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AGN s : Iron ABUNDANCE and cosmic time

Hagai Netzer Tel Aviv University. AGN s : Iron ABUNDANCE and cosmic time. With Benny Trakhtenbrot. Iron abundance trough time. FeII lines in AGNs Eigen vector 1 (EV1) AGNs at z=4.8 Black hole evolution Metallicity evolution. A useful dictionary. FeII lines in AGNs.

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AGN s : Iron ABUNDANCE and cosmic time

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  1. Hagai Netzer Tel Aviv University AGNs:Iron ABUNDANCE and cosmic time With Benny Trakhtenbrot

  2. Iron abundance trough time • FeII lines in AGNs • Eigen vector 1 (EV1) • AGNs at z=4.8 • Black hole evolution • Metallicity evolution A useful dictionary

  3. FeII lines in AGNs • The FeII line problem • Observations vs. photoionization models • The energy budget of the BLR • FeII/Hᵦ • FeII/MgII • FeII(2950)/FeII(4570)

  4. Are strong FeII lines related to iron abundance?

  5. Eigen vector 1 (EV1) • EV1 in the optical and its meaning • EV1 in the UV (3000A)

  6. FeII lines in AGNs • The FeII line problem • Observations vs. photoionization models • The energy budget of the BLR • FeII/Hᵦ • FeII/MgII • FeII(2950)/FeII(4570) Conclusion: 1. Much (but not all) of the FeII line intensities are due to Fe/α variations 2. (FeII 4570)/(Hᵦ) and (FeII 2950)/(MgII 2800) are telling the same story 3. FeII/MgII changing much less than FeII/Hb

  7. Black hole evolution Trakhtenbrot and Netzer 2012

  8. The z=4.8 Sample • 40 QSOs at z=4.65-4.95 • Optically selected from • SDSS (flux limited) • H-band spectroscopy with • VLT and Gemini-N Trakhtenbrot et al. 2011 Mor et al. 2012

  9. Two ways to explain FeII/MgII Changes in physical conditions Disk SED BLR gas density and/or ionization BLR dust Changes in metallicity Galaxy metallicity BLR gas metallicity SF related metallicity A combination of both

  10. FeII/MgIIvs BH mass and L/LEdd Matsuoka et al. 2011 2.3< z < 3.5

  11. Black hole evolution

  12. Growth rate: backward in time Most BHs did not have enough time to grow to their masses by accreting at the observed rates

  13. Going backward in time means going to smaller BH mass and larger L/LEdd

  14. Metallicity evolution - conclusions • BH mass increases and normalized accretion rate decreases in time • The iron abundance in the BLR decreases in time • Type I SNs did not have enough time to explain Fe/H at z=4.8 • Downsizing of the BH population anti-correlates with Fe/H • Possible explanations

  15. Sani et al, 2010Enhanced star formation in narrow‐line Seyfert 1 active galactic nuclei revealed by Spitzer

  16. Sani et al. 2010Enhanced star formation in narrow‐line Seyfert 1 active galactic nuclei revealed by Spitzer SFR

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