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CO in High-Redshift Galaxies (with applications to the M*-M BH relation)

CO in High-Redshift Galaxies (with applications to the M*-M BH relation). Desika Narayanan Harvard-Smithsonian CfA. T.J. Cox . Chris Hayward. Lars Hernquist. Yuexing Li. Patrik Jonsson. Quasars and Submillimeter Galaxies. SMGs ( z ~2-4): below. Quasars ( z ~2-6) above.

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CO in High-Redshift Galaxies (with applications to the M*-M BH relation)

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

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

  3. 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 (fg = 0.8) and scaled to z=3-6 • -Halo Masses: 1012-1013 M • -MMW Disks • -1:1 -->1:10 mergers and isolated (1:) GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line) Springel, Di Matteo & Hernquist (2005) Desika Narayanan Penn State - First GQGRBs

  4. Diffuse ISM GADGET (SPH) + SUNRISE (IR) + Turtlebeach (Molecular Line) GMC 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) Desika Narayanan Penn State - First GQGRBs

  5. co co co GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line) co co co co co 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 Narayanan et al. (2006,2008,2009) Desika Narayanan Penn State - First GQGRBs

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

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

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

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

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

  11. Quasars and Submillimeter Galaxies SMGs: below the M*-MBH relation Quasars: above the M*-MBH relation Alexander et al. 2006, 2008 Shields et al. 2006 Desika Narayanan Penn State - First GQGRBs

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

  13. Quasars and Submillimeter Galaxies smgs: below quasars: above Alexander et al. 2006, 2008 Shields et al. 2006 Desika Narayanan Penn State - First GQGRBs

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

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

  16. z~6 QSOs QSO Phase =120 km/s Narayanan, Li et al. (2008) Li et al. (2007) Walter et al. 20041 Desika Narayanan Penn State - First GQGRBs

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

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

  19. R. Wang et al. (2010) Desika Narayanan Penn State - First GQGRBs

  20. Conclusions M*-MBH relation not necessarily broken at high-z (from CO) Desika Narayanan Penn State - First GQGRBs

  21. Conclusions M*-MBH relation not (necessarily) broken at high-z (from CO) Desika Narayanan Penn State - First GQGRBs

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

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

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

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