1. Quasar & Black Hole Science for GSMT Central question: Why do quasars evolve?

2. BACKGROUND (1) 2DF, SLOAN, 2Mass, First and other surveys are revealing an ever more complete census of the quasar population from z=0 to 7.

3. Background (continued) The peak of quasar activity was at z~2, when the Universe was only 30% of its present age.

4. BACKGROUND (continued) Reionization of intergalactic hydrogen happened at z= 6.5-7.0

5. Background (continued) A detailed picture of the central engine has been developed  Black hole and accretion disk paradigm  Mostly inferred from spectroscopy and spectropolarimetry of spatially unresolved sources, in the X-ray, UV, optical, IR and radio.  Advances in numerical methods and theory

6. Background (continued) Black holes have been linked to the stellar/baryonic/CDM components of galaxies ● M(BH) --  (bulge) correlation has been found out to the Virgo cluster

7. Background (continued) Feedback to the IGM via UV radiation and shock energy is probably also important

8. Background (continued) The quasar phenomenon and the evolution of the quasar luminosity function is thus placed into the context of the evolution of galaxies and large scale structure

9. Key Measurements for Quasar Science (1) Direct imaging of central engines of quasars (2) Extend kinematic measurements of black hole masses to cosmological distances (3) Study quasar host galaxies (4) Deep quasar surveys ● What is the Seyfert galaxy population at z=7 ● What is the relationship of AGN to protogalaxies and the IGM, for z=2 - 7 GSMT will enable (2) – (4)

10. Synergy with Alma, JWST and Con-X ● Con-X will probe physics of the central supermassive black hole, studying general relativisitic effects in the plasma nearest the black hole ● Alma will probe molecular gas structures in the central engine and trace how black holes are “fed” with gas ● JWST will image dust in the cores of galaxies which is heated by the quasar accretion. ● GSMT will enable high resolution spectroscopy of quasars and their host galaxies, crucial for understanding all these observations, and putting them in the broader context of galaxy formation.

11. ● Accretion disk: 10^14 – 10^16 cm ● Broad Line Region 10 light days for Seyferts  1 light year for quasars ● Torus: 10-50 pc (???) ● Narrow Line Region: 100 pc to 500 pc ● Extended gas & dust disk: 200pc to 1 kpc ● Host Galaxy: 10 kpc+ Quasar Structures Host Galaxy Narrow Line Region And Extended Narrow Line Region Torus jet Accretion diskBroad line region

12. Diffraction Limit (arcseconds) Hubble Space Telescope0.042 JWST (6.5m)0.032 ALMA0.010 30m0.007 20/200.002