HD 142527 -的近距离环境的高对比度成像
High Contrast Imaging of the Close Environment of HD 142527 -
摘要：
上下文长期以来，人们一直认为年轻恒星周围的星周盘可能是行星的路标，自从最近发现嵌入的亚恒星伴星以来，这一观点更加强烈。根据模型，行星与盘的相互作用可能会在盘中产生大的结构、间隙、环或螺旋。从这个意义上说，赫比格恒星HD 142527特别引人注目，因为它巨大的圆盘显示出有趣的不对称性，这表明存在一个未知性质的动力学彼得伯。目标。我们的目标是获得HD 142527近距离拱星环境的深热图像，以重新成像所报告的近距离结构（空腔，旋臂）的磁盘，并寻找可能与它们的存在有关的恒星和亚恒星同伴。结果HD 142527的拱星环境首次以前所未有的空间分辨率显示在3.8微米的亚弧秒水平。我们的图像揭示了重要的径向和方位角的不对称性，使先前提出的圆盘椭圆形失效。它更像是一个明亮的不均匀的旋臂加上各种较暗的旋臂。我们还确认了一个内腔下降到30 AU和两个重要的倾角在0和135度的位置角。角差分成像的探测性能使探测行星质量状况的物理距离接近40天文单位。使用我们的检测地图连同蒙特卡罗模拟设置严格的限制存在的行星质量，褐矮星或恒星同伴作为半长轴的函数。它们严格限制了半长轴超过50天文单位的大质量巨行星的存在，即可能在径向延伸到145天文单位甚至更远的大圆盘空腔内。
英文摘要：
Context. It has long been suggested that circumstellar disks surrounding young stars may be the signposts of planets, and still more since the recent discoveries of embedded substellar companions. The planet-disk interaction may create, according to models, large structures, gaps, rings or spirals, in the disk. In that sense, the Herbig star HD 142527 is particularly compelling as, its massive disk displays intriguing asymmetries that suggest the existence of a dynamical peturber of unknown nature. Aims. Our goal was to obtain deep thermal images of the close circumstellar environment of HD 142527 to re-image the reported close-in structures (cavity, spiral arms) of the disk and to search for stellar and substellar companions that could be connected to their presence. Results. The circumstellar environment of HD 142527 is revealed at an unprecedented spatial resolution down to the sub arcsecond level for the first time at 3.8 microns. Our images reveal important radial and azimuthal asymmetries which invalidate an elliptical shape for the disk as previously proposed. It rather suggests a bright inhomogeneous spiral arm plus various fainter spiral arms. We also confirm an inner cavity down to 30 AU and two important dips at position angles of 0 and 135 deg. The detection performance in angular differential imaging enables the exploration of the planetary mass regime for projected physical separations as close as 40 AU. The use of our detection map together with Monte Carlo simulations sets stringent constraints on the presence of planetary mass, brown dwarf or stellar companions as a function of the semi-major axis. They severely constrain the presence of massive giant planets with semi-major axis beyond 50AU, i.e. probably within the large disk's cavity that radially extends up to 145 AU or even further outside.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
