Astronomy:NGC 2613
| NGC 2613 | |
|---|---|
.jpg) | |
| Observation data (J2000 epoch) | |
| Constellation | Pyxis |
| Right ascension | 08h 33m 22.841s[1] |
| Declination | −22° 58′ 25.21″[1] |
| Redshift | 0.005591[2] |
| Helio radial velocity | 1,675 km/s[3] |
| Distance | 78 Mly (24 Mpc)[3] |
| Apparent magnitude (V) | 11.6[2] |
| Characteristics | |
| Type | SA(s)b[4] |
| Mass | (7.50±0.87)×1011 M☉.[5] M☉ |
| Apparent size (V) | 7′.59 × 1′.70[6] |
| Notable features | Edge-on galaxy |
| Other designations | |
| IRAS 08311-2248, MCG-04-21-003, UGCA 141, PGC 23997[7] | |
NGC 2613 is a spiral galaxy in the southern constellation of Pyxis, next to the western constellation border with Puppis. It was discovered by the German-born astronomer William Herschel on November 20, 1784.[8] With an apparent visual magnitude of 10.5, the galaxy is faintly visible using a telescope with a 100 mm (4 in) aperture. It appears spindle-shaped as it is almost edge-on to observers on Earth.[9]
The morphological classification of NGC 2613 is SA(s)b,[4] indicating a spiral galaxy with no bar or ring, and moderately tightly-wound spiral arms. It is inclined by an angle of approximately 79° to the line of sight from the Earth[5] and is oriented with the long axis along a position angle of 133°.[4] The radius of neutral hydrogen in the galaxy is about 35 kpc,[10] and the mass of the neutral hydrogen is (8.73±0.32)×109 M☉. The galaxy has a combined dynamic mass of (7.50±0.87)×1011 M☉.[5]
NGC 2613 has an active galactic nucleus that is deeply embedded in obscuring gas and dust.[5] Emission data collected by the Very Large Array shows a feature resembling a tidal tail along the southeast side of the galaxy, which was most likely produced by an interaction with the small companion galaxy, ESO 495-G017, now located to the northwest of NGC 2613.[10]
On 20 March 2023, a supernova was observed in NGC 2613: SN 2023dtc (Type Ib, mag. 18).[11]
References
- ↑ 1.0 1.1 Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W. et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal 131 (2): 1163–1183. doi:10.1086/498708. ISSN 0004-6256. Bibcode: 2006AJ....131.1163S.
- ↑ 2.0 2.1 "NASA/IPAC Extragalactic Database". Results for NGC 6946. http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+2613&img_stamp=yes&extend=no.
- ↑ 3.0 3.1 Tully, R. Brent et al. (August 2016). "Cosmicflows-3". The Astronomical Journal 152 (2): 21. doi:10.3847/0004-6256/152/2/50. 50. Bibcode: 2016AJ....152...50T.
- ↑ 4.0 4.1 4.2 Chaves, Tara A.; Irwin, Judith A. (August 2001). "High-Latitude H I in NGC 2613: Structure and Dynamics". The Astrophysical Journal 557 (2): 646–658. doi:10.1086/321686. Bibcode: 2001ApJ...557..646C.
- ↑ 5.0 5.1 5.2 5.3 Li, Z. et al. (September 2006). "An XMM-Newton observation of the massive edge-on Sb galaxy NGC 2613". Monthly Notices of the Royal Astronomical Society 371 (1): 147–156. doi:10.1111/j.1365-2966.2006.10682.x. Bibcode: 2006MNRAS.371..147L.
- ↑ Paturel, G. et al. (December 2003). "HYPERLEDA. I. Identification and designation of galaxies". Astronomy and Astrophysics 412: 45–55. doi:10.1051/0004-6361:20031411. Bibcode: 2003A&A...412...45P.
- ↑ "NGC 2613". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NGC+2613.
- ↑ Seligman, Courtney. "NGC Objects: NGC 2600 - 2649". Celestial Atlas. https://cseligman.com/text/atlas/ngc26.htm#2613.
- ↑ O'Meara, Stephen James (2007). Steve O'Meara's Herschel 400 Observing Guide. Cambridge, United Kingdom: Cambridge University Press. p. 82. ISBN 978-0-521-85893-9. https://books.google.com/books?id=Nyh9fAC_tpIC&pg=PA82.
- ↑ 10.0 10.1 Irwin, Judith A.; Chaves, Tara (March 2003). "High-Latitude H I in NGC 2613: Buoyant Disk-Halo Outflow". The Astrophysical Journal 585 (1): 268–280. doi:10.1086/345891. Bibcode: 2003ApJ...585..268I.
- ↑ Transient Name Server entry for SN 2023dtc. Retrieved 21 March 2023.
External links
 |  |
