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dc.contributor.authorTriaud, Amaury H. M. J.
dc.contributor.authorMartin, David V.
dc.contributor.authorSégransan, Damien
dc.contributor.authorSmalley, Barry
dc.contributor.authorMaxted, Pierre F. L.
dc.contributor.authorAnderson, David R.
dc.contributor.authorBouchy, François
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorFaedi, Francesca
dc.contributor.authorGómez Maqueo Chew, Yilen
dc.contributor.authorHebb, Leslie
dc.contributor.authorHellier, Coel
dc.contributor.authorMarmier, Maxime
dc.contributor.authorPepe, Francesco
dc.contributor.authorPollacco, Don
dc.contributor.authorQueloz, Didier
dc.contributor.authorUdry, Stéphane
dc.contributor.authorWest, Richard
dc.identifier.citationTriaud , A H M J , Martin , D V , Ségransan , D , Smalley , B , Maxted , P F L , Anderson , D R , Bouchy , F , Collier Cameron , A , Faedi , F , Gómez Maqueo Chew , Y , Hebb , L , Hellier , C , Marmier , M , Pepe , F , Pollacco , D , Queloz , D , Udry , S & West , R 2017 , ' The EBLM Project : IV. Spectroscopic orbits of over 100 eclipsing M dwarfs masquerading as transiting hot-Jupiters ' , Astronomy & Astrophysics , vol. 608 , A129 .
dc.identifier.otherBibCode: 2017arXiv170707521T
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531500
dc.description.abstractWe 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 photometricallyby 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 anempirical 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 0.2M⊙ 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 resolutionof previous work. We compare the WASP/EBLM sample of tightly bound orbits with work in the literature on more distant companionsup 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 ∼3MJup, well before the deuterium-burning limit. This may shed light on the formation and migration history of massive gas giants.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.subjectBinaries: eclipsingen
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectBrown dwarfsen
dc.subjectStars: statisticsen
dc.subjectStars: luminosity function, mass functionen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleThe EBLM Project : IV. Spectroscopic orbits of over 100 eclipsing M dwarfs masquerading as transiting hot-Jupitersen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.description.statusPeer revieweden

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