The dust emission SED of X-ray emitting regions in Stephan's Quintet
G. Natale, R. J. Tuffs, C. K. Xu, C. C. Popescu, J. Fischera, U., Lisenfeld, N. Lu, P. Appleton, M. Dopita, P.-A. Duc, Y. Gao, W. Reach, J., Sulentic, M. Yun
TL;DR
This study investigates dust emission in Stephan's Quintet's X-ray regions, finding photon heating dominates over dust-gas collisions, with implications for gas cooling and star formation.
Contribution
It provides new insights into the dominant dust heating mechanisms in intergalactic shock regions of Stephan's Quintet.
Findings
Dust emission is mainly powered by photons.
Dust collisional heating may influence gas cooling.
Impacts on star formation morphology in SQ.
Abstract
We analysed the Spitzer maps of Stephan's Quintet in order to investigate the nature of the dust emission associated with the X-ray emitting regions of the large scale intergalactic shock and of the group halo. This emission can in principle be powered by dust-gas particle collisions, thus providing efficient cooling of the hot gas. However the results of our analysis suggest that the dust emission from those regions is mostly powered by photons. Nonetheless dust collisional heating could be important in determining the cooling of the IGM gas and the large scale star formation morphology observed in SQ.
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