GW190412 as a Third-generation Black Hole Merger from a Super Star Cluster

Rodriguez, Carl L.; Kremer, Kyle; Grudić, Michael Y.; Hafen, Zachary; Chatterjee, Sourav; Fragione, Giacomo; Lamberts, Astrid; Martinez, Miguel A. S.; Rasio, Frederic A.; Weatherford, Newlin C.; Ye, Claire S.

doi:10.3847/2041-8213/ab961d

Cited by 81 publications

(62 citation statements)

References 90 publications

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“…It is not clear if isolated stellar evolutionary models alone can consistently produce the c eff distribution in the detected events so far. Recent works by Rodriguez et al (2020) and Gerosa et al (2020) have also shown that it would be possible to reproduce these detections with repeated mergers of previous merger products in extremely large clusters. This would require that BHs are born with low natal spins, so as to retain more of the merger remnants.…”

Section: Spinsmentioning

confidence: 72%

“…However, recent works by Rodriguez et al (2020) and Gerosa et al (2020) have shown that the relative fraction of low-mass-ratio merger events can be enhanced by second-and third-generation mergers in dynamical environments, producing GW190412-like events as a result, though analysis by Kimball et al (2020) casts doubt on the hierarchical merger scenario for GW190412. Due to the efficiency of mass segregation, the remnant of a previous merger is expected to be twice as massive as the 1G BHs in the cluster (see also Samsing & Hotokezaka 2020).…”

Section: Massesmentioning

confidence: 99%

“…These results are extremely interesting in light of the recent detection of GW190521 (LIGO Scientific Collaboration & Virgo Collaboration 2020d), a merger event with a total mass of M 150  , whose components could be 2G BHs. Many studies have discussed the frequency and importance of successive mergers with 2G and higher BHs in massive clusters such as GCs, super star clusters, and nuclear star clusters (Antonini et al 2019;Rodriguez et al 2019Rodriguez et al , 2020Fragione & Silk 2020;Gerosa et al 2020;Samsing & Hotokezaka 2020). Mergers involving 2G BHs are expected to be more massive, potentially falling within the mass range of~M 46 133 - , the so-called upper mass gap, where no BHs are expected to be formed due to pair instability supernovae (Woosley & Heger 2015;Woosley 2017;Wen 2019).…”

Section: Merger Remnant Retentionmentioning

confidence: 99%

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Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Martinez

Fragione

Kremer

et al. 2020

ApJ

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Hierarchical triples are expected to be produced by the frequent binary-mediated interactions in the cores of globular clusters. In some of these triples, the tertiary companion can drive the inner binary to merger following large eccentricity oscillations, as a result of the eccentric Kozai-Lidov mechanism. In this paper, we study the dynamics and merger rates of black hole (BH) hierarchical triples, formed via binary-binary encounters in the CMC Cluster Catalog, a suite of cluster simulations with present-day properties representative of the Milky Way's globular clusters. We compare the properties of the mergers from triples to the other merger channels in dense star clusters, and show that triple systems do not produce significant differences in terms of mass and effective spin distribution. However, they represent an important pathway for forming eccentric mergers, which could be detected by LIGO-Virgo/Kamioka Gravitational-Wave Detector (LVK), and future missions such as LISA and the DECi-hertz Interferometer Gravitational wave Observatory. We derive a conservative lower limit for the merger rate from this channel of 0.35 Gpc −3 yr −1 in the local universe and up to~9% of these events may have a detectable eccentricity at LVK design sensitivity. Additionally, we find that triple systems could play an important role in retaining second-generation BHs, which can later merge again in the core of the host cluster. Unified Astronomy Thesaurus concepts: Astrophysical black holes (98); Black holes (162); Stellar mass black holes (1611); Gravitational wave astronomy (675); Gravitational wave detectors (676); Gravitational wave sources (677); Gravitational waves (678); Globular star clusters (656); Star clusters (1567); Trinary stars (1714)

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Section: Spinsmentioning

confidence: 72%

Section: Massesmentioning

confidence: 99%

Section: Merger Remnant Retentionmentioning

confidence: 99%

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Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Martinez

Fragione

Kremer

et al. 2020

ApJ

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“…It is exceptional on account of its mass ratio, which is inferred as = -+ q 0.28 0.06 0.13 assuming the fiducial parameter estimation prior. The large difference in component masses would not be surprising for a hierarchical merger (Rodriguez et al 2020;Gerosa et al 2020), so here we investigate how our results change including GW190412. For this, we use parameterestimation results for GW190412 from Zevin et al (2020).…”

Section: Appendix B Including Gw190412mentioning

confidence: 97%

Black Hole Genealogy: Identifying Hierarchical Mergers with Gravitational Waves

Kimball

Talbot

Berry

et al. 2020

ApJ

139

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In dense stellar environments, the merger products of binary black hole mergers may undergo additional mergers. These hierarchical mergers are naturally expected to have higher masses than the first generation of black holes made from stars. The components of hierarchical mergers are expected to have significant characteristic spins, imprinted by the orbital angular momentum of the previous mergers. However, since the population properties of first-generation black holes are uncertain, it is difficult to know if any given merger is first-generation or hierarchical. We use observations of gravitational waves to reconstruct the binary black hole mass and spin spectrum of a population including the possibility of hierarchical mergers. We employ a phenomenological model that captures the properties of merging binary black holes from simulations of globular clusters. Inspired by recent work on the formation of low-spin black holes, we include a zero-spin subpopulation. We analyze binary black holes from LIGO and Virgo's first two observing runs, and find that this catalog is consistent with having no hierarchical mergers. We find that the most massive system in this catalog, GW170729, is mostly likely a firstgeneration merger, having a 4% probability of being a hierarchical merger assuming a 5×10 5 M e globular cluster mass. Using our model, we find that 99% of first-generation black holes in coalescing binaries have masses below 44 M e , and the fraction of binaries with near-zero component spins is less than 0.16 (90% probability). Upcoming observations will determine if hierarchical mergers are a common source of gravitational waves.

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“…With a measured primary spin χ 1 ∼ 0.43 [3], GW190412 challenges previous predictions. Indeed, its unusual properties have already sparked numerous interpretations in the astrophysics community, ranging from isolated binaries with tidally spun-up secondaries [16][17][18] to dynamical assembly in young star clusters [19], gas-assisted migration in the disks of active galactic nuclei (AGN) [20], quadruple stars [21], and super star clusters [22].…”

Section: Introductionmentioning

confidence: 99%

Astrophysical Implications of GW190412 as a Remnant of a Previous Black-Hole Merger

2020

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GW190412 as a Third-generation Black Hole Merger from a Super Star Cluster

Cited by 81 publications

References 90 publications

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Black Hole Genealogy: Identifying Hierarchical Mergers with Gravitational Waves

Astrophysical Implications of GW190412 as a Remnant of a Previous Black-Hole Merger

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