The galaxy presents as a spiral type, exhibiting a well-defined central bulge that graduates in luminosity to the outer disk. The bulge appears to be slightly elongated, and is a relatively smooth structure.

Two prominent spiral arms emanate from the central region, winding moderately tightly around the core. These arms have a somewhat patchy appearance, exhibiting variations in stellar density and potentially regions of active star formation. There also appear to be two slightly fainter arms. 

Overall, the galaxy possesses a relatively high degree of rotational symmetry, lacking significant signs of major disturbances that may occur after a galaxy merger. There may be a slight interaction or minor disturbance occurring in the outer spiral arm regions. The arms have a well defined and structured appearance. 
