The SOPHIE search for northern extrasolar planets

Bouchy, F.; Ségransan, D.; Díaz, R. F.; Forveille, T.; Boisse, I.; Arnold, L.; Astudillo-Defru, N.; Beuzit, Jean-Luc; Bonfils, X.; Borgniet, S.; Bourrier, V.; Courcol, B.; Delfosse, X.; Demangeon, O.; Delorme, P.; Ehrenreich, D.; Hébrard, G.; Lagrange, Anne-Marie; Mayor, M.; Montagnier, G.; Moutou, C.; Naef, D.; Pepe, F.; Perrier, C.; Queloz, D.; Rey, J.; Sahlmann, J.; Santerne, A.; Santos, N. C.; Sivan, J. P.; Udry, S.; Wilson, Paul

doi:10.1051/0004-6361/201526347

Cited by 29 publications

(39 citation statements)

References 49 publications

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“…In this sense, the Neptunian desert might be similar to the short-period brown-dwarf desert (e.g., Grether & Lineweaver 2006;Cheetham et al 2015;Bouchy et al 2016), in the range of ∼20−80 M Jup , which distinguishes between planets and stellar companions (e.g., Armitage & Bonnell 2002;Ma & Ge 2014;Brandt et al 2014;Thies et al 2015). The two deserts, which are located apart by a factor of 300 in mass, indicate three distinctive populations of short-period companions: stellar companions, Jovian planets, and super-Earth planets.…”

Section: Discussionmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

299

351

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A few studies have reported a significant dearth of exoplanets with Neptune mass and radius with orbital periods below 2-4 d. This cannot be explained by observational biases because many Neptunian planets with longer orbital periods have been detected. The existence of this desert is similar to the appearance of the so-called brown-dwarf desert that suggests different formation mechanisms of planets and stellar companions with short orbital periods. Similarly, the Neptunian desert might indicate different mechanisms of formation and evolution for hot Jupiters and short-period super-Earths. We here follow a previous study and examine the location and shape of the desert in both the period-mass and period-radius planes, using the currently available large samples of planets. The desert in the period-mass plane has a relatively sharp upper edge, with a planetary mass that is inversely proportional to the planetary orbital period, while the lower, somewhat blurred, boundary is located along masses that are apparently linearly proportional to the period. The desert in the period-radius plane of the transiting planets is less clear. It seems as if the radius along the upper boundary is inversely proportional to the period to the power of one-third, while the lower boundary shows a radius that is proportional to the period to the power of two-thirds. The combination of the two upper bounds of the desert, in the period-mass and period-radius planes, yields a planetary mass-radius relation of R p /R Jup (1.2 ± 0.3)(M p /M Jup ) 0.27 ± 0.11 for 0.1 M p /M Jup 1. The derived shape of the desert, which might extend up to periods of 5-10 d, could shed some light on the formation and evolution of close-in planets.

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Section: Discussionmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

299

351

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“…This software has been used in particular in many CORALIE and HARPS radial velocity surveys in the past (e.g. Mayor et al 2011) and is discussed in more detail in Ségransan et al (2010) and Bouchy et al (2016).…”

Section: Orbit Fittingmentioning

confidence: 99%

The EBLM Project

Triaud

Martin

Ségransan

et al. 2017

A&A

125

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We present 2271 radial velocity measurements taken on 118 single-line binary stars, taken over eight years with the CORALIE spectrograph. The binaries consist of F/G/K primaries and M dwarf secondaries. They were initially discovered photometrically by the WASP planet survey, as their shallow eclipses mimic a hot Jupiter transit. The observations we present permit a precise characterisation of the binary orbital elements and mass function. With modelling of the primary star, this mass function is converted to a mass of the secondary star. In the future, this spectroscopic work will be combined with precise photometric eclipses to draw an empirical mass/radius relation for the bottom of the mass sequence. This has applications in both stellar astrophysics and the growing number of exoplanet surveys around M dwarfs. In particular, we have discovered 34 systems with a secondary mass below 0.2 M , and so we will ultimately double the number of known very low-mass stars with well-characterised masses and radii. The quality of our data combined with the amplitude of the Doppler variations mean that we are able to detect eccentricities as small as 0.001 and orbital periods to sub-second precision. Our sample can revisit some earlier work on the tidal evolution of close binaries, extending it to low mass ratios. We find some exceptional binary systems that are eccentric at orbital periods below three days, while our longest circular orbit has a period of 10.4 days. Amongst our systems, we note one remarkable architecture in J1146-42 that boasts three stars within one astronomical unit. By collating the EBLM binaries with published WASP planets and brown dwarfs, we derive a mass spectrum with twice the resolution of previous work. We compare the WASP/EBLM sample of tightly bound orbits with work in the literature on more distant companions up to 10 AU. We note that the brown dwarf desert appears wider, as it carves into the planetary domain for our short-period orbits. This would mean that a significantly reduced abundance of planets begins at ∼3 M Jup , well before the deuterium-burning limit. This may shed light on the formation and migration history of massive gas giants.

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“…To account for the instrumental drift of the SOPHIE spectrograph, wavelength calibrations are made every 2-3 hours during the night and this value is interpolated for each exposure in objAB mode only when the time between calibrations is not greater than four hours, resulting in a correction of the order of 1 ms −1 . HD17674 was part of the follow-up of ELODIE long periods (subprogram 5, or SP5; Boisse et al 2012;Bouchy et al 2009aBouchy et al , 2016. Subprogram 5 needs a higher level of precision to detect giant long-period planets (which are expected to have lower RV semi-amplitudes than SP2 planets) and to constrain the offset between ELODIE and SOPHIE.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Rey

Hébrard

Bouchy

et al. 2017

A&A

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We present new radial velocity measurements for three low-metallicity solar-like stars observed with the SOPHIE spectrograph and its predecessor ELODIE, both installed at the 193 cm telescope of the Haute-Provence Observatory, allowing the detection and characterization of three new giant extrasolar planets in intermediate periods of 1.7 to 3.7 years. All three stars, HD17674, HD42012 and HD29021 present single giant planetary companions with minimum masses between 0.9 and 2.5 M Jup . The range of periods and masses of these companions, along with the distance of their host stars, make them good targets to look for astrometric signals over the lifetime of the new astrometry satellite Gaia. We discuss the preliminary astrometric solutions obtained from the first Gaia data release.

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The SOPHIE search for northern extrasolar planets

Cited by 29 publications

References 49 publications

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

The EBLM Project

The SOPHIE search for northern extrasolar planets

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