Quantum Sensors with Matter Waves for GW Observation

Bertoldi, Andrea; Bouyer, Philippe; Canuel, B.

doi:10.1007/978-981-15-4702-7_5-1

Cited by 2 publications

(1 citation statement)

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“…While LISA will probe a BH mass range important for probing massive seeds, significantly smaller stellar seed mergers cannot be detected. The proposed interferometry mission DECIGO (Sato et al 2017), as well as ongoing and future experiments based on quantum interferometry with cold atoms, such as the terrestrial MAGIS-100 (Coleman 2018) or the AEDGE satellite (Bertoldi et al 2019) would fill in the gap between LIGO and LISA. This is warranted especially since the LIGO discoveries have already uncovered stellar-mass BHs more massive than had been expected (currently up to 85 M ; Abbott et al 2019), raising the possibility that the mass function extends to even higher masses.…”

Section: Mr23mentioning

confidence: 99%

The Assembly of the First Massive Black Holes

Inayoshi,

Visbal,

Haiman

2019

Preprint

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The existence of ∼10 9 M supermassive black holes (SMBHs) within the first billion year of the universe has stimulated numerous ideas for the prompt formation and rapid growth of BHs in the early universe. Here we review ways in which the seeds of massive BHs may have first assembled, how they may have subsequently grown as massive as ∼10 9 M , and how multi-messenger observations could distinguish between different SMBH assembly scenarios. We conclude the following:• The ultra-rare ∼10 9 M SMBHs represent only the tip of the iceberg.Early BHs likely fill a continuum from stellar-mass (∼ 10 M ) to the super-massive (∼ 10 9 ) regime, reflecting a range of initial masses and growth histories. • Stellar-mass BHs were likely left behind by the first generation of stars at redshifts as high as ∼ 30, but their initial growth was typically stunted due to the shallow potential wells of their host galaxies. • Conditions in some larger, metal-poor galaxies soon became conducive to the rapid formation and growth of massive 'seed' holes, via gas accretion and by mergers in dense stellar clusters. • BH masses depend on the environment (such as the number and properties of nearby radiation sources and the local baryonic streaming velocity), and on the metal enrichment and assembly history of the host galaxy. • Distinguishing between assembly mechanisms will be difficult, but a combination of observations by LISA (probing massive BH growth via mergers) and by deep multi-wavelength electromagnetic observations (probing growth via gas accretion) is particularly promising.

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Section: Mr23mentioning

confidence: 99%