Coma Berenices (dwarf galaxy)

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Coma Berenices Dwarf Galaxy[1]
Observation data (J2000 epoch)
Constellation Coma Berenices
Right ascension 12h 26m 59s[1]
Declination 23° 55′ 09″[1]
Distance

143 ± 13 kly (44 ± 4 kpc)[2]

137+5
−3
kly (42+2
−1
kpc)
[3]
Type dSph[2]
Apparent dimensions (V) 11.8′[2]
Apparent magnitude (V) 14.5 ± 0.5[2]
Other designations
Coma Dwarf,[1] PGC 4713557
See also: Galaxy, List of galaxies

Coma Berenices or Com is a dwarf spheroidal galaxy situated in the Coma Berenices constellation and discovered in 2006 in the data obtained by Sloan Digital Sky Survey.[2] The galaxy is located at the distance of about 44 kpc from the Sun and moves away from the Sun with the velocity of about 98 km/s.[2][4] It is classified as a dwarf spheroidal galaxy (dSph) meaning that it has an elliptical (ratio of axes ~ 5:3) shape with the half-light radius of about 70 pc.[2][5]

Com is one of the smallest and faintest satellites[note 1] of the Milky Way—its integrated luminosity is about 3700 times that of the Sun (absolute visible magnitude of about −4.1), which is much lower than the luminosity of the majority of globular clusters.[5] However, its mass is about 1.2 million solar masses, which means that galaxy's mass to light ratio is around 450. A high mass to light ratio implies that Com is dominated by the dark matter.[4]

The stellar population of Com consists mainly of old stars formed more than 12 billion years ago.[2] The metallicity of these old stars is also very low at [Fe/H] ≈ −2.53 ± 0.45, which means that they contain 350 times less heavy elements than the Sun.[6] The stars of Com were probably among the first stars to form in the Universe. Currently there is no star formation in Com. The measurements have so far failed to detect any neutral hydrogen in it—the upper limit is only 46 solar masses.[7]

Coma Dwarf is located near the Sagittarius Stream, which is made of stars stripped from the Sagittarius Dwarf Elliptical Galaxy. This association may indicate that Com is a former satellite of star cluster from that galaxy.[8]

Notes[edit]

  1. ^ Only Segue 1, Segue 2, Bootes II and Willman 1 are fainter.[5]

References[edit]

  1. ^ a b c d "SIMBAD Astronomical Database". Results for Coma Dwarf. Retrieved 2010-02-07. 
  2. ^ a b c d e f g h Belokurov, V.; Zucker, D. B.; Evans, N. W.; Kleyna, J. T.; Koposov, S.; Hodgkin, S. T.; Irwin, M. J.; Gilmore, G.; Wilkinson, M. I.; Fellhauer, M.; Bramich, D. M.; Hewett, P. C.; Vidrih, S.; De Jong, J. T. A.; Smith, J. A.; Rix, H. ‐W.; Bell, E. F.; Wyse, R. F. G.; Newberg, H. J.; Mayeur, P. A.; Yanny, B.; Rockosi, C. M.; Gnedin, O. Y.; Schneider, D. P.; Beers, T. C.; Barentine, J. C.; Brewington, H.; Brinkmann, J.; Harvanek, M.; Kleinman, S. J. (2007). "Cats and Dogs, Hair and a Hero: A Quintet of New Milky Way Companions". The Astrophysical Journal 654 (2): 897. arXiv:astro-ph/0608448. Bibcode:2007ApJ...654..897B. doi:10.1086/509718.  edit
  3. ^ Musella, Ilaria; Ripepi, Vincenzo; Clementini, Gisella et al. (2009). "Pulsating Variable Stars in the Coma Berenices Dwarf Spheroidal Galaxy". The Astrophysical Journal Letters 695 (1): L83–1L87. arXiv:0902.4230. Bibcode:2009ApJ...695L..83M. doi:10.1088/0004-637X/695/1/L83. 
  4. ^ a b 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. arXiv:0706.0516. Bibcode:2007ApJ...670..313S. doi:10.1086/521816.  edit
  5. ^ a b c 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. arXiv:0805.2945. Bibcode:2008ApJ...684.1075M. doi:10.1086/590336.  edit
  6. ^ 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. arXiv:0807.1925. Bibcode:2008ApJ...685L..43K. doi:10.1086/592432.  edit
  7. ^ Grcevich, J.; Putman, M. E. (2009). "H I in Local Group Dwarf Galaxies and Stripping by the Galactic Halo". The Astrophysical Journal 696: 385. arXiv:0901.4975. Bibcode:2009ApJ...696..385G. doi:10.1088/0004-637X/696/1/385.  edit
  8. ^ Belokurov, V.; Walker, M.G.; Evans, N.W. et al. (2009). "Segue 2: A Prototype of the Population of Satellites of Satellites". Mon. Not. R. Astron. Soc. 397 (4): 1748–1755. arXiv:0903.0818. Bibcode:2009MNRAS.397.1748B. doi:10.1111/j.1365-2966.2009.15106.x.