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dc.contributor.authorGill, S.
dc.contributor.authorMaxted, P. F. L.
dc.contributor.authorSouthworth, J.
dc.contributor.authorSmalley, B.
dc.contributor.authorGary, B. L.
dc.contributor.authorAnderson, D. R.
dc.contributor.authorBouchy, F.
dc.contributor.authorCameron, A. C.
dc.contributor.authorDominik, M.
dc.contributor.authorFaedi, F.
dc.contributor.authorGillon, M.
dc.contributor.authorGomez Maqueo Chew, Y.
dc.contributor.authorHebb, L.
dc.contributor.authorHellier, C.
dc.contributor.authorJørgensen, U. G.
dc.contributor.authorLonga-Peña, P.
dc.contributor.authorMartin, D. V.
dc.contributor.authorMcCormac, J.
dc.contributor.authorPepe, F. V.
dc.contributor.authorPollaco, D.
dc.contributor.authorQueloz, D.
dc.contributor.authorSégransan, D.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorTurner, O. D.
dc.contributor.authorTriaud, A. H. M.
dc.contributor.authorUdry, S.
dc.contributor.authorSnodgrass, R. G. West
dc.contributor.authorTurner, O. D.
dc.contributor.authorTriaud, A. H. M.
dc.contributor.authorUdry, S.
dc.contributor.authorWest, R. G.
dc.identifier.citationGill , S , Maxted , P F L , Southworth , J , Smalley , B , Gary , B L , Anderson , D R , Bouchy , F , Cameron , A C , Dominik , M , Faedi , F , Gillon , M , Gomez Maqueo Chew , Y , Hebb , L , Hellier , C , Jørgensen , U G , Longa-Peña , P , Martin , D V , McCormac , J , Pepe , F V , Pollaco , D , Queloz , D , Ségransan , D , Snodgrass , C , Turner , O D , Triaud , A H M , Udry , S , Snodgrass , R G W , Turner , O D , Triaud , A H M , Udry , S & West , R G 2019 , ' The EBLM Project VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey ' , Astronomy & Astrophysics , vol. 626 , A119 .
dc.identifier.otherPURE: 259407393
dc.identifier.otherPURE UUID: 1ba00f2a-e797-43b3-825b-6163712d6ecd
dc.identifier.otherORCID: /0000-0002-8863-7828/work/59222242
dc.identifier.otherWOS: 000472594000003
dc.identifier.otherScopus: 85068321543
dc.identifier.otherORCID: /0000-0002-3202-0343/work/75996689
dc.descriptionFunding: Science and Technology Facilities Council ST/N50434/1, ST/M001040/1, ST/N504348/1 and ST/P000495/1 (SG, PM, JE); European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement n◦ 803193/BEBOP).en
dc.description.abstractSome M-dwarfs around F-/G-type stars have been measured to be hotter and larger than predicted by stellar evolution models. Inconsistencies between observations and models need to be addressed with more mass, radius, and luminosity measurements of low-mass stars to test and refine evolutionary models. Our aim is to measure the masses, radii and ages of the stars in five low-mass eclipsing binary systems discovered by the WASP survey. We used WASP photometry to establish eclipse-time ephemerides and to obtain initial estimates for the transit depth and width. Radial velocity measurements were simultaneously fitted with follow-up photometry to find the best-fitting orbital solution. This solution was combined with measurements of atmospheric parameters to interpolate evolutionary models and estimate the mass of the primary star, and the mass and radius of the M-dwarf companion. We assess how the best fitting orbital solution changes if an alternative limb-darkening law is used and quantify the systematic effects of unresolved companions. We also gauge how the best-fitting evolutionary model changes if different values are used for the mixing length parameter and helium enhancement. We report the mass and radius of five M-dwarfs and find little evidence of inflation with respect to evolutionary models. The primary stars in two systems are near the “blue hook” stage of their post sequence evolution, resulting in two possible solutions for mass and age. We find that choices in helium enhancement and mixing-length parameter can introduce an additional 3−5% uncertainty in measured M-dwarf mass. Unresolved companions can introduce an additional 3−8% uncertainty in the radius of an M-dwarf, while the choice of limb-darkening law can introduce up to an additional 2% uncertainty. The choices in orbital fitting and evolutionary models can introduce significant uncertainties in measurements of physical properties of such systems.
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2018, ESO. This work has been made available online in accordance with the publisher's policies. This is the final published version of the work, which was originally published at
dc.subjectBinaries: eclipsingen
dc.subjectStars: atmospheresen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleThe EBLM Project VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP surveyen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
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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