Other
Scientific paper
Oct 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.228..963f&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 228, Oct. 15, 1987, p. 963-971. Research supported by t
Other
50
Astronomical Spectroscopy, Gas Cooling, Gas Dynamics, Quasars, Electron Density (Concentration), Gas Density, Gas Flow, Line Spectra, Photoionization, Radial Distribution
Scientific paper
Spatially-resolved optical spectra of the nebulosity around the quasar 3C48 show forbidden oxygen line emission extending to a radius of about 30 kpc. Assuming that the gas is photoionized by the quasar nucleus which has a spectrum unabsorbed shortward of 91.2 nm, the relative strengths of the O III and O II forbidden lines to indicate a gas density of at least 30 million/cu m. The observed gas is in clumps which are thinner than about 10 pc and is at a pressure consistent with a cooling flow such as that around the central galaxy in the poor cluster MKW3s. The total mass of observed gas is about 300 million solar masses. The commonly proposed galaxy collision or merger hypothesis for quasar nebulosity leads to the clumps being unconfined so that they rapidly disperse. A much higher total mass of cold gas (more than 10 to the 11th solar masses) is required so that the nebulosity can last for a collision time-scale and widespread emission can occur. As this far exceeds the mass of gas in normal galaxies, a galaxy collision is an unlikely explanation for 3C 48. A cooling flow around 3C 48 and other quasars is consistent with them lying in either poor or rich clusters and, through accretion, provides a direct link between the quasar nucleus and its environment.
Crawford Carolin S.
Fabian Andrea C.
Johnstone R. M.
Thomas Peter A.
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