Science with the TianQin observatory: Preliminary results on massive black hole binaries

Wang, Hai-Tian; Jiang, Zhen; Sesana, Alberto; Barausse, Enrico; Huang, S.; Wang, Yifan; Feng, Wen-Fan; Wang, Yan; Hu, Y. M.; Mei, Jianwei; Luo, Jun

doi:10.1103/physrevd.100.043003

Cited by 117 publications

(93 citation statements)

References 101 publications

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“…There have been many papers predicting rates for LISA (e.g. Klein et al 2016;Berti et al 2016;Salcido et al 2016;Bonetti et al 2019), as well as new predictions for the TianQin gravitational wave observatory, which is similar in construction to LISA (Wang et al 2019). Many rate prediction papers are built from semi-analytic models (SAM).…”

Section: Introductionmentioning

confidence: 99%

Probing Massive Black Hole Binary Populations with LISA

Katz

Kelley²,

Dosopoulou

et al. 2019

Monthly Notices of the Royal Astronomical Society

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ESA and NASA are moving forward with plans to launch LISA around 2034. With data from the Illustris cosmological simulation, we provide analysis of LISA detection rates accompanied by characterization of the merging massive black hole population. Massive black holes of total mass ∼ 10 5 − 10 10 M are the focus of this study. We evolve Illustris massive black hole mergers, which form at separations on the order of the simulation resolution (∼kpc scales), through coalescence with two different treatments for the binary massive black hole evolutionary process. The coalescence times of the population, as well as physical properties of the black holes, form a statistical basis for each evolutionary treatment. From these bases, we Monte Carlo synthesize many realizations of the merging massive black hole population to build mock LISA detection catalogs. We analyze how our massive black hole binary evolutionary models affect detection rates and the associated parameter distributions measured by LISA. With our models, we find massive black hole binary detection rates with LISA of ∼ 0.5 − 1 yr −1 for massive black holes with masses greater than 10 5 M . This should be treated as a lower limit primarily because our massive black hole sample does not include masses below 10 5 M , which may significantly add to the observed rate. We suggest reasons why we predict lower detection rates compared to much of the literature.

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Section: Introductionmentioning

confidence: 99%

Probing Massive Black Hole Binary Populations with LISA

Katz

Kelley²,

Dosopoulou

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…In the future, the third generation ground-based GW observatories, such as Einstein telescope (Punturo et al 2010;Sathyaprakash et al 2012), and space-borne GW observatories, such as LISA (Amaro-Seoane et al 2017), Pre-DECIGO (Kawamura et al 2006;Nakamura et al 2016), TianQin (Luo et al 2016;Wang et al 2019), and TianGO (Kuns et al 2020) will operate. The detection horizons of these detectors and aLIGO are shown in Figure 8.…”

Section: Discussionmentioning

confidence: 99%

On the population III binary black hole mergers beyond the pair-instability mass gap

Hijikawa,

Tanikawa,

Kinugawa

et al. 2021

Preprint

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We perform a binary population synthesis calculation incorporating very massive population (Pop.) III stars up to 1500 𝑀 , and investigate the nature of binary black hole (BBH) mergers. Above the pair-instability mass gap, we find that the typical primary black hole (BH) mass is 135-340 𝑀 . The maximum primary BH mass is as massive as 686 𝑀 . The BBHs with both of their components above the mass gap have low effective inspiral spin ∼ 0. So far, no conclusive BBH merger beyond the mass gap has been detected, and the upper limit on the merger rate density is obtained. If the initial mass function (IMF) of Pop. III stars is simply expressed as 𝜉 𝑚 (𝑚) ∝ 𝑚 −𝛼 (single power law), we find that 𝛼 2.8 is needed in order for the merger rate density not to exceed the upper limit. In the future, the gravitational wave detectors such as Einstein telescope and Pre-DECIGO will observe BBH mergers at high redshift. We suggest that we may be able to impose a stringent limit on the Pop. III IMF by comparing the merger rate density obtained from future observations with that derived theoretically.

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“…Neutron star (NS)-white dwarf (WD) binaries may have extremely short orbital periods and radiate GWs in the frequency range of 10 −4 -1 Hz. These compact binaries are therefore of interest for the GW detections of LISA [646,647], Taiji [648], and TianQin [649]. The model of a NS accreting a Roche-lobe filling (RLF) WD companion with orbital period in the range of ∼ (10-80) min can well explain the observed properties of ultracompact X-ray binary stars (UCXBs), whilst the model of a NS plus a low-mass RLF He star may also be one of the formation channels of UCXBs (e.g., ref.…”

Section: Orbital Evolution Of Ns-roche-lobe Filling Wd Binaries and Their Gwsmentioning

confidence: 99%

The Gravitational-wave physics II: Progress

Bian

Cai

Cao

et al. 2021

Sci. China Phys. Mech. Astron.

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It has been a half-decade since the first direct detection of gravitational waves, which signifies the coming of the era of the gravitational-wave astronomy and gravitational-wave cosmology. The increasing number of the detected gravitational-wave events has revealed the promising capability of constraining various aspects of cosmology, astronomy, and gravity. Due to the limited space in this review article, we will briefly summarize the recent progress over the past five years, but with a special focus on some of our own work for the Key Project "Physics associated with the gravitational waves" supported by the National Natural Science Foundation of China. In particular, (1) we have presented the mechanism of the gravitational-wave production during some physical processes of the early Universe, such as inflation, preheating and phase transition, and the cosmological implications of gravitational-wave measurements; (2) we have put constraints on the neutron star maximum mass according to GW170817 observations; (3) we have developed a numerical relativity algorithm based on the finite element method and a waveform model for the binary black hole coalescence along an eccentric orbit.

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Science with the TianQin observatory: Preliminary results on massive black hole binaries

Cited by 117 publications

References 101 publications

Probing Massive Black Hole Binary Populations with LISA

Probing Massive Black Hole Binary Populations with LISA

On the population III binary black hole mergers beyond the pair-instability mass gap

The Gravitational-wave physics II: Progress

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