AI 中文总结
该研究利用tSZ×FRB互相关的BP框架，打破反馈效率与非热压力支撑的简并，约束星系团气体性质，为流体静力学质量偏差及星系团宇宙学推断提供关键依据。
AI 中文摘要
标准观测探针缺乏表征星系群和星系团中反馈驱动气体抛射与非热压力支撑之间相互作用的灵敏度，现有模型也缺乏分解这种相互作用的框架。近期对tSZ×FRB互功率谱的首次探测（Takahashi等人，2025；Sharma等人，2026）被解读为对AGN反馈和σ₈的约束，但所用重子模型未对非热压力支撑进行独立参数化，导致反馈效率与气体热力学性质简并。我们证明，该互相关对星系团气体的热结构和非热结构具有灵敏度，这是两种单独的可观测量都无法实现的，因为tSZ效应示踪电子压力，而FRB仅示踪电子密度。利用Baryon Pasting（BP）框架，该框架分别对反馈效率ε_f和非热压力振幅A_nt进行参数化，我们表明它们的联合约束可打破这种简并。在无噪声极限下，添加互功率谱将r_cond从0.96降至0.08（降低12倍），并将联合品质因数提高19倍，约束能力集中在星系团内部尺度（ℓ≳3000）。近期的探测与我们的基准模型一致，且不支持弱反馈（不同数据集下ε_f的95%置信区间下限为2.40×10⁻⁶至3.67×10⁻⁶）。结合DSA-2000的5×10⁴个FRB与SO，我们预测A_nt的分数精度为3.8%，若结合CMB-HD则提升至2.3%。这些约束直接为流体静力学质量偏差提供信息，对基于eROSITA、SO和CMB-HD的星系团宇宙学推断具有直接意义。
英文摘要
Standard observational probes lack the sensitivity to characterize the interplay between feedback-driven gas ejection and non-thermal pressure support in groups and clusters, and current models lack the framework to disentangle it. Recent first detections of the tSZ$\times$FRB cross-power spectrum (Takahashi et al, 2025; Sharma et al 2026) have been interpreted as constraining AGN feedback and $σ_8$, but the baryon models used do not independently parameterize non-thermal pressure support, leaving feedback efficiency and gas thermodynamics degenerate. We demonstrate that this cross-correlation provides sensitivity to the thermal and non-thermal structure of cluster gas that neither observable alone can achieve, because the tSZ effect traces electron pressure while FRBs trace solely electron density. Using the Baryon Pasting (BP) framework, which separately parameterizes feedback efficiency $ε_f$ and non-thermal pressure amplitude $A_{\rm nt}$, we show that their joint constraint breaks this degeneracy. In the noise-free limit, adding the cross-power spectrum reduces $r_{\rm cond}$ from $0.96$ to $0.08$ (a 12-fold reduction) and improves the joint figure of merit by a factor of 19, with the constraining power concentrated at cluster interior scales ($\ell \gtrsim 3000$). Recent detections are consistent with our fiducial model and disfavor weak feedback ($ε_f^{95\%} \gtrsim 2.40\text{--}3.67 \times 10^{-6}$ across datasets). With $5\times10^4$ FRBs from DSA-2000 combined with SO, we forecast $3.8\%$ fractional precision on $A_{\rm nt}$, improving to $2.3\%$ with CMB-HD. These constraints directly inform the hydrostatic mass bias, with immediate implications for cluster-based cosmological inference from eROSITA, SO, and CMB-HD.
Comments17 pages, 6 figures, submitted to ApJ
