The GW morphologies used to quantify the search sensitivity. The first column shows the waveforms used. The second and third columns show the hrss values at which |$50\%$| and |$90\%$| detection efficiencies are achieved at an iFAR of 1 year. For the astrophysical waveforms the second and third columns show the luminosity distance at which these efficiencies are achieved.
| Morphology . | 50% . | 90% . |
|---|---|---|
| Gaussian pulses (linear) | hrss (|$10^{-20}\, \text{Hz}^{-1/2 }$|) | |
| τ = 0.1 ms | 5.3 | N/A |
| τ = 2.5 ms | 15.0 | N/A |
| sine–Gaussian wavelets (circular) | ||
| f0 = 100 Hz, Q = 9 | 4.9 | 11.0 |
| f0 = 235 Hz, Q = 9 | 1.0 | 1.9 |
| f0 = 361 Hz, Q = 9 | 0.9 | 1.7 |
| sine–Gaussian wavelets (elliptical) | ||
| f0 = 70 Hz, Q = 3 | 28.0 | 94.0 |
| f0 = 153 Hz, Q = 9.0 | 4.0 | 14.0 |
| f0 = 235 Hz, Q = 100 | 1.4 | 4.7 |
| f0 = 554 Hz, Q = 9.0 | 1.5 | 4.3 |
| f0 = 849 Hz, Q = 3 | 3.5 | 12.0 |
| White-noise bursts | ||
| flow = 150 Hz, Δf = 100 Hz, τ = 0.1 s | 1.9 | N/A |
| flow = 300 Hz, Δf = 100 Hz, τ = 0.1 s | 1.1 | N/A |
| flow = 700 Hz, Δf = 100 Hz, τ = 0.1 s | 1.2 | N/A |
| Astrophysical signals | distance (kpc) | |
| GW150914 | 809 | N/A |
| Supernova SFHx | 0.08 | 0.01 |
| Morphology . | 50% . | 90% . |
|---|---|---|
| Gaussian pulses (linear) | hrss (|$10^{-20}\, \text{Hz}^{-1/2 }$|) | |
| τ = 0.1 ms | 5.3 | N/A |
| τ = 2.5 ms | 15.0 | N/A |
| sine–Gaussian wavelets (circular) | ||
| f0 = 100 Hz, Q = 9 | 4.9 | 11.0 |
| f0 = 235 Hz, Q = 9 | 1.0 | 1.9 |
| f0 = 361 Hz, Q = 9 | 0.9 | 1.7 |
| sine–Gaussian wavelets (elliptical) | ||
| f0 = 70 Hz, Q = 3 | 28.0 | 94.0 |
| f0 = 153 Hz, Q = 9.0 | 4.0 | 14.0 |
| f0 = 235 Hz, Q = 100 | 1.4 | 4.7 |
| f0 = 554 Hz, Q = 9.0 | 1.5 | 4.3 |
| f0 = 849 Hz, Q = 3 | 3.5 | 12.0 |
| White-noise bursts | ||
| flow = 150 Hz, Δf = 100 Hz, τ = 0.1 s | 1.9 | N/A |
| flow = 300 Hz, Δf = 100 Hz, τ = 0.1 s | 1.1 | N/A |
| flow = 700 Hz, Δf = 100 Hz, τ = 0.1 s | 1.2 | N/A |
| Astrophysical signals | distance (kpc) | |
| GW150914 | 809 | N/A |
| Supernova SFHx | 0.08 | 0.01 |
The GW morphologies used to quantify the search sensitivity. The first column shows the waveforms used. The second and third columns show the hrss values at which |$50\%$| and |$90\%$| detection efficiencies are achieved at an iFAR of 1 year. For the astrophysical waveforms the second and third columns show the luminosity distance at which these efficiencies are achieved.
| Morphology . | 50% . | 90% . |
|---|---|---|
| Gaussian pulses (linear) | hrss (|$10^{-20}\, \text{Hz}^{-1/2 }$|) | |
| τ = 0.1 ms | 5.3 | N/A |
| τ = 2.5 ms | 15.0 | N/A |
| sine–Gaussian wavelets (circular) | ||
| f0 = 100 Hz, Q = 9 | 4.9 | 11.0 |
| f0 = 235 Hz, Q = 9 | 1.0 | 1.9 |
| f0 = 361 Hz, Q = 9 | 0.9 | 1.7 |
| sine–Gaussian wavelets (elliptical) | ||
| f0 = 70 Hz, Q = 3 | 28.0 | 94.0 |
| f0 = 153 Hz, Q = 9.0 | 4.0 | 14.0 |
| f0 = 235 Hz, Q = 100 | 1.4 | 4.7 |
| f0 = 554 Hz, Q = 9.0 | 1.5 | 4.3 |
| f0 = 849 Hz, Q = 3 | 3.5 | 12.0 |
| White-noise bursts | ||
| flow = 150 Hz, Δf = 100 Hz, τ = 0.1 s | 1.9 | N/A |
| flow = 300 Hz, Δf = 100 Hz, τ = 0.1 s | 1.1 | N/A |
| flow = 700 Hz, Δf = 100 Hz, τ = 0.1 s | 1.2 | N/A |
| Astrophysical signals | distance (kpc) | |
| GW150914 | 809 | N/A |
| Supernova SFHx | 0.08 | 0.01 |
| Morphology . | 50% . | 90% . |
|---|---|---|
| Gaussian pulses (linear) | hrss (|$10^{-20}\, \text{Hz}^{-1/2 }$|) | |
| τ = 0.1 ms | 5.3 | N/A |
| τ = 2.5 ms | 15.0 | N/A |
| sine–Gaussian wavelets (circular) | ||
| f0 = 100 Hz, Q = 9 | 4.9 | 11.0 |
| f0 = 235 Hz, Q = 9 | 1.0 | 1.9 |
| f0 = 361 Hz, Q = 9 | 0.9 | 1.7 |
| sine–Gaussian wavelets (elliptical) | ||
| f0 = 70 Hz, Q = 3 | 28.0 | 94.0 |
| f0 = 153 Hz, Q = 9.0 | 4.0 | 14.0 |
| f0 = 235 Hz, Q = 100 | 1.4 | 4.7 |
| f0 = 554 Hz, Q = 9.0 | 1.5 | 4.3 |
| f0 = 849 Hz, Q = 3 | 3.5 | 12.0 |
| White-noise bursts | ||
| flow = 150 Hz, Δf = 100 Hz, τ = 0.1 s | 1.9 | N/A |
| flow = 300 Hz, Δf = 100 Hz, τ = 0.1 s | 1.1 | N/A |
| flow = 700 Hz, Δf = 100 Hz, τ = 0.1 s | 1.2 | N/A |
| Astrophysical signals | distance (kpc) | |
| GW150914 | 809 | N/A |
| Supernova SFHx | 0.08 | 0.01 |
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