The EBLM Project: VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey

S. Gill; P. F. L. Maxted; J. A. Evans; D. F. Evans; J. Southworth; B. Smalley; B. L. Gary; D. R. Anderson; F. Bouchy; A. C. Cameron; M. Dominik; F. Faedi; M. Gillon; Y. Gomez Maqueo Chew; L. Hebb; C. Hellier; U. G. Jørgensen; P. Longa-Peña; D. V. Martin; J. McCormac; F. V. Pepe; D. Pollaco; D. Queloz; D. Ségransan; C. Snodgrass; O. D. Turner; Amaury Triaud; S. Udry; R. G. West

doi:10.1051/0004-6361/201833054

The EBLM Project: VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey

S. Gill, P. F. L. Maxted, J. A. Evans, D. F. Evans, J. Southworth, B. Smalley, B. L. Gary, D. R. Anderson, F. Bouchy, A. C. Cameron, M. Dominik, F. Faedi, M. Gillon, Y. Gomez Maqueo Chew, L. Hebb, C. Hellier, U. G. Jørgensen, P. Longa-Peña, D. V. Martin, J. McCormacF. V. Pepe, D. Pollaco, D. Queloz, D. Ségransan, C. Snodgrass, O. D. Turner, Amaury Triaud, S. Udry, R. G. West

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

7 Citations (Scopus)

177 Downloads (Pure)

Abstract

Some 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.

Original language	English
Article number	A119
Number of pages	29
Journal	Astronomy and Astrophysics
Volume	626
DOIs	https://doi.org/10.1051/0004-6361/201833054
Publication status	Published - 24 Jun 2019

Bibliographical note

36 pages, 29 Figures. Accepted for publication in Section 7. Stellar structure and evolution of Astronomy & Astrophysics

Keywords

astro-ph.SR
binaries: eclipsing
stars: atmospheres

Access to Document

10.1051/0004-6361/201833054Licence: None: All rights reserved

S._Gill_et_al_The_EBLM_Project_Astronomy_and_Astrophysics_2019
Checked for eligibility: 12/07/2019 This document appears in its final form in Astronomy and Astrophysics, copyright © ESO 2019. The final Version of Record can be found at: https://doi.org/10.1051/0004-6361/201833054
Final published version, 2.22 MBLicence: None: All rights reserved

Cite this

Gill, S., Maxted, P. F. L., Evans, J. A., Evans, D. F., Southworth, J., Smalley, B., Gary, B. L., Anderson, D. R., Bouchy, F., Cameron, A. C., Dominik, M., Faedi, F., Gillon, M., Chew, Y. G. M., Hebb, L., Hellier, C., Jørgensen, U. G., Longa-Peña, P., Martin, D. V., ... 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 and Astrophysics, 626, Article A119. https://doi.org/10.1051/0004-6361/201833054

@article{8a007079c4e848d9a071a9a56180d4e5,

title = "The EBLM Project: VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey",

abstract = "Some 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.",

keywords = "astro-ph.SR, binaries: eclipsing, stars: atmospheres",

author = "S. Gill and Maxted, {P. F. L.} and Evans, {J. A.} and Evans, {D. F.} and J. Southworth and B. Smalley and Gary, {B. L.} and Anderson, {D. R.} and F. Bouchy and Cameron, {A. C.} and M. Dominik and F. Faedi and M. Gillon and Chew, {Y. Gomez Maqueo} and L. Hebb and C. Hellier and J{\o}rgensen, {U. G.} and P. Longa-Pe{\~n}a and Martin, {D. V.} and J. McCormac and Pepe, {F. V.} and D. Pollaco and D. Queloz and D. S{\'e}gransan and C. Snodgrass and Turner, {O. D.} and Amaury Triaud and S. Udry and West, {R. G.}",

note = "36 pages, 29 Figures. Accepted for publication in Section 7. Stellar structure and evolution of Astronomy & Astrophysics",

year = "2019",

month = jun,

day = "24",

doi = "10.1051/0004-6361/201833054",

language = "English",

volume = "626",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Gill, S, Maxted, PFL, Evans, JA, Evans, DF, Southworth, J, Smalley, B, Gary, BL, Anderson, DR, Bouchy, F, Cameron, AC, Dominik, M, Faedi, F, Gillon, M, Chew, YGM, Hebb, L, Hellier, C, Jørgensen, UG, Longa-Peña, P, Martin, DV, McCormac, J, Pepe, FV, Pollaco, D, Queloz, D, Ségransan, D, Snodgrass, C, Turner, OD, Triaud, A, Udry, S & West, RG 2019, 'The EBLM Project: VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey', Astronomy and Astrophysics, vol. 626, A119. https://doi.org/10.1051/0004-6361/201833054

TY - JOUR

T1 - The EBLM Project

T2 - VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey

AU - Gill, S.

AU - Maxted, P. F. L.

AU - Evans, J. A.

AU - Evans, D. F.

AU - Southworth, J.

AU - Smalley, B.

AU - Gary, B. L.

AU - Anderson, D. R.

AU - Bouchy, F.

AU - Cameron, A. C.

AU - Dominik, M.

AU - Faedi, F.

AU - Gillon, M.

AU - Chew, Y. Gomez Maqueo

AU - Hebb, L.

AU - Hellier, C.

AU - Jørgensen, U. G.

AU - Longa-Peña, P.

AU - Martin, D. V.

AU - McCormac, J.

AU - Pepe, F. V.

AU - Pollaco, D.

AU - Queloz, D.

AU - Ségransan, D.

AU - Snodgrass, C.

AU - Turner, O. D.

AU - Triaud, Amaury

AU - Udry, S.

AU - West, R. G.

N1 - 36 pages, 29 Figures. Accepted for publication in Section 7. Stellar structure and evolution of Astronomy & Astrophysics

PY - 2019/6/24

Y1 - 2019/6/24

N2 - Some 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.

AB - Some 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.

KW - astro-ph.SR

KW - binaries: eclipsing

KW - stars: atmospheres

UR - http://www.scopus.com/inward/record.url?scp=85068321543&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201833054

DO - 10.1051/0004-6361/201833054

M3 - Article

SN - 0004-6361

VL - 626

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A119

ER -

The EBLM Project: VI. The mass and radius of five low-mass stars in F+M binaries discovered by the WASP survey

Abstract

Bibliographical note

Keywords

Access to Document

Fingerprint

Cite this