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2.1 kpc2) where Spitzer observations were performed. The preshock gas is mainly the H I gas contained in the tidal tail of NGC 7319. After the shock, the mass is distributed between the hot X-ray emitting plasma and the  gas (see text for details). Before the shock, most of the energy available is the kinetic energy of the H I gas that will be shocked. The shock splits the energy budget in two parts: thermal and kinetic energy. The former is stored in the hot plasma whereas the latter goes into turbulent motions that heat the gas. Observations show that mechanical energy is the dominant energy reservoir. b XMM-Newton observations of the extended X-ray emission in the shock and the tidal tail (Trinchieri et al. 2005). c H 
and O I optical line observations by Xu et al. (2003). d Based on extrapolation of H I observations in the tidal tail by Williams et al. (2002); Sulentic et al. (2001). e From Spitzer IRS observations. The line flux is summed over the S(0) to S(5) lines (Appleton et al. 2006). f This bulk kinetic energy is a lower limit because an unknown mass of turbulent cold molecular gas can contribute to this energy. g Luminosities are indicated assuming a distance to SQ of 94 Mpc. |
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