$z\leq 1$暗物质轮廓演化的观测证据
Observational Evidence of Evolving Dark Matter Profiles at $z\leq 1$
摘要：
利用KMOS红移一次光谱巡天（KROSS）研究了位于$z\sim 1$的256个盘状星系的暗物质晕。这个样本涵盖了红移$0.6 \leq z \leq 1.04$、有效半径$0.69 \leq R_e [\mathrm{kpc}] \leq 7.76$和恒星总质量$8.7 \leq log(M_{\mathrm{star}} \ [\mathrm{M_\odot}]) \leq 11.32$。我们提出了一个质量模型的方法来研究这些星系的旋转曲线，这使我们能够动态地计算与重子和暗物质晕的物理性质。对于前者，我们假设一个弗里曼盘，而对于后者，我们采用NFW和Burkert晕配置文件，分别。最后，我们将这两种情况的结果与最先进的宇宙学星系模拟（EAGLE，TNG 100和TNG 50）进行了比较。我们发现，{ \em核心}暗物质晕出现在半径为有效半径的1-3倍的主导量。它占总质量的比例与流体动力学星系模拟的结果非常一致。值得注意的是，我们发现$z\sim 1$恒星形成星系的暗物质核心比它们的本地同行更小，密度更大。我们的结论是，暗物质晕在过去的6.5 Gyrs逐渐扩大。也就是说，观测能够捕捉到暗物质对重子过程的响应（例如反馈），从而为我们提供了星系内部区域存在{ \em引力位涨落}的第一个经验证据，这可以通过深空探测和未来的任务来验证。
英文摘要：
We investigate the dark matter halos of 256 star-forming disc-like galaxies at $z\sim 1$ using the KMOS redshift one spectroscopic survey (KROSS). This sample covers the redshifts $0.6 \leq z \leq 1.04$, effective radii $0.69 \leq R_e [\mathrm{kpc}] \leq 7.76$, and total stellar masses $8.7 \leq log(M_{\mathrm{star}} \ [\mathrm{M_\odot}]) \leq 11.32$. We present a mass modelling approach to study the rotation curves of these galaxies, which allow us to dynamically calculate the physical properties associated with the baryons and the dark matter halo. For the former we assume a Freeman disc, while for the latter we employ the NFW and the Burkert halo profiles, separately. At the end, we compare the results of both cases with state-of-the-art cosmological galaxy simulations (EAGLE, TNG100 and TNG50). We find that the {\em cored} dark matter halo emerged as the dominant quantity from a radius 1-3 times the effective radius. Its fraction to the total mass is in good agreement with the outcome of hydrodynamical galaxy simulations. Remarkably, we found that the dark matter core of $z\sim 1$ star-forming galaxies are smaller and denser than their local counterparts. We conclude that dark matter halos have gradually expanded over the past 6.5 Gyrs. That is, observations are capable of capturing the dark matter response to the baryonic processes (e.g. feedbacks), and thus giving us the first empirical evidence of {\em gravitational potential fluctuations} in the inner region of galaxies, which can be verified with deep surveys and future missions.
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