深HST/STIS日冕仪成像观测$\eta$ Pictoris碎片盘：猫尾的散射光成分
Deep HST/STIS Coronagraphic Imaging of the $β$ Pictoris Debris Disk: On the Scattered Light Component of the Cat's Tail
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中文总结 AI 辅助
本研究利用HST/STIS深日冕仪成像探测到β Pic碎片盘猫尾的散射光成分，建模表明颗粒高度多孔且富含有机耐火材料，并估计碰撞前体质量与冥卫一相当，同时发现外尘埃晕的翘曲与不对称性。
中文摘要 AI 辅助
$\eta$ Pictoris碎片盘是一个独特的系统，其中JWST/MIRI的中红外日冕仪成像揭示了一个新的空间分辨子结构，称为猫尾。我们展示了$\eta$ Pic在散射光下的深HST/STIS日冕仪成像，结合了2012年至2025年间六个历元的观测，以寻找猫尾的散射光成分。我们首次利用HST/STIS将盘探测到500 au的投影分离度，在50至200 au之间的中平面大部分区域实现了信噪比>100。我们报告了猫尾子结构的可见光/近红外散射光成分的探测。通过注入-恢复分析，我们发现猫尾的散射光成分的总通量为MIRI F1550C通量的0.1-0.4%。利用测得的STIS与MIRI通量比，我们对猫尾的颗粒性质进行了建模，发现这些颗粒高度多孔且几乎完全由有机耐火材料组成，这与JWST/MIRI的发现一致。我们利用太阳系矮行星和本地星际介质尘埃中的有机物含量作为代理，来估计能够产生猫尾中可见的足够有机耐火材料的碰撞前体的大小。我们发现每个碰撞前体的质量必须至少为$1-3\ imes 10^{21}$ kg，与柯伊伯带中的冥卫一和鸟神星相当。此外，我们在$\eta$ Pic的外尘埃晕中发现了显著的翘曲形态和表面亮度不对称性。我们将观测到的晕形态和不对称性与可能由行星-盘相互作用产生的预测垂直结构进行了比较。
英文摘要
The $β$ Pictoris debris disk is a unique system where mid-infrared coronagraphic imaging with JWST/MIRI revealed a new spatially resolved substructure known as the Cat's Tail. We present deep HST/STIS coronagraphic imaging of $β$ Pic in scattered light, combining six epochs of observations between 2012 and 2025, in search of the scattered light component of the Cat's Tail. We detect the disk out to a projected separation of 500 au for the first time with HST/STIS, achieving SNR > 100 across much of the midplane between 50 and 200 au. We report the detection of the visible/near-infrared scattered light component of the Cat's Tail substructure. We find through injection-recovery analysis that the scattered light component of the Cat's Tail has a total flux of $0.1-0.4\%$ of the MIRI F1550C flux. Using the measured STIS-to-MIRI flux ratio, we model the Cat's Tail grain properties and find that the grains are highly porous and almost entirely composed of organic refractory material, which is in agreement with findings with JWST/MIRI. We use the organics content of Solar System dwarf planets and dust in the local ISM as a proxy to estimate the size of the colliding progenitors that can produce enough organic refractory material seen in the Cat's Tail. We find that each colliding progenitor must have a mass of at least $1-3\times 10^{21}$ kg, comparable to Charon and Makemake in our Kuiper Belt. Additionally, we find a prominent warped morphology and surface brightness asymmetry in the outer dust halo of $β$ Pic. We compare the observed halo morphology and asymmetry to predicted vertical structures, which may arise from planet--disk interactions.
发表机构
- The University of Arizona（亚利桑那大学）
- Centro de Astrobiología (CAB, CSIC-INTA)（天体生物学中心（CAB，CSIC-INTA））
- Space Telescope Science Institute（太空望远镜科学研究所）
- NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
机构由 AI 辅助整理，请以论文原文为准。
