NGC 1022 is a barred spiral galaxy located approximately 68[1] million light years away in the equatorial constellation of Cetus. It was discovered on September 10, 1785, by William Herschel. NGC 1022 is a member of the Cetus-Aries group of galaxies.[3]
| NGC 1022 | |
|---|---|
 | |
| Observation data (J2000 epoch) | |
| Constellation | Cetus |
| Right ascension | 02h 38m 32.74s[1] |
| Declination | −06° 40′ 38.96″[1] |
| Redshift | 0.004847[1] |
| Heliocentric radial velocity | 1,453 km/s |
| Distance | 67.7 Mly (20.75 Mpc)[1] |
| Apparent magnitude (V) | 11.34±0.13[2] |
| Apparent magnitude (B) | 12.09±0.13[2] |
| Characteristics | |
| Type | SBa[1] (R')SB(s)a;HII[2] SBa(r)p[3] |
| Apparent size (V) | 2.4′ × 2.0′[2] |
| Other designations | |
| NGC 1022, PGC 10010 | |
This galaxy has a morphological classification SBa,[1] indicating a central bar and tightly wound spiral arms. The elliptical outline of the galaxy has an isophotal axis ratio of 0.78[1] with an angular size of 2.4′ by 2.0′ and a position angle of 115°.[2] The galactic plane is inclined at an angle of 24° to the line of sight from the Earth. The central bar is boxy in shape with narrow spurs that are offset from the main axis.[4]
NGC 1022 is forming new stars at an estimated rate of 1.1 solar masses per year. Infrared observations of the nucleus suggests a high rate of star formation activity.[5] The circumnuclear region is home to three giant H II regions with one at the nucleus, a second to the northeast, and the third slightly to the northwest.[3] The galaxy was observed as part of a Hubble study of black holes.[6]
References
edit- ^ a b c d e f g h Ann, H. B.; et al. (2015). "A Catalog of Visually Classified Galaxies in the Local (z ~ 0.01) Universe". The Astrophysical Journal Supplement Series. 217 (2): 27–49. arXiv:1502.03545. Bibcode:2015ApJS..217...27A. doi:10.1088/0067-0049/217/2/27. S2CID 119253507.
- ^ a b c d e Gil de Paz, Armando; et al. (December 2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". The Astrophysical Journal Supplement Series. 173 (2): 185–255. arXiv:astro-ph/0606440. Bibcode:2007ApJS..173..185G. doi:10.1086/516636. S2CID 119085482.
- ^ a b c Franco, José; et al. (November 2000). "Decreasing Density Gradients in Circumnuclear H II Regions of Barred Galaxies NGC 1022, NGC 1326, and NGC 4314". The Astrophysical Journal. 544 (1): 277–282. arXiv:astro-ph/0007040. Bibcode:2000ApJ...544..277F. doi:10.1086/317189. S2CID 119012558.
- ^ Erwin, Peter; Debattista, Victor P. (June 2013). "Peanuts at an angle: detecting and measuring the three-dimensional structure of bars in moderately inclined galaxies". Monthly Notices of the Royal Astronomical Society. 431 (4): 3060–3086. arXiv:1301.0638. Bibcode:2013MNRAS.431.3060E. doi:10.1093/mnras/stt385.
- ^ Garcia-Barreto, J. A.; et al. (December 1991). "Circumnuclear star formation in the barred galaxy NGC 1022". Astronomy and Astrophysics. 252: 19. Bibcode:1991A&A...252...19G.
- ^ Garner, Rob (2020-01-24). "Hubble Sees Dusty Galaxy With Supermassive Center". NASA. Retrieved 2020-06-17.
External links
edit- "NASA/IPAC Extragalactic Database". Results for NGC 1022. Retrieved 2016-11-01.
- "Supermassive Influence". www.spacetelescope.org/. Retrieved 20 January 2020.
- "DSO Browser". Galaxy NGC 1022. Retrieved 2016-11-24.
Media related to NGC 1022 at Wikimedia Commons
