0----- Attempting Submission 2 (Thu Sep 12 15:10:08 GMT 2013) -----
HST Phase II Proposal 13321 (SQ_COS_Phase2_5targets.apt) successfully submitted.
----- Attempting Submission 3 (Wed Sep 25 13:03:15 GMT 2013) -----I specified the IRCS reference frame for the target acquisition stars instead of the Guide Star Catalog. The coordinates of the target acquisition stars are known to sub-arcescond precision, and the offset between the target acquisition star and the science source have been measured in the same frame of reference.COS Spectroscopy of the Stephan's Quintet Giant ShockStephan's Quintet, the most studied compact group, is an ideal laboratory to study how kinetic energy is dissipated, how gas cools, and how star formation is triggered in galaxy interactions. It hosts a dramatic 30 kpc X-ray emitting shocked region, triggered by a 1000 km/s galaxy collision. Our Spitzer and Herschel spectroscopy has revealed that H2, C+ and OI are important coolants in the shock, with luminosities exceeding that of X-rays. However, nothing is known about UV line cooling. Our models of the collision show that the kinetic energy is dissipated through a turbulent cascade, with a large range of shock velocities (from 600 down to 10 km/s in the H2 gas), with shock-excited UV emission lines possibly dominating the energy budget at intermediate velocities. Thus, we propose to observe the brightest ones (Lya, CIV, OVI) with COS by targeting different environments in the shock. Our key science goals are to (1) quantify the contribution of the UV lines to the total gas cooling, (2) understand why, despite large H2 masses, the star formation efficiency in the shock is very low, and (3) determine the origin of the diffuse UV emission detected with GALEX in the shock (is it continuum or line emission?). These observations are crucial to determine the dissipation rate and physical state of the gas and to understand the star formation efficiency. This problem is relevant to many other active phases of galaxy evolution, ranging from shocks in infrared luminous galaxies and AGN feedback, to gas cooling and formation of the first galaxies at high z.The project aims to explore the importance of key UV emission lines in the cooling side of the energy budget of the giant intergalactic shock structure in the Stephan's Quintet group. Previous observations with Spitzer and Herschel have shown that this huge intergroup structure shows powerful line cooling through pure rotational molecular lines in the mid-IR and almost as much cooling from the [CII] and [OI] far-IR fine-structure lines. Preliminary modeling suggests that energy from a galaxy collision is being dissipated through various cooling pathways, however nothing is known about the UV cooling. The COS spectroscopy is targeted at specific regions in the giant filament where we might expect powerful UV cooling from Lyman-alpha, CIV, OVI and other lines. The observations will allow us to 1) determine how important UV line cooling is as energy is progressively funneled by turbulence to smaller and smaller scales, 2) use the spectra to help understand the kinematics of warmer gas and its connection to the turbulent molecular gas already detected and specifically to look for mechanisms that might suppress star formation (negative feedback), and finally 3) to determine how much of the UV emission detected by GALEX across the shock-structure is attributed to line emission rather than diffuse continuum emission from faint massive stars. We request observations at moderate resolution using the G130M and G160M settings for the seven positions in the shock structure. In order to achieve continuous spectral coverage and minimize fixed pattern noise, observations in each grating will be made at two central wavelengths for G130M and G160M. 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