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

Spitzer Space Telescope observations revealed powerful mid-infrared (mid-IR) H2 rotational line emission from the Stephan's Quintet (SQ) X-ray emitting large scale shock associated with a collision between two galaxies. Because H2 forms on dust grains, the presence of H2 is physically linked to the survival of dust, and we expect some dust emission to come from the molecular gas. To test this interpretation, IR observations and dust modeling are used to identify and characterize the thermal dust emission from the shocked molecular gas. The spatial distribution of the IR emission allows us to isolate the faint PAH and dust continuum emission associated with the molecular gas in the SQ shock. We model the spectral energy distribution (SED) of this emission, and fit it to Spitzer observations. Faint PAH and dust continuum emission are detected in the SQ shock, outside star-forming regions. The 12/24um flux ratio in the shock is remarkably close to that of the diffuse Galactic interstellar medium, leading to a Galactic PAH/VSG abundance ratio. However, the properties of the PAH emission spectrum in the shock differ from that of the Galaxy, which may suggest an enhanced fraction of large and neutrals PAHs. The IR SED is consistent with the expected emission from dust associated with the warm (>150K) H2 gas, heated by a UV radiation field of intensity comparable to that of the solar neighborhood, in agreement with GALEX UV observations. The presence of PAHs and dust grains in the high-speed (1000km/s) galaxy collision suggests that dust survives. We propose that the dust that survived destruction was in pre-shock gas at densites larger than a few 0.1cm-3, which was not shocked at velocities larger than 200km/s. [abridged]