"The Infrared Surface Brightness of Normal Galaxies"
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     Abstract

  I. Introduction
     A. Discuss 2-component model
        1. PDR and SFR mixing
     B. clues to IR surf. br. drivers from literature 
        1. Discuss our results from paper on IC 10, N1313, N6946
        2. Review our simple model: Sigma ~ N_d*<U>

 II. Mid-IR Sample & Data
     A. Very briefly review the Key Project sample
        1. Morphs, FIR/B, 60/100, etc
     B. Briefly describe CAM data 
        1. refer to Silbermann '99
     C. ISOCAM Observations (~same as for paper on SB in nearby galaxy )
     D. Review flux, size measures/estimators

III. Physics of Surface Brightness
     A. Discuss measured/estimated s.b. and the roles of:
        1. Filling factor variations
        2. disk vs single central clump/concentration
        3. geometry; line-of-sight effects

 IV. Surface Brightness of Normal Galaxies
     A. MIR s.b. vs FIR s.b.                                 (FIGURE)
        1. tests s.b. in different locales/environments
           a. MIR <-> HII regions + cirrus; ionizing
           b. FIR <-> PDRs + cirrus (>= surface of HII regions);non-ionizing
        2. 1st order: strong correlation; as s.b increases, so do <U> & N_d
        3. 2nd order: FIR rises more rapidly than MIR
     B. (MIR+FIR) surf. br. vs 60/100                        (FIGURE)
        1. Mention that (a*MIR+b*FIR) may be a good estimator for total IR flux
        2. correlation shows surf. br. = fn(<U>)
     C. (MIR+FIR) surf. br. vs (MIR+FIR)/B                   (FIGURE)
        1. correlation shows surf. br. = fn(N_d) 
        2. correct for inclination, varying line-of-sight depths
     D. H-alpha Equivalent Width vs 60/100 and/or 7/15??     (FIGURE)
        1. trends are ambiguous except for low E.W.??

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Probably have separate paper on this topic:

  V. ISO-IRAS color-color diagram??????                      (FIGURE)
     A. Macro-physics: 2-COMPONENT mixing
        1. PDRs + SFRs  (cirrus + HII regions)
     B. Micro-physics: PAH destruction and 15 micron continuum rise
        1. plateau/rise for low 60/100 due to steadily increasing AFE 
           strength as heating intensity turns on.
        2. drop due to 15 micron continuum rise (and small effect due to
           PAH destruction).
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 VI. Discussion
     A. A simple model for drivers of IR s.b. is reviewed 
     B. s.b. trends for distant gals agree w/model derived from nearby gals.
        1. s.b. correlated with 60/100
           a. vertical scatter attributable to N_d scatter
        2. s.b. vs tau shows strong correlation
           a. vertical scatter attributable to U scatter
        3. s.b. vs 7/15 for distant gals shows less sharp inflection point
           than seen for the nearby gals b/c:
           a. the 15/7 colors are averaged over the galaxy.
           b. scatter due to varying geometries, dust content
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