2020/01/31 by Kai Liao, Shuxun Tian, Xuheng Ding · 33 citations
Physics and Astronomy · #Astronomy #Astrophysics #Binary black hole #Cosmology and Gravitation Theories #Dark matter #Einstein Telescope #Einstein radius #Galaxy #Gamma-ray bursts and supernovae #Gravitational lens #Gravitational wave #LIGO #Physics #Pulsars and Gravitational Waves Research #Redshift #astro-ph.CO #gr-qc
paper · pdf · doi:10.1093/mnras/staa1388
published in Monthly Notices of the Royal Astronomical Society 495(2), 2002-2006 (Oxford University Press) · 6 pages, 3 figures, accepted by MNRAS
arxiv created 2020/05/16 · openalex publication_date 2020/05/19 · arxiv updated 2020/06/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT Unlike the electromagnetic radiation from astrophysical objects, gravitational waves (GWs) from binary star mergers have much longer wavelengths and are coherent. For ground-based GW detectors, when the lens object between the source and the Earth has mass ∼1−105 M⊙, the diffraction effect should be considered since the chirping wavelengths are comparable to the scale of the barrier (its Schwarzschild radius). The waveform will thus be distorted as the fringes. In this work, we show that signals from the third-generation GW detectors like the Einstein Telescope (ET) would be a smoking gun for probing the nature of compact dark matter (CDM) or primordial black holes. Detection of the lensing effects becomes harder when the lens mass is smaller. ET is more sensitive than LIGO, the constraint is available for CDM mass >5 M⊙ while LIGO can only detect the mass >100 M⊙. For a null search of the fringes, one-year observation of ET can constrain the CDM density fraction to ∼10−2 to 10−5 in the mass range MCDM = 10−100 M⊙.