The M BH -  star relation at the highest redshifts Fabian Walter (MPIA)

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

Magorrian / M BH -  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)

Earliest epoch sources: longest ‘time baselines’ longest ‘time baselines’ Z=6 Z=0 Z=1000 Z=15 critical redshifts/timescales: critical redshifts/timescales: - z=4-6.4 (highest z QSO) corresponds to: Gyr after Big Bang …going to highest redshifts M bulge,  stars M BH black hole M gas gas M dyn dynamical mass Basic measurements: Credit: Caltech Media Need 3D!

Obtaining stellar disk masses difficult… 0.3–0.70.9–1.01.0– –1.31.3–1.51.5–1.61.6–1.81.8–1.91.9–2.12.1–2.9 z = z = e.g., QSOs in COSMOS HST imaging (e.g. Jahnke et al in prep) …hopeless at z>~2 Note: central source removed M bulge,  stars M BH black hole M gas gas M dyn dynamical mass

VLT M BH : NIR Spectroscopy of SDSS z~6 QSOs black hole masses M BH : black hole masses M BH : [empirical calib. from width of MgII, CIV lines] [empirical calib. from width of MgII, CIV lines] few 10 9 M sun, now down to 10 8 M sun few 10 9 M sun, now down to 10 8 M sun Kurk, FW et al M bulge,  stars M BH black hole M gas gas M dyn dynamical mass Kurk, FW, et al Jiang et al. 2007

 molecular gas: fuel for SF & AGN activity  cold H 2 invisible -> use CO as tracer  use conversion factor to get H 2 mass  [CO(J-(J-1))] = (115 GHz x J) M gas : Molecular Gas at High z M bulge,  stars M BH black hole M gas gas M dyn dynamical mass [115GHz = 2.7mm] note: all CO detections at J>3 high-z tail all high-z CO detections molecular line observations: - M gas from CO(1-0) - constrain dynamics! M bulge,  stars M BH black hole M gas gas M dyn dynamical mass redshift number of sources

Can CO be used to constrain M dyn ? Yes!  -> M dyn Walter, Weiss & Scoville 2002  CO in M82 (OVRO mosaic)

z=4: ‘cm’ Telescopes Riechers, FW et al GB T First measurements of total gas mass at z~4 through CO(1-0) Typically: M H2 = 4x10 10 M sun massive gas reservoirs [note: ‘low’ CO-to-H 2 conversion factor] [note: ‘low’ CO-to-H 2 conversion factor] M bulge,  stars M BH black hole M gas gas M dyn dynamical mass PSS2322 (z=4.1) BRI1202 (z=4.7) APM (z=3.9)

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] M bulge,  stars M BH black hole M gas gas M dyn dynamical mass  M gas = 2 x M sun  M dyn ~ 6 x M sun  M BH = 3 x 10 9 M sun M dyn ~ M gas M dyn ~ M gas M dyn = 20 M BH M dyn = 20 M BH breakdown of M-  relation? but: only one example/source Walter et al J (z=6.4) CO Perhaps most ‘prominent’ example: J at z=6.42

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

A Molecular Einstein Ring at z=4.1: J2322 Reconstruction & Lens Inversion (Method: Brewer & Lewis 2006) Riechers, FW ea model source plane model lens plane data - Grav. Lens: Zoom-in: 0.30” 0.09” (650 pc) Magnification: µ L =5.3 - r = 1.5 kpc disk + interacting component? M gas =1.7 x M o M dyn =2.6 x M o M dyn ~M gas ; M dyn ~ 20 M BH M dyn ~M gas ; M dyn ~ 20 M BH Blue/red: Blue/redshifted emission

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

M dyn ~ M gas M dyn ~ M gas M dyn = 17 M BH M dyn = 17 M BH Interacting Galaxy at z=4.4: BRI1335 spatially & dynamically resolved QSO host galaxy not lensed CO(2-1) 10 kpc 0.15” resolution (1.0 z=4.4) - M gas = 0.9 x M o - M dyn = 1.0 x sin -2 i M o - M BH = 6 x 10 9 M o (C IV )  CO: 5 kpc diameter, v co =420 km/s CO channel maps (  v=40 kms -1 ) at z=4.4 CO(2-1) Riechers, FW ea. 2007

Comparison to local relation Now: 4 sources at z>4 studied in detail Now: 4 sources at z>4 studied in detail In all cases: M gas ~ M dyn In all cases: M gas ~ M dyn M dyn ~ 20 M BH [cf. 700 M BH ] i.e. no room for massive stellar body i.e. no room for massive stellar body Black holes formed first in these objects Black holes formed first in these objects J (z=6.42) B (z=4.41) APM (z=3.91) z=0 J (z=4.12) Häring & Rix 2004 see also Coppin et al. astro/ph

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

The End

‘Calibrate’ QSOs at z=0 Measure M dyn for QSOs w/ accurate M BH PG (z=0.079) - CARMA M BH = M sun Riechers, FW et al, in prep. PG (z=0.086) PdBI M BH = M sun