Abstract
AbstractA proto-cluster core is the most massive dark matter halo (DMH) in a given proto-cluster. To reveal the galaxy formation in core regions, we search for proto-cluster cores at z ˜ 2 in ˜1.5deg2 of the COSMOS field. Using pairs of massive galaxies (log (M*/Mʘ) ≥ 11) as tracers of cores, we find 75 candidate cores. A clustering analysis and the extended Press-Schechter model show that their descendant mass at z = 0 is consistent with Fornax-like or Virgo-like clusters. Moreover, using the IllustrisTNG simulation, we confirm that pairs of massive galaxies are good tracers of DMHs massive enough to be regarded as proto-cluster cores. We then derive the stellar mass function and the quiescent fraction for member galaxies of the 75 candidate cores. We find that stellar mass assembly and quenching are accelerated as early as z ˜ 2 in proto-cluster cores.
Highlights
The most massive and largest dark matter haloes (DMHs) in today’s universe are called galaxy clusters
A theoretical study has studied galaxy evolution in proto-clusters (Muldrew et al 2018). They have found that galaxies in core regions have different properties from those in fields and the rest of the proto-cluster regions: a more top-heavy stellar mass function, a higher fraction of quiescent galaxies
× 1013 M We regard at z ∼ 2 typically evolves into DMHs with >∼ 2−3 × 1013 M
Summary
The most massive and largest dark matter haloes (DMHs) in today’s universe are called galaxy clusters. A proto-cluster typically extends to more than 20 comoving Mpc at z ∼ 2, being split into a number of DMHs and unbound regions. Among those substructures, we define the “core” of the protocluster as the most massive DMH. A theoretical study has studied galaxy evolution in proto-clusters (Muldrew et al 2018). They have found that galaxies in core regions have different properties from those in fields and the rest of the proto-cluster regions: a more top-heavy stellar mass function, a higher fraction of quiescent galaxies. We use a “pair” of massive galaxies (M∗ 1011 M ) as a tracer of cores
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