Right ascension 10 03 06.9 Redshift 403 ± 1 km/s Apparent size (V) 19′.1 × 3′.7 Constellation Hydra | Declination −26° 09′ 34″ Type SB(s)m Magnitude 10.4 Apparent magnitude (V) 10.4 | |
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Distance 4.3 ± 0.3 Mly (1.33 ± 0.08 Mpc) Similar Sextans B, Antlia Dwarf, Sextans A, IC 1613, Wolf–Lundmark–Melotte | ||
The spaceway ngc 3109
NGC 3109 is a small barred Magellanic type spiral or irregular galaxy around 4.2 Mly away in the direction of the constellation of Hydra. NGC 3109 is believed to be tidally interacting with the dwarf elliptical galaxy Antlia Dwarf. It was discovered by John Herschel on March 24, 1835 while he was in what is now South Africa.
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Size and morphology
NGC 3109 is classified as a Magellanic type irregular galaxy, but it may in fact be a small spiral galaxy. If it is a spiral galaxy, it would be the smallest in the Local Group. NGC 3109 has a mass of about 2.3×109 times the mass of the Sun, of which 20% is in the form of neutral hydrogen. It is oriented edge-on from our point of view, and may contain a disk and a halo. The disk appears to be composed of stars of all ages, whereas the halo contains only very old and metal-poor stars. NGC 3109 does not appear to possess a galactic nucleus.
From measurements of the neutral atomic hydrogen in the galaxy, it has been found that the disk of NGC 3109 is warped. The warp has the same radial velocity as gas in the Antlia Dwarf galaxy, indicating that the two galaxies had a close encounter approximately one billion years ago.
Composition
Based on spectroscopy of red giants in NGC 3109, it is known that the galaxy has a low metallicity, similar to that to the Small Magellanic Cloud. It is one of the most metal-poor galaxies in the Local group. NGC 3109 seems to contain an unusually large number of planetary nebulae for its luminosity. It also contains a substantial amount of dark matter.
Location
NGC 3109 is located about 1.3 megaparsecs (4.2 Mly) away, in the constellation Hydra. This puts it at the very outskirts of the Local Group. Its membership of the Local Group has been challenged, because it seems to be receding faster than estimates of the Local Group's escape velocity. It is distant enough from the largest members of the Local Group that it has not been tidally influenced by them.
