Irradiation of an Accretion Disk by a Jet: Spin Measurements of Black Holes Thomas Dauser in collaboration with J. Wilms, J. Garcia (CfA/UMd), R. Duro, C. S. Reynolds (UMd), N. Schartel (ESA-ESAC), K. Pottschmidt (CRESST/UMBC/NASA-GSFC), M. A. Nowak (MIT), and many others Dr. Karl Remeis Observatory Bamberg & ECAP
What can we learn from the Spin of a Black Hole Example: Galaxy Evolution Steady Growth Galaxy Mergers Bardeen (97) Volonteri et al. (25) King et al. (28).8.8.8 P(a).6.4 P(a).6.4 P(a).6.4.2.2.2 - spin a - spin a - spin a Spin: < a < (Rotation Velocity with respect to the Accretion Disk) Spin could distinguish Galaxy Evolution Models
What can we learn from the Spin of a Black Hole Example: Jet Formation Jet-Formation is connected in most models to the BH spin (e.g., Blandford & Znajek, 977) Jet Power Garofalo et al. (2): most powerful jets from retrograde (a = ) BHs Spin Measuring Jet-Power vs. Spin relation constrains Jet Models
Irradiation and Reflection Jet Accretion Disk
Irradiation and Reflection Jet (Reynolds, 996) Accretion Disk
Irradiation and Reflection 7 Jet Counts per unit energy (arb.) 6 5. (Reynolds, 996). Ionized Reflection (García & Kallman, 2; García et al., 2) Accretion Disk
Relativistic effects close to the black hole α[rg] -6-4 -2 2 4 6 4-2 β[rg] -2-4 E/Ee.4.3.2..9.8.6.4 - -.3 -.2 -....2.5. Redshift z (Dauser et al., 2) Rotating Black Hole: Metric depends on M (mass) and a (spin) special relativistic beaming, light bending, and gravitational redshift (Kerr, 963; Cunningham, 975; Fabian et al., 989; Laor, 99; Dovčiak et al., 24; Dauser et al., 2)
Broad Emission Lines α[rg] -6-4 -2 2 4 6 4-2 + β[rg] -2-4 E/Ee.4.3.2..9.8.6.4 - -.3 -.2 -....2.5. Redshift z = Flux [a.u.] 3 2.5 2.5 Fe Kα (6.4keV).5 4.5 5 5.5 6 6.5 7
Diagnostic potential: inclination.8 E/E e.9.. θ o 5 2 3 4 5 6 7 8 5 ǫ=.5 a=. 5.5 6 6.5 7 8 6 4 2 Flux [a.u.] θ = 4 θ = 8
Diagnostic potential: Irradiating Source h h=3r g h=r g h=25r g h=5r g h=r g h=5r g a=+.99 θ=4 2 8 6 4 Flux [a.u.] 2 5 6 7 determines the incident radiation on the accretion disk low height implies enhanced irradiation of the inner parts radially extended sources are also possible Jets
Diagnostic potential: black hole spin.8 E/E e.9.. a +. +.8 +.6 +.3 +..3.5. θ o =4 ǫ=3. 4 2 Flux [a.u.] 5 5.5 6 6.5 7 possible Spin values: a =... high Spin broad line
Observations of Broad Iron Lines. Ratio.5 4 5 6 7 8 AGN MCG 6-3-5: a >.98 (Brenneman & Reynolds, 26; Miniutti et al., 27) both instruments measure the same line shape stellar mass BH Cyg X-: a >.9 (Duro & Dauser et al., 2) most prominent Kα line in a stellar mass BH
... yes, broad lines are everywhere Data/Model.9...2.9...2 stellar mass Black Holes XTE J55 564..2.8 2 4 6 8 2 4 6 8 Cygnus X.. GRO J655 4 GRS 95+5 2 4 6 8 2 4 6 8 data/model.9.95.5. AGN NGC 3783 (Brenneman et al., 2) 5 Energy (kev) NGC 356 (Iwasawa et al., 24) after Miller (27)
Constraining the Spin from Observations How good can we distinguish high spin from low spin? extended Jet compact Jet high Spin low Spin.8.6.4.2.8.6.4.2 Flux [a.u.] Flux [a.u.] (a) (b) a =.99 a = a =.99 a =.5..5.95.5..5 Ratio Ratio 2 4 6 2 4 6 4 6.95
Constraining the Spin from Observations How good can we distinguish high spin from low spin? extended Jet compact Jet high Spin low Spin.8.6.4.2.8.6.4.2 Flux [a.u.] Flux [a.u.] (a) (b) a =.99 a = a =.99 a =.5..5.95.5..5 Ratio Ratio 2 4 6 2 4 6 4 6.95 A detected broad line yields the spin and indicates a compact emission region compact emission region. (Dauser et al., 23)
Robust Spin Estimation AGN H77 495: iron Kα and Lα line detected Dauser et al. (22) νfν[ 2 ergs s cm 2 ]. first AGN with detected iron Kα and Lα (see, e.g., Fabian et al., 29; Zoghbi et al., 2) Ratio..5.5.5 2 5 two reflection components with different ionization, high spin (a >.99), and low jet height (h < 4r g)
Robust Spin Estimation stellar mass BH Cyg X-: Broad Band Spectrum XMM-Newton RXTE-PCA RXTE-HEXTE Integral Duro & Dauser et al. (23, in prep.) νfν [ 6 ergs s cm 2 ] χ 5 2 5 3 - -3-5 5 2 5 2 5 Broad Band Coverage (Simultaneous observations) ( first robust stellar mass BH spin measurement) Cygnus X- is a fast rotating black hole (a >.9), and compact emission region (h < 4r g) Spin in agreement with the disk-spin method (Gou et al., 2)
Summary Relativistic effects distort reflection features produced close to the BH Broad Emission Lines Line Shapes are sensitive to the Spin and other parameters A detected broad line yields the spin and indicates a compact emission region compact emission region Additional information (e.g.,broad band spectra) is necessary for robust spin estimates.
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