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Measuring kinematic anisotropies with pulsar timing arrays

N. M. Jiménez Cruz Orcid Logo, Ameek Malhotra Orcid Logo, Gianmassimo Tasinato Orcid Logo, Ivonne Zavala Carrasco Orcid Logo

Physical Review D, Volume: 110, Issue: 6

Swansea University Authors: Ameek Malhotra Orcid Logo, Gianmassimo Tasinato Orcid Logo, Ivonne Zavala Carrasco Orcid Logo

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DOI (Published version): 10.1103/physrevd.110.063526

Abstract

Recent pulsar timing array (PTA) collaborations show strong evidence for a stochastic gravitational wave background (SGWB) with the characteristic Hellings-Downs interpulsar correlations. The signal may stem from supermassive black hole binary mergers, or early Universe phenomena. The former is expe...

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Published in: Physical Review D
ISSN: 2470-0010 2470-0029
Published: American Physical Society (APS) 2024
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URI: https://cronfa.swan.ac.uk/Record/cronfa67446
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spelling v2 67446 2024-08-21 Measuring kinematic anisotropies with pulsar timing arrays dd6ebf069325cdbdbeb597fa64d48063 0000-0001-8346-9995 Ameek Malhotra Ameek Malhotra true false cb754b073d1e4949c5e3db97744d3301 0000-0002-9835-4864 Gianmassimo Tasinato Gianmassimo Tasinato true false 2fb8d4bb665e9a89d3b3478c17f646f8 0000-0002-5589-9928 Ivonne Zavala Carrasco Ivonne Zavala Carrasco true false 2024-08-21 BGPS Recent pulsar timing array (PTA) collaborations show strong evidence for a stochastic gravitational wave background (SGWB) with the characteristic Hellings-Downs interpulsar correlations. The signal may stem from supermassive black hole binary mergers, or early Universe phenomena. The former is expected to be strongly anisotropic, while primordial backgrounds are likely to be predominantly isotropic with small fluctuations. In the case the observed SGWB is of cosmological origin, our relative motion with respect to the SGWB rest frame is a guaranteed source of anisotropy, leading to ⁡(10−3) energy density fluctuations of the SGWB. For such cosmological SGWB, kinematic anisotropies are likely to be larger than the intrinsic anisotropies, akin to the cosmic microwave background (CMB) dipole anisotropy. We assess the sensitivity of current PTA data to the kinematic dipole anisotropy, and we also forecast at what extent the magnitude and direction of the kinematic dipole can be measured in the future with an SKA-like experiment. We also discuss how the spectral shape of the SGWB and the location of the pulsars to monitor affect the prospects of detecting the kinematic dipole with PTA. In the future, a detection of this anisotropy may even help resolve the discrepancy in the magnitude of the kinematic dipole as measured by CMB and large-scale structure observations. Journal Article Physical Review D 110 6 American Physical Society (APS) 2470-0010 2470-0029 General Relativity and Quantum Cosmology (gr-qc); Cosmology and Nongalactic Astrophysics (astro-ph.CO) 11 9 2024 2024-09-11 10.1103/physrevd.110.063526 COLLEGE NANME Biosciences Geography and Physics School COLLEGE CODE BGPS Swansea University SU Library paid the OA fee (TA Institutional Deal) Swansea University 2024-09-13T11:40:43.2953235 2024-08-21T09:59:03.0236543 Faculty of Science and Engineering School of Biosciences, Geography and Physics - Physics N. M. Jiménez Cruz 0009-0003-4719-2126 1 Ameek Malhotra 0000-0001-8346-9995 2 Gianmassimo Tasinato 0000-0002-9835-4864 3 Ivonne Zavala Carrasco 0000-0002-5589-9928 4 67446__31310__49916fda1e374a929b69f714dc1823a6.pdf 67446.VoR.pdf 2024-09-13T11:39:12.7601566 Output 648424 application/pdf Version of Record true Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. true eng https://creativecommons.org/licenses/by/4.0/
title Measuring kinematic anisotropies with pulsar timing arrays
spellingShingle Measuring kinematic anisotropies with pulsar timing arrays
Ameek Malhotra
Gianmassimo Tasinato
Ivonne Zavala Carrasco
title_short Measuring kinematic anisotropies with pulsar timing arrays
title_full Measuring kinematic anisotropies with pulsar timing arrays
title_fullStr Measuring kinematic anisotropies with pulsar timing arrays
title_full_unstemmed Measuring kinematic anisotropies with pulsar timing arrays
title_sort Measuring kinematic anisotropies with pulsar timing arrays
author_id_str_mv dd6ebf069325cdbdbeb597fa64d48063
cb754b073d1e4949c5e3db97744d3301
2fb8d4bb665e9a89d3b3478c17f646f8
author_id_fullname_str_mv dd6ebf069325cdbdbeb597fa64d48063_***_Ameek Malhotra
cb754b073d1e4949c5e3db97744d3301_***_Gianmassimo Tasinato
2fb8d4bb665e9a89d3b3478c17f646f8_***_Ivonne Zavala Carrasco
author Ameek Malhotra
Gianmassimo Tasinato
Ivonne Zavala Carrasco
author2 N. M. Jiménez Cruz
Ameek Malhotra
Gianmassimo Tasinato
Ivonne Zavala Carrasco
format Journal article
container_title Physical Review D
container_volume 110
container_issue 6
publishDate 2024
institution Swansea University
issn 2470-0010
2470-0029
doi_str_mv 10.1103/physrevd.110.063526
publisher American Physical Society (APS)
college_str Faculty of Science and Engineering
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hierarchy_top_title Faculty of Science and Engineering
hierarchy_parent_id facultyofscienceandengineering
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department_str School of Biosciences, Geography and Physics - Physics{{{_:::_}}}Faculty of Science and Engineering{{{_:::_}}}School of Biosciences, Geography and Physics - Physics
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description Recent pulsar timing array (PTA) collaborations show strong evidence for a stochastic gravitational wave background (SGWB) with the characteristic Hellings-Downs interpulsar correlations. The signal may stem from supermassive black hole binary mergers, or early Universe phenomena. The former is expected to be strongly anisotropic, while primordial backgrounds are likely to be predominantly isotropic with small fluctuations. In the case the observed SGWB is of cosmological origin, our relative motion with respect to the SGWB rest frame is a guaranteed source of anisotropy, leading to ⁡(10−3) energy density fluctuations of the SGWB. For such cosmological SGWB, kinematic anisotropies are likely to be larger than the intrinsic anisotropies, akin to the cosmic microwave background (CMB) dipole anisotropy. We assess the sensitivity of current PTA data to the kinematic dipole anisotropy, and we also forecast at what extent the magnitude and direction of the kinematic dipole can be measured in the future with an SKA-like experiment. We also discuss how the spectral shape of the SGWB and the location of the pulsars to monitor affect the prospects of detecting the kinematic dipole with PTA. In the future, a detection of this anisotropy may even help resolve the discrepancy in the magnitude of the kinematic dipole as measured by CMB and large-scale structure observations.
published_date 2024-09-11T11:40:42Z
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