Document Type

Poster

Publication Date

Summer 2024

Abstract

Gravitational waves (GWs) are a natural phenomenon predicted by general relativity (GR) that are emitted when two compact objects inspiral in a compact binary coalescence (CBC). The systems detectable on Earth include binary black hole systems (BBHs), binary neutron star systems (BNS), and neutron star-black hole systems (NSBH). Another consequence of GR is that when these waves pass through spacetime deformed by gravity from other compact objects (perturbers), a glint is expected to appear. This glint is a copy of the gravitational wave that travels at a slightly slower speed near the perturber and with an amplitude a fraction of the original signal. This project focused on placing upper limits on how large a glint could be without being detected in LIGO and Virgo’s first through third observing runs. The search for these upper limits is necessary because a direct search for glints in the data resulted in none being found, so theoretical limits on these glints must be determined.

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