12 research outputs found
Outlook for detection of GW inspirals by GRB-triggered searches in the Advanced detector era
Short, hard gamma-ray bursts (GRBs) are believed to originate from the
coalescence of two neutron stars (NSs) or a NS and a black hole (BH). If this
scenario is correct, then short GRBs will be accompanied by the emission of
strong gravitational waves (GWs), detectable by GW observatories such as LIGO,
Virgo, KAGRA, and LIGO-India. As compared with blind, all-sky, all-time GW
searches, externally triggered searches for GW counterparts to short GRBs have
the advantages of both significantly reduced detection threshold due to known
time and sky location and enhanced GW amplitude because of face-on orientation.
Based on the distribution of signal-to-noise ratios in candidate compact binary
coalescence events in the most recent joint LIGO-Virgo data, our analytic
estimates, and our Monte Carlo simulations, we find an effective sensitive
volume for GRB-triggered searches that is about 2 times greater than for an
all-sky, all-time search. For NS-NS systems, a jet angle of 20 degrees, a
gamma-ray satellite field of view of 10% of the sky, and priors with generally
precessing spin, this doubles the number of NS-NS short-GRB and NS-BH short-GRB
associations, to ~3-4% of all detections of NS-NSs and NS-BHs. We also
investigate the power of tests for statistical excesses in lists of
subthreshold events, and show that these are unlikely to reveal a subthreshold
population until finding GW associations to short GRBs is already routine.
Finally, we provide useful formulas for calculating the prior distribution of
GW amplitudes from a compact binary coalescence, for a given GW detector
network and given sky location.Comment: 14 pages, 4 figures, published in PRD; this version includes changes
in final copyedited articl
Searching for stochastic gravitational waves using co-located interferometric detectors
Thesis (S.M.)--Massachusetts Institute of Technology, Dept. of Physics, 2006.Includes bibliographical references (p. 83-85).Despite their intrinsic advantages due to co-location, the two LIGO (Laser Interferometer Gravitational Wave Observatory) Hanford interferometers have not been used in the search for the stochastic gravitational wave background due to their coupling to a shared environment, which may be comparable to or exceed any gravitational signal. In this thesis, using data from LIGO's fourth science run, we demonstrate a technique to relate the H1-H2 coherence to coupling with physical environmental channels. We show that the correspondence is tight enough to correctly identify regions of high and low coupling and the nature of the coupling in the data set. A simple thresholding provides frequency vetoes, which we can use to derive a significantly cleaner coherence spectrum. Next, using this frequency veto technique and data from the first epoch of LIGO's fifth, currently running science run, we design, implement, and perform a search for astrophysical populations of gravitational wave emitters, which emit predominantly in the kilohertz region of the spectrum, a region totally inaccessible to detectors separated by thousands of kilometers. As well as providing us with a proof-of-concept, the results provide an advanced look at the physical results to come from H1-H2 by the end of S5.by Nickolas Fotopoulos.S.M
Detecting transient gravitational waves in non-Gaussian noise with partially redundant analysis methods
There is a broad class of astrophysical sources that produce detectable,
transient, gravitational waves. Some searches for transient gravitational waves
are tailored to known features of these sources. Other searches make few
assumptions about the sources. Typically events are observable with multiple
search techniques. This work describes how to combine the results of searches
that are not independent, treating each search as a classifier for a given
event. This will be shown to improve the overall sensitivity to
gravitational-wave events while directly addressing the problem of consistent
interpretation of multiple trials.Comment: 11 pages, 5 figure
Likelihood-ratio ranking of gravitational-wave candidates in a non-Gaussian background
We describe a general approach to detection of transient gravitational-wave
signals in the presence of non-Gaussian background noise. We prove that under
quite general conditions, the ratio of the likelihood of observed data to
contain a signal to the likelihood of it being a noise fluctuation provides
optimal ranking for the candidate events found in an experiment. The
likelihood-ratio ranking allows us to combine different kinds of data into a
single analysis. We apply the general framework to the problem of unifying the
results of independent experiments and the problem of accounting for
non-Gaussian artifacts in the searches for gravitational waves from compact
binary coalescence in LIGO data. We show analytically and confirm through
simulations that in both cases the likelihood ratio statistic results in an
improved analysis.Comment: 10 pages, 6 figure
Toward Early-Warning Detection of Gravitational Waves from Compact Binary Coalescence
Rapid detection of compact binary coalescence (CBC) with a network of
advanced gravitational-wave detectors will offer a unique opportunity for
multi-messenger astronomy. Prompt detection alerts for the astronomical
community might make it possible to observe the onset of electromagnetic
emission from (CBC). We demonstrate a computationally practical filtering
strategy that could produce early-warning triggers before gravitational
radiation from the final merger has arrived at the detectors.Comment: 16 pages, 7 figures, published in ApJ. Reformatted preprint with
emulateap
Improving the sensitivity of a search for coalescing binary black holes with nonprecessing spins in gravitational wave data
We demonstrate for the first time a search pipeline with improved sensitivity to gravitational waves from coalescing binary black holes with spins aligned to the orbital angular momentum by the inclusion of spin effects in the search templates. We study the pipeline recovery of simulated gravitational wave signals from aligned-spin binary black holes added to real detector noise, comparing the pipeline performance with aligned-spin filter templates to the same pipeline with nonspinning filter templates. Our results exploit a three-parameter phenomenological waveform family that models the full inspiral-merger-ringdown coalescence and treats the effect of aligned spins with a single effective spin parameter χ. We construct template banks from these waveforms by a stochastic placement method and use these banks as filters in the recently developed gstlal search pipeline. We measure the observable volume of the analysis pipeline for binary black hole signals with M_(total) and χ∈[0,0.85]. We find an increase in observable volume of up to 45% for systems with 0.2≤χ≤0.85 with almost no loss of sensitivity to signals with 0≤χ≤0.2. We also show that the use of spinning templates in the search pipeline provides for more accurate recovery of the binary mass parameters as well as an estimate of the effective spin parameter. We demonstrate this analysis on 25.9 days of data obtained from the Hanford and Livingston detectors in LIGO’s fifth observation run
Searching for stochastic gravitational waves using data from the two colocated LIGO Hanford detectors
Searches for a stochastic gravitational-wave background (SGWB) using terrestrial detectors typically involve cross-correlating data from pairs of detectors. The sensitivity of such cross-correlation analyses depends, among other things, on the separation between the two detectors: the smaller the separation, the better the sensitivity. Hence, a colocated detector pair is more sensitive to a gravitational-wave background than a noncolocated detector pair. However, colocated detectors are also expected to suffer from correlated noise from instrumental and environmental effects that could contaminate the measurement of the background. Hence, methods to identify and mitigate the effects of correlated noise are necessary to achieve the potential increase in sensitivity of colocated detectors. Here we report on the first SGWB analysis using the two LIGO Hanford detectors and address the complications arising from correlated environmental noise. We apply correlated noise identification and mitigation techniques to data taken by the two LIGO Hanford detectors, H1 and H2, during LIGO’s fifth science run. At low frequencies, 40–460 Hz, we are unable to sufficiently mitigate the correlated noise to a level where we may confidently measure or bound the stochastic gravitational-wave signal. However, at high frequencies, 460–1000 Hz, these techniques are sufficient to set a 95% confidence level upper limit on the gravitational-wave energy density of Ω(f) < 7.7 × 10[superscript -4](f/900 Hz)[superscript 3], which improves on the previous upper limit by a factor of ~180. In doing so, we demonstrate techniques that will be useful for future searches using advanced detectors, where correlated noise (e.g., from global magnetic fields) may affect even widely separated detectors.National Science Foundation (U.S.)United States. National Aeronautics and Space AdministrationCarnegie TrustDavid & Lucile Packard FoundationAlfred P. Sloan Foundatio