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Constraining PDS 70b’s Formation Mechanism with Multi-hydrogen-emission Observations
Research Notes of the AAS Pub Date : 2021-01-14 , DOI: 10.3847/2515-5172/abdaaa
Taichi Uyama 1, 2, 3 , Jun Hashimoto 4, 5 , Charles A. Beichman 1, 2 , Jean-Baptiste Ruffio 6 , Yuhiko Aoyama 7, 8 , Michael W. McElwain 9 , Ruobing Dong 10
Affiliation  

We present our Keck/OSIRIS observations of the Paβ emission line (1.282 μm) to investigate accretion mechanisms of PDS 70 planetary system. Our spectral differential imaging reduction to remove the stellar PSF resulted in null detection of Paβ at the locations of PDS 70b and c. The 5σ detection limit of Paβ compared with the theoretical model of Aoyama & Ikoma (2019) indicates the gas velocity onto PDS 70b is smaller than 70 km s−1, which suggests MUSE-based Hα studies overestimated the gas velocity and the mass of PDS 70b.



中文翻译:

用多氢发射观测来约束PDS 70b的形成机理

我们提出我们的PA的凯克/ OSIRIS观测β发射线(1.282  μ m)至调查PDS 70的行星系统的增生的机制。我们的光谱微分成像还原以除去恒星PSF导致零检测帕β在PDS 70b和C的位置。5 σ帕的检测极限β与青山&生驹(2019)的理论模型进行比较指示所述气体速度到PDS 70B是小于70公里S -1,这表明基于MUSE-H α研究高估了气体速度和PDS 70b的质量。

更新日期:2021-01-14
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