卡特彼勒项目：一套大型Milky Way Halo
The Caterpillar Project: A Large Suite of Milky Way Sized Halos
摘要：
我们提出了最大数量的银河系大小的暗物质晕模拟在非常高的质量（$\sim$ $10^4$ M $_\odot$ /粒子）和时间分辨率（$\sim$ 5百万年/快照）完成的日期，四倍于目前在文献中。这个初始套件包括$Caterpillar$ $Project$（www.caterpillarproject.org）的前24个光环，其项目目标是60 - 70个光环，完成后将公开。我们解决了$\sim$ 20,000重力约束subhalos维里半径内的每个主机晕。在由我们的空间分辨率设置的范围内，我们的收敛性非常好，并且对当前最先进的晕轮发现器进行了改进，以更好地以如此高的分辨率识别子结构（例如，平均而言，我们在10个以上的$\sim$ M $_\odot$的每个宿主晕中回收了4个$\sim$亚晕，否则使用常规方法是不会发现的）。对于我们的放松晕，内部配置文件是合理的Einasto配置文件（$α$ = 0.169 $\pm$ 0.023），虽然这取决于一个给定的晕的放松性质和组装历史。对所有晕取平均值，子结构质量分数为$f_{m,subs} = 0.121 \pm 0.041$，质量函数斜率为d $N$ /d $M\propto M^{-1.88 \pm 0.10}$，尽管我们发现固定晕质量的归一化值分散，因为在固定晕下质量下，浓度更高的主体具有更少的晕下。由于所有拉格朗日体积类型都包含在我们的样本中，因此没有拉格朗日体积选择产生的偏差。我们对264个低分辨率晕进行了详细的污染研究，从而获得了我们的目标分辨率（半径为$\sim$ $1.4 \pm 0.4$ Mpc的球体）的非常大的和前所未有的高分辨率区域，从而可以精确地研究大银河系中心半径的低质量矮星系和高红移的第一个恒星系统（$z \geq$ 10）。
英文摘要：
We present the largest number of Milky Way sized dark matter halos simulated at very high mass ($\sim$$10^4$ M$_\odot$/particle) and temporal resolution ($\sim$5 Myrs/snapshot) done to date, quadrupling what is currently available in the literature. This initial suite consists of the first 24 halos of the $Caterpillar$ $Project$ (www.caterpillarproject.org) whose project goal of 60 - 70 halos will be made public when complete. We resolve $\sim$20,000 gravitationally bound subhalos within the virial radius of each host halo. Over the ranges set by our spatial resolution our convergence is excellent and improvements were made upon current state-of-the-art halo finders to better identify substructure at such high resolutions (e.g., on average we recover $\sim$4 subhalos in each host halo above 10$^8$ M$_\odot$ which would have otherwise not been found using conventional methods). For our relaxed halos, the inner profiles are reasonably fit by Einasto profiles ($α$ = 0.169 $\pm$ 0.023) though this depends on the relaxed nature and assembly history of a given halo. Averaging over all halos, the substructure mass fraction is $f_{m,subs} = 0.121 \pm 0.041$, and mass function slope is d$N$/d$M\propto M^{-1.88 \pm 0.10}$ though we find scatter in the normalizations for fixed halo mass due to more concentrated hosts having less subhalos at fixed subhalo mass. There are no biases stemming from Lagrangian volume selection as all Lagrangian volume types are included in our sample. Our detailed contamination study of 264 low resolution halos has resulted in obtaining very large and unprecedented, high-resolution regions around our host halos for our target resolution (sphere of radius $\sim$$1.4 \pm 0.4$ Mpc) allowing for accurate studies of low mass dwarf galaxies at large galactocentric radii and the very first stellar systems at high redshift ($z \geq$ 10).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
