An image combining X-rays and optical light shows the scene of this collision. The impact between the dwarf galaxy and the spiral galaxy caused a shock wave — akin to a sonic boom on Earth — that generated hot gas with a temperature of about 6 million degrees. Chandra X-ray data, in purple, show the hot gas has a comet-like appearance caused by the motion of the dwarf galaxy. Optical data from the European Southern Observatory’s (ESO) Very Large Telescope (VLT) reveal the spiral galaxy in blue and white. X-ray point sources have been removed from this image to emphasize the diffuse emission.
Near the head of the comet-shaped X-ray emission is a region containing several optically bright stars and enhanced X-ray emission. Star formation may have been triggered by the shock wave, producing bright massive stars. In that case, X-ray emission would be generated by massive star winds and by the remains of supernova explosions as massive stars evolve.
The mass of the entire gas cloud is uncertain because it cannot be determined from the 2-D image whether the hot gas is concentrated in a thin pancake or distributed over a large spherical region. If the gas is a pancake, the mass is equivalent to 40 thousand Suns. If it is spread out uniformly, the mass could be much larger, about 3 million times as massive as the Sun. This range agrees with values for dwarf galaxies in the Local Group containing the Milky Way.
The hot gas should continue to glow in X-rays for tens to hundreds of millions of years, depending on the geometry of the collision. The collision itself should last for about 50 million years. Therefore, searching for large regions of hot gas in galaxies might be a way to estimate the frequency of collisions with dwarf galaxies and to understand how important such events are to galaxy growth.
An alternative explanation of the X-ray emission is that the hot gas cloud could have been produced by supernovae and hot winds from large numbers of massive stars, all located on one side of the galaxy. The lack of evidence of expected radio, infrared, or optical features argues against this possibility.