Abstract
With the increasing sensitivity of gravitational-wave detectors, we expect to observe multiple binary neutron-star systems through gravitational waves in the near future. The combined analysis of these gravitational-wave signals offers the possibility to constrain the neutron-star radius and the equation of state of dense nuclear matter with unprecedented accuracy. However, it is crucial to ensure that uncertainties inherent in the gravitational-wave models will not lead to systematic biases when information from multiple detections is combined. To quantify waveform systematics, we perform an extensive simulation campaign of binary neutron-star sources and analyze them with a set of four different waveform models. For our analysis with 38 simulations, we find that statistical uncertainties in the neutron-star radius decrease to ±250 m (2% at 90% credible interval) but that systematic differences between currently employed waveform models can be twice as large. Hence, it will be essential to ensure that systematic biases will not become dominant in inferences of the neutron-star equation of state when capitalizing on future developments.
| Original language | English (US) |
|---|---|
| Article number | L061301 |
| Journal | Physical Review D |
| Volume | 105 |
| Issue number | 6 |
| DOIs | |
| State | Published - Mar 15 2022 |
Bibliographical note
Funding Information:We thank Tatsuya Narikawa and the LVK Extreme Matter group for fruitful discussions and comments on the study. P. T. H. P. is supported by the research program of the Netherlands Organisation for Scientific Research (NWO). The work of I. T. was supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, under Contract No. DE-AC52-06NA25396, by the Laboratory Directed Research and Development program of Los Alamos National Laboratory under Projects No. 20190617PRD1 and No. 20190021DR, and by the U.S. Department of Energy, Office of Science, Office of Advanced Scientific Computing Research, Scientific Discovery through Advanced Computing (SciDAC) NUCLEI program. Computational resources have been provided by the Los Alamos National Laboratory Institutional Computing Program, which is supported by the U.S. Department of Energy National Nuclear Security Administration under Contract No. 89233218CNA000001, and by the National Energy Research Scientific Computing Center (NERSC), which is supported by the U.S. Department of Energy, Office of Science, under Contract No. DE-AC02-05CH11231. We also acknowledge usage of computer time on Lise/Emmy of the North German Supercomputing Alliance (HLRN) [Project No. bbp00049], on HAWK at the High-Performance Computing Center Stuttgart (HLRS) [Project No. GWanalysis 44189], and on SuperMUC NG of the Leibniz Supercomputing Centre (LRZ) [Project No. pn29ba]. M. W. C. acknowledges support from the National Science Foundation with Grants No. PHY-2010970 and No. OAC-2117997. All posterior samples and results are available on .
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