Resolving the terrestrial planet forming regions of HD 113766 and HD 172555 with MIDI MIDI observations of HD 113766 and HD 172555
Resolving the terrestrial planet forming regions of HD 113766 and HD 172555 with MIDI MIDI observations of HD 113766 and HD 172555
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使用 HD 113766 和 HD 172555 的 MIDI MIDI 观测解析 HD 113766 和 HD 172555 的类地行星形成区域
DOI：
10.1111/j.1365-2966.2012.20816.x
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发表时间：
2012
影响因子：
4.8
通讯作者：
Smith R
中科院分区：
文献类型：
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作者：
Smith R
我们提出了新的HD 113766和HD 172555的红外干涉和VISIR光谱观测。此外，我们目前的VISIR 11米和18米的成像观测HD 113766。这些来源代表了最年轻的（分别为16和1200万年）碎片盘主机上的100万Au规模的排放。我们发现，HD 113766的光盘是部分解决的基线为42-102米，与分辨率的变化与基线长度一致的高斯模型的光盘的半高全宽（FWHM）为1.2-1.6 Au（9-12 mas）。这与VISIR观测结果一致，该观测结果将发射的上限定为0.14弧秒（17 Au），没有证据表明在更大的距离上有扩展发射。对于HD 172555，在所有56-93米长的基线上，观测结果与盘状辐射的完全分辨率一致，使尘埃的距离大于1 Au（大于35 mas）。当结合TReCS成像的限制时，在1000米处的尘埃被限制在1-8 Au区域的某个地方。在0.18米的观测揭示了扩展的圆盘发射，它可能起源于一个宽圆盘的外边缘，其内部部分也被检测到，但在10米处无法分辨，或者来自一个空间上不同的组件。这些观测提供了最准确的直接测量尘埃的位置在1-8 Au，可能源于预期的碰撞在类地行星形成。这些意见提供了宝贵的限制模型的组成光盘在这个时代，并提供了一个基础，为今后的研究，更详细地审查碎片盘的形态。
We present new MIDI interferometric and VISIR spectroscopic observations of HD 113766 and HD 172555. Additionally, we present VISIR 11-m and 18-m imaging observations of HD 113766. These sources represent the youngest (16 and 12 Myr old, respectively) debris disc hosts with emission on≪ 10 au scales. We find that the disc of HD 113766 is partially resolved on baselines of 42–102 m, with variations in resolution with baseline length consistent with a Gaussian model for the disc with a full width at half-maximum (FWHM) of 1.2–1.6 au (9–12 mas). This is consistent with the VISIR observations which place an upper limit of 0.14 arcsec (17 au) on the emission, with no evidence for extended emission at larger distances. For HD 172555, the MIDI observations are consistent with complete resolution of the disc emission on all baselines of lengths 56–93 m, putting the dust at a distance of> 1 au (> 35 mas). When combined with limits from TReCS imaging, the dust at∼ 10 m is constrained to lie somewhere in the region of 1–8 au. Observations at∼ 18 m reveal extended disc emission which could originate from the outer edge of a broad disc, the inner parts of which are also detected but not resolved at 10 m, or from a spatially distinct component. These observations provide the most accurate direct measurements of the location of the dust at 1–8 au that might originate from the collisions expected during terrestrial planet formation. These observations provide valuable constraints for models of the composition of discs at this epoch and provide a foundation for future studies to examine in more detail the morphology of debris discs.