Abstract Searches for gravitational waves with km-scale laser interferometers often involve the long-wavelength approximation to describe the detector response. The prevailing assumption is that the corrections to the detector response due to its finite size are small and the errors due to the long-wavelength approximation are negligible. Recently, however, Baskaran and Grishchuk (2004 Class. Q...

The quantum noise of the light field is a fundamental noise source in interferometric gravitational wave detectors. Injected squeezed light is capable of reducing the quantum noise contribution to the detector noise floor to values that surpass the so-called Standard-Quantum-Limit (SQL). In particular, squeezed light is useful for the detection of gravitational waves at high frequencies where i...

Identifying the properties of the first generation of seeds of massive black holes is key to understanding the merger history and growth of galaxies. Mergers between ∼ 100M seed black holes generate gravitational waves in the 0.1–10Hz band that lies between the sensitivity bands of existing ground-based detectors and the planned space-based gravitational wave detector, the Laser Interferometer ...

Assessing the confidence of detection for candidate signals of gravitational waves is a particularly subtle matter. A fundamental step toward this achievement is the validation of the output data of the detectors involved. Here we present how this is accomplished in the operating resonant detector AURIGA by discriminating between satisfactory and unsatisfactory periods of operations on the basi...

Time-frequency based methods, particularly quadratic (Cohen's-class) representations, are often considered for detection in applications ranging from sonar to machine monitoring. We propose a method of obtaining near-optimal quadratic detectors directly from training data using Fisher's optimal linear discriminant to design a quadratic detector. This detector is optimal in terms of Fisher's sca...

ABSTRACT It is expected that interferometric gravitational wave detectors such as LIGO will be eventually limited by fundamental noise sources like shot noise and Brownian motion, as well as by seismic noise. In the commissioning process, other technical noise sources (electronics noise, alignment fluctuations) limit the sensitivity and are eliminated one by one. We propose here a way to correl...

Advancing further the theory of the optimal edge detector, as has been developed by Canny and Spacek, we derive the 'definitive' optimal edge operator. We show that the cubic spline approximation is, in practice, as good as the optimal edge detector.

Abstract In 2002, the interferometric gravitational wave detector GEO 600 took part in a coincident science run (S1) with other detectors world-wide. When completed, GEO will employ a dual-recycling scheme which will allow its peak sensitivity to be tuned over a range of frequencies in the detection band. Still in the commissioning phase, GEO was operated as a power-recycled Michelson for the d...

The LIGO Scientific Collaboration (LSC) glitch group is part of the LIGO detector characterization effort. It consists of data analysts and detector experts who, during and after science runs, collaborate for a better understanding of noise transients in the detectors. Goals of the glitch group during the fifth LIGO science run (S5) included (1) offline assessment of the detector data quality, ...

We consider the use of a microwave parametric converter for the direct detection of gravitational effects at the LHC. Because of the extra dimensions the strength of the gravitational interaction in the bulk grows at high energies. This leads to possibly detectable signals. The existence of additional dimensions has been widely discussed in connection with string theory [1]. It has been propose...