Beyond the Standard Model Explanations of GW190521

Sakstein, Jeremy; Croon, Djuna; McDermott, Samuel D.; Straight, Maria C.; Baxter, Eric J.

doi:10.1103/physrevlett.125.261105

Cited by 81 publications

(52 citation statements)

References 80 publications

(87 reference statements)

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“…Including GW190521, the M BHMG posterior is bimodal, with a second feature near 70M e . If this feature persists after future data releases, this will be intriguing evidence in favor of novel hypotheses that alter the location of PPISN (Croon et al 2020(Croon et al , 2021Sakstein et al 2020;Straight et al 2020).…”

Section: Resultsmentioning

confidence: 96%

“…This parameter a may be used to quantify the number of black holes that are the result of PPISN, as well as identify a mass for which PPISN becomes important, as shown in more detail in Appendix A. The parameterization in Equation (3) is sufficiently flexible to account for many different effects that might impact the onset of PPISN and thereby lead to a smooth change in the value of M BHMG , such as variations in metallicity or wind-loss rate (Farmer et al 2019;Vink et al 2021), a change in the nuclear reaction rates (Farmer et al 2019(Farmer et al , 2020Woosley & Heger 2021), or new physics (Croon et al 2020(Croon et al , 2021Sakstein et al 2020;Straight et al 2020;Ziegler & Freese 2020).…”

Section: Astrophysical Mass Functionmentioning

confidence: 99%

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Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Baxter

Croon

McDermott

et al. 2021

ApJL

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We introduce a novel black hole mass function that realistically models the physics of pair-instability supernovae with a minimal number of parameters. Applying this to all events in the LIGO-Virgo Gravitational-Wave Transient Catalog 2 (GWTC-2), we detect a peak at. Repeating the analysis without the black holes from the event GW190521, we find this feature at M BHMG = 54 ± 6 M e . These results establish the edge of the anticipated "black hole mass gap" at a value compatible with the expectation from standard stellar structure theory. The mass gap manifests itself as a discontinuity in the mass function and is populated by a distinct, less-abundant population of higher-mass black holes. We find that the primary black hole population scales with power-law index −1.95 ± 0.51 (−1.97 ± 0.44) with (without) GW190521, consistent with models of star formation. Using Bayesian techniques, we establish that our mass function fits a new catalog of black hole masses approximately as well as pre-existing phenomenological mass functions. We also remark on the implications of these results for constraining or discovering new phenomena in nuclear and particle physics. Unified Astronomy Thesaurus concepts: Astrophysical black holes (98); Black holes (162); Gravitational waves (678); Particle astrophysics (96); Gravitational wave astronomy (675); Nuclear astrophysics (1129); Stellar evolution (1599); Stellar populations (1622); Population III stars (1285); Helium burning (716)

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Section: Resultsmentioning

confidence: 96%

Section: Astrophysical Mass Functionmentioning

confidence: 99%

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Baxter

Croon

McDermott

et al. 2021

ApJL

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“…However, even allowing for a significant amount of mass in primordial black holes, merger rate predictions are sensitive assumptions about the initial distribution of such sources in binaries or small clusters (e.g., Ali-Haı ¨moud et al 2017;Korol et al 2020;De Luca et al 2020a) as well as possible accretion onto primordial black holes (De Luca et al 2020b). Meanwhile, some of the scenarios proposed for the formation of BH-BH binaries involve physics beyond the standard model (Sakstein et al 2020) and cosmological coupling (Croker et al 2021).…”

Section: Exoticamentioning

confidence: 99%

Rates of compact object coalescences

2022

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Gravitational-wave detections are enabling measurements of the rate of coalescences of binaries composed of two compact objects—neutron stars and/or black holes. The coalescence rate of binaries containing neutron stars is further constrained by electromagnetic observations, including Galactic radio binary pulsars and short gamma-ray bursts. Meanwhile, increasingly sophisticated models of compact objects merging through a variety of evolutionary channels produce a range of theoretically predicted rates. Rapid improvements in instrument sensitivity, along with plans for new and improved surveys, make this an opportune time to summarise the existing observational and theoretical knowledge of compact-binary coalescence rates.

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“…However, stars with mass above ≳200 M ⊙ and very low metallicity (typical of population III) can avoid disruption and form a population of intermediate mass BHs with masses above ∼135 M ⊙ [17][18][19][20][21][22][23][24][25][26]. It is not excluded that BHs within the mass gap might have an astrophysical origin due to hierarchical coalescences of smaller BHs [27][28][29][30][31][32][33], via direct collapse of a stellar merger between an evolved star and a main sequence companion [34,35], by rapid mass accretion in primordial dense clusters [36], or by beyond standard model physics that reduces the pair instability [37].…”

mentioning

confidence: 99%

GW190521 Mass Gap Event and the Primordial Black Hole Scenario

Desjacques²,

et al. 2021

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The LIGO/Virgo Collaboration has recently observed GW190521, the first binary black hole merger with at least the primary component mass in the mass gap predicted by the pair-instability supernova theory. This observation disfavors the standard stellar-origin formation scenario for the heavier black hole, motivating alternative hypotheses. We show that GW190521 cannot be explained within the primordial black hole (PBH) scenario if PBHs do not accrete during their cosmological evolution, since this would require an abundance which is already in tension with current constraints. On the other hand, GW190521 may have a primordial origin if PBHs accrete efficiently before the reionization epoch.

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Beyond the Standard Model Explanations of GW190521

Cited by 81 publications

References 80 publications

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Find the Gap: Black Hole Population Analysis with an Astrophysically Motivated Mass Function

Rates of compact object coalescences

GW190521 Mass Gap Event and the Primordial Black Hole Scenario

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