NGC 5962

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NGC 5962
NGC 5962, 32 inch Schulman Foundation telescope on Mt. Lemmon, courtesy Joseph D. Schulman.jpg
NGC 5962, 32 inch Schulman Foundation telescope on Mt. Lemmon, AZ
Observation data (J2000 epoch)
ConstellationSerpens Caput
Right ascension15h 36m 31.681s[1]
Declination+16° 36′ 27.93″[1]
Helio radial velocity1,957 km/s[2]
Distance119.5 Mly (36.64 Mpc)[2]
Group or clusterNGC 5962/5970 group[3]
Apparent magnitude (V)11.34[4]
Apparent magnitude (B)11.98[4]
Apparent size (V)1.490 × 1.073′[6] (NIR)
Other designations
NGC 5962, UGC 9926, LEDA 55588, MCG +03-40-011, PGC 55588[7][8]

NGC 5962 is a spiral galaxy in the equatorial constellation of Serpens Caput. It was discovered by the Anglo-German astronomer William Herschel on March 21, 1784.[9] The NGC 5962 galaxy is located at a distance of 120 million light years and is receding with a heliocentric radial velocity of 1,957 km/s.[2] It is the brightest member of the eponymously-named NGC 5962 group, which overlaps with the nearby NGC 5970 group; the two groups may be gravitationally bound.[3]

The morphological (shape) class of NGC 5962 in the infrared is SAB(rs,nrl)c. This notation indicates the galaxy has a bar structure around the nucleus (SAB), an inner pseudo-ring likely associated with the outer Lindblad resonance (rs), a ring-lens structure at the nucleus (nrl), and loosely-wound spiral arms (c).[5] In the optical band, this galaxy is classed as Hubble type SA(r)c,[10] displaying an inner ring with no visible bar. The galactic plane is inclined at an angle of 45°± to the line of sight from the Earth, giving it an oval profile with the major axis aligned along a position angle of 109°±.[11]

Ultraviolet image of the pseudo-ring structure in the center of the galaxy

Along with a populated nucleus, it has a relatively large core, but a small central bulge, in which the spiral arms begin to unfurl. There is some evidence for a low level of nuclear activity, and it has been classed as a nuclear H II region galaxy.[10] Based on its emission of far ultraviolet radiation, the pseudo-ring structure is actively undergoing star formation.[12] The galaxy is forming stars at the rate of M·yr−1.[13] There are two confirmed satellite galaxies; a third candidate proved to be too distant based on its redshift value.[14]

Two Type II-P supernova events have been detected in this galaxy: SN 2016afa was discovered February 12, 2016, then SN 2017ivu was spotted December 11, 2017.[15]


  1. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c Tully, R. Brent; et al. (2016). "Cosmicflows-3". The Astronomical Journal. 152 (2): 21. arXiv:1605.01765. Bibcode:2016AJ....152...50T. doi:10.3847/0004-6256/152/2/50. 50.
  3. ^ a b Zwaan, Martin A. (August 2001). "A targeted survey for H i clouds in galaxy groups". Monthly Notices of the Royal Astronomical Society. 325 (3): 1142–1148. arXiv:astro-ph/0103328. Bibcode:2001MNRAS.325.1142Z. doi:10.1046/j.1365-8711.2001.04514.x.
  4. ^ a b Gil de Paz, Armando; et al. (December 2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". The Astrophysical Journal Supplement Series. 173 (2): 185–255. arXiv:astro-ph/0606440. Bibcode:2007ApJS..173..185G. doi:10.1086/516636.
  5. ^ a b Herrera-Endoqui, M.; et al. (October 2015). "Catalogue of the morphological features in the Spitzer Survey of Stellar Structure in Galaxies (S4G)". Astronomy & Astrophysics. 582: 16. arXiv:1509.05328. Bibcode:2015A&A...582A..86H. doi:10.1051/0004-6361/201526047. A86.
  6. ^ Skrutskie, Michael F.; et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131: 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN 0004-6256.
  7. ^ "NASA/IPAC Extragalactic Database". Results for NGC 5962. Retrieved 2007-04-06.
  8. ^ "NGC 5962". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-12-29.
  9. ^ Seligman, Courtney. "NGC Objects: NGC 5950 - 5999". Celestial Atlas. Retrieved 2021-12-30.
  10. ^ a b Misselt, K. A.; et al. (November 1999). "Optical Long-Slit Spectroscopy of a Sample of Spiral Galaxies". The Publications of the Astronomical Society of the Pacific. 111 (765): 1398–1409. Bibcode:1999PASP..111.1398M. doi:10.1086/316450.
  11. ^ García-Gómez, C.; et al. (July 2004). "Deprojecting spiral galaxies using Fourier analysis. Application to the Ohio sample". Astronomy and Astrophysics. 421: 595–601. Bibcode:2004A&A...421..595G. doi:10.1051/0004-6361:20035735.
  12. ^ Comerón, S. (July 2013). "Inner rings in disc galaxies: dead or alive". Astronomy & Astrophysics. 555: 9. arXiv:1306.4515. Bibcode:2013A&A...555L...4C. doi:10.1051/0004-6361/201321983. L4.
  13. ^ Misiriotis, A.; et al. (April 2004). "Dust masses and star formation in bright IRAS galaxies. Application of a physical model for the interpretation of FIR observations". Astronomy and Astrophysics. 417: 39–50. arXiv:astro-ph/0312258. Bibcode:2004A&A...417...39M. doi:10.1051/0004-6361:20035602.
  14. ^ Mao, Yao-Yuan; et al. (February 2021). "The SAGA Survey. II. Building a Statistical Sample of Satellite Systems around Milky Way-like Galaxies". The Astrophysical Journal. 907 (2): 35. arXiv:2008.12783. Bibcode:2021ApJ...907...85M. doi:10.3847/1538-4357/abce58. 85.
  15. ^ Im, Myungshin; et al. (February 2019). "Intensive Monitoring Survey of Nearby Galaxies (IMSNG)". Journal of the Korean Astronomical Society. 52 (1): 11–21. arXiv:1901.11353. Bibcode:2019JKAS...52...11I. doi:10.5303/JKAS.2019.52.1.11.

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