Gravitational wave probes of dark matter: challenges and opportunities

Bertone, Gianfranco; Croon, Djuna; Amin, Mustafa A.; Boddy, Kimberly K.; Kavanagh, Bradley J.; Mack, Katherine J.; Natarajan, Priyamvada; Opferkuch, Toby; Schutz, Katelin; Takhistov, Volodymyr; Weniger, Christoph; Yu, Tien-Tien

doi:10.21468/scipostphyscore.3.2.007

Cited by 86 publications

(69 citation statements)

References 337 publications

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“…Understanding dark matter (DM) is one of the major scientific endeavours of this century [54,56]. Models to explain it range from ultralight bosons with masses ∼ 10 −22 eV to BHs with tens of solar masses.…”

Section: Bhs Gws and Dark Mattermentioning

confidence: 99%

Probing the nature of black holes: Deep in the mHz gravitational-wave sky

et al. 2021

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Black holes are unique among astrophysical sources: they are the simplest macroscopic objects in the Universe, and they are extraordinary in terms of their ability to convert energy into electromagnetic and gravitational radiation. Our capacity to probe their nature is limited by the sensitivity of our detectors. The LIGO/Virgo interferometers are the gravitational-wave equivalent of Galileo’s telescope. The first few detections represent the beginning of a long journey of exploration. At the current pace of technological progress, it is reasonable to expect that the gravitational-wave detectors available in the 2035-2050s will be formidable tools to explore these fascinating objects in the cosmos, and space-based detectors with peak sensitivities in the mHz band represent one class of such tools. These detectors have a staggering discovery potential, and they will address fundamental open questions in physics and astronomy. Are astrophysical black holes adequately described by general relativity? Do we have empirical evidence for event horizons? Can black holes provide a glimpse into quantum gravity, or reveal a classical breakdown of Einstein’s gravity? How and when did black holes form, and how do they grow? Are there new long-range interactions or fields in our Universe, potentially related to dark matter and dark energy or a more fundamental description of gravitation? Precision tests of black hole spacetimes with mHz-band gravitational-wave detectors will probe general relativity and fundamental physics in previously inaccessible regimes, and allow us to address some of these fundamental issues in our current understanding of nature.

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Section: Bhs Gws and Dark Mattermentioning

confidence: 99%

Probing the nature of black holes: Deep in the mHz gravitational-wave sky

et al. 2021

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“…Although the principal aim of experiments like Virgo is to directly detect the GW strain produced by compact objects like BH and NS, the same principle can be used to investigate the effects of DM particles. This can be achieved by looking for particles directly interacting with the detector and/or for GW signatures produced by DM particles in the proximity of astrophysical objects; for a review of all the DM candidates that can be investigated using GWs, see [54].…”

Section: Astrophysical Sourcesmentioning

confidence: 99%

Advanced Virgo: Status of the Detector, Latest Results and Future Prospects

et al. 2021

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The Virgo detector, based at the EGO (European Gravitational Observatory) and located in Cascina (Pisa), played a significant role in the development of the gravitational-wave astronomy. From its first scientific run in 2007, the Virgo detector has constantly been upgraded over the years; since 2017, with the Advanced Virgo project, the detector reached a high sensitivity that allowed the detection of several classes of sources and to investigate new physics. This work reports the main hardware upgrades of the detector and the main astrophysical results from the latest five years; future prospects for the Virgo detector are also presented.

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“…The science for the next generation of ground based detectors includes a survey of primordial stellar mass black holes formed in the early Universe (redshifts of ≈ 20) [28], test of matter in extreme environments, and the study of phenomena which radiate weaker gravitational waves than compact binary systems, such as the core-collapse of supernovae [29] and continuous gravitational waves emitted by neutron stars [30]. Cosmology will also bene t from a possible detection of primordial gravitational waves [31], and from tests of dark energy and dark matter theories [32,33]. Together with the launch of a space based gravitational wave detector, the future promises exciting scienti c explorations about our Universe, and possibly evidences for new physics, never anticipated before!…”

Section: Gravitational Wavesmentioning

confidence: 99%

Laser power stabilization via radiation pressure

et al. 2021

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This thesis reports a new active power stabilization scheme which can be implemented in high precision experiments, such as gravitational wave detectors. The novel aspect of the scheme is sensing laser power uctuations via the radiation pressure driven motion they induce on a movable mirror. The mirror position and its uctuations are determined by means of a weak auxiliary beam and a Michelson interferometer, which form an in-loop sensor for the proposed stabilization scheme. This sensing technique exploits the concept of a nondemolition measurement, since the power uctuations are inferred by measuring the uctuations in the phase observable of the auxiliary beam. This process results in higher in-loop signals for power uctuations than what would be achieved by a direct detection, e.g. via the traditional scheme where a fraction of the laser power is picked o and sensed directly by a photodetector. Other advantages of this scheme are that the full beam power is preserved and available for further use, and that it enables the generation of a strong bright squeezed out-of-loop beam.An extensive theoretical investigation on the concept of the new sensing scheme is presented. In this investigation, di erent schemes in which power uctuations are transferred to another observable of the light eld, e.g. phase or polarization, are compared to each other, and the advantages of the radiation pressure scheme are highlighted. Furthermore, a complete calculation of the fundamental limit of the proposed radiation pressure scheme, set by the quantum noise in the interferometer and the thermal noise of the movable mirror, is performed. The calculations show that a bright squeezed beam with a power of 4 W and up to 11 dB of squeezing might be achievable in the near future. Based on the results of the theoretical investigation, a proof-of-principle experiment was realized with microoscillator mirrors with masses ranging from 25 to 250 ng, and fundamental resonance frequencies from 150 to 210 Hz. Power stabilization in the frequency range from 1 Hz to 10 kHz was demonstrated. The results for the out-of-loop power stability are presented for di erent beam powers, and a relative power noise of 3.7 × 10 −7 Hz −1/2 was achieved at 250 Hz for 267 mW. The stability performance was limited by the structural thermal noise of the micro-oscillators, which was particularly high due to operation at room temperature. The results from the investigations conducted in this thesis are a promising step towards generation of a strong bright squeezed beam, and towards an improved stabilization scheme to be used in the future generation of gravitational wave detectors.

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Gravitational wave probes of dark matter: challenges and opportunities

Cited by 86 publications

References 337 publications

Probing the nature of black holes: Deep in the mHz gravitational-wave sky

Probing the nature of black holes: Deep in the mHz gravitational-wave sky

Advanced Virgo: Status of the Detector, Latest Results and Future Prospects

Laser power stabilization via radiation pressure

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