论文标题
VST Atlas Galaxy群集目录I：集群检测和质量校准
VST ATLAS Galaxy Cluster Catalogue I: cluster detection and mass calibration
论文作者
论文摘要
利用VST Atlas调查提供的南部天空的$ \ SIM4700 $ deg $^2 $光学覆盖范围，我们使用{\ sc orca}群集检测算法构建了一个新的光学选择星系组和簇的目录。该目录包含$ \ sim 22,000 $检测，带有$ n_ {200}> 10 $和$ \ sim9,000 $，带有$ n_ {200}> 20 $。我们使用机器学习估算簇的光度红移，并找到样品的红移分布以扩展到$ z \ sim0.7 $，峰值达到$ z \ sim0.25 $。我们使用MCXC，Planck，ACT DR5和SDSS Redmapper群集样品的质量来校准Atlas群集质量缩放量表。我们估计，Atlas样本为$> 95 \％$完整，$> 85 \％$ pure at $ z <0.35 $，在$ m _ {\ rm rm> 200m} $> $> $ 1 \ times10^{14} h^{-1}在$ z <0.35 $时，我们还发现Atlas样本比Redmapper更完整，恢复了Abell簇的$ \ sim40 \％$ $。与其他群集样本的质量功能相比，这种较高的样本完整性使$ z <0.35 $ Atlas群集质量函数更接近具有基于Planck CMB分析的参数的$λ$ CDM模型的预测。但是，观察到的地图集质量功能和模型之间的强烈紧张局势仍然存在。我们将对论文II中的地图集群集质量功能进行详细的宇宙学分析。将来，可以使用ATLAS样本来识别与X射线检测的Erosita簇的光学对应物。该目录还非常适合于4个辅助光谱目标选择。 Atlas群集目录可在http://astro.dur.ac.uk/cosmology/vstatlas/cluster_catalogue/上公开获得。
Taking advantage of $\sim4700$ deg$^2$ optical coverage of the Southern sky offered by the VST ATLAS survey, we construct a new catalogue of photometrically selected galaxy groups and clusters using the {\sc orca} cluster detection algorithm. The catalogue contains $\sim 22,000$ detections with $N_{200}>10$ and $\sim9,000$ with $N_{200}>20$. We estimate the photometric redshifts of the clusters using machine learning and find the redshift distribution of the sample to extend to $z\sim0.7$, peaking at $z\sim0.25$. We calibrate the ATLAS cluster mass-richness scaling relation using masses from the MCXC, Planck, ACT DR5 and SDSS redMaPPer cluster samples. We estimate the ATLAS sample to be $>95\%$ complete and $>85\%$ pure at $z<0.35$ and in the $M_{\rm 200m}$>$1\times10^{14}h^{-1}{\rm M}_\odot$ mass range. At $z<0.35$, we also find the ATLAS sample to be more complete than redMaPPer, recovering a $\sim40\%$ higher fraction of Abell clusters. This higher sample completeness places the amplitude of the $z<0.35$ ATLAS cluster mass function closer to the predictions of a $Λ$CDM model with parameters based on the Planck CMB analyses, compared to the mass functions of the other cluster samples. However, strong tensions between the observed ATLAS mass functions and models remain. We shall present a detailed cosmological analysis of the ATLAS cluster mass functions in paper II. In the future, optical counterparts to X-ray-detected eROSITA clusters can be identified using the ATLAS sample. The catalogue is also well suited for auxiliary spectroscopic target selection in 4MOST. The ATLAS cluster catalogue is publicly available at http://astro.dur.ac.uk/cosmology/vstatlas/cluster_catalogue/.
