LIGO: the Laser Interferometer Gravitational-Wave Observatory

Willems, P. A.

doi:10.1088/0034-4885/72/7/076901

Cited by 1,088 publications

(790 citation statements)

References 97 publications

(116 reference statements)

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“…In other words, EM transients help to place a compact binary coalescence into an astrophysical context. After having been operational intermittently during the last decade, the Laser Interferometer Gravitational Wave Observatory (LIGO) and VIRGO detectors are currently being upgraded [44][45][46]. By about 2016, they should reach their new design sensitivities, which are 10-15 times higher than those of the initial instruments, so that the accessible volume increases by more than three orders of magnitude.…”

Section: (E) Electromagnetic Transientsmentioning

confidence: 99%

The dynamic ejecta of compact object mergers and eccentric collisions

Rosswog

2013

Phil. Trans. R. Soc. A.

101

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Compact object mergers eject neutron-rich matter in a number of ways: by the dynamical ejection mediated by gravitational torques, as neutrino-driven winds and probably also a good fraction of the resulting accretion disc finally becomes unbound by a combination of viscous and nuclear processes. If compact binary mergers produce indeed gamma-ray bursts there should also be an interaction region where an ultra-relativistic outflow interacts with the neutrino-driven wind and produces moderately relativistic ejecta. Each type of ejecta has different physical properties and therefore plays a different role for nucleosynthesis and for the electromagnetic transients that go along with compact object encounters. Here we focus on the dynamic ejecta and present results for over 30 hydrodynamical simulations of both gravitational wave-driven mergers and parabolic encounters as they may occur in globular clusters. We find that mergers eject $\sim 1$% of a solar mass of extremely neutron-rich material. The exact amount as well as the ejection velocity depends on the involved masses with asymmetric systems ejecting more material at higher velocities. This material undergoes a robust r-process and both ejecta amount and abundance pattern are consistent with neutron star mergers being a major source of the "heavy" ($A>130$) r-process isotopes. Parabolic collisions, especially those between neutron stars and black holes, eject substantially larger amounts of mass and therefore cannot occur frequently without overproducing galactic r-process matter. We also discuss the electromagnetic transients that are powered by radioactive decays within the ejecta ("Macronovae"), and the radio flares that emerge when the ejecta dissipate their large kinetic energies in the ambient medium.Comment: accepted in Philosophical Transactions A; references update

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Section: (E) Electromagnetic Transientsmentioning

confidence: 99%

The dynamic ejecta of compact object mergers and eccentric collisions

Rosswog

2013

Phil. Trans. R. Soc. A.

101

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“…The culmination of a century-long search [1][2][3][4][5][6][7][8][9][10], GW detection is now emerging as a new tool with which to study the Universe, illuminating previously invisible astrophysical phenomena. In parallel, the developments of laser cooling and the laser frequency comb have given rise to optical atomic clocks with accuracies and stabilities at the 10 −18 level [11][12][13][14][15].…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave detection with optical lattice atomic clocks

et al. 2016

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We propose a space-based gravitational wave (GW) detector consisting of two spatially separated, dragfree satellites sharing ultrastable optical laser light over a single baseline. Each satellite contains an optical lattice atomic clock, which serves as a sensitive, narrowband detector of the local frequency of the shared laser light. A synchronized two-clock comparison between the satellites will be sensitive to the effective Doppler shifts induced by incident GWs at a level competitive with other proposed space-based GW detectors, while providing complementary features. The detected signal is a differential frequency shift of the shared laser light due to the relative velocity of the satellites, and the detection window can be tuned through the control sequence applied to the atoms' internal states. This scheme enables the detection of GWs from continuous, spectrally narrow sources, such as compact binary inspirals, with frequencies ranging from ∼3 mHz-10 Hz without loss of sensitivity, thereby bridging the detection gap between spacebased and terrestrial optical interferometric GW detectors. Our proposed GW detector employs just two satellites, is compatible with integration with an optical interferometric detector, and requires only realistic improvements to existing ground-based clock and laser technologies.

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“…The first generation detectors LIGO [1,2] and Virgo [3,4] have reached their design sensitivities and collected excellent data over several years of exposure. The second generation detectors, Advanced LIGO [5,6], Advanced Virgo [7], GEO-HF [8], and KaGra [9,10] are currently being built and commissioned.…”

Section: Introductionmentioning

confidence: 99%

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

2012

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International audienceCompact binary coalescences, such as binary neutron stars or black holes, are among the most promising candidate sources for the current and future terrestrial gravitational-wave detectors. While such sources are best searched using matched template techniques and chirp template banks, integrating chirp signals from binaries over the entire universe also leads to a gravitational-wave background (GWB). In this paper we systematically scan the parameter space for the binary coalescence GWB models, taking into account uncertainties in the star formation rate and in the delay time between the formation and coalescence of the binary, and we compare the computed GWB to the expected sensitivities of the second and third generation gravitational-wave detector networks. We find that second generation detectors are likely to detect the binary coalescence GWB, while the third generation detectors will probe most of the available parameter space. The binary coalescence GWB will, in fact, be a foreground for the third generation detectors, potentially masking the GWB background due to cosmological sources. Accessing the cosmological GWB with third generation detectors will therefore require identification and subtraction of all inspiral signals from all binaries in the detectors’ frequency band

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LIGO: the Laser Interferometer Gravitational-Wave Observatory

Cited by 1,088 publications

References 97 publications

The dynamic ejecta of compact object mergers and eccentric collisions

The dynamic ejecta of compact object mergers and eccentric collisions

Gravitational wave detection with optical lattice atomic clocks

Accessibility of the gravitational-wave background due to binary coalescences to second and third generation gravitational-wave detectors

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