演講資訊

摘要：

In this talk, I will introduce a new concept of identifying cosmic voids by adopting a void-cluster correspondence model that voids are the counterpart of massive clusters. To prove this concept we use a pair of LCDM simulations, a reference and its initial density-inverted mirror simulation, and study the relation between the effective size of voids and the mass of corresponding clusters. We find a power-law scaling relation between the void size and the corresponding cluster mass. We also find that the density profile of the identified voids follows a universal functional form. In the later part of the talk, I will show how one can identify these cluster-counterpart voids directly from the matter/galaxy density field without their counterpart information. The completeness and reliability we achieve in recovering cluster-counterpart voids are about 70-74 % from matter density fields and 60-67% from galaxy density fields depending on the mass scales of the voids. Our results demonstrate that we can apply this method to the galaxy redshift survey data to identify cosmic voids corresponding statistically to the galaxy clusters in a given mass range.