  In the hierarchical evolution framework of cosmology, larger halos grow
through matter accretion and halo mergers. To clarify the halo evolution, we
need to define the halo mass and radius physically. However, the
pseudo-evolution problem makes the process difficult. Thus, we aim to measure
the splashback radius, a physically defined halo radius for a large number of
halos with various mass and redshift, and to determine the most important
parameters to affect it. We use the typical definition of splashback radius
(Rsp) as the radius with the steepest radial density profile. In this work, we
measure Rsp of dark matter halos within the mass of 1e13-3e15Msun and redshifts
spanning 0.08-0.65. This is the measurement of the Rsp in the largest range of
halo mass and redshift. Using the shear catalog of the DECaLS DR8, we
investigate Rsp of halos associated with galaxies and galaxy clusters
identified in the various catalogs. Our finding reveals a trend wherein massive
halos demonstrate a larger Rsp, and the normalized splashback radius
(Rsp/R200m) shows a U-shaped mass evolution. The upturn in these relations
mainly comes from the contribution of massive halos with low redshifts. We
further find Rsp increases with the peak height, while Rsp/R200m has a negative
relation with the peak height. We also find the Rsp >~R200m for most halos,
indicating their low accretion rates. Our result is consistent with previous
literature across a wide range of mass, redshift, and peak height, as well as
the simulation work from More et al. (2015).
