标题： 通过太阳泽尔多维奇效应以模型无关的方式打破重子物质与暗物质的退耦合 显示英文标题

标题： Breaking the baryon-dark matter degeneracy in a model-independent way through the Sunyaev-Zeldovich effect

摘要： 我们提出了一种模型无关的\textit{贝塞尔参数插值}方法，利用中间红移数据来缓解重子物质和暗物质丰度之间的退化问题。 为此，我们首先插值观测的哈勃数据以提取关于（归一化的）哈勃常数$h_0$的宇宙限制，并插值星系团的角直径距离$D(z)$，这些距离是通过太阳跃迁-泽尔多维奇效应推断出来的，以约束空间曲率$\Omega_k$。 通过这样确定的哈勃点和$D(z)$，我们对限制重子的声波振荡（重子密度$\omega_b = h^2_0\Omega_b$和总物质密度$\omega_m = h^2_0\Omega_m$）的未相关数据进行插值，用相同的技术加强了对$h_0$和$\Omega_k$的限制。 我们没有采用通常通过宇宙微波背景得到的值来固定$\omega_b$以消除物质部门的退化，而是从相关的重子声波振荡中插值声学参数。 我们的Monte Carlo–马尔可夫链模拟结果表明，在$1$–$\sigma$的置信水平上与平坦的$\Lambda$CDM模型一致。 虽然我们的发现也大致适合它的非平坦扩展模型，在$1$–$\sigma$的范围内，但哈勃常数似乎在$2$–$\sigma$的置信水平上存在张力。 因此，我们还用我们的方法重新分析了哈勃张力，发现我们的预期稍微符合局部限制。 显示英文摘要

摘要： We propose a model-independent \textit{B\'ezier parametric interpolation} to alleviate the degeneracy between baryonic and dark matter abundances by means of intermediate-redshift data. To do so, we first interpolate the observational Hubble data to extract cosmic bounds over the (reduced) Hubble constant, $h_0$, and interpolate the angular diameter distances, $D(z)$, of the galaxy clusters, inferred from the Sunyaev-Zeldovich effect, constraining the spatial curvature, $\Omega_k$. Through the so-determined Hubble points and $D(z)$, we interpolate uncorrelated data of baryonic acoustic oscillations bounding the baryon ($\omega_b = h^2_0\Omega_b$) and total matter ($\omega_m = h^2_0\Omega_m$) densities, reinforcing the constraints on $h_0$ and $\Omega_k$ with the same technique. Instead of pursuing the usual treatment to fix $\omega_b$ via the value obtained from the cosmic microwave background to remove the matter sector degeneracy, we here interpolate the acoustic parameter from correlated baryonic acoustic oscillations. The results of our Monte Carlo--Markov chain simulations turn out to agree at $1$--$\sigma$ confidence level with the flat $\Lambda$CDM model. While our findings are roughly suitable at $1$--$\sigma$ with its non-flat extension too, the Hubble constant appears in tension up to the $2$--$\sigma$ confidence level. Accordingly, we also reanalyze the Hubble tension with our treatment and find our expectations slightly match local constraints.