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Large barred spiral galaxy in the constellation Perseus
UGC 2885 is a spiral galaxy with a relatively low surface brightness, but does not have as low of a surface brightness as other so-called giant low surface brightness galaxies.
UGC 2885 is classified as a field galaxy, being remarkably isolated from other galaxies. It is unknown how it got its cold gas which is necessary for star formation. 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.