Improving the Detection and Characterization of Standing Accretion Shock Instability Using Gravitational Waves

Core collapse supernovae occur when the iron core of a supermassive star reaches the Chandrasekar limit and collapses on itself. The explosion can sometimes contain a feature called the standing accretion shock instability (SASI). Using laser interferometry, we can detect gravitational waves that are the result of a core collapse supernova. The gravitational wave signals that result from a collapse are rare and the SASI cannot be detected at all amplitudes and locations within our galaxy. By injecting the triggers of simulated models of supernovae into real data, it can be used to test the abilities of additional pipelines and programs to analyze the detection. The goal of using these analytical pipelines is to improve the detection efficiency of SASI in core collapse supernovae across our galaxy. This detection can be used to estimate the SASI deterministic parameters of frequency and duration and to extract astrophysical information about the source. Using the new version of coherent Wave Burst (cWB) and introducing MuLaSEcC will result in better data that can be run through a green version of SASI-meter, a program designed to analyze and characterize the SASI component of core collapse supernovae. This improvement can be applied to real interferometric data and has the potential of discovering the first gravitational wave of a core collapse supernova and SASI component within our galaxy.