We use a distribution function analysis to estimate the mass of the Milky Way out to 100 kpc using a large sample of halo stars. These stars are compiled from the literature, and the majority (~95%) have 6D phase-space information. We pay particular attention to systematic effects, such as the dynamical influence of the Large Magellanic Cloud (LMC), and the effect of unrelaxed substructure. The LMC biases the (pre-LMC infall) halo mass estimates towards higher values, while realistic stellar halos from cosmological simulations tend to underestimate the true halo mass. After applying our method to the Milky Way data we find a mass within 100 kpc of M(< 100 kpc) = 6.31 +/- 0.32 (stat.) +/- 1.26 (sys.) x 10^11 M_Sun. For this estimate, we have approximately corrected for the reflex motion induced by the LMC using the Erkal et al. model, which assumes a rigid potential for the LMC and MW. Furthermore, stars that likely belong to the Sagittarius stream are removed, and we include a 5% systematic bias, and a 20% systematic uncertainty based on our tests with cosmological simulations. Assuming the mass-concentration relation for Navarro-Frenk-White haloes, our mass estimate favours a total (pre-LMC infall) Milky Way mass of M_200c = 1.05 +/- 0.25 x 10^12 M_Sun, or (post-LMC infall) mass of M_200c = 1.20 +/- 0.25 x 10^12 M_Sun when a 1.5 x 10^11 M_Sun mass of a rigid LMC is included.

中文翻译：

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使用晕星将银河系的质量提高到 100 kpc

我们使用分布函数分析，使用大量晕星样本估计银河系的质量高达 100 kpc。这些恒星是根据文献汇编而成的，大多数（~95%）具有 6D 相空间信息。我们特别关注系统效应，例如大麦哲伦星云 (LMC) 的动力学影响和未松弛子结构的影响。LMC 将（LMC 落入前的）晕质量估计值偏向更高的值，而来自宇宙学模拟的真实恒星晕往往会低估真正的晕质量。将我们的方法应用于银河系数据后，我们发现质量在 M(< 100 kpc) = 6.31 +/- 0.32 (stat.) +/- 1.26 (sys.) x 10^11 M_Sun 的 100 kpc 内。对于这个估计，我们使用 Erkal 等人对 LMC 引起的反射运动进行了近似校正。模型，假设 LMC 和 MW 具有刚性潜力。此外，可能属于人马座流的恒星被删除，我们包括 5% 的系统偏差和基于我们的宇宙学模拟测试的 20% 系统不确定性。假设 Navarro-Frenk-White 晕的质量浓度关系，我们的质量估计有利于 M_200c = 1.05 +/- 0.25 x 10^12 M_Sun，或（LMC 后坠落）银河系的总质量（LMC 坠落前）当包含 1.5 x 10^11 M_Sun 的刚性 LMC 质量时，M_200c 的质量 = 1.20 +/- 0.25 x 10^12 M_Sun。