Black Holes in Xian u Black holes u

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Black Holes in Xi`an u Black holes u Accretion disks u Jets u Winds

Black Holes in Xi`an u Black holes u Accretion disks u Jets u Winds and outflows u The broad line region

My Stamp Collection

My Stamp Collection

My Stamp Collection

My Stamp Collection

Black hole stamp

Black hole stamp

Black hole stamp Shai Kaspi The industry Brad Peterson

Black hole stamp Shai Kaspi The industry Brad Peterson

Fireworks in Xi`an 1 cm 1011 erg/sec M. Bentz

Fireworks in Xi`an 1 cm 1011 erg/sec M. Bentz

BH Mass Functions Greene & Ho in prep Jenny Greene

BH Mass Functions Greene & Ho in prep Jenny Greene

L/LEdd vs. redshift M=107. 6 M=108. 6 Accretion rate increases with z for all

L/LEdd vs. redshift M=107. 6 M=108. 6 Accretion rate increases with z for all mass BHs See also very interesting result by Y. M. Chen et al about duty cycle

The Fundamental Plane Relationship of Astrophysical Black Holes Ran Wang Alessandro Marconi

The Fundamental Plane Relationship of Astrophysical Black Holes Ran Wang Alessandro Marconi

MBH-L MBH-σ MBH-Mvir MBH-Wgrav Observed 1. 1± 0. 1 4. 0 ± 0. 3

MBH-L MBH-σ MBH-Mvir MBH-Wgrav Observed 1. 1± 0. 1 4. 0 ± 0. 3 Fundament 0. 35 ± 0. 05 0. 25 ± 0. 05 al 1. 0 ± 0. 1 0. 27 ± 0. 05 0. 7 ± 0. 1 0. 22 ± 0. 03 MBH-L 1. 1 0. 25 2. 6 0. 35 0. 87 0. 28 0. 56 0. 29 MBH-σ 1. 02 0. 38 4. 0 0. 25 0. 95 0. 33 0. 69 0. 29 MBH-Mvir 1. 14 0. 28 3. 18 0. 32 1. 0 0. 25 0. 66 0. 26 MBHWgrav 1. 32 0. 32 4. 14 0. 30 1. 18 0. 27 0. 25 Can this be generalized to AGN?

Accretion disk stamp Omer Blaes It is all magnetically driven Please Omer Will you

Accretion disk stamp Omer Blaes It is all magnetically driven Please Omer Will you give us back our corona? The X-ray astronomers

Undressing AGNs Why is this different from Seyfert 1 s (Paulina Lira)? Can the

Undressing AGNs Why is this different from Seyfert 1 s (Paulina Lira)? Can the BLR provide the mysterious screen? Covering=0. 1 Column density=1023 cm-2 Scattering probability=0. 01 See also poster

Relativistic disk lines Tahir Yaqoob 1. 25 -50% of all AGNs show relativistic disk

Relativistic disk lines Tahir Yaqoob 1. 25 -50% of all AGNs show relativistic disk lines - ? ? ? 5 5. 25 5. 75 6 6. 3 ke. V 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 ! 40 80 120 160 200 e. V

X-ray variability

X-ray variability

Characteristic time-scales scale with black hole mass – Phil Uttley >108 M 4 107

Characteristic time-scales scale with black hole mass – Phil Uttley >108 M 4 107 M 106 M

Jet stamp Wagner Boettecher Maraschi New opportunity

Jet stamp Wagner Boettecher Maraschi New opportunity

Relativistic jet outflow with G ≈ 10 g-q g 1 Proton-induced radiation mechanisms: n.

Relativistic jet outflow with G ≈ 10 g-q g 1 Proton-induced radiation mechanisms: n. Fn Qe, p (g, t) Injection, acceleration of ultrarelativistic electrons and protons Blazar Models n g 2 g n. Fn Synchrotron emission of primary e- n Hadronic Models

Chairman Wang said

Chairman Wang said

Jian-Min Wang Major questions jet formation/ejection from disk: are they really connected? how to

Jian-Min Wang Major questions jet formation/ejection from disk: are they really connected? how to form and quench? how to accelerate jets? jet fraction of the energy output from BH accretion? Binary BH in OJ 287? See several posters jet formation is BH mass-scale free? jet component? jet interaction with surrounding photons from disk, BLR?

Winds and Outflows stamp Xra But: y Ult r av iol et Mi d-I

Winds and Outflows stamp Xra But: y Ult r av iol et Mi d-I nfr Mike Brotherton does not like some of it … are d Gallagher 2006

vmax vs. Daox t e ~1 Daox

vmax vs. Daox t e ~1 Daox

Emission-Line Profiles at Low Flux Levels Mike Crenshaw

Emission-Line Profiles at Low Flux Levels Mike Crenshaw

Simple Geometric Model r = 0. 1 pc, = 45 , vr = vlos

Simple Geometric Model r = 0. 1 pc, = 45 , vr = vlos = - 490 km s-1 u Assume v = 0, then v = v. T = 2100 km s-1 (v. T = u 10, 000 km s-1 also shown)

Doron Chelouche Do we really need that level of sophistication? (the case of stellar

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.

More winds u M. Guainazzi – WA is also warm reflector (but 200 pc

More winds u M. Guainazzi – WA is also warm reflector (but 200 pc large) u F. Nicastro – WA is <0. 1 pc in size u Goncalves – He-like X-ray lines are good wind diagnostics

Broad Line Region stamp u Joe Shields – What is the physical origin of

Broad Line Region stamp u Joe Shields – What is the physical origin of the Baldwin effect (29 years is not enough. . ) u M. Joly – What is the origin of the extremely strong Fe. II lines (26 years is not enough. . )

Ari Laor - Why does RBLR L 1/2 Theory ? Netzer & Laor (1993)

Ari Laor - Why does RBLR L 1/2 Theory ? Netzer & Laor (1993) Dust suppression of line emission. Σion=1023 U, U=nγ/ne Dust= Σ/1021=100 U Line suppression for U>0. 01 Dust sublimation. Rsub≤ 0. 2 L 461/2 pc BLR is dust bounded 1021 1022 Lines IR D ty s u s ga BLR IR cont’ NLR Inevitable & no free parameters

2 D Transfer Function - W. Kollatschny 2 -D CCF : correlation of Hβ

2 D 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). Velocity-delay map Kollatschny 2003 a E Echo image c h Theoretical velocity-delay for different flows: He. II lines aremaps gravitationally shifted Keplerian disk BLR model: fast response of both outer line wings OVII is also gravitationally shifted at Welsh & Horne 1991, Horne et al. 2004 r=20 rs

More BLR goodies B. Welsh: BLR gas is falling in (? ? ) u

More BLR goodies B. Welsh: BLR gas is falling in (? ? ) u I. Strateva: double-peaked line profiles u F. Hamann: BLR metallicity goes with BH mass (but … L/L(Edd) and time dependence) u The SDSS industry (or: what can we learn by studying large samples? ) - Nagao u

Accretion disk Dr. Joe Shields Black holes Winds and outflows Xi`an, China Jets BLR

Accretion disk Dr. Joe Shields Black holes Winds and outflows Xi`an, China Jets BLR

October 21 2006 Dear Joe, Please review for us the other sessions Thanks ….

October 21 2006 Dear Joe, Please review for us the other sessions Thanks …. .