The EBLM project

Boetticher, Alexander von; Triaud, A. H. M. J.; Queloz, D.; Gill, Sam; Lendl, M.; Delrez, Laetitia; Anderson, D. R.; Cameron, A. Collier; Faedi, F.; Gillon, M.; Chew, Y. Gómez Maqueo; Hebb, Leslie; Hellier, C.; Jehin, Emmanuël; Maxted, P. F. L.; Martin, David V.; Pepe, F.; Pollacco, D.; Ségransan, D.; Smalley, B.; Udry, S.; West, R. G.

doi:10.1051/0004-6361/201731107

Cited by 34 publications

(28 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…All of our systems were identified with the CORALIE spectrograph, while distinguishing which of many candidates provided by the Wide Angle Search for Planets (WASP 1 ; Pollacco et al 2006) were indeed planets. Our paper is part of an ongoing investigation into eclipsing binaries with low mass (EBLM) following three previous instalments which focused on four specific targets (Triaud et al 2013;Gómez Maqueo Chew et al 2014;von Boetticher et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…However, taking the time to follow-up each of these photometrically is beyond the manpower of our team. While we intend to follow some systems 1 http://wasp-planets.net 2 For all of the published hot Jupiters in WASP and the few EBLM binaries published in Triaud et al (2013), Gómez Maqueo Chew et al (2014), von Boetticher et al (2017 improved transits/eclipses had been obtained with larger telescopes.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The EBLM Project

Triaud

Martin

Ségransan

et al. 2017

A&A

Self Cite

125

View full text Add to dashboard Cite

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.

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The EBLM Project

Triaud

Martin

Ségransan

et al. 2017

A&A

Self Cite

125

View full text Add to dashboard Cite

show abstract

“…Figure 3 shows posterior distribution of Kepler-503b on a mass-radius diagram for brown dwarfs and low-mass stars. Its mass and radius are comparable to those of the brown dwarf KOI-189b (Díaz et al 2014) and the metal-poor ([Fe/H]=−0.24 ± 0.16), low-mass star EBLM J0555-57Ab (von Boetticher et al 2017), with values that span the boundary between Land M-dwarfs. The mass of both KOI-189b and EBLM J0555-57Ab are within one standard deviation from Kepler-503b, but the estimated ages are very different.…”

Section: Constraints On Evolutionary Modelsmentioning

confidence: 73%

Kepler-503b: An Object at the Hydrogen Burning Mass Limit Orbiting a Subgiant Star

Cañas

Bender

Mahadevan

et al. 2018

ApJL

View full text Add to dashboard Cite

Using spectroscopic radial velocities with the APOGEE instrument and Gaia distance estimates, we demonstrate that Kepler-503b, currently considered a validated Kepler planet, is in fact a brown-dwarf/low-mass star in a nearly circular 7.2-day orbit around a subgiant star. Using a mass estimate for the primary star derived from stellar models, we derive a companion mass and radius of 0.075 ± 0.003 M (78.6 ± 3.1 M Jup ) and 0.099 +0.006 −0.004 R (0.96 +0.06 −0.04 R Jup ), respectively. Assuming the system is coeval, the evolutionary state of the primary indicates the age is ∼ 6.7 Gyr. Kepler-503b sits right at the hydrogen burning mass limit, straddling the boundary between brown dwarfs and very low-mass stars. More precise radial velocities and secondary eclipse spectroscopy with James Webb Space Telescope will provide improved measurements of the physical parameters and age of this important system to better constrain and understand the physics of these objects and their spectra. This system emphasizes the value of radial velocity observations to distinguish a genuine planet from astrophysical false positives, and is the first result from the SDSS-IV monitoring of Kepler planet candidates with the multi-object APOGEE instrument.

show abstract

“…The uncertainties in the host star properties dominate the error budget for the secondaries. The positions of the B components in the radius-mass diagram are shown in Figure 3, compared to other objects ranging from massive planets to brown dwarfs and small stars (Pont et al 2005(Pont et al , 2006Southworth 2011;Tal-Or et al 2011;Ofir et al 2012;Akeson et al 2013;Díaz et al 2013Díaz et al , 2014Moutou et al 2013;Triaud et al 2013;Zhou et al 2014;Bayliss et al 2017;von Boetticher et al 2017). The overplotted lines are theoretical solar metallicity radius-mass relations (Baraffe et al 2003(Baraffe et al , 2015.…”

Section: Discussionmentioning

confidence: 99%

Three Statistically Validated K2 Transiting Warm Jupiter Exoplanets Confirmed as Low-mass Stars

Shporer

Zhou

Vanderburg

et al. 2017

ApJL

View full text Add to dashboard Cite

We have identified three K2 transiting star-planet systems, K2-51 (EPIC 202900527), K2-67 (EPIC 206155547), and K2-76 (EPIC 206432863), as stellar binaries with low-mass stellar secondaries. The three systems were statistically validated as transiting planets, and through measuring their orbits by radial velocity (RV) monitoring we have derived the companion masses to be . Therefore, they are not planets but small stars, part of the small sample of low-mass stars with measured radius and mass. The three systems are at an orbital period range of 12-24 days, and the secondaries have a radius within 0.9-1.9 R J , not inconsistent with the properties of warm Jupiter planets. These systems illustrate some of the existing challenges in the statistical validation approach. We point out a few possible origins for the initial misclassification of these objects, including poor characterization of the host star, the difficulty in detecting a secondary eclipse in systems on an eccentric orbit, and the difficulty in distinguishing between the smallest stars and gas giant planets as the two populations have indistinguishable radius distributions. Our work emphasizes the need for obtaining medium-precision RV measurements to distinguish between companions that are small stars, brown dwarfs, and gas giant planets.

show abstract

The EBLM project

Cited by 34 publications

References 50 publications

The EBLM Project

The EBLM Project

Kepler-503b: An Object at the Hydrogen Burning Mass Limit Orbiting a Subgiant Star

Three Statistically Validated K2 Transiting Warm Jupiter Exoplanets Confirmed as Low-mass Stars

Contact Info

Product

Resources

About