Lucky imaging of transiting planet host stars with LuckyCam
Lucky imaging of transiting planet host stars with LuckyCam
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DOI：
10.1093/mnras/stt885
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发表时间：
2013-05
影响因子：
4.8
通讯作者：
F. Faedi;Tim D. Staley;Y. G. M. Chew;D. Pollacco;S. Dhital;S. Dhital;S. Barros;I. Skillen;L. Hebb;Craig D. Mackay;Christopher A. Watson
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文献类型：
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作者：
F. Faedi;Tim D. Staley;Y. G. M. Chew;D. Pollacco;S. Dhital;S. Dhital;S. Barros;I. Skillen;L. Hebb;Craig D. Mackay;Christopher A. Watson
我们获得了高分辨率，高对比度的光学成像在斯隆数字巡天i（'）波段与LuckyCam相机安装在2.56米北欧光学望远镜，寻找暗淡的恒星同伴16颗恒星窝藏过境系外行星。幸运成像技术使用非常短的曝光时间来获得近衍射极限的图像，产生亚弧秒的灵敏度，使我们能够在主行星宿主的视盘内寻找微弱的恒星同伴。在这里，我们报告了两个候选恒星同伴的行星主机TrES-1在分离\textless 6.5角秒，我们确认恒星同伴的CoRoT-2，CoRoT-3，TrES-2，TrES-4和HAT-P-7已经在文献中已知。我们没有确认Bergfors等人通过Lucky成像发现的HAT-P-8的候选伴侣，然而，最可能的原因是HAT-P-8是在较差的视觉条件下观察到的。我们的探测灵敏度限制，使我们能够把我们的样本中的行星宿主恒星的光谱类型和推定的绑定同伴的质量的限制。如果绑定，在这项工作中确定的恒星同伴将为行星形成和演化的模型提供严格的观测约束。此外，这些伴星可能会影响这些系统中系外行星的衍生物理性质。
We obtained high-resolution, high-contrast optical imaging in the Sloan Digital Sky Survey i(') band with the LuckyCam camera mounted on the 2.56 m Nordic Optical Telescope, to search for faint stellar companions to 16 stars harbouring transiting exoplanets. The Lucky imaging technique uses very short exposures to obtain near diffraction-limited images yielding sub-arcsecond sensitivity, allowing us to search for faint stellar companions within the seeing disc of the primary planet host. Here, we report the detection of two candidate stellar companions to the planet host TrES-1 at separations \textless 6.5 arcsec and we confirm stellar companions to CoRoT-2, CoRoT-3, TrES-2, TrES-4 and HAT-P-7 already known in the literature. We do not confirm the candidate companions to HAT-P-8 found via Lucky imaging by Bergfors et al., however, most probably because HAT-P-8 was observed in poor seeing conditions. Our detection sensitivity limits allow us to place constraints on the spectral types and masses of the putative bound companions to the planet host stars in our sample. If bound, the stellar companions identified in this work would provide stringent observational constraints to models of planet formation and evolution. In addition, these companions could affect the derived physical properties of the exoplanets in these systems.