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Interpreting Emission - and for specifics of AGN...

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Interpreting Emission-Line Spectra Because various emission lines sample different regimes of temperature, density, and ionization, emission spectra are uniquely powerful probes of conditions around active nuclei. Remember, though, that they do sample conditions around the central engine, which we can study only as it affects the surrounding gas. Important references on emission-line processes are Osterbrock, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei (University Science Books); Spitzer, Physical Processes in the Interstellar Medium (Wiley-Interscience); Aller, Physics of Thermal Gaseous Nebulae
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Unformatted text preview: , and for specifics of AGN applications, Davidson and Netzer 1979 (Rev. Mod. Phys. 51, 715) and Peterson's AGN textbook . Review of the recombination theory in the star-formation lecture will be helpful. Every state of an atom or ion has quantum numbers of importance here as follows: Each ( l,s ) pair has multiplicity g = 2s+1- the number of energy levels with distinct j . For historical reasons, different values of l=0,1,2,3 are denoted in spectroscopic notation by S,P,D,F (strong, principal, diffuse, faint), then G,H,. .. A spectroscopic term (atomic state) is denoted by n g L J ....
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