1. Black Hole Masses and accretion rates Thomas Boller Max-Planck Institut für extraterrestrische Physik, Garching

2. 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. 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 holes in X-ray binaries Canonical power-law with  =1.7 Rapid flux variation relative flux relative flux 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- Massive Black Holes Broad-line Seyfert 1 Narrow-Line Seyfert 1 relative flux relative flux Energy [keV] Energy [keV] Canonical power-law with  =1.7

4. 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 spectra Counts s -1 keV -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

5. Supercritical accretion in 1H0707-495 applies Slim disc model applies 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 disc in the  - dM/dt plane Mineshige 2000: All NLS1s from ASCA observations fall into the (dM/dt) / (L E /c 2 ) = (10 – 20) slim disc region Makishima 2000: Watarai 2001: L min and T bb give M min ~ 2. 10 6 M sun dM/dt ~ (10-20) (L E /c 2 ) ~ 6. 10 24 g s -1

6. Expected parameter changes due to black hole mass growth assumptions: NLS1 evolution starts in the slim disc regime (L ~ L edd ) dM/dt remains constant for some time and then gradually decreases Ionizing continuum decreases FWHM of emission lines increases HH [A] HH [OIII] Flux [A] Fe II [OIII] relative flux relative flux Energy [keV] Energy [keV] Huge soft X-ray excess in NLS1s Moderate soft X-ray excess In BLS1s Soft and hard power-law indices decreases Fe II multiplet emission decreases when ionizing continuum decreases

7. 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. 10 6 M sun ) accretion rate: 6. 10 24 g. s -1 (10 -3 earth mass per second) = 0.1 M sun / yr FWHM 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 yr NLS1 are the most rapidly growing black holes exp. growth linear growth Comparison with SDSS EDR Williams et al. 135 NLS1 out of 944 BLS1 assuming ~10 8 yr AGN phase mean NLS1s phase ~15 Millions years

8. 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/L edd dM/dt [eV] [10 44 ] [10 6 ] [M sun /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 Name L M L/L edd dM/dt [erg s -1 ] [M sun ] [M sun /yr] NGC 0315 1.2 10 43 1.3 10 9 1 10 -4 1 10 -6 NGC 1052 1.5 10 43 2.0 10 8 6 10 -4 1 10 -6 NGC 2681 7.0 10 39 5.6 10 7 1 10 -6 1 10 -8 3C 218 3.8 10 43 7.6 10 8 5 10 -4 1 10 -6 NGC 2728 6.3 10 39 4.0 10 7 1 10 -4 1 10 -6 M81 5.0 10 41 6.1 10 7 7 10 -5 7 10 -7 NGC 3125 3.2 10 41 5.9 10 5 4 10 -3 4 10 -5 NGC 3169 2.3 10 41 7.2 10 7 3 10 -5 3 10 -7 NGC 3245 2.4 10 40 2.4 10 8 1 10 -6 1 10 -8 NGC 3718 1.9 10 42 8.5 10 7 2 10 -4 2 10 -6 NGC 4125 1.5 10 40 3.1 10 8 3 10 -7 3 10 -9 NGC 4203 4.0 10 41 7.9 10 7 4 10 -5 4 10 -11 NGC 4278 4-0 10 41 1.6 10 9 2 10 -6 2 10 -13 … 34 LINERS from Cariollo et al. 1999, Satypal 05, Dudek 05 Boller, Tanaka (in prep.)

9. 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 emission to disentangle AGN contribution from other emission prosses Balestra, Boller

10. 10 AGN Workshop of the Israel Science Foundation: in celebration of Hagai Netzer´s 60th birthday 0 2 4 6 Time [10 9 yr] 10 6 10 8 10 10 [M sun ] IRAS 13224-3809 5 10 7 yr 1 10 8 yr 3 10 8 yr 5 10 8 yr 0 yr 8 10 8 yr 2 10 9 yr IRAS 13349 NGC 0315 0 yr 2 10 9 yr NGC 2728 0 yr 2 10 9 yr NGC 3125 0 yr Black Hole growths for NLS1s and LINERs

11. 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 LINER caveates: - separate nuclear emission -following Hagai´s comment: if SLOAN people are right, LINERs shift up

12. 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 fit to IRAS 13224-3809 strong residua Null hypothesis value <0.1 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…

13. 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. 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. 2003Netzer et al. 2004 Clear trend of FeII/H  with accretion rate for NLS1 and high-z QSO optical Fe II emission increases with accretion rate

15. 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 L min / L edd ~ 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 ~10 6 M sun and are rapidly growing in mass with ~ dM/dt ~ (1-20) (L E /c 2 ) 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