Dwarf galaxy problem
The dwarf galaxy problem is one that arises from numerical cosmological simulations that predict the evolution of the distribution of matter in the universe. Dark matter seems to cluster hierarchically and in ever increasing number counts for smaller and smaller sized halos. However, while there seems to be enough observed normal-sized galaxies to account for this distribution, the number of dwarf galaxies[1] is orders of magnitude lower than expected from simulation.[2] For comparison, there were observed to be around 38 dwarf galaxies in the Local Group, and only around 11 orbiting the Milky Way,[1] (for a detailed and more up to date list see Milky Way's satellite galaxies) yet one dark matter simulation predicted around 500 Milky Way dwarf satellites.[2]
This problem has two potential solutions. One is that the smaller halos do exist but only a few of them end up becoming visible because they have not been able to attract enough baryonic matter to create a visible dwarf galaxy. In support of this Keck observations in 2007 of eight newly discovered ultra-faint Milky Way dwarf satellites showed that six were around 99.9% dark matter (with a mass to light ratio of about 1000) [3] Other solutions may be that dwarf galaxies tend to be gobbled up or tidally stripped apart by larger galaxies due to complex interactions. This tidal stripping has been part of the problem in identifying dwarf galaxies in the first place, which is an extremely difficult task since these objects have low surface brightness and are highly diffused, so much that they are virtually unnoticeable even in our own backyard.
See also
- Dark galaxy
- Cold dark matter
- Cuspy halo problem (also known as "the core/cusp problem")
- List of unsolved problems in physics
References
- ^ a b Mateo, M. L. (1998). "Dwarf Galaxies of the Local Group". Annual Review of Astronomy and Astrophysics. 36 (1): 435–506. arXiv:astro-ph/9810070. Bibcode:1998ARA&A..36..435M. doi:10.1146/annurev.astro.36.1.435.
- ^ a b Moore, Ben (1999). "Dark Matter Substructure within Galactic Halos". Astrophysical Journal Letters. 524 (1): L19–L22. arXiv:astro-ph/9907411. Bibcode:1999ApJ...524L..19M. doi:10.1086/312287.
{{cite journal}}: Unknown parameter|coauthors=ignored (|author=suggested) (help) - ^ Simon, J. D. and 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:astro-ph/0706.0516. Bibcode:2007ApJ...670..313S. doi:10.1086/521816.
{{cite journal}}: Check|arxiv=value (help); Unknown parameter|month=ignored (help)CS1 maint: multiple names: authors list (link)
- Bullock (2010). "Notes on the Missing Satellites Problem". arXiv:1009.4505v1 [astro-ph.CO].
External links
- The End of Small Galaxies (SPACE.com) 22 May 2006 06:12 am ET
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