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The Seyfert galaxies in the Local Universe: from BeppoSAX to Simbol-X

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. +. +. Accretion. SMBH. Obscuration. Broad Band. A eff @ 6 keV. Broad Band. +. Broad Band. The scenario.

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The Seyfert galaxies in the Local Universe: from BeppoSAX to Simbol-X

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

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

  3. The Question: on how many Seyferts we will be able to make a “good” science withSimbol-X?The exercise: simulate theentire lifeof Simbol-Xto “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. General characteristcis of the sample Selection criteria All are sources pointed with NFI instruments • 113 Seyfert pointed by BeppoSAX • 105 detected in the 2-10 keV band • 43 type I • 62 type II • 163 datasets in total (many sources have • been observed more than once) • 84 observations of type I objects • 79 observations of type II objects • 81 out of 105 sources detected above 10 keV • 39 type I • 42 type II 1) Seyferts only 2) Redshift below 0.1 The “BeppoSAX” sample (Dadina 2007) Please, remember, from now on, each observation, treated singularly: i.e. two observations of the same object considered as observations of different objects!

  5. Used to simulate the expected SX results BeppoSAX spectral analysis 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) Cold reflection= PEXRAV (Magdziarz & Zdziarski 1995)

  6. Tot Tot Sey1 Sey1 Sey2 Sey2 R Log(Ec) Mean Properies of the continuum: “R and the 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 (Dadina 2007, submitted)

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

  8. Exp. Time 100 ks 50 ks 10 ks NH Γ R Ec F2-10 keV 0 0.5 150 1 CXB BKG integrated for 106 s (i.e. assumed blank-field bkg) 5 1.85 1 200 0.1 50 1.5 250 0.01 1022 cm-2 keV 10-11 c.g.s. The grid of models has been fit with the BeppoSAX archive and the ranges of R and Ec allowed to SX have been obtained The grid of simulated SX observations/models Each simulated spectra have been fit to obtain the uncertainties on the spectral parameters.

  9. Reflection SX limit BeppoSAX limit 100% detection above 10 keV We can study the reflection in type II objects! Simbol-X results on the reflection (1) 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

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

  11. Ec=200 keV 70 keV Ec=250 keV Ec=200 keV Ec=150 keV Ec=150 keV Energy (keV) Seyfert 1, F=1 Just a reminder… why we can study Ec up to 200 keV…

  12. Mainly lower limits for Type II objects… Simbol-X results (3) on Ec Again more than dubled the number of sources for which we can collect information on the Ec. Simbol-X limit BeppoSAX limit Caveat: for all sources that did not displayed evidences of cut-off in BeppoSAX data the Ec was set to Ec=200 keV

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

  14. RESULTS • 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) • 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 • 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. Simbol-X will permit to test on solid statistical basis the mean physical properties of Seyferts galaxies in the local Universe • Caveats: • Used simplified models (for instance…no W.A., no ionized refl….) • BeppoSAX archive collected in 6 years. • Work in progress…(to be tested the impact of higher internal bkg… • …more complex models…. )

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