论文标题
卫星星系的颜色和插入时间分布
Colour and infall time distributions of satellite galaxies in simulated Milky-Way analogs
论文作者
论文摘要
我们使用AURIGA模拟在不同的质量尺度（$ 10^5 m_ \ odot \ lisesim m_ \ star \ star \ sarter \ sillsim 10^{11} m_ \ odot $）中探测不同的卫星淬灭机制。我们的目标是了解观测和模拟中卫星颜色分布和恒星形成特性的起源。我们发现，Auriga模拟中的卫星种群最初旨在模拟牛油之路式的宿主星系，类似于当地体积卫星（Elves）调查的探索中的人群，以及银河类似物（SAGA）围绕的卫星在其亮度范围内的亮度范围内的亮度范围$ -12 \ ysimm mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim mim-m。和颜色 - 亮度范围$ -12 \ Lessim m_g \ Lessim -15 $。我们发现，在仿真和观察结果中，卫星从蓝色到红色范围$ -15 \ lyssim m_g \ Lessim -12 $过渡到红色，我们表明这种转变是由模拟中的环境效应驱动的。我们还证明，基于统计学上不同的形态学类型或形成恒星形成状态，模拟和观测中的颜色分布都可以分解为两个统计上不同的人群。在模拟中，这两个人群还具有统计上不同的内部时间分布。此处介绍的比较似乎表明，通过改进的精灵的目标选择可以解决野蛮分数与模拟之间的张力，但是在理解微弱星系的颜色方面仍然存在紧张局势，其中精灵似乎在Auriga中未回收大量微弱的蓝色卫星。
We use the Auriga simulations to probe different satellite quenching mechanisms operating at different mass scales ($10^5 M_\odot \lesssim M_\star \lesssim 10^{11} M_\odot$) in Milky Way-like hosts. Our goal is to understand the origin of the satellite colour distribution and star-forming properties in both observations and simulations. We find that the satellite populations in the Auriga simulations, which was originally designed to model Milky Way-like host galaxies, resemble the populations in the Exploration of Local VolumE Satellites (ELVES) Survey and the Satellites Around Galactic Analogs (SAGA) survey in their luminosity function in the luminosity range $-12 \lesssim M_V \lesssim -15$ and resemble ELVES in their quenched fraction and colour--magnitude distribution in the luminosity range $-12 \lesssim M_g \lesssim -15$. We find that satellites transition from blue colours to red colours at the luminosity range $-15 \lesssim M_g \lesssim -12$ in both the simulations and observations and we show that this shift is driven by environmental effects in the simulations. We demonstrate also that the colour distribution in both simulations and observations can be decomposed into two statistically distinct populations based on their morphological type or star-forming status that are statistically distinct. In the simulations, these two populations also have statistically distinct infall time distributions. The comparison presented here seems to indicate that the tension between the quenched fraction in SAGA and simulations is resolved by the improved target selection of ELVES, but there are still tensions in understanding the colours of faint galaxies, of which ELVES appears to have a significant population of faint blue satellites not recovered in Auriga.
