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Delphine Porquet MPE, Garching, Germany

AGN: Testing general relativity (Fe K α line) and high resolution plasma diagnostics (Warm Absorber). Delphine Porquet MPE, Garching, Germany. I. Testing general relativity (GR) in AGN.

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Delphine Porquet MPE, Garching, Germany

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  1. AGN: Testing general relativity (Fe Kα line) and high resolution plasma diagnostics (Warm Absorber) Delphine Porquet MPE, Garching, Germany

  2. I. Testing general relativity (GR) in AGN The Fe Kα line near 6.4-7 keV is a powerful tool to test GR in AGN and the physical conditions very close to the supermassive BH. • ASCA: Discovery of a very broad and intense line in the Seyfert 1 MCG-6-30-15 (Tanaka et al. 1995; Fabian et al. 1995, ….) • due to Doppler and gravitational redshifts from the inner parts of a disc around a supermassive black hole

  3. PG 1402+261 (z=0.164) Q0056-363 (z=0.162) XMM-Newton and Chandra have unveiled other various Fe K line shapes : • strongly blue-shifted features: emission Fe K line or partial covering. Outflow ? (e.g., Pounds et al. 02, Reeves et al. 04) • Narrow Gaussian lines (e.g., BLR, torus) • narrow red-shifted emission lines near 5.4 - 5.9 keV

  4. ESO 113-G010 (z=0.026) Red-shifted narrow emission Fe Kα line “Weak” (a few hundred eV) emission lines found near 5.4 - 5.9 keV in the AGN rest-frame Recently discovered thanks to XMM and Chandra in several AGN: NGC 3516 (Turner et al. 02); ESO 198-G24 (Guainazzi 03); NGC 7314 (Yaqoob 03), Mrk 766 (Turner et al. 04); IC 4329A (McKernan & Yaqoob 04); ESO 113-G010 (Porquet et al. 04) E= 5.38 +/- 0.11 keV EW= 265 +/- 146 eV Detected at 99% confidence level (Monte Carlo simulations) ESO 113-G010 (Porquet et al. 04)

  5. Red-shifted narrow emission Fe Kα line Possible interpretations: 1. Relativistic (~0.2c) ejected matter moving away from the observer 2. Localized hotspot on the disk following its illumination by flare (Nayakshin & Kazanas 01; Turner et al. 02, Dovciak et al 04) The energy, intensity and shape of the line is sensitive to the location of the hotspot on the disk (R, Ф), to the disk inclination (θ) and the spin of the BH. Map the line over an entire orbit of the hotspot will allow to determine: • Outflowing and/or inflowing velocity and location of the ejected matter (Scenario 1) • Disk inclination (θ) and the location of the hotspot (R, Ф) (scenario 2) • The mass of the BH (the orbital time scale is proportional to MBH: Torb≡310 (R3/2+a) MBH/107 [s]) • BH spinning or not.

  6. Hotspots:R=12 Rg Disc inclination: 17 deg Disc inclination: 60 deg Dovciak et al. 04

  7. E=5.4keV E=7.0keV XEUSSeyfert z=0.026L (2-10 keV)= 3e42 erg/s (QSO rest-frame) Simulations: Γ=2.0, E=5.4 or 7.0 keV, EW= 150eV Exposure = 1000 s Γ= 1.98 +/-0.03 E= 5.40 +/-0.01 keV EW= 156 +/-18 eV χ2/d.o.f.= 553/525, Χred=1.05 Γ= 2.00 +/-0.03 E= 7.00 +/-0.03 keV EW= 182 +/-32 eV χ2/d.o.f.=519/523, Χred=0.995

  8. XEUSQSO z=2.6 L(2-10 keV)= 3e42 erg/s or 3e44 erg/s (in QSO rest-frame) Simulations: Γ=2.0, E=5.4 keV, EW= 150eV Exposure = 1000 s L(2-10 keV)= 3e44 erg/s L(2-10 keV)= 3e42 erg/s Γ= 2.06 +/-0.10 E= 5.40 +/-0.01 keV EW= 180 (+49, -82) eV χ2/d.o.f.=54.5/53, Χred=1.03 Γ= 2.00 +/-0.01 E= 5.40 +/-0.03 keV EW= 155 +/-5 eV χ2/d.o.f.=395/383, Χred=1.03

  9. XEUS • Spectral resolution to follow a fast moving line (small BH mass) and low luminosity and/or high-z AGN • Sensitivity up to 10keV (detection of blue-shifted lines) • Excellent continuum estimation even for low luminosity and/or high-z AGN

  10. High resolution plasma diagnostics (Warm Absorber) Energy budget: inflow/outflow

  11. XEUS: Resolving Power

  12. Density Temperature Density and temperature ranges of the He-like ions (triplet) • With XEUS access: • To higher-Z He-like ions, such Fe: higher density and temperature ranges. • - To lower luminosity and/or high-z AGN: evolution of the BH environment material

  13. Ne IX OVII TW Hya: Classical T-Tauri (Kastner et al. 2002, Chandra/HETG) Ne IX triplet: ne ~ 1013 cm-3. O VII triplet: ne ≥ 1012 cm-3. High density plasma ; shock in accretion column ? Only accessible to few objects XEUS: T-Tauri -> proto-stars

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