Radio emission from accreting isolated black holes in our galaxy

Tsuna, D.; Kawanaka, Norita

doi:10.1093/mnras/stz1809

Cited by 18 publications

(17 citation statements)

References 75 publications

(113 reference statements)

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“…(See [58] and references therein for more details.) Direct measurement of isolated Galactic black holes, such as by radio observations [58,59], would significantly reduce the uncertainties in their properties.…”

Section: A Simulating Positions and Velocitiesmentioning

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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Section: A Simulating Positions and Velocitiesmentioning

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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“…Fender et al (2013), for instance, found that values larger than λ = 0.01 are excluded, under realistic assumptions, by observations of the local region, where a significant population of isolated BHs should be present. Tsuna et al (2018) and Tsuna & Kawanaka (2019) consider values between λ = 0.1 and λ = 10 −3 . The λ parameter may effectively capture the outflow of material that is expelled from the Bondi sphere, as suggested by several authors (Blandford & Begelman 1999).…”

Section: The Bhl Modelmentioning

confidence: 99%

“…Previous studies (Fender et al 2013;Tsuna et al 2018;Tsuna & Kawanaka 2019) obtained their estimates through Monte Carlo simulations of a BH population. Here, we adopt instead a semianalytical approach that allows us to perform a comprehensive parametric study associated with the physical model of accretion physics described above.…”

Section: E S T I M At I N G T H E N U M B E R O F V I S I B L E S O U R C E Smentioning

confidence: 99%

“…Such alternative emission could constitute a lower limit on the expected radio emission, which would be of particular interest in the absence of a jet. Tsuna & Kawanaka (2019) assumed a spherically symmetric outflow based on losing a fraction (1 − λ) of the accreting matter before reaching the BH, where λ is the suppression factor. Assuming a power-law radial dependence of the accretion rate, they used the escape velocity to conservatively estimate the power associated with such an outflow.…”

Section: The Emission Mechanism and Spectrummentioning

confidence: 99%

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Multiwavelength detectability of isolated black holes in the Milky Way

Scarcella

Gaggero

Connors

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Isolated black holes in our Galaxy have eluded detection so far. We present here a comprehensive study on the detectability of isolated stellar-mass astrophysical black holes that accrete interstellar gas from molecular clouds in both the local region and the Central Molecular Zone. We adopt a state-of-the-art model for the accretion physics backed up by numerical simulations, and study the number of observable sources in both the radio and X-ray band, as a function of a variety of parameters. We discuss in particular the impact of the astrophysical uncertainties on our prediction for the number of bright X-ray sources in the central region of the Galaxy. We finally consider future developments in the radio domain, and assess the potential of SKA to detect a population of astrophysical black holes accreting gas in our Galaxy.

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“…(See [56] and references therein for more details.) Direct observation of isolated Galactic black holes, such as by radio observations [56,57], would significantly reduce the uncertainties in their properties.…”

Section: A Simulating Positions and Velocitiesmentioning

confidence: 99%

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

Zhu,

Baryakhtar,

Papa

et al. 2020

Preprint

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Ultralight bosons can form large clouds around stellar-mass black holes via the superradiance instability and produce continuous gravitational wave signals with frequencies within the range of LIGO and Virgo. Unlike continuous gravitational waves from neutron stars, boson annihilation signals are clustered in frequency and have very small positive intrinsic frequency derivatives. We characterize the expected spin-0 boson annihilation ensemble signal from synthetic populations of isolated Galactic black holes. We explore how the different population parameters affect the resulting 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 a thousand signals loud enough to be in principle 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 a hundred detectable signals for some boson masses. A non-detection 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. However, due to the high signal density between 200 and 300 Hz, we urge caution when interpreting a null result for bosons between 4 and 6 × 10 −13 eV. Finally, we emphasize that the ensemble signal morphology would be the primary, perhaps sole, indicator that a continuous wave signal has a boson annihilation origin.

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Radio emission from accreting isolated black holes in our galaxy

Cited by 18 publications

References 75 publications

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

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

Multiwavelength detectability of isolated black holes in the Milky Way

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

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