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Masses of the Highest Redshift Quasars and Their Host Galaxies

Masses of the Highest Redshift Quasars and Their Host Galaxies. Hubble Fellowship Symposium 2008 STScI, Baltimore, MD March 10-12, 2008 Dominik A. Riechers California Institute of Technology. Hubble Fellowship HST-HF-01212.01-A. High Redshift Galaxy Zoo. z = 1000. Distant Galaxies:

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Masses of the Highest Redshift Quasars and Their Host Galaxies

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  1. Masses of the Highest Redshift Quasars and Their Host Galaxies Hubble Fellowship Symposium 2008 STScI, Baltimore, MD March 10-12, 2008 Dominik A. Riechers California Institute of Technology Hubble Fellowship HST-HF-01212.01-A

  2. High Redshift Galaxy Zoo z = 1000 • Distant Galaxies: • Quasar host galaxies • Radio galaxies • Ly- galaxies • GRB host galaxies • Ly-break galaxies • Submm galaxies • BzK galaxies • EROs, DRGs, … z = 15 z = 6 • Different populations? • Unified picture of galaxy evolution? • Mass/galaxy assembly? Credit: Caltech Media z = 0

  3. The role of Quasars (QSOs) • Most galaxies in universe have a central black hole • QSOs: • high accretion events • special phase in galaxy evolution • most luminous sources in universe black hole mass e.g., Häring & Rix 2004 • Origin of ‘Magorrian relation’ at z=0 ? • Mstars~700 MBH • [masses are correlated on scales • over 9 orders of magnitude!] stellar mass Question: do black holes and stars grow together? currently favored theories: yes complication: bright! Ideally, want to study mass compositions as f(z)

  4. …going to highest redshifts Z = 1000 Earliest epoch sources: longest ‘time baselines’ critical redshifts/timescales: - z=4-6.4 (highest z QSO) corresponds to: - 0.8-2 Gyr after Big Bang z = 15 z = 6 Basic measurements: MBH black hole Mbulge stars Mgas gas (& dust) Mdyn dynamical mass Credit: Caltech Media z = 0

  5. MBH: NIR Spectroscopy of SDSS z~6 QSOs MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass VLT Kurk, FW et al. 2007 ISAAC NIR spectra of z~6 QSOs: key lines: MgII, CIV black hole masses MBH: [empirical calib. from width of MgII, CIV lines] few 109 Msun Kurk, …, DR, et al. 2007

  6. z = 0.3–0.7 0.9–1.0 1.0–1.15 1.15–1.3 1.3–1.5 1.5–1.6 1.6–1.8 1.8–1.9 1.9–2.1 2.1–2.9 Note: central source removed …very tough at z>~2 Obtaining stellar disk masses difficult… MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass e.g., QSOs in COSMOS HST imaging Jahnke et al., in prep.

  7. Mgas: Molecular Gas at High z • molecular gas observations • at high-z help to constrain: • SFR (cosmic SF history) • Mgas (fuel for SF & evol. state) • Mdyn(hierarchical models, M-) • ngas, Tkin(conditions for SF) • evidence for mergers • (triggering of QSO activity & SF) ALMA Image courtesy: NRAO/AUI & ESO • detailed studies of molecular gas in the early universe: a main science goal for ALMA (see DSRP) • ground work? Tough, but can be done today for the brightest distant galaxies

  8. high-z tail Molecular Gas at High z MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass • molecular gas: fuel for SF, traces Mdyn & Mgas • >99% H2 – difficult to observe, use CO as tracer • rotational transitions of CO at [n x 115 GHz/(1+z)], • COthe only diagnostic to obtain information on high-z quasar host galaxies (z>4, <1.5 Gyr after BB) long  [115GHz = 2.7mm] all high-z CO detections Cumulative counts Detections per year Solomon & Vanden Bout (2005), DR (2007), PhD Thesis

  9. High-z CO Observations high-z Same observing bands (typ. 3mm) • Typically observed at - z=0: CO(1-0) - high-z: CO(3-2) and higher But: • CO(3-2) obs would miss a low excitation ‘cold‘ component like e.g. found in the Milky Way • only CO(1-0) traces full M(H2) Milky Way Weiss et al. (2005) MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass • need to observe CO(1-0) also at high z but: requires to go to ‘classical’ radio frequencies

  10. MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass CO(1-0) Spectroscopy @z>4Total Molecular Gas Masses APM 08279+5255 (z=3.91) • CO(1-0) detected at 7-12 in typ. 25h (on-source) • First-time detection of CO @z>4 with 100m single-dish telescopes! • Total molecular gas masses: M(H2)~5 x 1010Mo PSS J2322+1944 (z=4.12) GBT BR 1202-0725 (z=4.69) EB DR et al. (2006a)

  11. Resolving z>4 CO EmissionPaving the Road for ALMA • ultimate goal:resolve CO emission spatially/kinematically • Dynamical masses, host galaxy sizes, disk galaxies vs. mergers • compare to optical/NIR: evolution (?) of MBH- relation critical scale: 1 kpc = 0.15” @z=4-6 VLA • Only VLA can observe CO in z>4 QSOs at 0.15”/1 kpc resolution (B array, 10 km) • We don’t need ALMA for (all of) this! • Caveat: needs 50-80 hours per source • & the best weather conditions MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass

  12. Resolving the Gas Reservoirs Perhaps most ‘famous’ example: J1148+5251 at z=6.42 Mdyn=MBH+Mbulge+Mgas+Mdust (+MDM) J1148+5251 (z=6.4) • Mgas= 2 x 1010 Msun • Mdyn~ 6 x 1010 Msun • MBH = 3 x 109 Msun Mdyn ~ Mgas Mdyn = 20 MBH breakdown of relation seen at z=0? but: only one example/source MBH black hole Mbulge stars Mgas gas Mdyn dynamical mass 5 kpc reservoir Walter et al. (2004)

  13. HST ACS F814 PSS J2322+1944 (z=4.12):A Molecular Einstein Ring Lensed CO(2-1) VLA - 70h VLA B/C array - 0.30” resolution • Molecular Einstein Ring • Optical: double image • Differentially lensed • Lensing helps to zoom in, but interpretation depends on lens model Image courtesy: NRAO/AUI DR et al. (2008a), subm. v=42 km/s CO velocity channel maps

  14. Bayesian Reconstruction & Lens Inversion (Method: Brewer & Lewis 2006) A z=4.12 Molecular Einstein Ring Source Lens DR et al. (2008a), subm. Data v=42 km/s CO velocity channel maps • CO emission spatially & dynamically desolved • Grav. Lens: Zoom-in: 0.30” -> 0.15” (1.0 kpc) Magnification:µL=5.3 • r = 2.5 kpc disk + interacting component? • Mgas=1.7 x 1010Mo Mdyn=4.4 x 1010 sin-2i Mo • MBH=4.5 x 108Mo CO(2-1) 8.5 kpc

  15. BRI 1335-0417 (z=4.41):Interacting Galaxy CO(2-1) in BRI 1335-0417 (z=4.41) Not Lensed CO(2-1) 50h VLA BC array 0.15”resolution (1.0 kpc @ z=4.4) • CO: 5 kpc diameter, vco=420 km/s 10 kpc DR et al. (2008b), tbs spatially & dynamically resolved QSO host galaxy • Mgas = 9.2 x 1010Mo • Mdyn = 1.0 x 1011 sin-2iMo • MBH = 6 x 109Mo (C IV) Dv=44 kms-1 CO channel maps (red to blue)

  16. BRI 1335-0417 (z=4.41):A Major ‘Wet‘ Merger? CO(2-1) in BRI 1335-0417 (z=4.41) CO(1-0) in the Antennae (z=0) Both CO maps: 1.0 kpc resolution CO(1-0) on optical DR et al. (2008b), tbs • Distant Quasar Host Galaxy: BRI 1335-0417 (z=4.41) • Mgas = 9.2 x 1010Mo, 5 kpc scale, SFR=4650 Moyr-1 • Nearby Major Merger: NGC4038/39 – the Antennae • Mgas = 2.4 x 109Mo, 7 kpc scale, SFR=50 Moyr-1 Wilson et al. (2000) • same scale, higher mass & SF efficiency in BRI1335 => consistent

  17. Mdyn and the High-z MBH-Mbulge Relation APM08279+5255 (z=3.91) B1335-0417 (z=4.41) J1148+5251 (z=6.42) Now: 4 sources at z>4 studied in detail In all cases: Mgas ~ Mdyn Mdyn ~ 50 MBH [cf. 700 MBH] i.e. no room for massive stellar body Black holes formed first in these objects Bulge buildup through SF & mergers takes time J2322+1944 (z=4.12) z=0 Haering & Rix (2004) DR et al., in prep.

  18. Moving towards the ALMA era Really want to go beyond z>7 to probe into the Epoch of Reionization earliest structures in universe sources that contributed to reionization Are CO observations w/ ALMA the answer?

  19. CO Excitation in High-z Sources Observed CO Line Excitation CO at J>8 not highly excited! high z low z Weiss et al., in prep.

  20. Freq. of [CII] CO NOT EXCITED ALMA CO discovery space small EoR Sources: CO discovery space EoR

  21. Ionized Carbon at z=6.42 [CII] (ionized carbon): major cooling line of the ISM 2P3/2 - 2P1/2 fine-structure line --PDR / SF tracer Rest frequency: 1900 GHz (158 microns) ISO observations: [CII] carries high fraction of LFIR, much brighter than CO [CII] in J1148+5251, z=6.4 redshifted to 256 GHz/1.2 mm [CII] in J1148, z=6.4 Walter,…, DR et al., in prep. red:[CII]receding blue:[CII]approaching greyscale:CO(3-2) 2kpc (0.3”) beam First direct evidence for formation of stellar disk/bulge in host galaxy < 1Gyr after BB

  22. Summary • ‘mass budget’ of QSOs out to z=6.4 (multi-) • MBH, Mgas, Mdyn can be measured • density, temperature, dynamical structure of gas reservoirs • 4 objects at z~4-6: Mdyn ~ Mgas Mdyn ~ 50 MBH [vs. ~700 today] • black holes in QSOs may form before stellar body • theories need to account for this • demonstrated: • [CII] will be key diagnostic line for z>7 Universe • now: tip of the iceberg: ‘new’ IRAM PdBI, EVLA, ALMA: bright future for dark ages

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