Uncertainty limits on neutron star radius measurements with gravitational waves

Abstract

Upcoming observing campaigns with improved detectors will yield numerous detections of gravitational waves from neutron star binary inspirals. Rare loud signals together with numerous signals of moderate strength promise stringent constraints on the properties of neutron star matter, with a projected radius statistical uncertainty of 50-200 m with Oð2000Þ sources. Given this precision we revisit all analysis assumptions and identify sources of systematic errors, quantify their impact on radius extraction, and discuss their relative importance and ways to mitigate them.

Sensitivity of Neutron Star Observations to Three-nucleon Forces

“…The same conclusion would apply assuming that binaries are detected by the proposed Cosmic Explorer [85,86]. The large SNRs expected in the 3G era also require a careful assessment of waveform systematics which could bias the parameter reconstruction [84,[87][88][89]. However, our results strongly support the evidence that with the upcoming third generation detectors, our understanding of neutron star matter will make a great step forward into the direction of using NS observations to probe fundamental physics at the fermi scale.…”

Concurrent estimation of noise and compact-binary signal parameters in gravitational-wave data

“…However, the choice of PSD estimation method, specifically the off-source mean or median studied in [29], had a greater impact on the inferred parameter posterior than PSD marginalization. Similar conclusions were reached in [31] in the context of the impact of PSD misestimation on inferring the tidal deformability of neutron star binaries. The impact of marginalization could be more significant when precise calculations of Bayesian evidence are needed [29].…”

Emergence of microphysical viscosity in binary neutron star post-merger dynamics

“…Binary neutron star mergers [1,2] offer exciting prospects for constraining the dense matter equation of state (EoS) [3][4][5] (e.g., [6][7][8][9][10][11]). This can be done either by using the tidal deformability encoded in the inspiral gravitational wave signal [12][13][14][15][16][17][18][19], the potential presence of very massive neutron stars in gravitational wave events [20][21][22][23][24][25][26], or by using the combined information from electromagnetic counterparts [27][28][29][30][31].…”