Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals

Chen, Zhiwei; Lu, Youjun; Zhao, Yuetong

doi:10.3847/1538-4357/ac98b7

Cited by 10 publications

(12 citation statements)

References 105 publications

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“…The uncertainty here is due to the uncertainties of the local merger rate densities, while the prediction rate adopts the median value respectively. For comparison, we also list the results of sBBHs originating from the EMBS channel, using the same Monte Carlo procedures and a simple recipe for merger rate density analogous to that in Cao et al (2017) and Chen et al (2022).…”

Section: Resultsmentioning

confidence: 99%

“…Once the corresponding lensed host galaxies could be observed at the same time, it is possible to locate the relative positions of sBBHs in host galaxies by mapping time delay and magnification factors (e.g., Hannuksela et al 2020;Chen et al 2022;Wempe et al 2022), which provide a new probe to understand the origin of sBBHs according to their spatial distributions in host galaxies. Thus, it is crucial to study the detectability of both of these lensed events.…”

Section: Discussionmentioning

confidence: 99%

“…Thus, it is crucial to study the detectability of both of these lensed events. With the same settings analogous to those used in Chen et al (2022), one can multiply the detection rate of lensed sBBHs proposed in this paper to estimate the detection rate of both lensed events produced by dynamical channels with future sky surveys. That is 0.8 yr…”

Section: Discussionmentioning

confidence: 99%

“…In this paper, we estimate the detection number per year of lensed sBBHs originating from dynamical interactions in dense clusters with third-generation detectors and their networks, i.e., ET 3 and CE, 4 by adopting SIE (singular isothermal ellipsoid) + external shear model (e.g., Kochanek 1991;Witt & Mao 1997;Keeton & Kochanek 1998) as the lens model and applying more realistic templates (e.g., Biwer et al 2019;Khan et al 2019) to generate GW waveforms rather than the approach developed by Finn (1996). We then show that by multiplying the detection fraction proposed in Chen et al (2022), the detection rate of lensed sBBH having identifiable lensed host galaxies can be different for those produced by the dynamical channel and the EMBS channel, which may offer an opportunity to constrain the origin of sBBH mergers.…”

Section: Introductionmentioning

confidence: 98%

“…As shown in Chen et al (2022), the detection fraction of the host galaxies to the lensed GW events can be different if the sBBHs originated from different formation mechanisms. The fraction is ∼20% assuming an optimistic limiting magnitude for the evolution of massive binary stars (hereafter denoted as the EMBS channel, e.g., Belczynski et al 2016;Giacobbo & Mapelli 2018.…”

Section: Introductionmentioning

confidence: 99%

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Event Rate of Strongly Lensed Gravitational Waves of Stellar Binary Black Hole Mergers Produced by Dynamical Interactions

Chen

2023

ApJ

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Gravitational waves emitted from stellar binary black hole (sBBH) mergers can be gravitationally lensed by intervening galaxies and detected by future ground-based detectors. A great amount of effort has been put into the estimation of the detection rate of lensed sBBH originating from the evolution of massive binary stars (EMBS channel). However, sBBHs produced by the dynamical interaction in dense clusters (dynamical channel) may also be dominant in our universe and their intrinsic distribution of physical properties can be significantly different from those produced by massive stars, especially mass and redshift distribution. In this paper, we investigate the event rate of lensed sBBHs produced via the dynamical channel by Monte Carlo simulations and the number is 16 − 12 + 4.7 yr−1 for the Einstein telescope and 24 − 17 + 6.8 yr−1 for Cosmic Explorer, of which the median is about ∼2 times the rate of sBBHs originating from the EMBS channel (calibrated by the local merger rate density estimated for the dynamical and the EMBS channel, i.e., ∼ 14 − 10 + 4.0 and 19 − 3.0 + 42 Gpc − 3 yr − 1 , respectively). Therefore, one may constrain the fraction of both the EMBS and dynamical channels through the comparison of the predicted and observed number of lensed sBBH events statistically.

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Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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Event Rate of Strongly Lensed Gravitational Waves of Stellar Binary Black Hole Mergers Produced by Dynamical Interactions

Chen

2023

ApJ

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Testing an exact diffraction formula with gravitational wave source lensed by a supermassive black hole in binary systems

Guo,

Cao

2024

J. Cosmol. Astropart. Phys.

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When it comes to long-wavelength gravitational waves (GWs), diffraction effect becomes significant when these waves are lensed by celestial bodies. Typically, the traditional diffraction integral formula neglects large-angle diffraction, which is often adequate for most of cases. Nonetheless, there are specific scenarios, such as when a GW source is lensed by a supermassive black hole in a binary system, where the lens and source are in close proximity, where large-angle diffraction can play a crucial role. In our prior research, we have introduced an exact, general diffraction integral formula that accounts for large-angle diffraction as well. This paper explores the disparities between this exact diffraction formula and the traditional, approximate one under various special conditions. Our findings indicate that, under specific parameters — such as a lens-source distance of D LS = 0.1 AU and a lens mass of M L = 4 × 106 M ⊙ — the amplification factor for the exact diffraction formula is notably smaller than that of the approximate formula, differing by a factor of approximately rF ≃ 0.806. This difference is substantial enough to be detectable. Furthermore, our study reveals that the proportionality factor rF gradually increases from 0.5 to 1 as D LS increases, and decreases as M L increases. Significant differences between the exact and approximate formulas are observable when D LS ≲ 0.2 AU (assuming M L = 4 × 106 M ⊙) or when M L ≳ 2 × 106 M ⊙ (assuming D LS = 0.1 AU). These findings suggest that there is potential to validate our general diffraction formula through future GW detections.

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Multiband gravitational wave observations of stellar binary black holes at the low to middle and high frequencies

Zhao

Yan

et al. 2023

Monthly Notices of the Royal Astronomical Society

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The ground-based gravitational wave (GW) observatories discover a population of merging stellar binary black holes (BBHs), which are promising targets for multiband observations by the low-, middle-, and high-frequency GW detectors. In this paper, we investigate the multiband GW detections of BBHs and demonstrate the advantages of such observations in improving the localization and parameter estimates of the sources. We generate mock samples of BBHs by considering different formation models as well as the merger rate density constrained by the current observations (GWTC-3). We specifically consider the astrodynamical middle-frequency interferometer GW observatory (AMIGO) in the middle-frequency band and estimate that it may detect 21-91 BBHs with signal-to-noise ratio ϱ ≥ 8 in a 4-year observation period. The multiband observations by the low-frequency detectors [Laser Interferometer Space Antenna (LISA) and Taiji] and AMIGO may detect 5-33 BBHs with ϱLT ≥ 5 and ϱAMI ≥ 5, which can evolve to the high-frequency band within 4 years and can be detected by the Cosmic Explorer (CE) and Einstein Telescope (ET). The joint observations of LISA-Taiji-AMIGO-ET-CE may localize the majority of the detectable BBHs in sky areas of 7 × 10−7-2 × 10−3 deg2, which is improved by a factor of ∼120, ∼2.4 × 105, ∼1.8 × 104, or ∼1.2 × 104, comparing with those by only adopting CE-ET, AMIGO, LISA-Taiji, or LISA-Taiji-AMIGO. These joint observations can also lead to an improvement of the measurement precision of the chirp mass (symmetric mass ratio) by a factor of ∼5.5 × 104 (33), ∼16 (8), ∼120 (90), or ∼5 (5), comparing with those by CE-ET, AMIGO, LISA-Taiji, or LISA-Taiji-AMIGO.

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Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals

Cited by 10 publications

References 105 publications

Event Rate of Strongly Lensed Gravitational Waves of Stellar Binary Black Hole Mergers Produced by Dynamical Interactions

Event Rate of Strongly Lensed Gravitational Waves of Stellar Binary Black Hole Mergers Produced by Dynamical Interactions

Testing an exact diffraction formula with gravitational wave source lensed by a supermassive black hole in binary systems

Multiband gravitational wave observations of stellar binary black holes at the low to middle and high frequencies

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