The galaxy presents a well-defined spiral structure. Its disk is oriented at a nearly face-on inclination relative to the observer's line of sight. The central bulge is relatively small and displays a smooth, bright profile, indicative of an older stellar population. Spiral arms are prominent, displaying a tight winding pattern. The arms show a clumpy morphology with distinct regions of enhanced star formation, evidenced by the bluish tint within these regions. These areas suggest the presence of younger, hotter stars. Overall the galaxy appears relatively isolated with no obvious signs of major interactions or mergers. There may be some evidence of a subtle bar structure extending through the central region of the galaxy.
