Gravitational waves by gamma-ray bursts and the Virgo detector: the case of GRB 050915a

Acernese, F.; Amico, P.; Alshourbagy, M.; Antonucci, F.; Aoudia, S.; Astone, P.; Avino, S.; Babusci, D.; Ballardin, G.; Barone, F.; Barsotti, L.; Barsuglia, M.; Bauer, Th.; Beauville, F.; Bigotta, S.; Birindelli, S.; Bizouard, M. A.; Boccara, Claude; Bondu, F.; Bosi, L.; Bradaschia, C.; Braccini, S.; Brand, J. van den; Brillet, A.; Brisson, V.; Buskulic, D.; Calloni, E.; Campagna, E.; Carbognani, F.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande–Mottin, E.; Christensen, N.; Corda, Christian; Corsi, A.; Cottone, F.; Clapson, A. C.; Cleva, F.; Coulon, J.‐P.; Cuoco, E.; Dari, A.; Dattilo, V.; Davier, M.; Prete, M. Del; Rosa, R. De; Fiore, L. Di; Virgilio, A. Di; Dujardin, B.; Eleuteri, A.; Evans, M.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garufi, F.; Genin, É.; Gennai, A.; Giazotto, A.; Giordano, G.; Giordano, L.; Gouaty, R.; Grosjean, Daniel; Guidi, G. M.; Hamdani, S.; Hebri, S.; Heitmann, H.; Hello, P.; Huet, D.; Karkar, S.; Kreckelbergh, S.; Penna, P. La; Laval, M.; Leroy, N.; Letendre, N.; López, B.; Lorenzini, M.; Loriette, V.; Losurdo, G.; Mackowski, J.‐M.; Majorana, E.; Man, C. N.; Mantovani, M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Mazzoni, M.; Milano, L.; Menzinger, F.; Moins, C.; Moreau, Julien; Morgado, N.; Mours, B.; Nocera, F.; Palomba, C.; Paoletti, F.; Pardi, S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Piergiovanni, F.; Pinard, L.; Poggiani, R.; Punturo, M.; Puppo, P.; Putten, S. van der; Qipiani, K.; Rapagnani, P.; Reita, V.; Remillieux, A.; Ricci, F.; Ricciardi, I.; Ruggi, P.; Russo, G.; Solimeno, S.; Spallicci, A.; Tarallo, M.; Tonelli, M.; Toncelli, A.; Tournefier, E.; Travasso, F.; Tremola, C.; Vajente, G.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinet, J.-Y.; Vocca, H.; Yvert, M.

doi:10.1088/0264-9381/24/19/s29

Cited by 19 publications

(12 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using a lattice structure [49] we can implement the whitening filter in time domain. This is a procedure which is used for other pipeline [17,52] and which can be implemented also in adaptive way [53] taking care of non stationary noise.…”

Section: Whitening Proceduresmentioning

confidence: 99%

Image-based deep learning for classification of noise transients in gravitational wave detectors

Razzano

Cuoco

2018

Class. Quantum Grav.

View full text Add to dashboard Cite

The detection of gravitational waves has inaugurated the era of gravitational astronomy and opened new avenues for the multimessenger study of cosmic sources. Thanks to their sensitivity, the Advanced LIGO and Advanced Virgo interferometers will probe a much larger volume of space and expand the capability of discovering new gravitational wave emitters. The characterization of these detectors is a primary task in order to recognize the main sources of noise and optimize the sensitivity of interferometers. Glitches are transient noise events that can impact the data quality of the interferometers and their classification is an important task for detector characterization. Deep learning techniques are a promising tool for the recognition and classification of glitches. We present a classification pipeline that exploits convolutional neural networks to classify glitches starting from their timefrequency evolution represented as images. We evaluated the classification accuracy on simulated glitches, showing that the proposed algorithm can automatically classify glitches on very fast timescales and with high accuracy, thus providing a promising tool for online detector characterization.

show abstract

Section: Whitening Proceduresmentioning

confidence: 99%

Image-based deep learning for classification of noise transients in gravitational wave detectors

Razzano

Cuoco

2018

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…Over the last decade, the LIGO and Virgo gravitational wave (GW) detectors have carried out triggered (or targeted) GW searches in coincidence with Gamma-Ray Bursts (GRBs) and other electromagnetic transients [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15] as well as persistent electromagnetic sources [16][17][18][19][20][21][22][23][24][25][26][27][28]. These searches have traditionally been optimized to detect well-modeled "chirp" signals from neutron star (NS)-NS and/or black-hole (BH)-NS binary inspirals, unmodeled short ( 1 − 10 s) duration bursts of GWs in association with electromagnetic transients, and persistent (continuous) GWs from nearby rotating NSs.…”

Section: Introductionmentioning

confidence: 99%

Cross-correlation method for intermediate-duration gravitational wave searches associated with gamma-ray bursts

2016

View full text Add to dashboard Cite

Several models of gamma-ray burst progenitors suggest that the gamma-ray event may be followed by gravitational wave signals of 10 3 -10 4 seconds duration (possibly accompanying the so-called X-ray afterglow "plateaus"). We term these signals "intermediate-duration" because they are shorter than continuous wave signals but longer than signals traditionally considered as gravitational wave bursts, and are difficult to detect with most burst and continuous wave methods. The cross-correlation technique proposed by [S. Dhurandhar et al., Phys. Rev. D 77, 082001 (2008)], which so far has been used only on continuous wave signals, in principle unifies both burst and continuous wave (as well as matched filtering and stochastic background) methods, reducing them to different choices of which data to correlate on which time scales. Here we perform the first tuning of this cross-correlation technique to intermediate-duration signals. We derive theoretical estimates of sensitivity in Gaussian noise in different limits of the cross-correlation formalism, and compare them to the performance of a prototype search code on simulated Gaussian-noise data. We estimate that the code is likely able to detect some classes of intermediate-duration signals (such as the ones described in [A. Corsi & P. Mészáros, Astrophys. J., 702, 1171(2009]) from sources located at astrophysically-relevant distances of several tens of Mpc.

show abstract

“…Several searches for GWs associated with GRBs have been performed using data from LIGO and Virgo (Abbott et al 2005(Abbott et al , 2008b; Acernese et al 2007Acernese et al , 2008. Most recently, data from the fifth LIGO science run and the first Virgo science run were analyzed to search for coalescence signals or unmodeled GW bursts associated with 137 GRBs from (Abbott et al 2010b, 2010a.…”

Section: Introductionmentioning

confidence: 99%

Search for Gravitational Waves Associated With Gamma-Ray Bursts During Ligo Science Run 6 and Virgo Science Runs 2 and 3

Abadie¹,

Abbott²,

Abbott³

et al. 2012

ApJ

110

View full text Add to dashboard Cite

We present the results of a search for gravitational waves associated with 154 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments in 2009-2010, during the sixth LIGO science run and the second and third Virgo science runs. We perform two distinct searches: a modeled search for coalescences of either two neutron stars or a neutron star and black hole, and a search for generic, unmodeled gravitational-wave bursts. We find no evidence for gravitational-wave counterparts, either with any individual GRB in this sample or with the population as a whole. For all GRBs we place lower bounds on the distance to the progenitor, under the optimistic assumption of a gravitational-wave emission energy of 10 −2 M c 2 at 150 Hz, with a median limit of 17 Mpc. For short-hard GRBs we place exclusion distances on binary neutron star and neutron-star-black-hole progenitors, using astrophysically motivated priors on the source parameters, with median values of 16 Mpc and 28 Mpc, respectively. These distance limits, while significantly larger than for a search that is not aided by GRB satellite observations, are not large enough to expect a coincidence with a GRB. However, projecting these exclusions to the sensitivities of Advanced LIGO and Virgo, which should begin operation in 2015, we find that the detection of gravitational waves associated with GRBs will become quite possible.

show abstract

Gravitational waves by gamma-ray bursts and the Virgo detector: the case of GRB 050915a

Cited by 19 publications

References 40 publications

Image-based deep learning for classification of noise transients in gravitational wave detectors

Image-based deep learning for classification of noise transients in gravitational wave detectors

Cross-correlation method for intermediate-duration gravitational wave searches associated with gamma-ray bursts

Search for Gravitational Waves Associated With Gamma-Ray Bursts During Ligo Science Run 6 and Virgo Science Runs 2 and 3

Contact Info

Product

Resources

About