NGC 1311
Galaxy in the constellation Horologium
From Wikipedia, the free encyclopedia
NGC 1311 is a nearby late-type barred spiral galaxy, occasionally described as a dwarf irregular or emission-line galaxy, and a potential weak Seyfert 2 active galaxy candidate located in the Horologium constellation. It was discovered by John Herschel in 1837.[2][3][4][5][6][7][8][9]
| NGC 1311 | |
|---|---|
NGC 1311 | |
| Observation data (J2000 epoch) | |
| Constellation | Horologium |
| Right ascension | 03h 20m 06.9s[1] |
| Declination | −52° 11′ 08″[1] |
| Redshift | 0.001911 ± 0.000007[1] |
| Heliocentric radial velocity | 573 ± 2 km/s[1] |
| Distance | 4.932 ± 1.003 Mpc[1] |
| Apparent magnitude (V) | 13.0[1] |
| Apparent magnitude (B) | 13.4[1] |
| Characteristics | |
| Type | SBm[1] |
| Apparent size (V) | 3.0′ × 0.8′[1] |
| Other designations | |
| ESO 200-7, IRAS 03186-5222[1] | |
IC 1954 Group
Structure and star formation
NGC 1311’s structure is characteristic of a Magellanic barred spiral, with a weak bar and loosely wound spiral arms. Its star formation occurs in bursts, with 13 identified candidate star clusters showing ages clustered around 10 Myr, 100 Myr, and >1 Gyr. The galaxy’s isolation and low mass contribute to its distinct star-forming behavior, following the luminosity-metallicity relation typical of late-type dwarf galaxies.[11]
The Hubble Space Telescope revealed a population of star clusters with masses ranging from ~10³ to ~105 solar masses, with more massive clusters generally being older. Star formation is concentrated in two regions, each ~200 parsecs in size, at the east and west ends of a central bar-like structure. These regions host hot main-sequence stars and blue supergiants, with roughly half of the young stellar population located there.[12]