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Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data

Abbott, B. P. and Abbott, R. and Adhikari, R. X. and Ananyeva, A. and Anderson, S. B. and Appert, S. and Arai, K. and Araya, M. C. and Barayoga, J. C. and Barish, B. C. and Billingsley, G. and Biscans, S and Blackburn, J. K. and Bork, R. and Brooks, A. F. and Brunett, S. and Cahillane, C. and Callister, T. A. and Coughlin, M. W. and Couvares, P. and Coyne, D. C. and Ehrens, P. and Eichholz, J. and Etzel, T. and Feicht, J. and Gossan, S. E. and Grassia, P. and Gustafson, E. K. and Heptonstall, A. W. and Hulko, M. and Isi, M. and Kamai, B. and Kanner, J. B. and Kasprzack, M. and Kondrashov, V. and Korth, W. Z. and Kozak, D. B. and Lazzarini, A. and Lo, R. K. L. and Markowitz, A. and Maros, E. and Massinger, T. J. and Matichard, F. and McIver, J. and Meshkov, S. and Pedraza, M. and Quintero, E. A. and Reitze, D. H. and Richardson, J. W. and Robertson, N. A. and Rollins, J. G. and Sachdev, S. and Sanchez, E. J. and Sanchez, L. E. and Sun, L. and Taylor, R. and Torrie, C. I. and Trudeau, R. and Vajente, G. and Vass, S. and Venugopalan, G. and Wade, A. R. and Wallace, L. and Weinstein, A. J. and Willis, J. L. and Wipf, C. C. and Xiao, L. and Yamamoto, H. and Zhang, L. and Zucker, M. E. and Zweizig, J. and Barkett, K. and Chen, Y. and Li, X. and Ma, Y. and Pang, B. and Scheel, M. and Tso, R. and Varma, V. (2019) Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data. Astrophysical Journal, 879 (1). Art. No. 10. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20190503-131615500

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Abstract

We present a search for gravitational waves from 222 pulsars with rotation frequencies ≳10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015–2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711−6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 10^(38) kg m^2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2 × 10^(−8). We also place new limits on the emission amplitude at the rotation frequency of the pulsars.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ab20cbDOIArticle
https://arxiv.org/abs/1902.08507arXivDiscussion Paper
ORCID:
AuthorORCID
Adhikari, R. X.0000-0002-5731-5076
Arai, K.0000-0001-8916-8915
Billingsley, G.0000-0002-4141-2744
Blackburn, J. K.0000-0002-3838-2986
Callister, T. A.0000-0001-9892-177X
Isi, M.0000-0001-8830-8672
Kamai, B.0000-0001-6521-9351
Kanner, J. B.0000-0001-8115-0577
Korth, W. Z.0000-0003-3527-1348
Kozak, D. B.0000-0003-3118-8950
Massinger, T. J.0000-0002-3429-5025
Weinstein, A. J.0000-0002-0928-6784
Xiao, L.0000-0003-2703-449X
Zucker, M. E.0000-0002-2544-1596
Zweizig, J.0000-0002-1521-3397
Pang, B.0000-0002-5697-2162
Additional Information:© 2019 The American Astronomical Society. Received 2019 March 18; revised 2019 May 7; accepted 2019 May 8; published 2019 June 26. 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, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d'Innovació Recerca i Turisme and the Conselleria d'Educació i Universitat del Govern de les Illes Balears, the Conselleria d'Educació Investigació Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), 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, Development and Innovation Office Hungary (NKFI), 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, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources. The Nançay Radio Observatory is operated by the Paris Observatory, associated with the French CNRS. We acknowledge financial support from the "Programme National Gravitation, Références, Astronomie, Métrologie (PNGRAM) and "Programme National Hautes Énergies (PNHE) of CNRS/INSU, France. Work at the Naval Research Laboratory is supported by NASA. We gratefully acknowledge the continuing contributions of the NICER science team in providing up-to-date spin ephemerides for X-ray-bright pulsars of interest to the LVC. NICER is a 0.2–12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA. This work has been assigned LIGO document number LIGO-P1800344. Facilities: Arecibo - Arecibo observatory, Fermi - , LIGO - , Lovell - , Molonglo Observatory - , MtPO:26 m - , NICER - , NRT - , Parkes. - Software: Much of the analysis described in the paper was performed using the publicly available LALSuite library (LIGO Scientific Collaboration 2018). Production of many of the pulsar timing ephemerides used in this analysis was performed with Tempo206 and Tempo2 (Hobbs et al. 2006b). Figures in this publication have be produced using Matplotlib (Hunter 2007).
Group:LIGO
Funders:
Funding AgencyGrant Number
NSFUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Max-Planck-SocietyUNSPECIFIED
State of Niedersachsen/GermanyUNSPECIFIED
Australian Research CouncilUNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Stichting voor Fundamenteel Onderzoek der Materie (FOM)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Council of Scientific and Industrial Research (India)UNSPECIFIED
Department of Science and Technology (India)UNSPECIFIED
Science and Engineering Research Board (SERB)UNSPECIFIED
Ministry of Human Resource Development (India)UNSPECIFIED
Agencia Estatal de InvestigaciónUNSPECIFIED
Vicepresidència i Conselleria d'Innovació, Recerca i TurismeUNSPECIFIED
Conselleria d'Educació i Universitat del Govern de les Illes BalearsUNSPECIFIED
Conselleria d'Educació, Investigació, Cultura i Esport de la Generalitat ValencianaUNSPECIFIED
National Science Centre (Poland)UNSPECIFIED
Swiss National Science Foundation (SNSF)UNSPECIFIED
Russian Foundation for Basic ResearchUNSPECIFIED
Russian Science FoundationUNSPECIFIED
European CommissionUNSPECIFIED
European Regional Development Funds (ERDF)UNSPECIFIED
Royal SocietyUNSPECIFIED
Scottish Funding CouncilUNSPECIFIED
Scottish Universities Physics AllianceUNSPECIFIED
Hungarian Scientific Research Fund (OTKA)UNSPECIFIED
Lyon Institute of Origins (LIO)UNSPECIFIED
Paris Île-de-France RegionUNSPECIFIED
National Research, Development and Innovation Fund (NKFIA)UNSPECIFIED
National Research Foundation of KoreaUNSPECIFIED
Industry CanadaUNSPECIFIED
Ontario Ministry of Economic Development and InnovationUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC)UNSPECIFIED
International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)UNSPECIFIED
Research Grants Council of Hong KongUNSPECIFIED
National Natural Science Foundation of ChinaUNSPECIFIED
Leverhulme TrustUNSPECIFIED
Research CorporationUNSPECIFIED
Ministry of Science and Technology (Taipei)UNSPECIFIED
Kavli FoundationUNSPECIFIED
Subject Keywords:pulsars: general - stars: neutron - gravitational waves
Other Numbering System:
Other Numbering System NameOther Numbering System ID
LIGO DocumentP1800344
Record Number:CaltechAUTHORS:20190503-131615500
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190503-131615500
Official Citation:B. P. Abbott et al 2019 ApJ 879 10
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:95209
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 May 2019 21:22
Last Modified:26 Jun 2019 16:54

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