1,006 research outputs found
On the (In)Efficiency of the Cross-Correlation Statistic for Gravitational Wave Stochastic Background Signals with Non-Gaussian Noise and Heterogeneous Detector Sensitivities
Under standard assumptions including stationary and serially uncorrelated
Gaussian gravitational wave stochastic background signal and noise
distributions, as well as homogenous detector sensitivities, the standard
cross-correlation detection statistic is known to be optimal in the sense of
minimizing the probability of a false dismissal at a fixed value of the
probability of a false alarm. The focus of this paper is to analyze the
comparative efficiency of this statistic, versus a simple alternative statistic
obtained by cross-correlating the \textit{squared} measurements, in situations
that deviate from such standard assumptions. We find that differences in
detector sensitivities have a large impact on the comparative efficiency of the
cross-correlation detection statistic, which is dominated by the alternative
statistic when these differences reach one order of magnitude. This effect
holds even when both the signal and noise distributions are Gaussian. While the
presence of non-Gaussian signals has no material impact for reasonable
parameter values, the relative inefficiency of the cross-correlation statistic
is less prominent for fat-tailed noise distributions but it is magnified in
case noise distributions have skewness parameters of opposite signs. Our
results suggest that introducing an alternative detection statistic can lead to
noticeable sensitivity gains when noise distributions are possibly non-Gaussian
and/or when detector sensitivities exhibit substantial differences, a situation
that is expected to hold in joint detections from Advanced LIGO and Advanced
Virgo, in particular in the early phases of development of the detectors, or in
joint detections from Advanced LIGO and Einstein Telescope.Comment: 36 pages, 5 figures and 1 table, accepted for publication in Physical
Review
Astrophysical Sources of Stochastic Gravitational-Wave Background
We review the spectral properties of stochastic backgrounds of astrophysical
origin and discuss how they may differ from the primordial contribution by
their statistical properties. We show that stochastic searches with the next
generation of terrestrial interferometers could put interesting constrains on
the physical properties of astrophysical populations, such as the ellipticity
and magnetic field of magnetars, or the coalescence rate of compact binaries.Comment: 12 pages, 3 figures,accepted for publication in CQG, GWDAW12
conference proceedings version corrected in comparison published version
where we found an error in equation (4
A Semi-Parametric Approach to the Detection of Non-Gaussian Gravitational Wave Stochastic Backgrounds
Using a semi-parametric approach based on the fourth-order Edgeworth
expansion for the unknown signal distribution, we derive an explicit expression
for the likelihood detection statistic in the presence of non-normally
distributed gravitational wave stochastic backgrounds. Numerical likelihood
maximization exercises based on Monte-Carlo simulations for a set of large tail
symmetric non-Gaussian distributions suggest that the fourth cumulant of the
signal distribution can be estimated with reasonable precision when the ratio
between the signal and the noise variances is larger than 0.01. The estimation
of higher-order cumulants of the observed gravitational wave signal
distribution is expected to provide additional constraints on astrophysical and
cosmological models.Comment: 26 pages, 3 figures, to appear in Phys. Rev.
Second Einstein Telescope Mock Science Challenge : Detection of the GW Stochastic Background from Compact Binary Coalescences
We present the results of the search for an astrophysical gravitational-wave
stochastic background during the second Einstein Telescope mock data and
science challenge. Assuming that the loudest sources can be detected
individually and removed from the data, we show that the residual background
can be recovered with an accuracy of with the standard cross-correlation
statistic, after correction of a systematic bias due to the non-isotropy of the
sources.Comment: 15 pages, 4 figures, accepted for publication in Physical Review
Searching Gravitational Waves from Pulsars, Using Laser Beam Interferometers
We use recent population synthesis results to investigate the distribution of
pulsars in the frequency space, having a gravitational strain high enough to be
detected by the future generations of laser beam interferometers.
We find that until detectors become able to recover the entire population,
the frequency distribution of the 'detectable' population will be very
dependent on the detector noise curve. Assuming a mean equatorial deformation
, the optimal frequency is around 450 Hz for interferometers
of the first generation (LIGO or VIRGO) and shifts toward 85 Hz for advanced
detectors. An interesting result for future detection stategies is the
significant narrowing of the distribution when improving the sensitivity: with
an advanced detector, it is possible to have 90% of detection probability while
exploring less than 20% of the parameter space (7.5% in the case of ). In addition, we show that in most cases the spindown of
'detectable' pulsars represents a period shift of less than a tens of
nanoseconds after one year of observation, making them easier to follow in the
frequency space.Comment: 5 pages, 3 figures accepted for publication in Astronomy &
Astrophysic
Stochastic Gravitational Wave Background from Coalescing Binary Black Holes
We estimate the stochastic gravitational wave (GW) background signal from the
field population of coalescing binary stellar mass black holes (BHs) throughout
the Universe. This study is motivated by recent observations of BH-Wolf-Rayet
star systems and by new estimates in the metallicity abundances of star forming
galaxies that imply BH-BH systems are more common than previously assumed.
Using recent analytical results of the inspiral-merger-ringdown waveforms for
coalescing binary BH systems, we estimate the resulting stochastic GW
background signal. Assuming average quantities for the single source energy
emissions, we explore the parameter space of chirp mass and local rate density
required for detection by advanced and third generation interferometric GW
detectors. For an average chirp mass of 8.7, we find that detection
through 3 years of cross-correlation by two advanced detectors will require a
rate density, . Combining data from
multiple pairs of detectors can reduce this limit by up to 40%. Investigating
the full parameter space we find that detection could be achieved at rates for populations of coalescing binary BH
systems with average chirp masses of which are predicted by
recent studies of BH-Wolf-Rayet star systems. While this scenario is at the
high end of theoretical estimates, cross-correlation of data by two Einstein
Telescopes could detect this signal under the condition . Such a signal could potentially mask a primordial
GW background signal of dimensionless energy density, , around the (1--500) Hz frequency range.Comment: 22 pages, 5 figures, 2 tables, Accepted for publication by Ap
Measuring neutron-star ellipticity with measurements of the stochastic gravitational-wave background
Galactic neutron stars are a promising source of gravitational waves in the
analysis band of detectors such as LIGO and Virgo. Previous searches for
gravitational waves from neutron stars have focused on the detection of
individual neutron stars, which are either nearby or highly non-spherical. Here
we consider the stochastic gravitational-wave signal arising from the ensemble
of Galactic neutron stars. Using a population synthesis model, we estimate the
single-sigma sensitivity of current and planned gravitational-wave
observatories to average neutron star ellipticity as a function of
the number of in-band Galactic neutron stars . For the plausible
case of , and assuming one year of observation time
with colocated initial LIGO detectors, we find it to be
, which is comparable to current bounds on
some nearby neutron stars. (The current best upper limits are
) It is unclear if Advanced LIGO can
significantly improve on this sensitivity using spatially separated detectors.
For the proposed Einstein Telescope, we estimate that
. Finally, we show that stochastic
measurements can be combined with measurements of individual neutron stars in
order to estimate the number of in-band Galactic neutron stars. In this way,
measurements of stochastic gravitational waves provide a complementary tool for
studying Galactic neutron stars
Gravitation Wave Emission from Radio Pulsars Revisited
We report a new pulsar population synthesis based on Monte Carlo techniques,
aiming to estimate the contribution of galactic radio pulsars to the continuous
gravitational wave emission. Assuming that the rotation periods of pulsars at
birth have a Gaussian distribution, we find that the average initial period is
290 ms. The number of objects with periods equal to or less than 0.4 s, and
therefore capable of being detected by an interferometric gravitational antenna
like VIRGO, is of the order of 5100-7800. With integration times lasting
between 2 and 3 yr, our simulations suggest that about two detections should be
possible, if the mean equatorial ellipticity of the pulsars is
=10. A mean ellipticity an order of magnitude higher increases the
expected number of detections to 12-18, whereas for , no
detections are expectedComment: accepted for publication in A&A, 9 pages, 8 figure
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