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The EBLM Project : IV. Spectroscopic orbits of over 100 eclipsing M dwarfs masquerading as transiting hot-Jupiters

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Date
12/2017
Author
Triaud, Amaury H. M. J.
Martin, David V.
Ségransan, Damien
Smalley, Barry
Maxted, Pierre F. L.
Anderson, David R.
Bouchy, François
Collier Cameron, Andrew
Faedi, Francesca
Gómez Maqueo Chew, Yilen
Hebb, Leslie
Hellier, Coel
Marmier, Maxime
Pepe, Francesco
Pollacco, Don
Queloz, Didier
Udry, Stéphane
West, Richard
Keywords
Binaries: eclipsing
Techniques: photometric
Techniques: radial velocities
Brown dwarfs
Stars: statistics
Stars: luminosity function, mass function
QB Astronomy
QC Physics
NDAS
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Abstract
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 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.
Citation
Triaud , 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 . https://doi.org/10.1051/0004-6361/201730993
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201730993
ISSN
0004-6361
Type
Journal article
Rights
© 2017, EDP Sciences. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201730993
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  • University of St Andrews Research
URL
https://arxiv.org/abs/1707.07521
http://adsabs.harvard.edu/abs/2017arXiv170707521T
URI
http://hdl.handle.net/10023/12051

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