Constraints on the astrophysical environment of binaries with gravitational-wave observations

Cardoso, Vítor; Maselli, Andrea

doi:10.1051/0004-6361/202037654

Cited by 81 publications

(44 citation statements)

References 43 publications

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“…If dark matter is made of cold collisionless particles, the adiabatic growth of black holes may induce the formation of large overdensities (often referred to as "spikes") around supermassive [17][18][19] and intermediate-mass [20][21][22] astrophysical black holes, as well as around primordial black holes [23][24][25][26]. It is in principle possible to detect and characterize DM overdensities around black holes by measuring their impact on the gravitational waveform as BHs merge with other compact objects [27][28][29][30][31][32][33][34][35].…”

Section: Introductionmentioning

confidence: 99%

Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform

et al. 2020

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A dark matter overdensity around a black hole may significantly alter the dynamics of the black hole's merger with another compact object. We consider here intermediate mass-ratio inspirals of stellar-mass compact objects with intermediate-mass black holes "dressed" with dark matter. We first demonstrate that previous estimates based on a fixed dark-matter dress are unphysical for a range of binaries and dark-matter distributions by showing that the total energy dissipated by the compact object through dynamical friction, as it inspirals through the dense dark matter environment toward the black hole, is larger than the gravitational binding energy of the dark-matter dress itself. We then introduce a new formalism that allows us to selfconsistently follow the evolution of the dark-matter dress due to its gravitational interaction with the binary. We show that the dephasing of the gravitational waveform induced by dark matter is smaller than previously thought, but is still potentially detectable with the LISA space interferometer. The gravitational waves from such binaries could provide powerful diagnostics of the particle nature of dark matter.

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Section: Introductionmentioning

confidence: 99%

Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform

et al. 2020

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“…Searches for dark matter imprints on gravitational waveforms are not as developed [57][58][59][60][61][62][63]. Approaches using Newtonian expressions for dynamical friction, incorporating accretion but no backreaction on fluid-like dark matter configurations, find that the post-Newtonian (PN) phasing is affected at −5.5PN order [59,61]. For models where Fig.…”

Section: Constraints On Dark Mattermentioning

confidence: 99%

“…Such a theory-agnostic formalism can be mapped to violations of various fundamental aspects of GR, such as the strong equivalence principle (time variation of G at PN, scalar dipole radiation at PN), Lorentz invariance ( PN and 0PN), parity invariance (2PN), or a nonzero graviton mass (1PN) [ 65 , 66 ]. Such a formalism also allows us to probe dark matter effects (e.g., gravitational drag at PN or PN [ 61 , 64 ]) and frequency-dependent departures of the GW propagation speed from (in this case, the PN order depends on the form of the dispersion relation).…”

Section: Tests Of General Relativitymentioning

confidence: 99%

The effect of mission duration on LISA science objectives

et al. 2021

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The science objectives of the LISA mission have been defined under the implicit assumption of a 4-years continuous data stream. Based on the performance of LISA Pathfinder, it is now expected that LISA will have a duty cycle of $$\approx 0.75$$ ≈ 0.75 , which would reduce the effective span of usable data to 3 years. This paper reports the results of a study by the LISA Science Group, which was charged with assessing the additional science return of increasing the mission lifetime. We explore various observational scenarios to assess the impact of mission duration on the main science objectives of the mission. We find that the science investigations most affected by mission duration concern the search for seed black holes at cosmic dawn, as well as the study of stellar-origin black holes and of their formation channels via multi-band and multi-messenger observations. We conclude that an extension to 6 years of mission operations is recommended.

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“…Gas dynamics affect the waveform by slowing down or accelerating the inspiral (e.g. Kocsis et al 2011;Yunes et al 2011;Barausse et al 2014;D'Orazio & Loeb 2018;Derdzinski et al 2019;Cardoso & Maselli 2020;…”

Section: Introductionmentioning

confidence: 99%

Astrophysical Gravitational-Wave Echoes from Galactic Nuclei

Gondán,

Kocsis

2021

Preprint

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Galactic nuclei (GNs) are dense stellar environments abundant in gravitational-wave (GW) sources for LIGO, VIRGO, and KA-GRA. The GWs may be generated by stellar-mass black hole (BH) or neutron star mergers following gravitational bremsstrahlung, dynamical scattering encounters, Kozai-Lidov type oscillations driven by the central supermassive black hole (SMBH), or gasassisted mergers if present. In this paper, we examine a smoking gun signature to identify sources in GNs: the GWs scattered by the central SMBH. This produces a secondary signal, an astrophysical GW echo, which has a very similar time-frequency evolution as the primary signal but arrives after a time delay. We determine the amplitude and time-delay distribution of the GW echo as a function of source distance from the SMBH. Between 10% − 90% of the detectable echoes arrive within (1 − 100) 𝑀 6 sec after the primary GW for sources between 10 − 10 4 𝑟 S , where 𝑟 S = 2𝐺 𝑀/𝑐 2 , 𝑀 is the observer-frame SMBH mass, and 𝑀 6 = 𝑀/(10 6 M ). The echo arrival times are systematically longer for high signal-to-noise ratio (SNR) primary GWs, where the GW echo rays are scattered at large deflection angles. In particular, 10% − 90% of the distribution is shifted to (5 − 1800) 𝑀 6 sec for sources, where the lower limit of echo detection is 0.02 of the primary signal amplitude. We find that 5% − 30% (1% − 7%) of GW sources have an echo amplitude larger than 0.2 − 0.05 times the amplitude of primary signal if the source distance from the SMBH is 𝑟 = 50 𝑟 S (200 𝑟 S ). Non-detections can rule out that a GW source is near an SMBH.

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Constraints on the astrophysical environment of binaries with gravitational-wave observations

Cited by 81 publications

References 43 publications

Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform

Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform

The effect of mission duration on LISA science objectives

Astrophysical Gravitational-Wave Echoes from Galactic Nuclei

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