The MBH star relation at the highest redshifts

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

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

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)

Z=1000 …going to highest redshifts Earliest epoch sources: longest ‘time baselines’ Z=15 Z=6 critical redshifts/timescales: - z=4 -6. 4 (highest z QSO) corresponds to: - 0. 8 -2 Gyr after Big Bang Basic measurements: Need 3 D! Z=0 Mbulge, MBH Mgas Mdyn stars black hole gas dynamical mass

z= Obtaining stellar disk masses difficult… 0. 3– 0. 7 0. 9– 1. 0 Mbulge, MBH Mgas Mdyn stars black hole gas dynamical mass 1. 0– 1. 15– 1. 3– 1. 5– 1. 6– 1. 8 e. g. , QSOs in COSMOS Note: central source removed 1. 8– 1. 9– 2. 1– 2. 9 HST imaging (e. g. Jahnke et al in prep) …hopeless at z>~2

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

Mgas: Molecular Gas at High z § molecular gas: fuel for SF & AGN activity § cold H 2 invisible -> use CO as tracer § use conversion factor to get H 2 mass § n[CO(J-(J-1))] = (115 GHz x J) Mbulge , stars MBH black hole Mgas Mdyn dynamical mass [115 GHz = 2. 7 mm] number of sources all high-z CO detections high-z tail redshift note: all CO detections at J>3 molecular line observations: - Mgas from CO(1 -0) - constrain dynamics! Mbulge, MBH Mgas Mdyn stars black hole gas dynamical mass

Can CO be used to constrain Mdyn? Yes! § CO in M 82 (OVRO mosaic) Walter, Weiss & Scoville 2002 § -> Mdyn

Mbulge, MBH Mgas Mdyn stars black hole gas dynamical mass CO(1 -0) @ z=4: ‘cm’ Telescopes BRI 1202 (z=4. 7) PSS 2322 (z=4. 1) GB T APM 08279 (z=3. 9) Riechers, FW et al. 2006 First measurements of total gas mass at z~4 through CO(1 -0) Typically: MH 2 = 4 x 1010 Msun massive gas reservoirs [note: ‘low’ CO-to-H 2 conversion factor]

Mbulge, MBH Mgas Mdyn stars black hole gas dynamical mass Resolving the Gas Reservoirs Ultimate goal is to resolve gas emission. --> critical scale: 1 kpc 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] Perhaps most ‘prominent’ example: J 1148+5251 at z=6. 42 Walter et al. 2004 J 1148+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

HST ACS A Molecular Einstein Ring at z=4. 1: J 2322 CO(2 -1) @ z=4. 12 § Riechers, FW ea. 2008 § CO channel maps ( v=40 kms-1) at z=4. 1(!) CO(2 -1) at <0. 3” 70 h VLA B/C array difference in morphology: Molecular Einstein Ring Optical: double image Differentially lensed need model…

A Molecular In Einstein ve rsi on Ring at z=4. 1: J 2322 model lens plane data Riechers, FW ea. 2007 model source plane (M eth od: Br ew er & Le wis 20 06) - 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 1010 Mo Blue/red: Blue/redshifted emission Mdyn=2. 6 x 1010 Mo Mdyn~Mgas; Mdyn ~ 20 MBH

APM 08279 at z=3. 9: very compact emission Riechers, FW ea. 2007 @ VLA (0. 3” res. ) NIR X-ray -> Diff. magnification p -> very compact emission (~0. 5 kpc) Mdyn~Mgas velocity ! s ew n t s te a L position Riechers, FW et al.

Riechers, FW ea. 2007 Interacting Galaxy at z=4. 4: BRI 1335 CO(2 -1) not lensed 0. 15” resolution (1. 0 kpc @ z=4. 4) CO(2 -1) 10 kpc Þ CO: 5 kpc diameter, vco=420 km/s - Mgas = 0. 9 x 1011 Mo - Mdyn = 1. 0 x 1011 sin-2 i Mo spatially & dynamically resolved QSO host galaxy CO channel maps ( v=40 kms-1) at z=4. 4 - MBH = 6 x 109 Mo (C IV) Mdyn ~ Mgas Mdyn = 17 MBH

Comparison to local relation APM 08279+5255 (z=3. 91) B 1335 -0417 (z=4. 41) J 1148+5251 (z=6. 42) Now: 4 sources. J 2322+1944 at z>4(z=4. 12) studied in detail In all cases: Mgas ~ Mdyn ~ 20 MBH [cf. 700 MBH] i. e. no room for massive stellar body Black holes formed first in these objects z=0 Häring & Rix 2004 see also Coppin et al. astro/ph 0806. 061

Summary n ‘mass budget’ of QSOs out to z=6. 4 (multi- ) • MBH, Mgas, Mdyn can be measured Need kinematic (3 D) information to tackle problem n 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 n now: tip of the iceberg: ‘new’ IRAM, EVLA, ALMA, (E)ELT

The End

‘Calibrate’ QSOs at z=0 Measure Mdyn for QSOs w/ accurate MBH PG 1426+015 (z=0. 086) Pd. BI MBH=4. 3 108 Msun PG 1440+358 (z=0. 079) - CARMA MBH=2. 9 107 Msun Riechers, FW et al, in prep.