KIC 11285625: A double-lined spectroscopic binary with a<i>γ</i>Doradus pulsator discovered from<i>Kepler</i>space photometry

Debosscher, J.; Aerts, C.; Tkachenko, A.; Pavlovski, K.; Maceroni, C.; Kurtz, D. W.; Beck, P. G.; Bloemen, S.; Degroote, P.; Lombaert, R.; Southworth, J.

doi:10.1051/0004-6361/201321702

Cited by 57 publications

(61 citation statements)

References 30 publications

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“…This makes KIC 10031808 even more interesting, as examples of such stars in eclipsing systems, especially with well measured parameters, are very rare (e.g. Debosscher et al 2013;Guo et al 2016).…”

Section: Kic 10031808mentioning

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: Kic 10031808mentioning

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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“…Given that the light curves obtained with the standard extraction algorithm and provided by the Mikulski Archive for Space Telescopes (MAST) were shown to complicate the analyses for g-mode pulators and lead to a fake instrumental low frequencies (Debosscher et al 2013;Tkachenko et al 2013a), we applied the light curve extraction code developed based on customised masks by one of us (S.B.) to the pixel data.…”

Section: A Well-studied Kepler Star: Kic 11145123mentioning

confidence: 99%

Detecting non-uniform period spacings in theKeplerphotometry ofγDoradus stars: methodology and case studies

Reeth

Tkachenko

Aerts

et al. 2015

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Context. The analysis of stellar oscillations is one of the most reliable ways to probe stellar interiors. Recent space missions such as Kepler have provided us with an opportunity to study these oscillations with unprecedented detail. For many multi-periodic pulsators such as γ Doradus stars, this led to the detection of dozens to hundreds of oscillation frequencies that could not be found from groundbased observations. Aims. We aim to detect non-uniform period spacings in the Fourier spectra of a sample of γ Doradus stars observed by Kepler. Such detection is complicated by both the large number of significant frequencies in the space photometry and by overlapping nonequidistant rotationally split multiplets. Methods. Guided by theoretical properties of gravity-mode oscillation of γ Doradus stars, we developed a period-spacing detection method and applied it to Kepler observations of a few stars, after having tested the performance from simulations. Results. The application of the technique resulted in the clear detection of non-uniform period spacing series for three out of the five treated Kepler targets. Disadvantages of the technique are also discussed, and include the disability to distinguish between different values of the spherical degree and azimuthal order of the oscillation modes without additional theoretical modelling. Conclusions. Despite the shortcomings, the method is shown to allow solid detections of period spacings for γ Doradus stars, which will allow future asteroseismic analyses of these stars.

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“…For example, this was the case for KIC 11285625, a spectroscopic double-lined eclipsing binary with a γ Dor-type pulsating primary component. Because of the originally noisy composite spectra and a small contribution of the secondary component to the total light of the system, the resulting decomposed spectrum of the secondary was of insufficient S/N to determine spectral characteristics of this star (Debosscher et al 2013). Given that both components of this binary system are slow rotators showing a large number of spectral lines in their spectra, our denoising technique should be very robust in this case.…”

Section: Composite Spectra Of Binary Starsmentioning

confidence: 99%

“…A three-component average profile was computed for each stellar component of this binary system, which means that we solved for 2 × 3 = 6 LSD profiles simultaneously. The line masks for both stars were computed using the SynthV spectral synthesis code (Tsymbal 1996) and assuming effective temperature and surface gravity values of T 1,2 eff = 6950/6400 K and log g 1,2 = 4.0/4.2 dex for the primary and secondary, respectively (Debosscher et al 2013). Given a low S/N of the spectrum of the secondary component obtained in that work, the effective temperature of this star was estimated from the relative eclipse depths.…”

Section: Composite Spectra Of Binary Starsmentioning

confidence: 99%

Denoising spectroscopic data by means of the improved least-squares deconvolution method

Tkachenko

Reeth

Tsymbal

et al. 2013

A&A

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Context. The MOST, CoRoT, and Kepler space missions have led to the discovery of a large number of intriguing, and in some cases unique, objects among which are pulsating stars, stars hosting exoplanets, binaries, etc. Although the space missions have delivered photometric data of unprecedented quality, these data are lacking any spectral information and we are still in need of ground-based spectroscopic and/or multicolour photometric follow-up observations for a solid interpretation. Aims. The faintness of most of the observed stars and the required high signal-to-noise ratio (S/N) of spectroscopic data both imply the need to use large telescopes, access to which is limited. In this paper, we look for an alternative, and aim for the development of a technique that allows the denoising of the originally low S/N (typically, below 80) spectroscopic data, making observations of faint targets with small telescopes possible and effective. Methods. We present a generalization of the original least-squares deconvolution (LSD) method by implementing a multicomponent average profile and a line strengths correction algorithm. We tested the method on simulated and real spectra of single and binary stars, among which are two intrinsically variable objects. Results. The method was successfully tested on the high-resolution spectra of Vega and a Kepler star, KIC 04749989. Application to the two pulsating stars, 20 Cvn and HD 189631, showed that the technique is also applicable to intrinsically variable stars: the results of frequency analysis and mode identification from the LSD model spectra for both objects are in good agreement with the findings from literature. Depending on the S/N of the original data and spectral characteristics of a star, the gain in S/N in the LSD model spectrum typically ranges from 5 to 15 times. Conclusions. The technique introduced in this paper allows an effective denoising of the originally low S/N spectroscopic data. The high S/N spectra obtained this way can be used to determine fundamental parameters and chemical composition of the stars. The restored LSD model spectra contain all the information on line profile variations present in the original spectra of pulsating stars, for example. The method is applicable to both high-(>30 000) and low-(<30 000) resolution spectra, although the information that can be extracted from the latter is limited by the resolving power itself.

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KIC 11285625: A double-lined spectroscopic binary with aγDoradus pulsator discovered fromKeplerspace photometry

Cited by 57 publications

References 30 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

Detecting non-uniform period spacings in theKeplerphotometry ofγDoradus stars: methodology and case studies

Denoising spectroscopic data by means of the improved least-squares deconvolution method

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