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

I. Testing general relativity (GR) in AGN The Fe Kα line near keV is a powerful tool to test GR in AGN and the physical conditions very close to the supermassive BH. The Fe Kα line near 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 (Tanaka et al. 1995; Fabian et al. 1995, ….) Discovery of a very broad and intense line in the Seyfert 1 MCG (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

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

Red-shifted narrow emission Fe Kα line “Weak” (a few hundred eV) emission lines found near keV in the AGN rest-frame “Weak” (a few hundred eV) emission lines found near 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) 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) ESO 113-G010 (z=0.026) E= / keV EW= 265 +/- 146 eV Detected at 99% confidence level (Monte Carlo simulations) ESO 113-G010 (Porquet et al. 04)

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) (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. 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 M BH (the orbital time scale is proportional to M BH : Torb≡310 (R 3/2 +a) M BH /10 7 [s]) - - BH spinning or not.

Hotspots: R=12 R g Hotspots: R=12 R g Dovciak et al. 04 Disc inclination: 17 degDisc inclination: 60 deg

XEUS Seyfert z=0.026 L (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= /-0.03 E= /-0.01 keV EW= 156 +/-18 eV χ 2 /d.o.f.= 553/525, Χ red =1.05 Γ= /-0.03 E= /-0.03 keV EW= 182 +/-32 eV χ 2 /d.o.f.=519/523, Χ red =0.995 E=5.4keVE=7.0keV

XEUS QSO z=2.6 XEUS QSO 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 Γ= /-0.10 E= /-0.01 keV EW= 180 (+49, -82) eV χ 2 /d.o.f.=54.5/53, Χ red =1.03 Γ= /-0.01 E= /-0.03 keV EW= 155 +/-5 eV χ 2 /d.o.f.=395/383, Χ red =1.03 L(2-10 keV)= 3e42 erg/s L(2-10 keV)= 3e44 erg/s

XEUS  Spectral resolution to follow a fast moving line (small BH mass) and low luminosity and/or high-z AGN 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 and/or high-z AGN

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

XEUS: Resolving Power

Density and temperature ranges of the He-like ions (triplet) Density Temperature 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

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