发表机构
Texas Christian University; Presbyterian College; Space Telescope Science Institute; University of Notre Dame（德克萨斯基督教大学; 长老会学院; 太空望远镜科学研究所; 圣母大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本综述利用ULLYSES紫外光谱观测170颗OB星，结合HI与Hα发射，系统刻画了大麦哲伦云近侧恒星驱动外流的速度结构、质量流失率及反馈机制，揭示了风的多相性质与污染来源。
AI 中文摘要
我们利用170颗OB星的紫外吸收线光谱，辅以HI 21厘米发射和H$_{\alpha}$发射，研究了大麦哲伦云（LMC）近侧恒星驱动的外流。通过Voigt轮廓拟合和AOD分析SiII、OI和SII跃迁，我们绘制了前景气体的速度依赖结构。Voigt拟合分量的SiII柱密度从LMC盘平滑下降，并在$v_{\rm LMCSR} \approx -100$至$-200~{km~s^{-1}}$处达到最小值，标志着从较稠密、较慢的风向更弥散的高速物质的转变。与局部恒星形成率面密度的比较显示，较慢风分量存在适度的正相关，将其与近期大质量恒星反馈联系起来。对$+100\lesssim v_{\rm LSR} \lesssim +150~{km~s^{-1}}$范围内13个吸收体的光电离建模揭示了金属丰度、尘埃消耗和电离条件的广泛多样性，与多种可能的起源一致。虽然这一主要为电离气体的相当大部分与LMC风的高速延伸一致，但其中一部分可能源于银河系（MW）高速云（HVCs）和麦哲伦环星系介质（CGM）的污染。我们估计近侧冷气体外流质量约为${\sim}1.8\times10^{7}\\,M_{\odot}$，意味着$\dot{M}_{\rm out}\approx0.15$-$0.33\\,M_{\odot}\\,\mathrm{yr^{-1}}$和质量载荷因子$\eta\approx0.6$-1.3。在区域尺度上，30剑鱼座贡献约$\sim10\\%$，N11贡献约$\sim3\\%$的外流总质量，而尾随侧比前导侧含有更多风物质，与冲压剥离一致。这些结果提供了恒星反馈、星系环境和前景污染如何塑造从LMC涌现的多相风的全面运动学和物理特征描述。
英文摘要
We investigate nearside stellar-driven outflows from the Large Magellanic Cloud (LMC) using UV absorption-line spectroscopy of 170 OB stars, complemented by HI 21-cm emission and H$_α$ emission. Using Voigt-profile fitting and AOD analysis of SiII, OI, and SII transitions, we map the velocity-dependent structure of foreground gas. The SiII column densities for the Voigt-fitted components decline smoothly from the LMC disk and reach a minimum at $v_{\rm LMCSR} \approx -100$ to $-200~{km~s^{-1}}$, marking the transition from a denser, slower wind to more diffuse high-velocity material. Comparisons with local star-formation rate surface densities reveal a modest positive correlation for the slower wind component, linking it to recent massive-stellar feedback. Photoionization modeling of 13 absorbers in the $+100\lesssim v_{\rm LSR} \lesssim +150~{km~s^{-1}}$ range reveals wide diversity in metallicity, dust depletion, and ionization conditions, consistent with multiple possible origins. While a substantial fraction of this predominately ionized gas is consistent with the high-velocity extension of the LMC wind, part of it may arise from contamination by Milky Way (MW) high-velocity clouds (HVCs) and Magellanic circumgalactic medium (CGM). We estimate a nearside cool-gas outflow mass of ${\sim}1.8\times10^{7}\,M_{\odot}$, implying $\dot{M}_{\rm out}\approx0.15$-$0.33\,M_{\odot}\,\mathrm{yr^{-1}}$ and a mass-loading factor of $η\approx0.6$-1.3. On regional scales, 30 Doradus contributes $\sim10\%$ and N11 contributes $\sim3\%$ of the total outflow mass, while the trailing side contains more wind material than the leading side, consistent with ram-pressure stripping. These results provide the comprehensive kinematic and physical characterization of how stellar feedback, galactic environment, and foreground contamination shape the multiphase wind emerging from the LMC.
Comments36 pages, 19 Figures, 3 Tables, accepted for publication in ApJ
