Reynolds WarnerTalk

Black hole astrophysics in the new century: 

Black hole astrophysics in the new century Chris Reynolds Department of Astronomy University of Maryland Armitage & Reynolds (2004) X-ray probes of strong gravity and cosmic feedback

A new era of black hole research: 

A new era of black hole research Existence of both stellar and supermassive black holes seems secure Exotic physics required to escape black hole conclusion in Galactic Center Every galactic bulge seem to host a supermassive black hole Movie from Genzel group Similar work by Ghez group

The wider importance of black holes: 

The wider importance of black holes Supermassive black holes have cosmological importance… Energy output from black holes growth may be crucial factor in formation/evolution of massive galaxies Galaxy and SMBH growth coupled by powerful feedback processes Kormendy & Gebhardt (2001) Gebhardt et al. (2000) Ferrarese & Merritt (2000)

Open issues…: 

Open issues… Are black holes really described by General Relativity? Is the Kerr metric a good description of black hole spacetime? How does black hole accretion and jet production work? How is accretion energy channeled into radiation & kinetic energy? What is the role of black hole spin? How is massive black hole growth and galaxy formation coupled? How do feedback processes couple enormous spatial scales?

Outline: 

Outline Talk about progress due to developments in X-ray instrumentation Probing the strong gravity regime with X-ray spectroscopy The robustness of the relativistic signatures Confronting accretion disk theory with data Measurements of black hole spin Large scale environmental impact of black holes The cooling flow problem and the radio-galaxy solution Difficulties faced by radio-galaxy feedback models and possible solutions

I : PROBES OF THE STRONG GRAVITY REGIME: 

ASCA observation of MCG-6-30-15… Revealed extremely broadened/skewed iron emission line (Tanaka et al. 1995) Confirmed by XMM What are we seeing? Believe line to originate from surface layers of innermost accretion disk Line broadened and skewed by Doppler effect and gravitational redshifting I : PROBES OF THE STRONG GRAVITY REGIME Power-law continuum subtracted ASCA: Tanaka et al. (1995)

I : PROBES OF THE STRONG GRAVITY REGIME: 

ASCA observation of MCG-6-30-15… Revealed extremely broadened/skewed iron emission line (Tanaka et al. 1995) Confirmed by XMM What are we seeing? Believe line to originate from surface layers of innermost accretion disk Line broadened and skewed by Doppler effect and gravitational redshifting I : PROBES OF THE STRONG GRAVITY REGIME Power-law continuum subtracted XMM: Fabian et al. (2002)

I : PROBES OF THE STRONG GRAVITY REGIME: 

ASCA observation of MCG-6-30-15… Revealed extremely broadened/skewed iron emission line (Tanaka et al. 1995) Confirmed by XMM What are we seeing? Believe line to originate from surface layers of innermost accretion disk Line broadened and skewed by Doppler effect and gravitational redshifting I : PROBES OF THE STRONG GRAVITY REGIME Pseudo-Newtonian MHD simulation Ray-traced through Schwarzschild metric Armitage & Reynolds (2004)

Iron line from X-ray reflection: 

Iron line from X-ray reflection Backscattered spectrum from X-ray irradiation of the “cold” optically-thick disk… Fluorescence/radiative recomb.lines Radiative recombination continuum Compton backscattered continuum Self-consistent model of X-ray reflection from ionized disk (Ross & Fabian 2005)

Iron lines in AGN: 

Iron lines in AGN MCG-5-23-16 (Dewangan 2003) PG 1211+143 (Pounds 2003) IRAS 18325 (Iwasawa 2004) Lockman hole (Streblyanskaya et al 2004)

Iron lines in Galactic Black Hole Binaries: 

Iron lines in Galactic Black Hole Binaries GX 339-4 (XMM) GX 339-4 (CXO) GRS 1915+105 (CXO) XTE J1650-500 (XMM) JM Miller Rin=2.9+-0.1

COMPLEXITY FROM ABSORPTION: 

COMPLEXITY FROM ABSORPTION Must be careful to account for effects of absorption… MCG-6-30-15 (XMM-Newton) Brenneman & Reynolds, in prep

Slide13: 

Fitting 3-6keV and 8-10keV band, can reproduce “red-wing”curvature from iron-L absorption (Kinkhabwala 2003; PhD thesis) Generic prediction - significant iron K line absorption from FeXVII-FeXXIII (~6.4-6.6 keV) NW=4e22 log()=2.2

Slide14: 

MCG-6-30-15; 522ks Chandra-HETG observation [Young, Lee, Fabian, Reynolds et al., ApJ, 2005] Clearly do not see the FeXVII-FeXXIII abs lines that accompany a “broad-line mimicking” WA

TESTING BLACK HOLE ACCRETION DISK MODELS: 

TESTING BLACK HOLE ACCRETION DISK MODELS Current paradigm Accretion proceeds through disk due to MHD turbulence (Shakura & Sunyaev 1973; Balbus & Hawley 1991) Full GR-MHD simulations of non-radiative disks possible Radiatively-efficient disks Gross properties amenable to semi-analytic modeling Novikov & Thorne (1974) Geom. thin, efficient disk Material plunges into BH ballistically once within the innermost stable circular orbit Hirose et al. (2004); also see Koide et al. (2000), McKinney (2005), Komissarov (2005).

TESTING BLACK HOLE ACCRETION DISK MODELS: 

TESTING BLACK HOLE ACCRETION DISK MODELS Current paradigm Accretion proceeds through disk due to MHD turbulence (Shakura & Sunyaev 1973; Balbus & Hawley 1991) Full GR-MHD simulations of non-radiative disks possible Radiatively-efficient disks Gross properties amenable to semi-analytic modeling Novikov & Thorne (1974) Geom. thin, efficient disk Material plunges into BH ballistically once within the innermost stable circular orbit

TESTING BLACK HOLE ACCRETION DISK MODELS: 

TESTING BLACK HOLE ACCRETION DISK MODELS Current paradigm Accretion proceeds through disk due to MHD turbulence (Shakura & Sunyaev 1973; Balbus & Hawley 1991) Full GR-MHD simulations of non-radiative disks possible Radiatively-efficient disks Gross properties amenable to semi-analytic modeling Novikov & Thorne (1974) Geom. thin, efficient disk Material plunges into BH ballistically once within the innermost stable circular orbit a=0.9981

TESTING BLACK HOLE ACCRETION DISK MODELS: 

TESTING BLACK HOLE ACCRETION DISK MODELS Current paradigm Accretion proceeds through disk due to MHD turbulence (Shakura & Sunyaev 1973; Balbus & Hawley 1991) Full GR-MHD simulations of non-radiative disks possible Radiatively-efficient disks Gross properties amenable to semi-analytic modeling Novikov & Thorne (1974) Geom. thin, efficient disk Material plunges into BH ballistically once within the innermost stable circular orbit Deep Minimum of MCG-6-30-15 XMM (Reynolds et al. 2004)

Slide19: 

Iron lines broader than predicted from NT disk  Irradiation more centrally concentrated than NT prediction Underlying disk is NT-like, but X-ray irradiation does not track local dissipation (need light bending) Irradiation tracks a dissipation that is much more centrally concentrated than NT law

Gravitational light bending?: 

Gravitational light bending? Suppose X-ray source is base of a jet? X-rays will be gravitationally focused onto central parts of disk Can produce very centrally concentrated irradiation pattern! Data suggest h~few GM/c2 Geometry first discussed in Fe-K line context by Marttochia & Matt (1996) Applied to ASCA data for MCG-6-30-15 by Reynolds & Begelman (1997) Applied to XMM data for MCG-6-30-15 by Minuitti & Fabian (2004)

Slide21: 

Iron lines broader than predicted from NT disk  Irradiation more centrally concentrated than NT prediction Underlying disk is NT-like, but X-ray irradiation does not track local dissipation (need light bending) Irradiation tracks a dissipation that is much more centrally concentrated than NT law

Enhanced dissipation in central regions of disk?: 

Enhanced dissipation in central regions of disk? Recent work suggests importance of “torqued accretion disks” Magnetic fields may lead to continued extraction of energy/ang-momentum of matter plunging within ISCO Plunging matter exerts torque on rest of disk Work done by torque dissipated in innermost regions of the disk In extreme case, this might produce a Penrose process and allow the BH spin to be tapped. Analytic: Gammie (1999), Krolik (1999), Li (2000), Agol & Krolik (2000), Garofalo & Reynolds (2005) Numerical: Hawley (2000), Hawley & Krolik (2001), Armitage, Reynolds & Chiang (2001), Reynolds & Armitage (2003)

Enhanced dissipation in central regions of disk?: 

Enhanced dissipation in central regions of disk? Recent work suggests importance of “torqued accretion disks” Magnetic fields may lead to continued extraction of energy/ang-momentum of matter plunging within ISCO Plunging matter exerts torque on rest of disk Work done by torque dissipated in innermost regions of the disk In extreme case, this might produce a Penrose process and allow the BH spin to be tapped. Deep Minimum of MCG-6-30-15 XMM (Reynolds et al. 2004)

Enhanced dissipation in central regions of disk?: 

Enhanced dissipation in central regions of disk? Recent work suggests importance of “torqued accretion disks” Magnetic fields may lead to continued extraction of energy/ang-momentum of matter plunging within ISCO Plunging matter exerts torque on rest of disk Work done by torque dissipated in innermost regions of the disk In extreme case, this might produce a Penrose process and allow the BH spin to be tapped. Deep Minimum of MCG-6-30-15 XMM (Reynolds et al. 2004)

BLACK HOLE SPIN: 

BLACK HOLE SPIN Importance of spin Large energy store (upto 29% of rest mass energy) Spin may retain memory of black hole formation First step in testing Kerr metric Diagnose spin through its effects on the accretion disk structure Major effect change in the location of the innermost stable circular orbit (ISCO)

If we assume no X-ray reflection from within the ISCO…: 

If we assume no X-ray reflection from within the ISCO… For progressively more rapidly rotating BHs… ISCO moves inwards to a higher gravitational redshift region For given inclination, maximum redshift of iron line increases Applied to long (350ks) XMM dataset for MCG-6 Data strongly prefers rapidly spinning BH solution a = 0.950.04 Brenneman & Reynolds, in prep

If we assume no X-ray reflection from within the ISCO…: 

If we assume no X-ray reflection from within the ISCO… For progressively more rapidly rotating BHs… ISCO moves inwards to a higher gravitational redshift region For given inclination, maximum redshift of iron line increases Applied to long (350ks) XMM dataset for MCG-6 Data strongly prefers rapidly spinning BH solution a = 0.950.04 Brenneman & Reynolds, in prep

THE PROMISE OF CONSTELLATION-X: 

THE PROMISE OF CONSTELLATION-X Constellation-X Major component of NASA’s Beyond Einstein program Imaging spectroscopy with superior spectral resolution and collecting area Allows study of short-term broad iron line variability Dynamical timescale variability  trace orbits of distinct structures in disk Light crossing timescale variability  follow echos of X-ray flares across disk Constellation-X

THE PROMISE OF CONSTELLATION-X: 

THE PROMISE OF CONSTELLATION-X Constellation-X Major component of NASA’s Beyond Einstein program Imaging spectroscopy with superior resolution and collecting area Allows study of short-term broad iron line variability Dynamical timescale variability  trace orbits of distinct structures in disk Light crossing timescale variability  follow echos of X-ray flares across disk Armitage & Reynolds (2003)

THE PROMISE OF CONSTELLATION-X: 

THE PROMISE OF CONSTELLATION-X Constellation-X Major component of NASA’s Beyond Einstein program Imaging spectroscopy with superior resolution and collecting area Allows study of short-term broad iron line variability Dynamical timescale variability  trace orbits of distinct structures in disk Light crossing timescale variability  follow echos of X-ray flares across disk Armitage & Reynolds (2003) Similar features from outer disk already hinted at by XMM-Newton NGC3516 (Iwasawa et al. 2004) & Mrk 766 (Turner et al. 2005)

THE PROMISE OF CONSTELLATION-X: 

THE PROMISE OF CONSTELLATION-X Constellation-X Major component of NASA’s Beyond Einstein program Imaging spectroscopy with superior resolution and collecting area Allows study of short-term broad iron line variability Dynamical timescale variability  trace orbits of distinct structures in disk Light crossing timescale variability  follow echos of X-ray flares across disk Reynolds et al. (1999) Young & Reynolds (2000)

II : MASSIVE BLACK HOLES & MASSIVE GALAXY FORMATION: 

II : MASSIVE BLACK HOLES & MASSIVE GALAXY FORMATION Benson et al. (2003) Galaxy luminosity function Suppressed at high and low luminosity end compared with simply CDM predictions High-L suppression must be more efficient that star formation Do AGN suppress high-end of galaxy LF?

Cluster cooling flowsMassive galaxy suppression in action?: 

XMM-Newton observation of Virgo cluster Matsushita et al. (2002) Intracluster medium(ICM) Hot (107-108K), tenuous (0.001-0.1cm-3) plasma. THE COOLING FLOW PROBLEM Cluster cooling flows Massive galaxy suppression in action?

How can AGN jets heat ICM isotropically? : 

How can AGN jets heat ICM isotropically? Cocoon structure; Scheuer (1974) 2-d hydro simulations Reynolds et al. (2002) Can heat isotropically by either shock heating or dissipation of sound waves

Chandra observations of cooling-core clusters: 

Chandra observations of cooling-core clusters Cygnus-A Smith et al. (2002) Hydra-A Nulsen et al. (2004) Perseus-A Fabian et al. (2000) Abell 4059 / PKS2354-35 Heinz et al. (2002) Virgo/M87 Young et al. (2002) Synopsis: Jet-blown cavities common “Ghost” cavities common Strong shocks elusive!

Modeling the feedback loop: 

Modeling the feedback loop Feedback model  average AGN heating balances ICM cooling Analysis of ICM cavities shows that kinetic power and cooling luminosity are indeed related Nature must modulate AGN fueling according to ICM properties First attempts to model this… Ideal hydro model of jet/ICM interaction Jet power proportional to cooling flow rate FAIL to produce successful balance Mechanical luminosity (1042 erg/s) Cooling luminosity (1042 erg/s) Birzan et al. (2004) Also see McNamara (2000)

Does the “feedback” loop work?: 

Does the “feedback” loop work? Feedback model  average AGN heating balances ICM cooling Analysis of ICM cavities shows that kinetic power and cooling luminosity are indeed related Nature must modulate AGN fueling according to ICM properties First attempts to model this… Ideal hydro model of jet/ICM interaction Jet power proportional to cooling flow rate FAIL to produce successful balance Delayed fueling scenario Vernaleo & Reynolds, submitted Runaway cooling in the equatorial regions

Does the “feedback” loop work?: 

Does the “feedback” loop work? Feedback model  average AGN heating balances ICM cooling Analysis of ICM cavities shows that kinetic power and cooling luminosity are indeed related Nature must modulate AGN fueling according to ICM properties First attempts to model this… Ideal hydro model of jet/ICM interaction Jet power proportional to cooling flow rate FAILS to produce successful balance Delayed fueling scenario Vernaleo & Reynolds, submitted

What ingredients are missing from the feedback model?: 

What ingredients are missing from the feedback model? MHD and Plasma transport processes Thermal conduction and Viscosity Dissipation of wave energy New instabilities of the ICM atmosphere Precession of the jet axis Need to be quasi-isotropic on cooling timescale (few108 yr) Dissipation of energy stored in global ICM modes? Evidence for dissipation of sounds waves by thermal conduction (see Fabian, Reynolds et al. 2005)

What ingredients are missing from the feedback model?: 

What ingredients are missing from the feedback model? MHD and Plasma transport processes Thermal conduction and Viscosity Dissipation of wave energy New instabilities of the ICM atmosphere Precession of the jet axis Need to be quasi-isotropic on cooling timescale (few108 yr) Dissipation of energy stored in global ICM modes? 3C401 (Chandra and MERLIN cont.) Reynolds, Brenneman & Stocke (2005)

Conclusions: 

Conclusions New era of black hole research Detailed studies of black hole physics and relativistic accretion Impact of black holes on galactic scale structure Strong gravity studies with XMM and Chandra Robust signatures of strong gravity exist Measurements of black hole spin and signs of interesting spin-related astrophysics Constellation-X and LISA will bring tremendously exciting future Jetted AGN and cluster cooling flows Puzzles; how are ICM cores being heated? Need for more physics

Slide43: 

The End

Iron line variability: 

Iron line variability Model : Miniutti & Fabian (2004) Low flux data : Reynolds et al. (2004) High flux data : Fabian et al. (2002)

Enhanced dissipation in central regions of disk?: 

Enhanced dissipation in central regions of disk? Recent work suggests importance of “torqued accretion disks” Magnetic fields may lead to continued extraction of energy/ang-mtm of matter plunging within ISCO Plunging matter exerts torque on rest of disk Work done by torque dissipated in innermost regions of the disk In extreme case, this might produce a Penrose process and allow the BH spin to be tapped. Armitage, Reynolds & Chiang (2001) Reynolds & Armitage (2001)

The way forward: 

The way forward Better modeling More physics (MHD, plasma processes) Put in cosmological setting Better data More deep Chandra observations Direct kinematics from high-resolution X-ray spectroscopy (rebuild of Astro-E2?, Constellation-X) Simulated Astro-E2 XRS data Abell 4059 (z=0.049)