Pisces Overdensity

The topic of Pisces Overdensity is one that has captured the attention of many people as of late. From its impact on society to its implications on daily life, Pisces Overdensity has generated widespread interest in various fields. As we continue to explore and better understand Pisces Overdensity, new perspectives and questions arise that invite us to reflect on its importance and relevance. In this article, we will dive into the different facets of Pisces Overdensity, examining its influence in different areas and discussing its significance in the current context.

Not to be confused with Pisces Dwarf.
Pisces Overdensity
Observation data (J2000 epoch)
ConstellationPisces
Right ascension23h 19m 00s[1]
Declination+00° 00′ 00″[1]
Distance260 kly (80 kpc)[2]
Absolute magnitude (V)−10.35[3]
Characteristics
TypedIrr/dSph[3]
Apparent size (V)~1°[4]
Other designations
Pisces Plume[1]

The Pisces Overdensity is a clump of stars in the Milky Way's halo, which may be a disrupted dwarf spheroidal galaxy.[5] It is situated in the Pisces constellation and was discovered in 2009 by analysis of distribution of RR Lyrae stars in the data obtained by the Sloan Digital Sky Survey's data.[2] The galaxy is located at the distance of about 80 kpc from the Sun and moves towards it with a speed of about 75 km/s.[4]

The Pisces Overdensity is one of the faintest satellites of the Milky Way.[5] Its mass is estimated to be at least 105 Solar masses.[2] However it has a large size of about several degrees (around 1 kpc) and may be in a transitional phase between a gravitationally bound galaxy and completely unbound system.[4] The Pisces Overdensity is located near the plane, where the Magellanic Clouds lie. There may exist a connection between the Magellanic Stream and this galaxy.[2]

References

  1. ^ a b c "NAME Pisces Overdensity". SIMBAD. Centre de données astronomiques de Strasbourg.
  2. ^ a b c d Watkins, L. L.; et al. (2009), "Substructure revealed by RR Lyraes in SDSS Stripe 82", Monthly Notices of the Royal Astronomical Society, 398 (4): 1757–70, arXiv:0906.0498, Bibcode:2009MNRAS.398.1757W, doi:10.1111/j.1365-2966.2009.15242.x, S2CID 14409027.
  3. ^ a b Boyer, Martha L; Skillman, Evan D; Van Loon, Jacco Th; Gehrz, Robert D; Woodward, Charles E (2009). "Aspitzerstudy of Asymptotic Giant Branch Stars. Iii. Dust Production and Gas Return in Local Group Dwarf Irregular Galaxies". The Astrophysical Journal. 697 (2): 1993. arXiv:0903.3871. Bibcode:2009ApJ...697.1993B. doi:10.1088/0004-637X/697/2/1993. S2CID 12162514.
  4. ^ a b c Kollmeier, Juna A.; et al. (2009), "Spectroscopic Confirmation of the Pisces Overdensity", The Astrophysical Journal Letters, 705 (2): L158 – L162, arXiv:0908.1381, Bibcode:2009ApJ...705L.158K, doi:10.1088/0004-637X/705/2/L158, S2CID 9825846.
  5. ^ a b Belokurov, V.; et al. (2010), "Big fish, small fish: Two New Ultra-Faint Satellites of the Milky Way", The Astrophysical Journal Letters, 712 (1): L103–106, arXiv:1002.0504, Bibcode:2010ApJ...712L.103B, doi:10.1088/2041-8205/712/1/L103, S2CID 29195107.