来自$0.1 < z < 0.5$的XCS-HSC星系团团内光的增长
The Growth of Intracluster Light in XCS-HSC Galaxy Clusters from $0.1 < z < 0.5$
摘要：
我们估计内集群光（ICL）组件的样本中检测到的18个集群XMM集群调查（XCS）数据使用深（$\sim$ 26.8 mag）超级超级凸轮斯巴鲁战略计划DR 1（HSC SSP DR 1）$i$波段数据。我们应用一个休息帧$μ_{B} = 25 \ \mathrm{mag/arcsec^{2}}$等照度阈值，我们定义为ICL以下的$R_{X,500}$（X射线估计$R_{500}$）的光圈集中在Brilliant集群星系（BCG）的光。经过仔细的掩蔽和校正后，从背景扣除通量损失，我们恢复$\sim$ 20%的ICL通量，大约四倍于我们的估计，在相同的等照度水平（$\sim$ 5%）的典型背景。我们发现，ICL约占总星团恒星质量的$\sim$ 24%的平均值（$\sim$ 41%，包括50 kpc内的BCG中包含的通量）;这个值与其他观测研究和半解析/数值模拟相匹配，但显着小于最近的流体动力学模拟结果（即使在观测一致的方式测量）。我们没有发现任何证据的ICL通量与集群质量之间的任何联系，但发现一个增长率的$2-4$的ICL之间的$0.1 < z < 0.5$。我们的结论是，ICL是从$z \sim 1$的星团恒星质量的主要演化组成部分。我们的工作强调了在测量ICL时需要一种一致的方法，同时需要更深的成像，以便在尽可能宽的红移范围内明确地测量ICL（例如，来自Vera C. Rubin Observatory）。
英文摘要：
We estimate the Intracluster Light (ICL) component within a sample of 18 clusters detected in XMM Cluster Survey (XCS) data using deep ($\sim$ 26.8 mag) Hyper Suprime Cam Subaru Strategic Program DR1 (HSC-SSP DR1) $i$-band data. We apply a rest-frame $μ_{B} = 25 \ \mathrm{mag/arcsec^{2}}$ isophotal threshold to our clusters, below which we define light as the ICL within an aperture of $R_{X,500}$ (X-ray estimate of $R_{500}$) centered on the Brightest Cluster Galaxy (BCG). After applying careful masking and corrections for flux losses from background subtraction, we recover $\sim$20% of the ICL flux, approximately four times our estimate of the typical background at the same isophotal level ($\sim$ 5%). We find that the ICL makes up about $\sim$ 24% of the total cluster stellar mass on average ($\sim$ 41% including the flux contained in the BCG within 50 kpc); this value is well-matched with other observational studies and semi-analytic/numerical simulations, but is significantly smaller than results from recent hydrodynamical simulations (even when measured in an observationally consistent way). We find no evidence for any links between the amount of ICL flux with cluster mass, but find a growth rate of $2-4$ for the ICL between $0.1 < z < 0.5$. We conclude that the ICL is the dominant evolutionary component of stellar mass in clusters from $z \sim 1$. Our work highlights the need for a consistent approach when measuring ICL alongside the need for deeper imaging, in order to unambiguously measure the ICL across as broad a redshift range as possible (e.g. 10-year stacked imaging from the Vera C. Rubin Observatory).
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