NGC 3801

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NGC 3801
NGC 3801 GALEX.jpg
Multiwavelength image of NGC 3801, from ultraviolet to radio
Observation data (J2000 epoch)
Constellation Leo
Right ascension 11h 40m 16.9s [1]
Declination +17° 43′ 41″ [1]
Redshift 0.011064 ± 0.000007 [1]
Heliocentric radial velocity 3,317 ± 2 km/s [1]
Distance 169 ± 38 Mly (51.9 ± 11.6 Mpc) [1]
Apparent magnitude  (V)12.0 [2]
Characteristics
Type S0/a [1]
Apparent size  (V)3.5′ × 2.1′ [2]
Notable featuresmerger remnant, radio galaxy
Other designations
UGC 6635, MCG +03-30-040, 4C +17.52, PGC 36200 [1]

NGC 3801 is a lenticular galaxy located in the constellation Leo. It is about 150 million light years from Earth, and estimated to be about 170,000 light years in diameter. William Herschel discovered it on 17 April 1784. [3]

Contents

Characteristics

The morphology of NGC 3801 is disturbed, indicating that the galaxy underwent a merger with another gas rich galaxy. [4] A dust lane runs across the galaxy in its eastern half while a smaller one is visible perpendicular to that along the minor axis. A tidal tail about 1.2 arcminutes long extends to the east-southeast of the galaxy. The halo of the galaxy appears boxy. [5]

NGC 3801 has been found to emit radio waves. It is a compact Fanaroff–Riley type I radio galaxy, with the total extent of the jets being 40 arcseconds. Both jets appear to curve while the core is not visible in observations by the Very Large Array. [6] The radio jets have been found to heat the interstellar medium to a temperature of 1 and 0.7 keV. [7] A linear feature is visible in soft X-rays extending along the jet axis, possibly a tidal tail. [7]

CO imaging indicates the presence of an edge-on disk with a radius 2 kpc perpendicular to the radio jets axis, with a molecular gas mass of 3×108  M☉ , about 1% of the dynamical mass of the galaxy. There is also a clump of molecular gas not associated with the disk that appears to fall towards the galaxy. [6] The radio jet axis is aligned with the main HI disk of the galaxy. [4]

When observed in ultraviolet, the galaxy is shaped like an s-shape, with the western half being brighter than the eastern half, indicating the presence of a very warped disk. Both halves extend for 60–70 arcseconds. Small UV clumps appear along the galaxy, that indicate the presence of stars. The age of the stellar population in the clumps is estimated to be between 100 and 500 Myr, with most star forming activity taking place before 400 Myr. The location of the most vigorous starburst appears to be the central region of the galaxy. [8]

In the centre of NGC 3801 lies a supermassive black hole whose mass is estimated to be 108.28 ± 0.31 (93 – 390 millions) M☉ based on gas dynamics [9] or 108.43 M☉ based on stellar velocity dispersion. [7] The nucleus of the galaxy has been categorised as in between a Seyfert galaxy and a LINER. [8]

Nearby galaxies

NGC 3801 is the foremost galaxy of the galaxy group known as NGC 3801 group or LGG 246. Other members of the group include the galaxies NGC 3768, NGC 3790, NGC 3799, NGC 3800, NGC 3802, NGC 3806, NGC 3827, and NGC 3853. [10] NGC 3802 lies 2.3 arcminutes from NGC 3801 while NGC 3790 lies 7 arcminutes away. [11] HI imaging shows a hydrogen bridge that appears to link NGC 3801 and NGC 3802, indicating the two galaxies are interacting. [4]

See also

Related Research Articles

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<span class="mw-page-title-main">NGC 2974</span> Galaxy in the constellation Sextans

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<span class="mw-page-title-main">NGC 7720</span>

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References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 3801. Retrieved 2016-01-18.
  2. 1 2 "Revised NGC Data for NGC 3801". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ NGC 3801 cseligman.com Celestial Atlas
  4. 1 2 3 Emonts, B. H. C.; Burnett, C.; Morganti, R.; Struve, C. (1 April 2012). "Classical radio source propagating into outer H i disc in NGC 3801: Large-scale H i disc in NGC 3801". Monthly Notices of the Royal Astronomical Society. 421 (2): 1421–1430. arXiv: 1112.5221 . doi:10.1111/j.1365-2966.2011.20402.x. S2CID   118666200.
  5. ↑ Heckman, T. M.; Smith, Eric P.; Baum, Stefi A.; van Breugel, W. J. M.; Miley, G. K.; Illingworth, G. D.; Bothun, G. D.; Balick, B. (December 1986). "Galaxy collisions and mergers - The genesis of very powerful radio sources?". The Astrophysical Journal. 311: 526. Bibcode:1986ApJ...311..526H. doi:10.1086/164793.
  6. 1 2 Das, Mousumi; Vogel, Stuart N.; Verdoes Kleijn, Gijs A.; O’Dea, Christopher P.; Baum, Stefi A. (20 August 2005). "BIMA Millimeter‐Wave Observations of the Core‐Jet and Molecular Gas in the FR I Radio Galaxy NGC 3801". The Astrophysical Journal. 629 (2): 757–766. arXiv: astro-ph/0505285 . Bibcode:2005ApJ...629..757D. doi:10.1086/431640. S2CID   16263625.
  7. 1 2 3 Croston, J. H.; Kraft, R. P.; Hardcastle, M. J. (May 2007). "Shock Heating in the Nearby Radio Galaxy NGC 3801". The Astrophysical Journal. 660 (1): 191–199. arXiv: astro-ph/0702094 . Bibcode:2007ApJ...660..191C. doi:10.1086/513500. S2CID   7797196.
  8. 1 2 Hota, Ananda; Rey, Soo-Chang; Kang, Yongbeom; Kim, Suk; Matsushita, Satoki; Chung, Jiwon (May 2012). "NGC 3801 caught in the act: a post-merger star-forming early-type galaxy with AGN-jet feedback: NGC 3801: AGN feedback caught in the act?". Monthly Notices of the Royal Astronomical Society: Letters. 422 (1): L38–L42. arXiv: 1111.5325 . doi:10.1111/j.1745-3933.2012.01231.x. S2CID   30363280.
  9. ↑ Bosch, Remco C. E. van den (2 November 2016). "Unification of the Fundamental Plane and Super Massive Black Hole Masses". The Astrophysical Journal. 831 (2): 134. arXiv: 1606.01246 . Bibcode:2016ApJ...831..134V. doi: 10.3847/0004-637X/831/2/134 . S2CID   119216147.
  10. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
  11. ↑ Nilson, P. (1 January 1973). "Uppsala General Catalogue of Galaxies, 1973, Acta Universitatis Upsalienis, Nova Regiae Societatis Upsaliensis, Series v: a Vol". Nova Acta Regiae Soc. Sci. Upsaliensis Ser. V. Bibcode:1973UGC...C...0000N.
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