JWST/MIRI 成像搜索运动学探测到的原行星候选体
JWST/MIRI Imaging Search for Kinematically Detected Protoplanetary Candidates
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中文总结 AI 辅助
本研究利用JWST/MIRI日冕仪观测五个原行星盘，未探测到嵌入原行星点源，但通过定制方法给出了质量上限，凸显了观测挑战，并为未来极大望远镜研究提供参考。
中文摘要 AI 辅助
利用ALMA在CO谱线发射中观测到的运动学扰动，为嵌入的巨原行星群体塑造原行星盘结构提供了证据。我们展示了JWST/MIRI F1140C（$\lambda = 11.3~\mu$m）日冕仪对五个原行星盘（HD163296、RXJ1615.3-3255、RXJ1842.9-3532、SY Cha和LkCa 15）的观测，旨在直接探测此前根据气体运动学推断出的、在$\gtrsim$ 70 au轨道上运行的原行星候选体。数据分析采用了一种定制方法，该方法将参考PSF减法与部分分辨的内盘发射的前向建模相结合，否则内盘发射会在图像中主导衍射图样。这种方法提高了对小间距年轻伴星的灵敏度。在所有系统中均未探测到与嵌入原行星一致的点源。相反，在三个系统中，我们探测到了11.3 $\mu$m的延展发射，其追踪的外盘半径与CO探测到的半径相当。注入测试表明，在数百au的间距处，假设星周环境没有额外的热贡献，质量上限约为3-20 M$_J$。即使使用天基观测，这些上限仍大多高于从盘运动学推断出的$\sim1-5$ M$_J$质量，这主要是由于内盘和外盘的发射（和/或散射光）贡献所造成的限制。这些观测凸显了使用JWST/MIRI观测嵌入在其形成环境中的大间距原行星的挑战。所获得的经验可为未来使用极大望远镜的研究提供参考，该望远镜将探测气态巨行星发生率预期更高的间距。
英文摘要
Kinematic perturbations observed with ALMA in CO line emission provide evidence for a population of embedded giant protoplanets shaping the structure of protoplanetary disks. We present JWST/MIRI F1140C ($λ= 11.3~μ$m) coronagraphic observations of five protoplanetary disks, HD163296, RXJ1615.3-3255, RXJ1842.9-3532, SY Cha, and LkCa 15, with the goal of directly detecting candidate protoplanets orbiting at $\gtrsim$ 70 au previously inferred from gas kinematics. The data were analyzed using a bespoke methodology that combines reference PSF subtraction with forward modeling of partially resolved inner disk emission, which otherwise dominates the diffraction pattern in the images. This approach improves the sensitivity to young companions at small separations. No point source consistent with an embedded protoplanet is detected in any of the systems. Instead, in three systems we detect extended emission at $11.3~μ$m tracing the outer disk out to radii comparable to those probed by CO. Injection tests indicate upper mass limits of roughly $3-20$ M$_J$ at separations of a few hundred au, assuming no additional thermal contribution from circumplanetary environment. Even with space-based observations, these limits remain mostly above the $\sim1-5$ M$_J$ masses inferred from disk kinematics, largely due to the limitations imposed by emission (and/or scattered light) contributions from both the inner and outer disk. These observations highlight the challenges of observing protoplanets embedded in their forming environment at large separation with JWST/MIRI. Lessons learned can inform future studies with the Extremely Large Telescope, which will probe separations where the occurrence rate of gas giants is expected to be higher.
发表机构
- University of Zürich（苏黎世大学）
- Max-Planck Institute for Astronomy (MPIA)（马克斯·普朗克天文学研究所）
- Massachusetts Institute of Technology（麻省理工学院）
- Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité（巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎第七大学，巴黎索邦城）
- Space Telescope Science Institute（太空望远镜科学研究所）
- Johns Hopkins University（约翰斯·霍普金斯大学）
- ETH Zürich, Institute for Particle Physics and Astrophysics（苏黎世联邦理工学院，粒子物理与天体物理研究所）
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