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首页> 外文期刊>The Astrophysical journal >STRAINTS ON PRIMORDIAL NON-GAUSSINIY FROM THE HIGH-REDSHIFT CLUSTER MS 1054-03
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STRAINTS ON PRIMORDIAL NON-GAUSSINIY FROM THE HIGH-REDSHIFT CLUSTER MS 1054-03

机译：从高重复率群集MS 1054-03的主要非高斯INI应变

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The implications of the massive, X-ray selected cluster of galaxies MS 1054--03 at z = 0.83 are dis- cussed in light of the hypothesis that the primordial density fluctuations may be non-Gaussian. We gen- eralize the Press-Schechter (PS) formalism to the non-Gaussian case and calculate the likelihood that a cluster as massive as MS 1054 would have been found in the Einstein Medium Sensitvity Survey (EMSS). A flat universe (Ω_M + Ω_Λ = 1) is assumed, and the mass fluctuation amplitude is normalized to the present-day cluster abundance. The probability of finding an MS 1054-like cluster then depends only on Ω_M and the extent of primordial non-Gaussianity. We quantify the latter by adopting a specific func- tional form for the probability distribution function (PDF), denoted Ψ_λ, which tends to Gaussianity for λ 1 but is significantly non-Gaussian for λ≈＜ 10, and show how k is related to the more familiar sta- tistic T, the probability of ≥ 3 σ fluctuations for a given PDF relative to a Gaussian. Special attention is given to a careful calculation of the virial mass of MS 1054 from the available X-ray temperature, galaxy velocity, and weak-lensing data. We find that Gaussian initial density fluctuations are consistent with the data on MS 1054 only if Ω_M ≈＜ 0.2. For Ω_M ≥ 0.25 a significant degree of non-Gaussianity is required, unless the mass of MS 1054 has been substantially overestimated by X-ray and weak-lensing data. The required amount of non- Gaussianity is a rapidly increasing function of Ω_M for 0.25 ≤ Ω_M ≤ 0.45, with λ ≤ 1 (T ≈＞ 7) at the upper end of this range. For a fiducial Ω_M = 0.3, Ω_Λ = 0.7 universe, favored by several lines of evidence we obtain an upper limit λ≤ 10, corresponding to a T ≥ 3. This finding is consistent with the conclusions of Koyama, Soda, & Taruya, who applied the generalized PS formalism to low (z ≈＜ 0.1＝ and interme- diate (z ≈＜ 0.6＝ redshift cluster data sets.
机译：根据原始密度波动可能是非高斯的假设，讨论了在z = 0.83时由大量X射线选择的星系MS 1054--03的含义。我们将Press-Schechter（PS）形式主义一般化为非高斯情况，并计算出在爱因斯坦中等敏感度调查（EMSS）中会发现像MS 1054一样大的星团的可能性。假设一个平坦的宇宙（Ω_M+Ω_Λ= 1），并且将质量波动幅度标准化为当前的簇丰度。然后，找到类似MS 1054的簇的概率仅取决于Ω_M和原始非高斯性的程度。我们通过对概率分布函数（PDF）采用特定的函数形式来量化后者，表示为Ψ_λ，对于λ 1趋于高斯性，而对于λ≈＜10则明显非高斯性，并证明k是与更熟悉的统计量T有关，给定PDF相对于高斯的波动≥3σ的概率。要特别注意根据可用的X射线温度，星系速度和弱透镜数据仔细计算MS 1054的病毒质量。我们发现，只有当Ω_M≈＜0.2时，高斯初始密度波动才与MS 1054上的数据一致。对于Ω_M≥0.25，除非X射线和弱透镜数据大大高估了MS 1054的质量，否则就需要很大程度的非高斯性。对于0.25≤Ω_M≤0.45，所需的非高斯量是Ω_M的快速增加函数，而λ≤1（T≈＞ 7）在该范围的上限。对于基准Ω_M= 0.3，Ω_Λ= 0.7宇宙，受多条证据支持的情况，我们获得了λ≤10的上限，对应于T≥3。这一发现与Koyama，Soda和Taruya的结论一致。将广义PS形式主义应用于低（z≈＜0.1 ＝和中间（z≈＜0.6 ＝红移聚类数据集）。

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