The galaxy appears as a slightly elongated, luminous object. Its overall morphology seems relatively smooth, with a dominant central bulge region that is bright and concentrated. There is a hint of disk-like structure surrounding the bulge, although any spiral arms, if present, are not well-defined in this image.

The galaxy exhibits a yellowish-red hue, suggesting a population of older stars. The lack of strong blue emission indicates that the rate of active star formation is low. The overall color profile indicates a significant amount of dust obscuring the galaxy. A disturbance to the galaxy suggests that it is possibly merging with another smaller galaxy. This disturbance is the primary feature of this galaxy.

Based on these observations, the galaxy is likely an elliptical or lenticular galaxy that is undergoing a merger. Further spectroscopic analysis would be needed to determine the precise composition, age, and velocity distribution of its stellar populations, as well as to better characterize the nature of the merger and any related star formation activity.
