Reverberation mapping

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X-ray Line ProductionConsider X-rays illuminatingoptically-thick, cold acc n diskPhotoelectric absorption(energy dependent)photons are re-emitted viafluorescenceEmission lines & absorptionedges resultFe Kα most prominent due tocombination of abundance &fluorescence-yieldGeorge & Fabian ‘91
X-ray Line ProductionGeorge & Fabian ‘91, Reynolds 1996Ross & Fabian 2006Compton Scattering - hard photonsscatter with Compton recoilreducing scattered flux above 15keVLine energy (6.4-6.97keV) depends onionization
Page 1 and 2: Reverberation mappingOptical lines
Page 3 and 4: Reverberation mappingv =GM rGetting
Page 7 and 8: Light Crossing Time•Variations sm
Page 11 and 12: X-ray Observations of AGNWhat we ca
Page 13 and 14: Recap: The Power behind AGNSimple a
Page 15: Copious production of X-RaysUV phot
Page 19 and 20: Chandra/XMMSuzakuAbsorptionfrom out
Page 21 and 22: Profile distorted SR & GR- probe of
Page 23 and 24: GR Effects on Spectral featuresProf
Page 25 and 26: MCG-6-30-15: Poster ChildTanaka et
Page 27 and 28: Absorption or Reflection as the ori
Page 29 and 30: Light bending?Suzaku lightcurveMini
Page 31 and 32: Ambiguity: - X-ray AbsorptionNGC 35
Page 33 and 34: How much evidence is there forabsor
Page 35 and 36: More Evidence for ionized outflows:
Page 37 and 38: Seyfert Spectral Variability Behavi
Page 39 and 40: Partial Covering/Occultation, resur
Page 41: Summary• Large amounts of gas are

Reverberation mapping

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