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NGC 5962

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NGC 5962
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]
Heliocentric 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]
Characteristics
TypeSAB(rs,nrl)c[5]
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°±2° to the line of sight from the Earth, giving it an oval profile with the major axis aligned along a position angle of 109°±4°.[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 6 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]

References

  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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  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.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  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.

External links

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