Steering Astronomy Toward Gravitational Wave-Supernova Science Kiranjyot (Jasmine) Gill, 1 Dr. Michele Zanolin 1 With support from Marek Szczepanczyk 1 1 Physics Department, Embry-Riddle Aeronautical University, Prescott, AZ Abstract Physical Assumptions and Constraints Analysis: Distributions of the galaxies within 20 Mpc  infer core-collapse supernova rate (CCSN) Projected Outcome: Identify the best strategy to monitor galaxies and increase the chance of CCSN detection and therefore increase the probability of GW emission detection Acknowledgements Support provided by: LVC Organization ERAU URI  The current projected model exclusion range for advanced LIGO and extreme models is usually larger than the detection range and Coherent Wave Burst (CWB) + Bayes Wave + upgrades could expand ranges above by a factor of 2  20 Mpc  B= 10^{-20.8 – A/2.5}  Where B is the blue luminosity of each given galaxy, and A is the absolute magnitude of each given galaxy. Blue Luminosity units: erg (which is J) s -1 Absolute Magnitude units: parsecs  Using blue light luminosity to trace star formation, an estimated CCSN conversion rate per Milky Way unit mass (MWUM) of:  146 (8.5) 158 × CCSNe yr − 1 MWUM − 1 for spiral (elliptical) irregular galaxies  Galaxies possessing absolute magnitude fainter than -13  eliminated as little to no probability of becoming a CCSN host Core-Collapse supernovas (CCSNe) mark the dynamic and explosive end of the lives of massive stars by emitting the gravitational wave that is detectable by detectors such as LIGO. LIGO has been one of the first collaborations to create ways to collect and analyze data that would distinguish the gravitational waves from background noise produced on Earth. Optical observations of supernovas in the Local Universe provide trigger times (with a typical uncertainty of a few days) and precise sky locations, while an E&M observation would provide a core-collapse trigger time (with an uncertainty of a few seconds) and a sky location. We describe a method that takes into account optical and E&M observational techniques for detection of CCSNe within the Local Universe, which encompasses a volume of 20 Mpc. Providing distance sensitivity estimates for the rate of CCSNe within the Local Field and the Virgo Cluster specializes the implementation of the CCSNe rate toward specifically gravitational wave detection. Overview All< 50 Mpc 20 Mpc  Local Group (D < 3 Mpc), CCSN rate: × 10 − 2 CCSNe yr − 1 with major contributions from Andromeda (M31), Triangulum (M33), and the dwarf irregular galaxy IC 10, IC 1613, and NGC 6822  Outside of Local Group (D ~ 5 Mpc), CCSN rate: ×10 − 2 CCSNe yr − 1 with IC 342, the M 81 group, M83, and NGC 253 as significant contributors  D = 10 Mpc, CCSN rate: ×10 − 2 CCSNe yr -1 ; D= 20 Mpc, CCSN rate: ×10 − 2 CCSNe yr − 1  Use distance sensitive estimates for both the first and second generation LIGO networks by using GW waveforms extracted from four recent numerical simulation sets and two extreme phenomenological models for gravitational wave emission in core-collapse  Compilation of two publishable research papers; one focusing on the First Targeted Search for Gravitational-Wave Bursts from Core-Collapse Supernovae in Data of First-Generation Laser Interferometer Detectors, and Observing Gravitational Waves from Core-Collapse Supernovae Future Directions Breakdown of SN