Ursa Major II Dwarf

Ursa Major II Dwarf Galaxy[1]
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 08h 51m 30.0s[1]
Declination +63° 07′ 48″[1]
Distance 98 ± 16 kly (30 ± 5 kpc)[2]
Apparent magnitude (V) 14.3 ± 0.5[2]
Characteristics
Type dSph[2]
Apparent size (V) 32 ± 2′[3]
Other designations
UMa II galaxy, Ursa Major II Dwarf[1]

Ursa Major II Dwarf (UMa II dSph) is a dwarf spheroidal galaxy situated in the Ursa Major constellation and discovered in 2006 in the data obtained by the Sloan Digital Sky Survey.[2] The galaxy is located approximately 30 kpc from the Sun and moves towards the Sun with the velocity of about 116 km/s.[4] It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical (ratio of axes ~ 2:1) shape with the half-light radius of about 140 pc.[3]

Ursa Major II is one of the smallest and faintest satellites[note 1] of the Milky Way—its integrated luminosity is about 4000 times that of the Sun (absolute visible magnitude of about −4.2),[2] which is much lower than the luminosity of the majority of globular clusters. Uma II is even less luminous than some stars, like Canopus in the Milky Way. It is comparable in luminosity to Bellatrix in Orion. However, its mass is about 5 million solar masses, which means that galaxy's mass to light ratio is around 2000.[4] This may be an overestimate as the galaxy has somewhat irregular shape and may be in process of tidal disruption.[2]

The stellar population of Uma II consists mainly of old stars formed at least 10 billion years ago.[2] The metallicity of these old stars is also very low at [Fe/H] ≈ −2.44 ± 0.06, which means that they contain 300 times less heavy elements than the Sun.[5] The stars of Uma II were probably among the first stars to form in the Universe. Currently there is no star formation in Uma II. The measurements have so far failed to detect any neutral hydrogen in it—the upper limit is only 562 solar masses.[6]

See also

Notes

  1. ↑ Only Coma Berenices, Segue 1, Segue 2, Boötes II and Willman 1 are fainter.[3]

References

  1. 1 2 3 4 "SIMBAD Astronomical Database". Results for Ursa Major II. Retrieved 2011-11-19.
  2. 1 2 3 4 5 6 7 Zucker, D. B.; Belokurov, V.; Evans, N. W.; Kleyna, J. T.; Irwin, M. J.; Wilkinson, M. I.; Fellhauer, M.; Bramich, D. M.; Gilmore, G.; Newberg, H. J.; Yanny, B.; Smith, J. A.; Hewett, P. C.; Bell, E. F.; Rix, H. -W.; Gnedin, O. Y.; Vidrih, S.; Wyse, R. F. G.; Willman, B.; Grebel, E. K.; Schneider, D. P.; Beers, T. C.; Kniazev, A. Y.; Barentine, J. C.; Brewington, H.; Brinkmann, J.; Harvanek, M.; Kleinman, S. J.; Krzesinski, J.; Long, D. (2006). "A Curious Milky Way Satellite in Ursa Major". The Astrophysical Journal. 650: L41. Bibcode:2006ApJ...650L..41Z. arXiv:astro-ph/0606633 Freely accessible. doi:10.1086/508628.
  3. 1 2 3 Martin, N. F.; De Jong, J. T. A.; Rix, H. W. (2008). "A Comprehensive Maximum Likelihood Analysis of the Structural Properties of Faint Milky Way Satellites". The Astrophysical Journal. 684 (2): 1075. Bibcode:2008ApJ...684.1075M. arXiv:0805.2945 Freely accessible. doi:10.1086/590336.
  4. 1 2 Simon, J. D.; Geha, M. (2007). "The Kinematics of the Ultra‐faint Milky Way Satellites: Solving the Missing Satellite Problem". The Astrophysical Journal. 670: 313. Bibcode:2007ApJ...670..313S. arXiv:0706.0516 Freely accessible. doi:10.1086/521816.
  5. ↑ Kirby, E. N.; Simon, J. D.; Geha, M.; Guhathakurta, P.; Frebel, A. (2008). "Uncovering Extremely Metal-Poor Stars in the Milky Way's Ultrafaint Dwarf Spheroidal Satellite Galaxies". The Astrophysical Journal. 685: L43. Bibcode:2008ApJ...685L..43K. arXiv:0807.1925 Freely accessible. doi:10.1086/592432.
  6. ↑ Grcevich, J.; Putman, M. E. (2009). "H I in Local Group Dwarf Galaxies and Stripping by the Galactic Halo". The Astrophysical Journal. 696: 385. Bibcode:2009ApJ...696..385G. arXiv:0901.4975 Freely accessible. doi:10.1088/0004-637X/696/1/385.

Coordinates: 08h 51m 30s, +63° 07′ 48″

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