UGC 2885 is a spiral galaxy with a relatively low surface brightness. The central bulge is the most prominent feature of this galaxy, where a faint bar crosses its center.
UGC 2885 is classified as a field galaxy—a class of galaxies found in remote, under-dense and "vacant" sections of space, far from other major galaxies. NASA has reported that the theorized main source for disk growth for UGC 2885 came from the accretion of intergalactic hydrogen gas, rather than through the repeated process of galactic collision, as most galaxies are thought to grow.
The lack of interaction is evident from the near-perfect structure of the spiral arms and disk, lack of tidal tails, and modest rate of star formation—approximately 0.5 solar masses/year.
Additionally, despite being originally classified as an unbarred spiral galaxy, new Hubble images clearly show the presence of a small bar cutting across the ring structure of the core. This is peculiar, as most bars are thought to form through minor gravitational perturbations brought on by satellite and neighboring galaxies, which is something this galaxy lacks. This galaxy highlights that bars are able to form in spiral galaxies without the influence of another galaxy—this indicates that other forces, such as interactions between stars, gas and dust, as well as the gravitational influence of dark matter, might play a role in their development.
^Canzian, Blaise; Allen, R. J.; Tilanus, R. P. J. (1993). "Spiral structure of the giant galaxy UGC 2885 – H-alpha kinematics". The Astrophysical Journal. 406: 457. Bibcode:1993ApJ...406..457C. doi:10.1086/172457.
^Swift, B.; Li, W. D. (2002). "Supernovae 2002D, 2002E, 2002F, and 2002G". International Astronomical Union Circular (7797): 1. Bibcode:2002IAUC.7797....1S.
