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Probing the Geometry and Physics of the Emission Region of Active Galactic Nuclei Using Hard X-Ray Observations. Natasha Woods Mentors: Marco Ajello & Masaaki Hayashida. Outline. AGN & Unified Model Testing the Unified Model Results Conclusions. Introduction. AGN

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slide1

Probing the Geometry and Physics of the Emission Region of Active Galactic Nuclei Using Hard X-Ray Observations

Natasha Woods

Mentors: Marco Ajello & Masaaki Hayashida

slide2

Outline

  • AGN & Unified Model
  • Testing the Unified Model
  • Results
  • Conclusions
slide3

Introduction

  • AGN
    • Majority of energy output unrelated to stellar processes
    • Compact regions, galaxy center, exceedingly luminous
  • Classification
    • Radio luminosity
    • Spectral properties
slide4

Unified Model for AGN

  • All AGN are intrinsically the same
  • Perceived differences due to viewing orientation
  • SMBH, accretion disk, molecular torus, corona
evidence for against the unified model
Evidence For & Against the Unified Model
  • Polarized broad emission lines in Sy2
  • Sy1 <---> Sy2
  • Electron temperature
  • Fraction of absorbed sources
slide7

X-ray Spectra

  • X-Rays
  • IC Radiation
  • Direct, Transmitted, Reflected
reflection component
Reflection Component
  • IC reflection peak ~30keV, softening spectra (whiteboard)
  • Sy1 should have a larger reflection component and photon index than Sy2
high energy cut off
High Energy Cut-off
  • Corona's electrons expected to be thermal
  • Cut-offs for Sy1 and Sy2 should be compatible, corona's properties are independent of orientation
relevance
Relevance
  • ~100% CXB
  • Constrain cosmological models and black hole physics
sample population
Sample Population
  • ~200 sources
  • Swift-BAT hard X-ray Survey
  • 5 sigma significance level
  • 3 years exposure
  • Unbiased, blind search
slide12

Models for Spectra

  • Simple power law model (SPL) fit to individual spectra in Xspec11
gaussian and weighted averages
Gaussian and Weighted Averages
  • Gaussian poorly fit some data
  • Weighted Averages
    • based on errors
    • no model
stacked spectra
Stacked Spectra
  • S/N, mean properties
  • SPL and PEXRAV fit to spectra
results spl pexrav stacked spectra
Results: SPL & PEXRAV Stacked Spectra
  • PEXRAV>SPL
  • Photon Indices
  • Reflection
  • Energy Cut-off
conclusion
Conclusion
  • Photon Index Sy1 > Sy2
  • PEXRAV > SPL
  • Reflection compatible, large errors
  • Energy Cut-offs different
  • Future