656 research outputs found
Benefits of joint LIGO -- Virgo coincidence searches for burst and inspiral signals
We examine the benefits of performing a joint LIGO--Virgo search for
transient signals. We do this by adding burst and inspiral signals to 24 hours
of simulated detector data. We find significant advantages to performing a
joint coincidence analysis, above either a LIGO only or Virgo only search.
These include an increased detection efficiency, at a fixed false alarm rate,
to both burst and inspiral events and an ability to reconstruct the sky
location of a signal.Comment: 11 pages 8 figures, Amaldi 6 proceeding
Search for gravitational radiation from intermediate mass black hole binaries in data from the second LIGO-Virgo joint science run
Paper producido por "The LIGO Scientific Collaboration and the Virgo Collaboration". (En el registro se mencionan solo algunos autores de las decenas de personas que participan).Journal reference: Phys. Rev. D 89, 122003 (2014)This paper reports on an unmodeled, all-sky search for gravitational waves from merging intermediate mass black hole binaries (IMBHB). The search was performed on data from the second joint science run of the LIGO and Virgo detectors (July 2009 - October 2010) and was sensitive to IMBHBs with a range up to âŒ200 Mpc, averaged over the possible sky positions and inclinations of the binaries with respect to the line of sight. No significant candidate was found. Upper limits on the coalescence-rate density of nonspinning IMBHBs with total masses between 100 and 450 Mâ and mass ratios between 0.25 and 1 were placed by combining this analysis with an analogous search performed on data from the first LIGO-Virgo joint science run (November 2005 - October 2007). The most stringent limit was set for systems consisting of two 88 Mâ black holes and is equal to 0.12 Mpcâ3 Myrâ1 at the 90% confidence level. This paper also presents the first estimate, for the case of an unmodeled analysis, of the impact on the search range of IMBHB spin configurations: the visible volume for IMBHBs with nonspinning components is roughly doubled for a population of IMBHBs with spins aligned with the binary's orbital angular momentum and uniformly distributed in the dimensionless spin parameter up to 0.8, whereas an analogous population with antialigned spins decreases the visible volume by âŒ20%.http://journals.aps.org/prd/abstract/10.1103/PhysRevD.89.122003submittedVersionFil: Aasi, J. LIGO. California Institute of Technology; Estados Unidos de AmĂ©rica.Fil: Maglione, C. Argentinian Gravitational Wave Group; Argentina.Fil: Quiroga, G. Argentinian Gravitational Wave Group; Argentina.FĂsica de PartĂculas y Campo
Search of the Orion spur for continuous gravitational waves using a loosely coherent algorithm on data from LIGO interferometers
We report results of a wideband search for periodic gravitational waves from isolated neutron stars within the Orion spur towards both the inner and outer regions of our Galaxy. As gravitational waves interact very weakly with matter, the search is unimpeded by dust and concentrations of stars. One search disk (A) is 6.87° in diameter and centered on 20h10m54.71s+33°33âČ25.29âČâČ, and the other (B) is 7.45° in diameter and centered on 8h35m20.61sâ46°49âČ25.151âČâČ. We explored the frequency range of 50â1500 Hz and frequency derivative from 0 to â5Ă10â9ââHz/s. A multistage, loosely coherent search program allowed probing more deeply than before in these two regions, while increasing coherence length with every stage. Rigorous follow-up parameters have winnowed the initial coincidence set to only 70 candidates, to be examined manually. None of those 70 candidates proved to be consistent with an isolated gravitational-wave emitter, and 95% confidence level upper limits were placed on continuous-wave strain amplitudes. Near 169 Hz we achieve our lowest 95% C.L. upper limit on the worst-case linearly polarized strain amplitude h0 of 6.3Ă10â25, while at the high end of our frequency range we achieve a worst-case upper limit of 3.4Ă10â24 for all polarizations and sky locations
Search for gravitational waves associated with gamma-ray bursts during the first Advanced LIGO observing run and implications for the origin of GRB 150906B
We present the results of the search for gravitational waves (GWs) associated with Îł-ray bursts detected during the first observing run of the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO). We find no evidence of a GW signal for any of the 41 Îł-ray bursts for which LIGO data are available with sufficient duration. For all Îł-ray bursts, we place lower bounds on the distance to the source using the optimistic assumption that GWs with an energy of 10^(-2)M_âc^2 were emitted within the 16â500 Hz band, and we find a median 90% confidence limit of 71 Mpc at 150 Hz. For the subset of 19 short/hard Îł-ray bursts, we place lower bounds on distance with a median 90% confidence limit of 90 Mpc for binary neutron star (BNS) coalescences, and 150 and 139 Mpc for neutron starâblack hole coalescences with spins aligned to the orbital angular momentum and in a generic configuration, respectively. These are the highest distance limits ever achieved by GW searches. We also discuss in detail the results of the search for GWs associated with GRB 150906B, an event that was localized by the InterPlanetary Network near the local galaxy NGC 3313, which is at a luminosity distance of 54 Mpc (z = 0.0124). Assuming the Îł-ray emission is beamed with a jet half-opening angle â©œ30°, we exclude a BNS and a neutron starâblack hole in NGC 3313 as the progenitor of this event with confidence >99%. Further, we exclude such progenitors up to a distance of 102 Mpc and 170 Mpc, respectively
All-sky search for long-duration gravitational wave transients with initial LIGO
We present the results of a search for long-duration gravitational wave transients in two sets of data collected by the LIGO Hanford and LIGO Livingston detectors between November 5, 2005 and September 30, 2007, and July 7, 2009 and October 20, 2010, with a total observational time of 283.0 days and 132.9 days, respectively. The search targets gravitational wave transients of duration 10â500 s in a frequency band of 40â1000 Hz, with minimal assumptions about the signal waveform, polarization, source direction, or time of occurrence. All candidate triggers were consistent with the expected background; as a result we set 90% confidence upper limits on the rate of long-duration gravitational wave transients for different types of gravitational wave signals. For signals from black hole accretion disk instabilities, we set upper limits on the source rate density between 3.4 Ă 10â5 and 9.4 Ă 10â4 Mpcâ3 yrâ1 at 90% confidence. These are the first results from an all-sky search for unmodeled long-duration transient gravitational waves
Characterization of transient noise in Advanced LIGO relevant to gravitational wave signal GW150914
On 14 September 2015, a gravitational wave signal from a coalescing black hole binary system was observed by the Advanced LIGO detectors. This paper describes the transient noise backgrounds used to determine the significance of the event (designated GW150914) and presents the results of investigations into potential correlated or uncorrelated sources of transient noise in the detectors around the time of the event. The detectors were operating nominally at the time of GW150914. We have ruled out environmental influences and non-Gaussian instrument noise at either LIGO detector as the cause of the observed gravitational wave signal
Observing gravitational-wave transient GW150914 with minimal assumptions
The gravitational-wave signal GW150914 was first identified on September 14, 2015, by searches for
short-duration gravitational-wave transients. These searches identify time-correlated transients in multiple
detectors with minimal assumptions about the signal morphology, allowing them to be sensitive to
gravitational waves emitted by a wide range of sources including binary black hole mergers. Over the
observational period from September 12 to October 20, 2015, these transient searches were sensitive to
binary black hole mergers similar to GW150914 to an average distance of âŒ600 Mpc. In this paper, we
describe the analyses that first detected GW150914 as well as the parameter estimation and waveform
reconstruction techniques that initially identified GW150914 as the merger of two black holes. We find that
the reconstructed waveform is consistent with the signal from a binary black hole merger with a chirp mass
of âŒ30 Mâ and a total mass before merger of âŒ70 Mâ in the detector frame
High-energy neutrino follow-up search of gravitational wave event GW150914 with ANTARES and IceCube
Copyright © 2016 American Physical Society and reproduced in accordance with the publisher copyright policyWe present the high-energy-neutrino follow-up observations of the first gravitational wave transient GW150914 observed by the Advanced LIGO detectors on September 14, 2015. We search for coincident neutrino candidates within the data recorded by the IceCube and Antares neutrino detectors. A possible joint detection could be used in targeted electromagnetic follow-up observations, given the significantly better angular resolution of neutrino events compared to gravitational waves. We find no neutrino candidates in both temporal and spatial coincidence with the gravitational wave event. Within
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of the gravitational wave event, the number of neutrino candidates detected by IceCube and Antares were three and zero, respectively. This is consistent with the expected atmospheric background, and none of the neutrino candidates were directionally coincident with GW150914. We use this nondetection to constrain neutrino emission from the gravitational-wave event
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