# All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

Dated: 30 July 2021. Read this summary in PDF format (in English) and in other languages: Japanese .

While our knowledge of the population of
compact binary mergers continues to grow
with already 50
objects released in the GWTC-2 catalog, there remain many other possible sources of
yet-to-be-detected gravitational waves (GWs). As the
worldwide network of GW detectors also increases
to now include LIGO, Virgo,
and KAGRA, the possibilities of finding
GW signals from different astrophysical phenomena continue to grow.
Here we consider
transient gravitational waves on a "long" time scale, i.e., GWs whose energy is spread over seconds to several minutes.
One such source is provided by
compact binary coalescences
with large
eccentricity. The gravitational wave emission from these sources is well understood,
but there are computational difficulties in searching for their signals with template waveforms as is done
for binaries with negligible eccentricity.
There are also less well-understood sources, such as deformations on
magnetar
surfaces and matter
asymmetrically falling into a newborn neutron star.
Detection of gravitational waves from any of these sources would bring deep, new insights into poorly understood phenomena. For example, detection of gravitational waves from magnetars would help constrain the strength and shape of their magnetic field.
Because models that account for all of the important physics of such phenomena are not generally
available for these sources and are at least more uncertain than for compact
binary mergers, the techniques used to search for their signals are designed to operate making minimal or no assumptions. This enables the detection of signals of unknown shapes, required due to the wide range of potential sources, at the cost of less sensitivity to weaker signals. Of course, the possibility of as-yet-unpredicted sources is one of the most exciting.

## The analysis and the results

We search for a range of possible durations and emission frequencies for these long-duration gravitational-wave transients using three different pipelines. Using multiple pipelines has many benefits: (1) it provides robustness against noise glitches of instrumental or environmental origin that mimic the characteristics of the targeted signals (non-Gaussian transient noise events), as each pipeline has an independent treatment of such noise features and (2) different possible models/signal shapes are covered with different effectiveness by different pipelines and pipeline sensitivities to both astrophysical and "ad-hoc" models can be compared to identify the possible limits of each of them. Ad-hoc models considered include white noise band-limited (WNB) and sine-Gaussian (SG) signals. We also use astrophysical models for the possible signals emitted by a variety of objects. These include magnetars formed in a binary neutron star merger (Magnetar), black hole accretion disk instabilities (ADI), newly formed magnetars powering a gamma-ray burst plateau (where X-rays produced by the gamma-ray burst afterglow show a phase where the X-rays do not decay; GRBplateau), eccentric compact binary coalescence waveforms (ECBC), and broadband chirps from the accretion around rotating black holes within the innermost stable circular orbit (ISCOchirp). We considered different masses and eccentricities for the ECBC waveforms, different masses of the central black hole for ISCOchirp waveforms, and rotational frequencies and ellipticities of the magnetar due to its magnetic deformations for the Magnetar waveform. The durations of these signals vary from 6 s (ADI-B) to 470 s (GRBplateau), and their time-frequency spectrograms are shown in Figure 1.

None of the pipelines found any significant events coincident in both the Hanford and Livingston detectors. The loudest events in the 204 days of data when both detectors were operating are consistent with being noise. The Virgo detector did not contribute to this search due to its relatively lower sensitivity during the third observing period O3 (see Figure 2), but we expect it to be included during the next observation period, O4.

Given the absence of a detection, we derive upper limits on the gravitational-wave amplitude of long-duration gravitational-wave transients corresponding to the considered reference signal, using the results from the pipeline that is most sensitive to each model. We also set limits on the rates of the eccentric binary coalescences occurring in the Universe (see Figure 3). The limits we set are improved by about a factor of 2 over the last analysis. While detection would be preferred, the upper limits still inform us of the possible rates for these exotic systems. We look forward to O4 to find new astrophysical sources of gravitational waves.

## Find Out More:

- Visit our websites:
- Read a free preprint of the full scientific article. also available on arXiv.org.
- science summary for the observing period O1 (2017) version of the search
- science summary for the observing period O2 (2019) version of the search

## Glossary

**Accretion disk**: Mass of material (in the form of a disk) in orbital motion that slowly inspirals toward a massive central body.**Ad-hoc models**: Non-physical waveforms used solely to characterize pipeline capabilities and sensitivity.**Band-limiting**: The limiting of a signal's spread in the frequency domain.**Compact binary coalescence**: The merger of two dense, compact objects like neutron stars and black holes orbiting around each other.**Confidence level**: The percentage of the time the true value is expected to be contained within the quoted range.**Eccentricity**: A parameter that defines the amount an orbit deviates from a perfect circle.**Magnetar**: A type of neutron star with an extremely powerful magnetic field.**Megaparsec**: A megaparsec is a unit of length to measure distances to astronomical objects. A parsec is approximately equal to 3.26 light-years or 19.2 trillion miles, and a megaparsec is a million parsecs.**Neutron star**: Collapsed core of a dead star; they are typically around 1.4 times the mass of our Sun but only about 20 km across, making them incredibly dense.**Non-Gaussian**: A process that deviates from Normal (Gaussian) distributions; in the case of gravitational-wave detectors, the data generally follows Gaussian distributions with sharp deviations due to environmental and instrumental effects.**Pipeline**: Algorithm used to search for gravitational-wave candidates.**Strain**: Dimensionless relative change in length (e.g., of the arm of a gravitational-wave detector) due to gravitational waves.**Transient**: Astronomical phenomenon of short timescales; in contrast to astrophysical events lasting from thousands to billions of years.

## Figures from the Publication

For more information on these figures and how they were produced, read the freely available preprint. You can click on each figure for a bigger version.

**Figure 1:** Time-frequency spectrogram of the reference waveforms used in this search (see main text). They cover signals with a
durations range from 6 s (ADI-B) to 470 s (GRBplateau).

**Figure 2:** The GW root-sum-square strain amplitude (where the square root of the sum of squared amplitudes at different times is taken) versus mean frequency at 50%
detection efficiency and a false alarm rate of 1/(50 years). The red, green, and blue
curves are the averaged amplitude spectral noise densities for Hanford (H1),
Livingston (L1), and Virgo (V1) detectors to show that the search results follow
the detectors' sensitivity at different frequencies. The dashed lines show the h_{rss}, as a function of the frequency, associated with the conversion in GW of the energy equivalent to 1/100 of a solar mass (M_{⊙}) at different distances in megaparsecs (Mpc).

**Figure 3:** Upper limits at 90% confidence level on the
rate of eccentric compact binary coalescences as a function
of the distance. Only the best result is shown for each
waveform. The inset shows the ratio of the rates with
respect to O2 results for ECBC A to ECBC F.