Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published December 15, 2017 | Submitted + Published
Journal Article Open

First narrow-band search for continuous gravitational waves from known pulsars in advanced detector data

Abstract

Spinning neutron stars asymmetric with respect to their rotation axis are potential sources of continuous gravitational waves for ground-based interferometric detectors. In the case of known pulsars a fully coherent search, based on matched filtering, which uses the position and rotational parameters obtained from electromagnetic observations, can be carried out. Matched filtering maximizes the signal-to-noise (SNR) ratio, but a large sensitivity loss is expected in case of even a very small mismatch between the assumed and the true signal parameters. For this reason, narrow-band analysis methods have been developed, allowing a fully coherent search for gravitational waves from known pulsars over a fraction of a hertz and several spin-down values. In this paper we describe a narrow-band search of 11 pulsars using data from Advanced LIGO's first observing run. Although we have found several initial outliers, further studies show no significant evidence for the presence of a gravitational wave signal. Finally, we have placed upper limits on the signal strain amplitude lower than the spin-down limit for 5 of the 11 targets over the bands searched; in the case of J1813-1749 the spin-down limit has been beaten for the first time. For an additional 3 targets, the median upper limit across the search bands is below the spin-down limit. This is the most sensitive narrow-band search for continuous gravitational waves carried out so far.

Additional Information

© 2017 American Physical Society. Received 6 October 2017; published 28 December 2017. 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); 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); 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 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 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, Innovations, and Communications; International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR); Russian Foundation for Basic Research; Research Grants Council of Hong Kong; the Leverhulme Trust, the Research Corporation; 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. Pulsar observations with the Lovell telescope and their analyses are supported through a consolidated grant from the STFC in the U.K. The Nançay Radio Observatory is operated by the Paris Observatory, associated with the French CNRS.

Attached Files

Published - PhysRevD.96.122006.pdf

Submitted - 1710.02327.pdf

Files

PhysRevD.96.122006.pdf
Files (2.9 MB)
Name Size Download all
md5:22e494af1a061f9d0515ab45f3adbf4f
1.3 MB Preview Download
md5:c2ba5cda9649d88fa2dd603de7179a86
1.6 MB Preview Download

Additional details

Created:
August 19, 2023
Modified:
October 18, 2023