AGN: AGN: Testing general relativity (Fe KTesting general relativity (Fe Kαα line) and high line) and high

resolution plasma diagnostics (Warm Absorber)resolution plasma diagnostics (Warm Absorber)

Delphine PorquetDelphine Porquet

MPE, Garching, GermanyMPE, Garching, Germany

I. Testing general relativity (GR) in AGNI. Testing general relativity (GR) in AGN

The Fe KThe Fe Kαα line near 6.4-7 keV is a line near 6.4-7 keV is a powerful tool to test GR in AGN and the powerful tool to test GR in AGN and the physical conditions very close to the physical conditions very close to the supermassive BH. supermassive BH.

ASCA: ASCA: Discovery of a very broad and intense Discovery of a very broad and intense

line in the Seyfert 1 MCG-6-30-15 line in the Seyfert 1 MCG-6-30-15 (Tanaka et al. 1995; Fabian et al. 1995, ….)(Tanaka et al. 1995; Fabian et al. 1995, ….)

due to Doppler and gravitational due to Doppler and gravitational redshifts from the inner parts of a disc redshifts from the inner parts of a disc around a supermassive black hole around a supermassive black hole

strongly blue-shifted features: 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 linesNarrow Gaussian lines

(e.g., BLR, torus)(e.g., BLR, torus)

narrow red-shifted emission lines narrow red-shifted emission lines near 5.4 - 5.9 keVnear 5.4 - 5.9 keV

PG 1402+261 (z=0.164)

Q0056-363 (z=0.162)

XMM-Newton and Chandra have unveiledXMM-Newton and Chandra have unveiled other various Fe K line shapesother various Fe K line shapes : :

Red-shifted narrow emission Fe KRed-shifted narrow emission Fe Kαα line line ““Weak” (a few hundred eV) emission lines found near Weak” (a few hundred eV) emission lines found near 5.4 - 5.9 keV5.4 - 5.9 keV in the in the

AGN rest-frameAGN rest-frame

Recently discovered thanks to XMM and Chandra in several AGN: Recently discovered thanks to XMM and Chandra in several AGN: NGC 3516NGC 3516 (Turner et al. 02); (Turner et al. 02); ESO 198-G24ESO 198-G24 (Guainazzi 03); (Guainazzi 03); NGC 7314 NGC 7314

(Yaqoob 03), (Yaqoob 03), Mrk 766Mrk 766 (Turner et al. 04); (Turner et al. 04); IC 4329AIC 4329A (McKernan & Yaqoob 04); (McKernan & Yaqoob 04); ESO 113-G010ESO 113-G010 (Porquet et al. 04) (Porquet et al. 04)

ESO 113-G010 (z=0.026)

E= 5.38 +/- 0.11 keV EW= 265 +/- 146 eV

Detected at 99% confidence level (Monte Carlo simulations)

ESO 113-G010ESO 113-G010 (Porquet et al. 04) (Porquet et al. 04)

Red-shifted narrow emission Fe KRed-shifted narrow emission Fe Kαα line line

Possible interpretations:Possible interpretations: 1. 1. Relativistic (~0.2c) ejected matter moving away from the observer Relativistic (~0.2c) ejected matter moving away from the observer 2. Localized hotspot on the disk following its illumination by flare2. 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 The energy, intensity and shape of the line is sensitive to the location of the

hotspot on the disk (R, hotspot on the disk (R, ФФ), to the disk inclination (), to the disk inclination (θθ) and the spin of the BH. ) and the spin of the BH.

Map the line over an entire orbit of the hotspot will allow to determine: 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 Outflowing and/or inflowing velocity and location of the ejected matter

(Scenario 1)(Scenario 1)

- Disk inclination Disk inclination ((θθ) and the location of the hotspot (R, ) and the location of the hotspot (R, ФФ) (scenario 2)) (scenario 2)- The mass of the BH The mass of the BH (the orbital time scale is proportional to M(the orbital time scale is proportional to MBHBH: Torb≡310 (R3/2+a) MBH/107 [s])- BH spinning or not.

Hotspots:Hotspots:

R=12 RR=12 Rgg

Dovciak et al. 04

Disc inclination: 17 deg Disc inclination: 60 deg

XEUSXEUSSeyfert z=0.026Seyfert z=0.026

L (2-10 keV)= 3e42 erg/s (QSO rest-frame)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= 1.98 +/-0.03 E= 5.40 +/-0.01 keVEW= 156 +/-18 eVχ2/d.o.f.= 553/525, Χred=1.05

Γ= 2.00 +/-0.03 E= 7.00 +/-0.03 keVEW= 182 +/-32 eVχ2/d.o.f.=519/523, Χred=0.995

E=5.4keV E=7.0keV

XEUSXEUSQSO z=2.6 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= 2.06 +/-0.10 E= 5.40 +/-0.01 keVEW= 180 (+49, -82) eVχ2/d.o.f.=54.5/53, Χred=1.03

Γ= 2.00 +/-0.01 E= 5.40 +/-0.03 keVEW= 155 +/-5 eVχ2/d.o.f.=395/383, Χred=1.03

L(2-10 keV)= 3e42 erg/s L(2-10 keV)= 3e44 erg/s

XEUSXEUS

Spectral resolution to follow a fast moving line (small BH mass) 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)Sensitivity up to 10keV (detection of blue-shifted lines)

Excellent continuum estimation even for low luminosity Excellent continuum estimation even for low luminosity

and/or high-z AGNand/or high-z AGN

II.II. High resolution plasma diagnosticsHigh resolution plasma diagnostics

(Warm Absorber) (Warm Absorber)

Energy budget: inflow/outflow

XEUS: Resolving PowerXEUS: Resolving Power

Density and temperature rangesDensity and temperature ranges of the He-like ions (triplet) 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-TauriTW Hya: Classical T-Tauri ( (Kastner et al. 2002, Chandra/HETGKastner et al. 2002, Chandra/HETG))

Ne IX

OVII

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