Dependence of the reconstructed core-collapse supernova gravitational wave high-frequency feature on the nuclear equation of state in real interferometric data
R. Daniel Murphy, Alejandro Casallas-Lagos, Anthony Mezzacappa, M. Zanolin, Ryan E. Landfield, Eric J. Lentz, Pedro Marronetti, Javier M. Antelis, Claudia Moreno
Abstract
We present an analysis of gravitational wave (GW) predictions from five two-dimensional core collapse supernova (CCSN) simulations that varied only in the equation of state (EOS) implemented. The GW signals from these simulations are used to produce spectrograms in the absence of noise, and the emergent high-frequency feature (HFF) is found to differ quantitatively between simulations. Below 1 kHz, the HFF is well approximated by a first-order polynomial in time. The resulting slope was found to vary between 10% and 50% from model to model. Further, using real interferometric noise we investigated the current capabilities of GW detectors to resolve these differences in HFF slope for a Galactic CCSN. We find that, for distances up to 1 kpc, current detectors have the ability to resolve HFF slopes differing by 4.4%--15%. For further Galactic distances, current detectors are capable of distinguishing the upper and lower bounds of the HFF slope for groupings of our models that varied in EOS. With the higher sensitivity of future GW detectors, and with improved analysis of the HFF, our ability to resolve properties of the HFF will improve for all Galactic distances. This study shows the potential of using the HFF of CCSN produced GWs to provide insight into the physical processes occurring deep within CCSN during collapse, and in particular its potential to further constrain the EOS through GW detection.