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A Multiwavelength View of Powerful High-Redshift AGN

A Multiwavelength View of Powerful High-Redshift AGN. Ohad Shemmer Penn State University. ‘Active Galactic Nuclei: From Atoms to Black Holes’, Tel Aviv, February 22, 2006. A Multiwavelength, and extremely biased View of Powerful High-Redshift AGN. Ohad Shemmer Penn State University.

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A Multiwavelength View of Powerful High-Redshift AGN

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  1. A Multiwavelength View of Powerful High-Redshift AGN Ohad Shemmer Penn State University ‘Active Galactic Nuclei: From Atoms to Black Holes’, Tel Aviv, February 22, 2006

  2. A Multiwavelength, and extremely biased View of Powerful High-Redshift AGN Ohad Shemmer Penn State University ‘Active Galactic Nuclei: From Atoms to Black Holes’, Tel Aviv, February 22, 2006

  3. What have we learned about distant AGN? Barth+03 From the optical-near-IR: Fan+04 Overall, similar SEDs and emission line properties.

  4. What have we learned about distant AGN? Carilli+01 From the radio: Low-z Stern+00 High-z Similar RL/RQ fraction and overall SED.

  5. What have we learned about distant AGN? From the X-ray: OS+05 OS+05,06 No evolution in the X-ray spectral shape and intrinsic absorption.

  6. Distant SMBHs seem to feed and grow like local ones Central engines of AGN are not aware of the cosmic epoch in which they live Should investigate the full range of AGN physical properties, instead of focusing on evolution

  7. The role of powerful AGN (The Hβ factory) 0.52? Two related observational efforts: 1. Luminous AGN at z~2-3 with Hβ measurements 2. Multiwavelength properties of powerful AGN at z>4

  8. The starburst - ‘monster’ connection Maiolino+05 Hamann & Ferland 99 Direct and indirect evidence for the coexistence of starbursts and ‘monsters’ Bertoldi+03

  9. The metallicity-accretion rate relationship Hamann & Ferland 92, 93, 99 UV - optical - near-IR OS, Netzer+04 Important implications for the starburst-‘monster’ connection.

  10. The coexistence of starbursts and monsters PRELIMINARY mid-IR PI: R. Maiolino Evidence for starbursts in powerful, nearby and distant, AGN is piling up. [Are all of the above in conflict with [O II] (Ho 2005)?]

  11. Are there enormous NLRs? (Netzer Line Region) optical - near-IR Netzer, OS+04 Do powerful AGN blow off their NLRs? [Is this related to the luminosity-dependent obscuration, aka the ‘Steffen effect’?]

  12. What determines the AGN SED? X-ray - optical Steffen+06 (yesterday’s astro-ph) X-ray-to-optical spectral slope does not evolve and depends on UV luminosity. [Does αox depend primarily on the accretion rate?]

  13. Were AGN more X-ray variable in the past? X-ray OS+05 ‘Typical’ long-term X-ray variability is detected in powerful AGN at high-z. No significant short timescale (~1 hr in the rest frame) variations are detected.

  14. Is the photon index an accretion-rate indicator? X-ray - optical - near-IR OS, Brandt, Netzer+06 Photon index measurements in luminous, high accretion rate sources are still missing.

  15. The next step: MBH & L/LEdd in the most distant powerful AGN OS+06 (today’s astro-ph) X-ray Measurements of Hβ at z>4 require L-band spectroscopy. [Should wait for JWST.]

  16. Lineless quasars at high redshift: BL Lacs or a new type of unbeamed quasars? OS+06 (astro-ph/0602442) PRELIMINARY The mystery deepens PI: X. Fan

  17.  ? ? Are powerful AGN analogous to NLS1s? NLS1s Powerful AGN High accretion rate High accretion rate OS+04 Boller+96, Crenshaw+03 Super solar metallicity Super solar metallicity OS & Netzer 02 Hamann & Ferland 93, Dietrich+03 X-rays: steep spectral slope, extreme variations ? Boller+96, Leighly 99 Evidence for recent star formation ? Moran+96

  18. Conclusions Thank you Hagai

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