The observed galaxy presents an elongated, flattened morphology, indicative of a disk galaxy viewed nearly edge-on. A prominent central bulge, exhibiting a bright and smoothly distributed luminosity, dominates the galaxy's core. The bulge appears to be rounded. Extending from the central bulge, the disk is visible as a relatively thin structure. The disk's luminosity decreases with distance from the bulge, suggesting a gradual decline in stellar density. The disk exhibits hints of substructure, possibly indicating the presence of spiral arms. The redder hue of the central bulge, contrasted with the bluer hue of the disk, suggests a difference in stellar populations, with the bulge possibly containing a larger fraction of older, redder stars, while the disk may have a population of younger, bluer stars. There is no strong evidence for a major ongoing merger. Faint signs of a slight warp and/or minor disturbances are detected within the disk suggesting possible past or present gravitational interaction with a smaller companion galaxy.
