Abstract
- Received 30 June 2023
DOI:https://doi.org/10.1103/PhysRevD.108.029901
© 2023 American Physical Society
Physics Subject Headings (PhySH)
Gravitation, Cosmology & Astrophysics
Erratum: Outlook for detecting the gravitational-wave displacement and spin memory effects with current and future gravitational-wave detectors [Phys. Rev. D 107, 064056 (2023)]
Alexander M. Grant and David A. Nichols
Phys. Rev. D 108, 029901 – Published 17 July 2023
Images
Figure 1
A plot comparing the relative error in the SNR computed either from the full waveform or a waveform truncated in length. The specific SNRs that are computed are from the parts of the waveform that are odd under the transformation in Sec. II C, the displacement memory signal, and the spin memory signal.
Reuse & PermissionsFigure 2
The relative error in the SNR vs window length, for just the displacement and spin memory signals, using a window that pads both the beginning and end of the waveform. The error is computed by comparing against a window with a length of 10 s. The SNR is computed in the HLVKI detector at its O5 sensitivity, and for a range of masses between 10 and ; the remaining parameters are the same as in Footnote 13.
Reuse & PermissionsFigure 3
The relative error in the SNR, as a function of the length of the window (as a fraction of the length of the unwindowed waveform), for the odd part of the waveform. The window is applied over both the beginning of the waveform and a padded region at the end of the waveform of the same length. The error is computed by comparing with a window length of 0. As in Fig. 2, the SNR is computed in the HLVKI detector at its O5 sensitivity, for a range of masses between 10 and ; the parameters are the same as in Footnote 13.
Reuse & PermissionsFigure 4
The median accumulated SNR and 68% symmetric credible region for the displacement memory in second-generation detector networks as a function of run time for different realizations of binary-black-hole populations. The blue region corresponds to the O4 HLVK network at design sensitivity for all four detectors, which can be compared with the results of [47]. The orange region instead accounts for an upgrade to the O5 sensitivity of the HLVKI network after 1.5 years, as is currently planned [46], and the green region accounts for the addition of LIGO India after 2.25 years. The red dashed line is an SNR of 3, which corresponds via Eq. (2.12) to a log Bayes factor of 9, which would indicate strong evidence for the hypothesis that there is displacement memory in the population of black-hole mergers.
Reuse & PermissionsFigure 5
The median accumulated SNR and 68% symmetric credible region for the spin memory in the third-generation Cosmic Explorer detectors as a function of run time for different realizations of binary-black-hole populations. The blue and orange regions correspond to two- and three-detector networks, respectively. The green dashed line corresponds to an accumulated SNR of 3 and is reached by the median of the populations for Cosmic Explorer for a three-detector network.
Reuse & PermissionsFigure 6
The median rate of events with an SNR in the displacement memory higher than some given amount, in Cosmic Explorer with either a two- (orange) or three- (blue) detector network. Error bars correspond to the symmetric 68% confidence interval. The green line corresponds to seeing a single event over 5 years.
Reuse & PermissionsFigure 7
A plot of the final accumulated SNR after 0.1 years for a given memory signal in a particular detector network, as a function of redshift cutoff , as a fraction of the SNR computed using a redshift cutoff of .
Reuse & Permissions