Merger Hydrodynamics of the Luminous Cluster RXJ1347.5-1145
  We present an analysis of the complex gas hydrodynamics in the X-ray luminous
galaxy cluster RXJ1347.5-1145 caught in the act of merging with a subcluster to
its southeast using a combined $186$ ks Chandra exposure, $2.5$ times greater
than previous analyses. The primary cluster hosts a sloshing cold front spiral
traced by four surface brightness edges $5.^{\prime \prime}85^{+0.04}_{-0.03}$
west, $7.^{\prime \prime}10^{+0.07}_{-0.03}$ southeast, $11.^{\prime
\prime}5^{+1.3}_{-1.2}$ east, and $16.^{\prime \prime}7^{+0.3}_{-0.5}$
northeast from the primary central dominant galaxy, suggesting the merger is in
the plane of the sky. We measure temperature and density ratios across these
edges, confirming they are sloshing cold fronts. We observe the eastern edge of
the subcluster infall shock, confirming the observed subcluster is traveling
from the southwest to the northeast in a clockwise orbit. We measure a shock
density contrast of $1.38^{+0.16}_{-0.15}$ and infer a Mach number
$1.25\pm0.08$ and a shock velocity of $2810^{+210}_{-240}$ km s$^{-1}$.
Temperature and entropy maps show cool, low entropy gas trailing the subcluster
in a southwestern tail, consistent with core shredding. Simulations suggest a
perturber in the plane of the sky on a clockwise orbit would produce a sloshing
spiral winding counterclockwise, opposite to that observed. The most compelling
solution to this discrepancy is that the observed southeastern subcluster is on
its first passage, shock heating gas during its clockwise infall, while the
main cluster's clockwise cold front spiral formed from earlier encounters with
a second perturber orbiting counterclockwise.
