用MUSTANG-2对Zwicky 3146的高分辨率Sunyaev-Zel'dovich效应观测进行压力分布和质量估算
Pressure profiles and mass estimates using high-resolution Sunyaev-Zel'dovich effect observations of Zwicky 3146 with MUSTANG-2
摘要：
Zwicky 3146星系团是$z=0.291$的一个晃动的冷核心星系团，在X射线成像中，它似乎没有在团内介质（ICM）中表现出显着的压力子结构。已发表的$M_{500}$值范围在$3.88^{+0.62}_{-0.58}$到$22.50 \pm 7.58 \times 10^{14}$ M $_{\odot}$之间，其中基于ICM的估计值与报告的误差$<20$ \%表明，我们应该期望找到介于$6.53^{+0.44}_{-0.44} \times 10^{14}$ M $_{\odot}$（来自普朗克，具有$8.4σ$检测）和$8.52^{+1.77}_{-1.47} \times 10^{14}$ M $_{\odot}$（来自ACT，具有$14σ$检测）之间的质量。这一广泛的质量范围表明，所有方法都有足够的改进空间。在这里，我们调查的能力，以估计Zwicky 3146的质量通过Sunyaev-Zel'dovich（SZ）效应与MUSTANG-2在90 GHz的噪声水平优于$15\ μ$ K在中心，和$104σ$的集群检测的数据。我们从我们的SZ数据，这是在很好的协议，来自X射线数据的压力分布。从我们的SZ导出的压力分布，我们推断$M_{500}$和$M_{2500}$通过三种方法- $Y$ - $M$标度关系，维里定理，和流体静力学平衡-其中我们采用X射线约束\emph{XMM-Newton}的电子密度分布时，假设流体静力学平衡。根据模型和估计方法，我们的$M_{500}$估计值范围从$6.23 \pm 0.59$到$10.6 \pm 0.95 \times 10^{14}$ M $_{\odot}$，其中我们根据流体静力平衡的估计值为$8.29^{+1.93}_{-1.24}$（$\pm 19.1$ \% stat）${}^{+0.74}_{-0.68}$（$\pm 8.6$ \% sys，校准）$\times 10^{14}$ M $_{\odot}$。从$Y$ - $M$关系导出的基准质量为$8.16^{+0.44}_{-0.54}$（$\pm 5.5$ \% stat）${}^{+0.46}_{-0.43}$（$\pm 5.5$ \% sys，$Y$ - $M$）${}^{+0.59}_{-0.55}$（$\pm 7.0$ \% sys，cal.）$\times 10^{14}$ M $_{\odot}$ .
英文摘要：
The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at $z=0.291$ that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published $M_{500}$ values range between $3.88^{+0.62}_{-0.58}$ to $22.50 \pm 7.58 \times 10^{14}$ M$_{\odot}$, where ICM-based estimates with reported errors $<20$\% suggest that we should expect to find a mass between $6.53^{+0.44}_{-0.44} \times 10^{14}$ M$_{\odot}$ (from Planck, with an $8.4σ$ detection) and $8.52^{+1.77}_{-1.47} \times 10^{14}$ M$_{\odot}$ (from ACT, with a $14σ$ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than $15\ μ$K at the center, and a cluster detection of $104σ$. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer $M_{500}$ and $M_{2500}$ via three methods -- $Y$-$M$ scaling relations, the virial theorem, and hydrostatic equilibrium -- where we employ X-ray constraints from \emph{XMM-Newton} on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our $M_{500}$ estimates range from $6.23 \pm 0.59$ to $10.6 \pm 0.95 \times 10^{14}$ M$_{\odot}$, where our estimate from hydrostatic equilibrium, is $8.29^{+1.93}_{-1.24}$ ($\pm 19.1$\% stat) ${}^{+0.74}_{-0.68}$ ($\pm 8.6$\% sys, calibration) $\times 10^{14}$ M$_{\odot}$. Our fiducial mass, derived from a $Y$-$M$ relation is $8.16^{+0.44}_{-0.54}$ ($\pm 5.5$\% stat) ${}^{+0.46}_{-0.43}$ ($\pm 5.5$\% sys, $Y$-$M$) ${}^{+0.59}_{-0.55}$ ($\pm 7.0$\% sys, cal.) $\times 10^{14}$ M$_{\odot}$.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
