Gravitational-Wave Lensing Fringes by Compact Dark Matter at LIGO

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Abstract

Utilizing gravitational-wave (GW) lensing opens a new way to understand the history and structure of the universe. In spite of coarse angular resolution and short duration of observation, we show that LIGO can detect the GW lensing induced by small structures, in particular by compact dark matter (DM) of \(10 - 10^5 M_{\rm sun}\), which remains an interesting DM candidate. The lensing is detected through GW frequency chirping, creating the natural and rapid change of lensing patterns: frequency-dependent amplification and modulation of waveforms. As a highest-frequency GW detector, LIGO is a unique GW lab to probe such light compact DM. With design sensitivity of Advanced LIGO, one-year observation can detect as many as 1000 lensed GWs and constrain compact DM fraction as small as \(f_{\rm DM} \gtrsim 10^{-3}\).

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Observation of Gravitational Waves from a Binary Black Hole Merger

the LIGO Scientific Collaboration, the Virgo Collaboration (2016)

On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of \(1.0 \times 10^{-21}\). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1 {\sigma}. The source lies at a luminosity distance of \(410^{+160}_{-180}\) Mpc corresponding to a redshift \(z = 0.09^{+0.03}_{-0.04}\). In the source frame, the initial black hole masses are \(36^{+5}_{-4} M_\odot\) and \(29^{+4}_{-4} M_\odot\), and the final black hole mass is \(62^{+4}_{-4} M_\odot\), with \(3.0^{+0.5}_{-0.5} M_\odot c^2\) radiated in gravitational waves. All uncertainties define 90% credible intervals.These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

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Gravitational Waves from Mergin Compact Binaries: How Accurately Can One Extract the Binary's Parameters from the Inspiral Waveform?

Curt Cutler, Eanna Flanagan (1994)

The most promising source of gravitational waves for the planned detectors LIGO and VIRGO are merging compact binaries, i.e., neutron star/neutron star (NS/NS), neutron star/black hole (NS/BH), and black hole/black-hole (BH/BH) binaries. We investigate how accurately the distance to the source and the masses and spins of the two bodies will be measured from the gravitational wave signals by the three detector LIGO/VIRGO network using ``advanced detectors'' (those present a few years after initial operation). The combination \({\cal M} \equiv (M_1 M_2)^{3/5}(M_1 +M_2)^{-1/5}\) of the masses of the two bodies is measurable with an accuracy \(\approx 0.1\%-1\%\). The reduced mass is measurable to \(\sim 10\%-15\%\) for NS/NS and NS/BH binaries, and \(\sim 50\%\) for BH/BH binaries (assuming \(10M_\odot\) BH's). Measurements of the masses and spins are strongly correlated; there is a combination of \(\mu\) and the spin angular momenta that is measured to within \(\sim 1\%\). We also estimate that distance measurement accuracies will be \(\le 15\%\) for \(\sim 8\%\) of the detected signals, and \(\le 30\%\) for \(\sim 60\%\) of the signals, for the LIGO/VIRGO 3-detector network.