Black%20Hole%20Masses%20and%20accretion%20rates

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Black Hole Masses and accretion rates
Thomas Boller Max-Planck Institut für
extraterrestrische Physik, Garching
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Present knowledge on black hole masses and
accretion rates
The effect of mass accretion rate on X-ray
properties
Analysis of individual NLS1 spectra
Supercritical accretion in 1H0707-495
Accretion-rates and Black hole masses in extreme
accretion modes
Spectral complexity dependence on the accretion
rate
Metallicity dependence on the accretion rate
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The effect of mass accretion rate on X-ray
properties
Accretion-rate dependent differences may exist in
AGN as well
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Analysis of individual NLS1 spectra
Drop energy is time-dependent (7.1 keV in 2000,
7.5 in 2002), remains sharp even for 8.2 keV
drop in 13224, no Kb UTA absorption, therefore
high outflow v of neutral Fe of 0.05 and 0.15 c
are required
Both show a common characteristic shape - strong
soft X-ray excess - steep power-law with G
2.42.5
These features are typical for partial covering
phenomenon, or reflection dominated X-ray spectra
The hard tail gradually flattens towards high
energies and abruptly drops at around 7-8 keV
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Supercritical accretion in 1H0707-495
Slim disc model applies to such high accretion
rates and high disc
temperatures

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Expected parameter changes due to black hole mass
growth
assumptions NLS1 evolution starts in the slim
disc regime (L Ledd)
dM/dt remains constant for some time and then
gradually decreases
Soft and hard power-law indices decreases
Fe II multiplet emission decreases when
ionizing continuum decreases
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Simple picture for the optical line widths
evolution of Seyfert 1s
Assumptions all galaxies go through an AGN
phase the case for
1H0707 (a NLS1s starting with a small mass of 2
. 106 Msun) accretion
rate 6 . 1024 g . s-1 (10-3 earth mass per
second) 0.1 Msun/ yr
10000 km s-1
NLS1 BLS1 phase
exp. growth
90 Million years
Comparison with SDSS EDR Williams et al. 135 NLS1
out of 944 BLS1 assuming 108 yr AGN phase mean
NLS1s phase 15 Millions years
FWHM Hb km s-1
4600 km s-1
60 Million years
2000 km s-1
linear growth
25 Million years
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Growth time yr
when high accretion rate ceased, 1H0707 become
normal Seyfert 1s within a few 10s million yr
NLS1 are the most rapidly growing black holes
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Accretion-rates and Black hole masses in extreme
accretion modes
Low efficiency accretion
Super-Eddington Accretion
Name L M L/Ledd
dM/dt erg s-1 Msun
Msun/yr NGC 0315 1.2 1043
1.3 109 1 10-4 1 10-6 NGC 1052 1.5
1043 2.0 108 6 10-4 1 10-6 NGC 2681
7.0 1039 5.6 107 1 10-6 1 10-8 3C 218
3.8 1043 7.6 108 5 10-4 1 10-6 NGC
2728 6.3 1039 4.0 107 1 10-4 1 10-6
M81 5.0 1041 6.1 107 7 10-5 7
10-7 NGC 3125 3.2 1041 5.9 105 4 10-3 4
10-5 NGC 3169 2.3 1041 7.2 107 3 10-5 3
10-7 NGC 3245 2.4 1040 2.4 108 1 10-6 1
10-8 NGC 3718 1.9 1042 8.5 107 2 10-4 2
10-6 NGC 4125 1.5 1040 3.1 108 3 10-7 3
10-9 NGC 4203 4.0 1041 7.9 107 4 10-5 4
10-11 NGC 4278 4-0 1041 1.6 109 2 10-6 2
10-13 34 LINERS from Cariollo et al. 1999,
Satypal 05, Dudek 05
Name kT L M L/Ledd
dM/dt eV 1044 106
Msun/yr PHL 1092 128 60
10 3 0.03 NAB 0205 120 24
6 3 0.03 IRAS 13349 97 9
4 2 0.02 Akn 564 129
7 2 2 0.02 PG1211 117
4 2 2 0.02 1H0707 92
4 2 10 0.10 IRAS 13224 130
3 1 2 0.02 Mrk 335 130
3 1 2 0.02 PG1204
120 3 1 1 0.01 Mrk 1044
105 0.5 0.4 0.7 0.007 NGC 4051
130 0.01 0.1 0.2 0.002
Boller, Tanaka (in prep.)
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LINER galaxy IC 1459
Balestra, Boller
Separation of nuclear emission from optically
thin gas and point sources emission to
disentangle AGN contribution from other emission
prosses
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Black Hole growths for NLS1s and LINERs
IRAS 13224-3809
2 109 yr
5 108 yr
IRAS 13349
NGC 0315
2 109 yr
0 yr
3 108 yr
8 108 yr
106 108
1010
Msun
NGC 2728
1 108 yr
2 109 yr
0 yr
5 107 yr
0 yr
NGC 3125
0 yr
0 yr
0 2
4
6 Time
109 yr
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Accretion-rates dependence on Black hole masses
NLS1s

• LINER
• caveates
• - separate
• nuclear
• emission
• following
• Hagais comment
• if SLOAN people
• are right,
• LINERs
• shift up

LINERs
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Spectral Complexity in dependence on the
accretion rate
Power-law fit to IRAS 13224-3809 strong
residua Null hypothesis value lt0.1 in 2-10 keV
band 0.0 in 0.3 10 keV band e.g. low Null
hypothesis values indicative for spectral
complexity as soft excess, lines
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Spectral complexity correlates with accretion
rate
fit in the 2-10 keV range LINERS often as a
simple power-law NLS1s more complex -
soft excess - spectral curvature -
sharp spectral drops
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Metallicity dependence on the accretion rate
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Summary
X-ray observations on the disc temperature and
the luminosity allow to measure black hole masses
and accretion rate, independent from optical line
width relations The NLS1s are accreting at
luminosities close or above the Eddington
luminosity Lmin/ Ledd 1-2 The black body
temperature is high 90-120 eV and exceeds the
limit from standard geometrically thin accretion
discs The objects have relatively low black hole
masses of 106 Msun and are rapidly growing in
mass with dM/dt (1-20) (LE/c2) When the
high accretion rates are ceased NLS1s become
normal Seyfert 1s within a few 10s Million
years NLS1s are the most rapdily growing black
holes in the universe LINERS accrete at extreme
low Eddington luminosity ratios