Photometric orbits of seven detached eclipsing binaries

Popper, Daniel M.; Etzel, P. B.

doi:10.1086/112862

Cited by 389 publications

(313 citation statements)

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“…For the light curve analysis of Kepler and TrES data we used version 28 (v28) of the code jktebop (Southworth et al 2004a,b), which is based on the ebop program (Popper & Etzel 1981). As described in Paper I, the best fit was found on the complete Q0-Q17 Kepler light curve, but errors were estimated with a residual-shift (RS) method (Southworth et al 2011), run on data from each quarter separately.…”

Section: Light Curve Solutions and Absolute Parametersmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the results of our spectroscopic observations of eight detached eclipsing binaries (DEBs), selected from the Kepler Eclipsing Binary Catalog. Radial velocities (RVs) were calculated from high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory, and were used to characterize the targets in combination with the Kepler light curves. For each binary we obtained a full set of orbital and physical parameters, reaching precision below 3% in masses and radii for 5 pairs. By comparing our results with theoretical models, we assess the distance, age and evolutionary status of the researched objects. We also study eclipse timing variations of selected objects, and identify a new system with a γDor pulsator. Two systems are triples, and show lines coming from three components. In one case the motion of the outer star and the perturbation in the RVs of the inner binary are clearly visible and periodical, which allows us to directly calculate the mass of the third star, and inclination of the outer orbit. In the second case we only see a clear motion of the tertiary, and investigate two scenarios: that it is a linear trend coming from the orbital motion around the inner binary, and that it is caused by a planetary mass companion. When possible, we also compare our results with the literature, and conclude that only by combining photometry with RVs it is possible to obtain correct physical parameters of both components of a DEB.

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Section: Light Curve Solutions and Absolute Parametersmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…We fit the eclipse light curves using the Nelson & Davis (1972) models, with an adapted implementation of the JKTEBOP code (Popper & Etzel 1981;Southworth et al 2004). The free parameters in our fit are the phase of the eclipse, determined by the orbital parameter e cos ω, and the depth of the eclipse, determined by the surface brightness ratio between the planet and the star Sp/S⋆.…”

Section: Eclipse Light Curve Fittingmentioning

confidence: 99%

K s-band secondary eclipses of WASP-19b and WASP-43b with the Anglo-Australian Telescope★

Zhou

Bayliss

Kedziora-Chudczer

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report new K s band secondary eclipse observations for the hot-Jupiters WASP-19b and WASP-43b. Using the IRIS2 infrared camera on the Anglo-Australian Telescope (AAT), we measured significant secondary eclipses for both planets, with depths of 0.287 +0.020 −0.020 % and 0.181 +0.027 −0.027 % for WASP-19b and WASP-43b respectively. We compare the observations to atmosphere models from the VSTAR line-by-line radiative transfer code, and examine the effect of C/O abundance, top layer haze, and metallicities on the observed spectra. We performed a series of signal injection and recovery exercises on the observed light curves to explore the detection thresholds of the AAT+IRIS2 facility. We find that the optimal photometric precision is achieved for targets brighter than K mag = 9, for which eclipses as shallow as 0.05 % are detectable at > 5 σ significance.

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“…The model and the Markov Chain Monte Carlo algorithm used to take samples from the Bayesian posterior are implemented in the PASTIS package, which is described in detail in Díaz et al (2013, in prep.). Basically, we modeled the light curves with the EBOP code (Etzel 1981;Popper & Etzel 1981) using a quadratic limb-darkening law with coefficients interpolated from the tables of Claret & Bloemen (2011). To deal with the distortion of the transit shape arising from the finite integration time (Kipping 2010) of LC data, we oversampled the model to five times the original sampling rate and re-binned to the LC sampling rate before comparing them to the data.…”

Section: Modeling Of the Data And Parameter Estimationmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates

Díaz

Damiani

Deleuil

et al. 2013

A&A

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We report the discovery of a transiting brown dwarf companion to KOI-205, a K0 main-sequence star, in a 11.720125-day period orbit. The transits were detected by the Kepler space telescope, and the reflex motion of the star was measured using radial velocity observations obtained with the SOPHIE spectrograph. The atmospheric parameters of the host stars were determined from the analysis of high-resolution, high signal-to-noise ratio ESPaDOns spectra obtained for this purpose. Together with spectrophotometric measurements recovered from the literature, these spectra indicate that the star is a mildly metallic K0 dwarf with T eff 5237 ± 60 K. The mass of the companion is 39.9 ± 1.0 M Jup and its radius is 0.81 ± 0.02 R Jup , in agreement with current theoretical predictions. This is the first time a bona fide brown dwarf companion is detected in orbit around a star of this type. The formation and orbital evolution of brown dwarf companions is briefly discussed in the light of this new discovery.

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Photometric orbits of seven detached eclipsing binaries

Cited by 389 publications

References 0 publications

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

K s-band secondary eclipses of WASP-19b and WASP-43b with the Anglo-Australian Telescope★

SOPHIE velocimetry ofKeplertransit candidates

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