Black Holes: Black Holes: from stellar mass from stellar mass

to AGNto AGN

GiorgioGiorgio MattMatt (D(Dipartimento di Fisica, ipartimento di Fisica, Università Roma Tre, ItalyUniversità Roma Tre, Italy))

Plan of the talkPlan of the talk

Galactic Black Hole Binaries (10 MΘ )

ULX – Intermediate mass BH? (100-1000 MΘ )

Active Galactic Nuclei (radio-quiet, unobscured) (106-109 MΘ ) (With contributions from Stefano Bianchi and Gabriele Ponti)

Black holes, from S to XXLBlack holes, from S to XXL

log Tb = 2.1 log MBH - 0.98 log Lbol - 2.32(McHardy et al. 2006)

Is physics the same, whatever the mass? It is

accretion, after all....GR effects are scale

invariant Tdisc MBH

-1/4

Environment is different

Fundamental plane for BH

(Merloni et al. 2003, Falcke et al. 2004)

Black holes, from S to XXLBlack holes, from S to XXL

log Tb = 2.1 log MBH - 0.98 log Lbol - 2.32

(McHardy et al. 2006)

(Chiaberge 2007)

A distance artifact? (Bregman 2005 )

Black holes, from S to XXLBlack holes, from S to XXL

log Tb = 2.1 log MBH - 0.98 log Lbol - 2.32

(McHardy et al. 2006)

(Chiaberge 2007)

A distance artifact? Likely not (Merloni et al.

2006 )

Fundamental plane for BH

(Merloni et al. 2003, Falcke et al. 2004)

Why Simbol-X?Why Simbol-X?BH accreting systems emit over a broad band, with significant emission above 10 keV (at least in GBHB and in AGN. We want to know if this holds true also

for ULX! ). Hard X-ray emission is likely due to Comptonization with kT of several tens of keV or

more (see P.O. Petrucci’s talk)

The spectrum is usually rather complex, and

broad band coverage is required to

disentangle the different

components. Simplified (!!) version of the typical radio-quiet

AGN spectrum

General topicsGeneral topics

Primary emission: thermal/non thermal; kT; anisotropy effects; variability (so far only in a

handful of AGN, and in BHB in active states) (more in P.O. Petrucci’s talk)

Compton Reflection component: (AGN: relativistic vs. torus; GBHB: relation with states; ULX: is it there?); neutral vs. ionized; comparison with iron line EW (iron abundance; optical depth); reflection vs. absorption (e.g. the ~7 keV spectral

drop in NLSy1) (more from M. Dadina and G. Miniutti)

Relativistic effects: good knowledge of the underlying continuum (see J. Wilms’s talk, R.

Goosmann andM. Dovciak’s posters)

Galactic BH systemsGalactic BH systems

Gierlinski et al. 1999

BHB can be found in different states: low, intermediate,

high and very high, with many sources switching from one

state to the other.

The main driving parameters is believed to be the accretion

rate. Esin 1997

Galactic BH systems in Galactic BH systems in quiescence quiescence

Many sources, however, spend most of the time in

a quiescent state, with luminosities several orders of magnitude

lower than in the active states.

Not much is known about the quiescent state. Radiatively inefficient

flow?

The brightest BHB in quiescence have fluxes of (0.1-1)x10-12 cgs (e.g Kong et al. 2002): too faint for BeppoSAX and Suzaku,

butbright enough for Simbol-

X

Narayan et al. 1998

X-ray states are connected with radio emission and jets (see J.

Malzac’s talk)

Is hard X-ray emission in hard states also related to jets?

Does the reflection

component agrees with this

picture?Fender et al. 2004

GX339-4 in low/hard state(Miller et al. 2006)

Ultraluminous X-ray Ultraluminous X-ray sourcessources

The very nature of Ultraluminous X-ray sources (ULX; Lx>1039

erg/s) is still unclear. Intermediate Mass Black Holes or beamed

emission? Possibly a mixed bag, but in at least a few cases the IMBH

hypothesis is likely or at least tenable (e.g. Miller et al. 2004, Miniutti et al. 2006).

There are two spectral types of ULX: Power law (PL) and Convex spectrum (CS) (e.g Makishima 2007). Often both

components are present. Sources may switch to

one type to the other (like in

GBHB?).

IC 342 X-1 and X-2 (Kubota et al.

2001)

ULX: the role of Simbol-XULX: the role of Simbol-X• Is the high energy cutoff in the PL states lower than in

BHB, as seems to be the case in some objects?

• Is there always a PL component in the CS state? (and a CS component in the PL state?)

What is the dominant component?

• Is there a relation between ULX and GBHB states?

• More generally, how the ULX broad-band spectra compare with those of BHB and AGN?

• Is there a reflection component? (no iron line found yet!)

• Hard X-ray observations are needed ! (not available yet

because of confusion and lack of sensitivity)

AGN: the reflection componentAGN: the reflection component

The hard X-ray sensitivity of Simbol-X is ideal to search for reflection components in a large sample of sources, down to relatively faint ones, to map the circumnuclear

matter.

The reflection component gives

additional information to those provided by the iron line. In fact, the ratio of the line

EW and the reflection component depends

on the iron abundance and on the optical

depth of the reflecting matter.

>1024

1023

1022

(Matt, Guainazzi& Maiolino

2003)

An example: the IT effect An example: the IT effect (see S. (see S. Bianchi’s poster)Bianchi’s poster)

log(EWFe)=(1.73±0.03) + (-0.17±0.03) log(LX,44)

Bianchi et al. 2007

The Iwasawa-Taniguchi (a.k.a. X-ray Baldwin) effect is the anticorrelation between the EW of the iron line

(narrow core) and the X-ray luminosity (first discovered by Iwasawa & Taniguchi 1993)

An example: the IT effect An example: the IT effect (see S. (see S. Bianchi’s poster)Bianchi’s poster)

The IT effect may be due to a decrease with L of the covering factor

of the reflecting matter (a similar effect has been found by

Maiolino et al. 2007 using infrared data). log(EWFe)=(1.73±0.03) + (-0.17±0.03) log(LX,44)

Bianchi et al. 2007

Simbol-X can do the same for the

reflection component

(100 sources x 50 ks exposure= 5 Ms).

We’ll learn about the optical depth of the matter (BLR?

Torus?) and the iron abundance, and on their dependence

on the luminosity (Eddington ratio? BH mass?)

AGN: the origin of the soft AGN: the origin of the soft excessexcess

(see G. Ponti’s poster)(see G. Ponti’s poster)Somewhat paradoxically, thanks to its hard X-ray coverage Simbol-X can help solving the long standing problem of the

soft X-ray excess.

The soft X-ray excess was first discovered in the EXOSAT spectrum of

Mkn 841 (Arnaud et al. 1985). Mkn 841

(Petrucci et al. 2007)

The thermal disc interpretation

of the soft X-ray excess has two

problems: the derived temperatures are too high

and always the same (T M-1/4).

Is the soft excess related to atomic physics?

Two models: relativistically smeared absorption (Gierlinski & Done 2004) and ionized

disc reflection (Crummy et al. 2006)

Simbol-X can easily distinguish between the two models.

XMM-Newton data are usually well fitted by both models even in

bright sources because of the limited band. Even BeppoSAX and Suzaku are unable to

solve the issue.

SummarySummary

Simbol-X can explore for the first time the hard X-ray emission of GBHB in quiescence and of Ultraluminous X-ray Sources (IMBH

candidates)

In AGN, Simbol-X can significantly expand the number of sources with precise

measurement of the reflection component, searching for correlations with e.g. the

luminosity.

It can also help solving the more than 20 years old problem of the soft X-ray excess.