Revealing the Interaction between the X‐Ray Gas of Starburst Galaxy UGC 6697 and the Hot Intracluster Medium of A1367

We present the result from a CHANDRA observation of an X-ray luminousstarburst galaxy UGC 6697, which is embedded in the northwest hot region ofA1367 (5 - 6 keV). A very sharp X-ray edge (~ 13 times of surface brightnessjump) at the southeast and a long tail (at least 60 kpc from the nucleus) atthe northwest of the galaxy are detected, as expected if the galaxy is movingto the southeast. The X-ray edge, at the midway of the nucleus and thesoutheast optical disk edge, is also at the same position where the Halphaemission is truncated and a radio sharp edge is observed. The X-ray diffuseemission is also enhanced at the southeast, implying ram pressure compression.No extraplanar X-ray component is detected, probably due to the combiningeffects of weaker outflow activity than that in nuclear starbursts, andexternal confinement plus stripping. The diffuse thermal gas in UGC 6697 has atemperature of ~ 0.7 keV and a low iron abundance (~0.1 - 0.2 solar). An X-raypoint source (L (0.5-10 keV) ~ 2.8 x 10^{40} ergs s^{-1}) is detected on thenucleus, but not highly absorbed. Three off-center ultraluminous X-ray sources,all with L (0.5-10 keV) > 10^{40} ergs s^{-1}, are also detected. Based on themulti-wavelength data available, we favor that the interaction between theinterstellar medium (ISM) and the ICM plays a major role to trigger thestarburst in UGC 6697.