发表机构
Princeton University; University of Texas at Austin; Institute for Advanced Study; Johns Hopkins University（普林斯顿大学; 德克萨斯大学奥斯汀分校; 高等研究院; 约翰斯·霍普金斯大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究在RAMSES模拟中实现模型无关的暗物质加热，发现其显著改变矮星系周围介质的热结构及离子柱密度，为通过类星体吸收线观测约束暗物质模型提供了新途径。
AI 中文摘要
许多动机良好的暗物质（DM）模型，包括暗光子暗物质、类轴子粒子、惰性中微子和原初黑洞，都可以将能量沉积到普通物质中，并显著提高天体物理气体的热能。我们在RAMSES流体动力学模拟代码中提出了一种简单、模型无关的暗物质加热实现方案，该方案由有效局部热传递速率$\Gamma_{\rm heat}$参数化。通过对一个性质类似于WLM的孤立富气矮星系进行模拟，我们发现暗物质加热显著改变了周围介质（CGM）的热结构，同时几乎不改变恒星形成率和致密星际介质。对于$\Gamma_{\rm heat} = 10^{-27}$至$10^{-25}\\ {\rm s}^{-1}$，在10 kpc处的中性氢柱密度相对于对照模拟被抑制了0.6至3.9个量级。类似地，C II和Si II柱密度分别减少了4.1和5.5个量级，而C IV和Si IV则分别减少了2.2和3.0个量级。这些特征可通过类星体吸收线光谱观测到，因此对附近场矮星系CGM的观测为约束向普通物质注入热量的暗物质模型提供了一条有前景的途径。
英文摘要
Many well-motivated dark matter (DM) scenarios, including dark photon DM, axion-like particles, sterile neutrinos, and primordial black holes, can deposit energy into ordinary matter and significantly raise the thermal energy of astrophysical gas. We present a simple, model-independent implementation of DM-induced heating in the RAMSES hydrodynamic simulation code, parameterized by an effective local heat-transfer rate $Γ_{\rm heat}$. Using simulations of an isolated gas-rich dwarf galaxy with properties similar to WLM, we find that DM heating substantially alters the thermal structure of the circumgalactic medium (CGM) while leaving the star formation rate and the dense ISM nearly unchanged. For $Γ_{\rm heat} = 10^{-27}$ to $10^{-25}\ {\rm s}^{-1}$, the neutral hydrogen column at 10 kpc is suppressed by 0.6 to 3.9 dex relative to the control simulation. Similarly, the C II and Si II column densities decrease by 4.1 and 5.5 dex, and by 2.2 and 3.0 dex for C IV and Si IV. These signatures are accessible to quasar absorption-line spectroscopy, so CGM observations of nearby field dwarf galaxies provide a promising avenue for constraining dark matter models that inject heat into ordinary matter.
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