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Study of accretion and ejection flows around supermassive black holes in AGNs

MC reports after inputs taken from: CNES doc. (Ferrando et al.); SX-SciRD (Giommi et al.); DOC 40 (Costa et al.); with contributions from Giommi, Grandi, Migliori, Ponti. Selected issues on AGNs for Simbol-X. Issue n.3.

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Study of accretion and ejection flows around supermassive black holes in AGNs

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  1. MC reports after inputs taken from: CNES doc. (Ferrando et al.); SX-SciRD (Giommi et al.); DOC 40 (Costa et al.); with contributions from Giommi, Grandi, Migliori, Ponti Selected issues on AGNs for Simbol-X Issue n.3 Study ofaccretionand ejectionflows around supermassive black holes in AGNs Jet Characterise the particle content, geometry and velocity of the outflow/jet Characterise the geometry and velocity of the outflow/wind, and its impact on the host galaxy and cluster Issue n.2 Characterise the geometry and mode of the accretion flow Hot corona Issue n.1 Credit: A. Mueller

  2. Goal:Characterise the geometry and mode of accretion flow Open Problems: disentangle (heavy) absorption vs (blurred) reflection in RQs, and thermal vs. non-thermal in RLs (Key) Requirement:Broad-band (0.1-100 keV) spectra Impact on:BH astrophysics Issue n.1 Goal:Characterise the geometry and velocity of the outflow/wind, and its impact on the host galaxy and cluster Open Problems: confirm massive warm-absorbers in RQs, and non-thermal mapping in radio-lobes/hot-spots (Key) Requirement:Hard (2-20 keV) spectra + imaging Impact on:BH-galaxy and BH-cluster co-evolution Issue n.2 Goal:Characterise the particle content, geometry and velocity of the outflow Open Problems: confirm high-velocity, massive, & variable warm absorbers in RQs, and SSC vs SEC in RLs (Key) Requirement:Hard (2-20 keV) spectra + Broad-band spectra Impact on:Jet formation, acceleration physics, and cosmic backgrounds Issue n.3

  3. Goal:Characterise the geometry and mode of accretion flow Open Problems: disentangle (heavy) absorption vs (blurred) reflection in RQs, and thermal vs. non-thermal in RLs (Key) Requirement:Broad-band (0.1-100 keV) spectra Impact on:BH astrophysics Issue n.1 Q: Heavy absorber or blurred relativistic reflection? …This is the question… A: Hard X-ray spectra Simbol-X simulations To Be Done Reflection Absorption NLSy1: 1H0707-495 (Fabian et al. 2003;Tanaka et al. 2004)

  4. Goal:Characterise the geometry and mode of accretion flow Open Prolems: disentangle (heavy) absorption vs (blurred) reflection in RQs, and thermal vs. non-thermal in RLs (Key) Requirement:Broad-band (0.1-100 keV) spectra Impact on:BH astrophysics Issue n.1 Q: Thermal or non-thermal? A: Broad-band spectra Simbol-X simulations To Be Done 3C273: Grandi & Palumbo 2004, Science

  5. Goal:Characterise the geometry and velocity of the outflow/wind, and its impact on the host galaxy and cluster Open Problems: confirm massive warm-absorbers in RQs, and non-thermal mapping in radio-lobes/hot-spots (Key) Requirement:Hard (2-20 keV) spectra + imaging Impact on:BH-galaxy and BH-cluster co-evolution Issue n.2 Q: Massive high-velocity absorbers? PG1211+143 A: Highest possible throughput between 2-20 keV 2 Energy (keV) 5 7 10 Simbol-X simulation PDS456 2 Energy (keV) 5 7 10 Pounds et al. 2003,Reeves et al. 2003

  6. Goal:Characterise the geometry and velocity of the outflow/wind, and its impact on the host galaxy and cluster Open Problems: confirm massive warm-absorbers in RQs, and non-thermal mapping in radio-lobes/hot-spots (Key) Requirement:Hard (2-20 keV) spectra + imaging Impact on:BH-galaxy and BH-cluster co-evolution Issue n.2 Pictor A: Grandi, Migliori et al., in prep Q: Where/how is non-thermal emission in RGs and clusters? A: Detailed Imaging at high energies Simulated Images (TBD) Perseus Cluster: Fabian et al. 2006

  7. Goal:Characterise the particle content and geometry and velocity of the outflow Open Problems: confirm high-velocity, massive, & variable warm absorbers in RQs, and SSC vs SEC in RLs (Key) Requirement:Hard (2-20 keV) spectra + Broad-band spectra Impact on:Jet formation, acceleration physics, and cosmic backgrounds Issue n.3 Seyfert Gal NGC1365: Risaliti et al., 2005 Q: Massive and variable absorber? A: Highest possible throughput between 2-20 keV Simbol-X simulation

  8. Goal:Characterise the particle content, geometry and velocity of the outflow Open Problems: confirm high-velocity, massive, & variable warm absorbers in RQs, and SSC vs SEC in RLs (Key) Requirement:Hard (2-20 keV) spectra + Broad-band spectra Impact on:Jet formation, acceleration physics, and cosmic backgrounds Issue n.3 Q: SSC vs. SEC? A: Broad-band spectra (SED+flare behaviour) Giommi et al. 2006 Simulated spectra (TBD?)b

  9. Summary of key requirements TO BE QUANTIFIED!! Issue n.3 Study ofaccretionand ejectionflows around supermassive black holes in AGNs Broad-band spectra and SEDs Broad-band spectra and images Issue n.2 Broad-band Spectra Hot corona Issue n.1 Credit: A. Muller

  10. A proposal for discussion: Motivations of this proposal are to: - Keep ALL community involved - Keep scientific case up to date, and open to unkown ideas

  11. Effective areas Different designs Effective areas Comparison (in soft band)

  12. Background models Background spectra

  13. Issue 2: Heavy absorption or blurred reflection? Simulations Edges and absorption lines at E~7.1-9.0 keV (rest-frame) + vout~ 0.1-0.5c Eobserved~ 8-14 keV !! High energies are a MUST HAVE to detect and characterise highest velocity outflows!! (N.B: highest velocities = highest mass/kinetic energy)

  14. Issue 3: Characterisation of warm, high-v, and massive outflows Simulations Model: PL + 2 emission lines + 4 abs. lines Model with narrow emission and absorption lines: PL (Г=1.9, F(2-10)=10-11erg/cm2s, Exp.=50 ks) + 2 FeK emission lines (E1=5 keV, E2=6.4 keV, σ1= σ2=50 eV, EW1=EW2=100eV) + 4 FeK absorption lines (E1,2,3,4=7, 9, 12, 15 keV, σ1,2,3,4<50 eV, EW1,2,3,4=-100eV) Edges and absorption lines at E~7.1-9.0 keV (rest-frame) + vout~ 0.1-0.5c Eobserved~ 8-14 keV !! Acceleration Deceleration Eabs<100 eV  Idee would be to follow the evolution of blob ejections (or injections) N.B: Masses involved can be greater than Mearth (1027g/ejecta) >>10-11g in accelerators

  15. Issue 1: FeK lines, continuum reflection and High-E cut-off Model: Simulations Broad band capabilities are a MUST to characterise the reflection component and associated FeK line

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