Detecting Subsolar-Mass Primordial Black Holes in Extreme Mass-Ratio Inspirals with LISA and Einstein Telescope

Barsanti, Susanna; Luca, Valerio De; Maselli, Andrea; Pani, Paolo

doi:10.1103/physrevlett.128.111104

Cited by 25 publications

(7 citation statements)

References 104 publications

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“…Even more wave-like diffraction is found to be useful in probing galactic (sub)halos of the diffuse NFW mass profile [11][12][13][14] and cosmological matter power spectrum [15,16]. In more general, exquisite sensitivities to the chirp mass, eccentricity, and the last stage of mergers also open up new probes of wave dark matter [17], compact dark objects [18,19], dark matter captures [20], sub-solar mass black holes [21][22][23], and non-standard gravitation theories.…”

Section: Introductionmentioning

confidence: 99%

Solar diffraction of LIGO-band gravitational waves

Jung

Kim

2023

J. Cosmol. Astropart. Phys.

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We show that chirping gravitational waves in the LIGO frequency band f = 1–5000 Hz can be gravitationally diffracted by the Sun, due to the coincidence of its Fresnel length rF ∝ √1 AU/f and the solar radius r ⊙. This solar diffraction is potentially detectable through its frequency-dependent amplification of the wave. The detection rate with Einstein Telescope is estimated to be ∼ 1/1000 per year, with the optical depth ∝ (solar angular area on the sky)/4π. High-frequency regimes of merger and ringdown phases are found to be crucial. In addition to the discovery, we advocate that solar diffraction allows probing the inner solar density profile, as rF sweeps a range of solar radius during the chirping. These physics are captured by a formalism in terms of convergence and shear, which allows much easier estimation and more intuitive understanding. Solar diffraction can be a new opportunity with ongoing and future LIGO-band missions.

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Section: Introductionmentioning

confidence: 99%

Solar diffraction of LIGO-band gravitational waves

Jung

Kim

2023

J. Cosmol. Astropart. Phys.

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“…Also, in this case, the detection of subsolar mergers would indicate new physics. 35 While in the main text we focus on nearly equal mass mergers with q ≈ 1, other potentially interesting systems for the detection of subsolar objects are intermediate mass ratio inspirals, given the high precision in measuring the mass of the light object at subpercent level [323]. Due to the relevance of the low-frequency range for these observations, the implementation of the LF interferometer could in principle enhance the capability of detecting these systems.…”

Section: Other Pbh Signaturesmentioning

confidence: 99%

Science with the Einstein Telescope: a comparison of different designs

Branchesi¹,

Maggiore²,

Alonso³

et al. 2023

J. Cosmol. Astropart. Phys.

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145

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The Einstein Telescope (ET), the European project for a third-generation gravitational-wave detector, has a reference configuration based on a triangular shape consisting of three nested detectors with 10 km arms, where each detector has a 'xylophone' configuration made of an interferometer tuned toward high frequencies, and an interferometer tuned toward low frequencies and working at cryogenic temperature. Here, we examine the scientific perspectives under possible variations of this reference design. We perform a detailed evaluation of the science case for a single triangular geometry observatory, and we compare it with the results obtained for a network of two L-shaped detectors (either parallel or misaligned) located in Europe, considering different choices of arm-length for both the triangle and the 2L geometries. We also study how the science output changes in the absence of the low-frequency instrument, both for the triangle and the 2L configurations. We examine a broad class of simple 'metrics' that quantify the science output, related to compact binary coalescences, multi-messenger astronomy and stochastic backgrounds, and we then examine the impact of different detector designs on a more specific set of scientific objectives.

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“…From the resulting equilibrium distribution it is then possible to compute the rate of objects captured by the central black hole (see Eqs. (15)(16)(17) in [36]):…”

Section: A Crossing Ratementioning

confidence: 99%

“…The search for a solution to the dark matter problem [1][2][3][4] has led primordial black holes (PBHs) [5][6][7][8][9] to be considered as a serious candidate for several years now [10], especially in light of the as-of-today inconclusive results of the many experiments aimed at a direct detection of a dark matter particle [11,12]. If PBHs do exist and indeed constitute a fraction of the dark matter in the Universe, it is argued that they should clump at the center of galaxies, and supposedly orbit the supermassive black hole at their centers [13][14][15][16][17], with a mass function and abundance given by, e.g., [18]. Given the PBHs compact nature, their motion around the central supermassive black hole should be accompanied by loud gravitational wave (GWs) emission, whose detection, or lack thereof, could put constraints on the very existence of PBHs and on their relevance as a dark matter candidate.…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from an eccentric population of primordial black holes orbiting Sgr A$^{\star}$

Bondani¹,

Bonetti²,

Luca³

et al. 2023

Preprint

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Primordial black holes (PBH), supposedly formed in the very early Universe, have been proposed as a possible viable dark matter candidate. In this work we characterize the expected gravitational wave (GW) losses from a population of PBHs orbiting Sgr A , the super-massive black hole at the Galactic center (GC), and assess the signal detectability by the planned space-borne interferometer LISA and by the proposed next generation space-borne interferometer µAres. Assuming that PBHs indeed form the entire diffuse mass allowed to reside within the orbit of the S2 star, we compute an upper limit to the expected GW signal both from resolved and non-resolved sources, under the further assumptions of monochromatic mass function and thermally distributed eccentricities. By comparing with our previous work where PBHs on circular orbits were assumed, we show how the GW signal from high harmonics over a 10 year data stream increases by a factor of six the chances of LISA detectability, from the ≈ 10% of the circular case, to ≈ 60%, whereas multiple sources can be identified in 20% of our mock populations. The background signal, made by summing up all non resolved sources, should be certainly detectable thanks to the PBHs with higher eccentricity evolving under two body relaxation. In the case of µAres, because of its improved sensitivity in the µHz band, one third of the entire population of PBHs orbiting Sgr A would be resolved. The background noise from the remaining non resolved sources should be detectable as well.

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Detecting Subsolar-Mass Primordial Black Holes in Extreme Mass-Ratio Inspirals with LISA and Einstein Telescope

Cited by 25 publications

References 104 publications

Solar diffraction of LIGO-band gravitational waves

Solar diffraction of LIGO-band gravitational waves

Science with the Einstein Telescope: a comparison of different designs

Gravitational waves from an eccentric population of primordial black holes orbiting Sgr A$^{\star}$

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