Recent searches for continuous gravitational waves

Riles, K.

doi:10.1142/s021773231730035x

Cited by 151 publications

(142 citation statements)

References 432 publications

(742 reference statements)

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“…The canonical sources for CWs (see [3] for a review) are non-axisymmetric rotating neutron stars, emitting long-lasting and nearly monochromatic waves. When observed from Earth, these waves will be frequency modulated due to the Doppler effect produced by the daily rotation and orbital motion of the Earth around the Sun.…”

Section: Introductionmentioning

confidence: 99%

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Covas¹,

Effler²,

Goetz³

et al. 2018

Phys. Rev. D

142

157

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Searches are under way in Advanced LIGO and Virgo data for persistent gravitational waves from continuous sources, e.g. rapidly rotating galactic neutron stars, and stochastic sources, e.g. relic gravitational waves from the Big Bang or superposition of distant astrophysical events such as mergers of black holes or neutron stars. These searches can be degraded by the presence of narrow spectral artifacts (lines) due to instrumental or environmental disturbances. We describe a variety of methods used for finding, identifying and mitigating these artifacts, illustrated with particular examples. Results are provided in the form of lists of line artifacts that can safely be treated as non-astrophysical. Such lists are used to improve the efficiencies and sensitivities of continuous and stochastic gravitational wave searches by allowing vetoes of false outliers and permitting data cleaning.

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Section: Introductionmentioning

confidence: 99%

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Covas¹,

Effler²,

Goetz³

et al. 2018

Phys. Rev. D

142

157

View full text Add to dashboard Cite

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“…Another more exotic source of CWs are ultra-light bosons clouds orbiting BHs [4]. A comprehensive review of potential CW sources can be found in [5].…”

Section: Introductionmentioning

confidence: 99%

“…where I zz is the star moment of inertia around the rotation axis (z-axis) while = Ixx−Iyy Izz is the ellipticity. To date several CW investigations took place and, although no signal has been detected so far, stringent upper limits on the GW amplitude have been placed [5]. Each search uses a different method and is dependent on the parameter space investigated.…”

Section: Introductionmentioning

confidence: 99%

Directed search for continuous gravitational-wave signals from the Galactic Center in the Advanced LIGO second observing run

et al. 2020

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In this work we present the results of a search for continuous gravitational waves from the Galactic Center using LIGO O2 data. The search uses the Band-Sampled-Data directed search pipeline, which performs a semi-coherent wide-parameter-space search, exploiting the robustness of the Frequency-Hough transform algorithm. The search targets signals emitted by isolated asymmetric spinning neutron stars, located within the few inner parsecs of the Galactic Center. The frequencies covered in this search range between 10 Hz and 710 Hz with a spin-down range from −1.8 × 10 −9 Hz/s to 3.7 × 10 −11 Hz/s. No continuous wave signal has been detected and upper limits on the gravitational wave amplitude are presented. The most stringent upper limit at 95% confidence level, for Livingston detector, is ∼ 1.4 × 10 −25 at 163 Hz. To date, this is the most sensitive directed search for continuous gravitational-wave signals from the Galactic Center and the first search of this kind using LIGO second observing run.

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“…Rotating NSs are potential sources of high-frequency CWs [24,25]; a NS with a non-zero quadrupolar moment is expected to emit GWs at a frequency f GW = 2ν, where ν is the rotational frequency of the NS [26]. For known pulsars with measured time derivatives, a rough upper limit on the strength of emitted GWs can be obtained by assuming its spin-down is solely due to energy emitted in GWs.…”

Section: Continuous Gws or Compact Binary Coalescencesmentioning

confidence: 99%

Eclipses of continuous gravitational waves as a probe of stellar structure

et al. 2020

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Although gravitational waves only interact weakly with matter, their propagation is affected by a gravitational potential. If a gravitational wave source is eclipsed by a star, measuring these perturbations provides a way to directly measure the distribution of mass throughout the stellar interior. We compute the expected Shapiro time delay, amplification and deflection during an eclipse, and show how this can be used to infer the mass distribution of the eclipsing body. We identify continuous gravitational waves from neutron stars as the best candidates to detect this effect. When the Sun eclipses a far-away source, depending on the depth of the eclipse the timedelay can change by up to ∼ 0.034 ms, the gravitational-wave strain amplitude can increase by ∼ 4%, and the apparent position of the source in the sky can vary by 4 . Accreting neutron stars with Roche-lobe filling companion stars have a high probability of exhibiting eclipses, producing similar time delays but undetectable changes in amplitude and sky location. Even for the most rapidly rotating neutron stars, this time delay only corresponds to a few percent of the phase of the gravitational wave, making it an extremely challenging measurement. However, if sources of continuous gravitational waves exist just below the limit of detection of current observatories, nextgeneration instruments will be able to observe them with enough precision to measure the signal of an eclipsing star. Detecting this effect would provide a new direct probe to the interior of stars, complementing asteroseismology and the detection of solar neutrinos.

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Recent searches for continuous gravitational waves

Cited by 151 publications

References 432 publications

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Identification and mitigation of narrow spectral artifacts that degrade searches for persistent gravitational waves in the first two observing runs of Advanced LIGO

Directed search for continuous gravitational-wave signals from the Galactic Center in the Advanced LIGO second observing run

Eclipses of continuous gravitational waves as a probe of stellar structure

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