Accuracy in Measuring the Neutron Star Mass in Gravitational Wave Parameter Estimation for Black Hole-Neutron Star Binaries

Abstract

Recently, two gravitational wave (GW) signals, named as GW150914 and GW151226, have been detected by the two LIGO detectors. Although both signals were identified as originating from merging black hole (BH) binaries, GWs from systems containing neutron stars (NSs) are also expected to be detected in the near future by the Advanced detector network. In this work, we assess the accuracy in measuring the NS mass ($M_{ns}$) for the GWs from BH-NS binaries adopting the Advanced LIGO sensitivity with a signal-to-noise ratio of 10. By using the Fisher matrix method, we calculate the measurement errors ($\sigma$) in $M_{ns}$ assuming the NS mass of $1\le M_{ns}/M_{\odot }\le 2$ and low mass BHs with the range of $4\le M_{bh}/M_{\odot }\le 10$. We used the TaylorF2 waveform model where the spins are aligned with the orbital angular momentum, but here we only consider the BH spins. We find that the fractional errors ($\sigma /M_{ns}\times 100$) are in the range of $10\%-50\%$ in our mass region for a given dimensionless BH spin as ${\chi }_{bh}=0$. The errors tend to increase as the BH spin increases, and this tendency is stronger for higher NS masses (or higher total masses). In particular, for the highest mass NSs ($M_{ns}=2M_{\odot }$), the errors $\sigma$ can be larger than the true value of $M_{ns}$ if the dimensionless BH spin exceeds $\sim 0.6$.

5 pages, 2 figures, submitted to JKPS

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Cited by in corpus (1)

• Efficiency of nonspinning templates in gravitational wave searches for aligned-spin binary black holes