Ionized Absorbers/Emitters and Time-Evolving Photoionization Models for ``Sherpa''

Details Ionized Absorbers/Emitters and Time-Evolving Photoionization Models for ``Sherpa'' Ionized Absorbers/Emitters and Time-Evolving Photoionization Models for ``Sherpa''

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001tysc.confe.154n&link_type=abstract

Two Years of Science with Chandra, Abstracts from the Symposium held in Washington, DC, 5-7 September, 2001, meeting abstract.

Physics

Active Galaxies And Quasars

Scientific paper

We will present the ``Sherpa'' version of our resonant absorption and gas emission (absemi), plus time-evolving photoionization (timephot) models. Resonant absorption plus gas emission models can be used to fit X-ray high resolution spectra of ionized absorbers/emitters. These models depend on a number of parameters: (a) the equivalent hydrogen column density; (b) the element-by-element metallicity; (c) the covering factors (both radiative and geometric); (d) the equilibrium ionization parameter (or temperature, for thermal models); (e) the mean dispersion velocity; (f) the orbital velocity; (g) the bulk velocity; and (h) the source redshift. Time-evolving photoionization models, can be used to fit time-resolved absorption parameters - equivalent widths or optical depths - of given ionic transitions. These models depend upon two parameters: (a) the electron density in the absorber; and (b) a parameter measuring the departure from equilibrium at a given point (usually the first point) of the given lightcurve.

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