非常大望远镜对戈麦斯汉堡的观测：对年轻原行星候选者的洞察
Very Large Telescope observations of Gomez's Hamburger: Insights into a young protoplanet candidate
摘要：
行星被认为是在年轻恒星周围的气体和尘埃盘中形成的。特别是，有人提出巨行星可以通过中等质量恒星周围的大质量扩展盘的引力不稳定性形成。然而，我们仍然缺乏直接的观察来约束这一机制。我们已经空间解决了8.6和11.2 $μ$米发射的一个大规模的原行星盘看到边缘周围的A星，戈麦斯的汉堡包（GoHam），使用VISIR在甚大望远镜。位于中央恒星以南$350\pm50$ AU投影距离处的致密区域被发现具有减少的发射。这种不对称性与早期CO观测中发现的冷密度结构或团块的存在完全一致，我们得出与这些观测一致的物理特征：质量为0.8-11.4木星质量（尘埃与气体的质量比为0.01），半径约为10 $^2$天文单位，局部密度约为$10^{7}$ cm $^{-3}$。基于这一证据，我们认为，这个团块，我们称之为GoHam b，是一个有希望的候选人，年轻的原行星形成的引力不稳定性，可能是代表的大质量行星的前体观察到周围的A星，如HR 8799或Beta piccantine。需要在高角分辨率下进行更详细的研究，以更好地约束该物体的物理特性，从而证实这一提议。
英文摘要：
Planets are thought to form in the gas and dust disks around young stars. In particular, it has been proposed that giant planets can form through the gravitational instability of massive extended disks around intermediate-mass stars. However, we still lack direct observations to constrain this mechanism. We have spatially resolved the 8.6 and 11.2 $μ$m emission of a massive protoplanetary disk seen edge on around an A star, Gomez's Hamburger (GoHam), using VISIR at the Very Large Telescope. A compact region situated at a projected distance of $350\pm50$ AU south of the central star is found to have a reduced emission.This asymmetry is fully consistent with the presence of a cold density structure, or clump, identified in earlier CO observations, and we derive physical characteristics consistent with those observations: a mass of 0.8-11.4 Jupiter masses (for a dust-to-gas mass ratio of 0.01), a radius of about 10$^2$ astronomical units, and a local density of about $10^{7}$ cm$^{-3}$. Based on this evidence, we argue that this clump, which we call GoHam b, is a promising candidate for a young protoplanet formed by gravitational instability that might be representative of the precursors of massive planets observed around A stars, such as HR 8799 or Beta pictoris. More detailed studies at high angular resolution are needed to better constrain the physical properties of this object to confirm this proposal.
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