1,220 research outputs found
An efficient filter for detecting gravitational wave bursts in interferometric detectors
Typical sources of gravitational wave bursts are supernovae, for which no accurate models exist. This calls for search methods with high efficiency and robustness to be used in the data analysis of foreseen interferometric detectors. A set of such filters is designed to detect gravitational wave burst signals. We first present filters based on the linear fit of whitened data to short straight lines in a given time window and combine them in a non linear filter named ALF. We study the performances and efficiencies of these filters, with the help of a catalogue of simulated supernova signals. The ALF filter is the most performant and most efficient of all filters. Its performance reaches about 80% of the Optimal Filter performance designed for the same signals. Such a filter could be implemented as an online trigger (dedicated to detect bursts of unknown waveform) in interferometric detectors of gravitational waves
A First Comparison Between LIGO and Virgo Inspiral Search Pipelines
This article reports on a project that is the first step the LIGO Scientific
Collaboration and the Virgo Collaboration have taken to prepare for the mutual
search for inspiral signals. The project involved comparing the analysis
pipelines of the two collaborations on data sets prepared by both sides,
containing simulated noise and injected events. The ability of the pipelines to
detect the injected events was checked, and a first comparison of how the
parameters of the events were recovered has been completed.Comment: GWDAW-9 proceeding
Inference of proto-neutron star properties in core-collapse supernovae from a gravitational-wave detector network
The next Galactic core-collapse supernova (CCSN) will be a unique opportunity
to study within a fully multi-messenger approach the explosion mechanism
responsible for the formation of neutron stars and stellar-mass black holes.
State-of-the-art numerical simulations of those events reveal the complexity of
the gravitational-wave emission which is highly stochastic. This challenges the
possibility to infer the properties of the compact remnant and of its
progenitor using the information encoded in the waveforms. In this paper we
take further steps in a program we recently initiated to overcome those
difficulties. In particular we show how oscillation modes of the proto-neutron
star, highly visible in the gravitational-wave signal, can be used to
reconstruct the time evolution of their physical properties. Extending our
previous work where only the information from a single detector was used we
here describe a new data-analysis pipeline that coherently combines
gravitational-wave detectors' data and infers the time evolution of a
combination of the mass and radius of the compact remnant. The performance of
the method is estimated employing waveforms from 2D and 3D CCSN simulations
covering a progenitor mass range between 11\, and
40\, and different equations of state for both a network of
up to five second-generation detectors and the proposed third-generation
detectors Einstein Telescope and Cosmic Explorer. Our study shows that it will
be possible to infer PNS properties for CCSN events occurring in the vicinity
of the Milky Way, up to the Large Magellanic Cloud, with the current generation
of gravitational-wave detectors
A first comparison of search methods for gravitational wave bursts using LIGO and Virgo simulated data
We present a comparative study of 6 search methods for gravitational wave
bursts using simulated LIGO and Virgo noise data. The data's spectra were
chosen to follow the design sensitivity of the two 4km LIGO interferometers and
the 3km Virgo interferometer. The searches were applied on replicas of the data
sets to which 8 different signals were injected. Three figures of merit were
employed in this analysis: (a) Receiver Operator Characteristic curves, (b)
necessary signal to noise ratios for the searches to achieve 50 percent and 90
percent efficiencies, and (c) variance and bias for the estimation of the
arrival time of a gravitational wave burst.Comment: GWDAW9 proceeding
A comparison of methods for gravitational wave burst searches from LIGO and Virgo
The search procedure for burst gravitational waves has been studied using 24
hours of simulated data in a network of three interferometers (Hanford 4-km,
Livingston 4-km and Virgo 3-km are the example interferometers). Several
methods to detect burst events developed in the LIGO Scientific Collaboration
(LSC) and Virgo collaboration have been studied and compared. We have performed
coincidence analysis of the triggers obtained in the different interferometers
with and without simulated signals added to the data. The benefits of having
multiple interferometers of similar sensitivity are demonstrated by comparing
the detection performance of the joint coincidence analysis with LSC and Virgo
only burst searches. Adding Virgo to the LIGO detector network can increase by
50% the detection efficiency for this search. Another advantage of a joint
LIGO-Virgo network is the ability to reconstruct the source sky position. The
reconstruction accuracy depends on the timing measurement accuracy of the
events in each interferometer, and is displayed in this paper with a fixed
source position example.Comment: LIGO-Virgo working group submitted to PR
Gravity Wave and Neutrino Bursts from Stellar Collapse: A Sensitive Test of Neutrino Masses
New methods are proposed with the goal to determine absolute neutrino masses
from the simultaneous observation of the bursts of neutrinos and gravitational
waves emitted during a stellar collapse. It is shown that the neutronization
electron neutrino flash and the maximum amplitude of the gravitational wave
signal are tightly synchronized with the bounce occuring at the end of the core
collapse on a timescale better than 1 ms. The existing underground neutrino
detectors (SuperKamiokande, SNO, ...) and the gravity wave antennas soon to
operate (LIGO, Virgo, ...) are well matched in their performance for detecting
galactic supernovae and for making use of the proposed approach. Several
methods are described, which apply to the different scenarios depending on
neutrino mixing. Given the present knowledge on neutrino oscillations, the
methods proposed are sensitive to a mass range where neutrinos would
essentially be mass-degenerate. The 95 % C.L. upper limit which can be achieved
varies from 0.75 eV/c2 for large electron neutrino survival probabilities to
1.1 eV/c2 when in practice all electron neutrinos convert into muon or tau
neutrinos. The sensitivity is nearly independent of the supernova distance.Comment: 17 pages, 4 figure
The Minimal Supersymmetric Standard Model: Group Summary Report
CONTENTS: 1. Synopsis, 2. The MSSM Spectrum, 3. The Physical Parameters, 4.
Higgs Boson Production and Decays, 5. SUSY Particle Production and Decays, 6.
Experimental Bounds on SUSY Particle Masses, 7. References.Comment: 121 pages, latex + epsfig, graphicx, axodraw, Report of the MSSM
working group for the Workshop "GDR-Supersym\'etrie",France. Rep. PM/98-4
Detection in coincidence of gravitational wave bursts with a network of interferometric detectors (I): Geometric acceptance and timing
Detecting gravitational wave bursts (characterised by short durations and
poorly modelled waveforms) requires to have coincidences between several
interferometric detectors in order to reject non-stationary noise events. As
the wave amplitude seen in a detector depends on its location with respect to
the source direction and as the signal to noise ratio of these bursts are
expected to be low, coincidences between antennas may not be so likely. This
paper investigates this question from a statistical point of view by using a
simple model of a network of detectors; it also estimates the timing precision
of a detection in an interferometer which is an important issue for the
reconstruction of the source location, based on time delays.Comment: low resolution figure 1 due to file size problem
Reconstruction of the gravitational wave signal during the Virgo science runs and independent validation with a photon calibrator
The Virgo detector is a kilometer-scale interferometer for gravitational wave
detection located near Pisa (Italy). About 13 months of data were accumulated
during four science runs (VSR1, VSR2, VSR3 and VSR4) between May 2007 and
September 2011, with increasing sensitivity.
In this paper, the method used to reconstruct, in the range 10 Hz-10 kHz, the
gravitational wave strain time series from the detector signals is
described. The standard consistency checks of the reconstruction are discussed
and used to estimate the systematic uncertainties of the signal as a
function of frequency. Finally, an independent setup, the photon calibrator, is
described and used to validate the reconstructed signal and the
associated uncertainties.
The uncertainties of the time series are estimated to be 8% in
amplitude. The uncertainty of the phase of is 50 mrad at 10 Hz with a
frequency dependence following a delay of 8 s at high frequency. A bias
lower than and depending on the sky direction of the GW is
also present.Comment: 35 pages, 16 figures. Accepted by CQ
- …