The Seyfert galaxies in the Local The Seyfert galaxies in the Local Universe: from Universe: from BeppoSAXBeppoSAX to to

Simbol-XSimbol-X

Mauro DadinaINAF/IASF-BoDip. di Astronomia, UniBo

Bologna, May 15, 2007

The scenarioThe scenario

UMUM

X-ray X-ray EmissionEmission

mechanismsmechanisms

CXRBCXRB

CosmologyCosmologyGR effectsGR effects

AccretionAccretionSMBHSMBH ObscurationObscuration+ +

Broad Band

Broad Band

Aeff@ 6 keV+

Broad Band

Nearby Seyferts are unique laboratories to test:

(adapted by M. Polletta fromUrry & Padovani 1995)

The Question: on how many Seyferts we will be able to make a “good” science with

Simbol-X?

The exercise: simulate the entire lifeentire life of Simbol-X to “quantify” the scientific output of

the mission on this topic

Method: starting from the BeppoSAX archive

the expected results obtained with Simbol-Xhave been simulated

The “BeppoSAX” sample (Dadina 2007)The “BeppoSAX” sample (Dadina 2007)

Selection criteriaSelection criteria

1) Seyferts only

2) Redshift below 0.1

All are sources pointed withNFI instruments

General characteristcisGeneral characteristcisof the sampleof the sample

• 113 Seyfert pointed by BeppoSAX113 Seyfert pointed by BeppoSAX• 105 detected in the 2-10 keV band105 detected in the 2-10 keV band• 43 type I43 type I• 62 type II62 type II• 163 datasets in total (many sources have163 datasets in total (many sources have been observed more than once)been observed more than once)• 84 observations of type I objects84 observations of type I objects• 79 observations of type II objects79 observations of type II objects• 81 out of 105 sources detected above 10 keV81 out of 105 sources detected above 10 keV• 39 type I39 type I• 42 type II42 type II

Please, remember, from now on, each observation, treated singularly:i.e. two observations of the same object considered as observations of different objects!

Automatic procedures

Template models of increasing complexity

Absorbed power-law (NH,Gal + NH, int)

Absorbed powerl-law + Gaussian (Fekα)

Absorbed power-law + cold reflection + Gaussian

Absorbed Power-law + cold refl. + Gauss. + Soft-excess (power-law)

BeppoSAX spectral analysis

Cold reflection= PEXRAV (Magdziarz & Zdziarski 1995)

Used to simulatethe expected SX results

Tot

Sey1

Sey2

R

Tot

Sey1

Sey2

Log(Ec)

Rtot=1.01±0.09

RSey1=1.23±0.11

RSey2=0.87±0.14

Ectot=287±24 (keV)

EcSey1=230±22

EcSey2=376±42

Mean Properies of the continuum:Mean Properies of the continuum:““R and the Ec”R and the Ec”

(Dadina 2007, submitted)

Log(F)=1 ->10-11c.g.s x 100 ksF=Flux(2-10 keV) *sqrt(Texp) (here Texp in ksand Flux in units of 10-11 c.g.s.)DetectionAbove 10 keV

Reflection High-E cut-offBeppoSAX “available space”

How to compare the opportunities offered by the How to compare the opportunities offered by the two missionstwo missions?

2-10 keV flux Exposure time

The grid of simulated SX observations/modelsThe grid of simulated SX observations/models

NH Γ R Ec F2-10 keV

0 0.5 150 1

5 1.85 1 200 0.1

50 1.5 250 0.01

1022 cm-2 keV 10-11 c.g.s.

Exp. Time100 ks50 ks10 ks

CXB BKG integrated for 106 s(i.e. assumed blank-field bkg)

The grid of models has been fit with the BeppoSAX archive and the ranges of R and Ec allowed to SX have been obtained

Each simulated spectra have beenfit to obtain the uncertaintieson the spectral parameters.

Simbol-X results on the reflection (1)

100% detection above 10 keV

More than dubled the number of sources for which the reflected component can be investigated, thanks to the possibility to disentangle the reflection in the absorbed sources

We can study the reflection in type II objects!

Reflection

SX limit

BeppoSAXlimit

Simbol-X results on the reflection (2)

Seyfert 1

F=1

Ec=150 keV

We can investigate the long-term variabilityof R -> we can map the reflector….

But harderfor Seyfert 2….

Just a reminder… why we can study Ec up to 200 keV…

70 keV

Ec=200 keV

Ec=150 keV

Energy (keV)

Ec=250 keV

Ec=150 keV

Ec=200 keV

Seyfert 1, F=1

Simbol-X results (3) on Ec

BeppoSAXlimit

Simbol-X limit

Caveat: for all sourcesthat did not displayed evidencesof cut-off in BeppoSAX datathe Ec was set to Ec=200 keV

Again more than dubled the number of sources for which we can collect information on the Ec.

Mainly lower limits forType II objects…

New perpectives that Simbol-X capabilities may open….

If statistics is good enough..

We can (start to) test the UM using informationon the inclination angle of the reflector

Seyfert 1F=1

Cos(θ)

..again… harder to dofor Seyfert 2…

RESULTS

1. More than doubled the number of Seyferts for which we can simultaneusly obtain information on R and Ec (from 31 in the BeppoSAX archive to 65 in Simbol-X simulated archive)

2. Major improovements, on this topic, for type II objects. They were 12 in the BeppoSAX archive and become 31 in the simulated SX archive (broader band will help for the study of the Ec….)

3. Possible to map the reflector of bright objects via time-dependent studies

4. We can hope to have meaningful limits on inclination angles to test UM (23 objects in the simulated BeppoSAX/SX database) on bright/long observed sources.

Caveats:

1. Used simplified models (for instance…no W.A., no ionized refl….)2. BeppoSAX archive collected in 6 years.3. Work in progress…(to be tested the impact of higher internal bkg… …more complex models…. )

Simbol-X will permit to test on solid statistical basis the mean physical properties of Seyferts galaxies in the local Universe