NGC 4710

In this article we are going to explore NGC 4710, a topic that has captured the interest of many people in recent years. NGC 4710 is a fascinating topic that has generated a great debate in different areas, from science to popular culture. Throughout this article, we will examine different aspects related to NGC 4710, from its history and evolution, to its impact on today's society. In addition, we will analyze different perspectives and opinions on NGC 4710, with the aim of providing a complete and objective view on this topic. Without a doubt, NGC 4710 is a fascinating topic that leaves no one indifferent, and we are sure that this article will be of great interest to all types of readers.

NGC 4710
Hubble Space Telescope image of NGC 4710
Observation data (J2000 epoch)
ConstellationComa Berenices
Right ascension12h 49m 38.958s[1]
Declination+15° 09′ 55.76″[1]
Redshift0.00397±0.00011[2]
Heliocentric radial velocity1,129 km/s[3]
Distance54.5 ± 3.6 Mly (16.7 ± 1.1 Mpc)[4]
Apparent magnitude (V)11.9[5]
Apparent magnitude (B)11.60[3]
Characteristics
TypeS0a-S0/Sa[3]
Apparent size (V)3.0′ × 0.8′[3]
Other designations
NGC 4710, UGC 7980, PGC 43375[6][5]

NGC 4710 is an edge-on lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 21, 1784 by German-British astronomer William Herschel.[7] This galaxy has a B-band visual magnitude of 11.60 and an angular size of 3.0′ × 0.8′.[3] It is located at a distance of 54.5 ± 3.6 million light-years (16.7 ± 1.1 Mpc) from the Milky Way,[4] and is receding with a heliocentric radial velocity of 1,129 km/s.[3] This is a member of the Virgo Cluster, with a projected offset of ~6° from the cluster center and a cluster crossing time of around two billion years.[8]

The morphological classification of NGC 4710 is S0 or SA(r)0,[9] which indicates this is an unbarred lenticular galaxy[8] (SA) with an inner ring structure (r). It is inclined at an angle of 86° to the plane of the sky, with the major axis aligned along a position angle of 207°.[10] NGC 4710 has a relatively high gas abundance with a dusty nucleus. The stellar velocity distribution is characteristic of galaxies with a small bulge. Like the Milky Way, it has an X-shaped bulge which is a probable bar structure; hence it is likely a barred lenticular.[9][11] The star formation rate is 0.11±0.02 M☉·yr−1.[10] NGC 4710 possesses both thin and thick discs.[12]

Further reading

  • Gonzalez, Oscar A.; et al. (March 2017). "Peanut-shaped metallicity distributions in bulges of edge-on galaxies: the case of NGC 4710". Monthly Notices of the Royal Astronomical Society: Letters. 466 (1): L93 – L97. arXiv:1611.09547. Bibcode:2017MNRAS.466L..93G. doi:10.1093/mnrasl/slw232.
  • Welch, G. A.; Mitchell, G. F. (June 1994). "A Study of Molecular Gas in the Center of the S0 Galaxy NGC 4710". The Astrophysical Journal. 427: 770. Bibcode:1994ApJ...427..770W. doi:10.1086/174183.
  • Sage, L. J. (November 1990). "The properties and origins of molecular gas in the lenticular galaxies NGC 404, 4710 and 5195". Astronomy and Astrophysics. 239: 125–136. Bibcode:1990A&A...239..125S.

References

  1. ^ a b Skrutskie, Michael F.; et al. (February 1, 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN 0004-6256. S2CID 18913331.
  2. ^ Abazajian, Kevork N.; et al. (2009). "The Seventh Data Release of the Sloan Digital Sky Survey". The Astrophysical Journal Supplement Series. 182 (2): 543–558. arXiv:0812.0649. Bibcode:2009ApJS..182..543A. doi:10.1088/0067-0049/182/2/543. S2CID 14376651.
  3. ^ a b c d e f Boselli, A.; et al. (2014). "The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). IV. The role of the cluster environment on galaxy evolution". Astronomy & Astrophysics. 570: A69. arXiv:1407.4986. Bibcode:2014A&A...570A..69B. doi:10.1051/0004-6361/201424419. S2CID 119244700. A69.
  4. ^ a b Haynes, Martha P.; et al. (July 2018). "The Arecibo Legacy Fast ALFA Survey: The ALFALFA Extragalactic H I Source Catalog". The Astrophysical Journal. 861 (1): 49. arXiv:1805.11499. Bibcode:2018ApJ...861...49H. doi:10.3847/1538-4357/aac956. 49.
  5. ^ a b "NASA/IPAC Extragalactic Database". Results for NGC 4710. Retrieved 2007-04-02.
  6. ^ "NGC 4710". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-09-22.
  7. ^ Seligman, Courtney. "NGC Objects: NGC 4700 - 4749". Celestial Atlas. Retrieved 2024-04-10.
  8. ^ a b Wrobel, J. M.; Kenney, Jeffrey D. P. (November 1992). "Nuclear Molecular Gas in the Virgo Cluster S0 Galaxy NGC 4710". Astrophysical Journal. 399: 94. Bibcode:1992ApJ...399...94W. doi:10.1086/171905.
  9. ^ a b Gonzalez, O. A.; et al. (June 2016). "Comparing the properties of the X-shaped bulges of NGC 4710 and the Milky Way with MUSE". Astronomy & Astrophysics. 591. id. A7. arXiv:1603.02546. Bibcode:2016A&A...591A...7G. doi:10.1051/0004-6361/201527806.
  10. ^ a b Topal, Selçuk; et al. (December 2016). "Molecular gas kinematics and line diagnostics in early-type galaxies: NGC 4710 and NGC 5866". Monthly Notices of the Royal Astronomical Society. 463 (4): 4121–4152. arXiv:1609.01506. Bibcode:2016MNRAS.463.4121T. doi:10.1093/mnras/stw2257. {{cite journal}}: |last2= has generic name (help)
  11. ^ Bogdan, C. Ciambur; Graham, Alister W. (June 2016). "Quantifying the (X/peanut)-shaped structure in edge-on disc galaxies: length, strength, and nested peanuts". Monthly Notices of the Royal Astronomical Society. 459 (2): 1276–1292. arXiv:1603.00019. Bibcode:2016MNRAS.459.1276C. doi:10.1093/mnras/stw759. S2CID 118991786.
  12. ^ Kasparova, A. (2016). "The Diversity of Thick Galactic Discs". Monthly Notices of the Royal Astronomical Society: Letters. 460 (1): 89–93. arXiv:1604.07624. Bibcode:2016MNRAS.460L..89K. doi:10.1093/mnrasl/slw083. S2CID 119303521.