Messier 109
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| Barred spiral galaxy M109 | |
| Observation data Epoch J2000 |
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|---|---|
| Constellation | Ursa Major |
| Right ascension | 11h 57m 36.0s |
| Declination | +53° 22′ 28″ |
| Apparent dimension (V) | 7.6 × 4.7 moa |
| Apparent magnitude (V) | 10.6 |
| Characteristics | |
| Type | SB(rs)bc,LINER/HII |
| Astrometry | |
| Heliocentric radial velocity | 1048 ± 1km/s |
| Redshift | 0.003496 ± 0.000004 |
| Galactocentric velocity | 1121 ± 3km/s |
| Distance | 83.5 ± 24 Mly (25.60 ± 7.36 Mpc) |
| Other designations | |
| Database references | |
| SIMBAD |
Search M109 data
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| See also: Galaxy, List of galaxies | |
Messier 109 (also known as NGC 3992) is a barred spiral galaxy exhibiting a weak inner ring structure around the central bar approximately 83.5 ± 24 million light-years away in the constellation Ursa Major. M109 can be seen southeast of the star Phecda (γ UMa).
Messier 109 was discovered by Pierre Méchain in 1781. In 1783 Charles Messier catalogued NGC 3992 as his 109th object.
Between the 1920s through the 1950s, it was considered that Messier objects over 103 were not official, but in later years the additions became more widely accepted. David H. Levy mentions the modern 110 object catalog while Sir Patrick Moore gave the original to 104 but has M105-M109 listed as an addendum. By the late 1970s all 110 objects are commonly used among astronomers as they still are today.
In March 1956, supernova 1956A was observed in M109. SN 1956A was a type Ia supernova in the southeast part of the galaxy, glowing at magnitude 12.8 to 12.3 at its maximum. SN 1956A has been the only supernova observed in M109 since its discovery. It is also by far the most distant object in the Messier Catalog, followed by M91
M109 has three satellite galaxies (UGC 6923, UGC 6940 and UGC 6969) and possibly might have more. Detailed hydrogen line observations have been obtained from M109 and its satellites. M109's H I distribution is regular with a low level radial extension outside the stellar disc, while at exactly the region of the bar, there is a central H I hole in the gas distribution. Possibly the gas has been transported inwards by the bar, and because of the emptiness of the hole no large accretion events can have happened in the recent past.
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