The Double Galaxy Cluster Abell 2465 III. X-ray and Weak-lensing
  Observations
  We report Chandra X-ray observations and optical weak-lensing measurements
from Subaru/Suprime-Cam images of the double galaxy cluster Abell 2465
(z=0.245). The X-ray brightness data are fit to a beta-model to obtain the
radial gas density profiles of the northeast (NE) and southwest (SW)
sub-components, which are seen to differ in structure. We determine core radii,
central temperatures, the gas masses within $r_{500c}$, and the total masses
for the broader NE and sharper SW components assuming hydrostatic equilibrium.
The central entropy of the NE clump is about two times higher than the SW.
Along with its structural properties, this suggests that it has undergone
merging on its own. The weak-lensing analysis gives virial masses for each
substructure, which compare well with earlier dynamical results. The derived
outer mass contours of the SW sub-component from weak lensing are more
irregular and extended than those of the NE. Although there is a weak
enhancement and small offsets between X-ray gas and mass centers from weak
lensing, the lack of large amounts of gas between the two sub-clusters
indicates that Abell 2465 is in a pre-merger state. A dynamical model that is
consistent with the observed cluster data, based on the FLASH program and the
radial infall model, is constructed, where the subclusters currently separated
by ~1.2Mpc are approaching each other at ~2000km/s and will meet in ~0.4Gyr.
