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The M BH -  star relation at the highest redshifts

Investigating the relationship between black hole and star growth rates at highest redshifts, with a focus on the Magorrian relation and quasars. Utilizing observations and theoretical predictions to study mass compositions with redshift evolution.

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The M BH -  star relation at the highest redshifts

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  1. The MBH-star relation at the highest redshifts Fabian Walter (MPIA)

  2. black hole mass Häring & Rix 2004 • Origin of ‘Magorrian relation’ at z=0 ? • Mstars~700 MBH • [masses are correlated on scales of • over 9 orders of magnitude!] stellar mass Question: do black holes and stars grow together? complication: bright! Ideally, want to study mass compositions as f(z) 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

  3. Magorrian / MBH-star relation Z=0: The stellar bulge mass is related to the mass of central black hole Magorrian ea. 98, Gebhardt ea. 00, Ferrarese ea. 00, Tremaine ea. 02, Marconi & Hunt 03 • Theoretical Predictions: • No evolution with z (e.g., Granato ea. 04, Robertson ea. 06) • Sigma (mass) decreases with z (e.g., Croton ea. 06)

  4. Need 3D! …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: Mbulge,  stars MBH black hole Mgas gas Mdyn dynamical mass Credit: Caltech Media Z=0

  5. 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 …hopeless at z>~2 Obtaining stellar disk masses difficult… Mbulge,  stars MBH black hole Mgas gas Mdyn dynamical mass e.g., QSOs in COSMOS HST imaging (e.g. Jahnke et al in prep)

  6. MBH: NIR Spectroscopy of SDSS z~6 QSOs Mbulge, stars MBH black hole Mgas gas Mdyn dynamical mass VLT Kurk, FW et al. 2007 black hole masses MBH: [empirical calib. from width of MgII, CIV lines] few 109 Msun , now down to 108 Msun Kurk, FW, et al. 2007 Jiang et al. 2007

  7. all high-z CO detections molecular line observations: - Mgas from CO(1-0) - constrain dynamics! high-z tail number of sources Mbulge, stars MBH black hole Mgas gas Mdyn dynamical mass redshift note: all CO detections at J>3 Mgas: Molecular Gas at High z • molecular gas: fuel for SF & AGN activity • cold H2 invisible -> use CO as tracer • use conversion factor to get H2 mass • n[CO(J-(J-1))] = (115 GHz x J) Mbulge , stars MBH black hole Mgas gas Mdyn dynamical mass [115GHz = 2.7mm]

  8. Can CO be used to constrain Mdyn? Yes! • CO in M82 (OVRO mosaic) Walter, Weiss & Scoville 2002 • -> Mdyn

  9. Mbulge,  stars MBH black hole Mgas gas Mdyn dynamical mass CO(1-0) @ z=4: ‘cm’ Telescopes BRI1202 (z=4.7) PSS2322 (z=4.1) GBT APM 08279 (z=3.9) Riechers, FW et al. 2006 First measurements of total gas mass at z~4 through CO(1-0) Typically: MH2 = 4x1010 Msun massive gas reservoirs [note: ‘low’ CO-to-H2 conversion factor]

  10. Perhaps most ‘prominent’ example: J1148+5251 at z=6.42 J1148+5251 (z=6.4) CO • Mgas= 2 x 1010 Msun • Mdyn~ 6 x 1010 Msun • MBH = 3 x 109 Msun Mdyn ~ Mgas Mdyn = 20 MBH breakdown of M- relation? but: only one example/source Walter et al. 2004 Mbulge, stars MBH black hole Mgas gas Mdyn dynamical mass Resolving the Gas Reservoirs Ultimate goal is to resolve gas emission. --> critical scale: 1kpc We don’t need ALMA for (all of) this! VLA reaches 0.15” resolution (~1 kpc at z~4-6) [upgraded Plateau de Bure: 0.3”, also: CARMA]

  11. HST ACS A Molecular Einstein Ring at z=4.1: J2322 CO(2-1) @ z=4.12 • CO(2-1) at <0.3” • 70h VLA B/C array difference in morphology: Molecular Einstein Ring Optical: double image Differentially lensed need model… Riechers, FW ea. 2008 CO channel maps (v=40 kms-1) at z=4.1(!)

  12. Reconstruction & Lens Inversion (Method: Brewer & Lewis 2006) A Molecular Einstein Ring at z=4.1: J2322 model source plane model lens plane Riechers, FW ea. 2007 data • Grav. Lens: Zoom-in: 0.30” 0.09” (650 pc)Magnification:µL=5.3 • r = 1.5 kpc disk + interacting component? • Mgas=1.7 x 1010Mo Mdyn=2.6 x 1010Mo Blue/red: Blue/redshifted emission Mdyn~Mgas; Mdyn ~ 20 MBH

  13. Plateau de Bure CO(10-9): Latest news! p-v diagram velocity position APM08279 at z=3.9: very compact emission NIR X-ray @ VLA (0.3” res.) Riechers, FW ea. 2007 p -> very compact emission (~0.5 kpc) Mdyn~Mgas -> Diff. magnification Riechers, FW et al.

  14. Interacting Galaxy at z=4.4: BRI1335 CO(2-1) not lensed 0.15”resolution (1.0 kpc @ z=4.4) Riechers, FW ea. 2007 • CO: 5 kpc diameter, vco=420 km/s CO(2-1) 10 kpc • Mgas = 0.9 x 1011Mo • Mdyn = 1.0 x 1011 sin-2iMo • MBH = 6 x 109Mo (C IV) spatially & dynamically resolved QSO host galaxy Mdyn ~ Mgas Mdyn = 17 MBH CO channel maps (v=40 kms-1) at z=4.4

  15. Now: 4 sources at z>4 studied in detail In all cases: Mgas ~ Mdyn Mdyn ~ 20 MBH [cf. 700 MBH] i.e. no room for massive stellar body Black holes formed first in these objects APM08279+5255 (z=3.91) B1335-0417 (z=4.41) J1148+5251 (z=6.42) J2322+1944 (z=4.12) z=0 Häring & Rix 2004 Comparison to local relation see also Coppin et al. astro/ph 0806.061

  16. Summary • ‘mass budget’ of QSOs out to z=6.4 (multi-) • MBH, Mgas, Mdyn can be measured • 4 objects at z~4-6: Mdyn ~ Mgas Mdyn ~ 20 MBH [vs. ~700 today] • black holes in QSOs form before stellar body • theories need to account for this • now: tip of the iceberg: ‘new’ IRAM, EVLA, ALMA, (E)ELT Need kinematic (3D) information to tackle problem

  17. The End

  18. ‘Calibrate’ QSOs at z=0 Measure Mdyn for QSOs w/ accurate MBH PG1426+015 (z=0.086) PdBI MBH=4.3 108 Msun PG1440+358 (z=0.079) - CARMA MBH=2.9 107 Msun Riechers, FW et al, in prep.

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