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We report results from a   Chandra   study of the central regions of the nearby, X‐ray bright, Ophiuchus Cluster (  z = 0.03 ), the second‐brightest cluster in the sky. Our study reveals a dramatic, close‐up view of the stripping and potential destruction of a cool core within a rich cluster. The X‐ray emission from the Ophiuchus Cluster core exhibits a comet‐like morphology extending to the north, driven by merging activity, indicative of ram‐pressure stripping caused by rapid motion through the ambient cluster gas. A cold front at the southern edge implies a velocity of  1000 ± 200 km s −1   (  M ∼ 0.6 ). The X‐ray emission from the cluster core is sharply peaked. As previously noted, the peak is offset by 4 arcsec (∼2 kpc) from the optical centre of the associated cD galaxy, indicating that ram pressure has slowed the core, allowing the relatively collisionless stars and dark matter to carry on ahead. The cluster exhibits the strongest central temperature gradient of any massive cluster observed to date: the temperature rises from 0.7 keV within 1 kpc of the brightness peak to 10 keV by 30 kpc. A strong metallicity gradient is also observed within the same region. This supports a picture in which the outer parts of the cool core have been stripped by ram pressure due to its rapid motion. The cooling time of the innermost gas is very short,  ∼5 × 10 7  yr . Within the central 10 kpc radius, multiple small‐scale fronts and a complex thermodynamic structure are observed, indicating significant motions. These may be excited by the separation of the X‐ray peak from the cD galaxy and its associated dark matter potential. Beyond the central 50 kpc, and out to a radius of ∼150 kpc, the cluster appears relatively isothermal and has near constant metallicity. The exception is a large, coherent ridge of enhanced metallicity observed to trail the cool core and which is likely to have been stripped from it.

Ram‐pressure stripping of the cool core of the Ophiuchus Cluster