First search for gravitational waves from known pulsars with Advanced LIGO
By The Ligo Scientific Collaboration, T. Abbott, R. Abbott, T. Abbott, M. Abernathy, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso and 993 more. 2017
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We present the result of searches for gravitational waves from 200 pulsars using data from the first observing run of the Advanced LIGO detectors. We find no significant evidence for a gravitational-wave signal from any of these pulsars, but we are able to set the most constraining upper limits yet on their gravitational-wave amplitudes and ellipticities. For eight of these pulsars, our upper limits give bounds that are improvements over the indirect spin-down limit values. For another 32, we are within a factor of 10 of the spin-down limit, and it is likely that some of these will be reachable in future runs of the advanced detector. Taken as a whole, these new results improve on previous limits by more than a factor of two.
Subfields: Astronomy and Astrophysics, Oceanography
View Paper: https://www.semanticscholar.org/paper/0ab740ddbafd230b6f241c295fb4dc503bb4d0cd
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Citations in the corpus
- Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions (2017, background): “…new era, the Laser Interferometer Gravitational-Wave Observatory (LIGO) has demonstrated the existence of binary stellar-mass black hole systems (Abbott et al. 2016a, 2016b, 2016c, 2017a, 2017b) and continues to monitor the sky with broadband detectors for gravitational waves from compact…”
- Black hole and neutron star mergers in galactic nuclei (2018, background): “However, if the merger event drives a relativistic jet as evinced by the observations of GW170817/GRB170817A (Abbott et al. 2017) and detailed broadband modeling (Lazzati et al. 2018), then the density n of the medium in which the event occurs also plays an important role.”
- An introduction to Bayesian inference in gravitational-wave astronomy: Parameter estimation, model selection, and hierarchical models (2018, unknown): “Having defined this frame, we may rotate the binary by the phase of coalescence φ c in order to change the phase of the signal observed at Earth. u We emphasise that the phase at coalescence is distinct from φ , the azimuthal angle to the observer in the source frame, which transforms differently: Th”