S., additional, Díaz, R. F., additional, Santerne, A., additional, Santos, N. C., additional, Almenara, J.-M., additional, Barros, S. C. C., additional, Boisse, I., additional, Bouchy, F., additional, Bruno, G., additional, Courcol, B., additional, Deleuil, M., additional, Demangeon, O., additional, Guillot, T., additional, Montagnier, G., additional, Moutou, C., additional, Rey, J., additional, and Wilson, P. A., additional

Published
2019
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29. The SOPHIE search for northern extrasolar planets

Author

Hobson, M. J., primary, Díaz, R. F., additional, Delfosse, X., additional, Astudillo-Defru, N., additional, Boisse, I., additional, Bouchy, F., additional, Bonfils, X., additional, Forveille, T., additional, Hara, N., additional, Arnold, L., additional, Borgniet, S., additional, Bourrier, V., additional, Brugger, B., additional, Cabrera, N., additional, Courcol, B., additional, Dalal, S., additional, Deleuil, M., additional, Demangeon, O., additional, Dumusque, X., additional, Ehrenreich, D., additional, Hébrard, G., additional, Kiefer, F., additional, Lopez, T., additional, Mignon, L., additional, Montagnier, G., additional, Mousis, O., additional, Moutou, C., additional, Pepe, F., additional, Rey, J., additional, Santerne, A., additional, Santos, N., additional, Stalport, M., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2018
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30. SOPHIE velocimetry of Kepler transit candidates

Author

Almenara, J. M., primary, Díaz, R. F., additional, Hébrard, G., additional, Mardling, R., additional, Damiani, C., additional, Santerne, A., additional, Bouchy, F., additional, Barros, S. C. C., additional, Boisse, I., additional, Bonfils, X., additional, Bonomo, A. S., additional, Courcol, B., additional, Demangeon, O., additional, Deleuil, M., additional, Rey, J., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2018
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31. Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Author

Universitat Politècnica de Catalunya. Departament de Física, Crouzet, N., McCullough, Peter, Long, D., Montañes Rodriguez, Pilar, Lecavelier des Etangs, A, Ribas, Ignasi, Bourrier, V., Hébrard, G., Vilardell, Francesc, Deleuil, M., Herrero, Enrique, García Melendo, Enrique José, Akhenak, L., Foote, Cindy, Gary, B., Benny, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., Demangeon, O, Universitat Politècnica de Catalunya. Departament de Física, Crouzet, N., McCullough, Peter, Long, D., Montañes Rodriguez, Pilar, Lecavelier des Etangs, A, Ribas, Ignasi, Bourrier, V., Hébrard, G., Vilardell, Francesc, Deleuil, M., Herrero, Enrique, García Melendo, Enrique José, Akhenak, L., Foote, Cindy, Gary, B., Benny, P., Guillot, T., Conjat, M., Mékarnia, D., Garlitz, J., Burke, C. J., Courcol, B., and Demangeon, O

Abstract

© 2017. The American Astronomical Society. All rights reserved., Only a few hot Jupiters are known to orbit around fast rotating stars. These exoplanets are harder to detect and characterize and may be less common than around slow rotators. Here, we report the discovery of the transiting hot Jupiter XO-6b, which orbits a bright, hot, and fast rotating star: V = 10.25, T effsstarf = 6720 ± 100 K, v sin i sstarf = 48 ± 3 km s-1. We detected the planet from its transits using the XO instruments and conducted a follow-up campaign. Because of the fast stellar rotation, radial velocities taken along the orbit do not yield the planet's mass with a high confidence level, but we secure a 3s upper limit M p < 4.4 M Jup. We also obtain high-resolution spectroscopic observations of the transit with the SOPHIE spectrograph at the 193-cm telescope of the Observatoire de Haute-Provence and analyze the stellar lines profile by Doppler tomography. The transit is clearly detected in the spectra. The radii measured independently from the tomographic analysis and from the photometric light curves are consistent, showing that the object detected by both methods is the same and indeed transits in front of XO-6. We find that XO-6b lies on a prograde and misaligned orbit with a sky-projected obliquity ${\boldsymbol{\lambda }}=-20\buildrel{\circ}\over{.} 7\pm 2\buildrel{\circ}\over{.} 3$. The rotation period of the star is shorter than the orbital period of the planet: P rot < 2.12 days, P orb = 3.77 days. Thus, this system stands in a largely unexplored regime of dynamical interactions between close-in giant planets and their host stars., Peer Reviewed, Postprint (published version)

Published
2017

32. EPIC211089792 b: an aligned and inflated hot jupiter in a young visual binary

Author

Alexandre Santerne, Hébrard, G., Lillo-Box, J., Armstrong, D. J., Barros, S. C. C., Demangeon, O., Barrado, D., Debackere, A., Deleuil, M., Delgado Mena, E., Montalto, M., Pollacco, D., Osborn, H. P., Sousa, S. G., Abe, L., Adibekyan, V., Almenara, J. -M, André, P., Arlic, G., Barthe, G., Bendjoya, P., Behrend, R., Boisse, I., Bouchy, F., Boussier, H., Bretton, M., Brown, D. J. A., Carry, B., Cailleau, A., Conseil, E., Courcol, B., Dauchet, B., Dalouzy, J. -C, Deldem, M., Dubreuil, P., Fehrenbach, J. -M, Ferratfiat, S., Girelli, R., Gregorio, J., Jaecques, S., Kugel, F., Kirk, J., Labrevoir, O., Lachurié, J. -C, Lam, K. W. F., Le Guen, P., Martinez, P., Maurin, L., Mccormac, J., Pioppa, J-B, Quadri, U., Rajpurohit, A., Rey, J., Rivet, J. -P, Roy, R., Santos, N. C., Signoret, F., Strabla, L., Suarez, O., Toublanc, D., Tsantaki, M., Wilson, P. A., Bachschmidt, M., Colas, F., Gerteis, O., Louis, P., Mario, J. -C, Marlot, C., Montier, J., Perroud, V., Pic, V., Romeuf, D., Ubaud, S., and Verilhac, D.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

In the present paper we report the discovery of a new hot Jupiter, EPIC211089792 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25d, a mass of 0.73 +/- 0.04 Mjup, and a radius of 1.19 +/- 0.02 Rjup. The host star is a relatively bright (V=12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of Lithium, we find that the system might be as young as about 450 Myr. The observation of the Rossiter-McLaughlin effect shows the planet is aligned with respect to the stellar spin. Given the deep transit (20mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where the both stars are relatively bright., Submitted to ApJ

Published
2016

33. The SOPHIE search for northern extrasolar planets

Author

Rey, J., primary, Hébrard, G., additional, Bouchy, F., additional, Bourrier, V., additional, Boisse, I., additional, Santos, N. C., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Bonfils, X., additional, Borgniet, S., additional, Courcol, B., additional, Deleuil, M., additional, Delfosse, X., additional, Demangeon, O., additional, Díaz, R. F., additional, Ehrenreich, D., additional, Forveille, T., additional, Marmier, M., additional, Moutou, C., additional, Pepe, F., additional, Santerne, A., additional, Sahlmann, J., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2017
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34. Discovery of XO-6b: A Hot Jupiter Transiting a Fast Rotating F5 Star on an Oblique Orbit

Author

Crouzet, N., primary, McCullough, P. R., additional, Long, D., additional, Rodriguez, P. Montanes, additional, Etangs, A. Lecavelier des, additional, Ribas, I., additional, Bourrier, V., additional, Hébrard, G., additional, Vilardell, F., additional, Deleuil, M., additional, Herrero, E., additional, Garcia-Melendo, E., additional, Akhenak, L., additional, Foote, J., additional, Gary, B., additional, Benni, P., additional, Guillot, T., additional, Conjat, M., additional, Mékarnia, D., additional, Garlitz, J., additional, Burke, C. J., additional, Courcol, B., additional, and Demangeon, O., additional

Published
2017
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35. SOPHIE velocimetry of Kepler transit candidates: XIX. The transiting temperate giant planet KOI-3680b.

Author

Hébrard, G., Bonomo, A. S., Díaz, R. F., Santerne, A., Santos, N. C., Almenara, J.-M., Barros, S. C. C., Boisse, I., Bouchy, F., Bruno, G., Courcol, B., Deleuil, M., Demangeon, O., Guillot, T., Montagnier, G., Moutou, C., Rey, J., and Wilson, P. A.

Subjects
ASTRONOMICAL transits, PLANETARY systems, VELOCIMETRY, SPECTROGRAPHS, GAS giants
Abstract

Whereas thousands of transiting giant exoplanets are known today, only a few are well characterized with long orbital periods. Here we present KOI-3680b, a new planet in this category. First identified by the Kepler team as a promising candidate from the photometry of the Kepler spacecraft, we establish here its planetary nature from the radial velocity follow-up secured over 2 yr with the SOPHIE spectrograph at Observatoire de Haute-Provence, France. The combined analysis of the whole dataset allows us to fully characterize this new planetary system. KOI-3680b has an orbital period of 141.2417 ± 0.0001 days, a mass of 1.93 ± 0.20 MJup, and a radius of 0.99 ± 0.07 RJup. It exhibits a highly eccentric orbit (e = 0.50 ± 0.03) around an early G dwarf. KOI-3680b is the transiting giant planet with the longest period characterized so far around a single star; it offers opportunities to extend studies which were mainly devoted to exoplanets close to their host stars, and to compare both exoplanet populations. [ABSTRACT FROM AUTHOR]

Published
2019
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36. K2-30 b and K2-34 b: Two inflated hot Jupiters around solar-type stars

Author

Lillo-Box, J., primary, Demangeon, O., additional, Santerne, A., additional, Barros, S. C. C., additional, Barrado, D., additional, Hébrard, G., additional, Osborn, H. P., additional, Armstrong, D. J., additional, Almenara, J.-M., additional, Boisse, I., additional, Bouchy, F., additional, Brown, D. J. A., additional, Courcol, B., additional, Deleuil, M., additional, Delgado Mena, E., additional, Díaz, R. F., additional, Kirk, J., additional, Lam, K. W. F., additional, McCormac, J., additional, Pollacco, D., additional, Rajpurohit, A., additional, Rey, J., additional, Santos, N. C., additional, Sousa, S. G., additional, Tsantaki, M., additional, and Wilson, P. A., additional

Published
2016
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37. The SOPHIE search for northern extrasolar planets

Author

Díaz, R. F., primary, Rey, J., additional, Demangeon, O., additional, Hébrard, G., additional, Boisse, I., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Beuzit, J.-L., additional, Bonfils, X., additional, Borgniet, S., additional, Bouchy, F., additional, Bourrier, V., additional, Courcol, B., additional, Deleuil, M., additional, Delfosse, X., additional, Ehrenreich, D., additional, Forveille, T., additional, Lagrange, A.-M., additional, Mayor, M., additional, Moutou, C., additional, Pepe, F., additional, Queloz, D., additional, Santerne, A., additional, Santos, N. C., additional, Sahlmann, J., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2016
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38. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author

Santerne, A., primary, Hébrard, G., additional, Lillo-Box, J., additional, Armstrong, D. J., additional, Barros, S. C. C., additional, Demangeon, O., additional, Barrado, D., additional, Debackere, A., additional, Deleuil, M., additional, Mena, E. Delgado, additional, Montalto, M., additional, Pollacco, D., additional, Osborn, H. P., additional, Sousa, S. G., additional, Abe, L., additional, Adibekyan, V., additional, Almenara, J.-M., additional, André, P., additional, Arlic, G., additional, Barthe, G., additional, Bendjoya, P., additional, Behrend, R., additional, Boisse, I., additional, Bouchy, F., additional, Boussier, H., additional, Bretton, M., additional, Brown, D. J. A., additional, Carry, B., additional, Cailleau, A., additional, Conseil, E., additional, Coulon, G., additional, Courcol, B., additional, Dauchet, B., additional, Dalouzy, J.-C., additional, Deldem, M., additional, Desormières, O., additional, Dubreuil, P., additional, Fehrenbach, J.-M., additional, Ferratfiat, S., additional, Girelli, R., additional, Gregorio, J., additional, Jaecques, S., additional, Kugel, F., additional, Kirk, J., additional, Labrevoir, O., additional, Lachurié, J.-C., additional, Lam, K. W. F., additional, Guen, P. Le, additional, Martinez, P., additional, Maurin, L. P. A., additional, McCormac, J., additional, Pioppa, J-B., additional, Quadri, U., additional, Rajpurohit, A., additional, Rey, J., additional, Rivet, J.-P., additional, Roy, R., additional, Santos, N. C., additional, Signoret, F., additional, Strabla, L., additional, Suarez, O., additional, Toublanc, D., additional, Tsantaki, M., additional, Vienney, J.-M., additional, Wilson, P. A., additional, Bachschmidt, M., additional, Colas, F., additional, Gerteis, O., additional, Louis, P., additional, Mario, J.-C., additional, Marlot, C., additional, Montier, J., additional, Perroud, V., additional, Pic, V., additional, Romeuf, D., additional, Ubaud, S., additional, and Verilhac, D., additional

Published
2016
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39. The SOPHIE search for northern extrasolar planets

Author

Hébrard, G., primary, Arnold, L., additional, Forveille, T., additional, Correia, A. C. M., additional, Laskar, J., additional, Bonfils, X., additional, Boisse, I., additional, Díaz, R. F., additional, Hagelberg, J., additional, Sahlmann, J., additional, Santos, N. C., additional, Astudillo-Defru, N., additional, Borgniet, S., additional, Bouchy, F., additional, Bourrier, V., additional, Courcol, B., additional, Delfosse, X., additional, Deleuil, M., additional, Demangeon, O., additional, Ehrenreich, D., additional, Gregorio, J., additional, Jovanovic, N., additional, Labrevoir, O., additional, Lagrange, A.-M., additional, Lovis, C., additional, Lozi, J., additional, Moutou, C., additional, Montagnier, G., additional, Pepe, F., additional, Rey, J., additional, Santerne, A., additional, Ségransan, D., additional, Udry, S., additional, Vanhuysse, M., additional, Vigan, A., additional, and Wilson, P. A., additional

Published
2016
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40. The SOPHIE search for northern extrasolar planets

Author

Wilson, P. A., primary, Hébrard, G., additional, Santos, N. C., additional, Sahlmann, J., additional, Montagnier, G., additional, Astudillo-Defru, N., additional, Boisse, I., additional, Bouchy, F., additional, Rey, J., additional, Arnold, L., additional, Bonfils, X., additional, Bourrier, V., additional, Courcol, B., additional, Deleuil, M., additional, Delfosse, X., additional, Díaz,, R. F., additional, Ehrenreich, D., additional, Forveille, T., additional, Moutou, C., additional, Pepe, F., additional, Santerne, A., additional, Ségransan, D., additional, and Udry, S., additional

Published
2016
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41. SOPHIE velocimetry ofKeplertransit candidates

Author

Santerne, A., primary, Moutou, C., additional, Tsantaki, M., additional, Bouchy, F., additional, Hébrard, G., additional, Adibekyan, V., additional, Almenara, J.-M., additional, Amard, L., additional, Barros, S. C. C., additional, Boisse, I., additional, Bonomo, A. S., additional, Bruno, G., additional, Courcol, B., additional, Deleuil, M., additional, Demangeon, O., additional, Díaz, R. F., additional, Guillot, T., additional, Havel, M., additional, Montagnier, G., additional, Rajpurohit, A. S., additional, Rey, J., additional, and Santos, N. C., additional

Published
2016
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42. The SOPHIE search for northern extrasolar planets

Author

Bouchy, F., primary, Ségransan, D., additional, Díaz, R. F., additional, Forveille, T., additional, Boisse, I., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Beuzit, J.-L., additional, Bonfils, X., additional, Borgniet, S., additional, Bourrier, V., additional, Courcol, B., additional, Delfosse, X., additional, Demangeon, O., additional, Delorme, P., additional, Ehrenreich, D., additional, Hébrard, G., additional, Lagrange, A.-M., additional, Mayor, M., additional, Montagnier, G., additional, Moutou, C., additional, Naef, D., additional, Pepe, F., additional, Perrier, C., additional, Queloz, D., additional, Rey, J., additional, Sahlmann, J., additional, Santerne, A., additional, Santos, N. C., additional, Sivan, J.-P., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2015
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43. Photodynamical mass determination of the multiplanetary system K2-19

Author

Barros, S. C. C., primary, Almenara, J. M., additional, Demangeon, O., additional, Tsantaki, M., additional, Santerne, A., additional, Armstrong, D. J., additional, Barrado, D., additional, Brown, D., additional, Deleuil, M., additional, Lillo-Box, J., additional, Osborn, H., additional, Pollacco, D., additional, Abe, L., additional, Andre, P., additional, Bendjoya, P., additional, Boisse, I., additional, Bonomo, A. S., additional, Bouchy, F., additional, Bruno, G., additional, Cerda, J. Rey, additional, Courcol, B., additional, Díaz, R. F., additional, Hébrard, G., additional, Kirk, J., additional, Lachurié, J. C., additional, Lam, K. W. F., additional, Martinez, P., additional, McCormac, J., additional, Moutou, C., additional, Rajpurohit, A., additional, Rivet, J.-P., additional, Spake, J., additional, Suarez, O., additional, Toublanc, D., additional, and Walker, S. R., additional

Published
2015
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44. The SOPHIE search for northern extrasolar planets

Author

Courcol, B., primary, Bouchy, F., additional, Pepe, F., additional, Santerne, A., additional, Delfosse, X., additional, Arnold, L., additional, Astudillo-Defru, N., additional, Boisse, I., additional, Bonfils, X., additional, Borgniet, S., additional, Bourrier, V., additional, Cabrera, N., additional, Deleuil, M., additional, Demangeon, O., additional, Díaz, R. F., additional, Ehrenreich, D., additional, Forveille, T., additional, Hébrard, G., additional, Lagrange, A. M., additional, Montagnier, G., additional, Moutou, C., additional, Rey, J., additional, Santos, N. C., additional, Ségransan, D., additional, Udry, S., additional, and Wilson, P. A., additional

Published
2015
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45. K2-19, The first K2 muti-planetary system showing TTVs

Author

Barros, S. C. C., primary, Almenara, J. M., additional, Demangeon, O., additional, Tsantaki, M., additional, Santerne, A., additional, Armstrong, D. J., additional, Barrado, D., additional, Brown, D., additional, Deleuil, M., additional, Lillo-Box, J., additional, Osborn, H., additional, Pollacco, D., additional, Abe, L., additional, Andre, P., additional, Bendjoya, P., additional, Boisse, I., additional, Bonomo, A. S., additional, Bouchy, F., additional, Bruno, G., additional, Cerda, J. Rey, additional, Courcol, B., additional, Díaz, R. F., additional, Hébrard, G., additional, Kirk, J., additional, Lachurié, J. C., additional, Lam, K. W. F., additional, Martinez, P., additional, McCormac, J., additional, Moutou, C., additional, Rajpurohit, A., additional, Rivet, J.-P., additional, Spake, J., additional, Suarez, O., additional, Toublanc, D., additional, and Walker, S. R., additional

Published
2015
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46. SOPHIE velocimetry ofKeplertransit candidates

Author

Bourrier, V., primary, Lecavelier des Etangs, A., additional, Hébrard, G., additional, Santerne, A., additional, Deleuil, M., additional, Almenara, J. M., additional, Barros, S. C. C., additional, Boisse, I., additional, Bonomo, A. S., additional, Bruno, G., additional, Courcol, B., additional, Diaz, R. F., additional, Montagnier, G., additional, and Moutou, C., additional

Published
2015
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47. VizieR Online Data Catalog: Extrasolar planets. Radial velocities of 5 stars (Bouchy+, 2016)

Author

Bouchy, F., Segransan, D., Diaz, R. F., Forveille, T., Boisse, I., Arnold, L., Astudillo-Defru, N., Beuzit, J. -L, Bonfils, X., Borgniet, S., Bourrier, V., Courcol, B., Delfosse, X., Olivier Demangeon, Delorme, P., Ehrenreich, D., Hebrard, G., Lagrange, A. -M, Mayor, M., Montagnier, G., Moutou, C., Naef, D., Pepe, F., Perrier, C., Queloz, D., Rey, J., Sahlmann, J., Santerne, A., Santos, N. C., Sivan, J. -P, Udry, S., and Wilson, P. A.

48. VizieR Online Data Catalog: K2-30 b and K2-34 b K2 light curves (Lillo-Box+, 2016)

Author

Lillo-Box, J., Demangeon, O., Santerne, A., Susana Barros, Barrado, D., Hebrard, G., Osborn, H. P., Armstrong, D. J., Almenara, J. -M, Boisse, I., Bouchy, F., Brown, D. J. A., Courcol, B., Deleuil, M., Delgado Mena, E., Diaz, R. F., Kirk, J., Lam, K. W. F., Mccormac, J., Pollacco, D., Rajpurohit, A., Rey, J., Santos, N. C., Sousa, S. G., Tsantaki, M., and Wilson, P. A.

49. VizieR Online Data Catalog: HD17674, HD29021, and HD42012 radial velocities (Rey+, 2017)

Author

Rey, J., Hebrard, G., Bouchy, F., Bourrier, V., Boisse, I., Santos, N. C., Arnold, L., Astudillo-Defru, N., Bonfils, X., Borgniet, S., Courcol, B., Deleuil, M., Delfosse, X., Olivier Demangeon, Diaz, R. F., Ehrenreich, D., Forveille, T., Marmier, M., Moutou, C., Pepe, F., Santerne, A., Sahlmann, J., Segransan, D., Udry, S., and Wilson, P. A.

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