NGC 3656

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NGC 3656
Arp 155 - NGC 3656 (version 2).png
NGC 3656 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 11h 23m 38.7s [1]
Declination +53° 50′ 32″ [1]
Redshift 0.009640 ± 0.000037 [1]
Helio radial velocity 2,890 ± 11 km/s [1]
Distance 139 Mly (42.6 Mpc) [1]
Apparent magnitude  (V)12.3 [2]
Characteristics
Type (R')I0: pec [1]
Apparent size  (V)1.6′ × 1.6′ [1]
Notable featuresMerger remnant
Other designations
UGC 6403, Arp 155, VV 22a, CGCG 268-029, MCG +09-19-063, PGC 34989 [1]

NGC 3656 is a peculiar galaxy formed by the collision of two galaxies in the constellation of Ursa Major. It is located about 135 million light years away from Earth, which means, given its apparent dimensions, that NGC 3656 is approximately 70,000 light years across. It was discovered by William Herschel on April 14, 1789. [3]

Contents

Characteristics

NGC 3656 is a galaxy merger, created by the collision of two disk galaxies. The merger has created shells around the galaxy and two faint tidal tails. [4] The first tail emanates from a position angle of 260° and after bends to the north-northwest. Its total extent is about 180 arcseconds, towards a dwarf galaxy, and maybe even more, towards a second dwarf galaxy. Its width is 15 arcseconds. The other tail lies at the north-northeast part of the galaxy and is not as well defined as the other. [4] Other characteristics of the galaxy include the presence of a condensation at the south part of the galaxy connected with the rest of the galaxy with a ring-like feature and is associated with a bright shell. [4] [5]

A prominent feature of the galaxy is a dark lane running across the minor axis of the galaxy, similar to that observed in Centaurus A. [5] At the centre of the galaxy a warped molecular gas disk extending for about 7 kiloparsecs has been observed in H I imaging, with an estimated mass of 2×109M☉. [6] The inner part of the disk features more intense star formation. [7] The total star formation rate of the galaxy is estimated to be 1.1 M☉ per year. [8]

The nucleus of NGC 3656 has been found to rotate around an axis that is almost perpendicular to the rotation axis of the rest of the galaxy, which is another indication of a galaxy merger. [9]

Supernovae

Two supernovae have been observed in the galaxy, SN 1963K, with a peak apparent magnitude of 15, and SN 1973C, with a peak apparent magnitude of 17. Both supernovae were not specified as far as their type was concerned. [10]

Nearby galaxies

NGC 3656 is the foremost member in a galaxy group known as the NGC 3656 group. Another member is UGC 6422. A bit further away lies the galaxy NGC 3549 with its group. [11] Five dwarf galaxies with estimated masses between 2×108 and 2×109M☉ have been detected in HI imaging around the galaxy and are probably in the process of being accreted by NGC 3656. [6]

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<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

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<span class="mw-page-title-main">NGC 7674</span> Galaxy located in the constellation Pegasus

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<span class="mw-page-title-main">NGC 6907</span> Galaxy in the constellation Capricornus

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<span class="mw-page-title-main">NGC 5363</span> Galaxy in the constellation Virgo

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<span class="mw-page-title-main">NGC 2273</span> Galaxy in the constellation Lynx

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<span class="mw-page-title-main">NGC 1142</span> Interacting and distorted spiral galaxy in the constellation Cetus

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<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3656. Retrieved 2020-01-30.
  2. ↑ "Revised NGC Data for NGC 3656". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 3656 (= PGC 34989 = PGC 2452392 = Arp 155)". Celestial Atlas. Retrieved 19 November 2018.
  4. 1 2 3 Balcells, Marc (10 September 1997). "Two Tails in NGC 3656 and the Major Merger Origin of Shell and Minor-Axis Dust Lane Elliptical Galaxies". The Astrophysical Journal. 486 (2): L87–L90. arXiv: astro-ph/9707005 . Bibcode:1997ApJ...486L..87B. doi: 10.1086/310854 .
  5. 1 2 Balcells, Marc; Sancisi, Renzo (March 1996). "Gas Accretion in NGC 3656 (ARP 155)". The Astronomical Journal. 111: 1053. Bibcode:1996AJ....111.1053B. doi:10.1086/117850.
  6. 1 2 Balcells, Marc; van Gorkom, J. H.; Sancisi, Renzo; del Burgo, Carlos (October 2001). "HI in the Shell Elliptical Galaxy NGC 3656". The Astronomical Journal. 122 (4): 1758–1769. arXiv: astro-ph/0107165 . Bibcode:2001AJ....122.1758B. doi:10.1086/323310. S2CID   14421388.
  7. ↑ Young, Lisa M.; Bendo, George J.; Lucero, Danielle M. (1 February 2009). "Mid- to far-infrared emission and star formation in early-type galaxies". The Astronomical Journal. 137 (2): 3053–3070. arXiv: 0811.1381 . Bibcode:2009AJ....137.3053Y. doi: 10.1088/0004-6256/137/2/3053 .
  8. ↑ Smith, Beverly J.; Campbell, Kristen; Struck, Curtis; Soria, Roberto; Swartz, Douglas; Magno, Macon; Dunn, Brianne; Giroux, Mark L. (23 January 2018). "Diffuse X-Ray-emitting Gas in Major Mergers". The Astronomical Journal. 155 (2): 81. arXiv: 1712.04049 . Bibcode:2018AJ....155...81S. doi: 10.3847/1538-3881/aaa1a6 .
  9. ↑ Balcells, Marc; Stanford, S. A. (October 1990). "A counterrotating core in the merger remnant candidate NGC 3656 (ARP 155)". The Astrophysical Journal. 362: 443. Bibcode:1990ApJ...362..443B. doi:10.1086/169281.
  10. ↑ List of Supernovae IAU Central Bureau for Astronomical Telegrams. Retrieved 29 December 2015.
  11. ↑ 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 30 January 2020.


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