Constraints on Cosmic Strings from the LIGO-Virgo Gravitational-Wave Detectors

Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Accadia, T.; Acernese, F.; Adams, C.; Adams, T.; Adhikari, R. X.; Affeldt, C.; Agathos, M.; Aggarwal, N.; Aguiar, O. D.; Ajith, P.; Allen, B.; Allocca, A.; Ceron, E. Amador; Amariutei, D.; Anderson, R. A.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya, M. C.; Arceneaux, C. C.; Areeda, J. S.; Ast, S.; Aston, S. M.; Astone, P.; Aufmuth, P.; Aulbert, C.; Austin, Larry; Aylott, B. E.; Babak, S.; Baker, P. T.; Ballardin, G.; Ballmer, S. W.; Barayoga, J. C.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Bauchrowitz, J.; Bauer, Th.; Bebronne, M.; Behnke, B.; Bejger, M.; Beker, M. G.; Bell, A. S.; Bell, C.; Belopolski, Ilya; Bergmann, G.; Berliner, J. M.; Bersanetti, D.; Bertolini, A.; Bessis, D.; Betzwieser, J.; Beyersdorf, P. T.; Bhadbhade, T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, David; Blom, M.; Böck, O.; Bodiya, T. P.; Boër, M.; Bogan, C.; Bond, C.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bowers, J.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brannen, Carl; Brau, J.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brückner, Frank; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, Robert L.; Cadonati, L.; Cagnoli, G.; Bustillo, J. Calderón; Calloni, E.; Camp, J. B.; Campsie, P.; Cannon, K. C.; Canuel, B.; Cao, Junwei; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.; Castiglia, A.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chakraborty, R.; Chalermsongsak, T.; Chao, S.; Charlton, P.; Chassande–Mottin, E.; Chen, X.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow, J. H.; Christensen, N.; Chu, Q.; Chua, S.; Chung, S.; Ciani, G.; Clara, F.; Clark, D.; Clark, J. A.; Cleva, F.; Coccia, E.; Cohadon, P.-F.; Colla, A.; Colombini, M.; Constancio, M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M. W.; Coulon, J.‐P.; Countryman, S. T.; Couvares, P.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Craig, K.; Creighton, J. D. E.; Creighton, T. D.; Crowder, S. G.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Canton, T. Dal; Damjanic, M.; Danilishin, S. L.; D’Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza, H.; Davier, M.; Davies, G. S.; Daw, E. J.; Day, R.; Dayanga, T.; Rosa, R. De; Debreczeni, G.; Degallaix, J.; Pozzo, W. Del; Deleeuw, E.; Deléglise, S.; Denker, T.; Dent, T.; Dereli, H.; Dergachev, V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Fiore, L. Di; Lieto, A. Di; Palma, I. Di; Virgilio, A. Di; Díaz, M. C.; Dietz, A.; Dmitry, K.; Donovan, F.; Dooley, K. 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L.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Münch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nagy, M. F.; Kumar, D. Nanda; Nardecchia, I.; Nash, T.; Naticchioni, L.; Nayak, R. K.; Necula, V.; Nelemans, G.; Neri, I.; Néri, M.; Newton, G.; Nguyen, T. T.; Nishida, E.; Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Ochsner, E.; O’Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, Sang Hoon; Ohme, F.; Oppermann, P.; O’Reilly, B.; Larcher, W. Ortega; O’Shaughnessy, R.; Osthelder, C.; Ott, Christian D.; Ottaway, D. J.; Ottens, R. S.; Ou, J.; Overmier, H.; Owen, B. J.; Padilla, C.; Pai, A.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Paoletti, R.; Papa, M. A.; Paris, H. R.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Pedraza, M.; Peiris, P.; Penn, S.; Perreca, A.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pierro, V.; Pinard, L.; Pindor, B.; Pinto, I. M.; Pitkin, M.; Poeld, J.; Poggiani, R.; Poole, V.; Poux, C.; Predoi, V.; Prestegard, T.; Price, Larry R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Rácz, István; Radkins, H.; Raffai, P.; Raja, S.; Rajalakshmi, G.; Rakhmanov, M.; Ramet, C.; Rapagnani, P.; Raymond, V.; Re, V.; Reed, C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, Rolf; Riles, K.; Robertson, N. A.; Robinet, F.; Rocchi, A.; Roddy, S.; Rodriguez, Carl L.; Rodruck, M.; Roever, C.; Rolland, L.; Rollins, J. G.; Romano, R.; Romanov, G.; Romie, J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Salemi, F.; Sammut, L.; Sandberg, V.; Sanders, J. R.; Sannibale, V.; Santiago-Prieto, I.; Saracco, E.; Sassolas, B.; Sathyaprakash, B. S.; Saulson, P. R.; Savage, R. L.; Schilling, R.; Schnabel, R.; Schofield, R. M. 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doi:10.1103/physrevlett.112.131101

Cited by 113 publications

(118 citation statements)

References 40 publications

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“…Similar techniques have been implemented for detecting gravitational-wave bursts [94] and cosmic strings [95]. The training of the classifier uses two sets of data: a collection of coincidences associated with simulated signals and a collection of accidental coincidences that act as a proxy for the background.…”

Section: Ranking Eventsmentioning

confidence: 99%

Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005–2010

Aasi¹,

Abbott²,

Abbott³

et al. 2014

Phys. Rev. D

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We report results from a search for gravitational waves produced by perturbed intermediate mass black holes (IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency 50 ≤ f 0 =Hz ≤ 2000 and decay timescale 0.0001 ≲ τ=s ≲ 0.1 characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass 50 ≤ M=M ⊙ ≤ 450 and component mass ratios of either 1:1 or 4:1. For systems with total mass 100 ≤ M=M ⊙ ≤ 150, we report a 90% confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of 6.9 × 10 −8 Mpc −3 yr −1 . We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1% of their mass as gravitational waves in the fundamental, l ¼ m ¼ 2, oscillation mode, that is nearly three orders of magnitude more stringent than previous results.

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Section: Ranking Eventsmentioning

confidence: 99%

Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005–2010

Aasi¹,

Abbott²,

Abbott³

et al. 2014

Phys. Rev. D

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“…The main phenomenological consequence of a string network is the emission of Gravitational Waves (GWs) [28][29][30][31][32][33][34][35][36][37], generating bursts as well as a stochastic background of gravity waves. Indeed, several features such as cusps (points temporarily reaching the speed of light c = 1), kinks (discontinuities of the tangent vector created by intercommutation processes) and junctions, produce high frequency GW Bursts (GWBs).…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave bursts from cosmic string cusps and pseudocusps

2017

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We study the relative contribution of cusps and pseudocusps, on cosmic (super)strings, to the emitted bursts of gravitational waves. The gravitational wave emission in the vicinity of highly relativistic points on the string follows, for a high enough frequency, a logarithmic decrease. The slope has been analytically found to be − 4 /3 for points reaching exactly the speed of light in the limit c = 1. We investigate the variations of this high frequency behaviour with respect to the velocity of the points considered, for strings formed through a numerical simulation, and we then compute numerically the gravitational waves emitted. We find that for string points moving with velocities as far as 10 −3 from the theoretical (relativistic) limit c = 1, gravitational wave emission follows a behaviour consistent with that of cusps, effectively increasing the number of cusps on a string. Indeed, depending on the velocity threshold chosen for such behaviour, we show the emitting part of the string worldsheet is enhanced by a factor O(10 3 ) with respect to the emission of cusps only.

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“…Empirical upper bounds on Gµ/c 2 have been derived from null results for experiments involving gravitational lensing (Vilenkin 1981;Hogan & Narayan 1984;Vilenkin 1984;de Laix 1997;Bernardeau & Uzan 2001;Sazhin et al 2003Sazhin et al , 2006Christiansen et al 2008), gravitational wave background and bursts (Vachaspati & Vilenkin 1985;Economou et al 1992;Battye et al 1997;Damour & Vilenkin 2000Siemens et al 2006;Hogan 2006;Siemens et al 2007;Abbott et al 2007Abbott et al , 2009bAasi et al 2014;Abbott et al 2017), pulsar timing (Bouchet & Bennett 1990;Caldwell & Allen 1992;Kaspi et al 1994;Jenet et al 2006;DePies & Hogan 2007;Blanco-Pillado & Olum 2017;Blanco-Pillado et al 2018) and CMB radiation (Smoot et al 1992;Bennett et al 1996;Pogosian et al 2003Pogosian et al , 2004Tye et al 2005;Wyman et al 2005;Pogosian et al 2006;Seljak et al 2006;Spergel et al 2007;Bevis et al 2007;Fraisse 2007;Pogosian et al 2009;Ade et al 2014). presented the first observatio...…”

Section: Introductionmentioning

confidence: 99%

Prospects of cosmic superstring detection through microlensing of extragalactic point-like sources

Chernoff

Goobar

Renk

2019

Monthly Notices of the Royal Astronomical Society

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The existence of cosmic superstrings may be probed by astronomical time domain surveys. When crossing the line of sight to point-like sources, strings produce a distinctive microlensing signature. We consider two avenues to hunt for a relic population of superstring loops: frequent monitoring of (1) stars in Andromeda, lensed by loops in the haloes of the Milky-Way and Andromeda and (2) supernovae at cosmological distances, lensed by loops in the intergalactic medium. We assess the potential of such experiments to detect and/or constrain strings with a range of tensions, 10 −15 Gµ/c 2 10 −6 . The practical sensitivity is tied to cadence of observations which we explore in detail. We forecast that high-cadence monitoring of ∼ 10 5 stars on the far side of Andromeda over a year-long period will detect microlensing events if Gµ/c 2 ∼ 10 −13 , while ∼ 10 6 stars will detect events if 10 −13.5 < Gµ/c 2 < 10 −11.5 ; the upper and lower bounds of the accessible tension range continue to expand as the number of stars rises. We also analyse the ability to reject models in the absence of fluctuations. While challenging, these studies are within reach of forthcoming timedomain surveys. Supernova observations can hypothetically constrain models with 10 −12 < Gµ/c 2 < 10 −6 without any optimization of the survey cadence. However, the event rate forecast suggests it will be difficult to reject models of interest. As a demonstration, we use observations from the Pantheon Type Ia supernova cosmology data-set to place modest constraints on the number density of cosmic superstrings in a poorly tested region of the parameter space.

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Constraints on Cosmic Strings from the LIGO-Virgo Gravitational-Wave Detectors

Cited by 113 publications

References 40 publications

Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005–2010

Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005–2010

Gravitational wave bursts from cosmic string cusps and pseudocusps

Prospects of cosmic superstring detection through microlensing of extragalactic point-like sources

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