June 9th 2010Desika Narayanan Penn State - First GQGRBs CO in High-Redshift Galaxies (with applications to the M*-M BH relation) Desika Narayanan Harvard-Smithsonian CfA T.J. Cox Lars Hernquist Patrik Jonsson Chris Hayward Yuexing Li

June 9th 2010Desika Narayanan Penn State - First GQGRBs Quasars and Submillimeter Galaxies Shields et al. 2006Alexander et al. 2006, 2008 Quasars (z~2-6) aboveSMGs (z~2-4): below

June 9th 2010Desika Narayanan Penn State - First GQGRBs GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line) Physics Included in Hydrodynamics: -numerically follows DM, Gas, Stars and BH dynamics -Multi-phase McKee-Ostriker ISM -Star formation follows KS relations -BH growth and associated AGN feedback -Supernovae pressurization of ISM -Gas rich (f g = 0.8) and scaled to z=3-6 -Halo Masses: M  -MMW Disks -1:1 -->1:10 mergers and isolated (1:  ) Springel, Di Matteo & Hernquist (2005)

June 9th 2010Desika Narayanan Penn State - First GQGRBs GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line) GMC Diffuse ISM Physics Included in Monte Carlo IR RT: -IR transfer of stellar and AGN spectrum (starburst 99 for stars and Hopkins+ 07 for AGN) -dust radiative equilibrium -Kroupa IMF, MW Dust to Metals ratio -Stellar Clusters surrounded by HII regions and PDRs (MAPPINGS; Groves et al. 2008) Jonsson, Groves & Cox (2009)

June 9th 2010Desika Narayanan Penn State - First GQGRBs GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line) Narayanan et al. (2006,2008,2009) Physics Included in Monte Carlo CO RT -Mass spectrum of GMCs included as SISs -Molecular statistical equilibrium (collisions and radiation) -Pressure-driven H2 formation/destruction (based on observations of local galaxies) (Blitz & Rosolowsky 2006) -Milky Way Abundances for CO co

June 9th 2010Desika Narayanan Penn State - First GQGRBs Merger-driven origin for high-z Quasars and SMGs U Li et al. 2007,2008 (Yuexing’s Talk)

June 9th 2010Desika Narayanan Penn State - First GQGRBs Merger-driven origin for high-z Quasars and SMGs U DN et al. 2009,2010a,b Hayward, DN et al. 2010

June 9th 2010Desika Narayanan Penn State - First GQGRBs Connection between SMGs and QSOs U Narayanan et al. 2009,2010a,b Hayward, DN et al. 2010

June 9th 2010Desika Narayanan Penn State - First GQGRBs Connection between SMGs and QSOs U DN et al. 2009,2010a,b Hayward, DN et al Li et al. 2008

June 9th 2010Desika Narayanan Penn State - First GQGRBs Merger-driven origin for high-z Quasars and SMGs U Di Matteo, Springel & Hernquist 2005 DN

June 9th 2010Desika Narayanan Penn State - First GQGRBs Quasars and Submillimeter Galaxies Shields et al. 2006Alexander et al. 2006, 2008 Quasars: above the M*-M BH relationSMGs: below the M*-M BH relation

June 9th 2010Desika Narayanan Penn State - First GQGRBs The trip toward the Magorrian Relation for SMGs Alexamder et al. 2006,2008 Narayanan et al. 2010

June 9th 2010Desika Narayanan Penn State - First GQGRBs Quasars and Submillimeter Galaxies Shields et al. 2006Alexander et al. 2006, 2008 quasars: abovesmgs: below

June 9th 2010Desika Narayanan Penn State - First GQGRBs General Picture Merger: SMG phase Gas disks briefly destroyed Quasar Phase Gas disk reforms Elliptical Galaxy (Gas disk remains)

June 9th 2010Desika Narayanan Penn State - First GQGRBs General Picture Merger: SMG phase Gas disks briefly destroyed Quasar Phase Gas disk reforms Elliptical Galaxy (Gas disk remains) ~120 km/s  Walter et al. 2004

June 9th 2010Desika Narayanan Penn State - First GQGRBs z~6 QSOs QSO Phase  =120 km/s Narayanan, Li et al. (2008) Li et al. (2007) Walter et al

June 9th 2010Desika Narayanan Penn State - First GQGRBs CO FWHM-QSO Luminosity Relation Optically Luminous LOSs have small CO FWHMs because of molecular disk formation Narayanan, Li et al. (2008) FWHM

June 9th 2010Desika Narayanan Penn State - First GQGRBs Testable predictions Narayanan, Li et al. (2008) Li et al. (2007) R. Wang et al. (2010)

June 9th 2010Desika Narayanan Penn State - First GQGRBs R. Wang et al. (2010)

June 9th 2010Desika Narayanan Penn State - First GQGRBs Conclusions M*-M BH relation not necessarily broken at high-z (from CO)

June 9th 2010Desika Narayanan Penn State - First GQGRBs Conclusions M*-M BH relation not (necessarily) broken at high-z (from CO)

June 9th 2010Desika Narayanan Penn State - First GQGRBs Validity of Model Narayanan, Li, et al. 2008Walter et al. (2004)

June 9th 2010Desika Narayanan Penn State - First GQGRBs SMGs and Quasars on the Magorrian Relation Narayanan et al. 2010Alexander et al. 2006, 2008

June 9th 2010Desika Narayanan Penn State - First GQGRBs Selection Effect Highest B-band Luminosities have higher percentages of compatible sightlines because of selection effects: Narayanan, Li et al. (2008)