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at the Barcelona Supercomputing Center (Grant No. AECT-2022-2-0006 and No. FI-2024-2-0012) and at the Lluis Vives cluster for scientific calculations at the University of Valencia https:// www.uv.es/uvweb/servei-informatica/ca/serveis/. We acknowledge computa-tional resources provided by the CIT cluster of the LIGO Laboratory and supported by National Science Foundation (NSF) Grant No. PHY-0757058 and No. PHY0823459; and the support of the NSF CIT cluster for the provision of computational resources for our parameter inference runs. This material is based upon work supported by NSF's LIGO Laboratory which is a major facility fully funded by the National Science Foundation.r at the Barcelona Supercomputing Center (Grant No. AECT-2022-2-0006 and No. FI-2024-2-0012) and at the Lluis Vives cluster for scientific calculations at the University of Valencia https:// www.uv.es/uvweb/servei-informatica/ca/serveis/. We acknowledge computa-tional resources provided by the CIT cluster of the LIGO Laboratory and supported by National Science Foundation (NSF) Grant No. PHY-0757058 and No. PHY0823459; and the support of the NSF CIT cluster for the provision of computational resources for our parameter inference runs. This material is based upon work supported by NSF's LIGO Laboratory which is a major facility fully funded by the National Science Foundation.

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Numerical-relativity surrogate model for hyperbolic encounters of black holes: Challenges in parameter estimation

Publicado en:Physical Review d. 111 (4): 044024- - 2025-02-10 111(4), DOI: 10.1103/PhysRevD.111.044024

Autores: Fontbute, Joan; Andrade, Tomas; Luna, Raimon; Bustillo, Juan Calderon; Morras, Gonzalo; Jaraba, Santiago; Izquierdo, German Lopez

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Resumen

We present a surrogate numerical-relativity model for close hyperbolic black-hole encounters with equal masses and spins aligned with the orbital momentum. Our model, generated in terms of the Newman- Penrose scalar psi 4, spans impact parameters b/M is an element of [11, 15] and spin components chi i is an element of [-0.5, 0.5], modeling the (l, m) = (2, 0), (2, +2), (3, +2), and (4, +4) emission multipoles. The model is faithful to numerical- relativity simulations, yielding mismatches lower than 10-3. We test the ability of our model to recover the parameters of numerically simulated signals. We find that, despite the high accuracy of the model, parameter inference struggles to correctly capture the parameters of the source even for SNRs as large as 50 due to the strong degeneracies present in the parameter space. This indicates that correctly identifying these systems will require extremely large signal loudness, which is only typical of third generation detectors. Nevertheless, we also find that, if one attempts to infer certain combinations of such degenerated parameters, there might be a chance to prove the existence of this type of event, even with the current ground-based detectors, as long as these combinations make sense astrophysically and cosmologically.

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