NGC 5033
| NGC5033 | |
|---|---|
 | |
| Observation data (J2000epoch) | |
| Constellation | Canes Venatici[1] |
| Right ascension | 13h13m27.5s[2] |
| Declination | +36° 35′ 38″[2] |
| Redshift | 875 ± 1 km/s[2] |
| Apparent magnitude(V) | 10.8[2] |
| Characteristics | |
| Type | SA(s)c[2] |
| Apparent size(V) | 10.7′× 5.0′[2] |
| Other designations | |
| UGC8307,[2]PGC45948[2] | |
NGC 5033is an inclinedspiral galaxylocated in the constellationCanes Venatici.Distance estimates vary from between 38 and 60 millionlight yearsfrom theMilky Way.The galaxy has a very bright nucleus and a relatively faint disk. Significant warping is visible in the southern half of the disk. The galaxy's relatively large angular size and relatively high surface brightness make it an object that can be viewed and imaged by amateur astronomers. The galaxy's location relatively nearEarthand itsactive galactic nucleusmake it a commonly studied object for professional astronomers.
Threesupernovaehave been observed in NGC 5033: SN 1950C (type unknown, mag. 16.6),[3]SN 1985L (Type II,mag. 12.5),[4]and SN 2001gd (type IIb, mag. 16.5).[5]
Nucleus
[edit]NGC 5033 contains aSeyfertnucleus, a type ofactive galactic nucleus.[6]Like many other active galactic nuclei, this galaxy's nucleus is thought to contain asupermassive black hole.The bright emission seen in visible light (as well as other wavebands) is partially produced by the hot gas in the environment around this black hole.
Integral field spectroscopicobservations of the center of NGC 5033 indicate that the Seyfert nucleus is not located at the kinematic center of the galaxy (the point around which the stars in the galaxies rotate).[7]This has been interpreted as evidence that this galaxy has undergone a merger. The displacement of the Seyfert nucleus from the kinematic center may destabilize the rotation of gas in the center of the galaxy, which could cause gas to fall into the Seyfert nucleus. The gas would be compressed by the enormous gravitational forces in the center of the Seyfert nucleus and become hot, thus making the nucleus appear bright or "active".
Nearby galaxies
[edit]NGC 5033 and the nearby spiral galaxyNGC 5005comprise a physical galaxy pair.[8]The two galaxies weakly influence each other gravitationally, but they are not yet close enough to each other to be distorted by the tidal forces of the gravitational interaction. The fainterirregular galaxyIC 4182 is also a member of this group.
References
[edit]- ^R. W. Sinnott, ed. (1988).The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer.Sky Publishing Corporation and Cambridge University Press.ISBN978-0-933346-51-2.
- ^abcdefgh"NASA/IPAC Extragalactic Database".Results for NGC 5033.Retrieved2006-11-15.
- ^Transient Name Server entry for SN 1950C.Retrieved 28 March 2023.
- ^Transient Name Server entry for SN 1985L.Retrieved 28 March 2023.
- ^Transient Name Server entry for SN 2001gd.Retrieved 28 March 2023.
- ^L. C. Ho; A. V. Filippenko; W. L. W. Sargent (1997). "A Search for" Dwarf "Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies".Astrophysical Journal Supplement.112(2): 315–390.arXiv:astro-ph/9704107.Bibcode:1997ApJS..112..315H.doi:10.1086/313041.S2CID17086638.
- ^E. Meiavilla; A. Guijarro; A. Castillo-Morales; et al. (2005). "Asymmetrical structure of ionization and kinematics in the Seyfert galaxy NGC 5033".Astronomy and Astrophysics.433(1): 79–86.arXiv:astro-ph/0412410.Bibcode:2005A&A...433...79M.doi:10.1051/0004-6361:20034537.S2CID16034143.
- ^G. Helou; E. E. Salpeter; Y. Terzian (1982). "Neutral hydrogen in binary and multiple galaxies".Astronomical Journal.87:1443–1464.Bibcode:1982AJ.....87.1443H.doi:10.1086/113235.
External links
[edit]
Media related toNGC 5033at Wikimedia Commons
