The SOPHIE search for northern extrasolar planets

Wilson, Paul; Hébrard, G.; Santos, N. C.; Sahlmann, J.; Montagnier, G.; Astudillo-Defru, N.; Boisse, I.; Bouchy, F.; Rey, J.; Arnold, L.; Bonfils, X.; Bourrier, V.; Courcol, B.; Deleuil, M.; Delfosse, X.; Díaz, R. F.; Ehrenreich, D.; Forveille, T.; Moutou, C.; Pepe, F.; Santerne, A.; Ségransan, D.; Udry, S.

doi:10.1051/0004-6361/201527581

Cited by 51 publications

(79 citation statements)

References 102 publications

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“…Although different authors might have different criteria to classify an object as a brown dwarf, we note that ∼ 64% of the stars listed in Wilson et al (2016) were already given in the compilation by Ma & Ge (2014). Fifteen brown dwarf companions listed in Wilson et al (2016) were published after Ma & Ge (2014).…”

Section: The Stellar Samplementioning

confidence: 96%

Searching for chemical signatures of brown dwarf formation

Maldonado

Villaver

2017

A&A

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Context. Recent studies have shown that close-in brown dwarfs in the mass range 35-55 M Jup are almost depleted as companions to stars, suggesting that objects with masses above and below this gap might have different formation mechanisms. Aims. We aim to test whether stars harbouring "massive" brown dwarfs and stars with "low-mass" brown dwarfs show any chemical peculiarity that could be related to different formation processes. Methods. Our methodology is based on the analysis of high-resolution échelle spectra (R ∼ 57000) from 2-3 m class telescopes. We determine the fundamental stellar parameters, as well as individual abundances of C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, and Zn for a large sample of stars known to have a substellar companion in the brown dwarf regime. The sample is divided into stars hosting massive and low-mass brown dwarfs. Following previous works a threshold of 42.5 M Jup was considered. The metallicity and abundance trends of both subsamples are compared and set in the context of current models of planetary and brown dwarf formation. Results. Our results confirm that stars with brown dwarf companions do not follow the well-established gas-giant planet metallicity correlation seen in main-sequence planet hosts. Stars harbouring "massive" brown dwarfs show similar metallicity and abundance distribution as stars without known planets or with low-mass planets. We find a tendency of stars harbouring "less-massive" brown dwarfs of having slightly larger metallicity, [X Fe /Fe] values, and abundances of Sc ii, Mn i, and Ni i in comparison with the stars having the massive brown dwarfs. The data suggest, as previously reported, that massive and low-mass brown dwarfs might present differences in period and eccentricity. Conclusions. We find evidence of a non-metallicity dependent mechanism for the formation of massive brown dwarfs. Our results agree with a scenario in which massive brown dwarfs are formed as stars. At high-metallicities, the core-accretion mechanism might become efficient in the formation of low-mass brown dwarfs while at lower metallicities low-mass brown dwarfs could form by gravitational instability in turbulent protostellar discs.

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Section: The Stellar Samplementioning

confidence: 96%

Searching for chemical signatures of brown dwarf formation

Maldonado

Villaver

2017

A&A

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“…Using the astrometric method, which allows the determination of the orbital inclination, the dynamical masses of several BDs have been measured (e.g., Reffert & Quirrenbach 2011;Wilson et al 2016). Dynamical masses have also been measured for a dozen or more brown dwarf binaries (see, e.g., Table 1 in Béjar et al 2011, pp.…”

Section: And References Therein As Well As the Dwarfarchives 25mentioning

confidence: 99%

EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Nowak

Πάλλη

Gandolfi

et al. 2017

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We report the discovery of EPIC 219388192b, a transiting brown dwarf in a 5.3 day orbit around a member star of Ruprecht 147, the oldest nearby open cluster association, which was photometrically monitored by K2 during its Campaign 7. We combine the K2 time-series data with ground-based adaptive optics imaging and high-resolution spectroscopy to rule out false positive scenarios and determine the main parameters of the system. EPIC 219388192b has a radius of 1.01 0.03 R e , effective temperature T eff =5850± 85K, and iron abundance [Fe/H]=0.03±0.08dex. Its age, spectroscopic distance, and reddening are consistent with those of Ruprecht 147, corroborating its cluster membership. EPIC 219388192b is the first mature brown dwarf with precise determinations of mass, radius, and age, and serves as benchmark for evolutionary models in the substellar regime.

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“…Radial velocity surveys combined with astrometric data also show the brown dwarf desert to be real (Sahlmann et al 2011;Wilson et al 2016). Ground-based transit surveys, primarily sensitive to exoplanets with radii similar to or larger than Jupiter, seemed to confirm this desert by finding many Jupitermass objects, but very few brown dwarfs-see discoveries of WASP (Pollacco et al 2006), HATNet (Bakos et al 2004), HATSouth , and KELT ).…”

Section: Introductionmentioning

confidence: 96%

EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

Hojjatpanah¹,

Santerne²,

Dragomir³

et al. 2016

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We report the discovery of EPIC 201702477b, a transiting brown dwarf in a long period (40.73691±0.00037 day) and eccentric (e = 0.2281±0.0026) orbit. This system was initially reported as a planetary candidate based on two transit events seen in K2 Campaign 1 photometry and later validated as an exoplanet candidate. We confirm the transit and refine the ephemeris with two subsequent ground-based detections of the transit using the Las Cumbres Observatory Global Telescope 1 m telescope network. We rule out any transit timing variations above the level of ∼30 s. Using high precision radial velocity measurements from HARPS and SOPHIE we identify the transiting companion as a brown dwarf with a mass, radius, and bulk density of 66.9±1.7 M J , 0.757±0.065 R J , and 191±51 g cm −3 respectively. EPIC 201702477b is the smallest radius brown dwarf yet discovered, with a mass just below the H-burning limit. It has the highest density of any planet, substellar mass object, or main-sequence star discovered so far. We find evidence in the set of known transiting brown dwarfs for two populations of objects-high mass brown dwarfs and low mass brown dwarfs. The highermass population have radii in very close agreement to theoretical models, and show a lower-mass limit around 60 M J . This may be the signature of mass-dependent ejection of systems during the formation process.

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The SOPHIE search for northern extrasolar planets

Cited by 51 publications

References 102 publications

Searching for chemical signatures of brown dwarf formation

Searching for chemical signatures of brown dwarf formation

EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41 DAY ORBIT

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