Pisces II is a small irregular galaxy, with a moderately-aged and older stellar population of metal-poorstars, consisting primarily of stars formed about 10 billion years ago. The metallicity of these old stars is low, at −2.3 < [Fe/H] < −1.7, which means that the ratio of their mass that consists of heavy metals is less than that of the Sun. Its luminosity is about 10,000 times that of the Sun (absolute magnitude of about −5), which corresponds to the luminosity of an average globular cluster.
Potential past interactions
In 2016, follow-up work on Pisces II and Pegasus III highlighted that both lie relatively close to each other (within approximately 43 kiloparsecs), and share similar radial velocities in the Milky Way's rest frame. This suggests that these two satellite galaxies may actually be associated with one another, potentially having interacted in the past; however, further spectroscopic measurements are needed to confirm this.
12Andromeda II was also given the alias Pisces II by Martin et al. (2009), who also proposed aliases for several other satellite galaxies of the Andromeda Galaxy However, that name was later used by a different group unaware of these names, for this object.
↑In astronomy and physical cosmology, unlike other physical sciences, "heavy metals" refers to all elements except hydrogen and helium.
↑Martin, Nicolas F.; McConnachie, Alan W.; Irwin, Mike; Widrow, Lawrence M.; Ferguson, Annette M. N.; Ibata, Rodrigo A.; Dubinski, John; Babul, Arif; etal. (1 November 2009). "PAndAS' CUBS: Discovery of Two New Dwarf Galaxies in the Surroundings of the Andromeda and Triangulum Galaxies". The Astrophysical Journal. 705 (1): 758–765. arXiv:0909.0399. Bibcode:2009ApJ...705..758M. doi:10.1088/0004-637X/705/1/758. S2CID15277245.
Sand, David J; Strader, Jay; Willman, Beth; Zaritsky, Dennis; McLeod, Brian; Caldwell, Nelson; Seth, Anil; Olszewski, Edward (2012). "Tidal Signatures in the Faintest Milky Way Satellites: The Detailed Properties of Leo V, Pisces Ii, and Canes Venatici Ii". The Astrophysical Journal. 756 (1): 79. arXiv:1111.6608. Bibcode:2012ApJ...756...79S. doi:10.1088/0004-637X/756/1/79. S2CID46030862.