Cosmology with galaxy cluster phase spaces
Cosmology with galaxy cluster phase spaces
复制标题
星系团相空间的宇宙学
DOI：
10.1103/physrevd.96.023543
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发表时间：
2016
影响因子：
5
通讯作者：
D. Huterer
中科院分区：
文献类型：
--
作者：
Alejo Stark;C. Miller;D. Huterer
我们提出了一种用星系团相空间约束加速宇宙学的新方法。利用Fisher矩阵形式，我们预测了描述宇宙膨胀历史的宇宙学参数的约束条件。我们发现，我们的探测器有可能提供与其他宇宙探测器相当甚至更强的约束条件。更具体地说，有1000（100）个星团均匀分布在红移范围内 $ 0 \leq z \leq 0.8$，在应用了保守疗法后 $80\%$ 我们预测，在每个聚类上的先验质量分散和在所有其他参数上的边际化 $1\sigma$ 暗能量状态方程的约束 $w$ 物质密度参数 $\Omega_M$ 的 $\sigma_w = 0.138 (0.431)$ 和 $\sigma_{\Omega_M} = 0.007 (0.025)$ 在一个平坦的宇宙中。假设40％的质量散射并在哈勃常数上加入先验，我们可以对暗能量状态参数方程的CPL参数化进行约束 $w_0$ 和 $w_a$ 有100个星团在相同的红移范围内： $\sigma_{w_0} = 0.191 $ 和 $\sigma_{w_a} = 2.712$． 放弃平面假设，假设 $w=-1$ 我们还获得了物质和暗能量密度参数的竞争约束： $\sigma_{\Omega_M} = 0.101$ 和 $\sigma_{\Omega_{\Lambda}} = 0.197$ 对于100个均匀分布在范围内的集群 $ 0 \leq z \leq 0.8$ 在哈勃常数上加一个先验之后。我们还讨论了在近期和远期收紧约束的各种观测策略。
We present a novel approach to constrain accelerating cosmologies with galaxy cluster phase spaces. With the Fisher matrix formalism we forecast constraints on the cosmological parameters that describe the cosmological expansion history. We find that our probe has the potential of providing constraints comparable to, or even stronger than, those from other cosmological probes. More specifically, with 1000 (100) clusters uniformly distributed in the redshift range $ 0 \leq z \leq 0.8$, after applying a conservative $80\%$ mass scatter prior on each cluster and marginalizing over all other parameters, we forecast $1\sigma$ constraints on the dark energy equation of state $w$ and matter density parameter $\Omega_M$ of $\sigma_w = 0.138 (0.431)$ and $\sigma_{\Omega_M} = 0.007 (0.025)$ in a flat universe. Assuming 40\% mass scatter and adding a prior on the Hubble constant we can achieve a constraint on the CPL parametrization of the dark energy equation of state parameters $w_0$ and $w_a$ with 100 clusters in the same redshift range: $\sigma_{w_0} = 0.191 $ and $\sigma_{w_a} = 2.712$. Dropping the assumption of flatness and assuming $w=-1$ we also attain competitive constraints on the matter and dark energy density parameters: $\sigma_{\Omega_M} = 0.101$ and $\sigma_{\Omega_{\Lambda}} = 0.197$ for 100 clusters uniformly distributed in the range $ 0 \leq z \leq 0.8$ after applying a prior on the Hubble constant. We also discuss various observational strategies for tightening constraints in both the near and far future.