  We analyzed the Suzaku data of M86 and its adjacent regions to study the
extended emission around it. The M86 core, the plume, and the tail extending
toward the northwest were clearly detected, as well as the extended halo around
them. From the position angle $\sim45\deg$ to $\sim275\deg$, the surface
brightness distribution of the core and the extended halo was represented
relatively well with a single $\beta$-model of $\beta\sim0.5$ up to 15'-20'.
The X-ray spectra of the core was represented with a two-temperature model of
$kT\sim 0.9$ keV and $\sim0.6$ keV. The temperatures of the core and the halo
have a positive gradient in the center, and reach the maximum of $kT\sim1.0$
keV at $r\sim7'$, indicating that the halo gas is located in a larger scale
potential structure than that of the galaxy. The temperatures of the plume and
the tail were $0.86\pm0.01$ keV and $1.00\pm0.01$ keV. We succeeded in
determining the abundances of $\alpha$-element separately, for the core, the
plume, the tail, and the halo for the first time. Abundance ratios with respect
to Fe were consistent with the solar ratios everywhere, except for Ne. The
abundance of Fe was $\sim0.7$ in the core and in the plume, while that in the
tail was $\sim1.0$, but the difference was not significant considering the
uncertainties of the ICM. The abundance of the halo was almost the same up to
$r\sim10'$, and then it becomes significantly smaller (0.2-0.3) at
$r\gtrsim10'$, indicating the gas with low metal abundance still remains in the
outer halo. From the surface brightness distribution, we estimated the gas mass
($\sim3\times10^{10}M_\odot$) and the dynamical mass
($\sim3\times10^{12}M_\odot$) in $r<100$~kpc. The gas mass to the dynamical
mass ratio was $10^{-3}$-$10^{-2}$, suggesting a significant fraction of the
halo gas has been stripped.
