Do QSO Extended Emission Regions Result from Cooling Flows?

Details Do QSO Extended Emission Regions Result from Cooling Flows? Do QSO Extended Emission Regions Result from Cooling Flows?

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002cxo..prop.1266s&link_type=abstract

Chandra Proposal ID #04700368

Physics

Chandra Proposal Id #04700368

Scientific paper

Many low-redshift QSOs show strong optical emission extending over ranges of several tens of kiloparsecs. In general, the ionized gas shows no evident correlation with either the host galaxy morphology or the radio structure. While it can be shown that the gas is photoionized by the QSO, the origin of this gas is still quite uncertain. Crawford, Fabian, and colleagues have argued strongly that the gas originates in cooling flows, but a close study of one emission-line region indicates gas pressures inconsistent with such an origin; however, this conclusion is still somewhat model dependent. We propose here the first direct test of the presence of cooling flows in groups associated with 5 QSOs with luminous extended emission regions.

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