The SOPHIE search for northern extrasolar planets . I. A companion around HD 16760 with mass close to the planet/brown-dwarf transition

By F. Bouchy, G. Hébrard, S. Udry, X. Delfosse, I. Boisse, M. Desort, X. Bonfils, A. Eggenberger, David Ehrenreich, T. Forveille and 11 more. 2009

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We report on the discovery of a substellar companion or a massive Jupiter orbiting the G5V star HD 16760 using the spectrograph SOPHIE installed on the OHP 1.93-m telescope. Characteristics and performances of the spectrograph are presented, as well as the SOPHIE exoplanet consortium program. With a minimum mass of 14.3 MJup, an orbital period of 465 days and an eccentricity of 0.067, HD 16760b seems to be located just at the end of the mass distribution of giant planets, close to the planet/brown-dwarf transition. Its quite circular orbit supports a formation in a gaseous protoplanetary disk.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/abf932fbe7599c8fbb2bd497579133ef4c160423

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Citations in the corpus

PASTIS: Bayesian extrasolar planet validation. I. General framework, models, and performance (2014, methodology): “…such as the study of the bisector velocity span (Queloz et al. 2001), or the comparison of the RV signatures obtained using different correlation masks (Bouchy et al. 2009; Dı́az et al. 2012) are used to guarantee that the observed RV signal is not produced by an intricate blended stellar system.”
One of the closest exoplanet pairs to the 3:2 mean motion resonance: K2-19b and c (2015, methodology): “For more information about the SOPHIE spectrograph, we refer the interested readers to Perruchot et al. (2008) and Bouchy et al. (2009).”
KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, background): “The spectra were extracted from the detector images with the SOPHIE pipeline, which includes localization of the spectral orders on the 2D-images, optimal order extraction, cosmicray rejection, wavelength calibration and corrections of flat-field.”
Search for brown-dwarf companions of stars (2010, background): “In these high-precision programs, aiming at planet detection, they are easily spotted and characterised because of their large signatures, by far exceeding the radial velocity measurement precision (e.g. Patel et al. 2007; Bouchy et al. 2009).”
SOPHIE velocimetry of Kepler transit candidates XVII. The physical properties of giant exoplanets within 400 days of period (2015, methodology): “We observed the candidate sample with the SOPHIE spectrograph (Bouchy et al. 2009c) mounted on the 1.93 m telescope at the Observatoire de Haute-Provence (France).”
SOPHIE velocimetry of Kepler transit candidates VII. A false-positive rate of 35% for Kepler close-in giant candidates (2012, methodology): “…Kepler 1 According to Borucki et al. (2011b), a vetting flag of 4 means: “Insufficient follow-up to perform full suite of vetting tests”. targets with the SOPHIE spectrograph (Perruchot et al. 2008; Bouchy et al. 2009c) mounted on the 1.93-m telescope at the Observatoire de Haute-Provence, France.”
EXTRACTING RADIAL VELOCITIES OF A- AND B-TYPE STARS FROM ECHELLE SPECTROGRAPH CALIBRATION SPECTRA (2015, methodology): “…environmentally-stabilized spectrometers such as the HARPS-South and -North spectrographs (Mayor et al. 2003; Cosentino et al. 2012), SOPHIE at Haute-Provence (Bouchy et al. 2009), CHIRON at CTIO (Schwab et al. 2010), and the Planet Finder Spectrograph (PFS) at Magellan (Crane et al. 2006, 2010).”
The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “Their typical photon-noise errors range from 2 to 10 m s − 1 , depending on the stellar brightness and projected rotational velocity V sin i (Bouchy et al. 2009).”
The planet search programme at the ESO CES and HARPS - IV. The search for Jupiter analogues around solar-like stars (2012, background): “6 This effect looks similar to charge transfer inefficiency (CTI), which can also cause RV shifts of several m/s (Bouchy et al. 2009b).”
Wide double stars - I. The spectroscopic binaries: Double stars with wide separations in the AGK3 - I. The components that are themselves spectroscopic binaries (2011, methodology): “In 2007, we had the opportunity to obtain very accurate RV measurements with the Spectrographe pour l’Observation des PHénomènes des Intérieurs stellaires et des Exoplanètes (SOPHIE) installed on the 1.93-m telescope at OHP (Perruchot et al. 2008; Bouchy et al. 2009).”