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     Questions     Refs.   

(1) Galaxy ISMs: An Overview
(2) ISM Components & Observational Signatures
      (a) Introduction
      (b) Observational Signatures: General Considerations
      (c) Warm Ionized Gas
            (i)   Hydrogen Recombination Radiation
            (ii)  Collisionally Excited Fine Structure Lines
      (d) Hot Ionized Gas
      (e) Warm & Cold Atomic Gas
      (f) Molecular Gas
      (g) Dust
      (h) Relativistic Component
(3) Theories of the Multi-Phase ISM
(4) Gas in Disk Galaxies
(5) Gas in Elliptical Galaxies
(6) Gas in Galactic Nuclei
(7) Gas in Galaxy Halos
(8) Dust: Particles in the ISM
      (a) Overview
      (b) Quick Estimates of Important Properties
            (i)   Hydrogen Column for Significant Dust Opacity
            (ii)  Dust Number Density
            (iii)  Dust Temperature
            (iv)  Dust Emission Efficiency
      (c) The Importance of Dust
      (d) The Path Ahead
(9) Dust: Physical Properties
      (a) Dust Composition from ISM Gas Depletion
      (b) Dust Creation
      (c) Subsequent Growth & Destruction of Grains
      (d) Dust Grain Size Distribution
      (e) Interaction with Light: Mie Theory
      (f) Dust Temperatures
            (i)   Inferred from IR Emission
            (ii)  Equilibrium Td Estimates
            (iii)  Thermal Spikes from Single Photons
(10) Dust: Emission & Absorption
      (a) Line & Band Features
      (b) Dust Absorption
            (i)   Basic Scenario
            (ii)  Standard Extinction Law
            (iii)  Some Other Parameters
            (iv)  Variations in the Extinction Law
            (v)   Correcting for Reddening & Extinction
            (vi)  Gas to Dust Ratios
            (vii)  X-Ray Absorption
            (viii) Polarization
(11) Dust Emssion from Galaxies
      (a) Absorption of Light
            (i)   Inclination Effects
            (ii)  Perpendicular Opacity of Disks
            (iii)  Hidden Star Formation
      (b) Emission: Broad Band SEDs
            (i)   Four Contributions to the FIR
            (ii)   Other Factors Affecting the IR Output
            (iii)  Variation Along the Hubble Sequence
            (iv)   Starbursts
            (v)   AGN
      (c) Emission: Spectral Features