Space-Time around a Black Hole Accretion Disk is in the Space-Time.
Black Hole Masses and accretion rates
description
Transcript of Black Hole Masses and accretion rates
Black Hole Masses and accretion rates
Thomas BollerMax-Planck Institut für extraterrestrische Physik, Garching
2
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
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
Present knowledge on black hole masses and accretion rates
The effect of mass accretion rate on X-ray properties
3
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
The effect of mass accretion rate on X-ray properties
Accretion-rate dependent differences may exist in AGN as well
Low accretion rate: hard state
Black holesin X-ray binaries
Canonical power-law with =1.7Rapid flux variation
rel a
tive fl
ux
rel a
tive fl
ux
Energy [keV]Energy [keV]
High accretion rate: soft state
Black body type soft excess and significantly steeper power-law(~2.2-2.5)
Energy [keV]Energy [keV]
Super-MassiveBlack Holes
Broad-line Seyfert 1 Narrow-Line Seyfert 1
rel a
tive fl
ux
rel a
tive fl
ux
Energy [keV]Energy [keV] Energy [keV]Energy [keV]
Canonical power-law with =1.7
These features are typical for partial covering phenomenon, or reflection dominated X-ray spectra
Both show a common characteristic shape - strong soft X-ray excess - steep power-law with = 2.4~2.5
The hard tail gradually flattens towards high energies and abruptly drops at around 7-8 keV
IRAS 13224-3809
0.2 1 2 3 5 10 Energy [keV]
Analysis of individual NLS1 spectraC
oun
ts s
-1 k
eV-1
1H 0707-495
0.2 1 2 3 5 10 Energy [keV]
pn
MOS
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 K UTA absorption, therefore high outflow v of neutral Fe of 0.05 and 0.15 c are required
7.1,7.5 keV 8.2 keV
Supercritical accretion in 1H0707-495Slim disc model appliesapplies to such high accretion rates and high disc temperatures
Abramowicz 1988: Solutions for high accretion rates based on additional cooling due to horizontal advection of heat;adding a new branch to the Shakura-Sunyaev discin the - dM/dt plane
Mineshige 2000: All NLS1s from ASCA observations fall into the(dM/dt) / (LE/c2) = (10 – 20) slim disc region
Makishima 2000:Watarai 2001:
Lmin and Tbb give Mmin ~ 2.106 Msun
dM/dt ~ (10-20) (LE/c2) ~ 6.1024 g s-1
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
Ionizing continuum decreases
4
12
M
M~tT
4
12
M
M~tT
FWHM of emission lines increases 16
32
4
1
e M
M2n~tFWHM
H
[A]
H [OIII]
Flux
[A]
Fe II Fe II
[OIII]
4
12
M
M~tT
rela
tive
flux
rela
tive
flux
Energy [keV]Energy [keV] Energy [keV]Energy [keV]
Huge soft X-ray excess in NLS1s
Moderate soft X-ray excessIn BLS1s
Soft and hard power-law indices decreases
Fe II multiplet emission decreases when ionizingcontinuum decreases
Growth time [yr]8
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 FW
HM
H
[km
s-1]
2000 km s-1
25 Million years
60 Million years
4600 km s-1
10000 km s-1
90 Million years
NLS1 BLS1 phase
when high accretion rate ceased, 1H0707 become normal Seyfert 1s
within a few 10´s million yrNLS1 are the most rapidly growing black holes
exp.
gro
wth
linear growth
Comparison with SDSS EDRWilliams et al. 135 NLS1 out of 944 BLS1assuming ~108 yr AGN phasemean NLS1s phase ~15 Millions years
8
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
Accretion-rates and Black hole masses in extreme accretion modes
Super-Eddington Accretion Low efficiency accretion
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 0.03IRAS 13349 97 9 ~4 2 0.02Akn 564 129 7 ~2 2 0.02PG1211 117 4 ~2 2 0.021H0707 92 4 ~2 10 0.10IRAS 13224 130 3 ~1 2 0.02Mrk 335 130 3 ~1 2 0.02PG1204 120 3 ~1 1 0.01Mrk 1044 105 0.5 ~0.4 0.7 0.007NGC 4051 130 0.01 ~0.1 0.2 0.002
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
Boller, Tanaka (in prep.)
9
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
LINER galaxy IC 1459
Separation of nuclear emission from optically thin gas and point sources emissionto disentangle AGN contribution from other emission prosses
Balestra, Boller
10
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
0 2 4 6 Time [109 yr]
106
1
08
1010
[Msu
n]IRAS 13224-3809
5 107 yr
1 108 yr
3 108 yr
5 108 yr
0 yr
0 yr
8 108 yr
2 109 yr
IRAS 13349
NGC 03150 yr
2 109 yr
NGC 27280 yr 2 109 yr
NGC 3125
0 yr
Black Hole growths for NLS1s and LINERs
11
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
Accretion-rates dependence on Black hole masses
NLS1s
BLS1s
NLS1s
LINERs
BLS1s
LINERs
LINERcaveates:
- separate nuclear emission
-following Hagai´s comment: if SLOAN people are right, LINERs shift up
12
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
Spectral Complexity in dependence on the accretion rate
Power-law fitto IRAS 13224-3809
strong residua
Null hypothesis value <0.1in 2-10 keV band
0.0 in 0.3 10 keV band
e.g. low Null hypothesisvalues indicative forspectral complexityas soft excess, lines…
13
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
fit in the 2-10 keV range
LINERS often as a simple power-law
NLS1s more complex - soft excess - spectral curvature - sharp spectral drops
Spectral complexity correlates with accretion rate
14
AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday
Metallicity dependence on the accretion rate
13224 with super-Eddington accretion
Fe overabundance 3-10 required in all NLS1s with sharp spectral drop, even for reflection dominated model
Boller et al. 2003 Netzer et al. 2004
Clear trend of FeII/H with accretion rate for NLS1 and high-z QSO
optical Fe II emission increases withaccretion rate
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 10´s Million years
NLS1s are the most rapdily growing black holes in the universe
LINERS accrete at extreme low Eddington luminosity ratios