The Complex X‐Ray Morphology of NGC 7618: A Major Group‐Group Merger in the Local Universe?

We present results from a short Chandra ACIS-S observation of NGC 7618, the dominant central galaxy of a nearby ( z = 0.017309, d = 74.1 Mpc) group. We detect a sharp surface brightness discontinuity 14.4 kpc north of the nucleus subtending an angle of 130° with an X-ray tail extending ~70 kpc in the opposite direction. The temperature of the gas inside and outside the discontinuity is 0.79 ± 0.03 and 0.81 ± 0.07 keV, respectively. There is marginal evidence for a discontinuous change in the elemental abundance ( Z inner = 0.65 ± 0.25, Z outer = 0.17 ± 0.21 at 90% confidence), suggesting that this may be an "abundance" front. Fitting a two-temperature model to the ASCA GIS spectrum of the NGC 7618/UGC 12491 pair shows the presence of a second, much hotter ( T =~ 2.3 keV) component. We consider several scenarios for the origin of the edge and the tail, including a radio lobe/IGM interaction, nonhydrostatic "sloshing," equal-mass merger and collision, and ram pressure stripping. In the last case, we consider the possibility that NGC 7618 is falling into UGC 12491 or that both groups are falling into a gas-poor cluster potential. There are significant problems with the first two models, however, and we conclude that the discontinuity and tail are most likely the result of ram pressure stripping of the NGC 7618 group, as it falls into a larger dark matter potential.