标题： 关于宇宙丝状结构的宽度和轮廓 显示英文标题

标题： On the width and profiles of cosmic filaments

摘要： 我们使用IllustrisTNG模拟研究了宇宙丝状结构的宽度和轮廓。 丝状结构通过DisPerSE识别，使用模拟中的星系样本作为输入。 由于单个丝状结构的宽度在其主轴上可能显著变化，我们将每个丝状结构分成长度介于$1.5\,h^{-1}\,\mathrm{Mpc}$和$2.5\,h^{-1}\,\mathrm{Mpc}$之间的段，并测量它们的特性。 这些丝状结构段的典型宽度从红移$z = 2.0$时的约$0.3\,\mathrm{Mpc}$逐渐增加到$z = 0.0$时的约$1.0-1.5\,\mathrm{Mpc}$。 我们发现段宽度与线性晕质量密度几乎呈线性相关，这与之前的研究一致。 段宽度与线性恒星质量密度之间也观察到类似的线性关系，这为丝状结构宽度提供了一个潜在的估计器。 此外，不同宽度的丝状结构的密度轮廓表现出自相似性，可以用类似于等温$\beta$模型的统一公式来描述。 对于给定宽度的线段，重缩放后的密度剖面从$z = 2.0$到$z = 0.0$只有轻微的变化。 在纤维宽度内，气体温度从中心到边界缓慢降低，较宽的纤维通常包含比较窄的纤维更热的气体。 这些关于纤维宽度、密度和热剖面的趋势在 TNG50、TNG100 和 TNG300 模拟中都被一致观察到，并与早期研究的结果相符。 我们简要讨论了我们发现的潜在含义和应用。 显示英文摘要

摘要： We investigated the widths and profiles of cosmic filaments using the IllustrisTNG simulations. Filaments were identified with DisPerSE, using galaxy samples in simulations as input. Since the width of an individual filament can vary significantly along its spine, we divided each filament into segments with lengths between $1.5\,h^{-1}\,\mathrm{Mpc}$ and $2.5\,h^{-1}\,\mathrm{Mpc}$ and measure their properties. The typical width of these filament segments increases gradually from approximately $0.3\,\mathrm{Mpc}$ at redshift $z = 2.0$ to about $1.0-1.5\,\mathrm{Mpc}$ at $z = 0.0$. We find that the segment width correlates nearly linearly with the linear halo mass density, consistent with previous studies. A similar linear relation is observed between the segment width and the linear stellar mass density, providing a potential estimator for filament width. Furthermore, the density profiles of filaments with different widths exhibit self-similarity and can be described by a unified formula akin to the isothermal $\beta$-model. For segments with a given width, the rescaled density profiles show only mild evolution from $z = 2.0$ to $z = 0.0$. Within the filament width, the gas temperature decreases slowly from the center to the boundary, with thicker filaments generally containing hotter gas than thinner ones. These trends in filament width, density, and thermal profiles are consistently observed across the TNG50, TNG100, and TNG300 simulations, and align well with results from earlier studies. We briefly discuss the potential implications and applications of our findings.