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Chemical Abundances in AGN: the Mrk 279 Outflow

Chemical Abundances in AGN: the Mrk 279 Outflow. Nahum Arav University of Colorado Boulder Collaborators: Jack Gabel , Jelle Kaastra, Gerard A. Kriss , Kirk T. Korista,, Jennifer E. Scott, Daniel Proga, Katrien C. Steenbrugge, Ehud Behar, Ari Laor, Masao Sako.

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Chemical Abundances in AGN: the Mrk 279 Outflow

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  1. Chemical Abundances in AGN: the Mrk 279 Outflow Nahum Arav University of Colorado Boulder Collaborators: Jack Gabel, Jelle Kaastra, Gerard A. Kriss, Kirk T. Korista,, Jennifer E. Scott, Daniel Proga, Katrien C. Steenbrugge, Ehud Behar, Ari Laor, Masao Sako

  2. Using all velocity constraints: • For Cloudy solar abundances: C=2.45x10^-4 N=8.5x10^-5 O=4.9x10^-4 • Minimal reduced summed over 15 velocity bins = 4.2 for 44 (75-1-30) dof

  3. Using all velocity constraints: • For Cloudy solar abundances: C=2.45x10^-4 N=8.5x10^-5 O=4.9x10^-4 • Minimal reduced summed over 15 velocity bins = 4.2 for 44 (75-1-30) dof • For C=2.2 N=3.5 O=1.6 (times solar) Minimal reduced summed over 15 velocity bins = 1.2 for 41 (75-1-30-3) dof

  4. Chemical abundances in Mrk 279 • For solar abundances: C=2.45x10^-4 N=8.5x10^-5 O=4.9x10^-4 C=2.2 N=3.5 O=1.6 times solar 90% Confidence interval C= 1.5—2.9, N=2.4—4.6, O=0.9—2.4

  5. Summary: Modeling AGN outflows Analysis Key:Accurate Ionic column densities Obstacles: - The absorber is not an homogeneous full screen! - Velocity dependent covering factor (separate for continuum and BEL) Solutions • Data needed: Unblended doublets (CNO) and Lyman series, high S/N • Velocity dependent covering-factor and photoionization models The Mrk 279 outflow: U~-1 (UV) ~0 (X-ray) NH~10^20 Abundances C=2.2 N=3.5 O=1.6 solarunits

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