Coma Berenices or Com is a dwarf spheroidal galaxy situated in the Coma Berenices constellation and discovered in 2006 in data obtained by the 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]
| 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] |
| Apparent magnitude (V) | 14.5 ± 0.5[2] |
| Characteristics | |
| Type | dSph[2] |
| Apparent size (V) | 11.8′[2] |
| Other designations | |
| Coma Dwarf,[1] PGC 4713557 | |
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 and 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
editReferences
edit- ^ a b c d "NAME Coma Dwarf Galaxy". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-02-07.
- ^ 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): 897–906. arXiv:astro-ph/0608448. Bibcode:2007ApJ...654..897B. doi:10.1086/509718. S2CID 18617277.
- ^ 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. S2CID 11594422.
- ^ 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 (1): 313–331. arXiv:0706.0516. Bibcode:2007ApJ...670..313S. doi:10.1086/521816. S2CID 9715950.
- ^ 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): 1075–1092. arXiv:0805.2945. Bibcode:2008ApJ...684.1075M. doi:10.1086/590336. S2CID 17838966.
- ^ 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 (1): L43–L46. arXiv:0807.1925. Bibcode:2008ApJ...685L..43K. doi:10.1086/592432. S2CID 3185311.
- ^ Grcevich, J.; Putman, M. E. (2009). "H I in Local Group Dwarf Galaxies and Stripping by the Galactic Halo". The Astrophysical Journal. 696 (1): 385–395. arXiv:0901.4975. Bibcode:2009ApJ...696..385G. doi:10.1088/0004-637X/696/1/385.
- ^ 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. S2CID 20051174.