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Impact of spin in compact binary foreground subtraction for estimating the residual stochastic gravitational-wave background in ground-based detectors
Hanlin Song, Dicong Liang, Ziming Wang, and Lijing Shao
Phys. Rev. D 109, 123014 – Published 7 June 2024
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Abstract
Stochastic gravitational-wave (GW) background (SGWB) contains information about the early Universe and astrophysical processes. The recent evidence of SGWB by pulsar timing arrays in the nanohertz band is a breakthrough in the GW astronomy. For ground-based GW detectors, while in data analysis, the SGWB can be masked by loud GW events from compact binary coalescences (CBCs). Assuming a next-generation ground-based GW detector network, we investigate the potential for detecting the astrophysical and cosmological SGWB with non-CBC origins by subtracting recovered foreground signals of loud CBC events. The Fisher Information Matrix (FIM) method is adopted for quick calculation. As an extension of the previous studies, two more essential features are considered. Firstly, we incorporate nonzero aligned or antialigned spin parameters in our waveform model. Because of the inclusion of spins, we obtain significantly more pessimistic results than the previous work, where the residual energy density of foreground is even larger than the original CBC foreground. For the most extreme case, we observe that the subtraction results are approximately 10 times worse for binary black hole events and 20 times worse for binary neutron star events than the scenarios without accounting for spins. The degeneracy between the spin parameters and the symmetric mass ratio is strong in the parameter estimation process, and it contributes most to the imperfect foreground subtraction. Secondly, in this work, extreme CBC events with condition numbers of FIMs are preserved. The impacts of these extreme events on foreground subtraction are discussed. Our results have important implications for assessing the detectability of SGWB from non-CBC origins for ground-based GW detectors.
- Received 1 January 2024
- Accepted 13 May 2024
DOI:https://doi.org/10.1103/PhysRevD.109.123014
© 2024 American Physical Society
Physics Subject Headings (PhySH)
- Research Areas
Gravitational wave detectionGravitational wave sources
- Physical Systems
Binary stars
- Techniques
Data analysis
Gravitation, Cosmology & Astrophysics
Authors & Affiliations
Hanlin Song1, Dicong Liang2,3, Ziming Wang2, and Lijing Shao2,4,*
- 1School of Physics, Peking University, Beijing 100871, China
- 2Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
- 3Department of Mathematics and Physics, School of Biomedical Engineering, Southern Medical University, Guangzhou 510515, China
- 4National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
- *lshao@pku.edu.cn
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Issue
Vol. 109, Iss. 12 — 15 June 2024
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Images
Figure 1
Results from treatment (i) for 9- PE for BBHs (upper left) and BNSs (lower left), and 11- PE for BBHs (upper right) and BNSs (lower right). Each subfigure shows the total GW energy spectrum in black solid line and two components ( and ) of the residual GW energy spectrum for different . (dashed line) comes from the events that are not subtracted while (dash-dotted line) comes from the imperfect subtraction of the CBC foreground. For a direct check, the two panels on the left reproduce the results of Fig.2 in Zhou etal. [44] for the IMRPhenomD waveform.
Figure 3
Subfigure (a)shows number density distribution of the relative ratio and subfigure (b)shows absolute ratio . Both subfigures show results for the BNS 9- PE case with . Plots for events with high/low values (denoted with red/blue color) are shown separately. Three frequency bins are chosen for illustration. The distributions at 10, 100, 200, 400, 800, and 2000Hz have similar features, which are not shown here.
Figure 4
Parameter distributions of events with high and low values in four PE cases. In this figure, we set for BBH cases and for BNS cases. We show three parameters here: chirp mass in the observer frame , symmetric mass ratio , and orbital inclination angle . Red color denotes events with , while gray color denotes events with .
Figure 5
Contribution from each parameter to for BBHs (left panel) and BNSs (right panel). Each subfigure shows from 11- PE results (black solid line) and contribution from each parameter (dashed line). We choose equal to 8 and 12 for BBHs and BNSs respectively.
Figure 6
Subfigure (a)shows the relative ratio and subfigure (b)shows absolute ratio . Both subfigures show results for 9- PE (blue line) and 11- PE (red line) of BBHs. We set and choose three frequency bins to illustrate. The BNS case has a similar feature in our simulation, which is not shown here.
Figure 7
The foreground subtraction results are presented for the main method (from main text) with red color and the supplementary method (from this Appendix) with blue color. The left panels show the results for 9- PE, while the right panels show the results for 11- PE. In the top panels, each subfigure shows the with solid line and with with a dash-dotted line. In the bottom panels, each subfigure shows the results of against .