从Keck/NIRC2 L-带涡旋日冕照相研究HD 141569 A周围的内盘特征
Characterization of the inner disk around HD 141569 A from Keck/NIRC2 L-band vortex coronagraphy
摘要：
HD 141569 A是一颗主序星B9.5 Ve之前的恒星，被一个突出而复杂的拱星盘所环绕，可能仍处于从原行星到碎片盘阶段的过渡阶段。在这里，我们展示了HD 141569 A的第三个内盘组件的新图像，该组件是在最近安装在W.M.后面的近红外成像仪和光谱仪NIRC 2中的矢量涡旋日冕仪的调试过程中在L'波段（3.8微米）制作的。凯克天文台凯克II自适应光学系统。我们使用了参考点扩散函数减法，它揭示了从$\simeq 23$ AU的内部工作距离到$\simeq 70$ AU的最里面的磁盘组件。我们的检测的空间尺度大致对应于先前报道的光学和近红外散射光、热Q、N和8.6微米PAH发射。我们还看到尘埃位置从L '波段到H波段（VLT/SPHERE图像）再到可见光（HST/STIS图像）的向外进展，可能表明尘埃爆发。暖盘部分嵌套在1999年由HST NICMOS拍摄的两个外带（分别位于406和245 AU）的深处。我们用辐射转移程序MCFOST拟合了HD 141569 A的新L '波段图像和光谱能量分布。我们的最佳拟合模型倾向于纯橄榄石颗粒，并且与外带的成分一致。虽然我们的图像显示了一个假定的非常微弱的点状团块或源嵌入内盘，但我们没有在内盘和第一个外环之间的间隙内检测到任何真正的伴星，灵敏度为几个木星质量。
英文摘要：
HD 141569 A is a pre-main sequence B9.5 Ve star surrounded by a prominent and complex circumstellar disk, likely still in a transition stage from protoplanetary to debris disk phase. Here, we present a new image of the third inner disk component of HD 141569 A made in the L' band (3.8 micron) during the commissioning of the vector vortex coronagraph recently installed in the near-infrared imager and spectrograph NIRC2 behind the W.M. Keck Observatory Keck II adaptive optics system. We used reference point spread function subtraction, which reveals the innermost disk component from the inner working distance of $\simeq 23$ AU and up to $\simeq 70$ AU. The spatial scale of our detection roughly corresponds to the optical and near-infrared scattered light, thermal Q, N and 8.6 micron PAH emission reported earlier. We also see an outward progression in dust location from the L'-band to the H-band (VLT/SPHERE image) to the visible (HST/STIS image), likely indicative of dust blowout. The warm disk component is nested deep inside the two outer belts imaged by HST NICMOS in 1999 (respectively at 406 and 245 AU). We fit our new L'-band image and spectral energy distribution of HD 141569 A with the radiative transfer code MCFOST. Our best-fit models favor pure olivine grains, and are consistent with the composition of the outer belts. While our image shows a putative very-faint point-like clump or source embedded in the inner disk, we did not detect any true companion within the gap between the inner disk and the first outer ring, at a sensitivity of a few Jupiter masses.
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