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

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

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

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

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

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

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

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

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

13. 13 Were AGN more X-ray variable in the past? ‘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. OS+05 X-ray

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

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

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

17. Are powerful AGN analogous to NLS1s? NLS1sPowerful AGN   ? ? High accretion rate Super solar metallicity X-rays: steep spectral slope, extreme variations ? ? Evidence for recent star formation Hamann & Ferland 93, Dietrich+03 OS+04 Boller+96, Crenshaw+03 OS & Netzer 02 Boller+96, Leighly 99 Moran+96

18. Conclusions Thank youHagai