Missing in axion: Where are XENON1T’s big black holes?

Croon, Djuna; McDermott, Samuel D.; Sakstein, Jeremy

doi:10.1016/j.dark.2021.100801

Cited by 20 publications

(22 citation statements)

References 86 publications

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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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“…This anomaly has already garnered considerable interest . However, it was quickly noted that a solar ALP explanation is in conflict with astrophysical observations, including stellar evolution and cooling [8,16,[41][42][43], SN1987A [8,16], pulsating White Dwarfs (WDs) [8], and the predicted mass of astrophysical black holes [44], although this tension can be reduced in more complicated ALP scenarios [41,45]. Interestingly, WD cooling presents a different anomaly that can also be JHEP05(2021)159 explained by axions, but the preferred axion couplings appear to be in conflict with the results of XENON1T.…”

Section: Jhep05(2021)159 1 Introductionmentioning

confidence: 99%

Global fits of axion-like particles to XENON1T and astrophysical data

Athron

Balázs

Beniwal

et al. 2021

J. High Energ. Phys.

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The excess of electron recoil events seen by the XENON1T experiment has been interpreted as a potential signal of axion-like particles (ALPs), either produced in the Sun, or constituting part of the dark matter halo of the Milky Way. It has also been explained as a consequence of trace amounts of tritium in the experiment. We consider the evidence for the solar and dark-matter ALP hypotheses from the combination of XENON1T data and multiple astrophysical probes, including horizontal branch stars, red giants, and white dwarfs. We briefly address the influence of ALP decays and supernova cooling. While the different datasets are in clear tension for the case of solar ALPs, all measurements can be simultaneously accommodated for the case of a sub-dominant fraction of dark-matter ALPs. Nevertheless, this solution requires the tuning of several a priori unknown parameters, such that for our choices of priors a Bayesian analysis shows no strong preference for the ALP interpretation of the XENON1T excess over the background hypothesis.

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“…The excess of electronic recoil events seen in XENON1T [470] has a spectrum that matches the expected solar axion flux. However, the amplitude of the excess would require large couplings that would place the excess in conflict with more stringent astrophysical bounds [557,842,878,929]. The proposed nextgeneration liquid xenon TPC will enable this excess to be robustly tested, should it persist, perhaps leading to the discovery of solar axions.…”

Section: A Solar Axionsmentioning

confidence: 99%

A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics

Aalbers,

Abe,

Aerne

et al. 2022

Preprint

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The nature of dark matter and properties of neutrinos are among the most pressing issues in contemporary particle physics. The dual-phase xenon time-projection chamber is the leading technology to cover the available parameter space for Weakly Interacting Massive Particles (WIMPs), while featuring extensive sensitivity to many alternative dark matter candidates. These detectors can also study neutrinos through neutrinoless double-beta decay and through a variety of astrophysical

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Missing in axion: Where are XENON1T’s big black holes?

Cited by 20 publications

References 86 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

Global fits of axion-like particles to XENON1T and astrophysical data

A Next-Generation Liquid Xenon Observatory for Dark Matter and Neutrino Physics

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