Thermal Instabilities in the Wind of NGC 3783

Details Thermal Instabilities in the Wind of NGC 3783 Thermal Instabilities in the Wind of NGC 3783

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009sf2a.conf..155g&link_type=abstract

SF2A-2009: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, held 29 June - 4 July 2009 in

Astronomy and Astrophysics

Astrophysics

Scientific paper

Outflows in Active Galactic Nuclei play an important role for galaxy evolution and the enrichment of the intergalactic medium. In the X-ray range they appear as warm absorbers (WA). Thanks to the recently introduced Absorption Measure Distribution (AMD) method, the column densities of individual ionic species of the wind can be derived from observed X-ray spectra, which gives a new handle on constraining the physics of the WA. We report first results on the theoretical interpretation of an AMD analysis for the Seyfert galaxy NGC 3783. The AMD results based on the known 900-ksec Chandra observation suggest that the WA is in pressure equilibrium as was indicated before by spectral analysis. Conducting radiative transfer simulations for such a case we reproduce the measured ionic column-densities by adjusting several crucial parameters of the medium: the ionization parameter, the total column density, and the amount of micro-turbulence. We use the code TITAN that is particularly adequate to the radiative transfer in X-ray photoionized gases at constant total pressure. It turns out that the WA plasma is probably a clumpy, two-phase medium where cold, dense clumps are embedded in a hotter, diffuse gas.

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