Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run
Name
PhysRevD.99.122002.pdf
Description
Published version
Size
1.27 MB
Format
Unknown
Checksum (MD5)
f5566f905c08eeabc46fbb582ddb790b
Author(s)
LIGO Scientific Collaboration
Virgo Collaboration
Aggarwal, Nancy
Barnum, Sam
Barsotti, Lisa
Biscans, Sebastien
Buikema, Aaron
Demos, Nicholas
Donovan, Frederick J
Eisenstein, Robert Alan
Date Issued
2019
Journal
Physical Review D
Publisher
American Physical Society (APS)
Version
Final published version
Abstract
© 2019 us. American Physical Society. American Physical Society. Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrow-band algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400-6325, J1813-1246, J1833-1034, J1952+3252, and for new targets such as J0940-5428 and J1747-2809. For J1400-6325, J1833-1034, and J1747-2809, this is the first time the spin-down limit is surpassed.
MIT Department
LIGO (Observatory : Massachusetts Institute of Technology)
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1103/PHYSREVD.99.122002
