'Leo I' is a
dwarf spheroidal galaxy in the
constellation Leo. At about 820,000
light-years distant, it is a member of the
Local Group of galaxies and is thought to be one of the most distant satellites of the
Milky Way galaxy. It was discovered in 1950 by
Wilson on
photographic plates of the
National Geographic Society - Palomar Observatory Sky Survey, which were taken with the 48-inch
Schmidt camera at
Palomar Observatory.
[1][2]
The measurement of
radial velocities of some bright
red giants in Leo I have made possible to measure its mass. It was found to be at least (2.0 ± 1.0) × 10
7 MSun. The results are not conclusive, and do not deny or confirm the existence of a large
dark matter halo around the galaxy. However, it seems to be certain that the galaxy does not rotate.
It has been suggested that Leo I is a tidal debris stream in the outer
halo of the Milky Way. This hypothesis has not been confirmed, however.
Typical to a dwarf galaxy, the
metallicity of Leo I is very low, only one percent that of the
Sun. It seems that the galaxy experienced a major increase in its star formation rate between 6
Ga and 2 Ga (billion years ago). Some low-level activity may have continued until 200-500 Ma. Therefore it may be the youngest dwarf spheroidal satellite galaxy of the Milky Way. In addition, the galaxy may be embedded in a cloud of ionized gas with a mass similar to that of the whole galaxy.
No
globular clusters have been found in the galaxy.
Leo I is located only 12
arc minutes from
Regulus, the brightest star in the constellation. For that reason, the galaxy is sometimes called the ''Regulus Dwarf''. Scattered light from the star makes studying the galaxy more difficult, and it was not until the 1990s that it was detected visually.
External links
★
Astronomy Picture of the Day - Leo I
★
SEDS page on Leo I
★
'WIKISKY.ORG': SDSS image, Leo I dwarf galaxy
References
1. Leo I
2. Galaxies of the Local Group, , Sidney, Van den Bergh, Cambridge University Press, 2000, ISBN 0-521-65181-6