NGC 3396 is a peculiar barred irregular galaxy in the constellation Leo Minor. The galaxy lies about 80 million light years away from Earth, which means, given its apparent dimensions, that NGC 3396 is approximately 85,000 light years across.[1] It was discovered by William Herschel on December 7, 1785.[3]
| NGC 3396 | |
|---|---|
 NGC 3396 by Sloan Digital Sky Survey | |
| Observation data (J2000 epoch) | |
| Constellation | Leo Minor |
| Right ascension | 10h 49m 55.1s[1] |
| Declination | +32° 59′ 27″[1] |
| Redshift | 0.005537 ± 0.000002 [1] |
| Heliocentric radial velocity | 1,660 ± 1 km/s[1] |
| Distance | 81 ± 23 Mly (24.9 ± 4.4 Mpc)[1] |
| Apparent magnitude (V) | 12.0[2] |
| Characteristics | |
| Type | IBm pec [1] |
| Apparent size (V) | 2.9′ × 1.2′[1] |
| Notable features | Interacting galaxy |
| Other designations | |
| UGC 5935, Arp 270, VV 246b, MCG +06-24-018, PGC 32434 | |
Characteristics
editNGC 3396 forms an interacting pair with NGC 3395, a spiral galaxy that lies 1.5 arcminutes from NGC 3396. The mass ratio of the two galaxies is about 1.5 to 1, with NGC 3395 being the more massive of the two. The two galaxies appear separate but a bridge of material is visible between them and tidal tails are observed.[4] Dynamical modelling of the pair suggests that the two galaxies had a first close encounter in the past, which resulting in gas been stripped from NGC 3395 and forming a tidal tail to the south-east.[5] A second close encounter took place about 50 million years ago, resulting to starburst activity. The two galaxies will most likely merge in the next 500 million years.[5]
The galaxy hosts a number of HII regions that are star forming[6] with the region of most intense star formation being in the center of the galaxy.[7] The average size of the knots in NGC 3396 is an order of magnitude larger than those in NGC 3395.[8] The central region of NGC 3396 is estimated to host 1,000 to 2,000 Wolf-Rayet stars and tens of thousands of O-type stars.[7] The star formation rate in the circumnuclear is estimated to be 0.15 M☉ per year and in the rest of the galaxy 0.39 M☉.[6]
The nucleus of the galaxy has been found to be active and based on its spectrum it has been categorised as a LINER.[7] Kinematic analysis of the gas indicates there is gas inflow to the centre of the galaxy along its bar and also there is an biconal outflow element that could be galactic wind from a supermassive black hole in the nucleus.[6]
Nearby galaxies
editThe NGC 3395/3396 pair is part of the NGC 3430 Group or LGG 218. Other members of the group include the galaxies NGC 3381, NGC 3424, NGC 3430, NGC 3442, and IC 2604.[9][10] IC 2604 lies 14 arcmin to the south-west of the pair and IC 2608 14 arcmin to the south-east.[5] The group is part of the Leo II groups, which is part of the Virgo Supercluster.[11]
References
edit- ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3396. Retrieved 2024-03-26.
- ^ "Revised NGC Data for NGC 3396". spider.seds.org. Retrieved 30 March 2024.
- ^ Seligman, Courtney. "NGC 3396 (= PGC 32434, and with NGC 3395 = Arp 270)". Celestial Atlas. Retrieved 19 November 2018.
- ^ Braine, J.; Combes, F.; Casoli, F.; Dupraz, C.; Gerin, M.; Klein, U.; Wielebinski, R.; Brouillet, N. (1 March 1993). "A CO(1-0) and CO(2-1) survey of nearby spiral galaxies. I. Data and observations". Astronomy and Astrophysics Supplement Series. 97: 887–936. Bibcode:1993A&AS...97..887B. ISSN 0365-0138.
- ^ a b c Clemens, M. S.; Baxter, K. M.; Alexander, P.; Green, D. A. (19 September 1999). "Observations and modelling of the interacting galaxies NGC 3395 and 3396". Monthly Notices of the Royal Astronomical Society. 308 (2): 364–376. Bibcode:1999MNRAS.308..364C. doi:10.1046/j.1365-8711.1999.02730.x.
- ^ a b c Zaragoza-Cardiel, J.; Font-Serra, J.; Beckman, J. E.; Blasco-Herrera, J.; García-Lorenzo, B.; Camps, A.; Gonzalez-Martin, O.; Ramos Almeida, C.; Loiseau, N.; Gutiérrez, L. (17 April 2013). "Kinematics of Arp 270: gas flows, nuclear activity and two regimes of star formation". Monthly Notices of the Royal Astronomical Society. 432 (2): 998–1009. arXiv:1303.5020. doi:10.1093/mnras/stt527.
- ^ a b c Weistrop, D.; Nelson, C. H.; Angione, R.; Bachilla, R. (1 January 2020). "Physical Properties of the Star-forming Regions in the Interacting Galaxies NGC 3395/NGC 3396". The Astronomical Journal. 159 (1): 17. Bibcode:2020AJ....159...17W. doi:10.3847/1538-3881/ab58d3.
- ^ Hancock, Mark; Weistrop, Donna; Eggers, Diane; Nelson, Charles H. (April 2003). "Star-forming Knots in the UV-bright Interacting Galaxies NGC 3395 and NGC 3396". The Astronomical Journal. 125 (4): 1696–1710. Bibcode:2003AJ....125.1696H. doi:10.1086/368234.
- ^ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN 0365-0138.
- ^ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025.
- ^ "The Leo II Groups". www.atlasoftheuniverse.com. Retrieved 1 April 2024.
External links
edit
- NGC 3396 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images