1 / 16

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.

libitha
Télécharger la présentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related