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We present results from a deep (200 ks) Chandra observation of the early-typegalaxy NGC 4552 (M89) which is falling into the Virgo cluster. Previousshallower X-ray observations of this galaxy showed a remnant gas core, a tailto the South of the galaxy, and twin `horns' attached to the northern edge ofthe gas core [machacek05a]. In our deeper data, we detect a diffuse, lowsurface brightness extension to the previously known tail, and measure thetemperature structure within the tail. We combine the deep Chandra data witharchival XMM-Newton observations to put a strong upper limit on the diffuseemission of the tail out to a large distance (10$\times$the radius of theremnant core) from the galaxy center. In our two previous papers[roediger15a,roediger15b], we presented the results of hydrodynamicalsimulations of ram pressure stripping specifically for M89 falling into theVirgo cluster and investigated the effect of ICM viscosity. In this paper, wecompare our deep data with our specifically tailored simulations and concludethat the observed morphology of the stripped tail in NGC 4552 is most similarto the inviscid models. We conclude that, to the extent the transport processescan be simply modeled as a hydrodynamic viscosity, the ICM viscosity isnegligible. More generally, any micro-scale description of the transportprocesses in the high-$\beta$ plasma of the cluster ICM must be consistent withthe efficient mixing observed in the stripped tail on macroscopic scales.

Stripped elliptical galaxies as probes of ICM physics: III. Deep Chandra Observation of NGC 4552 - Measuring the Viscosity of the Intracluster Medium