The galaxy presents a disk-like morphology with a noticeable central bulge, potentially a classical bulge. The galaxy is viewed at a significant inclination, appearing elongated. Faint spiral arm structures are visible, wound relatively tightly around the central bulge, suggesting this could be a late-type spiral galaxy. The galaxy exhibits a brighter, more concentrated core, with a gradual decrease in luminosity towards the outer regions of the disk. The color gradient suggests a possible transition from an older stellar population in the bulge to younger stars in the spiral arms. The dust lanes are not clearly defined, implying a relatively uniform distribution of interstellar medium within the disk. There's no obvious sign of any major ongoing merger activity or tidal disturbances, though some minor irregularities might indicate past interactions.
