black holes in xi`an black holes accretion disks jets winds and outflows the broad line region

Black Holes in Xi`anBlack Holes in Xi`an

Black holesBlack holes Accretion disksAccretion disks JetsJets Winds and outflowsWinds and outflows The broad line regionThe broad line region

My Stamp CollectionMy Stamp Collection

My Stamp CollectionMy Stamp Collection

Black hole stampBlack hole stamp

Shai Kaspi

Black hole stamp

Brad Peterson

The industry

1011 erg/sec

1 cm

Fireworks in Xi`an

M. Bentz

BH Mass FunctionsBH Mass Functions

Greene & Ho in prep

Jenny Greene

L/LL/LEddEdd vs. redshift vs. redshift

Accretion rate increases with z for all mass BHs

See also very interesting result by Y.M. Chen et al about duty cycle

M=107.6

M=108.6

The Fundamental Plane The Fundamental Plane Relationship of Astrophysical Relationship of Astrophysical

Black HolesBlack Holes

The Fundamental Plane The Fundamental Plane Relationship of Astrophysical Relationship of Astrophysical

Black HolesBlack Holes

Ran WangRan Wang

Alessandro MarconiAlessandro MarconiRan WangRan Wang

Alessandro MarconiAlessandro Marconi

MMBHBH-L-LMMBHBH--σσMMBHBH-M-MvirvirMMBHBH-W-Wgravgrav

ObservedObservedFundameFundame

ntalntal

1.1±0.11.1±0.10.350.35

±0.05±0.05

4.04.0 ±0.3±0.30.250.25

±0.05±0.05

1.01.0 ±0.1±0.10.270.27

±0.05±0.05

0.70.7 ±0.1±0.10.220.22 ±0.03±0.03

MMBHBH-L-L 1.11.10.250.25

2.62.60.350.35

0.870.870.280.28

0.560.560.290.29

MMBHBH--σσ1.021.020.380.38

4.04.00.250.25

0.950.950.330.33

0.690.690.290.29

MMBHBH-M-Mvirvir1.141.140.280.28

3.183.180.320.32

1.01.00.250.25

0.660.660.260.26

MMBHBH-W-Wgravgrav1.321.320.320.32

4.144.140.300.30

1.181.180.270.27

0.70.70.250.25

Can this be generalized to AGN?

Omer Blaes

Accretion disk stamp

Please Omer

Will you give us back our corona?

The X-ray astronomers

It is all magnetically driven

Undressing AGNsUndressing AGNs

Why is this different from Seyfert 1s (Paulina Lira)?

Can the BLR provide the mysterious screen?

Covering=0.1

Column density=1023cm-2

Scattering probability=0.01

See also poster

00.5

11.5

22.5

33.5

44.5

5

Observed Energy

5 5.25 5.5 5.75 6 6.3 keV

0

0.5

1

1.5

2

2.5

3

3.5

4

EW eV

40 80 120 160 200 eV

Relativistic disk linesRelativistic disk linesTahir Yaqoob

1. 25-50% of all AGNs show relativistic disk lines - ???

2. We are trying hard but so far have not succeeded in measuring black hole spin

Jane Turner

Relativistic narrow lines are common and VERY strong !

X-ray variabilityX-ray variability

Characteristic time-scales scale Characteristic time-scales scale with black hole mass – Phil Uttleywith black hole mass – Phil Uttley

>108 M 4107 M 106 M

Jet stamp

Wagner

Boettecher

Maraschi

New opportunity

Blazar ModelsBlazar ModelsRelativistic jet outflow with ≈ 10

Injection, acceleration of ultrarelativistic electrons and

protons

Qe

,p (,

t)

Synchrotron emission of primary e-

F

Proton-induced radiation

mechanisms:

F

-q

Hadronic Models

Chairman Wang saidChairman Wang said

Major questionsMajor questions

jet formation/ejection from diskjet formation/ejection from disk : : are they really connectedare they really connected??

how to form and quenchhow to form and quench?? how to accelerate jetshow to accelerate jets??

jet fraction of the energyjet fraction of the energy output from BH accretionoutput from BH accretion??

jet formation is BH mass-scale freejet formation is BH mass-scale free??

jet componentjet component??jet interaction with surrounding photons from disk, jet interaction with surrounding photons from disk, BLRBLR??

Jian-Min Wang

Binary BH in OJ 287?

See several posters

Ultraviolet

X-ray

Mid-Infrared

Gallagher 2006

But:

Mike Brotherton does not like some of it …

Winds and Outflows stamp

vvmax max vs. vs. oxox

oxox

ee~~11

Emission-Line Profiles at Low Flux Levels

Mike Crenshaw

Simple Geometric Model

r = 0.1 pc, r = 0.1 pc, = 45 = 45, v, vrr = v = vloslos = - 490 km s = - 490 km s-1-1

Assume Assume vv = 0, then = 0, then vv = = vvT T = 2100 km s= 2100 km s-1-1 (v(vTT = 10,000 km s = 10,000 km s-1-1 also also

shown)shown)

Doron Chelouche

Do we really need that level of sophistication?(the case of stellar winds)

•Asymmetric UV emission lines

•Symmetric X-ray lines

Owocki et al.

KK LL

MM

1.0

0.1

More windsMore winds

M. Guainazzi – WA is also warm M. Guainazzi – WA is also warm reflector (but 200 pc large)reflector (but 200 pc large)

F. Nicastro – WA is <0.1 pc in sizeF. Nicastro – WA is <0.1 pc in size Goncalves – He-like X-ray lines are Goncalves – He-like X-ray lines are

good wind diagnosticsgood wind diagnostics

Broad Line Region stampBroad Line Region stamp

Joe ShieldsJoe Shields– What is the physical origin What is the physical origin

of the Baldwin effect (29 of the Baldwin effect (29 years is not enough..)years is not enough..)

M. JolyM. Joly– What is the origin of the What is the origin of the

extremely strong FeII lines extremely strong FeII lines (26 years is not enough ..)(26 years is not enough ..)

Ari Laor - Why does Ari Laor - Why does RRBLRBLR LL1/21/2 ??

Dust suppression of line emission.

Theory Netzer & Laor (1993)

BLR IR cont’ NLR

Σion=1023U, U=nγ/ne

IRLines

Dusty gas

Dust= Σ/1021=100U

Line suppression for U>0.01

Dust sublimation.

Rsub≤0.2L461/2 pc

BLR is dust bounded

Inevitable & no free parameters

2D Transfer Function - W. Kollatschny2D Transfer Function - W. Kollatschny

2-D CCF : correlation of Hβ line profile segments with cont. variations (grey scale)

Contours of correlation coefficient at levels of .85 to .925 (solid lines).

Dashed curves: theoretical escape velocity envelopes for masses of 0.5, 1., 2. 107 MO (from bottom to top).

Kollatschny 2003a

Theoretical velocity-delay maps for different flows: Keplerian disk BLR model: fast response of both outer line wings

Welsh & Horne 1991, Horne et al. 2004

Velocity-delay map

E

c

h

Echo image

HeII lines are gravitationally shifted

OVII is also gravitationally shifted at r=20rs

More BLR goodiesMore BLR goodies

B. Welsh: BLR gas is falling in (??)B. Welsh: BLR gas is falling in (??) I. Strateva: double-peaked line profilesI. Strateva: double-peaked line profiles F. Hamann: BLR metallicity goes with BH F. Hamann: BLR metallicity goes with BH

mass (but … L/L(Edd) and time mass (but … L/L(Edd) and time dependence)dependence)

The SDSS industry (or: what can we learn The SDSS industry (or: what can we learn by studying large samples?) - Nagaoby studying large samples?) - Nagao

Black holes

Accretion disk

Jets

Winds and outflows

BLR

Dr. Joe Shields

Xi`an, China

Dear Joe,

Please review for us the other sessions

Thanks …..

October 21 2006