Keck/OSIRIS Pa $β$高对比度成像和更新PDS ~ 70 b的限制
Keck/OSIRIS Pa$β$ high-contrast imaging and updated constraints on PDS~70b
摘要：
利用Keck/OSIRIS积分场光谱仪对PDS~70系统原行星的Pa $β$谱线进行了高对比度成像研究。我们将高分辨率光谱差分成像技术应用于OSIRIS $J$波段数据，但没有检测到Pa $β$线在使用\cite{Hashimoto2020}参数预测的水平。Pa $β$发射的缺乏表明基于MUSE的研究可能高估了H $α$的线宽。我们将我们的Pa $β$检测限与以前的H $α$通量和H $β$限值进行了比较，并估计PDS~70~b和c的$A_{\rm V}$分别为$\sim0.9$和2.0。特别是PDS~70~b的$A_{\rm V}$比高对比度近红外研究所暗示的要小得多，这表明红外连续光球和氢发射区存在于形成中的行星上方的不同高度。
英文摘要：
We present a high-contrast imaging search for Pa$β$ line emission from protoplanets in the PDS~70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS $J$-band data but did not detect the Pa$β$ line at the level predicted using the parameters of \cite{Hashimoto2020}. This lack of Pa$β$ emission suggests the MUSE-based study may have overestimated the line width of H$α$. We compared our Pa$β$ detection limits with the previous H$α$ flux and H$β$ limits and estimated $A_{\rm V}$ to be $\sim0.9$ and 2.0 for PDS~70~b and c respectively. In particular, PDS~70~b's $A_{\rm V}$ is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.
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