1. The Seyfert galaxies in the Local Universe: from BeppoSAX to Simbol-X Mauro Dadina INAF/IASF-Bo Dip. di Astronomia, UniBo Bologna, May 15, 2007

2. The scenario UM X-ray Emission mechanisms CXRB Cosmology GR effects Accretion SMBH Obscuration + + Broad Band A eff @ 6 keV + Broad Band Nearby Seyferts are unique laboratories to test: (adapted by M. Polletta from Urry & Padovani 1995)

3. entire life The Question: on how many Seyferts we will be able to make a “good” science with Simbol-X? The exercise: simulate the entire 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-X have been simulated

4. The “BeppoSAX” sample (Dadina 2007) Selection criteria 1) Seyferts only 2) Redshift below 0.1 All are sources pointed with NFI instruments General characteristcis of 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!

5. Automatic procedures Template models of increasing complexity Absorbed power-law (N H,Gal + N H, 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 simulate the expected SX results

6. Tot Sey1 Sey2 R Tot Sey1 Sey2 Log(Ec) R tot =1.01±0.09 R Sey1 =1.23±0.11 R Sey2 =0.87±0.14 Ec tot =287±24 (keV) Ec Sey1 =230±22 Ec Sey2 =376±42 Mean Properies of the continuum: “R and the Ec” (Dadina 2007, submitted)

7. Log(F)=1 ->10 -11 c.g.s x 100 ks F=Flux(2-10 keV) *sqrt(T exp ) (here T exp in ks and Flux in units of 10 -11 c.g.s.) Detection Above 10 keV ReflectionHigh-E cut-off BeppoSAX “available space” How to compare the opportunities offered by the two missions two missions? 2-10 keV fluxExposure time

8. The grid of simulated SX observations/models N H Γ R Ec F2-10 keV 0 0.5 150 1 5 1.85 1 200 0.1 50 1.5 250 0.01 10 22 cm -2 keV 10 -11 c.g.s. Exp. Time 100 ks 50 ks 10 ks CXB BKG integrated for 10 6 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 been fit to obtain the uncertainties on the spectral parameters.

9. 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 BeppoSAX limit

10. Simbol-X results on the reflection (2) Seyfert 1 F=1 Ec=150 keV We can investigate the long-term variability of R -> we can map the reflector…. But harder for Seyfert 2….

11. 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

12. Simbol-X results (3) on Ec BeppoSAX limit Simbol-X limit Caveat: for all sources that did not displayed evidences of cut-off in BeppoSAX data the 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 for Type II objects…

13. New perpectives that Simbol-X capabilities may open…. If statistics is good enough.. We can (start to) test the UM using information on the inclination angle of the reflector Seyfert 1 F=1 Cos(θ)..again… harder to do for Seyfert 2…

14. 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