Black hole spin from reflection Mari Kolehmainen amp Chris Done Durham University Maria Diaz Trigo ESO The Xray Universe 2011 Berlin Germany 27 30 June 2011 Black hole spin Specific angular momentum ID: 778606
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Slide1
The high mass accretion rate spectra of GX 339-4: Black hole spin from reflection?
Mari Kolehmainen & Chris Done,Durham UniversityMaria Diaz Trigo, ESO
The X-ray Universe 2011
Berlin, Germany
27 - 30 June 2011
Slide2Black hole spinSpecific angular momentum, described as a dimensionless parameter a
*a* : 0 - 0.998 Rin : 6 - 1.24 Rgcurrently 2 ways to determinedisc fitting Fe line
2
a
*
=0
a
*
=0.998
Slide3Black hole spin: disc fitting3
log ν f(ν)log ν
R
in
GX 339-4
Slide4Black hole spin: disc fitting4
log ν f(ν)log ν
R
in
GX 339-4
Slide5Black hole spin: disc fitting
5log ν f(ν)
log ν
R
in
GX 339-4
Slide6Black hole spin: Fe-line profile
6
Iron emission line from reflected emission
Fabian
et al. 2000
Slide7Comparing spin measurements: High mass accretion rate spectra
Disc continuum fittingdisc dominated spectraclassical high/soft stateFe line profile strong hard X-ray tailvery high/soft intermediate states
7
Slide8Comparing spin measurements: GX 339-4
Disc fitting gives upper limita* < 0.9 from RXTE spectra (Kolehmainen & Done 2010)
Fe line values highera*
= 0.94
from XMM-Newton
Burst mode soft intermediate state
(Miller et al. 2004)
a
*= 0.89
from Suzaku intermediate state
(Miller et al. 2008 vs. Yamada et al. 2009)a*= 0.94
from XMM-Newton LHS
(Reis et al. 2008 vs. Done & Diaz
Trigo
2010)
8
Slide9XMM-Newton EPIC pn Burst mode
Time resolution 7μs Pileup limit 60,000 counts/s Timing mode 30μs (800 counts/s) Duty cycle 3 %
photon collecting time/readout time
9
Slide10High mass accretion rate spectra of GX 339-4
Joint EPIC-pn/RXTE observations (0.7-25
keV)
Fast timing mode data,
not piled up!
3 disc dominated states
2 soft intermediate states
(SIMS)
10
4-7
keV
Slide11Below the RXTE energy band11
GX 339-43
keV
Slide12DISKBBsimplest multi-colour disc blackbody
KERRBBstress-free inner boundary condition, colour- temperature correction and relativistic smearingBHSPECcalculates radiative transfer through each disc annuliincludes all the relativistic
correctionsassumes Rin
=R
ISCO
Continuum fitting below 3
keV
:
Disc dominated state
12
Slide13DISKBBsimplest multi-colour disc blackbody
KERRBBstress-free inner boundary condition, colour- temperature correction and relativistic smearingBHSPECcalculates radiative transfer through each disc annuliincludes all the relativistic
correctionsassumes Rin
=R
ISCO
Continuum fitting below 3
keV
:
Disc dominated state
13
Slide14DISKBBsimplest multi-colour disc blackbody
KERRBBstress-free inner boundary condition, colour- temperature correction and relativistic smearingBHSPECcalculates radiative transfer through each disc annuliincludes all the relativistic
correctionsassumes Rin
=R
ISCO
Continuum fitting below 3
keV
:
Disc dominated state
14
Slide15Continuum fitting below 3 keV:
Disc dominated stateDisc modeluse this as seed photons for Comptonisation to make X-ray tail
(convolved with Simpl
(
Steiner et al. 2009
))
Reflection
of Comptonised continuum
using ionised reflection models of
Ross &
Fabian
Relativistic smearing (
kdblur
)
15
Slide16Continuum fitting below 3 keV:
Disc dominated state16
BHSPEC+reflected continuum
very steep continuum to make disc broader
high reflection fraction
misses high energies
residuals around 1
keV
Slide17Continuum fitting below 3 keV:
Disc dominated state17
BHSPEC+reflected continuum
very steep continuum to make disc broader
high reflection fraction
misses high energies
residuals around 1
keV
Slide18Continuum fitting below 3 keV:
Disc dominated state18
(
diskbb+compTT)+reflected
continuum
reasonable reflection
fraction+continuum
extrapolates to high energies
fit for different mass accretion rates
Slide19Continuum fitting below 3 keV:
Disc dominated state19
(
diskbb+compTT)+reflected
continuum
reasonable reflection
fraction+continuum
extrapolates to high energies
fit for different mass accretion rates
Slide20Continuum fitting below 3 keV:
Disc dominated state DATA vs. BHSPEC
20
Slide21Continuum fitting below 3 keV:
LMC X-3 DATA vs. BHSPEC
21
Slide22Previously derived a strict upper limit for the spin in
GX 339-4 from continuum fitting of disc dominated RXTEspectra (Kolehmainen & Done, 2010)a*
< 0.9 for any reasonable mass (<15M
),
distance
(>6 kpc) and inclination (i > 45°)
GX 339-4 widely studied in
terms of Fe-line
burst mode spectrum gave a
*
= 0.935
(e.g. Miller et al. 2004; Reis et al. 2008)
Soft intermediate state: the Fe line
22
Miller et al. 2004
Slide23Soft intermediate state: the Fe line
diskbb+podisc, power law tailcontinuum modelled by ignoring 4−7 keV
Residuals show a broad iron line
23
Obsid
0156760101
Slide24Soft intermediate state: the Fe line
(diskbb+compTT)+reflected continuumconvolved disc+thermal Comptonisation, ionised smeared reflection
Narrow line does not constrain
BH spin
24
Obsid
0156760101
Slide25ConclusionsWhat we ARE saying:
Burst mode goodReal disc spectra broader than diskbb or even BHSPECChanging the continuum model changes the shape of the Fe line profile (and black hole spin) 25What we are NOT saying:
The Fe line does not exist
Calibration issues are in the past
Slide2626
Slide2727
Slide28ConclusionsThe XMM-Newton Burst mode can actually be used to make science can look at the disc below 3 keV
even with the brightest objectsReal disc spectra are much broader than diskbbChanging the continuum model changes the shape of the iron line (and the BH spin)28
Slide29Continuum fitting below 3 keV:
Disc dominated stateDisc modeluse this as seed photons for Comptonisation (convolved with
Simpl
(
Steiner et al. 2009
))
to make X-ray tail
Relativistic smearing (
kdblur
)
Reflection
of Comptonised continuum
using ionised reflection models of
Ross &
Fabian
29
Slide30DISKBB
simplest multi-colour disc blackbodyKERRBBstress-free inner boundary condition, relativistic smearing and the colour- temperature correctionBHSPECcalculates radiative transfer
through each disc annuli
includes all the relativistic
corrections
assumes R
in
=R
ISCO
Continuum fitting below 3
keV
:
Disc dominated state
30
Slide31Continuum fitting past the disc dominated state: The model
tbabs × simpl*(diskbb+compTT) +
kdblur
*
refxion
*(
simpl
*(
diskbb+compTT
))
the major advantage comes from being able to fit for different mass accretion rates
31
Slide32Continuum fitting below 3 keV:
Disc dominated state DATA vs. BHSPEC Kerrbb
32
Slide33Burst mode observations of GX 339-4M = 10 MD = 8 kpc
i = 60°0093562701 (discy)0156760101 (SIMS)0410581201 (discy)0410581301
(SIMS)0410581701 (discy
)
33
Kolehmainen & Done 2010
Slide34Previously derived a strict upper limit for the spin in
GX 339-4 from continuum fitting of disc dominated RXTEspectra (Kolehmainen & Done, 2010)a* < 0.9 for any reasonable mass (<15M
) distance (>6 kpc) and
inclination (i > 45°)
The Fe-line and the BH spin
34
Slide35Broad iron emission line
profile a self consistent way to determine BH spinBlack hole spin: the Fe line profile
35
Miller et al. 2004