In 1943, this galaxy was one of twelvenebulae listed by American astronomerCarl Keenan Seyfert that showed broademission lines in theirnuclei.[11] Members of this class of objects became known asSeyfert galaxies, and they were noted to have a higher than normal surface brightness in their nuclei.[12] Observation of NGC 5548 during the 1960s withradio telescopes showed an enhanced level ofradio emission.[13]Spectrograms of the nucleus made in 1966 showed that the energized region was confined to a volume a fewparsecs across, where temperature were around14000 K and the plasma had a dispersion velocity of ±450 km/s.[14]
Among astronomers, the accepted explanation for the active nucleus in NGC 5548 is the accretion of matter onto asupermassive black hole (SMBH) at the core. This object is surrounded by an orbiting disk of accreted matter drawn in from the surroundings. As material is drawn into the outer parts of this disk, it becomesphotoionized, producing broad emission lines in the optical andultraviolet bands of theelectromagnetic spectrum. A wind of ionized matter, organized in filamentary structures at distances of 1–14 light days from the center, is flowing outward in the direction perpendicular to the accretion disk plane.[9]
The mass of the central black hole can be estimated based on the properties of the emission lines in the core region. Combined measurements yield an estimated mass of6.54+0.26 −0.25×107M☉. In other words, it is some 65 million times the mass of theSun. This result is consistent with other methods of estimating the mass of the SMBH in the nucleus of NGC 5548.[10] Matter is falling onto this black hole at the estimated rate of0.03 M☉ per year, whereas mass is flowing outward from the core at or above the rate of0.92 M☉ each year.[15] The inner part of the accretion disk surrounding the SMBH forms a thick, hotcorona spanning several light hours that is emittingX-rays. When this radiation reaches theoptically thick part of the accretion disk at a radius of around 1–2 light days, the X-rays are converted into heat.[16]
^abSkrutskie, Michael F.; Cutri, Roc M.; Stiening, Rae; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles A.; Capps, Richard W.; Chester, Thomas; Elias, Jonathan H.; Huchra, John P.; Liebert, James W.; Lonsdale, Carol J.; Monet, David G.; Price, Stephan; Seitzer, Patrick; Jarrett, Thomas H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Elizabeth V.; Evans, Tracey E.; Fowler, John W.; Fullmer, Linda; Hurt, Robert L.; Light, Robert M.; Kopan, Eugene L.; Marsh, Kenneth A.; McCallon, Howard L.; Tam, Robert; Van Dyk, Schuyler D.; Wheelock, Sherry L. (1 February 2006)."The Two Micron All Sky Survey (2MASS)".The Astronomical Journal.131 (2):1163–1183.Bibcode:2006AJ....131.1163S.doi:10.1086/498708.ISSN0004-6256.S2CID18913331.
^Adelman-McCarthy, J. K.; et al. (June 2009), "The SDSS Photometric Catalog, Release 7",VizieR On-line Data Catalog: II/294,Bibcode:2009yCat.2294....0A.
^abWisniewski, W. Z.; Kleinmann, D. E. (November 1968), "16. Multicolor photometry of Seyfert galaxies and measurement at 1.55 microns of the jet in M 87",Astronomical Journal,73:866–867,Bibcode:1968AJ.....73..866W,doi:10.1086/110721.
^abSlavcheva-Mihova, L.; Mihov, B. (February 2011), "Optical multiband surface photometry of a sample of Seyfert galaxies. I. Large-scale morphology and local environment analysis of matched Seyfert and inactive galaxy samples",Astronomy and Astrophysics,526: A43,arXiv:1011.1772,Bibcode:2011A&A...526A..43S,doi:10.1051/0004-6361/200913243,S2CID119263271. See Table 1.
^Burbidge, E. Margaret; Burbidge, G. R.; Prendergast, K. H. (May 1963), "The Rotation and Physical Conditions in the Seyfert Galaxy NGC 7469",Astrophysical Journal,137: 1022,Bibcode:1963ApJ...137.1022B,doi:10.1086/147580.
^Dibai, É. A.; Esipov, V. F.; Pronik, V. I. (February 1968), "The Nucleus of the Seyfert Galaxy NGC 5548",Soviet Astronomy,11: 553,Bibcode:1968SvA....11..553D.
