The galaxy presents as a spiral type, observed at an angle that is close to face-on. Two prominent spiral arms emanate from the central region. These arms are loosely wound and exhibit a clumpy structure, suggesting active star formation regions within the spiral arms. The central bulge appears moderate in size, with a bar structure that appears weak. Overall, there are no major signs of tidal disturbances or ongoing mergers, although there seems to be a minor disruption of the spiral arms and some irregularities in their distribution. The spiral arms appear to have a population of younger stars that are a bit less concentrated towards the center of the disk as older ones are.