论文标题
老板大壁超级克鲁斯特斯的高密度核心的演变
The evolution of high-density cores of the BOSS Great Wall superclusters
论文作者
论文摘要
嵌入丰富的星系群和星系组的星系超级集体的高密度核心（HDC）是在宇宙网络中形成的最早的大物体，也是当前或将来可能崩溃的最大物体。我们研究了Redshift $ Z \ of Boss长城（BGW）超级集体中HDC的动态状态和可能的演变，以了解宇宙中结构的增长和演变。我们在广泛的红移中得出了球形塌陷模型的密度对比度值，并使用这些值来研究BGW超级clus子的HDC的动态状态和可能的演变。 HDC的质量是使用其中的星系恒星质量计算的。我们发现了HDCS中周转和未来崩溃区域的质量和半径，并将其与当地超级群体的群体进行了比较。我们确定了BGW超级克鲁斯特人中的八个HDC。其周转区域的质量在$ m _ {\ mathrm {t}} \大约0.4-3.3 \ 3.3 \ times〜10^{15} h^{ - 1} m_ \ odot，$和radii，$ r _和radii的范围为$ r _ {\ mathrm {\ mathrm {t} $ {\ 3.5--7 heb of $ r _ {他们未来崩溃区域的半径在$ r _ {\ mathrm {fc}}} \左右的范围内\ of 4-8H^{ - 1} $ mpc。超级集体中各个内核之间的距离要大得多：$ 25-35H^{ - 1} $ mpc的顺序。 HDC的丰富度和大小与当地宇宙中最富有的超级群体的HDC相媲美。 BGW超级推动者可能会演变为几个较贫穷的超级克鲁斯群岛，其质量类似于当地超级克鲁斯特人。这可能会削弱$λ$ CDM模型的张力，该模型不会预测我们当地宇宙社区中大量非常丰富和大型超级群体的张力，并解释了为什么没有像本地宇宙中BGW那样伸长的超级集体器。
High-density cores (HDCs) of galaxy superclusters that embed rich clusters and groups of galaxies are the earliest large objects to form in the cosmic web, and the largest objects that may collapse in the present or future. We study the dynamical state and possible evolution of the HDCs in the BOSS Great Wall (BGW) superclusters at redshift $z \approx 0.5$ in order to understand the growth and evolution of structures in the Universe. We derived the density contrast values for the spherical collapse model in a wide range of redshifts and used these values to study the dynamical state and possible evolution of the HDCs of the BGW superclusters. The masses of the HDCs were calculated using stellar masses of galaxies in them. We found the masses and radii of the turnaround and future collapse regions in the HDCs and compared them with those of local superclusters. We determined eight HDCs in the BGW superclusters. The masses of their turnaround regions are in the range of $M_{\mathrm{T}} \approx 0.4 - 3.3\times~10^{15}h^{-1}M_\odot,$ and radii are in the range of $R_{\mathrm{T}} \approx 3.5 - 7 h^{-1}$Mpc. The radii of their future collapse regions are in the range of $R_{\mathrm{FC}} \approx 4 - 8h^{-1}$Mpc. Distances between individual cores in superclusters are much larger: of the order of $25 - 35h^{-1}$Mpc. The richness and sizes of the HDCs are comparable with those of the HDCs of the richest superclusters in the local Universe. The BGW superclusters will probably evolve to several poorer superclusters with masses similar to those of the local superclusters. This may weaken the tension with the $Λ$CDM model, which does not predict a large number of very rich and large superclusters in our local cosmic neighbourhood, and explains why there are no superclusters as elongated as those in the BGW in the local Universe.
