CHEX-MATE: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles
CHEX-MATE: Constraining the origin of the scatter in galaxy cluster radial X-ray surface brightness profiles
复制标题
CHEX-MATE：约束星系团径向 X 射线表面亮度剖面中的散射起源
DOI：
10.1051/0004-6361/202346189
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发表时间：
2023
影响因子：
6.5
通讯作者：
Bartalucci I
中科院分区：
文献类型：
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作者：
Bartalucci I
我们调查的统计特性和起源的CHEX-MATE样品，通过SZ效应选择118个星系团形成的空间分辨表面亮度分布内的散射。这些天体是从普朗克SZ星表中提取的，涵盖了很宽的质量范围，M500=[2 − 15]× 1014 M，红移z=[0.05，0.6]。 我们推导出表面亮度和发射测量配置文件，并确定了统计特性的完整的样品和子样品，根据其形态，质量和红移。我们发现，有一个临界尺度，R = 0.4R500，在此范围内，形态放松和干扰对象配置文件分歧。 在0.05R500下，每个子样本的中位数相差10倍。一旦应用适当的缩放，质量和红移选择的子样本之间没有显著差异。我们将CHEX-MATE与从THE THREE HUNDRED宇宙学模拟套件中抽取的115个星团样本进行比较。我们发现，模拟排放量的配置文件是系统比观测陡峭。这是第一次，模拟被用来打破组件造成的分布之间的分散。我们调查的行为的散射由于对象的对象的变化。我们发现，高散射，约110%，是由于在集群的核心气体的分布之间的真正差异。中间尺度，其特征在于在0.56的顺序上的散射的最小值，指示集群配置文件是最接近的自相似制度的区域。更大尺度的特征在于由于气体的复杂空间分布而增加散射。也是第一次，我们验证了由于投影效应的散射小于由于在所有考虑的尺度中真正的逐对象变化的散射。
We investigate the statistical properties and the origin of the scatter within the spatially resolved surface brightness profiles of the CHEX–MATE sample, formed by 118 galaxy clusters selected via the SZ effect. These objects have been drawn from thePlanckSZ catalogue and cover a wide range of masses,M500= [2 − 15]×1014M⊙, and redshift,z= [0.05, 0.6]. We derived the surface brightness and emission measure profiles and determined the statistical properties of the full sample and sub-samples according to their morphology, mass, and redshift. We found that there is a critical scale,R∼ 0.4R500, within which morphologically relaxed and disturbed object profiles diverge. The median of each sub-sample differs by a factor of ∼10 at 0.05R500. There are no significant differences between mass- and redshift-selected sub-samples once proper scaling is applied. We compare CHEX–MATE with a sample of 115 clusters drawn from the THE THREE HUNDRED suite of cosmological simulations. We found that simulated emission measure profiles are systematically steeper than those of observations. For the first time, the simulations were used to break down the components causing the scatter between the profiles. We investigated the behaviour of the scatter due to object-by-object variation. We found that the high scatter, approximately 110%, at is due to a genuine difference between the distribution of the gas in the core of the clusters. The intermediate scale, , is characterised by the minimum value of the scatter on the order of 0.56, indicating a region where cluster profiles are the closest to the self-similar regime. Larger scales are characterised by increasing scatter due to the complex spatial distribution of the gas. Also for the first time, we verify that the scatter due to projection effects is smaller than the scatter due to genuine object-by-object variation in all the considered scales.
影响因子：
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作者：
G. Tamburlini
通讯作者：
G. Tamburlini