Searches for gravitational waves from known pulsars at two harmonics in 2015–2017 LIGO data

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Abbott, B. P. and Angelova, S. V. and Birney, R. and Lockerbie, N. A. and Macfoy, S. and Reid, S., LIGO Scientific Collaboration, Virgo Collaboration (2019) Searches for gravitational waves from known pulsars at two harmonics in 2015–2017 LIGO data. Astrophysical Journal, 879 (1). ISSN 1538-4357 (https://doi.org/10.3847/1538-4357/ab20cb)

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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 1038 kg m2 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.

ORCID iDs

Abbott, B. P., Angelova, S. V., Birney, R., Lockerbie, N. A. ORCID logoORCID: https://orcid.org/0000-0002-1678-3260, Macfoy, S. and Reid, S.;
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