Gravitational-wave parameter inference with the Newman-Penrose scalar
Detection and parameter inference of gravitational-wave signals from compact mergers rely on the comparison of the incoming detector strain data () to waveform templates for the gravitational-wave strain ℎ() that ultimately rely on the resolution of Einstein’s equations via numerical relativity si...
| Autores: | , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Universidad de Santiago de Compostela (USC) |
| Repositorio: | Minerva. Repositorio Institucional de la Universidad de Santiago de Compostela |
| Idioma: | inglés |
| OAI Identifier: | oai:minerva.usc.gal:10347/45828 |
| Acceso en línea: | https://hdl.handle.net/10347/45828 |
| Access Level: | acceso abierto |
| Palabra clave: | Experimental studies of gravity General relativity Gravitational waves Astrophysics Gravitation |
| Sumario: | Detection and parameter inference of gravitational-wave signals from compact mergers rely on the comparison of the incoming detector strain data () to waveform templates for the gravitational-wave strain ℎ() that ultimately rely on the resolution of Einstein’s equations via numerical relativity simulations. These, however, commonly output a quantity known as the Newman-Penrose scalar 4() which, under the Bondi gauge, is related to the gravitational-wave strain by 4() =2ℎ()/2. Therefore, obtaining strain templates involves an integration process that introduces artifacts that need to be treated in a rather manual way. By taking second-order finite differences on the detector data and inferring the corresponding background noise distribution, we develop a framework to perform gravitational-wave data analysis directly using 4() templates. We first demonstrate this formalism, and the impact of integration artifacts in strain templates, through the recovery of numerically simulated signals from head-on collisions of Proca stars injected in Advanced LIGO noise. Next, we reanalyze the event GW190521 under the hypothesis of a Proca-star merger, obtaining results equivalent to those previously published [Phys. Rev. Lett. 126, 081101 (2021)], where we used the classical strain framework. We find, however, that integration errors would strongly impact our analysis if GW190521 was 4 times louder. Finally, we show that our framework fixes significant biases in the interpretation of the high-mass gravitational-wave trigger S200114f arising from the usage of strain templates. We remove the need to obtain strain waveforms from numerical relativity simulations, avoiding the associated systematic errors |
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