File:GW170814 signal.png
Summary
| Description |
English: Top row: Signal-to-noise ratio as a function of time. The peaks occur at different times in different detectors because gravitational waves propagate at the finite speed of light; this causes the signal to reach the detectors at different times. GW170814 arrived first in LIGO-Livingston, then 8 ms later in LIGO-Hanford and 6 ms after that in Virgo.
Middle row: Time-frequency representation of the strain data. The brighter a given pixel in any of the three 2D-maps, the larger the signal at this particular time and frequency with respect to the expected noise level. Note the characteristic "chirp" pattern of increasing frequency with time. Bottom row: Strain time series with the best waveforms selected by the matched filtering (black solid curves) and unmodeled search methods (gray bands) superimposed. |
| Date | |
| Source | https://doi.org/10.1103/PhysRevLett.119.141101 (GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence, Abbott et al., Physical Review Letters)Category:PNG created with Matplotlib#GW170814%20signal.png |
| Author | LIGO Scientific Collaboration and Virgo Collaboration |
| Other versions |
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