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

June 9th 2010 Desika Narayanan Penn State - First GQGRBs

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

Desika Narayanan Harvard-Smithsonian CfA

T.J. Cox

Lars Hernquist

Patrik Jonsson

Chris HaywardYuexing Li


Quasars and Submillimeter Galaxies

Shields et al. 2006Alexander et al. 2006, 2008

Quasars (z~2-6) aboveSMGs (z~2-4): below


GADGET (SPH) + SUNRISE (IR)+ Turtlebeach (Molecular Line)

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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:)

Springel, Di Matteo & Hernquist (2005)


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)


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

coco

coco

co

co

co

co


Merger-driven origin for high-z Quasars and SMGs

U

Li et al. 2007,2008

(Yuexing’s Talk)



U

DN et al. 2009,2010a,bHayward, DN et al. 2010


Connection between SMGs and QSOs

U

Narayanan et al. 2009,2010a,bHayward, DN et al. 2010


Connection between SMGs and QSOs

U

DN et al. 2009,2010a,bHayward, DN et al. 2010

Li et al. 2008



U

Di Matteo, Springel & Hernquist 2005

DN + 2010




Quasars: above the M*-MBH relationSMGs: below the M*-MBH relation


The trip toward the Magorrian Relation for SMGs

Alexamder et al. 2006,2008 Narayanan et al. 2010




quasars: above

smgs: below


General Picture

Merger: SMG phase

Gas disks briefly

destroyed

Quasar Phase

Gas disk reforms

Elliptical Galaxy

(Gas disk remains)


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


z~6 QSOs

QSO Phase

=120 km/s

Narayanan, Li et al. (2008)Li et al. (2007)

Walter et al. 20041


CO FWHM-QSO Luminosity RelationOptically Luminous LOSs have small CO FWHMs because of molecular disk formation

Narayanan, Li et al. (2008)

FWHM


Testable predictions

Narayanan, Li et al. (2008)Li et al. (2007)

R. Wang et al. (2010)


R. Wang et al. (2010)


Conclusions

M*-MBH relation not necessarily broken at high-z (from CO)


Conclusions

M*-MBH relation not (necessarily) broken at high-z (from CO)


Validity of Model

Narayanan, Li, et al. 2008 Walter et al. (2004)


SMGs and Quasars on the Magorrian Relation

Narayanan et al. 2010Alexander et al. 2006, 2008


Selection EffectHighest B-band Luminosities have higher percentages of compatible sightlines becauseof selection effects:

Narayanan, Li et al. (2008)

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

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