Assigned ID: 970 ----- Attempting Submission 1 (Sat Feb 26 02:57:10 GMT 2011) ----- HST Phase I Proposal 970 (prop_theory.apt) successfully submitted. ----- Attempting Submission 2 (Sat Feb 26 07:50:36 GMT 2011) ----- HST Phase I Proposal 970 (prop_theory.apt) successfully submitted. ----- Attempting Submission 3 (Sat Feb 26 08:13:11 GMT 2011) ----- HST Phase I Proposal 970 (prop_theory.apt) successfully submitted. ----- Attempting Submission 4 (Sat Feb 26 20:55:35 GMT 2011) ----- It is a remarkable fact that in the present day universe more than 50% of the baryonic matter is "missing'', in that it has not yet been accounted for observationally. Hydrodynamic simulations of structure formation predict that these baryons may reside in a Warm/Hot Intergalactic Medium (WHIM) with temperatures in the range 1e5-1e7 K. The WHIM is produced by the shock waves that occur as gas falls from the diffuse intergalactic medium onto the dense regions where galaxies form. Detecting signatures from the WHIM is one of the main science drives of the Cosmic Origins Spectrograph (COS). In this proposal I describe a set of theoretical computations of the absorption-line signatures of WHIM shocks, which are crucial to interpreting COS observational data. In particular, I focus on the detectable UV-absorption signatures associated with the radiative precursors of WHIM shocks.

QUASAR ABSORPTION LINES AND IGM 12 Small false 0.0 0.0 false false true false SUPPORTED