  We report $Suzaku$ X-ray observations of the dark subhalo associated with the
merging group of NGC 4839 in the Coma cluster. The X-ray image exhibits an
elongated tail toward the southwest. The X-ray peak shifts approximately $1'$
away from the weak-lensing mass center toward the opposite direction of the
Coma cluster center. We investigated the temperature, normalization, pressure,
and entropy distributions around the subhalo. Excluding the X-ray tail, the
temperature beyond the truncation radius is 8-10$~\rm keV$, which is two times
higher than that of the subhalo and the X-ray tail. The pressure is nearly
uniform excluding southern part of the subhalo at two times of the truncation
radius. We computed the gas mass within the truncation radius and the X-ray
tail. While the gas fraction within the truncation radius is about 5 times
smaller than that of regular groups, the gas mass in the subhalo and the X-ray
tail to weak-lensing mass ratio is consistent with that of regular groups.
Assuming the infall velocity, $2000~\rm km~s^{-1}$, the ram pressure is 1.4
times greater than gravitational force per unit area. Assuming the
Kelvin-Helmholtz instabilities, the total lost mass is approximately
$3\times10^{11}~M_{\odot}$. If this gas had originally been within the
truncation radius, the gas mass fraction of the subhalo would have been
comparable with those of regular groups before infalling to the Coma cluster.
