NGC 3395
| NGC 3395 | |
|---|---|
 NGC 3395 by Sloan Digital Sky Survey | |
| Observation data (J2000 epoch) | |
| Constellation | Leo Minor |
| Right ascension | 10h 49m 50.1s[1] |
| Declination | +32° 58′ 58″[1] |
| Redshift | 0.005394 ± 0.000002 [1] |
| Heliocentric radial velocity | 1,617 ± 1 km/s[1] |
| Distance | 54 ± 23 Mly (16.6 ± 6.9 Mpc)[1] |
| Apparent magnitude (V) | 11.8[2] |
| Characteristics | |
| Type | SAB(rs)cd pec [1] |
| Apparent size (V) | 2.1′ × 1.2′[1] |
| Notable features | Interacting galaxy |
| Other designations | |
| IC 2613, UGC 5931, Arp 270, VV 246b, MCG +06-24-017, PGC 32424 | |
NGC 3395 is a peculiar spiral galaxy in the constellation Leo Minor. The galaxy lies about 55 million light years away from Earth, which means, given its apparent dimensions, that NGC 3395 is approximately 35,000 light years across.[1] It was discovered by William Herschel on December 7, 1785.[3] NGC 3395 interacts with NGC 3396.
NGC 3395 forms an interacting pair with NGC 3396, a magellanic spiral galaxy that lies 1.5 arcminutes from the nucleus of NGC 3395. The mass ratio of the two galaxies is about 1.5 to 1. 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 northwest of the center, while star formation has also being in observed in the end of the spiral arm northeast of the nucleus and in three regions in the bridge between the two galaxies.[7] Three more star forming regions are visible in a tail southwest of the galaxy.[8] The average size of the knots in NGC 3395 is an order of magnitude smaller than those in NGC 3396.[9] The nucleus of NGC 3395 doesn't appear to be active.[7]
The 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.[10][11] 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.[12]
References[edit]
- ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 3395. Retrieved 2024-03-26.
- ^ "Revised NGC Data for NGC 3395". spider.seds.org. Retrieved 30 March 2024.
- ^ Seligman, Courtney. "NGC 3395 (= IC 2613 = PGC 32424, and with NGC 3396 = 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.
- ^ 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 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.
- ^ Smith, Beverly J.; Soria, Roberto; Struck, Curtis; Giroux, Mark L.; Swartz, Douglas A.; Yukita, Mihoko (10 February 2014). "Extra-Nuclear Starbursts: Young Luminous Hinge Clumps in Interacting Galaxies". The Astronomical Journal. 147 (3): 60. arXiv:1401.0338. Bibcode:2014AJ....147...60S. doi:10.1088/0004-6256/147/3/60.
- ^ 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. Archived from the original on 31 January 2016. Retrieved 20 March 2017.
- ^ "The Leo II Groups". www.atlasoftheuniverse.com. Retrieved 1 April 2024.
External links[edit]
- NGC 3395 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
