  Cosmological simulations of structure formation predict that galaxy clusters
continue to grow and evolve through ongoing mergers with group-scale systems.
During these merging events, the ram pressure applied by the intracluster
medium acts to strip the gas from the infalling groups, forming large tails of
stripped gas, which eventually become part of the main cluster. In this work,
we present a detailed analysis of our new deep Chandra observations of the NGC
4839 group falling into the nearby Coma cluster, providing a unique opportunity
to explore the way galaxy clusters in the local universe continue to grow. Our
analysis reveals a cold front feature at the leading head of the group,
preceded by a bow shock of hot gas in front with a Mach number of $\sim\! 1.5$.
The power spectrum of surface brightness fluctuations in the tail shows that
the slope gets less steep as the distance from the leading head increases,
changing from $-2.35_{-0.06}^{+0.07}$ at the inner part of the tail to
$-1.37_{-0.07}^{+0.09}$ at the outermost part of the tail. These values are
shallower than the slope of the Kolmogorov 2D power spectrum, indicating that
thermal conduction is being suppressed throughout the tail, enabling long-lived
small-scale turbulence, which would typically be washed out if thermal
conduction was not inhibited. The characteristic amplitude of surface
brightness fluctuations in the tail suggests a mild level of turbulence with a
Mach number in the range of 0.1-0.5, agreeing with that found for the infalling
group in Abell 2142.
