Ultra-fast disk wind from a high accretion rate black hole 1H

Transcription

1 Ultra-fast disk wind from a high accretion rate black hole 1H Kouichi Hagino (ISAS/JAXA) H. Odaka, C. Done, R. Tomaru, S. Watanabe, T. Takahashi K. Hagino et al. 2016, MNRAS, 461, 3954 BREAKING THE LIMITS Super-Eddington Accretion on Compact island

2 Ultra-fast outflows Blue-shifted absorption lines with v0.1c is found in a part of local AGN (Chartas ; Reeves+ 2003; Pounds+ 2003a,b; Tombesi+ 2010) Absorbers moving from the black hole with v0.1c: Ultra-fast outflow (UFO) PDS 456 A spectrum of the ultra-fast outflow kev 2 (Photons cm 2 s 1 kev 1 ) FeXXV kev FeXXVI kev v~0.3c The physical mechanism to launch / accelerate the UFO is unclear Super-Eddington island

3 Physical mechanisms of disk winds Continuum radiation driving - radiation pressure (via Thomson scattering) exceeds gravity - need super-eddington UV line radiation driving Working in super-eddington AGN Working in sub-eddington AGN like PDS radiation pressure by bound-bound transition with UV photons - σbb > σt - efficiently accelerate if materials are moderately ionized - AGN radiate lots of UV may be working for UFOs Thermal driving - thermal velocity exceeds the escape velocity - slow velocity Magnetic driving - depends on unknown magnetic field configuration Super-Eddington island

4 Super-Eddington winds in AGN Observation Theory kev 2 (Photons cm 2 s 1 kev 1 ) PDS 456 and most of UFOs UV line driving (Sub-Eddington) Lbol/LEdd<1 Nomura et al Continuum driving (Super-Eddington) Takeuchi et al Lbol/LEdd>>1 Are there any UFOs with high accretion rates (Super-Eddington AGN)? Super-Eddington island

5 Super-Eddington AGN: 1H A narrow line Seyfert 1 galaxy (MBH~ M ) Super-Eddington is required by fitting the optical data 10 0 (a) Lbol/LEdd=146 (a=0.998) Lbol/LEdd=59 (a=0.9) Lbol/LEdd=20 (a=0) MBH= E*F(E) (kev 2 cm -2 s -1 kev -1 ) (OM) (CTIO) Done & Jin 2016 Lbol/LEdd=6.3 (a=0.998) Lbol/LEdd=2.5 (a=0.9) Lbol/LEdd=0.9 (a=0) MBH= Super-Eddington island

6 X-ray spectra of 1H A most convincing evidence of a rapidly spinning black hole (Fabian+ 2004). Powerlaw continuum Dovciak et al Reflected component Soft excess Zoghbi, Fabian et al Reflected component Powerlaw continuum This model requires extreme conditions: - Black hole spin is close to maximum. - Incident radiation is strongly focused on the disk inner edge Super-Eddington island

7 kev 2 (Photons cm 2 s 1 kev 1 ) Disk wind interpretation We propose a disk wind interpretation for the strong Fe-K spectral feature. 1H is very similar to an archetypal wind source PDS 456 (MBH~10 9 M, vwind~0.3c, Ṁwind~10M /yr) The spectral feature in 1H seems to be made by the disk wind PDS 456 brightest PDS 456 faintest 1H brightest 1H faintest Super-Eddington island 10 Absorption line is very broad, which cannot be explained by turbulence A new spectral model of the wind is required to explain the broad absorption line

8 Our disk wind model A new X-ray spectral model of an accretion disk wind has already been constructed for the UFO in PDS 456 (Hagino et al. 2015). disk wind X-ray source accretion disk D biconical geometry with Ω/4π=0.15 Velocity distributions: v r (l) =v 0 +(v v 0 ) ( 1 R min R min + l ) β Based on the UV-line driven disk wind Ionization structure: 1-D along the stream line Monte Carlo radiation transfer simulation: MONACO (Odaka+ 2011) Self-consistently calculate both of the emission and absorption Physical processes Photoionization Photoexcitation Compton scattering Doppler effect Super-Eddington island

9 slow & dense X-ray source fast & thin Simulated spectra θincl=46 deg θincl=58 deg accretion disk Blue-shifted absorption & broad emission like the observation At large θincl - high density deep absorption - observe slower component broad Larger inclination angle produces a very broad absorption line just like 1H Super-Eddington island Energy 14 (kev) Normalized flux Normalized flux flux Transmitted deg θincl=46 deg (Δθ=1 deg) Transmitted Reprocessed broad emission line deg θincl=58 deg (Δθ=1 deg) 5759 deg total Reprocessed total (Transmitted+reprocessed) blue-shifted absorption lines shift to lower energy abs. edge deep&broad absorption lines

10 Application to the observations of 1H Spectra of 1H are composed of 3 components. Continuum absorption Fe-K features Fe-K feature: created by the highly ionized gas (ξ~ ) kev 2 (Photons cm 2 s 1 kev 1 ) Soft excess our disk wind model Continuum absorption: Low ionized gas (ξ=l/ nr ) is required partial covering absorption Soft excess: not consider in this work Super-Eddington island

11 Application to the observations of 1H Spectra of 1H are composed of 3 components. than PG1244, though this is po! Fe-K Simple feature: wind models fit to 1H0 Highly ionized Continuum wind Fe-K created al. 2007), by the while highly more comple absorption features ionized Γ =2.6 gas (Hagino (ξ~ et) al. 2016), w Low ionized Hence the data are consistent our disk wind model clumps expected if it does have a high require this. Continuum Thusabsorption: there is no obvious i Low twoionized NLS1 where gas (ξ=l/ they have sim nr1h ) is has required higher inclination requires higher mass accretion partial covering 1H0707 is more super-edding absorption wind which explains its lack Soft excess shielding the NLR, suppressin Soft to PG1244 excess: (Leighly 2004). The not Eddington consider flow in this leading work to stron inclination angle means that the igure 3. Aschematic picture of the clumpy wind geometry from a superddington flow which could explain the difference in X-ray properties be- of sight for 1H Super-Eddington island kev 2 (Photons cm 2 s 1 kev 1 )

12 Spectral fit with the disk wind model kev 2 (Photons cm 2 s 1 kev 1 ) χ 2 ν=52.5/55 θincl=64.1 ( ) Obs3 kev 2 (Photons cm 2 s 1 kev 1 ) χ 2 ν=43.1/51 θincl=70.9 ( ) Obs Reproduced the structure above ~7 kev The spectra of 1H can be explained by the ultra-fast outflow (Mwind/ MEdd=0.2, v=0.2c) Super-Eddington island

13 Comparison with NuSTAR data The extrapolation of our wind model for Obs15 gives a good fit to the NuSTAR spectra Higher energy spectrum is also explained by our disk wind model!! kev 2 (Photons cm 2 s 1 kev 1 ) χ 2 ν=99.41/80 XMM-Newton Obs15 NuSTAR FPM-A/B ( ) Wind model for XMM Obs Super-Eddington island

14 Small residuals at ~6-7 kev However, there is a small residual at ~6-7 kev This could be residual reflection from the disk kev 2 (Photons cm 2 s 1 kev 1 ) χ (a) Wind model χ 2 ν=133.4/ Super-Eddington island

15 Reflection from the wider angle wind? Alternatively, the additional emission is possibly from a wider angle wind. Continuum-driven wind in super- Eddington accretion disk Naturally expected in super- Eddington accretion Driven by the radiation pressure via Thomson scattering, not boundbound transitions: Continuum-driven disk wind R/rs Hashizume et al The wind in 1H is possibly a continuum-driven disk wind Super-Eddington island

16 An extremely fast wind in APM Now, we are working on the extremely fast wind in APM v~0.7c is reported in this source by Chartas et al. (2009) Clearly, the absorption line in APM is less blue-shifted than that of PDS 456 We are trying to model the spectra without extremely fast wind Super-Eddington island

17 Conclusions We applied our new X-ray spectral model for the ultra-fast outflows to a super-eddington AGN: 1H The strong Fe-K feature in XMM-Newton/Suzaku/NuSTAR spectra of 1H are successfully reproduced by our disk wind model. Our disk wind model under-predict the emission lines, suggesting a wider angle wind by the continuum radiation driving mechanism. A super-eddington AGN 1H has an ultra-fast outflow Super-Eddington island