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Spitzer Space Telescope observations revealed powerful mid-infrared (mid-IR)H2 rotational line emission from the Stephan's Quintet (SQ) X-ray emittinglarge scale shock associated with a collision between two galaxies. Because H2forms on dust grains, the presence of H2 is physically linked to the survivalof dust, and we expect some dust emission to come from the molecular gas. Totest this interpretation, IR observations and dust modeling are used toidentify and characterize the thermal dust emission from the shocked moleculargas. The spatial distribution of the IR emission allows us to isolate the faintPAH and dust continuum emission associated with the molecular gas in the SQshock. We model the spectral energy distribution (SED) of this emission, andfit it to Spitzer observations. Faint PAH and dust continuum emission aredetected in the SQ shock, outside star-forming regions. The 12/24um flux ratioin the shock is remarkably close to that of the diffuse Galactic interstellarmedium, leading to a Galactic PAH/VSG abundance ratio. However, the propertiesof the PAH emission spectrum in the shock differ from that of the Galaxy, whichmay suggest an enhanced fraction of large and neutrals PAHs. The IR SED isconsistent with the expected emission from dust associated with the warm(>150K) H2 gas, heated by a UV radiation field of intensity comparable to thatof the solar neighborhood, in agreement with GALEX UV observations. Thepresence of PAHs and dust grains in the high-speed (1000km/s) galaxy collisionsuggests that dust survives. We propose that the dust that survived destructionwas in pre-shock gas at densites larger than a few 0.1cm-3, which was notshocked at velocities larger than 200km/s. [abridged]

Observations and modeling of the dust emission from the H2-bright galaxy-wide shock in Stephan's Quintet