The galaxy presents an interacting morphology, characterized by at least two distinct, luminous components, indicative of an ongoing or recent merger event. The most prominent component displays a smooth, centrally concentrated light profile, potentially representing the remnant core of a progenitor galaxy. A second, slightly less luminous component exhibits a more diffuse and elongated structure, possibly a tidal tail or a disrupted disk. A third, compact region is also visible. The overall color appears relatively red, suggesting a significant population of older stars and/or dust obscuration. The system does not appear to be dominated by strong spiral arm structures or active star formation regions, indicating a relatively low star formation rate. Further investigation would be needed to classify the precise stage of interaction and determine the physical properties of the merging galaxies.
