Searching for dark photon dark matter in LIGO O1 data

Guo, Huai-Ke; Riles, K.; Yang, F. W.; Zhao, Yue

doi:10.1038/s42005-019-0255-0

Cited by 79 publications

(62 citation statements)

References 36 publications

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“…It would be important to study this question in more detail in the future. Finally, we should note that if ultralight dark matter photons couple directly to ordinary matter, they could also produce another kind of observable signal in GW interferometers by inducing displacements on the LIGO mirrors [120][121][122][123]. Since our results mainly apply to ultralight bosons for which non-gravitational interactions are negligible, our constraints complement those searches.…”

Section: Discussionmentioning

confidence: 62%

First search for a stochastic gravitational-wave background from ultralight bosons

et al. 2019

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Ultralight bosons with masses in the range 10 −13 eV ≤ m b ≤ 10 −12 eV can induce a superradiant instability around spinning black holes (BHs) with masses of order 10-100 M⊙. This instability leads to the formation of a rotating "bosonic cloud" around the BH, which can emit gravitational waves (GWs) in the frequency band probed by ground-based detectors. The superposition of GWs from all such systems can generate a stochastic gravitational-wave background (SGWB). In this work, we develop a Bayesian data analysis framework to study the SGWB from bosonic clouds using data from Advanced LIGO and Advanced Virgo, building on previous work by Brito et.al. [1]. We further improve this model by adding a BH population of binary merger remnants. To assess the performance of our pipeline, we quantify the range of boson masses that can be constrained by Advanced LIGO and Advanced Virgo measurements at design sensitivity. Furthermore, we explore our capability to distinguish an ultralight boson SGWB from a stochastic signal due to distant compact binary coalescences (CBC). Finally, we present results of a search for the SGWB from bosonic clouds using data from Advanced LIGO's first observing run. We find no evidence of such a signal. Due to degeneracies between the boson mass and unknown astrophysical quantities such as the distribution of isolated BH spins, our analysis cannot robustly exclude the presence of a bosonic field at any mass. Nevertheless, we show that under optimistic assumptions about the BH formation rate and spin distribution, boson masses in the range 2.0 × 10 −13 eV ≤ m b ≤ 3.8 × 10 −13 eV are excluded at 95% credibility, although with less optimistic spin distributions, no masses can be excluded. The framework established here can be used to learn about the nature of fundamental bosonic fields with future gravitational wave observations.

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Section: Discussionmentioning

confidence: 62%

First search for a stochastic gravitational-wave background from ultralight bosons

et al. 2019

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“…Since the coherence length of DPDM in this mass-range is much larger than the separation between various GW detectors on Earth (or the future LISA detector), the crosscorrelation between measurements from individual GW detectors can be used significantly enhance the signal-to-noise ratio of the otherwise stochastic signal. The first searches for DPDM, using LIGO's first observing run from the detectors in Hanford and Livingston, O1, have been conducted [203], and the constraints obtained already exceed those of fifth force searches for DM masses m ∼ 10 −14 − 10 −13 eV. Both methodological improvements of the analysis technique and additional data have the potential to further strengthen constraints on the coupling parameter ε 2 by more than an order of magnitude.…”

Section: Direct Dm Detection With Gw Experiments 51 Searches With Inmentioning

confidence: 99%

Gravitational wave probes of dark matter: challenges and opportunities

Bertone

Croon²,

Amin

et al. 2020

SciPost Phys. Core

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In this white paper, we discuss the prospects for characterizing and identifying dark matter using gravitational waves, covering a wide range of dark matter candidate types and signals. We argue that present and upcoming gravitational wave probes offer unprecedented opportunities for unraveling the nature of dark matter and we identify the most urgent challenges and open problems with the aim of encouraging a strong community effort at the interface between these two exciting fields of research.

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“…Canonical sources of continuous waves include neutron stars with mass deformations or internal fluid oscillation modes (see [2] for a recent review). Scenarios involving more exotic emitters of continuous waves are also being explored and can provide evidence for-or disfavor the presence of-new physics beyond the Standard Model of particle physics [3][4][5][6][7]. A particularly well-motivated target is the axion, proposed to solve the strong-CP problem in particle physics [8][9][10]; axions and axionlike particles are also promising dark matter candidates (see, e.g., [11] for a review).…”

Section: Introductionmentioning

confidence: 99%

Characterizing the continuous gravitational-wave signal from boson clouds around Galactic isolated black holes

Zhu

Baryakhtar²,

Papa

et al. 2020

Phys. Rev. D

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Ultralight bosons can form large clouds around stellar-mass black holes via the superradiance instability. Through processes such as annihilation, these bosons can source continuous gravitationalwave signals with frequencies within the range of LIGO and Virgo. If boson annihilation occurs, then the Galactic black hole population will give rise to many gravitational signals; we refer to this as the ensemble signal. We characterize the ensemble signal as observed by the gravitational-wave detectors; this is important because the ensemble signal carries the primary signature that a continuous wave signal has a boson annihilation origin. We explore how a broad set of black hole population parameters affects the resulting spin-0 boson annihilation signal and consider its detectability by recent searches for continuous gravitational waves. A population of 10 8 black holes with masses up to 30M ⊙ and a flat dimensionless initial spin distribution between zero and unity produces up to 1000 signals loud enough in principle to be detected by these searches. For a more moderately spinning population, the number of signals drops by about an order of magnitude, still yielding up to 100 detectable signals for some boson masses. A nondetection of annihilation signals at frequencies between 100 and 1200 Hz disfavors the existence of scalar bosons with rest energies between 2 × 10 −13 and 2.5 × 10 −12 eV. Finally, we show that, depending on the black hole population parameters, care must be taken in assuming that the continuous wave upper limits from searches for isolated signals are still valid for signals that are part of a dense ensemble: Between 200 and 300 Hz, we urge caution when interpreting a null result for bosons between 4 × 10 −13 and 6 × 10 −13 eV.

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Searching for dark photon dark matter in LIGO O1 data

Cited by 79 publications

References 36 publications

First search for a stochastic gravitational-wave background from ultralight bosons

First search for a stochastic gravitational-wave background from ultralight bosons

Gravitational wave probes of dark matter: challenges and opportunities

Characterizing the continuous gravitational-wave signal from boson clouds around Galactic isolated black holes

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