Astronomy:NGC 4203
| NGC 4203 | |
|---|---|
 NGC 4203 (SDSS) | |
| Observation data (J2000 epoch) | |
| Constellation | Coma Berenices |
| Right ascension | 12h 15m 05.0s[1] |
| Declination | +33° 11′ 50″[1] |
| Redshift | 0.003620[2] |
| Helio radial velocity | 1,083[3] km/s |
| Galactocentric velocity | 1,093[3] km/s |
| Distance | 49.84 ± 0.46 Mly (15.28 ± 0.14 Mpc)[3] |
| Group or cluster | Coma I |
| Apparent magnitude (V) | 11.99[4] |
| Apparent magnitude (B) | 12.98[4] |
| Characteristics | |
| Type | SAB0−[5] |
| Apparent size (V) | 2.467′ × 2.319′[6] |
| Other designations | |
| 2MASX J12150502+3311500, LEDA 39158, UGC 7256, UZC J121505.0+331152, Z 187-29 .[7] | |
NGC 4203 is the New General Catalogue identifier for a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 20, 1787 by English astronomer William Herschel,[8] and is situated 5.5° to the northwest of the 4th magnitude star Gamma Comae Berenices and can be viewed with a small telescope.[9] The morphological classification of NGC 4203 is SAB0−,[5] indicating that it has a lenticular form with tightly wound spiral arms and a weak bar structure at the nucleus.[10]
This galaxy has a fairly large reservoir of neutral hydrogen containing on the order of a billion solar masses (M☉), but it is only undergoing a low rate of new star formation. Hence, the inner star formation of the galaxy is fairly old; roughly ten billion years on average. The neutral hydrogen is arranged in two ring-like structures, with the outer ring having nine times the mass of the inner. In the central region there is around 2.5×107 M☉ of molecular hydrogen, plus dust structures within 980 ly (300 pc) of the nucleus. The gas in the outer disk may have been accreted from the inter-galactic medium, or captured during a close encounter with a dwarf galaxy.[11]
The nucleus of the galaxy contains a low-ionization nuclear emission-line region of type 1.9. This is being generated by a supermassive black hole of an estimated (6±1)×107 M☉. An influx of gas of around 2×10−2 M☉/yr is sufficient to explain the measured X-ray luminosity. The time-varying emissions from the region are perhaps best explained by an infalling red supergiant star that is losing mass to the black hole along a contrail.[12]
NGC 4203 is a member of the Coma I Group[13][14][15] which is part of the Virgo Supercluster.[16]
References
- ↑ 1.0 1.1 Myers, S. T. et al. (May 2003), "The Cosmic Lens All-Sky Survey - I. Source selection and observations", Monthly Notices of the Royal Astronomical Society 341 (1): 1–12, doi:10.1046/j.1365-8711.2003.06256.x, Bibcode: 2003MNRAS.341....1M.
- ↑ Kochanek, C. S. et al. (October 2001), "The K-Band Galaxy Luminosity Function", The Astrophysical Journal 560 (2): 566–579, doi:10.1086/322488, Bibcode: 2001ApJ...560..566K.
- ↑ 3.0 3.1 3.2 Tully, R. Brent et al. (October 2013), "Cosmicflows-2: The Data", The Astronomical Journal 146 (4): 25, doi:10.1088/0004-6256/146/4/86, 86, Bibcode: 2013AJ....146...86T.
- ↑ 4.0 4.1 Véron-Cetty, M.-P.; Véron, P. (July 2010), "A catalogue of quasars and active nuclei", Astronomy and Astrophysics 518: A10, doi:10.1051/0004-6361/201014188, Bibcode: 2010A&A...518A..10V.
- ↑ 5.0 5.1 Erwin, Peter; Debattista, Victor P. (June 2013), "Peanuts at an angle: detecting and measuring the three-dimensional structure of bars in moderately inclined galaxies", Monthly Notices of the Royal Astronomical Society 431 (4): 3060–3086, doi:10.1093/mnras/stt385, Bibcode: 2013MNRAS.431.3060E.
- ↑ Skrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W. et al. (1 February 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal 131 (2): 1163–1183. doi:10.1086/498708. ISSN 0004-6256. Bibcode: 2006AJ....131.1163S. https://ui.adsabs.harvard.edu/abs/2006AJ....131.1163S/abstract.
- ↑ "NGC 4203". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=NGC+4203.
- ↑ Seligman, Courtney (November 23, 2012), "NGC Objects: NGC 4200 - 4249", Celestial Atlas, http://cseligman.com/text/atlas/ngc42.htm#4203, retrieved 2015-01-04.
- ↑ O'Meara, Steve (2007), Herschel 400 Observing Guide, Cambridge University Press, p. 190, ISBN 978-0521858939, https://books.google.com/books?id=Nyh9fAC_tpIC&q=NGC+4203&pg=PA190.
- ↑ de Vaucouleurs, G. et al. (1991), "Third reference catalogue of bright galaxies, version 9", The Astronomical Journal 108: 2128, doi:10.1086/117225, Bibcode: 1994AJ....108.2128C, https://heasarc.gsfc.nasa.gov/W3Browse/all/rc3.html, retrieved 2015-11-25.
- ↑ Yıldız, Mustafa K. et al. (July 2015), "Star formation in the outer regions of the early-type galaxy NGC 4203", Monthly Notices of the Royal Astronomical Society 451 (1): 103–113, doi:10.1093/mnras/stv992, Bibcode: 2015MNRAS.451..103Y.
- ↑ Devereux, Nick (December 2011), "Time Variable Broad-line Emission in NGC 4203: Evidence for Stellar Contrails", The Astrophysical Journal 743 (1): 10, doi:10.1088/0004-637X/743/1/83, 83, Bibcode: 2011ApJ...743...83D.
- ↑ R. B. Tully (1988). Nearby Galaxies Catalog. Cambridge: Cambridge University Press. ISBN 978-0-521-35299-4.
- ↑ A. Garcia (1993). "General study of group membership. II - Determination of nearby groups". Astronomy and Astrophysics Supplement 100: 47–90. Bibcode: 1993A&AS..100...47G.
- ↑ Giuricin, Giuliano; Marinoni, Christian; Ceriani, Lorenzo; Pisani, Armando (2000). "Nearby Optical Galaxies: Selection of the Sample and Identification of Groups" (in en). The Astrophysical Journal 543 (1): 178. doi:10.1086/317070. ISSN 0004-637X. Bibcode: 2000ApJ...543..178G. http://stacks.iop.org/0004-637X/543/i=1/a=178.
- ↑ Gregory, Stephen A.; Thompson, Laird A. (April 15, 1977). "The Coma i Galaxy Cloud" (in en). The Astrophysical Journal 213: 345–350. doi:10.1086/155160. ISSN 0004-637X. Bibcode: 1977ApJ...213..345G.
External links
- NGC 4203 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
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