The SOPHIE spectrograph: design and technical key-points for high throughput and high stability

Perruchot, S.; Kohler, D.; Bouchy, F.; Richaud, Y.; Richaud, Pierre; Moreaux, Gabriel; Merzougui, M.; Sottile, R.; Hill, L.; Knispel, G.; Regal, X.; Meunier, Jean-Pierre; Ilovaisky, S. A.; Coroller, H. Le; Gillet, Denis; Schmitt, J. H. M. M.; Pepe, F.; Fleury, Michel; Sоsnowska, Danuta; Vors, Patrick; Mégevand, D.; Blanc, Pierre-Éric; Carol, C.; Point, Apache; Laloge, A.; Brunel, J.-C.

doi:10.1117/12.787379

Cited by 114 publications

(38 citation statements)

References 8 publications

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“…The measured eccentricity is based on fitting a Keplerian orbital motion on the radial velocity measurements collected by H09 with the SOPHIE spectrometer (Perruchot et al 2008; Bouchy et al 2009) together with transit photometry. Li et al (2010) studied the case of WASP‐12 with that value of eccentricity, and found a large implied mass‐loss and dissipation of tidal energy in the planet.…”

Section: Introductionmentioning

confidence: 99%

Orbital eccentricity of WASP-12 and WASP-14 from new radial velocity monitoring with SOPHIE★

Husnoo

Pont

Hébrard

et al. 2011

Monthly Notices of the Royal Astronomical Society

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As part of the long‐term radial velocity monitoring of known transiting planets, we have acquired new radial velocity data for the two transiting systems WASP‐12 and WASP‐14, each harbouring a gas giant on a close orbit (orbital period of 1.09 and 2.24 d, respectively). In both cases, the initial orbital solution suggested a significant orbital eccentricity, 0.049 ± 0.015 for WASP‐12b and 0.091 ± 0.003 for WASP‐14b. Since then, measurements of the occultation of WASP‐12 in the infrared have indicated that one projection of the eccentricity (e cos ω) was close to zero, casting doubt on the eccentricity from the initial radial velocity orbit. Our measurements show that the radial velocity data are compatible with a circular orbit. A MCMC analysis taking into account the presence of correlated systematic noise in both the radial velocity and photometric data gives e= 0.017+0.015−0.010. In contrast, we confirm the orbital eccentricity of WASP‐14b, and refine its value to e= 0.0877 ± 0.0030, a 10σ detection. WASP‐14b is thus the closest presently known planet with a confirmed eccentric orbit.

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Section: Introductionmentioning

confidence: 99%

Orbital eccentricity of WASP-12 and WASP-14 from new radial velocity monitoring with SOPHIE★

Husnoo

Pont

Hébrard

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…A model fit to the first transit event indicated a Jupitersized planet on an equatorial transit (for values, see Table 1). Alerted by this event, two spectra of CoRoT-9 were obtained with the SOPHIE spectrograph 7 To assign reliable absolute values to the size and mass of the CoRoT9b planet, a precise characterization of the planet host star is required. Spectra taken at the Thüringer Landessternwarte and with the UVES spectrograph on the Very Large Telescope Unit 2 (ESO) indicated a G3V star of nearly solar metallicity.…”

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confidence: 99%

A transiting giant planet with a temperature between 250 K and 430 K

Deeg

Moutou

Erikson

et al. 2010

Nature

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115

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“…The 1.93 m telescope at the Observatoire de Haute Provence, France, can observe with sophie (Spectrographe pour l'Observation des Phénomènes des Intérieurs stellaires et des Exoplanètes) (Perruchot et al 2008). The wavelength range is 3870Å to 6940Å with a resolving power of R = 70000 (high-resolution mode).…”

Section: Observations and Data Treatmentunclassified

The classification of frequencies in the γ Doradus/δ Scuti hybrid star HD 49434★

Brunsden

Pollard

Cottrell

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Hybrid stars of the γ Doradus and δ Scuti pulsation types have great potential for asteroseismic analysis to explore their interior structure. To achieve this, mode identifications of pulsational frequencies observed in the stars must be made, a task which is far from simple. In this work we begin the analysis by scrutinizing the frequencies found in the CoRoT photometric satellite measurements and ground-based high-resolution spectroscopy of the hybrid star HD 49434. The results show almost no consistency between the frequencies found using the two techniques and no characteristic period spacings or couplings were identified in either dataset. The spectroscopic data additionally show no evidence for any long term (5 year) variation in the dominant frequency. The 31 spectroscopic frequencies identified have standard deviation profiles suggesting multiple modes sharing (l, m) in the δ Scuti frequency region and several skewed modes sharing the same (l, m) in the γ Doradus frequency region. In addition, there is a clear frequency in the γ Doradus frequency region that appears to be unrelated to the others. We conclude HD 49434 remains a δ Scuti/ γ Doradus candidate hybrid star but more sophisticated models dealing with rotation are sought to obtain a clear picture of the pulsational behaviour of this star.

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The SOPHIE spectrograph: design and technical key-points for high throughput and high stability

Cited by 114 publications

References 8 publications

Orbital eccentricity of WASP-12 and WASP-14 from new radial velocity monitoring with SOPHIE★

Orbital eccentricity of WASP-12 and WASP-14 from new radial velocity monitoring with SOPHIE★

A transiting giant planet with a temperature between 250 K and 430 K

The classification of frequencies in the γ Doradus/δ Scuti hybrid star HD 49434★

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