Search for gravitational radiation from Supernova 1993J

Mauceli, Evan; Geng, Z. K.; Hamilton, W. O.; Johnson, W. W.; Merkowitz, Stephen M.; Morse, A.; Solomonson, N.; Astone, P.; Bassan, M.; Bonifazi, P.; Carelli, P.; Coccia, E.; Cosmelli, C.; Fafone, V.; Frasca, S.; Modena, I.; Modestino, G.; Pallottino, G. V.; Pizzella, G.; Rapagnani, P.; Ricci, F.; Terenzi, R.; Visco, M.

doi:10.1103/physrevd.56.6081

Cited by 4 publications

(2 citation statements)

References 3 publications

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“…From these data we generated histograms which show the number of events as a function of voltage squared. Once V 2 ∝ T figure 6 shows how it fits with a thermal distribution [18]…”

Section: Some Results From Data Analysismentioning

confidence: 99%

The Schenberg data acquisition and analysis: results from its first commissioning run

Costa

Aguiar

Oliveira

et al. 2008

Class. Quantum Grav.

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The Mario Schenberg gravitational wave detector has started its commissioning phase at the Physics Institute of the University of Sao Paulo. We have collected almost 200 h of data from the instrument in order to check out its behavior and performance. We have also been developing a data acquisition system for it under a VXI System. Such a system is composed of an analog-to-digital converter and a GPS receiver for time synchronization. We have been building the software that controls and sets up the data acquisition. Here we present an overview of the Mario Schenberg detector and its data acquisition system, some results from the first commissioning run and solutions for some problems we have identified.

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“…From these data we generated histograms which show the number of events as a function of voltage squared. Once V 2 ∝ T figure 6 shows how it fits with a thermal distribution [18]…”

Section: Some Results From Data Analysismentioning

confidence: 99%

The Schenberg data acquisition and analysis: results from its first commissioning run

Costa

Aguiar

Oliveira

et al. 2008

Class. Quantum Grav.

View full text Add to dashboard Cite

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“…Analysis of data recorded by Geograv for SN1987A (Amaldi et al 1987) and by Explorer-Allegro for SN1993J (Mauceli et al 1997), showed that there are GW candidate events, which the authors themselves do not consider as real signals because the GW energy calculated for a standard pulse with a duration τ g = 1 ms (and hence bandwidth 1 kHz) gives E gw ≈ 10 3 M c 2 for both supernovae. However, in the case of pulse duration of about 1 s (and hence bandwidth 1 Hz) the GW energy needed for producing the same GW amplitude is about 1 M c 2 .…”

Section: Discussionmentioning

confidence: 99%

Statistics of the detection rates for tensor and scalar gravitational waves from the Local Galaxy universe

Baryshev

Paturel

2001

A&A

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Abstract. We use data on the local 3-dimensional galaxy distribution for studying the statistics of the detection rates of gravitational waves (GW) coming from supernova explosions. We consider both tensor and scalar gravitational waves which are possible in a wide range of relativistic and quantum gravity theories. We show that statistics of GW events as a function of sidereal time can be used for distinction between scalar and tensor gravitational waves because of the anisotropy of spatial galaxy distribution. For calculation of the expected amplitudes of GW signals we use the values of the released GW energy, frequency and duration of GW pulse which are consistent with existing scenarios of SN core collapse. The amplitudes of the signals produced by Virgo and the Great Attractor clusters of galaxies is expressed as a function of the sidereal time for resonant bar detectors operating now (IGEC) and for forthcoming laser interferometric detectors (VIRGO). Then, we calculate the expected number of GW events as a function of sidereal time produced by all the galaxies within 100 Mpc. In the case of axisymmetric rotational core collapse which radiates a GW energy of 10 −9 M c 2 , only the closest explosions can be detected. However, in the case of nonaxisymmetric supernova explosion, due to such phenomena as centrifugal hangup, bar and lump formation, the GW radiation could be as strong as that from a coalescing neutron-star binary. For radiated GW energy higher than 10 −6 M c 2 and sensitivity of detectors at the level h ≈ 10 −23 it is possible to detect Virgo cluster and Great Attractor, and hence to use the statistics of GW events for testing gravity theories.

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Observational Limit on Gravitational Waves from Binary Neutron Stars in the Galaxy

et al. 1999

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Using optimal matched filtering, we search 25 hours of data from the LIGO 40-m prototype laser interferometric gravitational-wave detector for gravitational-wave chirps emitted by coalescing binary systems within our Galaxy. This is the first test of this filtering technique on real interferometric data. An upper limit on the rate R of neutron star binary inspirals in our Galaxy is obtained: with 90% confidence, R , 0.5 h 21 . Similar experiments with LIGO interferometers will provide constraints on the population of tight binary neutron star systems in the Universe.

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Search for gravitational radiation from Supernova 1993J

Cited by 4 publications

References 3 publications

The Schenberg data acquisition and analysis: results from its first commissioning run

The Schenberg data acquisition and analysis: results from its first commissioning run

Statistics of the detection rates for tensor and scalar gravitational waves from the Local Galaxy universe

Observational Limit on Gravitational Waves from Binary Neutron Stars in the Galaxy

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