Second Einstein Telescope Mock Data and Science Challenge: Low Frequency Binary Neutron Star Data Analysis

TL;DR

This paper presents an improved method for generating mock data and analyzes low frequency binary neutron star signals with a new pipeline, demonstrating enhanced detection and parameter estimation capabilities for the Einstein Telescope.

Contribution

It introduces an improved mock data generation method and a low latency analysis pipeline, achieving significant improvements in detecting and characterizing binary neutron star signals at low frequencies.

Findings

Able to discern overlapping signals from long-duration waveforms

High detection efficiency across analysis runs

Order of magnitude improvement in parameter recovery accuracy

Abstract

The Einstein Telescope is a conceived third generation gravitational-wave detector that is envisioned to be an order of magnitude more sensitive than advanced LIGO, Virgo and Kagra, which would be able to detect gravitational-wave signals from the coalescence of compact objects with waveforms starting as low as 1Hz. With this level of sensitivity, we expect to detect sources at cosmological distances. In this paper we introduce an improved method for the generation of mock data and analyse it with a new low latency compact binary search pipeline called gstlal. We present the results from this analysis with a focus on low frequency analysis of binary neutron stars. Despite compact binary coalescence signals lasting hours in the Einstein Telescope sensitivity band when starting at 5 Hz, we show that we are able to discern various overlapping signals from one another. We also determine the detection efficiency for each of the analysis runs conducted and and show a proof of concept method for estimating the number signals as a function of redshift. Finally, we show that our ability to recover the signal parameters has improved by an order of magnitude when compared to the results of the first mock data and science challenge. For binary neutron stars we are able to recover the total mass and chirp mass to within 0.5% and 0.05%, respectively.