First astrometric constraints on parity-violation in the gravitational wave background
Astrometry, the precise measurement of stellar positions and velocities, offers a promising approach to probing the low-frequency stochastic gravitational wave background (SGWB). Notably, astrometric vector sky maps are sensitive to parity-violating SGWB signals, which cannot be distinguished using...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:dnet:digitalcsic_::5ca4e0864ddcb03a89b8c72e883759c3 |
| Acceso en línea: | http://hdl.handle.net/10261/427888 https://www.scopus.com/inward/record.uri?eid=2-s2.0-105013866750&doi=10.1088%2F1475-7516%2F2025%2F08%2F057&partnerID=40&md5=59a7182d9c006e4ba84a2696d906985e |
| Access Level: | acceso abierto |
| Palabra clave: | gravitational waves / theory Gravitational waves in GR and beyond: theory Statistical sampling techniques |
| Sumario: | Astrometry, the precise measurement of stellar positions and velocities, offers a promising approach to probing the low-frequency stochastic gravitational wave background (SGWB). Notably, astrometric vector sky maps are sensitive to parity-violating SGWB signals, which cannot be distinguished using pulsar timing array observations in an isotropic SGWB. We present the first astrometric constraints on parity-violating SGWB using quasar catalogs from Gaia DR3 and VLBA data. By analyzing the EB correlation in the two-point correlation function of the proper motions of the quasars, we find 2σ constraints on the parity-violating SGWB amplitude h 702ΩV = -0.020 ± 0.025 from Gaia DR3 and h 702ΩV = -0.004 ± 0.010 from VLBA. These constraints are valid in the frequency range 4.2 × 10-18 Hz < f < 1.1 × 10-8 Hz. Although not currently a tight constraint on theoretical models, this first attempt lays the groundwork for future investigations using more precise astrometric data. © 2025 The Author(s) |
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