Performance of the Canada‐France‐Hawaii Telescope Adaptive Optics Bonnette

Rigaut, François; Salmon, Derrick; Arsenault, Robin; Thomas, Jim; Lai, Olivier; Rouan, D.; Véran, Jean-Pierre; Gigan, P.; Crampton, D.; Fletcher, J. M.; Stilburn, James R.; Boyer, Corinne; Jagourel, Pascal

doi:10.1086/316126

Cited by 145 publications

(100 citation statements)

References 22 publications

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“…HD 14348 and HD 18757 were observed as filler targets during a program dedicated to mass measurements for M dwarfs at the 3.6 m Canada-France-Hawaii Telescope (CFHT) using PUEO, the CFHT Adaptive Optics Bonnette (Rigaut et al 1998), and the KIR infrared camera (Doyon et al 1998). The observing procedure is described by Delfosse et al (1999).…”

Section: High-resolution Imaging With Pueomentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Bouchy

Ségransan

Díaz

et al. 2015

A&A

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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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Section: High-resolution Imaging With Pueomentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Bouchy

Ségransan

Díaz

et al. 2015

A&A

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“…We observed θ Cygni at high angular resolution and high contrast with the adaptive-optics (AO) instrument PUEO (Rigaut et al 1998) mounted on the 3.6-m Canada-France-Hawaii Telescope (CFHT, USA). The near-infrared camera used, KIR (Doyon et al 1998), has a field of view of ∼35 × 35 , with a scale of ∼0.035 per pixel.…”

Section: Imaging Datamentioning

confidence: 99%

Extrasolar planets and brown dwarfs around A–F type stars

Desort¹,

Lagrange²,

Galland³

et al. 2009

A&A

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Aims. In the framework of the search for extrasolar planets and brown dwarfs around early-type main-sequence stars, we present the results obtained on the early F-type star θ Cygni. Methods. ELODIE and SOPHIE at the Observatoire de Haute-Provence (OHP) were used to obtain 91 and 162 spectra, respectively. Our dedicated radial-velocity measurement method was used to monitor the star's radial velocities over five years. We also used complementary, high angular resolution and high-contrast images taken with PUEO at the CFHT. Results. We show that θ Cygni radial velocities are quasi-periodically variable, with a 150-day period. These variations are not due to the 0.35-M stellar companion that we detected in imaging at more than 46 AU from the star. The absence of correlation between the bisector velocity span variations and the radial velocity variations for this 7 km s −1 v sin i star, as well as other criteria, indicate that the observed radial velocity variations do not stem from stellar spots. The observed amplitude of the bisector velocity span variations also seems to rule out stellar pulsations. However, we observe a peak in the bisector velocity span periodogram at the same period as the one found in the radial velocity periodogram, which indicates a probable link between these radial velocity variations and the low-amplitude lineshape variations with a stellar origin. Long-period variations are not expected from this type of star to our knowledge. If a stellar origin (hence of new type) were to be confirmed for these long-period radial velocity variations, this would have several consequences on the search for planets around main-sequence stars, both in terms of observational strategy and data analysis. An alternative explanation for these variable radial velocities is the presence of at least one planet of a few Jupiter masses orbiting at less than 1 AU; however, this planet alone does not explain all observed features, and the θ Cygni system is obviously more complex than a planetary system with 1 or 2 planets. Conclusions. The available data do not allow us to distinguish between these two possible origins. A vigourous follow-up in spectroscopy and photometry is needed to get a comprehensive view of the star intrinsic variability and/or its surrounding planetary system. Key words. techniques: radial velocities -stars: early-type -stars: planetary systems -stars: individual: θ Cygni Based on observations made with the ELODIE and SOPHIE spectrographs at the Observatoire de Haute-Provence (CNRS, France) and with the PUEO adaptive optics system at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National

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“…We used the MR3 configuration covering the Ca triplet (8500Å) region. This configuration was favoured above the classical Mg2 (5200Å) wavelength range because PUEO, like all other adaptive optics systems, performs better at longer wavelength (Rigaut et al 1998). The selected spatial sampling of 0.…”

Section: Observationsmentioning

confidence: 99%

The M 31 double nucleus probed with OASIS and HST

Bacon

Emsellem

Combes

et al. 2001

A&A

103

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Abstract. We present observations with the adaptive optics assisted integral field spectrograph OASIS of the M 31 double nucleus in the spectral domain around the Calcium triplet at a spatial resolution better than 0. 5 F W HM. These data are used to derive the two-dimensional stellar kinematics within the central 2 . Archival WFPC2/HST images in the F300W, F555W and F814W bands are revisited to perform a photometric decomposition of the nuclear region. We also present STIS/HST kinematics obtained from the archive. The luminosity distribution of the central region is well separated into the respective contributions of the bulge, the nucleus including P1 and P2, and the so-called UV peak. We then show, using the OASIS kinematical maps, that the axis joining P1 and P2, the two local surface brightness maxima, does not coincide with the kinematic major-axis, which is also the major-axis of the nuclear isophotes (excluding P1). We also confirm that the velocity dispersion peak is offset by ∼0. 2 from the UV peak, assumed to mark the location of the supermassive black hole. The newly reduced STIS/HST velocity and dispersion profiles are then compared to OASIS and other published kinematics. We find significant offsets with previously published data. Simple parametric models are then built to successfully reconcile all the available kinematics. We finally interpret the observations using new N-body simulations. The nearly Keplerian nuclear disk of M 31 is subject to a natural m = 1 mode, with a very slow pattern speed (3 km s −1 /pc for MBH = 7 10 7 M ), that can be maintained during more than a thousand dynamical times. The resulting morphology and kinematics of the mode can reproduce the M 31 nuclear-disk photometry and mean stellar velocity, including the observed asymmetries. It requires a central mass concentration and a cold disk system representing between 20 and 40% of its mass. Such a slow mode could be excited when interstellar clouds from the more external gaseous disk infall towards the centre. Nuclear disks formed from accreted gas are possible candidates for the precursors of these types of structures, and may be common in central regions of galaxies.

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Performance of the Canada‐France‐Hawaii Telescope Adaptive Optics Bonnette

Cited by 145 publications

References 22 publications

The SOPHIE search for northern extrasolar planets

The SOPHIE search for northern extrasolar planets

Extrasolar planets and brown dwarfs around A–F type stars

The M 31 double nucleus probed with OASIS and HST

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