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The structure of AGNs from X-ray eclipses . Guido Risaliti (CfA & INAF-Arcetri). M. Salvati, E. Nardini (INAF-Arcetri) , R. Maiolino (INAF-Roma) , G. Matt, S. Bianchi (Roma3) , V. Braito (Leicester) , M. Elvis, G. Fabbiano, (CfA). Ubiquitous Variability of N H in Seyfert Galaxies.

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The structure of AGNs from X-ray eclipses


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slide1

The structure of AGNs from X-ray eclipses

Guido Risaliti

(CfA & INAF-Arcetri)

M. Salvati, E. Nardini (INAF-Arcetri), R. Maiolino (INAF-Roma), G. Matt, S. Bianchi (Roma3), V. Braito (Leicester), M. Elvis, G. Fabbiano, (CfA)

slide2

Ubiquitous Variability of NH in Seyfert Galaxies

NH variable in 23/25

sources

Timescales from

months to years

Clumpy absorber

Sub-parsec distance

Risaliti, Elvis & Nicastro 2002

Leicester - Jan 04, 2009

slide3

Ubiquitous Variability of NH in Seyfert Galaxies

Common also on short time scales!

(~10 sources with confirmed occultations in hours-days)

  • Method:
  • * Detection of candidate occultations
  • * Confirmation through spectral analysis
  • Applications:
  • * Physical parameters of the X-ray source and the X-ray absorber
  • * Hints on the geometrical structure of the absorbing clouds
  • * Shape of the absorbing clouds
  • * POSSIBLE EXPERIMENT OF DISK TOMOGRAPHY
slide5

 No absorption,

“standard” model

 NH~1023cm-2,

C.F. ~ 80%

No continuum spectral variation

slide6

Ubiquitous Variability of NH in Seyfert Galaxies

Eclipses on short time scales are common !

(~10 sources with confirmed occultations in hours-days)

(Risaliti et al. 2010)

slide7

Finding more sources with eclipses in ~hours-days

NGC 4388

NGC 4151

DNH~2*1023 cm-2

DT~15 hours

DNH~3*1023 cm-2

DT<15 days

DNH~1023 cm-2

DT~2 days

UGC 4203

NGC 7582

DNH~1023 cm-2

DT~20 hours

(Bianchi et al. 2009)

slide8

General results:

Eclipses of the X-ray source are COMMON in nearby AGN

DNH ~ 1023-1024cm-2

V > 103 km/s

D ~ 1013 cm

n ~ 1010-1011 cm-2

X-ray absorber = BLR clouds

X-ray source size ~ a few RG

slide9

Structure of the absorber

HR

NGC 1365 Suzaku

NH

CF

Maiolino et al. 2010

slide10

Tomography of the X-ray source

A Relativistic Iron Line in NGC 1365

(Risaliti et al. 2009)

  • It is really a relativistic line
  • Long look (>300 ks)
  • Source in Compton-thin state
  • Complete 10-hours C-thick eclipse during obs.

Assumptions:

slide14

CONCLUSIONS

  • Variability on short time scales is common in local AGNs
  •  X-ray absorber == BLR clouds
  •  Size of the X-ray source ~ a few RG
  • Detailed analysis of the highest S/N X-ray eclipses:
  •  “Cometary” shape of clouds
  • Possible tests of GR effects & disk tomography