High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Evans, D. F.; Southworth, J.; Maxted, P. F. L.; Skottfelt, J.; Hundertmark, M.; Jørgensen, U. G.; Dominik, M.; Alsubai, K. A.; Andersen, M. I.; Bozza, V.; Bramich, D. M.; Burgdorf, M.; Ciceri, S.; D’Ago, G.; Jaimes, R. Figuera; Gu, Shenghong; Haugbølle, Troels; Hinse, T. C.; Juncher, D.; Kains, N.; Kerins, E.; Korhonen, H.; Küffmeier, M.; Mancini, L.; Peixinho, N.; Popovas, A.; Rabus, M.; Rahvar, S.; Schmidt, R. W.; Snodgrass, C.; Starkey, D.; Surdej, Jean; Tronsgaard, R.; Essen, C. von; Wang, Yibo; Wertz, O.

doi:10.1051/0004-6361/201527970

Cited by 51 publications

(25 citation statements)

References 133 publications

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“…We calculated the probability of such a chance alignment, as well as the probability of observing a binary companion at the separation and magnitude ratio measured, using the methods outlined in Evans et al (2016) and . Background contamination was modeled using v1.6 of the TRILEGAL galaxy model (Girardi et al 2005) with galactic coordinates l = 55.9, b = −82.4, while the binary population model was based on the results of Raghavan et al (2010).…”

Section: Resultsmentioning

confidence: 99%

“…Both stars were assumed to be on the main sequence with = g log 4.5. The model atmospheres were scaled to the stellar surface areas using the empirical temperature-radius relationship presented in Evans et al (2016). To constrain our model, we assumed that the effective temperature given in A15, derived from the combined HARPS spectra of both objects, was minimally affected by WASP-20 B.…”

Section: Resultsmentioning

confidence: 99%

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Wasp-20 Is a Close Visual Binary With a Transiting Hot Jupiter

Evans

Southworth

Smalley

2016

ApJL

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We announce the discovery that WASP-20 is a binary stellar system, consisting of two components separated by 0.2578±0 0007 on the sky, with a flux ratio of 0.4639±0.0015 in the K-band. It has previously been assumed that the system consists of a single F9 V star, with photometric and radial velocity signals consistent with a lowdensity transiting giant planet. With a projected separation of approximately 60 au between the two components, the detected planetary signals almost certainly originate from the brighter of the two stars. We reanalyze previous observations allowing for two scenarios, "planet transits A" and "planet transits B," finding that both cases remain consistent with a transiting gas giant. However, we rule out the "planet transits B" scenario because the observed transit duration requires star B to be significantly evolved, and therefore have an age much greater than star A. We outline further observations that can be used to confirm this finding. Our preferred "planet transits A" scenario results in the measured mass and radius of the planet increasing by 4σ and 1σ, respectively.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Wasp-20 Is a Close Visual Binary With a Transiting Hot Jupiter

Evans

Southworth

Smalley

2016

ApJL

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“…A recent NIR survey (Ngo et al 2015) of exoplanetary systems with known close-in giants finds that hot Jupiter hosts are twice as likely as field stars to be found in a multiple star system, with a significance of 2.8σ. However, the binarity rates of systems containing hot Jupiters remains unclear: 12% (Roell et al 2012), 38% (Evans et al 2016), 51% (Ngo et al 2015).…”

Section: Stellar Multiplicity and Close-in Planets Revisitedmentioning

confidence: 99%

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

Ziegler

Law

Morton

et al. 2017

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The Robo-AO Kepler Planetary Candidate Survey is observing every Kepler planet candidate host star with laser adaptive optics imaging to search for blended nearby stars, which may be physically associated companions and/or responsible for transit false positives. In this paper, we present the results of our search for stars nearby 1629 Kepler planet candidate hosts. With survey sensitivity to objects as close as ∼0 15, and magnitude differences Δm 6, we find 223 stars in the vicinity of 206 target KOIs; 209 of these nearby stars have not been previously imaged in high resolution. We measure an overall nearby-star probability for Kepler planet candidates of  12.6% 0.9% at separations between 0 15 and 4 0. Particularly interesting KOI systems are discussed, including 26 stars with detected companions that host rocky, habitable zone candidates and five new candidate planet-hosting quadruple star systems. We explore the broad correlations between planetary systems and stellar binarity, using the combined data set of Baranec et al. and this paper. Our previous 2σ result of a low detected nearby star fraction of KOIs hosting close-in giant planets is less apparent in this larger data set. We also find a significant correlation between detected nearby star fraction and KOI number, suggesting possible variation between early and late Kepler data releases.

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“…The image had a FWHM of 5.9 pixels (0.53 arcsec) in both spatial scales and showed no evidence for stars sufficiently close by to contaminate the light curves obtained of this object. The lower limit on the spatial resolution of this instrument is approximately 0.5 arcsec, imposed by triangular coma present in the telescope optics (Skottfelt et al 2015; see also Evans et al 2016a).…”

Section: Accounting For the Companion Starmentioning

confidence: 99%

Contamination from a nearby star cannot explain the anomalous transmission spectrum of the ultrashort period giant planet WASP-103 b

Southworth¹,

Evans²

2016

Mon. Not. R. Astron. Soc.

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The planet in the WASP-103 system is an excellent candidate for transmission spectroscopy because of its large radius and high temperature. Application of this technique found a variation of radius with wavelength which was far too strong to be explained by scattering processes in the planetary atmosphere. A faint nearby star was subsequently detected, whose contamination of the transit light curves might explain this anomaly. We present a reanalysis of published data in order to characterise the faint star and assess its effect on the measured transmission spectrum. The faint star has a mass of 0.72 ± 0.08 M ⊙ and is almost certainly gravitationally bound to the planetary system. We find that its effect on the measured physical properties of the planet and host star is small, amounting to a planetary radius larger by 0.6σ and planetary density smaller by 0.8σ. Its influence on the measured transmission spectrum is much greater: the spectrum now has a minimum around 760 nm and opacity rises to both bluer and redder wavelengths. It is a poor match to theoretical spectra and the spectral slope remains too strong for Rayleigh scattering. The existence of the faint nearby star cannot therefore explain the measured spectral properties of this hot and inflated planet. We advocate further observations of the system, both with high spatial resolution in order to improve the measured properties of the faint star, and with higher spectral resolution to confirm the anomalous transmission spectrum of the planet.

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High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Cited by 51 publications

References 133 publications

Wasp-20 Is a Close Visual Binary With a Transiting Hot Jupiter

Wasp-20 Is a Close Visual Binary With a Transiting Hot Jupiter

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

Contamination from a nearby star cannot explain the anomalous transmission spectrum of the ultrashort period giant planet WASP-103 b

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