发表机构
Institute for Astronomy, University of Hawai’i at Manoa; Department of Physics, Institute of Science Tokyo; Department of Physics, Virginia Tech; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, The University of Tokyo; Department of Physics, Florida State University（夏威夷大学马诺阿分校天体物理研究所; 东京科学大学物理系; 弗吉尼亚理工大学物理系; 东京大学宇宙线起源研究机构（Kavli IPMU）; 佛罗里达州立大学物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究探究LRDs是否可作为激波驱动的高能中微子源，通过模型计算其对IceCube弥散中微子强度的贡献，发现其贡献最高可达约13%，需更大样本与改进模型进一步约束。
AI 中文摘要
小红点（Little Red Dots, LRDs）是致密的高红移天体，其物理本质仍不确定。它们的光学光谱与IIn型超新星（Type IIn supernovae, SNe IIn）有诸多相似之处，这催生了一种观点，即它们的辐射由与周围致密物质相互作用的激波提供能量。本研究探究此类相互作用是否能为LRDs提供能量，并对IceCube探测到的弥散高能中微子强度产生贡献。在我们的简化模型中，快速的中心引擎外流驱动激波穿过致密周围物质，最终在LRDs光球附近停滞，同时部分物质继续穿过激波。我们探索了由SNe IIn以及观测和推断的LRDs性质所确定的参数范围，发现激波光度在2.2e43至3.5e44 erg/s之间的解是存在的。我们利用宇宙射线加速的分析框架以及致密激波环境中的强子相互作用，计算了产生的高能中微子辐射，并对宇宙学尺度上的LRDs总体进行了积分。对于我们基于SNe IIn的基准宇宙射线参数，在2e5 GeV以下的平均预测贡献，从最低光度五分位的约0.2%增加到最高光度五分位的约2%；而一个说明性的更高效率案例则达到了IceCube弥散中微子强度的约13%。当前LRDs普查的不完整性及其物理本质的不确定性，限制了对宇宙射线参数和L_s分布的约束。需要更大的LRDs样本，结合改进的物理模型和完整的种群合成研究，才能约束LRDs对弥散中微子背景的总贡献。
英文摘要
Little Red Dots (LRDs) are compact, high-redshift sources whose physical nature remains uncertain. Their optical spectra bear many similarities to Type IIn supernovae (SNe IIn), motivating a scenario in which their emission is powered by shocks interacting with dense surrounding material. We investigate whether such interactions can power LRDs and contribute to the diffuse high-energy neutrino intensity measured by IceCube. In our simplified model, a fast central-engine outflow drives a shock through dense surrounding material before stalling near the LRD photosphere, while some material continues to flow through the shock. We explore parameter ranges motivated by SNe IIn and the observed and inferred properties of LRDs, finding solutions with shock luminosities from 2.2e43 to 3.5e44 erg/s. Using an analytical framework for cosmic-ray acceleration and hadronic interactions in dense shock environments, we calculate the resulting high-energy neutrino emission and integrate it over the cosmological LRD population. For our fiducial SNe IIn-based cosmic-ray parameters, the average predicted contribution below 2e5 GeV increases from about 0.2% for the lowest-luminosity quintile to about 2% for the highest-luminosity quintile, while an illustrative higher-efficiency case reaches about 13% of the IceCube diffuse neutrino intensity. The incompleteness of the current LRD census and uncertainties in their physical nature limit constraints on the cosmic-ray parameters and the distribution of L_s. Larger LRD samples, together with improved physical models and a full population-synthesis study, will be required to constrain the total LRD contribution to the diffuse neutrino background.
