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NGC 4294

Summary

NGC 4294 is a barred spiral galaxy[2] with flocculent spiral arms[3] located about 55 million light-years away[2] in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784[4] and is a member of the Virgo Cluster.[5][6][7]

NGC 4294
SDSS image of NGC 4294
Observation data (J2000 epoch)
ConstellationVirgo
Right ascension12h 21m 17.8s[1]
Declination11° 30′ 38″[1]
Redshift0.001184[1]
Heliocentric radial velocity355 km/s[1]
Distance55 Mly (17 Mpc)[1]
Group or clusterVirgo Cluster
Apparent magnitude (V)12.5[1]
Characteristics
TypeSB(s)cd[1]
Size~52,000 ly (16 kpc) (estimated)[1]
Apparent size (V)3.2 x 1.2[1]
Other designations
KCPG 330B, VCC 465, IRAS 12187+1147, UGC 7407, MCG +02-32-009, PGC 39925, CGCG 70-24, SDSS J122117.82+113037.6[1]

NGC 4294 appears to be undergoing ram-pressure[8][9] stripping edge-on.[8]

Physical characteristics edit

NGC 4294 hosts many H II regions.[10][3]

Interaction with NGC 4299 edit

NGC 4294 appears to be in a pair with NGC 4299[11][12][10][13][9][14][15] and may be possibly tidally interacting.[11][12][10][13][3][9][14][15]

Effects of a tidal interaction on NGC 4294 are evident as the galaxy has a disturbed optical and HI morphology,[12][10] a high global star formation rate,[13][3] and has an observed asymmetry in polarized radio continuum emission.[15]

HI tail edit

Chung et al. identified that NGC 4294 has a one sided[16][17] 88,000 ly (27 kpc) tail of neutral atomic hydrogen (HI).[9][18] The tail points to the southwest[16][14] and appears to be a result of ram-pressure.[18][19][9] The tail has no optical counterpart[9][16] and is oriented parallel to the HI tail found in NGC 4299.[16]

As the tail has no optical counterpart, this makes the probability of the tail being caused by tidal interaction low. However, NGC 4299 lies 88,000 ly (27 kpc) from NGC 4294 and the two galaxies have almost the same velocity, with a difference of 120 km/s. This means that the scenario of the tail originating from a tidal interaction cannot be ruled out entirely.[9]

Black Hole edit

NGC 4294 may harbor an intermediate-mass black hole with an estimated mass ranging from 3,000 (3*10^3) to 20,000 (2*10^4) solar masses.[20]

References edit

  1. ^ a b c d e f g h i j "Results for NGC 4294". NASA/IPAC Extragalactic Database. Retrieved 2021-12-13.
  2. ^ a b "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2019-02-21.
  3. ^ a b c d Fathi, K.; Beckman, J. E.; Piñol-Ferrer, N.; Hernandez, O.; Martínez-Valpuesta, I.; Carignan, C. (2009-10-20). "PATTERN SPEEDS OF BARS AND SPIRAL ARMS FROM Hα VELOCITY FIELDS". The Astrophysical Journal. 704 (2): 1657–1675. arXiv:0909.1816. Bibcode:2009ApJ...704.1657F. doi:10.1088/0004-637X/704/2/1657. ISSN 0004-637X. S2CID 118625116.
  4. ^ "New General Catalog Objects: NGC 4250 - 4299". cseligman.com. Retrieved 2018-08-14.
  5. ^ Binggeli, B.; Sandage, A.; Tammann, G. A. (September 1985). "Studies of the Virgo Cluster. II - A catalog of 2096 galaxies in the Virgo Cluster area. V - Luminosity functions of Virgo Cluster galaxies". The Astronomical Journal. 90: 1681. Bibcode:1985AJ.....90.1681B. doi:10.1086/113874. ISSN 0004-6256.
  6. ^ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 978-0-521-35299-4.
  7. ^ "Detailed Object Classifications". ned.ipac.caltech.edu. Retrieved 2019-02-21.
  8. ^ a b Mei, S.; Gwyn, S. D. J.; Cuillandre, J.-C.; Côté, P.; Ferrarese, L.; Cucciati, O.; Voyer, E.; Heinis, S.; Driel, W. van (2012-09-01). "The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) - II. Constraints on star formation in ram-pressure stripped gas". Astronomy & Astrophysics. 545: A142. arXiv:1209.0272. Bibcode:2012A&A...545A.142B. doi:10.1051/0004-6361/201219957. ISSN 0004-6361. S2CID 44781835.
  9. ^ a b c d e f g Chung, Aeree; van Gorkom, J. H.; Kenney, Jeffrey D. P.; Crowl, Hugh; Vollmer, Bernd (2009-12-01). "Vla Imaging of Virgo Spirals in Atomic Gas (Viva). I. The Atlas and the H I Properties". The Astronomical Journal. 138 (6): 1741–1816. Bibcode:2009AJ....138.1741C. doi:10.1088/0004-6256/138/6/1741. ISSN 0004-6256.
  10. ^ a b c d Smith, Beverly J.; Madden, Suzanne C. (1997-07-01). "Interstellar Gas in Low Mass Virgo Cluster Spiral Galaxies". The Astronomical Journal. 114: 138–146. arXiv:astro-ph/9704135. Bibcode:1997AJ....114..138S. doi:10.1086/118460. ISSN 0004-6256. S2CID 14627848.
  11. ^ a b Dickel, J. R.; Rood, H. J. (1980-08-01). "The dynamics of some binary galaxies". The Astronomical Journal. 85: 1003–1009. Bibcode:1980AJ.....85.1003D. doi:10.1086/112763. ISSN 0004-6256.
  12. ^ a b c Warmels, R. H. (1988-01-01). "The H I properties of spiral galaxies in the Virgo Cluster. I - Westerbork observations of 15 Virgo Cluster galaxies. II - One-dimensional Westerbork observations of 21 galaxies". Astronomy and Astrophysics Supplement Series. 72: 19–87. Bibcode:1988A&AS...72...19W. ISSN 0365-0138.
  13. ^ a b c Koopmann, Rebecca A.; Kenney, Jeffrey D. P. (2004-10-01). "Halpha Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies". The Astrophysical Journal. 613 (2): 866–885. arXiv:astro-ph/0406243. Bibcode:2004ApJ...613..866K. doi:10.1086/423191. ISSN 0004-637X. S2CID 17519217.
  14. ^ a b c Vlahakis, C.; Verstappen, J.; Smith, M. W. L.; Pohlen, M.; Grossi, M.; Fritz, J.; Looze, I. De; Clemens, M.; Ciesla, L. (2012-09-01). "The Herschel Virgo Cluster Survey - XI. Environmental effects on molecular gas and dust in spiral disks". Astronomy & Astrophysics. 545: A75. arXiv:1207.5051. Bibcode:2012A&A...545A..75P. doi:10.1051/0004-6361/201219689. ISSN 0004-6361. S2CID 53701670.
  15. ^ a b c Kenney, J. D. P.; Otmianowska-Mazur, K.; Chyzy, K. T.; Urbanik, M.; Chung, A.; Beck, R.; Soida, M.; Vollmer, B. (2013-04-04). "Large-scale radio continuum properties of 19 Virgo cluster galaxies The influence of tidal interactions, ram pressure stripping, and accreting gas envelopes". Astronomy and Astrophysics. 553: A116. arXiv:1304.1279. Bibcode:2013A&A...553A.116V. doi:10.1051/0004-6361/201321163. S2CID 119190841.
  16. ^ a b c d Chung, Aeree; van Gorkom, J. H.; Kenney, Jeffrey D. P.; Vollmer, Bernd (2007-04-20). "Virgo Galaxies with Long One-Sided HI Tails". The Astrophysical Journal. 659 (2): L115–L119. arXiv:astro-ph/0703338. Bibcode:2007ApJ...659L.115C. doi:10.1086/518034. ISSN 0004-637X. S2CID 13021118.
  17. ^ Holwerda, B. W.; Pirzkal, N.; de Blok, W. J. G.; van Driel, W. (2011-10-01). "Quantified HI Morphology V: HI Disks in the Virgo Cluster". Monthly Notices of the Royal Astronomical Society. 416 (4): 2447–2454. arXiv:1104.3305. Bibcode:2011MNRAS.416.2447H. doi:10.1111/j.1365-2966.2011.18662.x. S2CID 119285975.
  18. ^ a b Elmegreen, Bruce G.; Elmegreen, Debra Meloy (2010-10-20). "Tadpole Galaxies in the Hubble Ultra Deep Field". The Astrophysical Journal. 722 (2): 1895–1907. arXiv:1009.1530. Bibcode:2010ApJ...722.1895E. doi:10.1088/0004-637X/722/2/1895. ISSN 0004-637X. S2CID 119167225.
  19. ^ Falcón-Barroso, Jesús; Knapen, Johan H. (2013-09-02). Secular Evolution of Galaxies. Cambridge University Press. ISBN 978-1-107-03527-0.
  20. ^ Davis, Benjamin L.; Soria, Roberto; Graham, Alister W. (2019). "Expected intermediate mass black holes in the Virgo cluster. II. Late-type galaxies". Monthly Notices of the Royal Astronomical Society. 484 (1): 814. arXiv:1811.03232. Bibcode:2019MNRAS.484..814G. doi:10.1093/mnras/sty3068. S2CID 119303249.

External links edit

 
Wikimedia Commons has media related to NGC 4294.
  • NGC 4294 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images

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