We present results from a mosaic of nine Chandra observations of M86 and the surrounding field .
We detect three main diffuse components : the Virgo ICM at \sim 2.4 keV , the extended halo of M86 at \sim 1.2 keV , and the cooler central and stripped gas of M86 at \sim 0.8 keV .
The most striking feature is a long tail of emission , which consists of a plume \sim 4′north of M86 and two main extensions emanating from the plume .
Based on the morphology and temperature structure of the tail , we conclude that it is formed by ram pressure stripping of M86 as it falls into the Virgo cluster and interacts with the Virgo ICM , in agreement with earlier work .
The tail is 150 kpc in projection , and a simple estimate gives a lower limit on the true length of the tail of 380 kpc , making this the longest ram pressure stripped tail presently known .
The total gas mass in the plume ( \sim 7 \times 10 ^ { 8 } { M _ { \odot } } ) and tail ( \sim 1 \times 10 ^ { 9 } { M _ { \odot } } ) is about three times that in the core of M86 , which supports the scenario where most of the gas was stripped rapidly and recently .
The projected position of the plume can be understood if M86 has an aspherical potential , as suggested by optical isophotes .
Ram pressure stripping from an aspherical potential can also explain the split “ double tails ” seen in M86 and in other Virgo cluster galaxies in the field .
The large line-of-sight velocity of M86 ( 1550 km s ^ { -1 } with respect to M87 ) , its position relative to the Virgo cluster , and the orientation of the tail tightly constrain its orbital parameters .
The data are inconsistent with a radial orbit , and imply inner and outer turning radii of r _ { i } \approx 300 kpc and r _ { o } \gtrsim 8.8 Mpc , indicating that M86 is , at best , only weakly bound to the Virgo cluster .