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The Spitzer GLIMPSE and MIPSGAL surveys have revealed a wealth of details ofthe Galactic plane. We use them to study the energetics and dust properties ofM16, one of the best known SFR. We present MIPSGAL observations of M16 at 24and 70 $\mu$m and combine them with previous IR data. The MIR image shows ashell inside the molecular borders of the nebula. The morphologies at 24 and 70$\mu$m are different, and its color ratio is unusually warm. The FIR imageresembles the one at 8 $\mu$m that enhances the molecular cloud. We measure IRSEDs within the shell and the PDRs. We use the DUSTEM model to fit the SEDs andconstrain dust temperature, dust size distribution, and ISRF intensity relativeto that provided by the star cluster NGC6611. Within the PDRs, the dusttemperature, the dust size distribution, and the ISRF intensity are inagreement with expectations. Within the shell, the dust is hotter and an ISRFlarger than that provided by NGC6611 is required. We quantify two solutions.(1) The size distribution of the dust in the shell is not that of interstellardust. (2) The dust emission arises from a hot plasma where UV and collisionswith electrons contribute to the heating. We suggest two interpretations forthe shell. (1) The shell matter is supplied by photo-evaporative flows arisingfrom dense gas exposed to ionized radiation. The flows renew the shell matteras it is pushed by the stellar winds. Within this scenario, we conclude thatmassive SFR such as M16 have a major impact on the carbon dust sizedistribution. The grinding of the carbon dust could result from shattering incollisions within shocks driven by the interaction between the winds and theshell. (2) We consider a scenario where the shell is a SNR. We would bewitnessing a specific time in the evolution of the SNR where the plasmapressure and temperature would be such that the SNR cools through dustemission.

Tracing the Energetics and Evolution of Dust with Spitzer: a Chapter in the History of the Eagle Nebula