发表机构
Institute of Astronomy and Physics, Inner Mongolia University; School of Physical Science and Technology, Inner Mongolia University; Center for Frontier Science, Chiba University; Department of Physics, Graduate School of Science, Chiba University（内蒙古大学天文与物理学院; 内蒙古大学物理科学与技术学院; 千叶大学前沿科学中心; 千叶大学理学研究科物理学系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过替换NFW轮廓为带核轮廓，分析两个星系团透镜系统，发现中心暗物质核大小影响哈勃常数推断，并转化为自相互作用暗物质截面约束。
AI 中文摘要
中心暗物质分布探测了暗物质的本质和重子物理，但其对时间延迟宇宙学的影响尚未被充分探索。我们更新了先前对星系团透镜类星体SDSS J1004+4112和MACS J1149.5+2223中超新星Refsdal的分析，将主晕密度轮廓从椭圆Navarro-Frenk-White（NFW）轮廓替换为带核的椭圆NFW轮廓，并研究了中心暗物质核对哈勃常数$H_0$的影响。我们联合推断$H_0$和无量纲核大小参数$\beta=r_{\rm c}/r_{\rm s}$，而最亮星系团（BCG）要么与星系团成员星系的标度关系相关联，要么单独建模，其质量要么自由，要么根据Chabrier或Salpeter初始质量函数（IMF）的恒星质量估计赋予高斯先验。对于SDSS J1004+4112，对$\beta$和$H_0$的约束强烈依赖于BCG的处理方式。当不添加BCG恒星质量先验时，暗示存在大核；而对BCG质量的合理假设则倾向于近尖点晕，$\beta\sim 10^{-3}$。对于MACS J1149.5+2223，无先验时获得大核$\beta\sim 0.5$，而假设Salpeter IMF时则偏好中等核$\beta=0.0410^{+0.0865}_{-0.0276}$。MACS J1149.5+2223对$H_0$的约束对BCG处理方式稳定，支持其稳健性。对于Salpeter先验情况，我们得到$H_0=65.9^{+3.5}_{-3.4}\mathrm{~km~s^{-1}~Mpc^{-1}}$，不同的BCG假设使$H_0$中位数变化小于$1\sigma$。核大小约束被转化为自相互作用暗物质截面，从SDSS J1004+4112给出95%上限$\sigma/m<0.035\\,\mathrm{cm}^{2}\\,\mathrm{g}^{-1}$，从MACS J1149.5+2223给出68%范围$\sigma/m=0.071^{+0.15}_{-0.045}\\,\mathrm{cm}^{2}\\,\mathrm{g}^{-1}$。
英文摘要
The central dark matter distribution probes the nature of dark matter and baryon physics, yet its impact on time-delay cosmography is not fully explored. We update previous analyses of the cluster-lensed quasar SDSS J1004+4112 and the supernova Refsdal in MACS J1149.5+2223 by replacing the main halo density profile from an elliptical Navarro-Frenk-White (NFW) profile to a cored elliptical NFW profile and investigating the impact of the central dark matter core on the Hubble constant $H_0$. We jointly infer $H_0$ and the dimensionless core size parameter $β=r_{\rm c}/r_{\rm s}$, while the Brightest Cluster Galaxy (BCG) is either tied to the scaling relation of cluster member galaxies or modeled separately, with its mass left free or assigned a Gaussian prior from the stellar mass estimate for a Chabrier or Salpeter initial mass function (IMF). For SDSS J1004+4112, constraints on both $β$ and $H_0$ strongly depend on the treatment of the BCG. A large core is implied when no prior is added to the BCG stellar mass, while a reasonable assumption on the BCG mass prefers a nearly cuspy halo with $β\sim 10^{-3}$. For MACS J1149.5+2223, a large core of $β\sim 0.5$ is obtained with no prior, while a modest core of $β=0.0410^{+0.0865}_{-0.0276}$ is preferred when the Salpeter IMF is assumed. The constraint on $H_0$ from MACS J1149.5+2223 is stable against the BCG treatment, supporting its robustness. For the Salpeter-prior case, we obtain $H_0=65.9^{+3.5}_{-3.4}\mathrm{~km~s^{-1}~Mpc^{-1}}$, and different BCG assumptions change the median $H_0$ by less than $1σ$. The core size constraints are translated into the self-interacting dark matter cross section, giving a 95% upper limit of $σ/m<0.035\,\mathrm{cm}^{2}\,\mathrm{g}^{-1}$ from SDSS J1004+4112 and the 68% range of $σ/m=0.071^{+0.15}_{-0.045}\,\mathrm{cm}^{2}\,\mathrm{g}^{-1}$ from MACS J1149.5+2223.
Comments15 pages, 4 figures, submitted
