论文标题
最终估计重的局部价值
First estimate of the local value of the baryonic streaming velocity
论文作者
论文摘要
几项研究表明，巴元和暗物质之间的相对流速度（SV）对结构形成的影响。我们首次限制了银河系形成的SV的局部值。我们使用半分析模型a松体来模拟银河系状星系的形成。来自毛毛虫模拟的质量和暗物质合并树的高分辨率高分，使在高红移处的最小祖细胞中的恒星形成准确地模拟了恒星形成。 A斜纹的有效半分析性质使我们能够运行许多具有各种局部SV值的模拟。我们对SV影响的调查表明，它在高红移时延迟了恒星形成。但是，在红移Z = 0时，SV对银河系或卫星的总恒星质量没有影响。我们发现，极为贫穷的金属和超金属贫困的星星受SV的影响，因此可以用来限制其局部值。 SV的本地最佳值为$ V_ \ MATHRM {SV} = 1.75^{+0.13} _ { - 0.28} \，σ_\ Mathrm {Sv} $，基于四个独立的观察力。我们进一步发现，SV减少了发光的银河系卫星的数量，但这种减少不足以解决缺失的卫星问题。
Several studies have shown the influence of the relative streaming velocity (SV) between baryons and dark matter on the formation of structures. For the first time, we constrain the local value of the SV in which the Milky Way was formed. We use the semi-analytical model A-SLOTH to simulate the formation of Milky Way-like galaxies. The high resolution in mass and time of the dark matter merger trees from the Caterpillar simulation enables to accurately model star formation in the smallest progenitor halos at high redshift. The efficient semi-analytical nature of A-SLOTH allows us to run many simulations with various values of the local SV. Our investigation on the influence of the SV shows that it delays star formation at high redshift. However, at redshift z=0, the SV has no effect on the total stellar mass in the Milky Way nor its Satellites. We find that extremely metal-poor and ultra metal-poor stars are affected by the SV, and can hence be used to constrain its local value. The local optimal value of the SV is $v_\mathrm{SV} =1.75^{+0.13}_{-0.28}\,σ_\mathrm{SV}$, which is based on four independent observables. We further find that the SV decreases the number of luminous Milky Way satellites, but this decrease is not enough to solve the missing satellite problem.
