Abstract
We present results from the first directed search for nontensorial gravitational waves. While general relativity allows for tensorial (plus and cross) modes only, a generic metric theory may, in principle, predict waves with up to six different polarizations. This analysis is sensitive to continuous signals of scalar, vector, or tensor polarizations, and does not rely on any specific theory of gravity. After searching data from the first observation run of the advanced LIGO detectors for signals at twice the rotational frequency of 200 known pulsars, we find no evidence of gravitational waves of any polarization. We report the first upper limits for scalar and vector strains, finding values comparable in magnitude to previously published limits for tensor strain. Our results may be translated into constraints on specific alternative theories of gravity.
Original language | English |
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Article number | 031104 |
Journal | Physical Review Letters |
Volume | 120 |
Issue number | 3 |
DOIs | |
Publication status | Published - 19 Jan 2018 |
Funding
We have presented the results of the first direct search for nontensorial gravitational waves. This is also the first search targeted at known pulsars that is sensitive to any of the five measurable polarizations of the gravitational perturbation allowed by a generic metric theory of gravity. From the analysis of O1 data from both aLIGO observatories, we have found no evidence of signals from any of the 200 pulsars targeted. In the absence of a clear signal, we have produced the first direct upper limits for scalar and vector strains (Fig. 4 , and tables in the Supplemental Material [45] ). The values of the 95%-credible upper limits are comparable in magnitude to previously published GR constraints, reaching h ∼ 1.5 × 10 - 26 for pulsars whose frequency is in the most sensitive band of our instruments. This means that, to 95% credibility, none of the pulsars in our set is emitting gravitational waves (tensorial or otherwise) at the frequencies analyzed with enough power for them to reach Earth with amplitudes larger than our upper limits. Our results have been obtained in a theory-independent fashion. However, our upper limits on nontensorial strain can be translated into model-dependent constraints on beyond-GR theories by picking a specific alternative theory and emission mechanism. To do so, one should use the upper limits produced under the assumption of a signal model that incorporates the same polarizations allowed by the theory one wishes to constrain; these may not necessarily be those in Fig. 4 (e.g., for limits on a scalar-tensor theory, one needs upper limits from H s t ). However, this also requires nontrivial knowledge of the dynamics of spinning neutron stars under the theory of interest. While it is conventional to compare the sensitivity of continuous wave searches to the canonical spin-down limit for each pulsar, it is not possible to do so here without committing to a specific theory of gravity. This is because doing so would require specific knowledge of how each polarization contributes to the effective gravitational-wave stress energy, how matter couples to the gravitational field, how the waves propagate (dispersion and dissipation), and what the angular dependence of the emission pattern is. However, analogs of the canonical spin-down limit for specific theories may be obtained from the results presented here by using the strain upper limits obtained assuming the sub-hypotheses with polarizations corresponding to that theory, as mentioned above. We have demonstrated the robustness of searches for generalized polarization states (tensor, vector, or scalar) in gravitational waves from spinning neutron stars. Furthermore, even in the absence of a detection, we were able to obtain novel constraints on the strain amplitude of nontensorial polarizations. In the future, once a signal is detected, similar methods will allow us to characterize the gravitational polarization content and, in so doing, perform novel tests of general relativity. Although this search assumed an emission frequency of twice the rotational frequency of the source, this restriction will be relaxed in future analyses. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen, Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Economía y Competitividad, the Conselleria d’Economia i Competitivitat and Conselleria d’Educació, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Fundaçao de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. 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Funders | Funder number |
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Brazilian Ministry of Science, Technology, and Innovation | |
Department of Science and Technology, India, Science & Engineering Research Board | |
National Research Foundation of Korea, Industry Canada | |
National Science Centre of Poland | |
Natural Science and Engineering Research Council Canada | |
National Science Foundation | |
Directorate for Mathematical and Physical Sciences | |
Division of Human Resource Development | |
Kavli Foundation | |
Canadian Institute for Advanced Research | |
Centre Eau Terre Environnement, Institut National de la Recherche Scientifique | |
Ontario Ministry of Economic Development and Innovation | |
Science and Technology Facilities Council | |
Leverhulme Trust | |
Royal Society | |
Scottish Funding Council | |
Scottish Universities Physics Alliance | |
European Commission | |
Australian Research Council | |
Council of Scientific and Industrial Research, India | |
Fundação de Amparo à Pesquisa do Estado de São Paulo | |
Science and Engineering Research Board | |
Russian Foundation for Basic Research | |
Nederlandse Organisatie voor Wetenschappelijk Onderzoek | |
Ministerio de Economía y Competitividad | |
Hungarian Scientific Research Fund | |
Instituto Nazionale di Fisica Nucleare | |
Centre National de la Recherche Scientifique | |
Ministerio de Ciencia y Tecnología | |
Universitat de les Illes Balears | |
Istituto Nazionale di Fisica Nucleare |