Robo-Ao Kepler Planetary Candidate Survey. Iii. Adaptive Optics Imaging of 1629 Kepler Exoplanet Candidate Host Stars

Ziegler, Carl; Law, Nicholas M.; Morton, Tim; Baranec, Christoph; Riddle, Reed; Atkinson, Dani; Baker, Anna; Roberts, Sarah; Ciardi, David R.

doi:10.3847/1538-3881/153/2/66

Cited by 92 publications

(63 citation statements)

References 95 publications

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“…Reported by Couteau (1983) as a visual binary, with components of V magnitudes 10.97 and 14.80, separated in 1982 by 1.16 arcsec. Re-observed only recently by Ziegler et al (2017), who give the separation of 1.32 arcsec, and ∆mag = 1.90 ± 0.05 at 6000Å (from Robo-AO) and 1.54 ± 0.04 in K p band (from Gemini-N/NIRI). Identified for the first time as an eclipsing binary by the TrES survey, and later by ASAS-K. By analysing the TrES light curve only, Devor et al (2008) estimated the masses of both components: 1.209(13) and 1.208(13) M ⊙ for the primary and secondary, respectively.…”

Section: Targetsmentioning

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: Targetsmentioning

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 performed an independent check of the photometry using the pipeline described in Law et al (2014a) and Ziegler et al (2017). For sources with close separations, the later values are preferred, given the explicit de-blending, reducing the measured contrast for these objects over straight aperture photometry.…”

Section: Photometrymentioning

confidence: 99%

Robo-AO Discovery and Basic Characterization of Wide Multiple Star Systems in the Pleiades, Praesepe, and NGC 2264 Clusters

Hillenbrand

Zhang

Riddle

et al. 2018

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We identify and roughly characterize 66 candidate binary star systems in the Pleiades, Praesepe, and NGC 2264 star clusters, based on robotic adaptive optics imaging data obtained using Robo-AO at the Palomar 60″ telescope. Only ∼10% of our imaged pairs were previously known. We detect companions at red optical wavelengths, with physical separations ranging from a few tens to a few thousands of au. A three-sigma contrast curve generated for each final image provides upper limits to the brightness ratios for any undetected putative companions. The observations are sensitive to companions with a maximum contrast of ∼6 m at larger separations. At smaller separations, the mean (best) raw contrast at 2″ is 3 8 (6 m ), at 1″ is 3 0 (4 5), and at 0 5 is 1 9 (3 m ). Pointspread function subtraction can recover nearly the full contrast in the closer separations. For detected candidate binary pairs, we report separations, position angles, and relative magnitudes. Theoretical isochrones appropriate to the Pleiades and Praesepe clusters are then used to determine the corresponding binary mass ratios, which range from 0.2 to 0.9 in = q m m 2 1 . For our sample of roughly solar-mass (FGK type) stars in NGC 2264 and sub-solarmass (K and early M-type) primaries in the Pleiades and Praesepe, the overall binary frequency is measured at ∼15.5%±2%. However, this value should be considered a lower limit to the true binary fraction within the specified separation and mass ratio ranges in these clusters, given that complex and uncertain corrections for sensitivity and completeness have not been applied.

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“…To date we have reported the optical detection of 53 contaminating companions within 2.5 in a sample of 715 KOIs ) and 206 companions within ∼ 4 to 1629 KOIs Ziegler et al 2016). The addition of near-infrared observations to the existing visible data permits us to perform characterization of the detected stars, estimate their photometric parallax and the likelihood of physical association between primary/companion pairs, and calculate reinterpreted sizes for individual planet candidates.…”

Section: Introductionmentioning

confidence: 99%

Probability of the Physical Association of 104 Blended Companions to Kepler Objects of Interest Using Visible and Near-Infrared Adaptive Optics Photometry

Atkinson

Baranec

Ziegler

et al. 2016

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We determine probabilities of physical association for stars in blended Kepler Objects of Interest, and find that 14.5% +3.8%−3.4% of companions within ∼ 4 are consistent with being physically unassociated with their primary. This produces a better understanding of potential false positives in the Kepler catalog and will guide models of planet formation in binary systems. Physical association is determined through two methods of calculating multi-band photometric parallax using visible and near-infrared adaptive optics observation of 84 KOI systems with 104 contaminating companions within ∼ 4 . We find no evidence that KOI companions with separation of less than 1 are more likely to be physically associated than KOI companions generally. We also reinterpret transit depths for 94 planet candidates, and calculate that 2.6% ± 0.4% of transits have R > 15R ⊕ , which is consistent with prior modeling work.

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Robo-Ao Kepler Planetary Candidate Survey. Iii. Adaptive Optics Imaging of 1629 Kepler Exoplanet Candidate Host Stars

Cited by 92 publications

References 95 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

Robo-AO Discovery and Basic Characterization of Wide Multiple Star Systems in the Pleiades, Praesepe, and NGC 2264 Clusters

Probability of the Physical Association of 104 Blended Companions to Kepler Objects of Interest Using Visible and Near-Infrared Adaptive Optics Photometry

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