X-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre

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1 X-ray data analysis Andrea Marinucci Università degli Studi Roma Tre

2 Goal of these lectures X-ray data analysis why? what? how?

3 Why? Active Galactic Nuclei (AGN) Physics in a nutshell Reprocessed emission: circumnuclear material Nuclear radiation: inner engine MBH= Msun

4 Optical spectrum of an AGN

5 Classification The very first classification criterion is the ratio between the emission in the radio and the optical bands: LR/LO ~ 10

6 Classification Radio galaxies are mostly elliptical galaxies with a luminosity in the range LR~ erg/s. The intense radio emission is due to the presence of jets and spatially extended sources are divided into two classes, depending upon their morphology.

7 Classification FRI and FRII Jet Lobe Hot-spots Fanaroff-Riley I (FRI): decreasing luminosity with the distance from the nucleus, LR< 1041 erg/s, z<0.2 Fanaroff-Riley II (FRI): maximum luminosity in the lobes, LR> 1041 erg/s, high z sources

8 Classification The second discrimination factor is the presence or lack of broad emission lines in the optical/uv spectrum

9 Classification: type 1 and 2 AGN FWHMs~ km/s The widths of these lines are due to Keplerian velocities at distances of pc (Broad Line Region) The density of the emitting gas is cm-3, inferred by the observed ratio between permitted and forbidden observed atomic transitions. Only observed in Type 1 AGN!

10 Classification: type 1 and 2 AGN FWHMs~ km/s The widths of these lines are due to Keplerian velocities at distances of pc (Broad Line Region) The density of the emitting gas is cm-3, inferred by the observed ratio between permitted and forbidden observed atomic transitions. Only observed in Type 1 AGN!

11 Classification: type 1 and 2 AGN FWHMs~ km/s Distances > 100 pc (Narrow Line Region) The density of the emitting gas is cm-3 The difference between the two classes is believed to be only due to our line of sight

12 Unification Model Antonucci & Miller, 1985

13 Unification Model

14 Spectral Energy Distribution (SED)

15 Optical/UV emission Big Blue Bump: Thermal emission from a plasma with T=105±1 K Peak around 1216 and the spectrum can be well approximated with two power laws Small bump: Balmer series + FeII lines ( A)

16 Infrared (2-200 m) The IR bump is present in every AGN and it can be ascribed to thermal emission (~2000 K) from dust in the central regions (at higher temperatures dust grains would sublimate). At higher wavelenghts the efficiency of this process decreases (submillimeter break). Dust sublimation radius: minimum distance from the nucleus at which dust grains with a determined chemical composition may exist Nenkova, 2008

17 X-rays Accretion Physics Accretion accumulation of matter onto some object under the influence of gravity When matter reaches the surface of the compact object kynetic energy is transformed into heat, with a consequent irradiation. Schwarzchild's radius 0.1 for a Neutron Star 0.06 for a non-rotating BH 0.42 for a maximally spinning BH Shapiro & Teukolsky (1983)

18 X-rays Accretion Physics The viscosity redistributes the angular momentum so that some of the matter spreads outwards taking angular momentum with it and thus allows the rest of the matter to spiral inwards. At the same time, the viscosity acts as a frictional force which results in the dissipation of heat. The matter in the accretion disc drifts gradually inwards until it reaches the last stable orbit, at which point it spirals irretrievably into the BH. Shakura & Sunyaev (1973) Pringle (1981) There is, however, a limit because, if the luminosity were too great, radiation pressure would blow away the infalling matter.

19 X-rays Accretion Physics The Eddington luminosity, is found by balancing the inward force of gravity against the outward pressure of the radiation. Outward force on the electron = Flux density of photons for a given luminosity L Inward gravitational force It is the maximum luminosity a spherically symmetric source of mass M can emit in a steady state.

20 X-rays Accretion Physics The predicted spectrum of a geometrically thin (H<<R), optically thick (the emission can be approximated as blackbody radiation at each radius ) accretion disk is a multi-temperature black-body: A typical value for an AGN would be T 105 K, while it is higher ( 107 K) for low mass Galactic Black Holes. These temperatures correspond to UV and soft X-ray bands, respectively, which accounts for the observed emission of the two classes of objects. Pringle (1981)

21 X-rays ( kev) Accretion disc + Corona Therefore in unobscured sources, we can directly study the nuclear radiation Two-phase model Kte, Haardt & Maraschi (1994) kt = 50 kev kt = 100 kev kt = 150 kev The primal emission of an AGN in the X-ray band can be well aproximated with a power-law with = and a highenergy cutoff between kev

22 X-rays Accretion disc + Corona George&Fabian (1991) Matt et al. (1991) Reynolds et al. (1991) The interaction between the accretion disc and the corona is a fundamental ingredient for the total emission of a Type 1 AGN. The spectral shape of the reprocessed emission strongly depends from the ionisation structure of the disc.

23 X-rays Accretion disc + Corona

24 X-rays Circumnuclear material Unobscured AGN NH< 1022 cm-2 Obscured AGN NH> 1022 cm-2 Remember: every experiment has its own laboratory!

25 X-rays Circumnuclear material Compton -Thin NH< 1024 cm-2 Obscured AGN Compton -Thick NH> 1024 cm-2 Matt et al. (2003)

26 X-rays Circumnuclear material Compton -Thin NH< 1024 cm-2 Obscured AGN Compton -Thick NH> 1024 cm-2 For Compton-thin sources EW(Fe Ka)~100 ev, for Compton-thick sources EW(Fe Ka)~1000 ev. The EW of the iron line against the reflection continuum only (upper data) and the total continuum (lower data) as a function of the column density of a face-on torus (Matt et al. 2003).

27 X-rays Circumnuclear material

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