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XEUS andStrong Gravity from
Black Holes AC Fabian IoA Cambridge UK
With help from Giovanni Miniutti, Jon Miller,Chris Reynolds, Rubens Reis and Randy Ross
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Accretion makes massive blackholes
2
1)1( cz •
!=+ "
#
#$
Soltan 82
Mean redshift Radiative efficiency
Light Mass density in BH
η > 0.1Observations
Much of the radiation originates within 6Rg
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Strong Gravity Effects
• Gravitational redshift• Gravitational light bending• Dragging of inertial frames in
Kerr metric (ISCO depends onBH spin)
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Information from spectra andvariability
• X-ray ‘reflection’ givesimportant clues in thespectrum
• Variability timescalesand spectral changesshow differentspectral components
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Reflection from photoionized matter(Ross & Fabian 93, 05)
Also see Young+, Nayakshin+, Ballantyne+, Rozanska+, Dumont+
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Schwarzschild
Kerr
Fabian+89, Laor 90…Dovciak+04; Beckwith+Done05
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Suzaku
Strength and behaviour of line impliesGRAVITATIONAL LIGHT BENDING
MCG-6-30-15
Red wing due to largegravitational redshift
implying BH rapidly spinning
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Incidence of broad lines in XMM database Guainazzi+06 (see also Nandra+06)
Emphasises needfor good data
Broad lines found in>50% of spectra with
>150,000 counts
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Not just a line but wholereflection spectrum
Add relativistic blurring
Soft excess – broad iron line – Compton hump
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Crummy+05 22 PG QSO +12 Seyf1
Soft Excesses
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MCG-6 Suzaku: Miniutti+06
Observed reflection requires strong iron emission line
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Probing Black Hole Spin
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Assumption: measurements of rms determine (or constrain) a
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ISCO conjecture• Measure Rin from spectra ⇒ RISCO ⇒ spin?• B decreases Rin (Begelman & Reynolds, Gammie,
Krolik, Hawley…)??• BUT low ionization ⇒thin, slowly accretion disc,
which is not plunging, so Rin ~ RISCO
Computations show that Rin measured from iron lineis within ~0.5rg of Risco (Reynolds & Fabian 07)
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Density
Azimuthal field
Reynolds & Fabian 07 in press
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Reynolds & Fabian (ApJ in press)
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Assume illumination bysource on symmetry axis
of accretion disk atDs=6rg
Reynolds & Fabian (ApJ in press)
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Primary method… measure black hole spinusing the width/profile of the broad iron
line…Non-spinningRapidly-spinning
KERRDISK modelBrenneman & Reynolds (2006)
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GX339-4 Miller et al 04,07
LSVHS
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J. MillerSuzaku J Miller submitted
GX339-4
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Galactic BH:Disk hot, so line
Comptonized
Ross+Fabian07
GBH
AGN
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GX339-4withXMM
R Reis
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• Main point here is to demonstratethat we are seeing the accretion flowat ~2rg in several objects.
• This requires a rapidly spinning blackhole.
• Precise determination of spin requiresmodelling of flows and systematics.Current work suggests
~5%.
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XEUS z=0.5
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How does it vary?
Iwasawa+ Shih+ Fabian+ Vaughan+ McHardy+ Uttley+ Reynolds+
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Variable power-law
Quasi-constant reflection-dominated component
Schematic picture of the two-componentmodel
Data consistent withhighly variable power-law + quasi-constant reflection
spectrum
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Difference spectrum: (High flux)-(Low flux)
is a power-law modified by absorption
1 keV 10 keV
So we know which large scale features are due to absorption
Ratio to power-law
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Light bending model in Kerrspacetime
Miniutti et al 03; Miniutti & Fabian 04; earlier work by Matt+see also Tsuebsuwong, Malzac+06
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MCG-6 XMM 2000+2001 dataLarsson+06
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Variability
RMS fractional variability spectrum
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Mkn 335 2007 low state Grupe+07submitted
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• Broad iron lines enable the determinationof black hole spin
• Also enables study of the accretion flowand strong gravity effects (redshift andlight bending) of extreme gravity – howgravity works and powers quasars
• Next stage requires more photons fromAGN (which are relatively MUCH brighterthan GBH on a “per-light-crossing-time”basis)
• This implies next generation X-raytelescopes
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Armitage & Reynolds
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Arcs trace orbits ofdisk material aroundblack hole… can be
compared withpredicted GR orbits
Iron line intensity as function of energy and time.
Theoretical
Orbiting hot spots
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Andy Young andChris Reynolds
M=107 MsunF2-10=5×10-11
a=0.998
Reverberation
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Brightest lines are about 2 ph m-2 s-1
Need sources with high L/LEdd for broad lines(NLS1/GXRB)
Typically means•BH mass of 106-108 Msun•or timescales of 100s to 104s.
Therefore to study such BH on theirintrinsic variabilitylight crossing timescalesinner orbital period
⇒ effective collecting area at 6 keV in m2 class
XEUS has have the potential tomaker MAJOR advances
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