用MIDI解算类地行星形成区HD113766和HD172555
Resolving the terrestrial planet forming regions of HD113766 and HD172555 with MIDI
摘要：
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微米和18微米成像观察HD 113766。这些源代表了最年轻的（分别为1600万年和1200万年）碎片盘宿主，其发射尺度<<10 AU。我们发现HD 113766的盘在42- 102 m的基线上部分分辨，其分辨率随基线长度的变化符合高斯模型，其半高宽为1.2-1.6AU（9- 12 mas）。这与VISIR观测结果一致，其上限为0。“14（17 AU）的发射，没有证据表明在更大的距离延长发射。对于HD 172555，在所有56- 93米的基线上，射电望远镜的观测结果与盘状辐射的完全分辨率一致，使尘埃的距离>1AU（> 35 mas）。当结合TReCS成像的限制时，约10 μ m的尘埃被限制在1-8AU区域的某个地方。~ 18 um处的观察显示扩展的圆盘发射可能源自宽圆盘的外边缘，其内部部分也可以在10 um处被检测到但无法分辨，或者来自空间上不同的成分。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陆地行星形成。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。
英文摘要：
We present new MIDI interferometric and VISIR spectroscopic observations of HD113766 and HD172555. Additionally we present VISIR 11um and 18um imaging observations of HD113766. These sources represent the youngest (16Myr and 12Myr old respectively) debris disc hosts with emission on <<10AU scales. We find that the disc of HD113766 is partially resolved on baselines of 42-102m, with variations in resolution with baseline length consistent with a Gaussian model for the disc with FWHM of 1.2-1.6AU (9-12mas). This is consistent with the VISIR observations which place an upper limit of 0."14 (17AU) on the emission, with no evidence for extended emission at larger distances. For HD172555 the MIDI observations are consistent with complete resolution of the disc emission on all baselines of lengths 56-93m, putting the dust at a distance of >1AU (>35mas). When combined with limits from TReCS imaging the dust at ~10um is constrained to lie somewhere in the region 1-8AU. Observations at ~18um 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 10um, or from a spatially distinct component. These observations provide the most accurate direct measurements of the location of dust at 1-8AU 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.
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