The HARPS search for southern extra-solar planets

Correia, A. C. M.; Couetdic, J.; Laskar, Jacques; Bonfils, X.; Mayor, M.; Bertaux, Jean-Loup; Bouchy, F.; Delfosse, X.; Forveille, T.; Lovis, C.; Pepe, F.; Perrier, C.; Queloz, D.; Udry, S.

doi:10.1051/0004-6361/200912700

Cited by 139 publications

(141 citation statements)

References 44 publications

(58 reference statements)

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“…Its low rotation rate and weak magnetic activity suggest an age older than ∼0.1 Gyr. Its kinematics place it in the young disk population (Correia et al 2010), but this does not put a strong constraint on its age (i.e., 5 Gyr, Leggett 1992 (Nidever et al 2002) with the BANYANII tool (Malo et al 2013;Gagné et al 2014), we obtain a significant probability (P=85.1%) that this system is a member of the βPictoris moving group, which is comparable to its other bona fide members (Gagné et al 2014). Its UVW space velocity and XYZ galactic position place it at 5.05±1.80 km s −1 and 13.3±15.9 pc from the locus of known βPictoris moving group members.…”

Section: Rv Variable Targetsmentioning

confidence: 82%

A High-Precision Near-Infrared Survey for Radial Velocity Variable Low-Mass Stars Using Cshell and a Methane Gas Cell

Gagné

Plavchan

Gao

et al. 2016

ApJ

232

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We present the results of a precise near-infrared (NIR) radial velocity (RV) survey of 32 low-mass stars with spectral types K2-M4 using CSHELL at the NASA InfraRed Telescope Facility in the K band with an isotopologue methane gas cell to achieve wavelength calibration and a novel, iterative RV extraction method. We surveyed 14 members of young (≈25-150 Myr) moving groups, the young field star εEridani, and 18 nearby (<25 pc) low-mass stars and achieved typical single-measurement precisions of 8-15 m s −1 with a long-term stability of 15-50 m s −1 over longer baselines. We obtain the best NIR RV constraints to date on 27 targets in our sample, 19 of which were never followed by high-precision RV surveys. Our results indicate that very active stars can display long-term RV variations as low as ∼25-50 m s −1 at ≈2.3125 μm, thus constraining the effect of jitter at these wavelengths. We provide the first multiwavelength confirmation of GJ876bc and independently retrieve orbital parameters consistent with previous studies. We recovered RV variabilities for HD160934AB and GJ725AB that are consistent with their known binary orbits, and nine other targets are candidate RV variables with a statistical significance of 3σ-5σ. Our method, combined with the new iSHELL spectrograph, will yield long-term RV precisions of 5 m s −1 in the NIR, which will allow the detection of super-Earths near the habitable zone of mid-M dwarfs.

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Section: Rv Variable Targetsmentioning

confidence: 82%

A High-Precision Near-Infrared Survey for Radial Velocity Variable Low-Mass Stars Using Cshell and a Methane Gas Cell

Gagné

Plavchan

Gao

et al. 2016

ApJ

232

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“…of this solution, in the same way as achieved for other planetary systems (e.g. Correia et al 2005Correia et al , 2009Correia et al , 2010. For each planet, the system is integrated on a regular 2D mesh of initial conditions, with varying semi-major axis and eccentricity, while the other parameters are retained at their nominal values (Table 5).…”

Section: Stability Analysismentioning

confidence: 99%

“…For each initial condition, the system is integrated over 10 3 yr and a stability criterion is derived with the frequency analysis of the mean longitude (Laskar 1990(Laskar , 1993. As in Correia et al (2005Correia et al ( , 2009Correia et al ( , 2010, the chaotic diffusion is measured by the variation in the frequencies. The red zone corresponds to highly unstable orbits, while the dark blue region can be assumed to be stable on a billion-year timescale.…”

Section: Stability Analysismentioning

confidence: 99%

An extreme planetary system around HD 219828

Santos

Santerne

Faria

et al. 2016

A&A

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Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims. We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods. We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results. We announce the discovery of a long period (P = 13.1 yr) massive (m sin i = 15.1 M Jup ) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M ⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions. The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.

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“…For each initial condition, the system is integrated over 200 yr and a stability criterion is derived with the frequency analysis of the mean longitude (Laskar 1990(Laskar , 1993. As in Correia et al (2005Correia et al ( , 2009Correia et al ( , 2010, the chaotic diffusion is measured by the variation in the frequencies. The red zone corresponds to highly unstable orbits, while the dark blue region can be assumed to be stable on a billion-year timescale.…”

Section: Secular Couplingmentioning

confidence: 99%

The HARPS search for southern extra-solar planets

Bonfils

Curto

Correia

et al. 2013

A&A

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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 sin i = 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).

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The HARPS search for southern extra-solar planets

Cited by 139 publications

References 44 publications

A High-Precision Near-Infrared Survey for Radial Velocity Variable Low-Mass Stars Using Cshell and a Methane Gas Cell

A High-Precision Near-Infrared Survey for Radial Velocity Variable Low-Mass Stars Using Cshell and a Methane Gas Cell

An extreme planetary system around HD 219828

The HARPS search for southern extra-solar planets

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