Showing papers by "François Bouchy published in 2013"
TL;DR: In this paper, the radial velocities of GJ 163 (HIP 19394), a M3 dwarf monitored by the ESO/HARPS search for planets, were collected over a period of eight years.
Abstract: The meter-per-second precision achieved by today’s velocimeters enables us to search for 1−10 M ⊕ planets in the habitable zone of cool stars. This paper reports on the detection of three planets orbiting GJ 163 (HIP 19394), a M3 dwarf monitored by our ESO/HARPS search for planets. We made use of the HARPS spectrograph to collect 150 radial velocities of GJ 163 over a period of eight years. We searched the radial-velocity time series for coherent signals and found five distinct periodic variabilities. We investigated the stellar activity and called into question the planetary interpretation for two signals. Before more data can be acquired we concluded that at least three planets are orbiting GJ 163. They have orbital periods of P b = 8.632 ± 0.002, P c = 25.63 ± 0.03, and P d = 604 ± 8 days and minimum masses m sini = 10.6 ± 0.6, 6.8 ± 0.9, and 29 ± 3 M ⊕ , respectively. We hold our interpretations for the two additional signals with periods P (e ) = 19.4 and P (f ) = 108 days. The inner pair presents an orbital period ratio of 2.97, but a dynamical analysis of the system shows that it lays outside the 3:1 mean motion resonance. The planet GJ 163c, in particular, is a super-Earth with an equilibrium temperature of T eq = (302 ± 10)(1 − A )1/4 K and may lie in the so-called habitable zone for albedo values (A = 0.34 − 0.89) moderately higher than that of Earth (A ⊕ = 0.2−0.3).
96 citations
TL;DR: The CoRoT-7b is the first known transiting rocky planet, and it was discovered by the CoRoTs-2 satellite as discussed by the authors, which has acquired more than 163,000 light curves and detected about 500 planet candidates.
91 citations
TL;DR: In this paper, the authors reported three new transiting hot-Jupiter planets discovered from the WASP surveys combined with radial velocities from OHP/SOPHIE and Euler/CORALIE and photometry from Euler and TRAPPIST.
Abstract: We report three new transiting hot-Jupiter planets discovered from the WASP surveys combined with radial velocities from OHP/SOPHIE and Euler/CORALIE and photometry from Euler and TRAPPIST. All three planets are inflated, with radii 1.7-1.8 Rjup. All orbit hot stars, F5-F7, and all three stars have evolved, post-MS radii (1.7-2.2 Rsun). Thus the three planets, with orbits of 1.8-3.9 d, are among the most irradiated planets known. This reinforces the correlation between inflated planets and stellar irradiation.
75 citations
TL;DR: In this paper, the authors used the HARPS spectrograph to collect 150 radial velocities of GJ163 over a period of 8 years and concluded that at least 3 planets are orbiting GJ 163, with orbital periods of P_b=8.6, 6.8+-0.002, P_c=25.63+- 0.03 and P_d=604+-8 days.
Abstract: The meter-per-second precision achieved by today velocimeters enables the search for 1-10 M_Earth planets in the habitable zone of cool stars. This paper reports on the detection of 3 planets orbiting GJ163 (HIP19394), a M3 dwarf monitored by our ESO/HARPS search for planets. We made use of the HARPS spectrograph to collect 150 radial velocities of GJ163 over a period of 8 years. We searched the RV time series for coherent signals and found 5 distinct periodic variabilities. We investigated the stellar activity and casted doubts on the planetary interpretation for 2 signals. Before more data can be acquired we concluded that at least 3 planets are orbiting GJ163. They have orbital periods of P_b=8.632+-0.002, P_c=25.63+-0.03 and P_d=604+-8 days and minimum masses msini = 10.6+-0.6, 6.8+-0.9, and 29+-3 M_Earth, respectively. We hold our interpretations for the 2 additional signals with periods P_(e)=19.4 and P_(f)=108 days. The inner pair presents an orbital period ratio of 2.97, but a dynamical analysis of the system shows that it lays outside the 3:1 mean motion resonance. GJ163c, in particular, is a super-Earth with an equilibrium temperature of T_eq = (302+-10) (1-A)^(1/4) K and may lie in the so called habitable zone for albedo values (A=0.34-0.89) moderately higher than that of Earth (A_Earth=0.2-0.3).
63 citations
Posted Content•
TL;DR: In this paper, the authors outline the science case for a high-fidelity, high-resolution spectrograph with wide wavelength coverage at the E-ELT Flagship science drivers include: the study of exoplanetary atmospheres with the prospect of the detection of signatures of life on rocky planets; the chemical composition of planetary debris on the surface of white dwarfs; the spectroscopic study of protoplanetary and proto-stellar disks; the extension of Galactic archaeology to the Local Group and beyond; spectroscopy studies of the evolution of galaxies with samples that
Abstract: Building on the experience of the high-resolution community with the suite of VLT high-resolution spectrographs, which has been tremendously successful, we outline here the (science) case for a high-fidelity, high-resolution spectrograph with wide wavelength coverage at the E-ELT Flagship science drivers include: the study of exo-planetary atmospheres with the prospect of the detection of signatures of life on rocky planets; the chemical composition of planetary debris on the surface of white dwarfs; the spectroscopic study of protoplanetary and proto-stellar disks; the extension of Galactic archaeology to the Local Group and beyond; spectroscopic studies of the evolution of galaxies with samples that, unlike now, are no longer restricted to strongly star forming and/or very massive galaxies; the unraveling of the complex roles of stellar and AGN feedback; the study of the chemical signatures imprinted by population III stars on the IGM during the epoch of reionization; the exciting possibility of paradigm-changing contributions to fundamental physics The requirements of these science cases can be met by a stable instrument with a spectral resolution of R~100,000 and broad, simultaneous spectral coverage extending from 370nm to 2500nm Most science cases do not require spatially resolved information, and can be pursued in seeing-limited mode, although some of them would benefit by the E-ELT diffraction limited resolution Some multiplexing would also be beneficial for some of the science cases (Abridged)
59 citations
TL;DR: In this article, the authors presented the detection and characterization of two new transiting, close-in, giant extrasolar planets KOI200 b and KOI-889 b, which were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite, then established their planetary nature thanks to the radial velocity followup jointly secured with the spectrographs SOPHIE and HARPS-N.
Abstract: We present the detection and characterization of the two new transiting, close-in, giant extrasolar planets KOI-200 b and KOI-889 b. They were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite, then we established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N. Combined analyses of the whole datasets allow the two planetary systems to be characterized. The planet KOI-200 b has mass and radius of 0.68 +/- 0.09 M-Jup and 1.32 +/- 0.14 R-Jup; it orbits in 7.34 days a F8V host star with mass and radius of 1.40(-0.11)(+0.14) M-circle dot and 1.51 +/- 0.14 R-circle dot. The planet KOI-889 b is a massive planet with mass and radius of 9.9 +/- 0.5 M-Jup and 1.03 +/- 0.06 R-Jup; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 +/- 0.3 days, and mass and radius of 0.88 +/- 0.06 M-circle dot and 0.88 +/- 0.04 R-circle dot. Both planets lie on eccentric orbits and are located just at the frontier between regimes where the tides can explain circularization and where tidal effects are negligible. The two planets are among the first ones detected and characterized thanks to observations secured with HARPS-N, the new spectrograph recently mounted at the Telescopio Nazionale Galileo. These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N.
50 citations
Posted Content•
TL;DR: In this paper, the HARPS spectrograph was used to conduct a survey of ~850 nearby solar-type stars, and in the course of the past nine years, they have monitored the radial velocity of HD103774, HD109271, and BD-061339.
Abstract: The vast diversity of planetary systems detected to date is defying our capability of understanding their formation and evolution. Well-defined volume-limited surveys are the best tool at our disposal to tackle the problem, via the acquisition of robust statistics of the orbital elements. We are using the HARPS spectrograph to conduct our survey of ~850 nearby solar-type stars, and in the course of the past nine years we have monitored the radial velocity of HD103774, HD109271, and BD-061339. In this work we present the detection of five planets orbiting these stars, with m*sin(i) between 0.6 and 7 Neptune masses, four of which are in two multiple systems, comprising one super-Earth and one planet within the habitable zone of a late-type dwarf. Although for strategic reasons we chose efficiency over precision in this survey, we have the capability to detect planets down to the Neptune and super-Earth mass range, as well as multiple systems, provided that enough data points are made available.
48 citations
TL;DR: In this article, the authors presented the detection and characterization of two new transiting, close-in, giant extrasolar planets KOI200b and KOI-889b, which were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite, then established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N.
Abstract: We present the detection and characterization of the two new transiting, close-in, giant extrasolar planets KOI-200b and KOI-889b. They were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite, then we established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N. Combined analyses of the whole datasets allow the two planetary systems to be characterized. The planet KOI-200b has mass and radius of 0.68 +/- 0.09 M_Jup and 1.32 +/- 0.14 R_Jup; it orbits in 7.34 days a F8V host star with mass and radius of 1.40 (+0.14/-0.11) M_Sun and 1.51 +/- 0.14 R_Sun. KOI-889b is a massive planet with mass and radius of 9.9 +/- 0.5 M_Jup and 1.03 +/- 0.06 R_Jup; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 +/- 0.3 days, and mass and radius of 0.88 +/- 0.06 M_Sun and 0.88 +/- 0.04 R_Sun. Both planets lie on eccentric orbits and are located just at the frontier between regimes where the tides can explain circularization and where tidal effects are negligible. The two planets are among the first ones detected and characterized thanks to observations secured with HARPS-N, the new spectrograph recently mounted at the Telescopio Nazionale Galileo. These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N.
46 citations
TL;DR: The first radial velocity confirmation of a non-transiting planet discovered with transit timing variations was reported in this article, with an orbital period of $22.10 \pm 0.25\,$ days.
Abstract: The exoplanet KOI-142b (Kepler-88b) shows transit timing variations (TTVs) with a semi-amplitude of $\sim 12\,$ hours, earning the nickname of "king of transit variations". Only the transit of the planet b was detected in the Kepler data with an orbital period of $\sim 10.92\,$ days and a radius of $\sim 0.36$ R$_{\mathrm{Jup}}$. The TTVs together with the transit duration variations (TDVs) of KOI-142b were analysed by Nesvorny et al. (2013) who found a unique solution for a companion perturbing planet. The authors predicted an outer non-transiting companion, KOI-142c, with a mass of $0.626\pm 0.03$ M$_{\mathrm{Jup}}$ and a period of $22.3397^{+0.0021}_{-0.0018}\,$days, and hence close to the 2:1 mean-motion resonance with the inner transiting planet. We report independent confirmation of KOI-142c using radial velocity observations with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We derive an orbital period of $22.10 \pm 0.25\,$days and a minimum planetary mass of $0.76^{+0.32}_{0.16}\,$ M$_{\mathrm{Jup}}$, both in good agreement with the predictions by previous transit timing analysis. Therefore, this is the first radial velocity confirmation of a non-transiting planet discovered with transit timing variations, providing an independent validation of the TTVs technique.
37 citations
Tel Aviv University1, University of Geneva2, Spanish National Research Council3, University of La Laguna4, Institut d'Astrophysique de Paris5, Centre national de la recherche scientifique6, German Aerospace Center7, Aix-Marseille University8, European Space Research and Technology Centre9, Leiden University10
TL;DR: In this paper, the authors present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1\₄780, also referred to as LRc1_E 1/1/780, which is the smallest and densest late M-dwarf reported so far.
Abstract: We present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1\₄780. Analysis of the CoRoT lightcurve and the HARPS spectroscopic follow-up observations of this faint (m(V) = 16) candidate revealed an eclipsing binary composed of a late F-type primary (T-eff = 6090 +/- 200 K) and a low-mass, dense late M-dwarf secondary on an eccentric (e = 0.4) orbit with a period of similar to 20.7 days. The M-dwarf has a mass of 0.096 +/- 0.011 M-circle dot, and a radius of 0.104(-0.006)(+0.026) R-circle dot, which possibly makes it the smallest and densest late M-dwarf reported so far. Unlike the claim that theoretical models predict radii that are 5-15% smaller than measured for low-mass stars, this one seems to have a radius that is consistent and might even be below the radius predicted by theoretical models.
36 citations
TL;DR: In this paper, the authors present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1_4780, which is composed of a late F-type primary and a low-mass, dense late M-dwarf secondary on an eccentric (e = 0.4) orbit with a period of ~20.7 days.
Abstract: We present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1_4780. Analysis of the CoRoT lightcurve and the HARPS spectroscopic follow-up observations of this faint (m_V = 16) candidate revealed an eclipsing binary composed of a late F-type primary (T_eff = 6090 +/- 200 K) and a low-mass, dense late M-dwarf secondary on an eccentric (e = 0.4) orbit with a period of ~20.7 days. The M-dwarf has a mass of 0.096 +/- 0.011 M_Sun, and a radius of 0.104 +0.026/-0.006 R_Sun, which possibly makes it the smallest and densest late M-dwarf reported so far. Unlike the claim that theoretical models predict radii that are 5%-15% smaller than measured for low-mass stars, this one seems to have a radius that is consistent and might even be below the radius predicted by theoretical models.
TL;DR: In this article, a giant planet was detected around the young F-type star HD113337 in the frame of the search for extrasolar planets and brown dwarfs around early-type main-sequence stars.
Abstract: In the frame of the search for extrasolar planets and brown dwarfs around early-type main-sequence stars, we present the detection of a giant planet around the young F-type star HD113337. We estimated the age of the system to be 150 +100/-50 Myr. Interestingly, an IR excess attributed to a cold debris disk was previously detected on this star. The SOPHIE spectrograph on the 1.93m telescope at Observatoire de Haute-Provence was used to obtain ~300 spectra over 6 years. We used our SAFIR tool, dedicated to the spectra analysis of A and F stars, to derive the radial velocity variations. The data reveal a 324.0 +1.7/-3.3 days period that we attribute to a giant planet with a minimum mass of 2.83 +- 0.24 Mjup in an eccentric orbit with e=0.46 +- 0.04. A long-term quadratic drift, that we assign to be probably of stellar origin, is superimposed to the Keplerian solution.
Aix-Marseille University1, Institut d'Astrophysique de Paris2, New Mexico State University3, Ames Research Center4, European Space Research and Technology Centre5, Spanish National Research Council6, German Aerospace Center7, Janssen Pharmaceutica8, University of Paris-Sud9, University of Texas at Austin10, University of Vienna11, University of São Paulo12, University of Liège13, Austrian Academy of Sciences14, Tel Aviv University15, University of Göttingen16, University of Cologne17, University of Geneva18, Paris Diderot University19
TL;DR: In this article, the authors reported the discovery of two transiting exoplanets, CoRoT-25b and CoRoTs26b, both of which are in the Saturn mass-regime.
Abstract: We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 M Jup , a radius of 1.08-0.10 +0.3 R Jup and hence a mean density of 0.15-0.06 +0.15 g cm-3 . The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0 +1.8 -Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 M Jup , a radius of 1.26-0.07 +0.13 R Jup , and a mean density of 0.28-0.07 +0.09 g cm-3 , it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52-0.15 +0.08 and 0.26-0.08 +0.05 , respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.
Posted Content•
TL;DR: SPIRou, a near infrared spectropolarimeter, is a project of new instrument to be mounted at the Canada France Hawaii Telescope in 2017, with the main objectives of SPIRou is to reach a radial velocity accuracy better than 1 m/s in the YJHK bands as mentioned in this paper.
Abstract: SPIRou, a near infrared spectropolarimeter, is a project of new instrument to be mounted at the Canada France Hawaii Telescope in 2017. One of the main objectives of SPIRou is to reach a radial velocity accuracy better than 1 m/s in the YJHK bands. SPIRou will make a cornerstone into the characterization of Earth-like planets, where the exoplanet statistics is very low. This is even more true for planets transiting M dwarfs, since only 3 low-mass planets have been secured so far to transit such stars. We present here all the synergies that SPIRou will provide to and benefit from photometric transit-search programs from the ground or from space (Kepler, CHEOPS, TESS, PLATO 2.0). We also discuss the impact of SPIRou for the characterization of planets orbiting actives stars.
01 Nov 2013
TL;DR: SPIRou, a near infrared spectropolarimeter, is a project of new instrument to be mounted at the Canada France Hawaii Telescope in 2017, with the main objectives of SPIRou is to reach a radial velocity accuracy better than 1 m.s−1 in the YJHK bands.
Abstract: SPIRou, a near infrared spectropolarimeter, is a project of new instrument to be mounted at the Canada France Hawaii Telescope in 2017. One of the main objectives of SPIRou is to reach a radial velocity accuracy better than 1 m.s−1 in the YJHK bands. SPIRou will make a cornerstone into the characterization of Earth-like planets, where the exoplanet statistics is very low. This is even more true for planets transiting M dwarfs, since only 3 low-mass planets have been secured so far to transit such stars. We present here all the synergies that SPIRou will provide to and benefit from photometric transit-search programs from the ground or from space (Kepler, CHEOPS, TESS, PLATO 2.0 ). We also discuss the impact of SPIRou for the characterization of planets orbiting actives stars.
01 Jan 2013
TL;DR: The HARPS system has been used for almost a decade and has detected most of the known low-mass planets orbiting M dwarfs (m sin i < 20M⊕), including the least massive (GJ581e, msini = 1.9M) and the first potentially habitable planets (gJ581c&d GJ667Cc, GJ163c) as mentioned in this paper.
Abstract: Searching for planets around stars with different masses probes the outcome of planetary formation for different initial conditions. The low-mass M dwarfs are also the most frequent stars in our Galaxy and potentially therefore, the most frequent planet hosts. This has motivated our search for planets around M dwarfs with HARPS. That observing program has now run for almost a decade and detected most of the known low-mass planets orbiting M dwarfs (m sin i < 20M⊕), including the least massive (GJ581e, msini = 1.9M⊕) and the first potentially habitable planets (GJ581c&d GJ667Cc, GJ163c). This proceeding shortly reviews the detections made with HARPS, reports on the occurrence of planets around M dwarfs and how they mesh up with planet formation theory. It also highlights our sensitivity to low-mass habitable planets, the first direct measure of ⊕, and the recent detection of a transiting planet the size of Uranus.