NGC 3396

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NGC 3396
NGC3396 - SDSS DR14.jpg
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 featuresInteracting galaxy
Other designations
UGC 5935, Arp 270, VV 246b, MCG +06-24-018, PGC 32434

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]

Contents

Characteristics

NGC 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

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. [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]

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<span class="mw-page-title-main">NGC 753</span> Galaxy in the constellation Andromeda

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<span class="mw-page-title-main">NGC 759</span> Galaxy in the constellation Andromeda

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<span class="mw-page-title-main">NGC 3665</span> Galaxy in the constellation Ursa Major

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<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

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<span class="mw-page-title-main">NGC 691</span> Galaxy in the constellation Aries

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<span class="mw-page-title-main">NGC 680</span> Galaxy in the constellation Aries

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<span class="mw-page-title-main">NGC 973</span> Galaxy in the constellation Triangulum

NGC 973 is a giant spiral galaxy located in the constellation Triangulum. It is located at a distance of circa 200 million light-years from Earth, which, given its apparent dimensions, means that NGC 973 is about 230,000 light years across. It was discovered by Lewis Swift on October 30, 1885.

<span class="mw-page-title-main">NGC 2974</span> Galaxy in the constellation Sextans

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<span class="mw-page-title-main">NGC 1241</span> Galaxy in the constellation Eridanus

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<span class="mw-page-title-main">NGC 4324</span> Galaxy in the constellation of Virgo

NGC 4324 is a lenticular galaxy located about 85 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on March 4, 1862. NGC 4324 has a stellar mass of 5.62 × 1010M☉, and a baryonic mass of 5.88 × 1010M☉. The galaxy's total mass is around 5.25 × 1011M☉. NGC 4324 is notable for having a ring of star formation surrounding its nucleus. It was considered a member of the Virgo II Groups until 1999, when its distance was recalculated and it was placed in the Virgo W Group.

<span class="mw-page-title-main">Leo II Groups</span> Series of galaxy clusters

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<span class="mw-page-title-main">NGC 871</span> Barred spiral galaxy in Aries

NGC 871 is a barred spiral galaxy in the Aries constellation. Its discovery and first description was realized by William Herschel on October 14, 1784 and the findings made public through his Catalogue of Nebulae and Clusters of Stars in 1786.

<span class="mw-page-title-main">NGC 2445</span> Galaxy in the constellation Lynx

NGC 2445 is a peculiar ring galaxy in the constellation Lynx. The galaxy lies about 200 million light years away from Earth, which means, given its apparent dimensions, that NGC 2445 is approximately 100,000 light years across. It was discovered by Édouard Stephan on January 18, 1877. The galaxy interacts with another galaxy, NGC 2444, and as a result its shape is distorted and new stars are formed.

<span class="mw-page-title-main">NGC 5953</span> Galaxy in the constellation Serpens

NGC 5953 is a peculiar spiral galaxy in the constellation Serpens. The galaxy lies about 80 million light years away from Earth, which means, given its apparent dimensions, that NGC 5953 is approximately 35,000 light years across. It was discovered by William Herschel on April 17, 1784. NGC 5953 interacts with NGC 5954 forming a pair known as Arp 91.

<span class="mw-page-title-main">NGC 3395</span> Galaxy in the constellation Leo Minor

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. It was discovered by William Herschel on December 7, 1785. NGC 3395 interacts with NGC 3396.

<span class="mw-page-title-main">NGC 3995</span> Galaxy in the constellation Ursa Major

NGC 3995 is a Magellanic spiral galaxy in the constellation Ursa Major. The galaxy lies about 100 million light years away from Earth based on the Tully–Fisher relation, which means, given its apparent dimensions, that NGC 3995 is approximately 80,000 light years across, while based on redshift it lies 170 million light years away. It was discovered by Heinrich d'Arrest on February 5, 1864.

<span class="mw-page-title-main">NGC 3994</span> Galaxy in the constellation Ursa Major

NGC 3994 is a spiral galaxy in the constellation Ursa Major. The galaxy lies about 160 million light years away from Earth, which means, given its apparent dimensions, that NGC 3994 is approximately 70,000 light years across. It was discovered by Heinrich d'Arrest on April 6, 1864.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3396. Retrieved 2024-03-26.
  2. ↑ "Revised NGC Data for NGC 3396". spider.seds.org. Retrieved 30 March 2024.
  3. ↑ Seligman, Courtney. "NGC 3396 (= PGC 32434, and with NGC 3395 = Arp 270)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ 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.
  5. 1 2 3 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 .
  6. 1 2 3 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 .
  7. 1 2 3 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 .
  8. ↑ 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.
  9. ↑ 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.
  10. ↑ 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.
  11. ↑ "The Leo II Groups". www.atlasoftheuniverse.com. Retrieved 1 April 2024.
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