Gravitational-Wave and Gravitational-Wave Memory Signatures of Core-Collapse Supernovae

Understand

In this paper, we calculate the energy, signal-to-noise ratio, detection range, and angular anisotropy of the matter, matter memory, and neutrino memory gravitational wave (GW) signatures of 21 three-dimensional initially non-rotating core-collapse supernova (CCSN) models carried to late times.

• We find that inferred energy, signal-to-noise ratio, and detection range are angle-dependent quantities, and that the spread of possible energy, signal-to-noise, and detection ranges across all viewing angles generally increases with progenitor mass.
• When examining the low-frequency matter memory and neutrino memory components of the signal, we find that the neutrino memory is the most detectable component of a CCSN GW signal, and that DECIGO is best-equipped to detect both matter memory and neutrino memory.
• Moreover, we find that the polarization angle between the $h_+$ and $h_{\times}$ strains serves as a unique identifier of matter and neutrino memory.