用MUSE寻找原行星
Searching for proto-planets with MUSE
摘要：
原行星盘包含有空隙、环和螺旋等结构，这些结构被认为是由盘和嵌入的原行星之间的相互作用产生的。然而，只有少数行星候选者被发现在原行星盘内运行，其中大多数被质疑与盘特征混淆。我们的目标是发现更多的原行星候选人与MUSE，与改善高分辨率光谱差分成像（HRSDI）技术的第二个目标，通过分析仪器残差的MUSE。我们分析了MUSE对五颗年轻恒星的观测，并应用HRSDI技术进行了高对比度成像。在30 min积分时间下，MUSE可达到5个$σ$检测限，在0.075”和0.25”下，表观H $α$线通量分别降至10 $^{-14}$和10 $^{-15}$ erg s $^{-1}$ $^{-2}$。除PDS 70 b和c外，我们在PDS 70、J1850-3147和V1094 Sco（低至0.1”）中未检测到任何明显的吸积特征。MUSE通过测量多个波长下空间方向上的噪声特性，避免了小样本统计问题。我们在HD 163296中探测到两个不对称的原子喷流。HRSDI技术在应用于MUSE数据时允许我们在小间隔处达到光子噪声极限（即，< 0.5”）。由于光谱分辨率更高，MUSE可以实现比SPHERE/ZIMPOL更微弱的检测限（$\sim$ 5倍）。MUSE有一些仪器问题，限制了强点源情况下出现的对比度，这些强点源可以是由于高Strehl观测而产生的空间点源，也可以是由于高线-连续比而产生的光谱点源。我们修改了HRSDI技术，以更好地处理仪器伪影，提高检测限。
英文摘要：
Protoplanetary disks contain structures such as gaps, rings, and spirals, which are thought to be produced by the interaction between the disk and embedded protoplanets. However, only a few planet candidates are found orbiting within protoplanetary disks, and most of them are being challenged as having been confused with disk features. We aim to discover more proto-planetary candidates with MUSE, with a secondary aim of improving the high-resolution spectral differential imaging (HRSDI) technique by analyzing the instrumental residuals of MUSE. We analyzed MUSE observations of five young stars and applied the HRSDI technique to perform high-contrast imaging. With a 30 min integration time, MUSE can reach 5$σ$ detection limits in apparent H$α$ line flux down to 10$^{-14}$ and 10$^{-15}$ erg s$^{-1}$ cm$^{-2}$ at 0.075" and 0.25", respectively. In addition to PDS 70 b and c, we did not detect any clear accretion signatures in PDS 70, J1850-3147, and V1094 Sco down to 0.1". MUSE avoids the small sample statistics problem by measuring the noise characteristics in the spatial direction at multiple wavelengths. We detected two asymmetric atomic jets in HD 163296. The HRSDI technique when applied to MUSE data allows us to reach the photon noise limit at small separations (i.e., < 0.5"). With a higher spectral resolution, MUSE can achieve fainter detection limits in apparent line flux than SPHERE/ZIMPOL by a factor of $\sim$5. MUSE has some instrumental issues that limit the contrast that appear in cases with strong point sources, which can be either a spatial point source due to high Strehl observations or a spectral point source due to a high line-to-continuum ratio. We modified the HRSDI technique to better handle the instrumental artifacts and improve the detection limits.
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