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We present analyses of Spitzer observations of 29P/Schwassmann-Wachmann 1using 16 $\mu$m IRS "blue" peak-up (PU) and 24 $\mu$m and 70 $\mu$m MIPS imagesobtained on UT 2003 November 23 and 24 that characterize the Centaur'slarge-grain (10-100 $\mu$m) dust coma during a time of non-outbursting"quiescent" activity. Estimates of $\epsilon f \rho$ for each band (16 $\mu$m(2600 $\pm$ 43 cm), 24 $\mu$m (5800 $\pm$ 63 cm), and 70 $\mu$m (1800 $\pm$ 900cm)) follow the trend between nucleus size vs. $\epsilon f \rho$ that wasobserved for the WISE/NEOWISE comet ensemble. A coma model was used to derive adust production rate in the range of 50-100 kg/s. For the first time, a colortemperature map of SW1's coma was constructed using the 16 $\mu$m and 24 $\mu$mimaging data. With peaks at $\sim$ 140K, this map implies that coma water icegrains should be slowly sublimating and producing water gas in the coma. Weanalyzed the persistent 24 $\mu$m "wing" (a curved southwestern coma) featureat 352,000 km (90$''$) from the nucleus attributed by Stansberry et al. (2004)to nucleus rotation and instead propose that it is largely created by solarradiation pressure and gravity acting on micron sized grains. We performed comaremoval to the 16 $\mu$m PU image in order to refine the nucleus' emittedthermal flux. A new application of the Near Earth Asteroid Thermal Model(NEATM; Harris 1998) at five wavelengths (5.730 $\mu$m, 7.873 $\mu$m, 15.80$\mu$m, 23.68 $\mu$m, and 71.42 $\mu$m) was then used to refine SW1's effectiveradius measurement to $R = 32.3 \pm 3.1$ km and infrared beaming parameter to$\eta = 1.1 \pm 0.2$, respectively.

Characterization of Thermal Infrared Dust Emission and Refinements to the Nucleus Properties of Centaur 29P/Schwassmann-Wachmann 1