Investigating the asymmetry of young stellar outflows: A combined MUSE-X-Shooter study of the Th 28 jet

This record contains supplementary tables and figures for the article 'Investigating the asymmetry of young stellar outflows: A combined MUSE-X-Shooter study of the Th 28 jet' by A. Murphy, E. T. Whelan, F. Bacciotti, D. Coffey, F. Comeron, J. Eisloffel, B. Nisini, S. Antoniucci, J. M. Alcala and T. P. Ray, accepted for publication by Astronomy & Astrophysics. Abstract: Characterising stellar jet asymmetries is key to providing robust constraints for jet launching models, and hence to understanding the underlying mechanisms of jet launching. This study aims to characterise the asymmetric properties of the bipolar jet from the Classical T Tauri Star Th 28. We combine data from integral field spectroscopy with VLT/MUSE and high-resolution spectra from VLT/X-Shooter to map optical emission line ratios in both jet lobes. We carry out a diagnostic analysis of these ratios to compare the density, electron temperature, and ionisation fraction within both lobes. The mass accretion rate is derived from the emission lines at the source, and compared with the mass outflow rate derived in both lobes using the estimated densities and measured [O I]λ6300 and [S II]λ6731 luminosities. The blue-shifted jet shows a significantly higher electron temperature and moderately higher ionisation fraction than the red-shifted jet. In contrast to previous studies we also estimate higher densities n H in the blue-shifted jet by a factor ∼2. These asymmetries are traced to within 1′′ (160 au) of the source in the line ratio maps. We find Ṁacc = 2.4 × 10^−7 M⊙ yr ^−1 , with an estimated obscuration factor of ∼54 due to grey scattering around the star. Estimated values of Ṁout range between 0.66 – 13.7 × 10^−9 M⊙ yr^−1 in the blue-shifted jet and 5-9 × 10^−9 M⊙ yr^−1 in the red-shifted jet. The emission line maps and diagnostic results suggest that the jet asymmetries originate close to the source and are likely intrinsic to the jet. Furthermore, the combined dataset allows access to a broad array of accretion tracers. This in turn enables a more accurate estimation of the mass accretion rate, revealing Ṁacc higher by a factor > 350 than would otherwise be determined. Summary of supplemental material: Table 1: Emission lines detected in X-shooter observations of the jet. Fluxes are measured from the red-shifted jet lobe. Tables 2 and 3: Mass accretion rates measured from MUSE and X-Shooter observations of Th 28, respectively, assuming an on-source extinction of 2.5 mags. Tables 4 and 5: As in Tables 2 and 3, for an on-source extinction of 1.26 mags. Figures 1-4: Position-velocity maps of detected emission lines from the UV and VIS arms of the X-shooter observations. Figure 5: Accretion luminosities measured from MUSE and X-Shooter data, before and after correction for on-source obscuration. Left and right panels show the corresponding values if the fluxes are corrected for a wavelength-dependent extinction of 2.5 and 1.26 mags, respectively.本数据集包含由A. Murphy、E. T. Whelan、F. Bacciotti、D. Coffey、F. Comeron、J. Eisloffel、B. Nisini、S. Antoniucci、J. M. Alcala及T. P. Ray共同撰写的论文《年轻恒星外流的不对称性研究：Th 28喷流的MUSE与X-Shooter联合观测研究》的补充表格与附图，该论文已被《天文学与天体物理学》（Astronomy & Astrophysics）接收待刊。 摘要： 对恒星喷流不对称性进行表征，可为喷流抛射模型提供可靠约束，进而帮助我们理解喷流抛射的内在物理机制。本研究旨在表征经典金牛T星（Classical T Tauri Star）Th 28所产生的双极喷流的不对称特性。我们联合使用甚大望远镜（Very Large Telescope, VLT）的MUSE积分场光谱数据，以及X-Shooter的高分辨率光谱数据，对双极喷流的两个瓣区的光学发射线比值进行成像测绘。我们对这些发射线比值开展诊断分析，以对比两个瓣区的物质密度、电子温度及电离度。我们从源区的发射线推导出物质吸积率，并结合估算的物质密度与实测的[O I]λ6300、[S II]λ6731光度，计算得到两个瓣区的物质外流率，随后将二者进行对比。相较于红移喷流，蓝移喷流的电子温度显著更高，电离度也适度更高。与以往研究不同，本研究还估算出蓝移喷流的氢原子数密度（n_H）高出红移喷流约2倍。在发射线比值成像图中，这些不对称性可追溯至距离源区1′′（160 au）以内的区域。本研究测得吸积率Ṁacc为2.4×10^−7 M⊙ yr^−1，同时估算出恒星周围的灰散射导致的遮蔽因子约为54。蓝移喷流的外流率Ṁout估算值介于0.66~13.7×10^−9 M⊙ yr^−1之间，红移喷流的外流率则介于5~9×10^−9 M⊙ yr^−1之间。发射线成像图与诊断分析结果表明，喷流的不对称性起源于源区附近，且大概率是喷流本身的固有特性。此外，本联合数据集可使用多种吸积示踪剂，进而实现更精准的吸积率估算：相较于常规方法，本研究测得的吸积率高出350倍以上。 补充材料概述： 表1：X-Shooter观测喷流时探测到的发射线。其流量由红移喷流瓣区测得。 表2与表3：分别基于MUSE与X-Shooter对Th 28的观测数据，在假设源区消光为2.5星等的前提下测得的吸积率。 表4与表5：与表2、表3的观测条件一致，仅将源区消光假设为1.26星等。 图1至图4：X-Shooter观测的紫外（UV）与可见光（VIS）波段中，探测到的发射线的位置-速度成像图。 图5：基于MUSE与X-Shooter数据测得的吸积光度，分别展示了源区遮蔽校正前后的结果。左、右子图分别对应将流量校正为2.5星等与1.26星等的波长相关消光后的对应数值。