Time lags and reverberation in the lamp-post geometry of the compact corona illuminating a black-hole accretion disc

Transcription

1 Time lags and reverberation in the lamp-post geometry of the compact corona illuminating a black-hole accretion disc Michal Dovčiak Astronomical Institute Academy of Sciences of the Czech Republic, Prague Astrophysics group seminar, School of Physics, University of Bristol 13 th March 214

2 Acknowledgement StrongGravity ( ) EU research project funded under the Space theme of the 7th Framework Programme on Cooperation Title: Probing Strong Gravity by Black Holes Across the Range of Masses Institutes: AsU, CNRS, UNIROMA3, UCAM, CSIC, UCO, CAMK Webpages: en.html

3 Active Galactic Nuclei scheme Urry C. M. & Padovani P. (1995) Unified Schemes for Radio-Loud Active Galactic Nuclei PASP, 17, 83

4 Active Galactic Nuclei X-ray spectrum Fabian A.C. (25) X-ray Reflections on AGN, in proceedings of The X-ray Universe 25, El Escorial, Madrid, Spain, 26-3/9/25

5 References Blandford & McKee (1982) ApJ reverberation of BLR L o (v,t) = dt L p (t )Ψ(v,t t ) Stella (199) Nature time dependent Fe Kα shape (a = ) Matt & Perola (1992) MNRAS Fe Kα response and black hole mass estimate t GM/c 3 time dependent light curve, centroid energy and line equivalent width (h = 6, 1; a = ; θ o ) Campana & Stella (1995) MNRAS line reverberation for a compact and extended source (a = ) Reynolds, Young, Begelman & Fabian (1999) ApJ fully relativistic line reverberation (h = 1; a =, 1) more detailed reprocessing, off-axis flares ionized lines for Schwarzschild case, outward and inward echo, reappearance of the broad relativistic line

6 References Wilkins & Fabian (213) MNRAS fully relativistic, extended corona, propagation effects Cackett et al. (214) MNRAS Fe Kα reverberation in lamp-post model

7 Scheme of the lamp-post geometry central black hole mass, spin compact corona with isotropic emission height, photon index accretion disc Keplerian, geometrically thin, optically thick ionisation due to illumination (L p, h, M, a, n H, q n ) local re-processing in the disc REFLIONX with different directional emissivity prescriptions relativistic effects: Doppler and gravitational energy shift light bending (lensing) aberration (beaming) light travel time Ω r out corona black hole r in h M a δ i δ e observer Φ accretion disc

8 Time delay t [GM/c 3 ] a = r [GM/c 2 ] height y Time delay (a = 1., θo = 6 ) x y Total time delay (a = 1., θo = 6, h = 3) x total light travel time includes the lamp-to-disc and disc-to-observer part first photons arrive from the region in front of the black hole which is further out for higher source contours of the total time delay shows the ring of reflection that develops into two rings when the echo reaches the vicinity of the black hole

9 Light curve.25.2 a =, h = 3, t = 1 inclination a = 1, h = 3, t = 1 inclination Photon flux.15.1 Photon flux t [GM/c 3 ] t [GM/c 3 ] the flux for Schwarzschild BH is much smaller than for Kerr BH due to the hole below ISCO (no inner ring in Schwarzschild case) the shape of the light curve differs substantially for different spins the duration of the echo is quite similar the higher the inclination the sooner first photons will be observed magnification due to lensing effect at high inclinations

10 Dynamic spectrum signature of outer and inner echo in dynamic spectra large amplification when the two echos separate intrinsically narrow Kα line can acquire weird shapes

11 Transfer function for reverberation Stationary emission from the accretion disc: G = g µ e l F (E) = r dr dϕ G(r,ϕ)F l (r,ϕ,e/g) g = E E l Response to the on-axis primary emission: F (E,t) = dt r dr dϕ G(r,ϕ) N p (t )N inc (r)m(r,ϕ,e/g,t + t pd )δ([t t do ] [t + t pd ]) µ e = cosδ e l = ds o dsl N inc = ginc Γ dω p ds inc Line reverberation: F (E,t) = dt N p (t ) r dr dϕ Ψ (r,ϕ)δ(e ge rest )δ([t t ] [t pd + t do ]) }{{} t Ψ = g G N inc M Transfer function response to a flare [N p (t ) = δ(t )]: r Ψ(E,t) = Ψ (g, t) 1 (r, ϕ) F (E,t) = g = E/E rest t pd + t do = t E rest dt N p (t )Ψ(E,t t ) (g, t) (r,ϕ) = g r ( t) ϕ g ( t) g ( t) ϕ r

12 Caustics Schwarzschild case the black curves show the points where the energy shift contours are tangent to the time delay ones contour of ISCO in energy-time plane is shown by the blue curve the correspondent points A, B, C, D and E are shown in each plot for better understanding

13 Caustics extreme Kerr case the black curves show the points where the energy shift contours are tangent to the time delay ones contour of ISCO in energy-time plane is shown by the blue curve the correspondent points A, B, C, D and E are shown in each plot for better understanding

14 Caustics θo = 5, h = x g y t I plots of infinite magnification in the x-y (top) and g-t (bottom) planes I the plots for Schwarzschild case (red) above ISCO are very similar to the extreme Kerr case (blue) I the shape of these regions change with inclination

15 Dynamic spectrum narrow spectral line

16 Dynamic spectrum neutral disc

17 Dynamic spectrum ionised disc E 2 F (E)

18 Definition of the phase lag F refl (E,t) = N p (t) ψ(e,t) ˆFrefl (E,f ) = ˆN p (f ). ˆψ(E,f ) where ˆψ(E,f ) = A(E,f )e iφ(e,f ) if then N p (t) = cos(2πft) and ˆψ(E) = A(E)e iφ(e) F refl (E,t) = A(E)cos{2πf [t + τ(e)]} where τ(e) φ(e) 2πf F(E,t) N p (t) (ψ r (E,t) + δ(t)) ˆF (E,f ) ˆN p (f ).( ˆψ r (E,f ) + 1) and tanφ tot (E,f ) = A r(e,f )sinφ r (E,f ) 1 + A r (E,f )cosφ r (E,f )

19 Parameter values and integrated spectrum E 2 x F(E) 1 1 a = 1, h = 3, θ o = 3 reflected primary E [kev] M = 1 8 M a = 1 () θ o = 3 (6 ) h = 3 (1.5, 6, 15, 3) L p =.1L Edd Γ = 2 (1.5, 3) n H =.1 (.1, 5, 5,.2) 1 15 cm 3 q n = 2 (, 5, 3) Energy bands: soft excess:.3.8 kev primary: 1 3 kev iron line: 3 9 kev Compton hump: 15 4 kev

20 Phase lag dependence on geometry relative photon flux a = 1, θ o = 3 height [GM/c 2 ] t [ks] a = 1, θ o = 3-15 height [GM/c 2 ] f [µhz] relative photon flux a = 1, θ o = 6 height [GM/c 2 ] t [ks] a = 1, θ o = 6-1 height [GM/c 2 ] f [µhz] reflected photon flux decreases with height primary flux increases with hight the delay of response is increasing with height the duration of the response is longer the phase lag increases with height, it depends mainly on the average response time and magnitude of relative photon flux the phase lag null points are shifted to lower frequencies for higher heights due to longer timescales of response

21 Phase lag dependence on geometry.12.1 a = 1, θ o = 3 height [GM/c 2 ] a = 1, θ o = 6 height [GM/c 2 ] relative photon flux and the phase lag increase with inclination for low heights relative photon flux t [ks] relative photon flux t [ks] the delay and duration of response do not change much with the inclination and thus the phase lag null points frequencies change only slightly a = 1, θ o = 3 a = 1, θ o = height [GM/c 2 ] f [µhz] height [GM/c 2 ] f [µhz]

22 Phase lag dependence on spin and energy band relative photon flux a =, h = 3, θ o = 6 energy band.3-.8 kev 1-3 kev 3-9 kev 15-4 kev t [ks] a =, h = 3, θ o = energy band.3-.8 kev kev 15-4 kev f [µhz] relative photon flux a = 1, h = 3, θ o = 6 energy band.3-.8 kev 1-3 kev 3-9 kev 15-4 kev t [ks] a = 1, h = 3, θ o = 6 energy band kev 3-9 kev 15-4 kev f [µhz] the relative flux in the energy band where primary dominates may in some cases be larger than that in Kα and Compton hump energy bands the magnitude of the phase lag in different energy bands differs (in extreme Kerr case the larger lag in SE is due to larger ionisation near BH) the magnitude of the phase lag is smaller in Schwarzschild case due to the hole in the disc under the ISCO the null points of the phase lag change only slightly with energy and spin

23 Ionisation a = 1, h = 3, θ o = 3 ξ ionisation r [GM/c 2 ] f [µhz] the phase lag in Kα band is shown the reflection component of the spectra are steeper for higher ionisation the magnitude of the phase lag depend on ionisation the null points of the phase lag does not change with the ionisation

24 Directionality and photon index a = 1, h = 3, θ o = 3-6 directionality darkening -7 isotropic brightening f [µhz] a = 1, h = 3, θ o = 3 Np:Nr f [µhz] a = 1, h = 3, θ o = 3 photon index f [µhz] the phase lag in SE band is shown the magnitude of the phase lag changes in all three cases the null points of the phase lag does not change with different directionility dependences or power-law photon index

25 Phase lag energy dependence for low f : A r (E,f ) A E (E)A f (f ) φ r (E,f ) φ r (f ) and τ(e,f ) 1 2πf atan [A r (E,f ) A r (E,f )] sinφ r (f ) 1 + [A r (E,f ) + A r (E,f )] cosφ r (f ) + A r (E,f )A r (E,f ) and for f such that φ r (f ) = ± π 2 : τ(e,f ) 1 2πf [A r(e,f ) A r (E,f )]

26 Phase lag energy dependence a = 1, h = 3, θ o = energy band.3-.8 kev kev 15-4 kev f [µhz] a = 1, h = 3, θ o = 6 energy band kev 3-9 kev 15-4 kev f [µhz] a = 1, h = 3, θ o = 3 a = 1, h = 3, θ o = 6.1 f = 4µHz f = 13µHz E 2 x F(E).1 f = 4µHz f = 12µHz E 2 x F(E) E [kev] E [kev] the energy dependence of the phase lag follows the spectral shape perfectly at particular frequencies

27 Phase lag energy dependence a =, h = 3, θ o = 3-5 energy band kev 3-9 kev 15-4 kev f [µhz] a =, h = 3, θ o = energy band.3-.8 kev kev 15-4 kev f [µhz] a =, h = 3, θ o = 3 a =, h = 3, θ o = 6.1 f = 3µHz f = 11µHz E 2 x F(E).6.5 f = 3µHz f = 1µHz E 2 x F(E) E [kev] E [kev] if the second phase lag maximum is too small the phase lag energy dependence does not follow the spectral shape that well

28 Summary two aspects of reverberation in the timing and frequency domains the response of the disc peaks in the vicinity of the black hole the phase lag is used to get information on the system properties the frequency dependence of the phase lag is mainly due to geometry (height of the corona) the magnitude of the phase lag depends on many details of the model (height, spin, ionisation, unisotropy, energy,...) extended corona brings several new parameters (size, propagation speed, ignition position, inhomogeinities) broadens the response of the disc