Chemical%20Abundances%20in%20AGN:%20%20the%20Mrk%20279%20Outflow

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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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Using all velocity constraints

• For Cloudy solar abundances
• C2.45x10-4 N8.5x10-5 O4.9x10-4
• Minimal reduced summed over 15
• velocity bins 4.2 for 44 (75-1-30) dof

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Using all velocity constraints

• For Cloudy solar abundances
• C2.45x10-4 N8.5x10-5 O4.9x10-4
• Minimal reduced summed over 15
• velocity bins 4.2 for 44 (75-1-30) dof
• For C2.2 N3.5 O1.6 (times solar)
• Minimal reduced summed over 15
• velocity bins 1.2 for 41 (75-1-30-3) dof

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Chemical abundances in Mrk 279

• For solar abundances
• C2.45x10-4 N8.5x10-5 O4.9x10-4
• C2.2 N3.5 O1.6 times solar
• 90 Confidence interval
• C 1.52.9, N2.44.6, O0.92.4

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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)
  NH1020
• Abundances C2.2 N3.5 O1.6 solar units