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A low-surface-brightness galaxy, or LSB galaxy, is a diffuse galaxy with a surface brightness that, when viewed from Earth, is at least one magnitude lower than the ambient night sky. Most LSBs are dwarf galaxies, and most of their baryonic matter is in the form of neutral gaseous hydrogen, rather than stars. They appear to have over 95% of their mass as non-baryonic dark matter. There appears to be no supernova activity in these galaxies. Rotation curve measurements indicate an extremely high mass-to-light ratio, meaning that stars and luminous gas contribute only very little to the overall mass balance of an LSB. The centers of LSBs show no large overdensities in stars, unlike e.g. the bulges of normal spiral galaxies. Therefore, they seem to be dark-matter-dominated even in their centers, which makes them excellent laboratories for the study of dark matter. In comparison to the more well-studied high-surface-brightness galaxies, LSBs are mainly isolated field galaxies, found in regions devoid of other galaxies. In their past, they had fewer tidal interactions or mergers with other galaxies, which could have triggered enhanced star formation. This is an explanation for the small stellar content. LSB galaxies were theorized to exist in 1976 by Mike Disney. The first LSB galaxy verified to exist was Malin 1, discovered in 1986. As such, it was also the first giant LSB galaxy identified. At the time of its discovery, it was the largest spiral galaxy known (by scale-length measurement).〔 Scientific American, "The Ghostliest Galaxies", GD Bothun, Vol. 276, No. 2, ''February 1997'', pp.40-45, 〕〔 Ken Crosswell, ("Malin 1: A Bizarre Galaxy Gets Slightly Less So" ), ''22 January 2007'' 〕 == Examples == * Andromeda V * Pegasus Dwarf Spheroidal Galaxy * IC 10 * NGC 45 * Malin 1 〔 * Malin 2 〔 * Phoenix Dwarf * Sagittarius Dwarf Irregular Galaxy (SagDIG) * Sextans A * Sextans B * Wolf–Lundmark–Melotte galaxy (WLM) 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Low-surface-brightness galaxy」の詳細全文を読む スポンサード リンク
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