The galaxy appears to be a spiral type, observed at a non-negligible inclination. It exhibits a prominent central bulge, which dominates the inner region's luminosity, as well as spiral arm features that appear flocculent. The color gradient suggests the bulge is comprised of older stellar populations, while bluer tones in the disk region may indicate ongoing star formation. The overall structure suggests a moderate amount of disturbance with no evidence of recent merger activity. The galaxy appears quite large. The disk component seems to be relatively thick.
