The SOPHIE search for northern extrasolar planets

Boisse, I.; Eggenberger, A.; Santos, N. C.; Lovis, C.; Bouchy, F.; Hébrard, G.; Arnold, L.; Bonfils, X.; Delfosse, X.; Desort, M.; Díaz, R. F.; Ehrenreich, D.; Forveille, T.; Gallenne, A.; Lagrange, A. M.; Moutou, C.; Udry, S.; Pepe, F.; Perrier, C.; Perruchot, S.; Pont, F.; Queloz, D.; Santerne, A.; Ségransan, D.; Vidal‐Madjar, A.

doi:10.1051/0004-6361/201014909

Cited by 119 publications

(178 citation statements)

References 47 publications

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“…Systematic effects were corrected in the SOPHIE measurements. All the spectra taken before June 2011 are corrected for the seeing effect (Boisse et al 2010(Boisse et al , 2011. Spectra taken after June 2011 are corrected using a set of standard stars that are monitored every night.…”

Section: Observations and Datamentioning

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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Section: Observations and Datamentioning

confidence: 99%

An extreme planetary system around HD 219828

Santos

Santerne

Faria

et al. 2016

A&A

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“…The parallaxes are derived from the new H reduction (van Leeuwen 2007). The stellar rotation parameter v sin i is derived from the calibration of the SOPHIE cross-correlation function by Boisse et al (2010) with an uncertainty of ∼1 km s −1 . The time span of the observations and the numbers of the ELODIE and SOPHIE measurements are listed in Table 1.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

“…Seeing change at the fiber input introduced radial velocity changes. This so-called seeing effect on SOPHIE has been described by Boisse et al (2010Boisse et al ( , 2011, Díaz et al (2012), and Bouchy et al (2013). Considering that variations in the pupil illumination produce a differential RV effect along spectral orders, the difference between RVs measured in each half of the spectral orders can be used to partially correct the main RV.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

“…Ages were estimated using the method 1 described by da Silva et al (2006) using PARSEC stellar tracks and isochrones from Bressan et al (2012). The stellar activity level was estimated from the emission in the core of the Ca II H and K-bands measured on each SOPHIE spectra with the calibration described in Boisse et al (2010). The average values derived from this analysis are reported in Table 2 with an estimated uncertainty of 0.05.…”

Section: Stellar Characteristicsmentioning

confidence: 99%

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The SOPHIE search for northern extrasolar planets

Bouchy

Ségransan

Díaz

et al. 2015

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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-yr 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 M Jup orbiting solar-type stars with periods longer than ten years. An upper mass limit of these companions is provided using astrometric H 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.

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“…Every spectrum produces a clean CCF with a peak contrast of 11.45 ± 0.10% of the continuum, and a full width at half maximum FWHM = 12.61 ± 0.08 km s −1 . The photon-noise uncertainty of the radial velocities, determined from the SNR of the spectra and the contrast and the FWHM of the CCF (see Boisse et al 2010, for the details), is typically ±18 m s −1 . It is quite large by the SOPHIE standard because the star is an early-type and a moderately fast rotator (V sin i s = 8.0 ± 1.0 km s −1 and T eff = 6570 ± 80 K; see below).…”

Section: Radial Velocity Measurements With Sophiementioning

confidence: 99%

The retrograde orbit of the HAT-P-6b exoplanet

Hébrard

Ehrenreich

Bouchy

et al. 2011

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We observed the transit of the HAT-P-6b exoplanet across its host star with the SOPHIE spectrograph (OHP, France). The resulting stellar radial velocities display the Rossiter-McLaughlin anomaly and reveal a retrograde orbit: the planetary orbital spin and the stellar rotational spin point in approximately opposite directions. A fit to the anomaly measures a sky-projected angle λ = 166 • ± 10 • between these two spin axes. All seven known retrograde planets are hot Jupiters with masses M p < 3 M Jup . About two thirds of the planets in this mass range, however, are prograde and aligned (λ 0 • ). In contrast, most of the more massive planets (M p > 4 M Jup ) are prograde but misaligned. Different mechanisms may therefore be responsible for planetary obliquities above and below ∼3.5 M Jup .

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The SOPHIE search for northern extrasolar planets

Cited by 119 publications

References 47 publications

An extreme planetary system around HD 219828

An extreme planetary system around HD 219828

The SOPHIE search for northern extrasolar planets

The retrograde orbit of the HAT-P-6b exoplanet

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