Astronomy:Canis Major Overdensity
| Canis Major Overdensity | |
|---|---|
| Observation data (J2000 epoch) | |
| Constellation | Canis Major |
| Right ascension | 07h 12m 35.0s[1] |
| Declination | −27° 40′ 00″[1] |
| Distance | 25,000 ly |
| Characteristics | |
| Type | Irr |
| Number of stars | 1 billion (1×109) |
| Apparent size (V) | 12 degrees × 12 degrees |
| Other designations | |
| CMa Dwarf,[1] PGC 5065047 | |
The Canis Major Overdensity (CMa Overdensity) or Canis Major Dwarf Galaxy (CMa Dwarf) is a disputed dwarf irregular galaxy in the Local Group, located in the same part of the sky as the constellation Canis Major.
The supposed small galaxy contains a relatively high percentage of red giants and is thought to contain an estimated one billion stars in all.
At the time of its announcement, the Canis Major Dwarf Galaxy is classified as an irregular galaxy and is thought to be the closest neighboring galaxy to the Earth's location in the Milky Way, being located about 25,000 light-years (7.7 kiloparsecs) away from the Solar System[2] and 42,000 ly (13 kpc) from the Galactic Center. It has a roughly elliptical shape and is thought to contain as many stars as the Sagittarius Dwarf Elliptical Galaxy, the previous contender for closest galaxy to Earth, though later studies disputed this conclusion.
Discovery
The existence of a strong elliptical-shaped stellar overdensity was reported in November 2003 by an international team of French, Italian, British, and Australian astronomers, who claimed their study pointed to a newly discovered dwarf galaxy: the Canis Major Dwarf Galaxy.[3] This structure is located closer to the Sun than the center of this galaxy, at approximately 7.7 kpc (25,000 ly) from the Sun.
The team of astronomers that discovered it was collaborating on analysis of data from the Two-Micron All Sky Survey (2MASS), a comprehensive survey of the sky in infrared light, which is not blocked by gas and dust as severely as visible light. Because of this technique, scientists were able to detect a very significant overdensity of class M giant stars in a part of the sky occupied by the Canis Major constellation, along with several other related structures composed of this type of star, two of which form broad, faint arcs.
Characteristics
Some astronomers believe that the CMa overdensity is a dwarf galaxy in the process of being pulled apart by the gravitational field of the more massive Milky Way galaxy. The main body of the CMa is extremely degraded. Tidal disruption causes a filament of stars to trail behind it as it orbits the Milky Way, forming a complex ringlike structure, sometimes referred to as the Monoceros Ring, which wraps around the Milky Way three times,[4] The stream of stars was discovered in the early 21st century by astronomers conducting the Sloan Digital Sky Survey. The Monoceros Ring is similar to the Virgo Stellar Stream which is thought to be the result of the Milky Way tearing stars and gases from the Sagittarius Dwarf Spheroidal Galaxy into a Stellar Stream. It was in the course of investigating the Monoceros Ring, and a closely spaced group of globular clusters similar to those associated with the Sagittarius Dwarf Elliptical Galaxy, that the CMa Overdensity was discovered.
Globular clusters thought to be associated with the CMa include NGC 1851, NGC 1904, NGC 2298 and NGC 2808, all of which may have been part of the galaxy's globular cluster system before accreting into the Milky Way. NGC 1261 is another nearby cluster, but its velocity differs enough to make its relationship to the system unclear. Additionally, Dolidze 25 and H18 are open clusters that may have formed when the dwarf galaxy perturbed material in the galactic disk, stimulating star formation.[3]
The discovery of the CMa and subsequent analysis of the stars associated with it has provided some support for the current theory that galaxies may grow in size by swallowing their smaller neighbors. Martin et al.[3] believe that the preponderance of evidence points to the accretion of a small satellite galaxy of the Milky Way which was orbiting roughly in the plane of the galactic disk.
Dispute
Several studies cast doubts on the true nature of this overdensity.[5] Some research suggests that the trail of stars is actually part of the warped galactic thin disk and thick disk population and not a result of the collision of the Milky Way with a dwarf spheroidal galaxy.[6] Investigation of the area in 2009 yielded only ten RR Lyrae variable stars which is consistent with the Milky Way's halo and thick disk populations rather than a separate dwarf spheroidal galaxy.[7]
In fiction
British science fiction writer Stephen Baxter included the Canis Major Overdensity in his novella "Mayflower II" as the destination of the eponymous starship.
See also
- Messier 79
- Galaxy formation and evolution
- Stellar kinematics
- Milky Way
- Sagittarius Dwarf Spheroidal Galaxy
- Monoceros Ring
- Virgo Stellar Stream
References
- ↑ 1.0 1.1 1.2 "NASA/IPAC Extragalactic Database". http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Canis+Major+Dwarf#ObjNo1.
- ↑ "Astronomers find nearest galaxy to the Milky Way". http://astro.u-strasbg.fr/images_ri/canm-e.html.
- ↑ 3.0 3.1 3.2 N. F. Martin; R. A. Ibata; M. Bellazzini; M. J. Irwin; G. F. Lewis; W. Dehnen (2004). "A dwarf galaxy remnant in Canis Major: the fossil of an in-plane accretion onto the Milky Way". Monthly Notices of the Royal Astronomical Society 348 (12): 12. doi:10.1111/j.1365-2966.2004.07331.x. Bibcode: 2004MNRAS.348...12M.
- ↑ Maggie Masetti (14 April 2011). "The Nearest Galaxies". NASA. http://heasarc.nasa.gov/docs/cosmic/nearest_galaxy_info.html. See section "The Canis Major Dwarf".
- ↑ Lopez-Corredoira, M.; Moitinho, A.; Zaggia, S.; Momany, Y.; Carraro, G.; Hammersley, P. L.; Cabrera-Lavers, A.; Vazquez, R. A. (Jul 2012). "Comments on the "Monoceros" affair". arXiv:1207.2749 [astro-ph.GA].
- ↑ Momany, Y.; Zaggia, S. R.; Bonifacio, P.; Piotto, G.; De Angeli, F.; Bedin, L. R.; Carraro, G. (July 2004). "Probing the Canis Major stellar over-density as due to the Galactic warp". Astronomy and Astrophysics 421 (2): L29. doi:10.1051/0004-6361:20040183. Bibcode: 2004A&A...421L..29M.
- ↑ Mateu, Cecilia; Vivas, A. Katherina; Zinn, Robert; Miller, Lissa R.; Abad, Carlos (2009). "No Excess of RR Lyrae Stars in the Canis Major Overdensity". The Astronomical Journal 37 (5): 4412–23. doi:10.1088/0004-6256/137/5/4412. Bibcode: 2009AJ....137.4412M.
External links
- "Canis Major Dwarf". http://messier.seds.org/more/cma_dw.html.
- "NAME CMa Dwarf Galaxy". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NAME+CMa+Dwarf+Galaxy.
| Location | Milky Way → Milky Way subgroup → Local Group → Local Sheet → Virgo Supercluster → Laniakea Supercluster → Observable universe → Universe Each arrow (→) may be read as "within" or "part of". |  | |||||||
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Coordinates: 
07h 12m 35.0s, −27° 40′ 00″
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