Active Galactic Nuclei and X-ray Astronomy | Lecture Part II

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AGN Core Concepts
Spectral Components
X-ray Continuum & Disk
Corona & Power Law
X-ray Absorbers
Reflection & Iron Line
Probing Black Holes
Reverberation Mapping

AGN Core Concepts

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    Supermassive black holes, ranging from 10^5 to 10^10 solar masses, power AGN through accretion.

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    Accretion efficiency is roughly 10%, converting mass into immense luminosity.

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    The unifying model explains AGN types by viewing angle and obscuration, not intrinsic differences.

The unified model of Active Galactic Nuclei (AGN), including the roles of the supermassive black hole, accretion disk, and dusty torus.
Fundamentals of radiative transfer and high-energy astrophysics, particularly X-ray emission mechanisms like synchrotron radiation, thermal bremsstrahlung, and inverse Compton scattering.
Basic concepts of General and Special Relativity, specifically gravitational redshift, light bending, and relativistic beaming near strong gravitational fields.
Introductory astronomical spectroscopy, including how spectral lines are formed, Doppler-shifted, and broadened by thermal and kinematic motion.
Advanced analysis of relativistic reflection features, such as the Fe K-alpha line profile, to determine supermassive black hole spin.
AGN feedback mechanisms and their evolutionary impact on host galaxies, including the M-sigma relation and the quenching of star formation.
Multi-messenger astrophysics of AGN, exploring their connection to high-energy cosmic rays and neutrino emissions.
Hands-on data reduction and spectral modeling using tools like XSPEC with data from modern X-ray space telescopes like Chandra, XMM-Newton, and NuSTAR.
770 views15likes56:05@IUCAALiveOriginal Release: 2020-06-03

Active galactic nuclei (AGN) produce characteristic X-ray spectra through complex interactions between the accretion disk, hot corona, and surrounding material, where the power-law continuum from inverse Compton scattering in the hot corona (~100 keV) illuminates the cooler accretion disk, producing fluorescent emission lines (particularly the iron K-alpha line at 6.4 keV) that are significantly broadened by relativistic effects near the black hole, allowing astronomers to probe the extreme gravitational environment and measure black hole spin.