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Galaxy in the constellation Reticulum From Wikipedia, the free encyclopedia
NGC 1559 is a barred spiral galaxy in the constellation Reticulum. It was discovered on 6 November 1826 by Scottish astronomer James Dunlop.[2]
| NGC 1559 | |
|---|---|
NGC 1559 imaged by the Hubble Space Telescope | |
| Observation data (J2000.0 epoch) | |
| Constellation | Reticulum |
| Right ascension | 4h 17m 35.8s[1] |
| Declination | −62° 47′ 1″[1] |
| Redshift | 1304 ± 4 km/s[1] |
| Apparent magnitude (V) | 11[1] |
| Characteristics | |
| Type | SB(s)cd[1] |
| Apparent size (V) | 3.5′ × 2.0′[1] |
| Other designations | |
| PGC 14814[1] | |
NGC 1559 is a Seyfert galaxy, i.e. it has a quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, the host galaxy is clearly detectable. Although it was originally thought to be a member of the Dorado Group,[3] subsequent observations have shown that it is in fact not a member of any galaxy group or cluster and does not have any nearby companions.[4][5] NGC 1559 has massive spiral arms and strong star formation.[4] It contains a small bar which is oriented nearly east-west and spans 40″.[4] Its bar and disc are the source of very strong radio emissions.[4]
Four supernovae have been observed in NGC 1559. Australian amateur astronomer Robert Evans[6] discovered the first three: SN 1984J (type II, mag. 13.5),[7] SN 1986L (type II, mag. 13.5),[8] and SN 2005df (Type Ia, mag 12.3).[9] SN 2009ib (type IIP, mag. 14.7)[10] was discovered on 6 August 2009.
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