NGC 2964

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NGC 2964
NGC2964-hst-R814GB40.jpg
Observation data (J2000 epoch)
ConstellationLeo
Right ascension 09h 42m 54.2s[1]
Declination31° 50′ 51″[1]
Redshift0.004430 ± 0.000040 [1]
Helio radial velocity1,328 ± 12 km/s[1]
Distance60.8 ± 11 Mly (18.7 ± 3.3 Mpc)[1]
Apparent magnitude (V)11.2 [2]
Characteristics
TypeSAB(r)bc [1]
Apparent size (V)2′.9 × 1′.6[1]
Other designations
UGC 5183, CGCG 152-056, MCG +05-23-027, B2 0939+32B, PGC 27777[1]

NGC 2964 is an intermediate spiral galaxy located in the constellation Leo. It is located at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 2964 is about 60,000 light years across. It was discovered by William Herschel on December 7, 1785.[3]

There is evidence that the galaxy has a weak bar running across the minor axis of the galaxy. The galaxy has four spiral arms, two emerging from ansae at each end of the bar and the others emerging near the centre of the bar, with the arms emerging from the ends of the bar being of higher surface brightness. All but the west arm have knotty appearance.[4] The outer parts of the galaxy present twisted stellar kinematics, but otherwise the rotation is quite regular.[5]

Spiral dust lanes have been observed running towards the centre, where star formation possibly takes place.[6] A circumnuclear ring observed in [OIII]/H-beta could the be site of active star formation.[5] Another indication of a nuclear star forming ring is the detection of double peaked carbon monoxide emission lines.[7] The central region of the galaxy has a stellar population of young-intermediate age, probably created by constant starburst activity that lasted for about 5 billion years.[8] The total star formation rate of NGC 2964 is estimated to be about 4 M per year.[9]

The nucleus of NGC 2964 appears to feature HII region activity.[10] The spectographic study of the nucleus revealed double peaked emission lines, which can be attributed to an ionisation cone created by an active galactic nucleus.[5] In the centre of NGC 2964 is believed to lie a supermassive black hole whose upper mass limit is estimated to be between 1.4 and 24 million M.[11]

NGC 2964 is the brightest galaxy in a galaxy group known as the NGC 2964 group. Other members of the group include NGC 2968, NGC 2970, NGC 3003, NGC 3011, NGC 3021. Other nearby galaxies include NGC 3118, NGC 3067, NGC 3032, NGC 3026, and their galaxy groups.[12] NGC 2964 forms a non-interacting pair with NGC 2968, which lies 5.8 arcminutes away.[8] A hydrogen bridge has been found to connect the two galaxies, while a tail extends towards NGC 2970.[13]

References[edit]

  1. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 2964. Retrieved 2019-01-18.
  2. ^ "Revised NGC Data for NGC 2964". spider.seds.org. Retrieved 25 November 2018.
  3. ^ NGC 2964 cseligman.com
  4. ^ Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near‐Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. arXiv:astro-ph/0206320. doi:10.1086/342340.
  5. ^ a b c Ganda, K.; Falcon-Barroso, J.; Peletier, R. F.; Cappellari, M.; Emsellem, E.; McDermid, R. M.; Tim de Zeeuw, P.; Carollo, C. M. (21 March 2006). "Late-type galaxies observed with SAURON: two-dimensional stellar and emission-line kinematics of 18 spirals". Monthly Notices of the Royal Astronomical Society. 367 (1): 46–78. doi:10.1111/j.1365-2966.2005.09977.x.
  6. ^ Carollo, C. M.; Stiavelli, M.; de Zeeuw, P. T.; Mack, J. (December 1997). "Spiral Galaxies with WFPC2.I.Nuclear Morphology, Bulges, Star Clusters, and Surface Brightness Profiles". The Astronomical Journal. 114: 2366. doi:10.1086/118654.
  7. ^ 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.
  8. ^ a b Ganda, Katia; Peletier, Reynier F.; McDermid, Richard M.; Falcón-Barroso, Jesús; De Zeeuw, P. T.; Bacon, Roland; Cappellari, Michele; Davies, Roger L.; Emsellem, Eric; Krajnović, Davor; Kuntschner, Harald; Sarzi, Marc; Van De Ven, Glenn (September 2007). "Absorption-line strengths of 18 late-type spiral galaxies observed with SAURON". Monthly Notices of the Royal Astronomical Society. 380 (2): 506–540. arXiv:0706.3624. doi:10.1111/j.1365-2966.2007.12121.x.
  9. ^ Zhou, Zhi-Min; Cao, Chen; Wu, Hong (25 November 2014). "Star Formation Properties in Barred Galaxies. III. Statistical Study of Bar-Driven Secular Evolution Using a Sample of Nearby Barred Spirals". The Astronomical Journal. 149 (1): 1. doi:10.1088/0004-6256/149/1/1.
  10. ^ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search for "Dwarf Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". The Astrophysical Journal Supplement Series. 112 (2): 315–390. doi:10.1086/313041.
  11. ^ Beifiori, A.; Sarzi, M.; Corsini, E. M.; Bontà, E. Dalla; Pizzella, A.; Coccato, L.; Bertola, F. (10 February 2009). "Upper Limits on the Masses of 105 Supermassive Black Holes from Hubble Space Telescope/Space Telescope Imaging Spectrograph Archival Data". The Astrophysical Journal. 692 (1): 856–868. doi:10.1088/0004-637X/692/1/856.
  12. ^ 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.
  13. ^ Walker, Lisa May; Johnson, Kelsey E.; Gallagher, Sarah C.; Privon, George C.; Kepley, Amanda A.; Whelan, David G.; Desjardins, Tyler D.; Zabludoff, Ann I. (25 January 2016). "Global properties of neutral hydrogen in compact groups". The Astronomical Journal. 151 (2): 30. doi:10.3847/0004-6256/151/2/30.

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