The Allegro gravitational wave detector: Data acquisition and analysis

Abstract

We discuss the data acquisition and analysis procedures used on the Allegro gravity wave detector, including a full description of the filtering used for bursts of gravity waves. The uncertainties introduced into timing and signal strength estimates due to stationary noise are measured, giving the windows for both quantities in coincidence searches. ͓S0556-2821͑96͒01414-2͔ PACS number͑s͒: 04.80.Nn

Effect of energy deposited by cosmic-ray particles on interferometric gravitational wave detectors

“…The values of the coefficient α for fused silica and sapphire at 300 K, are 5.5 × 10 −7 /K and 5.0 × 10 −6 /K, respectively. The coefficient α of the alloy Al5056 [80], which is the most popular material of bar resonators [6,7,8,9], is 2.3 × 10 −5 /K. From the above discussion, the advantages of interferometers, the higher strain sensitivity and wider observation band, are canceled by their larger detector size, because exotic-particle detectors must have good displacement sensitivity, not strain sensitivity.…”

“…The upper limits of the flux of nuclearite [69,70] from the operation of resonators were reported [20,21]. Here, we discuss interferometers as exotic-particle detectors in comparison with resonators (bars [6,7,8,9,10]). …”

“…Observation runs have already been performed in several interferometer (LIGO [1], VIRGO [2], GEO [3], TAMA [4], CLIO [5]) and resonator (ALLEGRO [6], EX-PLORER [7], NAUTILUS [8], AURIGA [9], NIOBE [10], MARIO SCHENBERG [11]) projects. In order of gravitational wave detection, the reduction of noise and fake triggers is crucial, since the gravitational wave amplitude and number of events are expected to be small and rare.…”

Big bang nucleosynthesis, matter-antimatter regions, extra relativistic species, and relic gravitational waves

“…Various resonant mass detectors are now operating [21][22][23][24][25]. In [38], the first experiment of cross-correlation…”

“…The experimental efforts are converging towards the possibility of direct detection of stochastically distributed gravitational waves [19,20]. Various resonant mass detectors are now operating at a typical frequency of the order of kHz (Allegro [21], Auriga [22], Explorer [23], Nautilus [24], Niobe [25]) and four Michelson interferometers (GEO-600 [26],TAMA-400 [27], LIGO [29] and VIRGO [28]) will soon be operating in a wide frequency band from a few Hz up to 10 kHz. It is interesting, in the context of ABBN, to elaborate on the possibility that the additional relativistic species are of gravitational origin.…”