Home Search Collections Journals About Contact us My IOPscience

A first search for coincident gravitational waves and high energy neutrinos using LIGO, Virgo and ANTARES data from 2007

This article has been downloaded from IOPscience. Please scroll down to see the full text article. JCAP06(2013)008 (http://iopscience.iop.org/1475-7516/2013/06/008)

View the table of contents for this issue, or go to the journal homepage for more

Download details: IP Address: 128.183.97.246 The article was downloaded on 10/07/2013 at 18:39

Please note that terms and conditions apply. JCAP06(2013)008 hysics P in its 5 line ANTARES , -Virgo data were analysed 10.1088/1475-7516/2013/06/008 LIGO , stroparticle stroparticle doi: A [email protected] , [email protected] , and Virgo, respectively. The osmology and and osmology LIGO C 1205.3018

gravitational waves / experiments, neutrino astronomy We present the results of the first search for gravitational wave bursts associated [email protected]

ournal of ournal An IOP and SISSA journal An IOP and 2013 IOP Publishing Ltd and Sissa Medialab srl E-mail: [email protected] [email protected] c Keywords: ArXiv ePrint: Abstract. The ANTARES collaboration, thethe LIGO Virgo scientific collaboration collaboration and

A first search forgravitational coincident waves and highneutrinos energy using LIGO, VirgoANTARES and data from 2007 J with high energythat neutrinos. are Together, not these observedsearch uses by messengers neutrinos conventional could detected photon by reveal astronomy, the new, particularly underwater neutrino at hidden telescope high sources energy. Our Received April 8, 2013 Accepted April 22, 2013 Published June 7, 2013 configuration during the periodand first January science runs - of September 2007, which coincided with the fifth for candidate gravitational-wave signalsevents. coincident in No time significantjoint and coincident high direction events with energy were thecompare neutrino observed. them neutrino - with We gravitational densities place wave of limits emission merger on and events the core-collapse in events. density the of local universe, and JCAP06(2013)008 9 9 6 4 5 9 7 7 8 9 2 8 3 20 12 12 13 19 15 16 11 11 17 22 10 18 10 21 11 17 19 15 10 33 15 20 33 22 17 –1– 3.2.1 LIGO 3.2.2 Virgo 4.3.1 Description4.3.2 of the algorithm Azimuthal degeneracy of the reconstruction 6.3.1 Injected6.3.2 waveforms Exclusion distances 2.1 Canonical long gamma-ray bursts from massive stars sion 2.2 Low-luminosity GRBs and engine-driven supernovae 2.4 Bursting magnetars 2.3 Mergers and short gamma-ray bursts 2.5 Cosmic string kinks and cusps 3.2 Network of interferometers 3.1 The ANTARES neutrino telescope 3.3 Joint data taking periods 4.1 HEN4.2 data sample Trigger4.3 levels Reconstruction strategy 4.4 Criteria4.5 for HEN event Angular selection 4.6 error Analysis sensitivity and selected HEN candidates 6.1 Per-HEN6.2 GW candidates Search6.3 for a cumulative GW excess: upper binomial limits test 5.1 Search5.2 procedure GW5.3 event analysis GW5.4 search optimisation Low-frequency and high-frequency GW analyses 7.1 Upper7.2 limits on GW-HEN Comparison populations of limits with existing estimates 2 Candidate sources for high-energy neutrino and gravitational wave emis- Contents 1 Introduction 3 GW and HEN detectors 4 Selection of HEN candidates 5 GW search method 6 Coincident search results 7 Astrophysical implications 8 Conclusions The ANTARES collaboration The LIGO and the Virgo collaboration JCAP06(2013)008 ], ], 24 and 127 Collab- LIGO ]and[ ] using data ]. 39 ]). HENs and 12 26 ]andGRBs[ 58 25 ], whereas the most ANTARES 5 ]. These limits, however, ]. The sensitivity of such 33 ]. All-sky model-dependent 7 17 ]. The exclusion distances of 19 ]), GWs carry information on the , 15 146 HEN and GW signals is a strong al- , , 4 ], and jet-driven CCSNe [ 85 GeV) neutrinos (HENs) and gravitational 13 ]. Scientific Collaboration and Virgo placed limits 134 –2– , 59 ] and SGRs [ , 20 LIGO 45 , 6 , 1 ], relativistic shock breakout in compact CCSN progenitor ]. The 143 99 ], SGRs and blazars [ ]. A joint GW-HEN search was first proposed in [ , , 11 29 85 , 130 , 10 , 80 , 8 temporally and spatially coincident 113 , 38 ] and a similar study was carried out with ANTARES data [ 13 ], and cosmic string cusps [ 147 The above HEN and GW searches used timing and sky location information from ob- A search for While HENs are expected to be produced in interactions between relativistic protons Searches for HENs and GWs from such events have thus far relied on blind (i.e., un- Simultaneous emission of GWs and HENs has been proposed in a rangeObservational of constraints cataclysmic on HEN and GW emission from some of these phenomena these searches were, however, not sufficiently large to expectservations of a events GW in detection. theHEN sources electromagnetic may spectrum. be intrinsically Ascopes, electromagnetically potentially but faint, large sufficiently dust-obscured, luminous subset or in ofbut missed GWs by GW are and tele- HEN and not to limited beativistic to, detected. jets partially Such or sources [ may completely include, choked GRBs with, perhaps, only mildly rel- on the GW emission in GRBs [ blind all-sky searches is limitedtiming by and a sky much locations larger from background compared electromagnetic to observations. searches based on oration has placed limits onas the HEN well flux as from a gamma-ray diffuse flaringdo muon blazars not neutrino [ flux yet from strongly extragalacticrelativistic constrain sources outflows HEN [ [ emission and ultra-high-energy cosmic-ray production in Virgo have carried out asitive number such of search all-sky for searches forrecent model-independent GWs. allsky GW search The bursts for most wasconstraints binary recent published and inspiral-merger on in most can [ cosmic sen- be string found in GW [ emission have been placed [ waves (GWs), neither ofare which becoming have new yet tools been for directly exploring observed the from Universe. and astrophysical the sources, external radiation field of the source (e.g., [ triggered) all-sky searches. Anperformed all-sky [ search for point sources of HENs in IceCube data was from the IceCube detector at various levels of completion. Similarly, the stars [ intricate multi-dimensional dynamics inGWs the are source’s thus complementary central messengers. regions (e.g., [ cosmic events including gamma-ray burstsgamma (GRBs), repeater outbursts core-collapse (SGRs), supernovae and, (CCSNe), potentially, soft- cosmic string cusps in thehave early already universe. been obtained.emission in The GRBs IceCube [ collaboration recently placed limits on the HEN 1 Introduction Multi-messenger astronomy is enteringexperimental a techniques stimulating that period will open withcomponents. new the windows In recent of cosmic development particular, radiation of both observation in high-energy all ( its and constraints on joint GW-HEN signals based on the interpretation of independent GW ternative to electromagnetically triggeredHENs or individually. blind Such a all-skybut search analyses still is that enjoys independent search a ofA for much bias similar GWs reduced from idea background or electromagneticneutrino thanks observations, has detector to been timing LVD used [ and in sky the location follow-up constraints. of candidate GW events by the low-energy JCAP06(2013)008 - ]. de- 20 , 4 6 ], and LIGO ]). This 144 149 and conclude ]. 7 we describe the 3 144 HEN telescope and ] than a blind all-sky ] after rescaling for a 6 116 , 89 ] has been done in [ , 5 ANTARES 63 , 54 we discuss sources of coincident HEN describes the search for GWs coincident . These numbers are broadly consistent 2 ◦ ]. Here we present the first direct search 5 1.3, due to the better inherent background 43 –30 ∼ -Virgo network with the detectors operating ◦ is sensitive to HENs with energies greater than data, then the GW data around the time of the –3– LIGO , which is the dominant process (see, e.g., [ μ ν + μ ANTARES ) production ratios of (1 : 2 : 0), changing to approximately ν ANTARES τ ν +¯ e +¯ -Virgo analysis targets model-independent burst GW signals with ν ]), Fermi-accelerated relativistic protons interact with high-energy τ + ν 146 : + reactions leading to pions or kaons, whose decay results in neutrinos, e science run (S5) and the first Virgo science run (VSR1) were carried μ LIGO ν , and Virgo detectors and the joint data taking period. Section pγ → +¯ μ μ ν ν LIGO and Virgo GW observatories from January to September 2007. At this time, + ]. The : LIGO was still under construction and operating with only 5 active lines. At the same + e 1 s and frequencies in the 60 Hz to 500 Hz band. The GW search is extended in , 27 ν μ  +¯ → e LIGO ν + . We discuss the astrophysical implications of the results in section Statistical analyses of theThis HEN paper sample show is no organized sign as of follows. associated GW In bursts. section We analyze a total of 158 HEN events detected at times when two or more of the The basic principle of the analysis presented here is that of a “triggered” search: HEN 6 π sion 100 GeV [ scribes how the HEN samplein was time selected. and Section tion direction with thewith HEN considerations events. of the We potential present for future the joint results GW-HEN of searches. the search in sec- ANTARES and GW emission and expected prospects for their detection. In section frequency up to 2000 Hzof only for such a a subset search of with the the HEN current events, because GW the analysis computational pipeline cost is prohibitive. with estimates for thecoalescence special signals case associated of with dedicated short matched-filter GRBs searches for [e.g., compact binary durations rejection of these specialisedtriggered searches). search will In be either newvalueofthetriggeredsearchevenwhentherelativedetectionrateislow[ case, detections most not of found the by the GW all-sky events blind found search, by illustrating the the smaller distance improvement factor (typically gives ( HEN emission is expected fromcommon baryon-loaded scenario relativistic (e.g., astrophysical [ outflows. In the most e.g., 2 Candidate sources for high-energy neutrino and gravitational wave emis- outflow photons in for coincident GW-HEN events, using data taken by the and HEN observational results were derived in [ Virgo detectors were operating. by the ANTARES time, the fifth out. This was the first joint run of the ∼ near their design sensitivities. candidates are identified in the It has been shown to have a distance reach up to a factor of 2 larger [ HEN event are analyzedmethod for has a been GW applied previously incident in from searches the for GWs HEN associated estimated with arrival GRB direction. triggers [ This predicts a detectionblind rate search for for the beaming angles triggered in search the of range between 5 0.1 and 6 times that of the search of the GWdepends also data, on due theto beaming to of the the the subset reduced triggerused signal, of background. since in sources the The this oriented triggered expected paper search towards is rate to Earth. only of the sensitive The detections LIGO-Virgo comparison blind of all-sky the search [ analysis method JCAP06(2013)008 , 2 . ]. c 76 X  d , 112 ]and 8 M in the counts 2 69 2 , − γ c  42 10 M  1 − GW (a black hole with E to 10 2 ]. c 85  ]. 10 Mpc) one would expect M ∼ 2 collapsar 100 and isotropic equivalent ]. Its GW emission, however, 104 − ]. Typical LGRBs are strongly  10 (an extremely rapidly spinning, 151 ]. 110 ]) and, thus, on the properties of 5 , ∼ ]. LGRBs are detected at a rate of ]). The HEN spectrum depends on 85 83 50 Mpc ( and the directly detectable GW strain , 40 GW ∼ 1 123 76 E − , , 8 cm ], the probability for detection in the 5-line 107 50% for a source at 10 Mpc, which decreases is the time over which 90% of the 1 , ∼ − 76 ]). In both scenarios, HEN emission may result 90 g 68 –4– T 2 [ ), but a significant fraction of local CCSNe may s 109 1 49 − 2.2 -scale water- or ice-Cherenkov detector (e.g., [ 2s; − 3 ] and may continue well into the afterglow phase [ . Equivalently, the minimum GW energy emission de- millisecond magnetar  10 21 erg s − 128 ≈ 90 53 T 4 − ]. Such a scenario may be unlikely given model predictions for ]) or a Gc 93 to 10 , 1 150 − . For example, a source at 10 Mpc needs a quadrupole moment of 61 , ]) is 1 -ray monitors on satellite observatories such as Swift/BAT [ -Virgo network at this distance is approximately − γ that is changing on a millisecond timescale to be detectable by a GW ]. It is important to note, however, that Swift/BAT and Fermi/GBM 103 140 erg s 2 % that at least one HEN is detected for a source at a given distance 51 detector for HENs from the various potential sources by estimating the 105 40% of the prompt emission of all GRBs, respectively. This is due to limited 10 Mpc) LGRB will have a bright multi-wavelength afterglow and may be X , LIGO ∼ ∼ = 46 detector can be estimated to be for frequencies between 100 Hz and 1000 Hz [ P (100 km) 2 c ×  ]). Based on the flux predictions of [ 90% and  M GW emission occurs, at lowest and generally dominant order, via accelerated quadrupo- In the following, we discuss a number of astrophysical scenarios in which both HENs The most extreme scenario for GW emission in LGRBs is dynamical fragmentation of The central engine of LGRBs is expected to either be a HEN emission from canonical LGRBs is expected to have appreciable flux for energies ∼ 2% for a source at 50 Mpc. Note that these are most likely optimistic estimates, since ANTARES M 146 ∼ 1 , lar mass-energy dynamics.GW The emission (e.g., coupling [ constant in the standard quadrupole formula for tectable by the miss Fermi/GBM [ scales with (distance) and GWs may be emitted at detectable levels. 2.1 Canonical long gamma-rayLong-duration bursts GRBs from (LGRBs; massive stars are detected) arenormally observationally leading implicated to core-collapse to supernova explosions be [ related to the collapse of massive stars detector sensitive to a strain of 10 order 1/(few days) by fields of view, technicalA downtime, nearby and (say orbital passes through the South Atlantic Anomaly. accompanied by a CCSN (see section the spectrum of the accelerated protons (e.g., [ to 10 (1 : 1 : 1) at Earth due to flavor oscillations (e.g., [ ∼ 85 ANTARES a collapsing extremely rapidlytwo differentially protoneutron spinning stars stellar [ corethe into rotational a configuration coalescing of system GRB of progenitor stars [e.g., would be very strong, leading to emitted energies more detailed analyses suggest lower HEN fluxes from GRBs [e.g., to beamed and mostluminosities likely of have 10 jets with Lorentz factors Γ extremely magnetized neutron star; e.g., [ have been missed by CCSN surveys based on galaxy catalogs [ the astrophysical source.line In this section,probability we provide estimates of the sensitivity of the 5- from a relativistic expandingbreaks fireball. out of HENs the may stellar envelope begin [ to be produced even before the jet an accretion disk; [ in the range 100 GeV to 100 TeV. For a LGRB at of order 1 (100) HEN events in a km JCAP06(2013)008 , 2 c 92  and M would 22 8 − 2 of order − c at 10 kpc 10  10 ], low-order 20 ]. × M GW . 7 ∼ − 1 2 E , 141 c − ] for a source at 10 6 ]. few  /Virgo detectors, GW 10 92 . ∼ ∼ M 2 E 119 c ∼ h h  M LIGO GW 2 E − Hz with ]. For a source at 10 Mpc, a 3 to 10 124 10 2 c ×  was estimated in [ = 1 — dominated non-axisymmetric ]). LL-GRBs are much more easily ]. A typical GW strain for a deformed M 20 could be of order 1 m 3 ] while the outer regions are inefficiently − ) and the small observable volume (due ]. This part of the GW signal will only − 110 131 GW , , 2.1 126 10 120 E to 10 83 , ∼ 118 Hz to few , 21 , 2 64 black hole. This corresponds to − –5– 57 67 10 10  , at 10 Mpc and frequencies in the 100 Hz to 1000 Hz × M 66 ∼ 21 ]. This and the subsequent ringdown of the newborn , h − 55 ]. 10 117 ∼ 122 h , and radius of 12 km, spinning with a period of 1 ms may be  central black hole, this would yield strains of -ray flux (e.g., [ 121 ]. γ M .  2 4 66 . It is thus detectable only for a Galactic source [ c . M 2  c at a source distance of 10 kpc and emitted energies  M ]. If a black hole with an accretion disk forms, a second phase of GW 20 1 M − at 10 Mpc. If the deformation lasted for 100 ms, − 7 118 − between 100 Hz and 1000 Hz [ 22 , − 2 10 to 10 95 c to 10 10 ,  ∼ 2 21 c × ]. − M 67  7 GW 10 fragment and a 8 − In the collapsar scenario, accretion onto the protoneutron star eventually leads to its In the initial collapse of the progenitor star’s core, a rapidly rotating protoneutron star The accretion torus may be unstable to the Papaloizou-Pringle instability or to co- In more moderate scenarios backed by computational models, GW emission from LGRBs In the speculative suspended accretion model for GRB accretion disks [ In its early evolution, the protoneutron star (or protomagnetar, depending on its mag- More interesting are hydrodynamic instabilities in the accretion disk/torus that forms M 141 few E 2 ,  − ∼ |∼ M h 124 be emitted at 2000 Hz [ black hole leads to a GW burst at few collapse to a spinning black hole [ protoneutron star of 1 emission may come from various hydrodynamic instabilities in the accretion disk [e.g., is formed. In this| process, a linearly-polarized GW signal is emitted with typical GW strains 10 and emitted energies in the most sensitive band of rotation-type instabilities [ 2.2 Low-luminosity GRBsLow-luminosity and GRBs (LL-GRBs; engine-driven also supernovae frequently referredof to as long X-ray flashes) GRBs form a with subclass low is likely toCCSN proceed, [ at least initially, in a very similar fashion as in a rapidly spinning 10 Mpc and GW frequenciesdisk of 100 instability Hz to in 200 Hz a for disk a around a 10 band. Depending on the initial black hole spin, turbulence powered by black-hole spindownthis may emit results strong in GWs. anthe In the innermost anti-chirp frequency stable behavior, domain, orbit, since whichestimates most moves suggest out of GW in the strains radius as emission the is black expected hole is to spun occur down. near Simple missed by observations than LGRBs (see section be detectable for Galactic events and is thusnetic not field) relevant may be here. spinning nearinduce breakup. ellipsoidal This can deformations induce various ofelliptically-polarized rotational GW instabilities the that emission protoneutron [ star, leading to strong, quasi-periodic, which could observe such an event out to approximately 20 Mpc to 40 Mpc [ to 10 50 Hz to 1000 Hz frequency band of highest sensitivity of the initial h after seconds of hyperaccretion ontohot, efficiently the neutrino newborn cooled black and hole. thus thin The [e.g., inner parts of the disk are cooled and form aof thick this accretion torus torus. into Gravitational onelike instability or may objects multiple lead overdense and to regions1 fragmentation then that may inspiral could into condense to the neutron-star- central black hole [ JCAP06(2013)008 ]. 50 erg, 10 ,for 147 , × 51 ]. The /Virgo. 133 10 to 50 10 96 143 , =2 , ∼ × , 65 ANTARES 3 50 and we shall jet LIGO 130 E ≈ ]. – 0 2.1 E 136 128 , , = jet ]. Moreover, all GRB- 113 135 ], the relativistic shock , E 50 152 112 , , ]. For a simple estimate of the 110 108 , 114 , 83 84 ], Γ = 3 and , 38 38 ]. Five of the seven GRBs that have been detector, one may resort to the HEN flux es- 142 –6– , =1Mpc. ]) that the transition between engine-driven CCSNe, 2 s) are rarer than LGRBs and expected to result 135 50 96 , d  , 90 100 ANTARES 90 , , T 10 Mpc at which the probability of HEN detection by the 5- 51 97 , 50% at , ∼ ∼ 50 52 10 ] for refined results). Assuming a jet with Γ = 300, that exhibit luminous radio emission [e.g., d 85 detector is 10%. Hence, only the closest and/or the most powerful SGRBs ] (but see [ 76 -ray flux, and the SGRB variability time scale [ γ ]. The isotropic equivalent energy of SGRBs is 2 to 3 orders of magnitude smaller The GW emission processes that may be active in LL-GRBs and engine-driven CC- Type Ic-bl CCSNe occur also without LL-GRB or LGRB, but are frequently identified The GW emission from NS-NS and BH-NS mergers is well studied [see Theory suggests (e.g., [ The efficiency of HEN emission in SGRBs depends on the efficiency of proton accelera- ANTARES 114 engine-driven CCSNe , the detection probability is 2.3 Mergers andShort-duration short GRBs gamma-ray bursts (SGRBs; power output ofduration the of engine the determines centraland engine’s the make operation energy a determines normal of if LGRB.energetic the the If CCSN jet jet it can explosion fails and leavebreakout to is the its through emerge, progenitor likely the Lorentz the star stellar LGRB to factor. is surface result. “choked” could The and then a As beSNe more responsible suggested isotropic are for by a most [ LL-GRB. likley very similar to the LGRB case discussed in section erg, one finds a distance CCSNe are highlycompact energetic hydrogen/helium and poor progenitor ofbecause star they the and have spectroscopic relativistically the Doppler-broadened postfix type spectral -bl Ic-bl features. stands subclass.as for “broad Ic line,” indicates a to their lowrate luminosity) of suggests canonical an LGRBs event [ rate that may be significantly higher than the unambigously associated with a CCSN are LL-GRBs [ from double neutron star68 (NS-NS) and/or neutron star - black hole (BH-NS) mergers [e.g., LL-GRBs with CCSNe, and canonicalby LGRBs a may central be engine continuous.simply that All launches depend are a on likely collimated to the bipolar be power jet-like driven output outflow and and duration their variety of may central engine operation [ not consider them furthercollapse here. outcomes involving relativistic HEN flows.most emission Since likely is LL-GRBs expected much andunderstanding more from engine-driven the CCSNe the frequent HEN are entire that emission range from canonical such of LGRBs, events stellar [ much effort has been devoted to line may be detectable. reviews]. Most of thethe emission binary comes sweeps through from the the 50 late Hz inspiral to and 1000 Hz merger band phase of during highest which sensitivity of than the energy of LGRBs. Their jets have most likely lower Lorentz factors of Γ timates of [ tion, the and wider opening angles.SGRBs are Due much to easier theirmuch to short smaller. miss duration observationally and than LGRBs low and isotropic their equivalent observable energy, volume is detection probability in the 5-line It is worthwhile todetector consider from the LL-GRBs and probability engine-drivento of CCSNe, be detection in involved. of which mildly HENsfactor The relativistic of in detection jets the the are probability jet. likely 5-line depends Using strongly the on reference parameters the of energy [ and the Lorentz JCAP06(2013)008 , ]. ]. 2 c 13  102 .The , M 1 ], some 6 − 70 ]orbya − in X-rays 106 200 kpc for 1 ]) and GW , ]. However, 139 ANTARES erg s and IceCube − 86 ≈ 15 to 10 ], based on the 47 101 , 2 , 56 50 erg s 4 c d  45 42 ]. Theoretical upper , M 10 7 62 37 ]. Cosmic strings form ]and[ ∼ − ]. ANTARES 87 2 125 , GeV and up to the Planck 91 30 Mpc for equal-mass NS-NS 11 ∼ . At the time of this analysis the 10 2 c ∼  M ]. A search of IceCube data for HENs detector show that, 1 − 23 ], depending on details of the underlying 35 GeV energy range. Up to a few events per ]: detectors such as IceCube and to 10 11 88 2 –7– c 10   ANTARES M 2 − 1 s which reach peak luminosities of . 0 ]. The detectability of the 2004 giant are of the Galactic SGR ∼ ]. 78 134 is of order 10 ] for the 5-line , 88 ]. ]. The kinks and cusps decay, which is expected to lead to ultra-high GW 111 , E 153 125 , 60 reactions [ -scale detector are predicted in [ , 50 Mpc for a BH-NS binary with a mass ratio of 4 : 1, and a dedicated merger 98 3 ∼ ], including ultra-high-energy neutrinos (UHENs; e.g., [ 59 pγ G. Giant flares are believed to be caused either by magnetic stresses fracturing the 82 15 10 keV) periodic X-ray emissions with periods ranging from 5 to 10 s. They exhibit , 10 − /Virgo network had maximum sensitive distances of 47 -rays. There are a number of known SGRs and anomalous X-ray pulsars [ While not designed specifically for UHENs, HEN detectors like Significant emission of GWs in SGR giant flares may come from the potential excitation ∼ γ B favoured model for these objectsof is a magnetar, a neutron star with an extreme magnetic field and of which have had rare hard spectrum giant flares with luminosities of up to 10 scale [ bursts [e.g., have some sensitivity to UHENs in the initially as smooth loops,and but cusps through [e.g., interactionsenergy and cosmic self-interactions ray may emission develop kinks with energies in excess of which can bestudies probed that by investigated the thegest LIGO/Virgo excitation much network weaker of for emission magnetar aobservatories that pulsational [ Galactic may modes not source in be [ more detectable detail even with sug- advanced-generation GW 2.5 Cosmic stringCosmic kinks strings and cusps aredicted topological by defects grand unified that theories may and form superstring in theory [e.g., the early Universe and are pre- year for a km LIGO repetitive outbursts lasting The total emitted large-scale rearrangement of the magnetosphericThe field due sudden to release magnetic reconnectionacceleration of [ of energy pair plasma and thatof may magnetic HENs have field in some baryon rearrangement loading, lead thus leading to toshould the the detect emission multiple creation HEN and events fromloading similar Galactic is SGR eruptions, sufficiently providedgiant high. the flare baryon of The SGRfrom 1806-20, AMANDA-II regular (non-giant) did detector, Galactic not SGR which detect flares HENs was also found [ operating no significant during coincident the events [ 1806-20 by HEN detectors was estimated in [ Estimates based on [ magnetar crust and leading to a large-scale rearrangement of the internal field [ binaries and 2.4 Bursting magnetars Soft-gamma repeaters (SGRs) and anomaloussoft X-ray (2 pulsars are X-ray pulsars with quiescent search on this data did not find any evidence for GW candidates [ of nonradial pulsational modes with kHz-frequencies in the magnetar [ baryon-rich flares, suggesting that similarGalaxy. flares could be detected from anywhere within the limits on the possible strength of the GW emission were placed by [ the energy reservoir associatednetar. with They a found change in an the upper magnetic limit potential for energy the of emitted the GW mag- energy of 10 JCAP06(2013)008 ], 71 ]. In 36 ]. ]. The tele- ]. Installing 17 28 32 detector (Astronomy with ], but no limits on UHENs 9 sr, with most of the Galactic plane π ANTARES GeV energy range [ –8– 9 on the sea bed, at a depth of 2475 m, 40 km off the sky coverage is 3.5 2 data for neutrinos that have passed through Earth (see GeV to 10 6 ANTARES ANTARES ]. ]. The burst shape is expected to be generic, so that matched-filtering GW ] and others, but have not yet constrained many emission scenarios from cosmic 101 134 ], hosted in pressure resistant glass spheres, called optical modules (OMs) [ ), the present data set does not contain any potential UHEN events. , 132 30 60 3.1 The three-dimensional grid of PMTs is used to measure the arrival time and position of The rate of GW bursts from a network of cosmic strings depends on the string tension The search for very energetic HENs performed with one year of IceCube-40 data did not the detector at greatthe depths PMTs serves in to a attenuate darkvolume environment. this of background At the high and detector energiesupgoing also significantly the muons, greater allows the large than to total muon the operate rangebeing instrumented makes observable volume. the and sensitive By the searching Galactic for Center being visible 70% of the sidereal day. its full configuration, it isPMTs, composed storeys, of regularly 12 distributed detectionthe along lines, 350 each sea m, comprising bed. the up first toline The 25 storey was first triplets being put of detection in located operation line2007, 100 m in was so above September installed 2006 that and andwith a three connected an more total in instrumentation lines line early of werethe (containing 2006; connected 5 an measurement in the lines ensemble January of second of weretelescope environmental oceanographic taking reached parameters), sensors its data dedicated were nominal to in connected configuration,2008. with 2007. by 12 the lines Five immersed end and additional of taking lines, 2007. data, in together Cherenkov May The photons induced bywater. the This passage information, of together relativistic43 with charged degrees), the particles is characteristic throughincident emission the used neutrino. angle sea to of The the determinemuons, accuracy light produced the of (about by the direction neutrinos, directionproduced of from information by the the allows overwhelming cosmic muon background to ray from and distinguish interactions downgoing upgoing hence in muons, the infer atmosphere that above of the the detector [ coast of Toulon, France.(PMTs) The [ detector is a three-dimensional array of photomultiplier tubes were reported.NuMoon A [ number ofstrings dedicated [e.g., UHEN experiments exist, including ANITA [ 3.1 The ANTARES neutrinoSince telescope the Earth actsmainly as uses the a detection shield ofinteractions against upgoing in muons all the as particles matter a except around signature of neutrinos, the muon-neutrino detector. a charged-current neutrino The telescope 3 GW and HEN detectors a Neutrino Telescopehigh-energy-neutrino and telescope Abyss and environmental isscope RESearch) operating covers is in an currently the area the Northern of hemisphere only about [ deep 0.1 km sea emission model. Since Earthwe is are opaque only to considering UHENs, downgoing events must be selected. Since section and other network parameters,tectors and [ individual bursts may be detectable with advanced de- reveal any neutrinos in the 10 analysis approaches may be employed.in A 15 first days search of for LIGO GW bursts data from from cosmic early string 2005 cusps did not reveal any candidate events [ JCAP06(2013)008 ). 1 40 Hz) < ], chains ], on 2007 48 22 interferometers in LIGO detectors, Virgo therefore ] able to detect the quadrupolar LIGO 18 ]. The main instrumental difference 21 –9– and Virgo interferometers are undergoing upgrades to ], was held from 2005 November 4 to 2007 October 1. 4 km interferometers, while above 500 Hz it is dominated 14 sensitivity. During 2007, above 300 Hz, the Virgo detector LIGO LIGO observatories: one located at Hanford, WA and the other at LIGO . 1 is the seismic isolation system based on super-attenuators [ LIGO instruments are designed to detect gravitational waves with frequencies science run, S5 [ 40 Hz to several kHz, with a maximum sensitivity near 150 Hz (see figure LIGO ∼ LIGO 200 Hz, laser shot noise corrected for the Fabry-Perot cavity response yields an LIGO ∼ is a network of interferometric gravitational wave detectors consisting of three inter- ]. The advanced instruments will commence operations around 2015. There are two The The time-of-flight separation between the Virgo and Hanford observatories is 27 ms, At the time of writing the 79 with respect to In fact, seismicfrequencies noise is dominates determined mainlyAbove at by lower thermal frequencies noise,effective and strain with the noise contributions that sensitivity fromand rises other at L1 linearly sources. intermediate detectors withfirst-year during frequency. averages, the The while average second theyears. sensitivities year H2 of of detector the the had H1 S5 about run the3.2.2 were same about average sensitivity Virgo 20% in betterThe Virgo both than detector, V1, the is inson Cascina interferometer near with Pisa, orthogonal Italy. Fabry It Perot is arms a 3 [ km long power-recycled Michel- where Virgo surpasses the had sensitivity similar to the by shot noise, see figure ferometers in the U.S.A..laser interferometers These with detectors orthogonalstrain are Fabry-Perot in all arms space [ kilometer-scale produced power-recycled bypoints the of Michelson each GW. arm Multiple extend reflectionsof the between effective the mirrors optical instrument. located length of at each the arm, end and enhance the sensitivity of passive attenuatorsattenuators capable is of a filtering significant reduction seismic of disturbances. the detector The noise benefit at from very low super- frequency ( 3.2 Network of3.2.1 interferometers LIGO LIGO Livingston, LA. The HanfordH1, site and houses a two interferometers: secondinterferometer, L1. one with with The 2 km 4 observatories kmto are arms, arms, a separated denoted denoted time-of-flight by H2. separation a of distance The of 10 ms. 3000 Livingston km, observatory corresponding ranging has from one 4 km and 25 ms betweenangular Virgo sensitivity and of Virgo Livingston. is complementary Due to to that of the the different orientation of its arms, the enhances the sky coveragedetectors of are the crucial network. to Moreover, reject simultaneous environmental observations and of instrumental multiple effects. Over one year ofsimultaneous science-quality operation data at were collected theirfor with design H1, all sensitivity, three with H2, duty and factors L1. of 75%, The 76%, Virgo and detector 65% started its first science run, VSR1 [ “advanced” configurations with distance10 sensitivity [ improved by approximately a factor of 3.3 Joint dataThe taking fifth periods JCAP06(2013)008 was stime μ , while the ANTARES in situ 5-line (5L), VSR1

and Virgo detectors during S5. ANTARES 3 pe or 10 pe depending on the /Virgo, the remaining equivalent ≥ 3 10 LIGO K activity and bioluminescence) and 40 LIGO ]. The first level is applied 31 LIGO Hanford 4km 20070318 LIGO Hanford 4km 20070514 LIGO Hanford 2km 4km 20070830 LIGO Livingston Virgo 3km 20070905 frequency (Hz) –10– 2 10

20 21 22 23 19

10 10 10 10 10

) noise amplitude (Hz amplitude noise =91days. 1/2 obs T data sample used in the analysis is composed of runs from 2007 selected trigger system is multi-level [ . Noise amplitude spectral densities of the four ANTARES ANTARES Figure 1 the burst fraction (flashessents the of most light probable emitted countingeach rate by PMT of marine over a the given organisms). whole OMfraction run computed of The from (typically time baseline the a during rate rate few whichbaseline. distributions the hours). repre- in OM The The counting data burst rates selected exceedand fraction for by corresponds this a more search to burst than are the fraction 20% requiredcriteria, the lower to the estimated than have active a 40%, time baseline with isrestricting rate 103.4 80% below the days of 120 out data kHz all of to OMs the the 244.8 being concomitant days active. of period the With with 5-line these period. quality Finally, when time of observation is 4.2 Trigger levels The remaining levels intervene after allon data are disk. sent to Trigger thelevel, shore decisions L0, station are is and based before a beingthe simple on written analog threshold calculations signal of of done about the atin PMT. 0.3 the three The photo-electron second same (pe) levels. level storey equivalent trigger,configuration). charge The within L1, applied is The 20 first ns to based L2 trigger on or triggerwindow two hits (roughly coincident requires with L0 the the hits large maximum presence muon charge of transit ( time at across least the five detector) L1 and hits that in each a pair of 2.2 and S5 data coversthe the subject period of between the January analysis 27 presented and here. September 30, 2007; these data are operating in its 5 line configuration. The concomitant set of 4.1 HEN dataThe sample 4 Selection of HEN candidates according to various quality criteria, basedrent, mainly counting on rates), environmental configuration parameters (e.g.duration and sea of behaviour cur- the of run, the alignmentthe detector of counting the during detector). rate the of Two given basic run a quantities (e.g. given are used OM: to the characterise baseline rate ( May 18. The Virgo duty factor over VSR1 was 78%. During this period, JCAP06(2013)008 i i ) ). t q γ i d ( -like 4.4 (4.1) 2 D .The χ 0 t value, but 2 ]whichwas χ 2n.Here +20ns. =50misthe is the average 34 0 q d n/c and the expected i ij t is the speed of light d c ≤ , j ij t . and are then combined to recon-  i ) γ i 4.2 0 d ( d D ) i q ¯ q ( Q + ) of one track point at a given time 2 i 2 i : t 0 γ i σ Δ ,z d –11– 0  ,y hit =1 0 i  N x 1 of photons from the track or bright-point (see section NDF -minimisation approach. Its strict hit selection leads to a 2 from the muon track. In the second term, ¯ γ i t χ is the time residuals between the hit time = γ i i t 2 t ) accounts for the angular acceptance of the OMs, while χ i q − ( γ i t Q is the timing error, set to 10 ns for charges larger than 2.5 pe and to = i degrees of freedom, based on the time differences between the hit times i σ t is the index of refraction. ) and the position ( n θ, φ NDF are the time difference and distance between hits ij d and ij t arrival time of the photons primarily designed to be used on-line. 4.3.1 Description ofThe the algorithm algorithm is based on a reconstruction algorithm used for this analysis is a fast and robust method [ variable with typical distance at which theof signal 1 in pe. one PMT The from function a Cherenkov light front is of the order penalises large amplitude hitsquality originating from parameter large allows distance thethe tracks. isolation subsequent A of analysis. proper a cut high on the purity fit neutrino4.3.2 sample, which is Azimuthal crucial degeneracyFor in a of particle the trajectory reconstructed reconstruction fromdetector a lines, Cherenkov there cone giving always hits exists on an only alternative two trajectory straight having an identical a different direction.the The plane degenerate formed trajectory by the is two the lines. mirror As image a of consequence, each the event original reconstructed track with only in two high purity up-down separationdetector while is keeping ignored: a good theare detector efficiency. considered lines The as are exactto a treated geometry the single as of optical straight the OM and modulesmerged centered the into altitude. on one 3 hit. the OMs Allits of line. hits The charge each time at is storey of Thus, the theselection. the the same sum merged It hit’s floor hit of requests in altitude is the ain that coincidence coincidence corresponds charges. two of of within next-to-adjacent the 2 The 20 floors. ns earliest L1 algorithm hit are hits uses The in in the the quality two L1 adjacent group of floors hits and the within as reconstruction 80 a ns is or seed measured 160 for ns by the a hit 20 ns otherwise. Δ struct tracks usingMuons their are arrival assumed timewhich to and the cross charge induced the Cherenkov asin light detector measured the originates. at by PMTs The the the isits time speed used corresponding direction and of in charge ( OM. information light a of minimisation along the procedure a hits to straight obtain line the from track parameters, namely, 4.3 Reconstruction strategy Hits selected according to the criteria described in section hit charge calculated from all hits which have been selected for the fit and In this expression, The quality function is then extended with a term that accounts for measured hit charges and the expected arrival time and the calculated photon travel distances L1 hits are causally related according to the following condition: Δ in vacuum and Δ JCAP06(2013)008 is 0 (4.2) m , is associated 2 b is close to zero, χ depending on the 0 θ 2 t χ , is the quality factor 2 t χ , 2  0 0 θ 0 ]). σ − ) m Ω 77 0 θ  ln of selected events (black points), compared to −  δ 2 0 and [ 1 σ (Ω 2 − 4.6 e –12– π 2 1 √ is related to the shape of the distribution and ). The first parameter used, 0 σ 4.1 (Ω) = P reduces the number of such events and decreases the contribution of mis- 2 b χ shows the distribution of the sine of the declination of the events selected with 2 is a location parameter, . Distribution of the sine of the declination 0 θ Acuton Figure the final cuts, which is globally consistent4.5 with background. Angular error The distribution of thereconstructed muon space track angle can Ω be described between by the a true log-normal neutrino distribution: arrival direction and the a scaling parameter. In all cases for our study, the location parameter associated with the reconstructed particle track, whereas the second one, with a bright-point, lightevents emitted from from large a electromagneticinstance. point-like showers, source likely to inside appear the in detector. downgoing This muon rejects bundles for arrival direction of thewhich candidate reduce - the fraction the of muonwhile misreconstructed contamination optimising muons increases to the less close sensitivity than (see to 20% section the over the horizon whole - sample, reconstructed muons in the background. Further cuts are applied on Figure 2 lines will have two equiprobablethe arrival subsequent directions, GW which analysis. must be taken into4.4 account during Criteria forThe HEN initial sample event of selection reconstructed eventsdowngoing contains muons both from upgoing cosmic neutrino induced raymuons muons interactions are and in misreconstructed the as atmosphere.lations, upgoing are Some and devised of the to the selectionA reduce atmospheric cuts, minimum this based of contamination on 6 sotracks Monte-Carlo hits as simu- are on to kept maximise at forcomputed the least further according discovery 2 analysis. potential. to lines Quality equation are cuts ( required are to then reconstruct applied a based track. on Only two upgoing quantities Monte-Carlo expectations (sum ofpoints). atmospheric muons and atmospheric neutrinos, orange (or grey) where JCAP06(2013)008 2 − E around ◦ ) obtained with at high energy percentile of the for 3-line events, 4.2 ◦ . This number is 5 ◦ . th 3 and 10 ◦ spectrum, together with the 2 percentile error region for our − th E at 100 GeV, improving to 1 ◦ 5 . for 2-line events. 2 shows an example of distribution of the ◦ 3 ∼ percentiles of the distribution. th and 15 –13– ◦ at low energy (100 GeV) and 2 ◦ and 90 ; this window lies between 5 3 percentiles of the distribution. The distribution is normalised th th energy spectrum, 2 − E 0 is always satisfied. This distribution depends on the energy associated (median) and the 90 > th ) ], much smaller than the typical size of the 90 0 θ 148 . Example of space angle distribution with the associated fit to equation ( − We define the angular search window for the GW analysis as the 90 One of the main variables to describe the performance of a neutrino telescopeFor those events is of our the selected sample reconstructed with at least three lines the angular We note that the typical angular distance between galaxies within 10 Mpc is a few depending on declination, and between 10 100 TeV. For 2-line events, whenthe selecting the angular reconstructed accuracy track closer varies to the between true direction, 3 distribution, also indicated in figure best-fit parametrisation and the 50 (100 TeV). HEN events. This impliescandidates that if we it can turns associate out to a be potential of host4.6 cosmic galaxy origin. to any Analysis of sensitivity the andThe HEN selected limit-setting potential HEN of candidates 5 the line analysis, data orobtained period. sensitivity, over has been an Specifically, quantifieddepends ensemble the for on of sensitivity the the simulated is whole declination experiments defined of with as the no the potential true median source. signal. 90% For upper our The limit sample sensitivity and assuming an space angle for a sample of Monte Carlo neutrinos with an to the track (estimatedparametrisation through is the used number duringcal of the photons signal GW detected) for and search thereconstructed its to neutrino scanned declination. compute arrival directions the direction. This inside significance the Figure of angular a search hypotheti- window centred around the angular resolution, defined asneutrino the direction median and of theestimated the from reconstructed distribution simulations. track, of also the indicated angle in between the figure resolution true is, assuming an to unity. degrees [ a sample of Monte-Carlo HENindicate events, the for 50 a given declination and a given number of hits. The arrows and (Ω Figure 3 JCAP06(2013)008 ]. 13 . N). ; i.e., at ◦ -12 4.3.2 ◦ 2 lines 3 lines 47 (43 and IceCube − 1 ANTARES ANTARES https://dcc.ligo.org/cgi-bin/DocDB/ShowDocu ), in the following we consider only these 5.2 0 90 RA (h) –14– -90 Sky Map 80 -80 . This best sensitivity is reached below 1 − s 70 2 -70 − 60 -60 GeV cm 50 6 -50 . − is a sky map of the candidate HEN events, where the degenerate solutions 10 40 4 -40 ≈ 30 -30 dE dN 20 . Skymap of the selected 216 HEN events in equatorial coordinates. A line connects the 2 -20 10 0 -10 E

Of these HEN events, 158 occurred at times when at least two gravitational-wave de- With the selection previously described, 181 runs corresponding to 104 days of live time Finally, we note that IceCube operated in its 22-string configuration for part of 2007 [ DEC (deg) DEC Details of each of the HEN candidate events are given at 1 declinations which are always below the horizon at the latitude of tectors were operating. Sincefrom two background or noise more detectors (as are described required in to section discriminate GW signals for 2 line events can be seen. were kept for the2 analysis. lines and The eventsbe selection with searched has at for been leastneutrinos possible 3 divided to counterparts be lines. into in analysed: events3 the Each 198 reconstructed lines. with of subsequent with two the Figure GW possible mirror directions analysis. and solutions 18 This for reconstructed results with 2 at in line least events 216 will remaining 158 HEN candidates: 144 2-line events and 14 3-line events. ment?docid=p1200006 Figure 4 associated mirror solutions for events reconstructed with two lines as described in section steady flux, usingto the be selection criteria described, the best sensitivity has been estimated However, this data waswith only observed X-ray used or for gamma-raydependent emission, time-dependent such searches searches as over applied GRBs; the theresensitivities to were in sky. source no 2007 untriggered, directions indicates Furthermore, time- thattions a the (the comparison bulk southern of of sky) ourindependently. such HEN that neutrino it triggers is come unlikely from that declina- IceCube could have detected the source JCAP06(2013)008 X- on-source ]. All detectors operating at the time 20 –15– ], which is conservative enough to encompass most 41 496 s [ ± performs a coherent analysis of data from arbitrary networks ]. A threshold is placed on the map to retain the largest 1% 94 ], which has been used in similar searches for GWs associated with which is the expected polarisation for a GW source observed from 2 137 polarised GWs, as the resulting background reduction outweighs the impact of rejecting X-Pipeline ]. 20 algorithm [ linearly , 6 In addition to the marginalised circular polarization sum, a second ranking statistic The basic search procedure follows that used in [ Empirically it is found that the circular polarisation restriction also improves the overall detection prob- 2 is computed based ontributed a background maximum-likelihood noise analysisstatistic with of is the no often event assumption found assumingthe to on power-law GW provide dis- the detector signal-noise noise. GW separationimportance due polarization. Other are to combinations the “null” of In non-Gaussian combinations the nature practice designed data of this are to also cancel constructed. out Of the particular GW signal from the given near the rotationalof axis pixels [ by energyneighbours (squared clustering; amplitude). eachevent cluster Surviving cluster of pixels is pixels assigned arepixels; a is grouped combined this considered using energy combined next-nearest- as by energy summing is a the used candidate energy as GW values the of ranking event. its statistic constituent for The the events. ability for some linearly polarised GWs. Pipeline 5 GWsearchmethod 5.1 Search procedure One of thetriggered simplest analysis searches that that scanscross-correlating may GW data be data from performed aroundand pairs combining the direction of GW time of detectors. and the of This neutrino the HEN search event putative data exploits to neutrino is knowledge improve event a the of by GW the search time sensitivity. We use the of the trigger anddata which from pass each data-quality detectorbeing requirements are analysed are so first used that whiteneddata for a and stream. GW the time-delayed The signal GW according data frommaps search. to that are are the direction then The summed sky would Fouriereach transformed coherently appear location detector’s to simultaneous (using frequency-dependent produce in sensitivity amplitude each and time-frequencythe and response maps. weightings to phase) The the are with skypolarized chosen location weighting GW in to determined question; signal, by maximise the signal-to-noise ratio expected for a circularly GRBs [ theoretical models of GWGWs and and HEN HENs emission. duecoincidence The to windows maximum used. a expected non-zero time mass delay effect between for either particle is much smaller than the of gravitational wave detectors,Each trigger while is being analysed independentlybased robust of against on the others, background background withtrigger, noise the noise thereby fluctuations. analysis maximising characteristics parameters the optimised and search detector sensitivity. performance5.2 at the GW time eventIn analysis of our that GW search,and a angular neutrino search candidate window (and eventis mirror-image is the window, characterised range for of by the possible its 2-line timeand events). arrival delays the (both time, Also associated positive important direction, and gravitational-wave negative) emission.window between the for This neutrino quantity the emission is neutrino; referredsymmetric it to on-source is window as the of the time interval which is searched for GW signals. We use a JCAP06(2013)008 .We 5hours . 1 6.3.1 ± 496 s on-source ± ]. These tests are applied 145 ], and are described in detail 53 (based on circularly polarized GW energy ) background trials for each HEN. window, defined as all data within 3 5.2 (10 –16– O off-source 01 is subjected to additional checks to try to determine the . 0 p< ]. All surviving on-source events are assigned a false alarm probability by used; i.e., this is a blind analysis). These tests also determine which of the 49 not ]. Events are also characterised by their duration, central time, bandwidth, and central Once the thresholds have been fixed, these consistency tests are applied to the on-source Finally, the analysis is repeated after “injecting” (adding) simulated GW signals to the The time-frequency analysis is repeated for Fourier transform lengths of 1/128, 1/64, This time-frequency analysis is performed for all of the data in the 145 of the neutrino time,quality excluding requirements the as on-source in thesource interval. data on-source The provide analysis same a are set samplethe used of of for neutrino background detectors the that event, and off-source does butwith data- data. not with the contain These statistical neutrino. any off- signal features To associatedafter enlarge similar with applying the to background time the sample, shiftssuch data we time of searched also slides multiples in repeat we of the association were 6 off-source able analysis s to to produce the data from one or more detectors; with to the on-source, off-sourcediscarded. and injection The events; thresholds events are failingthose optimised one by which or testing more give a of preset1% the these range when best tests of thresholds are applied overall andevents detection to selecting are efficiency a at randomtwo a sample ranking fixed of statistics false backgroundor discussed alarm and powerlaw in probability injection noise) of section gives eventsranking the statistic. (the better on-source detection efficiency; the winnerevents is and to selected the as remainingsurviving the off-source on-source final and event with injection the eventsis largest (those taken significance not to (highest used energy for beloudest or tuning). event the powerlaw [ The statistic) best candidate for a gravitational wave signal and is referred to as the comparison to the distributionevent with of probability loudest events from the off-source trials. Any on-source use these simulations to optimise and assess the sensitivity of5.3 the search, as discussed GW below. search optimisation The sensitivity of searchesof for gravitational-wave non-Gaussian bursts fluctuations tendsbackground, to of be events the limited that background by overlapdisturbances the noise, in are presence discarded. time known In within asthe addition known coherent glitches. to instrumental and this incoherent and/or “veto” To energies step, environmental reduce are GW applied consistency this to tests each comparing event [ on-source data. The amplitudes and morphologies tested are discussed in section in [ frequency. 1/32, 1/16, 1/8, 1/4 s,also to repeated maximise over the a sensitivityThis grid to grid of GW is sky signals designed positions ofdetectors such different covering that is the durations. the 90% less It maximum containmentor is that relative region sky timing 0.5 of ms. positions error the between overlap HEN. discarded. any When in Finally, pair the time-frequency, GW of events the events GW are highest-ranked decimated from event to different a is rate Fourier kept of transforms and 0.25 Hz lengths the before others being written to disk. sky location; comparison to correspondingfor “incoherent” identifying combinations provides events powerful due tests to background noise fluctuations [ window. To estimate therepeated for significance all coincident of data the in the resulting GW candidates, the same analysis is JCAP06(2013)008 10%) of the ∼ . We also set a 004, which is not . 6.2 500 Hz), where our =0  p f , the most likely detectable 2 . At the same time, the computational cost 1 values is tested for consistency with the null p –17– . 6.3 01 to become a candidate event. We found no candidates in . =0 p analysis increases at high frequencies. This is due in part to the extra data values have been determined for the loudest events associated with each p X-Pipeline After the significant given a trialsfrom factor analysis of of 158 the (this H1,of statement H2, detector is and performance V1 quantified at data; below).and the follow-up scans time This checks of as were event data performed, indicated came fromlous including by detector behaviour. checks monitoring and programs environmental While monitoring and these equipmentreveal operator to checks that logs, look did it for not occurred anoma- uncovergravitational during a wave burst a physical signal glitching cause associated period for with the in any event, V1. of they We our did conclude sample that of we 158 have neutrino no events. clear the high frequency search.18064 background For trials the yielded low-frequency a candidate, refined additional false time alarm shifts probability totaling of signals at extra-galacticdetectors distances have are maximum in sensitivity, see the figure low-frequency band ( 6 Coincident search results 6.1 Per-HEN GWWe candidates analysed GW datasearch, in and 14 coincidence neutrino withsis, events 158 only for neutrino one thebelow candidates neutrino high the for trigger frequency threshold the had search. of a low frequency In corresponding the GW low event frequency with analy- false alarm probability hypothesis (no GW signal) using the binomial test, discussed in section 5.4 Low-frequency andGiven high-frequency our knowledge GW of analyses possible GW sources discussed in section of the 158 HEN events, the collectivefrequentist set upper of limit ontrigger, the as strength discussed of in gravitational section waves associated with each neutrino of the to be analysed, butmuch also smaller than to one theregions: GW need period. 60 for Hz We finer-resolution to therefore skyHEN 500 split events Hz grids — the and to such gravitational a 500 keep Hz wave searchregion band time is to of computationally into delay 2000 feasible Hz. two the errors while GW coveringcores The the low-frequency detectors. have highest-sensitivity band characteristic is However, frequenciesbe analysed compact for detectable for objects GW all from emission suchfrom Galactic above as nearby 500 sources neutron Hz. galaxies. such stars Suchevents Since as or emissions is the collapsar soft might computational prohibitive gamma cost withanalysis repeater of the on giant a the current high-frequency flares, 3-line analysis search HEN or pipeline, for events possibly we only. all perform HEN The 3-line the events 500 Hz are a to small 2000 Hz subset ( origin of the event andaccuracy additional of background the time false slide alarm trials probability are estimate. performed to improve the total trigger list andcomputational have cost the for smallest processing. sky Tosky position reduce grid the uncertainties, for computational and cost the therefore further, high-frequencythe the we search loss use smallest as the of same was sensitivity usedof is at acceptable. the low The low-frequency frequencies, high-frequency analysis afteridentical analysis determining (independent automated is that tuning, procedure. performed background independently low- In estimation, frequency the and etc.) following high-frequency using searches sections separately. the we will present the results of the JCAP06(2013)008 ]. tail 20 (6.1) p , values =1for 16 p tail N values we wish to test. p 0 10 : . ] we compute the binomial i k p values. − tail p ≤ N ) values measured in the low- and for each HEN loudest event are ,N i −2 p p 10 [1 p values are consistent with the null − ∈ p values i (1 p k i measured loudest event probabilities in −4 p 10 ! k N )! ! k probability p N −6 − –18– 10 .Foreach = 8 for the low frequency band and N N ( p ] is taken as the most significant deviation from the tail i is the number of the smallest = ≤ N N tail −8 k  tail 10 values for the loudest GW event associated with each neutrino ,N ... N p )= 5−sigma excursion measured null hypothesis [1 values which may be due to gravitational wave signals. i or more events with ; i.e., ≤ p i ∈ p ( 3 N i −10 i p 1 0 2 ≥ 10

10 10 10 P ≤ number of HENs of number 2 )for p i show the cumulative distribution of p ≤ ( i 6 1 ≥ ) of getting p i P to be 5% of p ( and i 5 ≥ tail values to the null distribution to determine if there is a statistically significant P N p . Distribution of observed is the number of HEN events analysed (158 in the 60 Hz to 500 Hz band and 14 in 013. Deviations this large or larger occur in approximately 64% of experiments under the null ) smaller than that computed from the true measured . i N The lowest Figures Briefly, the binomial test sorts the set of 0 p ( i ∼ ≥ 3 high-frequency analyses. Inhypothesis. both cases the measured the high frequency band. null hypothesis. To assess the significance of the deviation, we repeat the test using drawn from a uniformP distribution and count the fraction of such trials which give a lowest probability 6.2 Search for a cumulativeA excess: quantitative analysis binomial of test take the account significance of ofthe the binomial any trials test, candidate factor which gravitational-wave due has event been to must applied the in number previous of GRB-triggered GW neutrino searches events [ analysed. We use Figure 5 We choose hypothesis. The black line shows the threshold for a 5-sigma deviation from the null hypothesis. analysed in the low frequency analysis. The red dot indicates the largest deviation of the low Under the null hypothesis, the false alarm probabilities Here the 500 Hz to 2000 Hz band), and from the uniform distribution nullp hypothesis; this occurs due to having the three loudest events below expected to bemeasured uniformly distributed between 0 and 1. The binomial test compares the excess of (one or more) small ascending order: JCAP06(2013)008 . 1 p tail with (6.3) (6.2) (6.4) p ι such that for 90% D , ) 0 0

t 10 is the duration parameter. − t τ . ( 0 ) , and use central frequencies of 0 0 t πf dt . −2 /f  − and astrophysically motivated GW 10 ) t t ( = 1, this is constrained to occur for ( cos 2 =1 0 2 × 2 ) τ h πf tail 2 0 t τ N 4 − ad hoc t −4 ( )+ t sin 2 10 − ( e 2 2 + ) probability p 1 4 2 0 h t –19– τ )  4 − 2 is the root-sum-square signal amplitude: t ( rss  h πτ − rss −6 e is the central time, and  h (2 10 1 4 ) ) 0 ι ≡ values for the loudest GW event associated with each neutrino 2 t 2 rss p 5−sigma excursion measured null hypothesis h rss πτ h 2 (2 −8 ι

10 1 0

10 10 (1 + cos number of HENs of number the probability of detection is 0.9 or greater. waveforms are Gaussian-modulated sinusoids: = =cos + × 90% to the rotational axis. We select the inclination uniformly in cos h h D ι ad hoc ≤ D . We consider a simulated signal detected if it produces an event louder than the ]. This corresponds to a nearly on-axis system, such as would be expected for 5.2 ◦ . Distribution of observed is the central frequency, 5 , 0 ◦ f [0 ∈ Deviations this large orThe larger black occur dot in shows approximately the 66% threshold of for experiments a under 5-sigma the deviation null hypothesis. from the null hypothesis. any distance Here 100 Hz, 150 Hz, andhigh-frequency search. 300 Hz The for quantity the low-frequency analysis and 554 Hz and 1000 Hz for the waveforms. The 6.3.1 Injected waveforms As in GRB-triggered searches, we use a mix of association with an observed long GRB. We chose loudest on-source event afterlevel all lower event limit tests on have the been distance applied. to We the define source a as 90% the confidence maximum distance 6.3 GW upperThe limits sensitivity of the GWtrigger, search we is add determined simulated by GW ain signals Monte-Carlo section to analysis. the For on-source each data neutrino and repeat the analysis described Figure 6 ι This waveform is consistentinclination with angle the GW emission from a rotating system viewed from an from the uniform distribution null hypothesis; since analysed in the high frequency analysis. The red dot indicates the largest deviation of the low JCAP06(2013)008 ]. ]. ); = 2 90% 43 (6.5) 138 D , GW E 131 , 119 , typical distance  . This corresponds the limits scale as 118 2 , c M  64 GW (typical of core-collapse 35) M . E 2 and Virgo detectors. 2 1 c −  − ], and discussion in section M https://dcc.ligo.org/cgi-bin/DocDB/ 8 =10 − LIGO 124 . , GW 2 E 93 =10 . For binary neutron star systems of D , 2 8 0 f 67 GW , 2 rss E and h 66 ) this amplitude is related to the total energy 3 7 , and the one for a black-hole - neutron-star ◦ c This is defined as the maximum distance 2 5 G  π 3 –20– M 2 5 ι< 35 . We set the component spins to zero in each case. .   there is a probability of at least 0.9 that such a GW sig- M =1 GW ]. 35 E 2 . 90% ◦ m D 30 . , =1 . For example, for = ≤ ◦ 2 . 2 / 1 [0 1 D ) m m 2 ∈ considered here ( , c ι ι   ) for the HEN trigger, to account for the uncertainty in the true HEN M M 4.2 2 ANTARES with and black hole - neutron star systems of (5 − =5 ι 10  1 / M m we find typical distance limits between 5 Mpc and 17 Mpc in the low-frequency GW 35) E 2 . ( c 1  /Virgo and ∝ in a narrow-band gravitational-wave burst by − For each HEN trigger, the injections are distributed uniformly in time over the on-source For astrophysical injections we use the gravitational-wave emission of inspiraling neutron For each type of gravitational wave simulated, the distributions of exclusion distances M 2 Upper limits for each waveform and HEN trigger are available at 35 3 − . 90% GW limits are 5 Mpc and 10 Mpc respectively. For the sine-Gaussian waveforms with to the optimistic limit oflapsing possible cores gravitational-wave of emission rapidly by various rotating processes massive in stars the ([ col- 10 nal would have produced anFor event louder inspirals, than the each loudest distanceamplitude on-source event corresponds to actually each measured. to distance aergy for in well-defined the gravitational sine-Gaussian amplitude. waves. waveforms For as concreteness, We well, we can by select associate assuming a an fixed en- D supernovae) a signal would only be observable from a Galactic source. window. The injectionbility sky distribution positions ( are selected randomly following the estimated proba- E Motivated by estimates ofuniformly the in cos jet opening angle for short GRBs, we select the inclination system with band and of order 1 Mpc in the high-frequency band. For other Observational constraints on joint sourcesHowever, of they GW are and HEN basedand signals on have independent the been GW interpretation derived and in andare [ HEN the the combination observational first results. of derivedLIGO previously from The published a results joint presented GW-HEN in analysis, this using section concomitant data obtained with 7 Astrophysical implications ShowDocument?docid=p1200006 direction of incidence. The polarizationdistributed angle uniformly. (orientation Finally, of the therandomly rotational amplitude axis to and on simulate arrival the the time sky) effect is at of each calibration detector6.3.2 errors is in perturbed the Exclusion distances For each waveform type wesource associated set with a a 90% given confidence HEN level trigger. lower limit on the distance to a GW such that for any distance For the small values of more conservative estimates based on simulations have been made in [ for our neutrino sample are shown in figures star and black holeSpecifically, binaries, we which use are the post-Newtonian widely modelwith thought for to component the be inspiral masses of the a progenitors double of neutron star short system GRBs. (1 JCAP06(2013)008 2 c (7.1) M 2 − =10 GW E . b obs F 3 . 2 VT ≤ –21– 90 days is the duration of coincident observations. ≈ GW-HEN ρ obs T ,where obs /T 3 . of joint GW-HEN sources: . Low-frequency analysis: the top plot is the histogram for the sample of analysed neutrinos . High-frequency analysis: the histogram for the sample of analysed neutrinos of the distance GW-HEN 7.1 Upper limits onThe GW-HEN present populations search for GWcoincident and events. HEN This correlations implies incoincidences space a of and 90% time 2 confidence revealed level no upper evidence limit for on the rate of detectable Figure 8 exclusions at the 90% confidence level554 Hz for the and 2 1000 frequencies Hz. of circular sine-Gaussian models considered: is assumed. The bottomconsidered: plot shows NS-NS the and distance BH-NS. exclusions for the 2 families of binary inspiral models Figure 7 of the distance exclusionsered: at the 100 Hz, 90% 150 confidence Hz level and for 300 Hz. the A 3 standard types siren of gravitational sine-Gaussian wave models emission consid- of This can be expressedρ as a limit on the rate density (number per unit time per unit volume) JCAP06(2013)008 1 8 ],  − − 75 [ with yr 10 . 3 1 2 ], after − c − ∼  73 yr HEN tele- LGRB GW-HEN M 3 Mpc ρ 2 7 − − − NS-NS ρ 10 10 / Mpc ANTARES ∼ 5 − GW 10. E 10 ∼ ANTARES SGRB at low frequencies gives b ≡ × ρ is estimated in [ F 2 2 01 c 1 . 0  − ∼ E gives M yr 2 ◦ 3 − − ] derived from independent GW- SNIbc 43 ρ ) approximate limits on the popula- = 1 yr, an improvement of a factor 10 ,where ]. This is similar to the abundance of =10 Mpc 1 8 7.1 74 − − obs ], and well below the reach of the present of joint GW-HEN emitting systems were T GW yr 3 10 300, while 30 3 E ∼ − × b 3 ], and [ F –22– Mpc ∼ ). With GW-HEN ], relatively close to the obtained limit 115 3 1 ρ − gives − 44 ], [ [ ◦ ]. The GW emission associated with long GRBs is 10 yr is the volume of universe probed by the present analysis 1 LGRB 72 3 76 ρ − × V − . For LGRB-like sources, related to the collapse of massive 2 yr [see for example 1 / 3 01 3 − . 1 − 0 − Mpc − yr under our optimistic assumptions of GW emission in this sce- E GW interferometers, opens the way to a novel multi-messenger 2 ), and 3 b HEN signals. yr 1 − 4 − 3 F Mpc − − 10 − 4 yr  ], while the typical GW horizon from the inspiral model is 5 Mpc − × 3 Mpc b LIGO 76 − 10 2 Mpc is suggested in [ F − 5 × 1 − =12Mpcusing[  10 − 2 Mpc LGRB GW-HEN 3 × yr ∼ 50 ρ − 3 b d to 10 − F 10 1 SNII  − × SGRB GW-HEN is the beaming factor (the ratio of the total number of sources to the number with ρ Mpc ρ 2 yr b / 6 3 3 01 F − We take as fiducial sources two classes of objects: the final merger phase of the coa- A total rate of long GRBs of . − − =4Mpcusing[ 0 For example, for a jet opening angle of 5 4 E b 50 SGRB GW-HEN a typical horizonHEN distance distances of in 10 Mpction each density. to case For yields 20 SGRB-like Mpcρ from sources, in equation related GW. to ( the Using merger the of lower two of compact objects, the we GW find and 7.2 Comparison of limitsAfter correcting with for beaming existing effects, estimates a local rate density of SGRBs of whereas correcting for beamingcore-collapse effects; supernovae. these sources The are local closely rate related of to SNIbc Type is II and Type Ibc search ( highly uncertain; our optimistic assumption of extracted for the firstthese time limits using are theHEN consistent analysis observations. with More of the stringent coincidentanalyses limits ones GW-HEN using will obtained data. other be data in available We by sets [ note performing provided by similar that the coincidence same instruments. stars, we find to 10 Mpc dependingincreases on to the binary masses. For long GRBs (LGRB) the HEN horizon on the detection distanceproducing is coincident required GW in order to begin constraining the fraction of mergers nario. Acollapse factor events 10 producing coincident only weaklya beamed is required GW-HEN improvement required signals, of which in 2 translates on order into the to detection begin distance. constraining the fraction of stellar 8 Conclusions This first joint GW-HEN search using 2007 data, obtained with the scope and the Virgo/ astronomy. Limits on the rate density binary neutron star mergers, their assumed progenitors, estimated to be Mpc to 10 Here jets oriented towards Earth 5 lines isd 50%. In the case of short GRBs (SGRBs), the HEN horizon is estimated to be for typical GW-HEN sources. lescence of two compactGRB-like), objects both (short followed GRB-like), byhorizon or the as the emission the collapse distance of for of a which a the relativistic probability massive hadronic to object detect jet. at (long least We 1 define HEN the in HEN F JCAP06(2013)008 ur and LIGO energies alter- eenne (FEDER on y Ciencia, the egion Provence-Alpes-Cote ], and the advanced 81 [ Laboratory, the Science and Tech- energie atomique et aux ´ LIGO HEN telescope in its 22 string configuration neutrino telescope: Centre National de la and begin to constrain the fraction of stellar al’´ KM3NeT –23– o of the Govern de les Illes Balears, the Founda- IceCube SNII/SNIbc science run S6 and second and third Virgo science ρ ANTARES ≤ egion Alsace (contrat CPER), R´ LIGO ], are likely to coincide as well. They will give other opportunities LGRB GW-HEN 79 ρ telescope has taken data with first 10 then 12 active lines since the end of De- epartement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium f¨ Document Number LIGO-P1200006. /Virgo S5-VSR1 periods and the Future observing runs involving IceCube, The authors also acknowledge the financial support of the funding agencies for the For instance, the sixth collapse events accompanied byEarth. the coincident The emission analysisLIGO of of relativistic these jets data beamed is towards underway, and a similar analysis using data from the runs VSR2,3 coveredANTARES the period fromcember 7 2007. July Theirfactor 2009 required enhanced to to sensitivities obtain 21 should October permit 2010. a combined analysis Meanwhile, to the gain the is being finalized. advanced Virgo projects [ to look for potential coincident GW-HEN emissions. Bildung und Forschung (BMBF),Italy; Germany; Stichting voor Istituto Fundamenteel Nazionale Onderzoekvoor di Wetenschappelijk der Onderzoek Fisica Materie (NWO), Nucleare (FOM), theRussian Nederlandse (INFN), Federation Netherlands; organisatie for Council young of scientistssia; and the leading President National scientific of Authority schools the supporting forInnovacion grants, (MICINN), Scientific Rus- Prometeo Research of (ANCS),They Generalitat also Romania; Valenciana acknowledge Ministerio the (GVA) and technical deoperation support Multi-Dark, and Ciencia of the Spain. e Ifremer, CC-IN2P3 AIM forLIGO and the Foselev computing Marine facilities. for This the publication sea has been assigned Recherche Scientifique (CNRS), Commissariat ` nology Facilities Council ofNiedersachsen/Germany the for United support Kingdom, of thetector, Max-Planck-Society, the and and the construction the Italian andde State Istituto operation Nazionale la of di of Recherche Fisica Scientifique theauthors Nucleare for GEO600 also and the gratefully de- the acknowledge construction French theAustralian Centre and support National Research operation of Council, of the research the thewealth by International of Virgo these Science detector. Australia, agencies and Linkages theNazionale The by program Council the di of of Fisica the ScientificConselleria Nucleare Common- and d’Economia of Industrial Hisenda Italy, Research i thetion of Innovaci´ Spanish for India, the Ministerio Fundamental Research Istituto Scientific de on Research, Educaci´ the Matter Polish supportedgramme Ministry of by of Foundation the Science for and Netherlandsthe Polish Scottish Higher Organisation Science, Universities Education, the for Physics the Royal Alliance,tion, FOCUS Society, The the the Pro- National Carnegie Aeronautics Scottish Trust, and Fundingthe the Space Council, Research Leverhulme Administra- Corporation, Trust, and the the David Alfred and P. Lucile Sloan Packardconstruction Foundation. Foundation, and operation of the natives (CEA), Agence Nationalfund de and la Marie Curie Recherche Program), (ANR), R´ d’Azur, Commission D´ Europ´ Acknowledgments The authors gratefully acknowledge thedation support for of the the United construction States and National operation Science Foun- of the JCAP06(2013)008 , ]. Phys. (2009) , ] 744 ]. ] SPIRE 706 Erratum [ ]. IN (2012) 122007 Astrophys. J. ][ Astron. SPIRE , , IN SPIRE ][ D85 IN Astrophys. J. ]. ][ , Search for Gravitational All-sky search for Predictions for the Rates Search for Search for Gravitational Erratum ibid. ]. [ arXiv:0907.2227 (2011) 092003 [ arXiv:1001.0165 (2011) 141101 [ Searching for soft relativistic SPIRE IN Phys. Rev. SPIRE 106 , arXiv:0808.2050 D83 ][ [ IN ][ ]. arXiv:1111.7314 (2008) L45 ]. [ (2010) 346 ]. (2010) 1453 arXiv:1204.4219 [ 683 710 SPIRE Phys. Rev. SPIRE SPIRE 715 IN , Search for Gravitational Wave Bursts from Search for gravitational waves associated with Beating the spin-down limit on gravitational IN Search for gravitational waves associated with IN ][ (2008) 211102 ][ ][ Phys. Rev. Lett. ]. , arXiv:1011.4079 Time-Dependent Searches for Point Sources of Limits on Neutrino Emission from Gamma-Ray An absence of neutrinos associated with cosmic-ray Constraints on the Extremely-high Energy Cosmic Search for muon neutrinos from Gamma-Ray Bursts 101 (2012) 351 ]. (2012) 082002 –24– arXiv:1003.2480 [ Search for Gravitational Wave Bursts from Six collaboration, J. Abadie et al., ]. collaboration, J. Abadie et al., collaboration, J. Abadie et al., collaboration, J. Abadie et al., collaboration, J. Abadie et al., SPIRE Astrophys. J. Astrophys. J. 484 , IN , Astrophys. J. D85 SPIRE collaboration, R. Abbasi et al., ][ , IN SPIRE ][ (2011) L35 [ Virgo Virgo Virgo Virgo Virgo IN ]. ]. Nature arXiv:1111.7030 ][ arXiv:1103.4250 , arXiv:1005.4655 [ 734 ROTSE Phys. Rev. Lett. (2010) 173001 Phys. Rev. , SPIRE SPIRE , 27 IN IN ][ ][ -ray bursts (2012) A60 [ arXiv:1205.2216 γ [ arXiv:0805.4758 Astrophys. J. (2011) 079902] [ (2010) 102001 539 , collaboration, R. Abbasi et al., collaboration, R. Abbasi et al., collaboration, R. Abbasi et al., collaboration, R. Abbasi et al., collaboration, collaboration, R. Abbasi et al., arXiv:1104.0075 [ ]. ]. collaboration, J. Abadie et al., D84 D82 (2012) 12 SPIRE SPIRE arXiv:1202.2788 arXiv:1101.1448 IN IN gravitational-wave bursts in the[ second joint LIGO-Virgo run [ Magnetars [ of Compact Binary CoalescencesClass. Observable Quant. by Grav. Ground-based Gravitational-wave Detectors IceCube IceCube L203-L204] [ IceCube jets in Core-collapse SupernovaeAstrophys. with the IceCube Optical Follow-up Program Soft Gamma Repeaters Waves from Low MassScience Compact Runs Binary 2 Coalescence in and LIGO’s 3 Sixth Science Run and Virgo’s IceCube with the IceCube neutrino telescope Virgo gravitational-wave inspiral signals associatedfifth with and short Virgo’s Gamma-Ray first Bursts science during run LIGO’s IceCube Rev. Waves from Compact Binary Coalescence in LIGO and Virgo Data from S5 and VSR1 Neutrinos with the 40-String(2012) and 1 22-String Configurations of IceCube [ Bursts with the 40 String IceCube Detector wave emission from the Crab pulsar 760 gamma-ray bursts during LIGO science run 6 and Virgo science runs 2 and 3 acceleration in IceCube ibid. Neutrino Flux with the IceCube 2008-2009 Data [5] LIGO scientific sollaboration, [8] [4] [3] LIGO scientific sollaboration, [7] LIGO scientific collaboration, [1] LIGO scientific sollaboration, [6] LIGO scientific collaboration, J. Abadie et al., [2] LIGO scientific sollaboration, [9] [16] LIGO scientific collaboration, B. Abbott et al., [13] [10] [12] [15] LIGO scientific collaboration, B. Abbott et al., [11] [14] LIGO scientific collaboration, B. Abbott et al., References JCAP06(2013)008 , ]. ]. ]. D with ] SPIRE ] μ SPIRE IN SPIRE ]. ν Astrophys. IN IN ][ , (2012) 204 ][ ][ Phys. Rev. 36 , SPIRE (2012) 53 IN ]. (2010) 179 Proceedings of the ][ . 760 (2012) 224 34 ,in Search for low energy arXiv:0711.3041 ]. [ SPIRE arXiv:0904.4718 [ IN B 714 arXiv:1011.3772 (2005) 132 [ ][ (2011). arXiv:0905.0005 SPIRE [ astro-ph/0610029 [ Astropart. Phys. IN (2008) 114045 , Astrophys. J. ][ , A 555 25 astro-ph/0403207 [ (2011) 16 Contributions to the 32nd International Search for Neutrino Emission from Search for Cosmic Neutrino Point Measurement of Atmospheric Neutrino Phys. Lett. Astropart. Phys. (2009) 076901 (2009) 062002 , , (2009) L68 (2007) 107 72 ]. LIGO: The Laser interferometer Stacked Search for Gravitational Waves from First LIGO search for gravitational wave ]. B 696 D80 Limits on the high-energy gamma and neutrino 701 ANTARES: the first undersea neutrino telescope astro-ph/0607233 Zenith distribution and flux of atmospheric Study of large hemispherical photomultiplier tubes The data acquisition system for the ANTARES Search for a diffuse flux of high-energy arXiv:1112.0478 [ , ınez et al., ınez et al., ınez et al., ınez et al., (2004) 399 A 570 SPIRE Virgo: a laser interferometer to detect gravitational SPIRE –25– IN arXiv:1104.1607 [ Search for gravitational-wave bursts associated with ]. IN ][ 421 ][ Class. Quant. Grav. Phys. Lett. Nucl. Instrum. Meth. Phys. Rev. an-Mart´ an-Mart´ an-Mart´ an-Mart´ , , , , SPIRE Astrophys. J. Rept. Prog. Phys. IN , [ , (2011) 11 (2006) 221101 ]. ]. ]. ]. ]. 97 SPIRE SPIRE SPIRE SPIRE SPIRE P03012 A 656 IN IN IN IN IN arXiv:0908.3824 Nucl. Instrum. Meth. 7 [ Status of Virgo , arXiv:0709.0766 ][ ][ ][ ][ ][ Astron. Astrophys. [ , collaboration, S. Adri´ collaboration, J. Aguilar et al., collaboration, J. Aguilar et al., collaboration, S. Adri´ collaboration, J. Aguilar et al., collaboration, J. Aguilar et al., collaboration, S. Adri´ collaboration, S. Adri´ collaboration, M. Ageron et al., JINST collaboration, A. Achterberg et al., Phys. Rev. Lett. collaboration, T. Accadia et al., ]. ]. , collaboration, B. Abbott et al., (2010) 1438 2012 , (2008) 062004 715 SPIRE SPIRE arXiv:1007.1777 IN IN arXiv:1207.3105 physics/0510031 arXiv:1111.3473 arXiv:1206.0645 gamma-ray bursts using dataJ. from LIGO Science Run 5 and Virgo Science Run 1 Virgo ANTARES the ANTARES neutrino telescope [ ANTARES VIRGO waves ANTARES ANTARES Cosmic Ray Conference (ICRC 2011) by the ANTARES collaboration 32th International Cosmic-Ray Conference 77 ANTARES ANTARES ANTARES [ ANTARES ANTARES Nucl. Instrum. Meth. gravitational-wave observatory [ the 2006 SGR 1900+14 Storm neutrino in correlation withdetectors the in 8 2001 events observed by the EXPLORER and NAUTILUS bursts from cosmic (super)strings [ IceCube fluxes from the SGRdetector 1806-20 giant flare of December 27th, 2004 with the AMANDA-II muons measured with the 5-line ANTARES detector for the antares neutrino[ telescope Gamma-Ray Flaring Blazars with the ANTARES Telescope [ 39 gamma-ray bursts using data from the second, third and fourth LIGO runs Neutrino Telescope Sources with Four Year Data of the ANTARES Telescope Oscillations with the ANTARES Neutrino Telescope [ [20] [24] [29] M. Aglietta, P. Antonioli, G. Bari, C. Castagnoli, W. Fulgione et al., [32] [21] [30] [25] [31] [33] [26] [27] [28] [18] LIGO scientific collaboration, B. Abbott et al., [19] LIGO scientific collaboration, B. Abbott et al., [17] LIGO scientific collaboration, B. Abbott et al., [22] F. Acernese et al., [23] JCAP06(2013)008 , , ] , , ]. (1989) The (2005) ]. SPIRE 23 (2011) D40 IN (2009) 653 ][ ]. Annals Phys. (2011) 652 107 , SPIRE ]. arXiv:0711.0107 IN [ 34 499 ][ SPIRE The Burst Alert Measurement of the IN Phys. Rev. ]. SPIRE , (2005) 143 ][ IN ][ Astropart. Phys. ]. 120 ]. , SPIRE gr-qc/0405044 [ IN Bounding the Time Delay Phys. Rev. Lett. Simulations of ]. ][ (2008) 114039 , ]. SPIRE SPIRE Search method for coincident events Astropart. Phys. IN 25 IN , Astron. Astrophys. ][ SPIRE ][ astro-ph/0007329 , [ SPIRE IN IN ][ astro-ph/0206454 AIP Conf. Ser., Vol. 727, Gamma-Ray (2004) S1775 Upper limits on gravitational-wave signals [ ][ Space Sci. Rev. , Extremely High Energy Neutrinos from Cosmic astro-ph/0502521 [ 21 ,in Sedimentation and fouling of optical surfaces at ]. Observational Constraints on Multi-messenger A fast algorithm for muon track reconstruction arXiv:1108.2509 [ –26– SPIRE Are low luminosity GRBs generated by relativistic jets? (2001) 037302 eV cosmic ray and particle physics with kilometer scale (2003) 253 hep-ph/0505017 IN ]. arXiv:1107.1346 [ 20 Class. Quant. Grav. ][ , 19 10 IceHEP high energy physics at the south pole D63 (2005) 061103 astro-ph/0702539 The Intrinsic and oscillated astrophysical neutrino flavor ratios arXiv:1101.4669 SPIRE ]. , E. Fenimore and M. Galassi eds. (2004), pg. 684. [ [ ]. ]. IN 95 Revealing the supernova-gamma-ray burst connection with TeV ][ (2011) 085006 Class. Quant. Grav. (2011) L55 [ SPIRE (2006) 1049 , SPIRE SPIRE IN IN IN (2011) 1 Phys. Rev. ][ D84 739 , (2007) 416 ][ ][ Cosmic Strings and Ultrahigh-Energy Cosmic Rays hep-ph/0510389 A21 The GLAST Burst Monitor [ 35 Astropart. Phys. , ]. 664 ]. collaboration, P. Amram et al., collaboration, J. Aguilar et al., Phys. Rev. Lett. , ]. Phys. Rev. arXiv:1108.3001 SPIRE [ , SPIRE IN [ IN (2006) 2660 [ SPIRE astro-ph/0507410 IN arXiv:0904.1066 arXiv:1105.4116 from LIGO and IceCube detectors ANTARES 321 Telescope (BAT) on the Swift MIDEX mission [ neutrinos neutrino telescopes Strings the antares site Astrophys. J. Lett. between High-energy Neutrinos andAstropart. Gravitational-wave Phys. Transients from Gamma-ray Bursts Core-collapse rate from the Supernova Legacy Survey [ 251101 Sources of Gravitational Waves and High-energy Neutrinos ANTARES Astrophys. J. Magnetically-Driven Supernova and Hypernova Explosions in the Context of Rapid Rotation Bursts: 30 Years of Discovery [ Mod. Phys. Lett. based on loudest events and its application to the ANTARES neutrino telescope [ 557 seismic attenuation performance of the VIRGO superattenuator 3968 [39] Y. Aso, Z. Marka, C. Finley, J. Dwyer, K. Kotake et al., [36] [50] O. Bromberg, E. Nakar and T. Piran, [41] B. Baret, I. Bartos, B. Bouhou, A. Corsi, I. Di Palma et al., [37] L. Anchordoqui and F. Halzen, [42] S. Barthelmy, L. Barbier, J. Cummings, E. Fenimore, N. Gehrels et al., [51] A. Burrows, L. Dessart, E. Livne, C.D. Ott and J. Murphy, [38] S. Ando and J.F. Beacom, [46] P.N. Bhat et al., [45] V. Berezinsky, E. Sabancilar and A. Vilenkin, [35] J. Alvarez-Muniz and F. Halzen, [40] H. Athar, C. Kim and J. Lee, [44] G. Bazin, N. Palanque-Delabrouille, J. Rich, V. Ruhlmann-Kleider, E. Aubourg et al., [43] I. Bartos, C. Finley, A. Corsi and S. Marka, [49] P.R. Brady, J.D. Creighton and A.G. Wiseman, [34] [48] S. Braccini, L. Barsotti, C. Bradaschia, G. Cella, A. Di Virgilio et al., [47] P. Bhattacharjee, JCAP06(2013)008 D , ] AIP ] , ] D82 ]. Ann. Rev. ]. , Phys. Rev. (2012) 8 , , SPIRE Living Rev. Rel. Phys. Rev. Lett. , IN 15 , SPIRE ]. Phys. Rev. ][ IN , [ Mon. Not. Roy. arXiv:0806.4953 [ (2007) L21 , arXiv:0907.2290 [ arXiv:1011.5004 SPIRE ]. IN 382 Coherent network analysis ][ Mon. Not. Roy. Astron. Soc. ]. , ]. SPIRE ]. Living Rev. Rel. IN ]. How common are long Gamma-Ray , (2009) 1171 ][ SPIRE (2008) 064056 The Gravitational Wave Burst Signal SPIRE , Wiley-VCH, Hoboken, NJ, U.S.A. IN astro-ph/0204358 [ (2012) 049901 arXiv:1210.3095 IN ][ SPIRE 702 , SPIRE ]. ][ IN 85 Outlook for detection of GW inspirals by IN Gamma-ray bursts, supernova kicks and D78 The Swift Gamma-Ray Burst Mission ][ ][ astro-ph/0106113 SPIRE [ ]. Gamma-Ray Bursts in the Swift Era IN ]. (2002) L63 Observational Constraints on the Ultra-high Energy gr-qc/0104026 ][ –27– Gravitational wave emission from core collapse of [ Gravitational-Wave Physics and Astronomy: An Phys. Rev. SPIRE Astrophys. J. 579 , , IN Erratum ibid. SPIRE arXiv:0909.1531 ][ [ IN ], [ (2002) 430 arXiv:1102.3421 [ ][ Mon. Not. Roy. Astron. Soc. Lett. arXiv:1002.3662 , Gravitational wave bursts from cusps and kinks on cosmic Gravitational wave bursts from cosmic strings Gravitational waves from gravitational collapse astro-ph/0405233 ]. ]. 565 [ Binary Neutron Star Mergers GRB beaming and gravitational-wave observations ]. GRB afterglow plateaus and Gravitational Waves: multi-messenger (2001) 064008 Maximum gravitational-wave energy emissible in magnetar flares Do soft gamma repeaters emit gravitational waves? Astron. Astrophys. J. (2009) 567 SPIRE SPIRE On the trigger mechanisms for SGR giant flares , astro-ph/0504493 aros, SPIRE IN IN 47 D64 IN [ gr-qc/0605002 ][ ][ esz´ [ (2010) 1926 [ (2011) 104014 (2004) 637 collaboration, N. Gehrels et al., gr-qc/0004075 (1998) 397. [ arXiv:1003.2961 Simulating a faint gamma-ray burst population [ Astrophys. J. , 407 727 . D83 336 collaboration, P. Gorham et al., ]. ]. ]. Phys. Rev. , 360 (2005) L77 [ (2006) 082005 (2000) 3761 (2011) 1 SPIRE SPIRE SPIRE IN IN IN arXiv:0708.2106 arXiv:1204.3858 [ [ (2010) 022004 Lett. GRB-triggered searches in the advanced detector era Astrophys. arXiv:1206.0703 Swift Science from Core Collapse of Rotating Stars [ signature of a millisecond magnetar? gravitational radiation 74 massive stars technique for discriminating gravitational-wave bursts from instrumental noise Phys. Rev. Astron. Soc. ANITA Cosmic Neutrino Flux from the Second Flight of the ANITA Experiment 85 Introduction to Theory, Experiment(2011). and Data Analysis Conf. Proc. 14 Astron. Astrophys. strings Bursts in the Local[ Universe? [ [63] A. Dietz, N. Fotopoulos, L. Singer and C. Cutler, [62] J.A. de Freitas Pacheco, [54] H.-Y. Chen and D.E. Holz, [69] [64] H. Dimmelmeier, C.D. Ott, A. Marek and H.-T. Janka, [55] A. Corsi and P. M´ [67] C.L. Fryer and K.C.B. New, [61] M.B. Davies, A. King, S. Rosswog and G. Wynn, [66] C.L. Fryer, D.E. Holz and S.A. Hughes, [53] S. Chatterji, A. Lazzarini, L. Stein, P.J. Sutton, A. Searle et al., [60] T. Damour and A. Vilenkin, [56] A. Corsi and B.J. Owen, [70] R. Gill and J.S. Heyl, [71] [57] D.M. Coward, [59] T. Damour and A. Vilenkin, [58] J.D.E. Creighton and W.G. Anderson, [52] R. Chapman, N.R. Tanvir, R.S. Priddey and A.J. Levan, [68] N. Gehrels, E. Ramirez-Ruiz and D.B. Fox, [65] J.A. Faber and F.A. Rasio, JCAP06(2013)008 , ] ] , ]. ]. ]. ]. ]. SPIRE , ]. SPIRE IN [ IN SPIRE SPIRE IN IN ][ SPIRE ]. ][ IN ][ SPIRE arXiv:1204.0857 [ ][ astro-ph/0503279 IN [ (2004) 429 [ ]. (2009) 012047 SPIRE 20 Neutrinos from IN (1976) 1387 ]. 171 ][ SPIRE IceCube non-detection of (2012) 29 (2009) 329 IN [ A9 Gamma-Ray Bursts Jet-induced explosions of core SPIRE (2005) 1013 752 498 IN ,in astro-ph/9904419 ]. ][ astro-ph/0511239 astro-ph/0009327 [ 633 arXiv:1112.1076 [ (2011) 1326. arXiv:1209.3027 J. Phys. TeV-PeV neutrinos from giant flares of (2010) 084006. collaboration, J.J. Hernandez-Rey, , , Astropart. Phys. (1987) 1007 47 SPIRE , Advanced LIGO: The next generation of 27 IN arXiv:0711.2580 [ [ aros, J. Phys. Conf. Ser. , Astrophys. J. esz´ Electromagnetic transients as triggers in searches (1999) L107 [ D36 (2006) 823 [ (2001) 639 , TeV photons and neutrinos from giant Ultrahigh-Energy Cosmic Rays from Neutrino Emission from Gamma-Ray Burst Astrophys. J. ee–Aix Marseille II, Marseilles, France (2010). –28– , 524 (2012) 231101 Astron. Astrophys. 453 327 , The Luminosity and angular distributions of long astro-ph/0311488 [ erran´ 108 Adv. Space Res. (2008) 063007 Phys. Rev. , edit´ , ]. Class. Quant. Grav. ]. ]. astro-ph/0503348 , On the Rates of Gamma-Ray Bursts and Type Ib/c Supernovae D77 KM3NeT Consortium , The GRB-supernova connection (2005) 412 High-energy neutrinos from reverse shocks in choked and successful The batse-swift luminosity and redshift distributions of Short Gamma-Ray Bursts and Gravitational Waves from (2007) L73. SPIRE edelaM´ SPIRE SPIRE IN 619 Astrophys. J. Lett. IN IN Astron. Astrophys. ][ , 657 , Phys. Rev. Lett. ][ ][ , Phys. Rev. Search for high energy neutrinos emitted by point-like sources with ANTARES , collaboration, Soft gamma repeaters Topology of Cosmic Domains and Strings Mon. Not. Roy. Astron. Soc. ]. ]. , Magnetic deformation of magnetars for the giant flares of the soft gamma-ray Astrophys. J. scientific collaboration, G.M. Harry et al., , SPIRE SPIRE arXiv:0904.4011 IN arXiv:0811.0684 astro-ph/0302524 IN [ C. Kouveliotou et al. eds., Cambridge University Press Cambridge, U.K. (2011), pg. 169. collapse supernovae repeaters GRBs soft-gamma repeaters flares magnetars and the case of SGR 1806-20 relativistic jets Fireballs, Revised Superconducting Cosmic Strings Astrophys. J. Lett. [ gravitational wave detectors GRBs: Constraints on the fireball properties LIGO ANTARES Neutrino Telescopes in the[ Mediterranean Sea Ph.D. thesis, Universit´ Dynamically Formed Merging Binaries [ short-duration grbs individual gamma-ray bursts in[ the BATSE catalog for gravitational waves from compact binary mergers [84] S. Horiuchi and S. Ando, [90] A. Khokhlov, P. Hoeflich, E. Oran, J. Wheeler and L. Wang, [86] K. Hurkey, [87] K. Ioka, [73] D. Guetta, T. Piran and E. Waxman, [78] F. Halzen, H. Landsman and T. Montaruli, [88] K. Ioka, S. Razzaque, S. Kobayashi and P. M´ [91] T. Kibble, [74] D. Guetta and L. Stella, [83] J. Hjorth and J.S. Bloom, [85] S. Hummer, P. Baerwald and W. Winter, [82] C.T. Hill, D.N. Schramm and T.P. Walker, [76] D. Guetta, D. Hooper, J. Alvarez-Muniz, F. Halzen and E. Reuveni, [75] D. Guetta and M.D. Valle, [80] H.-N. He, R.-Y. Liu, X.-Y. Wang, S. Nagataki, K. Murase et al., [79] [89] L.Z. Kelley, I. Mandel and E. Ramirez-Ruiz, [81] [77] G. Halladjian, [72] D. Guetta and T. Piran, JCAP06(2013)008 , , , ] Mon. ]. , ]. ]. ]. , (2001) 215 Phys. Rev. , SPIRE (2011) 251102 SPIRE SPIRE SPIRE IN IN IN ]. IN ][ B 500 ][ 106 ][ ][ (2007) 1111 ]. ]. ]. SPIRE Mon. Not. Roy. Astron. 662 Core-collapse supernovae astro-ph/0605208 IN , [ ]. ][ SPIRE SPIRE ]. IN Phys. Lett. SPIRE IN Unifying the Zoo of Jet-Driven , ][ The Fermi Gamma-Ray Burst IN ][ SPIRE ][ ]. IN ]. ]. arXiv:1103.0880 SPIRE Phys. Rev. Lett. ][ arXiv:1110.5107 arXiv:1206.1314 , IN astro-ph/0604437 [ (2006) 2259 [ Astrophys. J. ][ SPIRE , SPIRE SPIRE 69 Gravitational waves from the IN IN IN ][ Bursts of gravitational radiation from ][ ][ arXiv:1111.0970 [ (2011) 659 [ (2013) 318 [ (2012) 111 arXiv:1206.2924 astro-ph/9810274 [ (2011) 1317. [ 418 14 astro-ph/0511711 (2006) 051101 [ –29– 756 arXiv:0908.0450 47 [ (2012) 68 97 astro-ph/0103275 [ (2011) 434. Rept. Prog. Phys. 750 , Cosmic Strings as Emitters of Extremely High Energy Low Luminosity Gamma-Ray Bursts as a Unique Population: Collapsars: Gamma-ray bursts and explosions in ‘failed (1999) 262 Polarized gravitational waves from gamma-ray bursts Gravitational radiation from gamma-ray burst progenitors astro-ph/0212539 astro-ph/0610043 astro-ph/0210211 [ TeV neutrinos from successful and choked gamma-ray bursts ]. ]. [ [ 332 On the excitation of f-modes and torsional modes by magnetar ]. (2012) 085008 High Energy Neutrino Flash from Far-UV/X-ray Flares of (2006) 1594 (2009) 791 524 Astrophys. J. aros, aros, C. R. Physique On the Redshift Distribution of Gamma Ray Bursts in the Swift Era , , SPIRE SPIRE 367 702 esz´ esz´ D86 SPIRE IN IN Phys. Rev. Lett. The protomagnetar model for gamma-ray bursts IN (2001) 171102 ][ ][ , Astrophys. J. (2007) 394 (2003) L89 (2003) 861 ][ , 87 The multi-wavelength properties of Anomalous X-ray Pulsars and Soft Astron. Nachr. 661 585 589 Magnetar giant flares and afterglows as relativistic magnetized explosions Gamma-Ray Bursts Astrophys. J. , Mon. Not. Roy. Astron. Soc. Tellar forensics with the supernova-GRB connection — Ludwig Biermann Award Multiple physical elements to determine the gravitational-wave signatures of , Phys. Rev. , , (2011) 2031. Astrophys. J. ]. , aros and E. Waxman, aros, (2012) 027301. On the excitation of f modes and torsional modes by magnetar giant flares esz´ esz´ 413 SPIRE astro-ph/0605200 IN arXiv:1105.5035 astro-ph/0102454 Astrophys. J. Monitor [ Stellar Explosions giant flares Gamma-ray Repeaters Adv. Space Res. supernovae’ core-collapse supernovae Not. Roy. Astron. Soc. Phys. Rev. Lett. D85 Luminosity Function, Local Rate and Beaming Factor Neutrinos Astrophys. J. Soc. [ missed by optical surveys [ Papaloizou-Pringle instability in black hole-torus systems Astrophys. J. Gamma-Ray Bursts Lecture 2010 [ superconducting cosmic strings and the neutrino mass spectrum [97] T. Le and C.D. Dermer, [99] Z. Li, [96] D. Lazzati, B.J. Morsony, C.H. Blackwell and M.C. Begelman, [94] S. Kobayashi and P. M´ [98] Y. Levin and M. van Hoven, [95] K. Kotake, [93] S. Kobayashi and P. M´ [92] K. Kiuchi, M. Shibata, P.J. Montero and J.A. Font, [102] M. Lyutikov, [105] C. Meegan, G. Lichti, P. Bhat, E. Bissaldi, M.S. Briggs et al., [100] E. Liang, B. Zhang and Z. Dai, [109] B.D. Metzger et al., [106] S. Mereghetti, [107] P. M´ [104] S. Mattila, T. Dahlen, A. Efstathiou, E. Kankare, J. Melinder et al., [103] A. MacFadyen and S. Woosley, [108] P. M´ [112] K. Murase and S. Nagataki, [101] C. Lunardini and E. Sabancilar, [110] M. Modjaz, [111] H.J. Mosquera Cuesta and D. Morejon Gonzalez, JCAP06(2013)008 ] ]. ] ]. , ]. , , SPIRE SPIRE 650 IN IN ]. SPIRE ][ ][ Mon. Not. IN , The Influence (2013) 124 ][ (1984) 721. (2011) 161103 Class. Quant. SPIRE ]. , astro-ph/0607104 IN [ 767 [ 208 astro-ph/0701748 106 [ Astrophys. J. ]. , Dynamics and SPIRE Correlated Gravitational IN First results of the NuMoon (2005) 109903] (2004) 1143 ][ SPIRE ]. (2006) L5 arXiv:0807.2562 astro-ph/0509729 94 [ [ IN 76 ]. (2007) 166 ]. ][ Astrophys. J. astro-ph/0303505 651 [ , ]. SPIRE 442 hep-th/0412244 Phys. Rev. Lett. IN SPIRE [ , , SPIRE ]. IN High Energy Neutrinos and Cosmic-Rays IN SPIRE ][ (2009) 268 ][ IN (2005) 2351 Erratum ibid. ][ [ SPIRE arXiv:1001.1570 IN Astrophys. J. Rev. Mod. Phys. Identifying Elusive Electromagnetic Counterparts Neutrino tomography of gamma-ray bursts and TeV neutrinos from core collapse supernovae and High energy neutrinos from a slow jet model of Phys. Rept. A 602 (2003) 083001 , A20 ][ , Mon. Not. Roy. Astron. Soc. , (2009) S102 ]. , –30– astro-ph/0610696 Hyperaccreting black holes and gamma-ray bursts The Local Rate and the Progenitor Lifetimes of D68 The dynamical stability of differentially rotating discs Instabilities in self-gravitating gaseous discs SPIRE A 604 (2010) A51 [ IN arXiv:1204.0512 (2004) 181101 [ ][ astro-ph/9807028 ]. ]. [ arXiv:1010.5550 514 93 ]. ]. [ Black Hole Formation in Failing Core-Collapse Supernovae (2007) 1173 [ Mod. Phys. Lett. Phys. Rev. arXiv:0809.0695 [ , Fragmentation of Collapsar Disks and the Production of Gravitational , SPIRE SPIRE (1991) 353. SPIRE SPIRE IN IN 658 aros and E. Waxman, aros and E. Waxman, aros and E. Waxman, Nucl. Instrum. Meth. IN IN , ][ ][ (1999) 356 (2011) 70 ][ ][ esz´ esz´ esz´ 248 (2012) 024026 Introduction to cosmic F- and D-strings 518 730 Phys. Rev. Lett. Nucl. Instrum. Meth. astro-ph/0511254 Coincidences between Gravitational Wave Interferometers and High Energy D86 [ , , The Gravitational Wave Signature of Core-Collapse Supernovae Short-Hard Gamma-Ray Bursts The physics of gamma-ray bursts Astron. Astrophys. (2009) 063001 ]. ]. , Astrophys. J. , 26 SPIRE SPIRE astro-ph/0407064 arXiv:1012.1853 astro-ph/0405503 arXiv:1210.6362 IN IN massive stellar collapses Astrophys. J. hypernovae [ Roy. Astron. Soc. with constant specific angular momentum of Model Parameters onCollapse the Prediction of Gravitational wave Signals from Stellar Core Wave and Neutrino SignalsPhys. from Rev. General-Relativistic Rapidly Rotating Iron Core Collapse experiment [ Gravitational Wave Signature of Collapsar Formation (2006) 281 [ to Gravitational Wave Mergers:[ an end-to-end simulation core collapse supernovae Neutrino Telescopes [ from Low-Luminosity Gamma-Ray Bursts? Grav. Astrophys. J. [ Short-Hard Gamma-Ray Bursts: Synthesis and Predictions for LIGO Waves [128] S. Razzaque, P. M´ [131] S. Scheidegger, R. Kaeppeli, S. Whitehouse, T. Fischer and M. Liebendoerfer, [126] R. Popham, S. Woosley and C. Fryer, [125] J. Polchinski, [129] S. Razzaque, P. M´ [132] O. Scholten, S. Buitink, J. Bacelar, R. Braun, A. de Bruyn et al., [119] C. Ott, C. Reisswig, E. Schnetter, E. O’Connor, U. Sperhake et al., [121] J.C. Papaloizou and G.J. Savonije, [122] J.C.B. Papaloizou and J.E. Pringle, [123] T. Piran, [116] S. Nissanke, M. Kasliwal and A. Georgieva, [127] T. Pradier, [118] C.D. Ott, [120] C. Ott, E. Abdikamalov, E. O’Connor, C. Reisswig, R. Haas et al., [117] E. O’Connor and C.D. Ott, [114] E. Nakar, [115] E. Nakar, A. Gal-Yam and D.B. Fox, [130] S. Razzaque, P. M´ [124] A.L. Piro and E. Pfahl, [113] K. Murase, K. Ioka, S. Nagataki and T. Nakamura, JCAP06(2013)008 , ]. 392 Phys. Nature , SPIRE 743 , , D73 IN 275 (2011) ][ 28 , Gravitational ]. (2010) 053034 -ray burst γ ]. Phys. Rev. 12 Gravitational wave (2006) 1014 , Astrophys. J. ]. SPIRE , IN SPIRE 442 Relativistic ejecta from ][ X-Pipeline: An Analysis IN , S.W. Hawking and SPIRE arXiv:1201.5599 ][ [ (2007) 083009 IN ][ Mon. Not. Roy. Astron. Soc. Nature Class. Quant. Grav. , New J. Phys. , , , D76 High-energy Cosmic Rays and Mon. Not. Roy. Astron. Soc. , ]. (2012) 022003 astro-ph/0102317 [ SPIRE Performance of an externally triggered arXiv:1201.5462 Phys. Rev. [ , IN D86 ][ astro-ph/9701231 [ e Paris Sud, LAL 11-119 (2011). ]. Low-luminosity gamma-ray bursts as a distinct GRB 300 Years of Gravitation –31– Low-luminosity gamma-ray bursts as a distinct GRB ]. ]. ,in SPIRE aros and Z.-G. Dai, The Soft gamma repeaters as very strongly magnetized IN SPIRE (2001) 071101 SPIRE Phys. Rev. esz´ ][ IN High-energy neutrinos from cosmological gamma-ray burst (2012) 586413 Coalescence of Black Hole-Neutron Star Binaries IN , ]. [ 87 (1997) 2292 Gravitational Wave Signatures of ]. ]. ][ gr-qc/0308016 TeV neutrinos and GeV photons from shock breakout in [ 78 2012 SPIRE A relativistic type Ibc supernova without a detected SPIRE SPIRE (2011) 6. IN IN IN ]. ][ 14 (1993) 273 ][ ][ , Ph.D. thesis, Universit´ gr-qc/0603115 [ Gamma-ray bursts from stellar mass accretion disks around black holes 405 SPIRE Gravitational radiation Phys. Rev. Lett. Neutrinos from Cosmic Accelerators Including Magnetic Field and Flavor Effects IN (2004) 044007 , arXiv:1004.2896 [ Searching for gravitational waves associated with gamma-ray bursts in 2009-2010 Phys. Rev. Lett. , D69 (2010) 513. arXiv:0908.3665 arXiv:0705.0027 astro-ph/0604389 fireballs package for autonomous gravitational-wave[ burst searches 463 [ Astrophys. J. (2011) 30 radiation from gamma-ray burstsRev. as observational opportunities for LIGO and VIRGO W. Israel eds., Cambridge University Press Cambridge, U.K. (1987). supernovae 085016. population a firmer case from multiple criteria constraints Adv. High Energy Phys. Living Rev. Relat. population: a firmer case(2009) from 91. multiple criteria constraints Neutrinos from Semi-relativistic Hypernovae neutron stars - 1. Radiative mechanism for outbursts (1995) 255 [ LIGO-Virgo data Magnetohydrodynamically-Driven Core-Collapse Supernova Explosions X-ray flash XRF 060218[ and the rate of cosmic explosions (2006) 105001 bursts from cosmic (super)strings: Quantitative analysis and constraints gravitational-wave burst search [146] E. Waxman and J.N. Bahcall, [137] P.J. Sutton, G. Jones, S. Chatterji, P.M. Kalmus, I. Leonor et al., [150] S.E. Woosley, [141] M.H.M. van Putten, A. Levinson, H.K. Lee, T. Regimbau, M. Punturo et al., [147] E. Waxman and A. Loeb, [149] W. Winter, [148] D.J. White, E.J. Daw and V.S. Dhillon, [136] A.M. Soderberg et al., [143] X.-Y. Wang, S. Razzaque, P. M´ [142] F.J. Virgili, E.W. Liang and B. Zhang, [139] C. Thompson and R.C. Duncan, [144] M. Was, [138] T. Takiwaki and K. Kotake, [140] K.S. Thorne, [135] A.M. Soderberg, S. Kulkarni, E. Nakar, E. Berger, D.B. Fox et al., [133] M. Shibata and K. Taniguchi, [134] X. Siemens, J. Creighton, I. Maor, S. Ray Majumder, K. Cannon et al., [145] M. Was, P.J. Sutton, G. Jones and I. Leonor, JCAP06(2013)008 637 (2012) 190 756 ]. Astrophys. J. , SPIRE IN GRB 120422A: A ][ Astrophys. J. , arXiv:1107.1689 [ Are gravitational waves from giant magnetar flares ]. –32– SPIRE IN ][ (2012) 024030 ]. The Progenitor stars of gamma-ray bursts D85 SPIRE IN ][ Phys. Rev. astro-ph/0508175 [ , arXiv:1206.0298 [ observable? Low-luminosity Gamma-ray Burst Driven by Central Engine (2006) 914 [152] B.-B. Zhang, Y.-Z. Fan, R.-F. Shen, D. Xu, F.-W. Zhang et al., [153] B. Zink, P.D. Lasky and K.D. Kokkotas, [151] S. Woosley and A. Heger, JCAP06(2013)008 , , , , , , , 7 2 , , , 45 12 † , 13 , 67 , , , , , , , , 21 15 , , 96 8 , , 11 105 6 23 59 25 11 44 9 , 81 , , 9 13 , 14 89 , , 24 , , 56 , , , 45 ,H. 8 88 , , 12 , , , 82 , , , 2 , 74 60 53 , , 26 , 5 , , 85 20 54 94 , 11 42 ,J.Busto , ,S.Anvar , 53 80 66 ,J.Cao , 8 52 8 , 2 99 19 6 , 12 a 52 63 , 5 53 , T. Accadia , , ,C.C.Hsu , , , ,J.Schmid 6 , D. Barker 11 , R. Bassiri 44 6 31 ,D.Lo 52 44 ,J.Ruiz-Rivas , T. Chiarusi 22 19 42 66 ,C.Donzaud 30 , L. Moscoso ,F.Simeone , E. Visser oßl , A. Margiotta ,F.Cleva , 37 , S. Bose 17 6 ,S.Ast 8 ,C.Curtil ofer 19 ,J.D.Zornoza , S. Biagi , V. Flaminio 41 23 10 56 ,R.Biswas , 9 , R. Bondarescu 24 , D. Blair 2 , M. Hamal ,C.T.Y.Chung 42 37 , M. Bebronne 23 2 24 49 60 , M. Branchesi 79 ,G.Anton 8 ,B.E.Aylott , L. Cadonati , J. Petrovic 5 103 ,J.H¨ , J. Brunner 76 , B. Canuel , A. Chincarini 6 53 , C. Tamburini 8 , I. Belopolski , M. Cavagli` , ,H.J.Bulten 67 23 ,E.AmadorCeron , G. Riccobene 95 38 44 98 52 ,C.Affeldt 69 , 101 8 , I. Bartos ,G.Lim 57 5 , 42 , M. Brinkmann 59 20 ,P.Sapienza , N. Beveridge , G. Giacomelli 24 ,P.Vernin ,M.Abernathy , S. Ferry , A. Enzenh¨ , T. Chalermsongsak 82 6 ,V.Bertin ,J.Birch , V. Boschi 2 13 , V. Kulikovskiy ,O.Kavatsyuk , C. Bond 1 , Ph. Charvis 49 , R. Shanidze ,A.Creusot 43 6 2 13 89 6 , C. Distefano 10 42 53 2 , M. Marcelin , A. Rostovtsev evre 28 53 , , D. Zaborov , 6 ,M.C.Araya ,J.H.Clayton 17 , G. Hallewell ,C.Bell 13 ,K.Payet , B. Herold 52 , M. Morganti 13 52 ,J.C.B.Barayoga 42 , C. Reed , L. Blackburn 94 , Th. S. Bauer , T. Bulik ,Y.Chen 16 44 ,R.L.Byer 35 13 3 34 58 , S. Caudill 9 s , ,S.S.Y.Chua , K. Cannon 42 , M. Anghinolfi 53 64 80 , M. Taiuti ,C.Aulbert , 4 97 18 44 e 23 52 52 ala¸ 104 , M.C. Bouwhuis , M. Ferri , K. Geyer , ,V.B.Braginsky , A. Brillet , A. Allocca , R. Adhikari ,D.Lef` , S. Basa , U. Katz 9 , M. Vecchi 9 ,P.Coyle ,T.Seitz 15 ,Z.Charif 53 16 56 av˘ anchez-Losa 49 9 , 53 48 19 40 2 ,M.A.Barton , , 23 9 11 , E. Cesarini , M. Born 6 ,K.Arai 14 , H. Yepes 56 ,Y.Bao , J. Betzwieser ,C.Buy , , C. Bogan ,U.Emanuele 42 42 , T. D. Abbott ,K.Roensch 56 andez-Rey , G. Billingsley , C. Racca ,A.S.Bell 6 30 64 53 ,X.Chen , S. Mangano 52 45 , 65 , 8 8 42 ,J.A.Clark 20 ,A.S´ 7 8 , G. Guillard 76 8 96 ussler ,M.Andr´ , A. Deschamps , S. Caride 52 6 ,I.Kreykenbohm 67 ,P.Gay 3 ,G.E.P˘ –33– 9 2 20 60 8 ,D.A.Brown ,B.Baret ,P.Campsie a 2 ,T.Montaruli , B. Bouhou 42 79 6 1 ,J.K.Blackburn , P. Addesso , P. Aufmuth , R. Bork ,P.R.Brady , Th. Stolarczyk ,J.Bauchrowitz , A. Kappes , N. Christensen , D. Lattuada , S. Cecchini 42 8 ,P.Fermani ,T.Eberl 50 , B. Allen 59 ,F.Sch¨ 6 84 1 2 24 ,D.O.Bridges , H. Costantini 6 3 , C. Cepeda ,J.J.Hern´ , F. Louis 59 , M. Barsuglia 2 , K. Graf 42 , S. Ballmer 23 103 , A. Robert ,W.Chen 91 , E. Presani , R. Abbott 24 , V. Van Elewyck 17 23 65 , E. de Wolf , D. Buskulic 2 9 13 , M.G. Beker 2 63 ,A.Albert 36 42 ,T.P.Bodiya , S. Galat` 28 93 2 , A. Bertolini 70 ,I.A.Bilenko ee ,D.E.Clark ,A.Meli ere 53 , I. Dekeyser ,W.G.Anderson ,L.Carbone 20 , alez 59 67 59 8 , A. Kouchner 20 ,J-J.Aubert 42 52 63 6 , J. Carr , ,E.Black ,J.B.Camp , D. Palioselitis 8 , L. Core 39 ,J.Batch ,A.F.Brooks ,K.Fehn 16 , ,T.Adams ,P.Ajith , D.F.E. Samtleben 77 , G. Larosa 47 ,J.Chow 10 2 8 , M. Bou-Cabo , , O. Kalekin , G. Cella , Y. Hello 19 25 53 49 8 55 33 , , T. Briant , 13 , D. Drouhin 8 , D. Atkinson , R. Bonnand , 46 ,C.Vall´ 28 63 102 , C. Rivi` 24 52 53 , L. Barsotti 22 14 32 25 , J. Wilms , J.J.M. Steijger , , S. Loucatos , C. Bradaschia ,J-P.Schuller 6 , 23 ,T.Pradier 8 † 6 , M. Bejger 44 , ,F.Clara 12 52 , G. Ballardin 22 24 , J-L. Fuda , 35 ,O.Bock omez-Gonz´ , B. P. Abbott 61 6 24 8 arloganu 58 62 ,S.Martini 11 , I. Al Samarai ock 1 42 1 , E. Nezri , T. Bhadbade , C. Kopper 6 ,J.M.Berliner ,M.P.Decowski 75 30 , S. Escoffier ,C.Adams , ,A.Basti , F. Carbognani 74 ınez , C. Bogazzi ,S.B.Anderson , J. Burguet–Castell 2 , E. Calloni ,C.Cˆ ,H.S.Cho , M. Kadler 15 , E. Chassande-Mottin ,J.P.G´ , B. Barr , 48 ,P.Astone 29 44 92 , , G. Lambard , 13 58 92 , Q. Dorosti 84 , R. Coniglione 15 , R. Cavalieri 63 ,R.Richter , B. Vallage , V. Popa 39 , K. Agatsuma , 8 6 , ,F.Sch¨ , M. Britzger 19 ,J.Breyer 48 14 ,A.J.Heijboer 2 , , M. A. Bizouard , G.V. Russo 49 , 6 46 8 , 100 6 , L. Bonelli , G. Wijnker 8 ,G.Ciani 18 77 ,P.Baker ,M.Blom 74 32 19 14 77 90 , T. Astraatmadja 6 27 24 , H. Loehner 35 ,U.Fritsch 46 ınez-Mora , B. Behnke 13 83 13 ,M.Neff 1 , M. Spurio 80 , S. Braccini 61 6 59 , J. Abadie 33 6 6 67 , an-Mart´ 86 42 32 niga u˜ C. D. Capano M. Rujoiu F. Acernese M. Benacquista F. Bondu M. Bitossi P. Charlton D. Amariutei P. T. Beyersdorf S. Babak J. Z´ S. Chung A. Chiummo L. Bosi J. E. Brau B. Bland G. Cagnoli S. M. Aston A. Trovato Presti H. Motz M. Bastarrika R. Lahmann M. Agathos V. Brisson A. Spies D. Beck S. Wagner F. Barone A. Buonanno J. Schnabel F. Cavalier P. Kooijman J.A. Mart´ P. Piattelli C. Richardt J-P. Ernenwein A. Capone F. Folger M. de Jong M. Ardid G. De Bonis C. Bigongiari M. Circella V. Giordano D. Dornic van Haren The LIGO and the VirgoJ. collaboration Aasi The ANTARES collaboration S. Adri´ JCAP06(2013)008 , , , , , , , , , , , , , 53 65 49 24 , 15 63 42 , , , 42 106 , 49 , , 120 , 66 , , , 24 52 14 , , 109 130 50 , , , 44 , , 52 59 , , , , 97 44 , 128 , 106 , 102 , 98 , 44 76 8 , 53 , 42 42 arka , 87 82 81 53 42 , , , , 76 88 67 65 , 52 , 53 44 ,R.Day 86 25 , , , , , , , 67 ,T.Evans , 119 52 24 49 66 110 ,A.Gennai 129 103 49 , 65 ,S.M´ , G. Kang 44 ,A.Conte , F. Donovan , , S. Meshkov 63 , ,M.A.Frei , C. Gray , 98 , V. Malvezzi , M. Jacobson 45 15 99 53 56 ,J.R.Leong ,V.V.Frolov , , A. Giazotto 113 60 ,C.Lawrie 53 44 , 78 , 55 , M. Edwards 118 , T. Meier ,Y.M.Kim , M. Holtrop 45 65 49 53 52 , K. Haughian ,L.S.Finn 52 , 135 ,C.A.Costa 44 ,D.Keitel 53 , R. Gustafson 67 49 , , S. D’Antonio , D. Fazi , V. Herrera , F. Y. Khalili 58 25 52 ,D.C.Coyne 42 , 53 ,S.H.Huttner , H. Heitmann , W. Del Pozzo 42 52 , uck 80 , M. Lorenzini , N. Fotopoulos 56 42 53 49 , M. MacInnis , 24 93 , J. Hanson 49 84 ,V.Kringel 52 ,E.J.Daw ,M.Evans , L. Matone 44 ,P.E.Lindquist 46 ,A.DiLieto ,E.Genin 53 ,D.I.Jones 52 8 , 42 77 44 5 65 , L. Gammaitoni 126 , L. Cunningham 46 , F. Marion 98 , , A. Grant , W. Katzman ,M.L.Gorodetsky 52 , R. Kurdyumov ,K.Izumi , K. Grover ,H.L¨ ,A.Dietz ,I.W.Martin 84 44 86 42 , N. Kim 84 65 98 , K. Holt 44 42 ,M.Frede 53 59 74 89 , K. Kokeyama ,M.Edgar , , ,H.M.Lee , M. Colombini , R. A. Mercer ,P.Fritschel ,A.Corsi 42 24 , D. E. McClelland 134 56 52 53 88 , I. Maksimovic ,S.Husa ıaz 15 81 , alez 53 62 , N. Lastzka , , 59 134 , S. Kandhasamy , M. Favata , J. Logue 14 56 52 67 ,K.D.Giardina , M. Cowart ,M.Mehmet 14 ,R.W.P.Drever 52 , F. Fidecaro 60 ,K.Evans 119 , D. Kozak 56 119 ,L.A.Forte , J. Degallaix ,F.Kawazoe 80 97 , M. Davier , M. T. Hartman ,T.G.F.Li 63 115 ,G.Gemme 42 endez 69 , 49 55 ,M.C.Heintze , S. L. Danilishin 74 ,L.DiFiore ,M.D´ ,E.K.Gustafson 90 , C. Hanna 96 111 ,A.Ivanov , K. Kim ,R.Kumar ,F.Matichard 121 91 53 24 , J. Kline 114 , 59 112 , M. Granata 112 ,A.W.Heptonstall ,A.Khalaidovski , H. Grote 53 64 45 ,G.Gonz´ , A. Cumming , 58 104 , M. Lubinski 52 , F. Frasconi ,W.W.Johnson , M. Galimberti , F. Marchesoni 44 43 , F. Martelli 53 ,H.K.Lee 60 , A. Colla 122 52 , B. Lantz ,K.A.Hodge , ,N.Cornish 123 64 , B. Machenschalk ,T.Eberle 15 ,J.Li 24 , 63 , B. Hughey 125 122 25 94 52 75 , , E. Katsavounidis 44 65 102 , D. Lodhia , T. Etzel 59 118 , R. McCarthy ,E.Forsi 14 , E. Majorana ,B.F.Farr 80 , D. Friedrich , F. Ferrini 24 42 , V. Kalogera 53 65 ,D.F.Men´ 42 131 50 136 , 53 25 , , , I. Kowalska , S. Giampanis 42 , J. Hanks –34– 59 , M. Drago 52 , H. Daveloza ,D.M.Coward 52 , R. Gupta ,G.D.Meadors 24 42 , T. Isogai 49 , S. Kawamura ,P.Kumar , H. Kim 44 , 42 64 , C. Griffo 49 , E. D. Harstad , G. Gelencser 94 113 , J. Gair , G. Debreczeni , J. Lough 59 , A. Heidmann 53 ,I.S.Heng 98 , E. Jesse , A. Masserot , A. Di Virgilio , 103 † 133 , D. Hoak , S. Klimenko 64 49 , 67 ,E.Goetz ,P.B.Graff 88 125 44 , M. Damjanic 111 ,S.Dwyer 71 65 52 , J. Marque , S. Dhurandhar ,C.H.Lee , S. Frasca 44 65 , Z. Keresztes 42 108 ,A.M.Cruise 58 53 ,S.Foley ,M.Cordier , R. Engel , , 53 80 ar 42 , A. Langley 98 , 61 77 , V. Lhuillier 42 74 84 65 52 ,M.Mantovani ,E.J.Howell 59 52 ,R.Kasturi 106 111 45 , E. Macdonald , K. Mailand asp´ ,P.Kalmus ,S.Fairhurst 44 77 113 , G. Mendell , 44 ,R.Inta 42 , G. Mazzolo , I. Ferrante , C. N. Colacino , C. Kim 80 , C. Guido ,J.McIver oczi 107 ,T.T.Fricke 63 59 , , S. Hild 65 , M. Fyffe , S. Dorsher 58 , B. Daudert 91 ,W.Z.Korth 89 139 ,N.A.Lockerbie ,P.Couvares , 42 , K. Kawabe ,D.DeBra 130 90 , G. Hammond 53 60 42 63 , K. Mason , G. Kuehn 56 , 58 106 82 88 ,P.Leaci 47 ,J.A.Giaime , G. Losurdo ,I.W.Harry , E. Maros , J. Heefner , 56 101 , J. Gleason 42 72 , J. S. Kissel 52 ,S.Franco , K. Dahl , C. Graef , 49 85 49 ,L.Ju , R. DeRosa 46 67 83 ,M.E.G´ 44 ,M.A.Hendry 127 8 49 , P. Jaranowski 84 60 45 68 ,J.-C.Dumas , M. Landry 42 , J. Hough , R. Flaminio 47 63 , ,D.G.Keppel , G. Endr˝ 96 , N. Letendre 119 , A. M. Gretarsson ,T.R.Corbitt , V. Mandic 80 64 ,Z.Liu 103 46 ,R.Frey 42 42 olak 77 59 60 ,T.D.Creighton 96 124 60 , J. Macarthur ,B.K.Kim 56 , V. Dattilo , V. Fafone , C. Gill 53 ,P.J.Fulda , D. Feldbaum ,D.R.Ingram ,N.Mavalvala ,G.McIntyre ,M.Kasprzack , , S. Doravari , S. Koranda , M. Mageswaran ,S.Ghosh 53 66 ,J.Franc 132 ,Z.Du , M. Di Paolo Emilio 93 , , P.-F. Cohadon 55 53 ,G.M.Guidi 49 ,J.N.Marx 52 ,J.-P.Coulon 79 53 , D. Hammer 42 , 50 , , 137 138 ,A.LeRoux , K. Kaufman 82 ,A.Kr´ 42 53 52 ,A.C.Melissinos , R. De Rosa 123 , R. Gouaty , M. Hewitson 61 58 , 60 , J.-F. Hayau 52 , M. Lormand 92 52 107 104 , 42 53 61 ,Y.Liu ,D.L.Kinzel ,G.M.Harry , 85 53 53 52 , W. Kells 55 ,R.M.Cutler ,S.Hooper ,F.Garufi , , , A. Markosyan ,N.Leroy ,Y.J.Jang 78 105 ,D.Cook , R.J.G. Jonker ,P.Ehrens 42 42 ,P.K.Lam 52 , G. Hemming , V. Dergachev 106 , I. Mandel ,A.Freise 64 52 52 63 59 66 118 90 42 48 ,R.P.Fisher 44 98 101 65 77 50 82 63 121 arka ´ A. Gergely E. James I. Leonor N. Man P. J. King T. Huynh-Dinh R. A. Matzner D. Kelley R. M. Martin E. A. Khazanov A. Melatos M. Heurs V. Kondrashov A. Lazzarini R. J. S. Greenhalgh P. Hello J. B. Kanner J. Harms V. Litvine D. M. Macleod K. Hayama B. Krishnan R. Conte V. Loriette Z. M´ P. Kwee T. Hong S. C. McGuire A. P. Lundgren E. Cuoco R. Jones H. Kaufer J. M. Hallam K. L. Dooley M. Factourovich S. Grunewald T. Dent S. Gil-Casanova T. Dayanga J.-D. Fournier M.-K. Fujimoto A. Effler Z. Frei M. Coughlin H. Fehrmann J. C. Driggers J. D. E. Creighton I. Fiori K. Danzmann I. Di Palma J. Garcia L. S. Goßler E. Coccia JCAP06(2013)008 , , , , , , , , , , , , , 80 49 44 65 , 59 56 , , 80 58 42 , 56 80 76 , , 110 58 , , , , 42 , 42 , 101 , , 42 , , 59 , 65 49 48 56 53 , , 45 , 47 , , 76 67 , 116 , 42 46 , 113 52 , 65 98 , , 46 , 42 53 , 49 , , , , S. Vass 25 25 , , , , ıa ,K.Ryan , , , 84 50 52 , B. Sorazu 142 42 44 , 85 45 , ,L.Wen , 24 24 63 90 ,C.C.Wipf , 50 , C. Pankow 103 , , 53 49 50 101 , , L. Wade 53 92 119 ,K.A.Thorne ,R.S.Ottens , S. Roddy , , L. Williams 103 ,L.R.Price , S. Susmithan 98 , A. E. Villar ,F.J.Raab 52 , T. Nash 103 , 59 52 , , C. Tomlinson 42 103 98 140 106 89 90 58 , 113 63 ,M.Roberts , M. Pihlaja ,J.Slutsky ,R.G.Oldenberg , R. Mittleman , A. Wanner , R. Romano ,L.G.Prokhorov ,S.E.Strigin , B. Shapiro , J.-P. Zendri , E. Tournefier 101 136 ,C.Ramet 88 97 , T. Reed 51 42 58 e ,S.E.Whitcomb 96 74 44 53 44 103 141 74 ,F.Seifert , , ,P.Ruggi 115 ,B.Mours 125 59 , , G. Persichetti ,Y.Pan ,D.Simakov 52 42 120 , L. Nuttall ,J.Veitch ,L.Santamar´ , N. Morgado 53 ,G.Vajente 53 , 103 , 64 14 , R. Poggiani , D. Talukder , J. Yablon 114 59 , K. Somiya 74 42 59 , J. Miller 52 52 ,T.Welborn 52 , 116 44 ,M.Sung , A. Wade , T. Nguyen 59 65 116 47 53 65 ,P.Thomas , ,A.Rocchi ,A.Mullavey 76 , H. Yang 44 8 , A. A. van Veggel , W. Winkler , K. Riles 144 , A. Mytidis 46 8 , A. Vicer´ 61 74 92 , V. Pierro , X. Wang ,R.M.S.Schofield 53 49 44 ,S.H.Oh , J. Steinlechner , J. Zweizig , , P. A. Willems ,B.S.Sathyaprakash 89 udiger ,D.J.Ottaway 89 , 60 , T. Prestegard 53 , 59 , A. Pasqualetti , 52 65 59 84 ,D.Sigg , M. Zanolin 141 88 ,K.A.Strain 50 ,C.M.Reed 88 52 47 101 , M. Shaltev 56 , ,C.I.Torrie , J. D. Romano 72 , A. Perreca 74 ,S.M.Scott ,R.Quitzow-James ,K.V.Tokmakov , C. Palomba , G. Moreno 107 46 74 42 ,J.T.Whelan , M. Rakhmanov , R. Weiss ,G.A.Prodi , ,A.R¨ 103 , G. Mitselmakher , J. Worden , K. Mossavi 44 74 81 131 59 , V. Sannibale zny ,M.V.Plissi 53 42 , G. Vedovato 53 44 108 76 , 49 47 , ,B.J.J.Slagmolen , ,G.Newton 121 , L. Taffarello 106 , L. Milano , , 65 53 60 , , R. Riesen 52 52 ,H.Vahlbruch 56 87 63 46 84 , M. Wang 66 , 106 ,J.J.Oh 52 15 , M. E. Normandin , , S. Mukherjee 86 ,C.C.Yancey 96 145 ,E.Steinert ,V.Predoi 42 ,P.G.Murray , B. Sassolas 49 ,C.D.Ott 14 ,F.Vetrano ,R.Stone ,E.L.Robinson 5 ,S.P.Vyatchanin 58 ,J.Scott 117 ,M.E.Zucker 66 84 ,V.Re , C. Wilkinson ,S.Penn , M. Parisi ,X.Siemens 103 42 45 42 , 50 59 , R. Schnabel † , S. van der Putten , , A. Zadro˙ 59 ,A.P.M.terBraack ,N.D.Smith-Lefebvre , C. Titsler 53 42 56 60 8 –35– , L. Winkelmann ,T.Z.Summerscales 53 , , 119 ,S.Rowan , ,R.Prix 115 , D. Moraru , F. Piergiovanni ,C.V.Torres 45 42 60 52 , J. G. Rollins 142 , S. Sankar 53 ,R.Wooley 49 , 52 61 , K. Wette , 52 53 ,I.Neri 42 , S. Mosca ,P.Raffai 94 53 , , M. Tacca ,V.Quetschke 57 45 , A. Vecchio ,C.Michel , 59 53 ,Y.Wan , 44 52 53 44 74 59 , 52 14 , D. A. Shaddock , F. Ricci 52 77 24 42 121 ,A.J.Weinstein 101 , L. Palladino 52 ,M.Prato , D. Ugolini ,G.R.Skelton 42 ,H.J.Pletsch ,G.H.Ogin , D. Nolting 132 ,V.P.Mitrofanov 53 , G. Mueller 60 42 66 , uring over 93 , E. Saracco 44 65 63 , D. Murphy , C. Vorvick 60 58 52 , M. Stefszky ,A.Stochino , D. Verkindt , C. Robinson ,M.Yvert ,N.Zotov 86 , C. Osthelder , R. Taylor 143 , M. Pedraza , T. L Sidery 140 85 77 107 80 56 53 , G. Woan 146 , 24 ,V.Raymond 65 , , K. Wiesner 147 ,P.Schwinberg , J. Nelson ,M.A.Papa ,C.R¨ , R. Schilling , L. Rolland , O. Torre , S. Privitera ,A.L.Stuver , P. Puppo ,H.Miao 53 , K. Yamamoto ,A.Th¨ 52 15 58 , 50 , 58 57 73 106 ,M.Tse 59 ,R.J.E.Smith 59 , , H. Radkins 25 51 , V. Sandberg , , 89 , L. Wallace 86 , M. Wimmer 49 , A. Page , G. Szeifert , 42 , C. Poux , 52 14 49 61 113 42 ,S.R.Morriss 24 70 65 53 81 63 24 88 , A. Sergeev 48 111 , , T. Westphal 105 ,E.Oelker , M. Vavoulidis , C. Van Den Broeck , M. Pitkin , F. Nocera ,D.H.Reitze 55 , M. Pickenpack 63 52 64 65 , H. Vocca 54 51 64 , ,A.M.Sintes 44 ,C.Zhao 82 ,M.Weinert 124 acz 8 ,S.R.P.Mohapatra , J. Munch nska 8 42 ,C.L.Mueller 42 77 63 53 ,F.Robinet , , S. Yoshida , G. Santostasi , S. Steplewski 44 103 52 , D. Passuello , V. Necula , 42 ,I.R´ 44 , H. Wittel 53 25 , 42 15 , T. Mori , 54 ,M.Rodruck ,M.Principe ,M.Punturo , , E. Thrane , G. Traylor ,C.M.F.Mingarelli , 56 , L. Sperandio ,R.L.Savage ,M.S.Meyer , M. Tonelli , R. Paoletti ,A.Nitz , S. P. Tarabrin ,S.Reid ,R.Sturani 52 ,B.F.Whiting 8 , M. West , K. Venkateswara ,B.J.Owen 24 14 53 53 ,B.Swinkels ,D.Rosi´ 87 , B. Willke , L. Sammut ,B.F.Schutz , D. H. Shoemaker ,M.R.Smith 44 , , 64 107 , H. Yamamoto , R. Vaulin , 50 25 119 , R. O’Shaughnessy , S. Vitale 63 55 101 58 , P. Rapagnani 82 , J. O’Dell 74 , 106 , 53 , 49 ,M.Was , ,M.Pichot 50 49 42 110 53 53 92 52 52 43 140 ,I.M.Pinto 86 , F. Postiglione ,D.Sentenac 49 9 , , L. Singer 49 82 , 99 , L. Zhang 56 ,S.J.Waldman 24 24 111 52 106 42 84 53 49 52 52 42 , M. Mohan 96 56 , 56 52 uller-Ebhardt old B. O’Reilly F. Paoletti L. Pinard C. Rodriguez P. J. Sutton J. H. Romie M. Phelps A. S. Stroeer K. S. Thorne P. Wessels B. Schulz F. C. Speirits D. Sellers I. Santiago-Prieto D. J. White A. Morgia F. Zhang Y. Minenkov R. Passaquieti R. L. Ward A. G. Wiseman D. S. Rabeling A. Singer N. A. Robertson C. M. Mow–Lowry J.-Y. Vinet P. R. Saulson O. Puncken P. Shawhan P. J. Veitch J. P¨ D. B. Tanner L. Naticchioni H. Overmier T. Regimbau B. Moe B. Rankins F. Salemi J. F. J. van den Brand H. M¨ E. Ochsner J. R. Smith M. Vasuth F. Travasso I. Yakushin M. Prijatelj A. Nishizawa S. Steinlechner M. Wade D. Yeaton-Massey A. Toncelli R. Williams C. Messenger JCAP06(2013)008 o, 08800 ote d’Azur ateau-Gombert, rue ´ Etoile Site de Chˆ on de Paterna, CSIC - Universitat de urnberg, Sternwartstr. 7, 96049 a, Viale Andrea Doria 6, 95125 Catania, Italy ole de l’ –36– at Erlangen-N¨ urnberg, Erlangen Centre for Astroparticle Physics, a di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy a, Viale Berti Pichat 6/2, 40127 Bologna, Italy a La Sapienza, P.le Aldo Moro 2, 00185 Roma, Italy o Integrada de les Zones Costaneres (IGIC) - Universitat ere - Institut de recherche sur les lois fondamentales de l’Univers - ere - Institut de recherche sur les lois fondamentales de l’Univers - e, CNRS/IN2P3, Marseille, France e Blaise Pascal, CNRS/IN2P3, Laboratoire de Physique at Erlangen-N¨ etecteurs et d’Informatique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, ısica Corpuscular, Edificios Investigaci´ o per a la Gesti´ e de Nice Sophia-Antipolis, CNRS/INSU, IRD, Observatoire de la Cˆ e, Universit´ u, Barcelona, Spain encia. C/ Paranimf 1 , 46730 Gandia, Spain. e du Sud Toulon-Var, 83957, La Garde Cedex, France CNRS-INSU/IRD UM 110 e Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris e Pierre et Marie Curie, BP 48, 06235 Villefranche-sur-mer, France ecnica de Val` eric Joliot-Curie 38, 13388 Marseille Cedex 13, France encia, Apdo. de Correos 22085, 46071 Valencia, Spain e, 75205 Paris, France ed´ eoazur - Universit´ Fr´ Dipartimento di Fisica ed Astronomia dell’Universit` Universiteit Utrecht, Faculteit Betawetenschappen, PrincetonpleinNetherlands 5, 3584 CCUniversiteit Utrecht, The van Amsterdam, InstituutAmsterdam, voor The Hoge-Energie Netherlands Fysica, ScienceMoscow Park State 105, University, 1098 Skobeltsyn XG InstituteRussia of Nuclear Physics,INFN Leninskie - gory, 119991 Sezione Moscow, di Catania, Viale Andrea Doria 6, 95125 Catania, Italy Dipartimento di Fisica dell’Universit` University Mohammed I, LaboratoryMorocco of Physics of MatterRoyal and Netherlands Radiations, Institute B.P.717, for OujdaNetherlands Sea 6000, Research (NIOZ), LandsdiepDr. 4,1797 Remeis-Sternwarte SZ and ’t ECAP, Horntje Universit¨ (Texel), The Val` Univ Paris-Sud , 91405Kernfysisch Orsay Versneller Cedex, Instituut France (KVI),Groningen, University of The Groningen, Netherlands ZernikelaanDirection 25, des 9747 Sciences AA deService la de Mati` Physique desINFN Particules, - CEA Sezione Saclay, 91191 di Gif-sur-Yvette Pisa, Cedex, Largo France B. Pontecorvo 3, 56127 Pisa, Italy Bamberg, Germany G´ INFN - Sezione diINFN Bari, - Via Laboratori E. Nazionali OrabonaMIO, del 4, Mediterranean Sud 70126 Institute (LNS), Bari, of ViaFrance; Italy Oceanography, Universit´ S. Aix-Marseille Sofia University, 13288, 62, Marseille, 95123 Cedex Catania, 9, Italy Cit´ INFN - Sezione diDipartimento Bologna, di Viale Fisica C. dell’Universit` Berti-PichatIFIC 6/2, - 40127 Instituto Bologna, de Italy F´ INFN -Sezione di Roma,Dipartimento P.le di Aldo Fisica Moro dell’Universit` 2,Clermont 00185 Universit´ Roma, Italy Nikhef, Science Park, Amsterdam,APC, The Universit´ Netherlands LAM - Laboratoire d’Astrophysique de Marseille, Pˆ Technical University of Catalonia, LaboratoryVilanova i of la Applied Geltr´ Bioacoustics,INFN Rambla - Exposici´ Sezione diFriedrich-Alexander-Universit¨ Genova, Via Dodecaneso 33, 16146 Genova, Italy Direction des Sciences deService la d’Electronique Mati` des D´ Corpusculaire, BP 10448, 63000 Clermont-Ferrand, France and Universit´ Institut d’Investigaci´ CPPM, Aix-Marseille Universit´ GRPHE - Institut universitaireColmar, de France technologie de Colmar, 34 rue du Grillenbreit BP 50568 - 68008 France Erwin-Rommel-Str. 1, 91058 Erlangen, Germany Polit` 8 9 4 5 6 7 1 2 3 33 29 30 31 32 26 27 28 21 22 23 24 25 17 18 19 20 11 12 13 14 15 16 10 JCAP06(2013)008 edeSavoie, eve, 1211, Geneva, edeGen` ote d’Azur, F-06304 Nice, France e de Strasbourg et CNRS/IN2P3 23 rue agurele, Romania at zu Berlin –37– ur Gravitationsphysik, D-30167 Hannover, Germany ur Gravitationsphysik, D-14476 Golm, Germany ora, Poland a, Via Dodecaneso 33, 16146 Genova, Italy lystok, Poland eaire et Corpusculaire, Universit´ at Hannover, D-30167 Hannover, Germany e Paris-Sud, IN2P3/CNRS, F-91898 Orsay, France ´ Swierk-Otwock, Poland e Nice-Sophia-Antipolis, CNRS, Observatoire de la Cˆ a di Siena, I-53100 Siena, Italy a di Napoli ’Federicoa II’, di Complesso Salerno, Universitario I-84084 di Fisciano Monte (Salerno), S.Angelo, Italy I-80126 Napoli, Italy lystok University 15-424 Bia epartement de Physique Nucl´ Also at University ofOn Leiden, leave the of Netherlands absenceAlso at at the Accademia Humboldt-Universit¨ Navale di Livorno, Livorno, Italy Universit´ San Jose State University, SanMoscow State Jose, University, CA Moscow, 95192, 119992,LAL, U.S.A. Russia Universit´ ESPCI, CNRS, F-75005 Paris,NASA/Goddard France Space Flight Center,University Greenbelt, of MD Western 20771, Australia, U.S.A. Crawley,The WA Pennsylvania 6009, State Australia University, University Park, PA 16802, U.S.A. IM-PAN 00-956 Warsaw, Poland Astronomical Observatory Warsaw University 00-478CAMK-PAN Warsaw, 00-716 Poland Warsaw, Poland Bia NCBJ 05-400 Institute of Astronomy 65-265The Zielona University G´ of Texas at Brownsville, Brownsville, TX 78520, U.S.A. Montana State University, Bozeman, MTEuropean 59717, Gravitational U.S.A. Observatory (EGO),Syracuse I-56021 University, Cascina Syracuse, (PI), NY Italy 13244,LIGO U.S.A. - Massachusetts InstituteColumbia of University, Technology, New Cambridge, York, MA NY 02139,Stanford 10027, U.S.A. University, Stanford, U.S.A. CA 94305, U.S.A. National Astronomical Observatory ofUniversity Japan, of Tokyo Wisconsin–Milwaukee, 181-8588, Milwaukee, Japan WIUniversit` 53201, U.S.A. University of Florida, Gainesville,LIGO FL - 32611, Hanford U.S.A. Observatory, Richland,University of WA 99352, Birmingham, U.S.A. Birmingham,Albert-Einstein-Institut, B15 Max-Planck-Institut 2TT, f¨ United Kingdom Universit` LIGO - Livingston Observatory, Livingston,Cardiff LA University, Cardiff, 70754, CF24 U.S.A. 3AA,University of United Sannio Kingdom atAlbert-Einstein-Institut, Benevento, I-82100 Max-Planck-Institut f¨ Benevento, ItalyLeibniz and Universit¨ INFN (Sezione diVU Napoli), University Italy Amsterdam, De Boelelaan 1081, 1081 HV Amsterdam, the Netherlands LIGO - California InstituteCalifornia of State Technology, Pasadena, University CA Fullerton, FullertonSUPA, 91125, CA University U.S.A. of 92831 Glasgow, U.S.A. Glasgow,Laboratoire G12 d’Annecy-le-Vieux 8QQ, de United Physique Kingdom des Particules (LAPP), Universit´ INFN, Sezione di Napoli,Universit` Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy Switzerland du Loess, BP 28,ITEP 67037 - Strasbourg Institute Cedex for 2,Moscow, Theoretical Russia France and Experimental Physics,Dipartimento B. di Cheremushkinskaya Fisica 25, dell’Universit` 117218 CNRS/IN2P3, F-74941 Annecy-Le-Vieux, France D´ Institute for Space Sciences,IPHC-Institut R-77125 Pluridisciplinaire Bucharest, Hubert M˘ Curien - Universit´ 82 76 77 78 79 80 81 69 70 71 72 73 74 75 62 63 64 65 66 67 68 55 56 57 58 59 60 61 48 49 50 51 52 53 54 43 44 45 46 47 37 38 39 40 41 42 34 35 36 JCAP06(2013)008 ut 29-33, Hungary e dos Campos, SP, Brazil os ´ e Pierre et Marie Curie, 4 Place Jussieu, ao Jos´ e de Rennes 1, 35042 Rennes, France –38– er 9, Hungary om t´ es (LMA), IN2P3/CNRS, F-69622 Villeurbanne, Lyon, France eriaux Avanc´ and University, Budapest, 1117 Hungary a di Roma Tora Vergata, I-00133 dell’Aquila, Roma, I-67100 Italy L’Aquila, Italy a di Trento, I-38050 Povo, Trento, Italy a di Padova, I-35131 Padova, Italy a di Perugia, I-06123 Perugia, Italy a degli Studi di Urbino ’Carlo Bo’, I-61029 Urbino, Italy os Lor´ otv¨ Lund Observatory, Box 43, SE-221 00, Lund, Sweden Perimeter Institute for TheoreticalAmerican Physics, University, Ontario, Washington, N2L DC 2Y5, 20016,University Canada U.S.A. of New Hampshire,University Durham, of NH Southampton, 03824, Southampton, U.S.A. Korea SO17 Institute 1BJ, of United Science Kingdom Hobart and and Technology William Information, Smith DaejeonInstitute Colleges, 305-806, of Geneva, Korea Applied NY Physics, 14456, Nizhny U.S.A. Novgorod, 603950, Russia Northwestern University, Evanston, IL 60208,Rochester U.S.A. Institute of Technology, Rochester,E¨ NY 14623, U.S.A. University of Cambridge, Cambridge,University CB2 of 1TN, Szeged, United 6720 Kingdom Rutherford Szeged, Appleton D´ Laboratory, HSIC,Embry-Riddle Chilton, Aeronautical Didcot, University, Oxon Prescott, OX11 AZ 0QX 86301 United U.S.A. Kingdom University of Minnesota, Minneapolis,INFN, MN Gruppo 55455, Collegato U.S.A. diUniversit` Trento, I-38050 Povo, Trento, Italy INFN, Sezione di Padova,Universit` I-35131 Padova, Italy California Institute of Technology, Pasadena, CA 91125, U.S.A. INFN, Sezione di RomaUniversit` Tor Vergata, I-00133 Roma,Universit` Italy Instituto Nacional de PesquisasThe Espaciais, University 12227-010 of - Sheffield, S˜ Wigner Sheffield RCP, S10 RMKI, 2TN, H-1121 UnitedInter-University Budapest, Kingdom Centre Konkoly for Thege Astronomy Mikl´ and Astrophysics, Pune - 411007, India The University of Mississippi,Charles University, MS Sturt 38677, University, Wagga U.S.A. Wagga,Caltech-CaRT, NSW Pasadena, 2678, CA Australia 91125, U.S.A. Pusan National University, Busan 609-735,Australian Korea National University, Canberra, ACTCarleton 0200, College, Australia Northfield, MNThe 55057, University U.S.A. of Melbourne, Parkville, VIC 3010, Australia Universitat de les IllesUniversity Balears, of E-07122 Massachusetts Palma - deCanadian Amherst, Mallorca, Institute Amherst, Spain for MA Theoretical 01003,Canada Astrophysics, U.S.A. University of Toronto,Tsinghua Toronto, Ontario, University, Beijing M5S 100084 3H8, China University of Michigan, AnnLouisiana Arbor, State MI University, 48109, Baton U.S.A. Rouge, LA 70803, U.S.A. Universit` INFN, Sezione di Firenze,Universit` I-50019 Sesto Fiorentino, Italy University of Oregon, Eugene,Laboratoire OR Kastler 97403, Brossel, U.S.A. ENS,F-75005 CNRS, Paris, UPMC, France Universit´ University of Maryland, College Park, MD 20742 U.S.A. Institut de Physique deLaboratoire Rennes, des CNRS, Mat´ Universit´ Washington State University, Pullman, WAINFN, 99164, Sezione U.S.A. di Perugia, I-06123 Perugia, Italy 99 93 94 95 96 97 98 88 89 90 91 92 83 84 85 86 87 133 127 128 129 130 131 132 120 121 122 123 124 125 126 113 114 115 116 117 118 119 106 107 108 109 110 111 112 100 101 102 103 104 105 JCAP06(2013)008 –39– Trinity University, San Antonio, TXUniversity 78212, of U.S.A. Washington, Seattle, WA,Southeastern 98195-4290, Louisiana U.S.A. University, Hammond, LADeceased 70402, U.S.A. Southern University and A&MUniversity College, of Baton Rochester, Rouge, Rochester, LAUniversity NY 70813, of 14627, U.S.A. Adelaide, U.S.A. Adelaide,National SA Institute 5005, for Australia MathematicalLouisiana Sciences, Tech Daejeon University, Ruston, 305-390, LA Korea McNeese 71272, State U.S.A. University, Lake Charles,Andrews LA University, Berrien 70609 Springs, U.S.A. MI 49104 U.S.A. Hanyang University, Seoul 133-791, Korea Seoul National University, Seoul 151-742,University of Korea Strathclyde, Glasgow,The G1 University 1XQ, of United Texas Kingdom at Austin, Austin, TX 78712, U.S.A. † 146 147 139 140 141 142 143 144 145 134 135 136 137 138