# Search for high-energy neutrinos from binary neutron
Star Merger GW170817 with ANTARES, IceCube, and
the Pierre Auger Observatory

A. Albert, M. André, M. Anghinolfi, M. Ardid, J.-J. Aubert, J. Aublin, T.

Avgitas, B. Baret, J. Barrios-Martí, S. Basa, et al.

► To cite this version:

A. Albert, M. André, M. Anghinolfi, M. Ardid, J.-J. Aubert, et al. Search for high-energy neutrinos from binary neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory. Astrophysical Journal Letters, 2017, 850 (2), pp.L35. 10.3847/2041-8213/aa9aed. hal-01669864

HAL Id: hal-01669864

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# Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory

ANTARES Collaboration, IceCube Collaboration, The Pierre Auger Collaboration, and LIGO Scientific Collaboration and Virgo Collaboration
(See the end matter for the full list of authors.)

Received 2017 October 15; revised 2017 November 9; accepted 2017 November 10; published 2017 November 29

## Abstract

The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for high-energy neutrinos from the merger in the GeV–EeV energy range using the ANTARES, IceCube, and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within ±500 s around the merger time. Additionally, no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for high-energy neutrinos within the 14 day period following the merger, but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The non-detection is consistent with model predictions of short GRBs observed at a large off-axis angle.

**Key words:** gamma-ray burst: general – gravitational waves – neutrinos

## 1. Introduction

The observation of binary neutron star mergers with multiple cosmic messengers is a unique opportunity that enables the detailed study of the merger process and provides insight into astrophysical particle acceleration and high-energy emission (e.g., Faber & Rasio 2012; Bartos et al. 2013; Berger 2014; Abbott et al. 2017a). Binary neutron star mergers are prime sources of gravitational waves (GWs; e.g., Abadie et al. 2010), which provide information on the neutron star masses and spins (e.g., Veitch et al. 2015). Kilonova/macronova observations of the mergers provide further information on the mass ejected by the disruption of the neutron stars (e.g., B. Abbott et al. 2017, in preparation; Metzger 2017).

Particle acceleration and high-energy emission by compact objects are currently not well understood (e.g., Mészáros 2013; Kumar & Zhang 2015) and could be deciphered by combined information on the neutron star masses, ejecta mass, and gamma-ray burst (GRB) properties, as expected from multi-messenger observations. In particular, the observation of high-energy neutrinos would reveal the hadronic content and dissipation mechanism in relativistic outflows (Waxman & Bahcall 1997). A quasi-diffuse flux of high-energy neutrinos of cosmic origin has been identified by the IceCube observatory (Aartsen et al. 2013a, 2013b). The source population producing these neutrinos is currently not known.

On 2017 August 17, the Advanced LIGO (Aasi et al. 2015) and Advanced Virgo (Acernese et al. 2015) observatories recorded a GW signal, GW170817, from a binary neutron star inspiral (Abbott et al. 2017b). Soon afterward, Fermi-GBM and INTEGRAL

detected a short GRB, GRB 170817A, from a consistent location (Abbott et al. 2017a; Goldstein et al. 2017; Savchenko et al. 2017). Subsequently, ultraviolet, optical, and infrared emission was observed from the merger, consistent with kilonova/macronova emission. Optical observations allowed the precise localization of the merger in the galaxy NGC 4993, at equatorial coordinates $\alpha(J2000.0) = 13^h09^m48^s085$, $\delta(J2000.0) = -23^\circ22'53.0''343$ (Abbott et al. 2017c; Coulter et al. 2017a, 2017b), and at a distance of ~40 Mpc. At later times, X-ray and radio emissions were also observed (Abbott et al. 2017c), consistent with the expected afterglow of a short GRB at high viewing angles (e.g., Abbott et al. 2017a).

High-energy neutrino observatories continuously monitor the whole sky or a large fraction of it, making them well suited for studying emission from GW sources, even for unknown source locations or for emission prior to or after the GW detection (Adrián-Martínez et al. 2016a; Albert et al. 2017a). It is also possible to rapidly analyze the recorded data and inform other observatories in the case of a coincident detection, significantly reducing the source localization uncertainty compared to that provided by GW information alone.

In this Letter, we present searches for high-energy neutrinos in coincidence with GW170817/GRB 170817A by the three most sensitive high-energy neutrino observatories: (1) the ANTARES neutrino telescope (hereafter ANTARES; Ageron et al. 2011), a 10 megaton-scale underwater Cherenkov neutrino detector located at a depth of 2500 m in the Mediterranean Sea; (2) the IceCube Neutrino Observatory (hereafter IceCube; Aartsen et al. 2017), a gigaton-scale neutrino detector installed 1500 m deep in the ice at the geographic South Pole, Antarctica; and (3) the Pierre Auger Observatory (hereafter Auger; Aab et al. 2015b), a cosmic-ray air-shower detector consisting of 1660 water-Cherenkov stations spread over an area of ~3000 km$^2$. All three detectors joined the low-latency

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Original content from this work may be used under the terms of the [Creative Commons Attribution 3.0 licence](https://creativecommons.org/licenses/by/3.0/). Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
multi-messenger follow-up effort of LIGO-Virgo starting with LIGO's second observation run, O2.

Upon the identification of the GW signal GW170817, preliminary information on this event was rapidly shared with partner observatories (Abbott et al. 2017c). In response, IceCube (Bartos et al. 2017a, 2017b, 2017c), ANTARES (Ageron et al. 2017a, 2017b), and Auger (Alvarez-Muniz et al. 2017) promptly searched for a neutrino counterpart and shared their initial results with partner observatories. Subsequently, the three facilities carried out a more in-depth search for a neutrino counterpart using the precise localization of the source.

This Letter is organized as follows. In Section 2, we present the neutrino searches carried out by ANTARES, IceCube, and Auger, as well as the results obtained. In Section 3, we present constraints on processes in the merger that can lead to neutrino emission. We summarize our findings and conclude in Section 4.

## 2. Searches and Results

Neutrino observatories detect secondary charged particles produced in neutrino interaction with matter. Surface detectors, such as Auger, use arrays of widely spaced water-Cherenkov detectors to observe the air-shower particles created by high-energy neutrinos. In detectors such as ANTARES and IceCube, three-dimensional arrays of optical modules deployed in water or ice detect the Cherenkov radiation from secondary charged particles that travel through the instrumented detector region. For these detectors, the secondary particles can create two main event classes: track-like events from charged-current interactions of muon neutrinos and from a minority of tau neutrino interactions and shower-like events from all other interactions (neutral-current interactions and charged-current interactions of electron and tau neutrinos). While energy deposition in track-like events can happen over distances of $O(\text{km})$, shower-like events are confined to much smaller regions.

For all detectors, neutrino signals must be identified on top of a persistent background of charged particles produced by the interaction of cosmic-ray particles with the atmosphere above the detectors. This discrimination is done by considering the observed direction and energy of the charged particles. Surface detectors focus on high-energy ($\gtrsim 10^{17}$eV) showers created close to the detector by neutrinos from near-horizontal directions. In-ice and in-water detectors can select well-reconstructed track events from the up-going direction where the Earth is used as a natural shield for the dominant background of penetrating muons from cosmic-ray showers. By requiring the neutrino interaction vertex to be contained inside the instrumented volume, or requiring its energy to be sufficiently high to be incompatible with the down-going muon background, even neutrino events originating above the horizon are identifiable. Neutrinos originating from cosmic-ray interactions in the atmosphere are also observed and constitute the primary background for up-going and vertex-contained event selections.

All three observatories, ANTARES, IceCube, and Auger, performed searches for neutrino signals in coincidence with the binary neutron star merger event GW170817, each using multiple event selections. Two different time windows were used for the searches. First, we used a $\pm 500$ s time window around the merger to search for neutrinos associated with prompt and extended gamma-ray emission (Baret et al. 2011; Kimura et al. 2017). Second, we searched for neutrinos over a longer 14 day time window following the GW detection, to

cover predictions of longer-lived emission processes (e.g., Gao et al. 2013; Fang & Metzger 2017).

### 2.1. ANTARES

The ANTARES neutrino telescope has been continuously operating since 2008. Located deep (2500 m) in the Mediterranean Sea, 40 km from Toulon (France), it is a 10 Mt-scale array of photosensors, detecting neutrinos with energies above $O(100)$ GeV.

Based on the originally communicated locations of the GW signal and the GRB detection, high-energy neutrino candidates were initially searched for in the ANTARES online data stream, relying on a fast algorithm that selects only up-going neutrino track candidates (Adrián-Martínez et al. 2016b). No up-going muon neutrino candidate events were found in a $\pm 500$ s time window centered on the GW event time—for an expected number of atmospheric background events of $\sim 10^{-2}$ during the coincident time window. An extended online search during $\pm 1$ hr also resulted in no up-going neutrino coincidences.

As it subsequently became clear, the precise direction of origin of GW170817 in NGC 4993 was above the ANTARES horizon at the detection time of the binary merger (see Figure 1). Thus, a dedicated analysis looking for down-going muon neutrino candidates in the online ANTARES data stream was also performed. No neutrino counterparts were found in this analysis. The results of these low-latency searches were shared with follow-up partners within a few hours for the up-going search and a few days for the down-going search (Ageron et al. 2017a, 2017b).

Here, ANTARES used an updated high-energy neutrino follow-up of GW170817 that includes the shower channel. It was performed with the offline-reconstructed data set that incorporates dedicated calibration in terms of positioning, timing, and efficiency (Aguilar et al. 2011, 2007; Adrián-Martínez et al. 2012). The analysis has been optimized to increase the sensitivity of the detector and extended to the longer time window of 14 days.

The search for down-going neutrino counterparts to GW170817 was made feasible as the large background affecting this data set can be drastically suppressed by requiring a time and space coincidence with the GW signal. It was optimized, independently for tracks and showers, such that a directional coincidence with NGC 4993 within the search time window of $\pm 500$ s would have $3\sigma$ significance. Muon neutrino candidates were selected by applying cuts on the estimated angular error and the track quality reconstruction parameter. While ANTARES is sensitive to neutrino events with energy as small as $O(100 \text{ GeV})$, the energy range corresponding to the 5%–95% quantiles of the neutrino flux for an $E^{-2}$ signal spectrum is equal to [32 TeV; 22 PeV]. For such a flux, the median angular uncertainty, defined as the median value of the distribution of angles between the reconstructed direction of the event and the true neutrino direction, is equal to $0^{\circ}$5.

Shower events were selected by applying a set of cuts primarily devoted to reducing the background rate (Albert et al. 2017b). The energy range corresponding to the 5%–95% quantiles of the neutrino flux for an $E^{-2}$ signal spectrum is equal to [23 TeV; 16 PeV], while the median angular error is $6^{\circ}$ with this set of relaxed cuts.

No events temporally coincident with GW170817 were found. Five background track events (likely atmospheric muons), not compatible with the source position, were detected
<figure><img src="image_4.png" /><figcaption>**Figure 1.** Localizations and sensitive sky areas at the time of the GW event in equatorial coordinates: GW 90% credible-level localization (red contour; Abbott et al. 2017b), direction of NGC 4993 (black plus symbol; Coulter et al. 2017b), directions of IceCube's and ANTARES's neutrino candidates within 500 s of the merger (green crosses and blue diamonds, respectively), ANTARES's horizon separating down-going (north of horizon) and up-going (south of horizon) neutrino directions (dashed blue line), and Auger's fields of view for Earth-skimming (darker blue) and down-going (lighter blue) directions. IceCube's up-going and down-going directions are on the northern and southern hemispheres, respectively. The zenith angle of the source at the detection time of the merger was 73.8° for ANTARES, 66.6° for IceCube, and 91.9° for Auger.</figcaption></figure>

(see Figure 1). We used this non-detection to constrain the neutrino fluence (see Figure 2) that was computed as in Adrián-Martínez et al. (2016a).

The search over 14 days is restricted to up-going events, but includes all neutrino flavors (tracks and showers). We applied quality cuts optimized for point-source searches that give a median pointing accuracy of 0.4° and 3°, respectively, for track and shower events (Albert et al. 2017b). No events spatially coincident with GRB 170817A were found.

Compared to the upper limits obtained for the short time window of ±500 s, those limits are significantly less stringent above 1 PeV, where the absorption of neutrinos by the Earth becomes important for up-going events. Below 10 TeV, the constraints computed for the 14 day time window are stricter due to the better acceptance in this energy range for up-going neutrino candidates compared to down-going events (see Figure 2).

## 2.2. IceCube

IceCube is a cubic-kilometer-size neutrino detector (Aartsen et al. 2017) installed in the ice at the geographic South Pole in Antarctica between depths of 1450 m and 2450 m. Detector construction was completed in 2010, and the detector has operated with a ~99% duty cycle since. IceCube searched for neutrino signals from GW170817 using two different event selection techniques.

The first search used an online selection of through-going muons, which is used in IceCube's online analyses (Aartsen et al. 2016; Kintscher & The IceCube Collaboration 2016) and follows an event selection similar to that of point source searches (Aartsen et al. 2014a). This event selection picks out primarily cosmic-ray-induced background events, with an expectation of 4.0 events in the northern sky (predominantly generated by atmospheric neutrinos) and 2.7 events in the southern sky (predominantly muons generated by high-energy cosmic rays interactions in the atmosphere above the detector) per 1000 s. For source locations in the southern sky, the sensitivity of the down-going event selection for neutrinos below 1 PeV weakens rapidly with energy due to the rapidly

increasing atmospheric muon background at lower energies. Events found by this track selection in the ±500 s time window are shown in Figure 1. No events were found to be spatially and temporally correlated with GW170817.

A second event selection, described in Wandkowski et al. (2017), was employed offline. This uses the outermost optical sensors of the instrumented volume to veto incoming muon tracks from atmospheric background events. Above 60 TeV, this event selection has the same performance as the high-energy starting-event selection (Aartsen et al. 2014b). Below this energy, additional veto cuts similar to those described in Aartsen et al. (2015) are applied, in order to maintain a low background level at energies down to a few TeV. Both track- and cascade-like events are retained. The event rate for this selection varies over the sky, but is overall much lower than for the online track selection described above. Between declinations -13° and -33°, the mean number of events in a two-week period is 0.4 for tracks and 2.5 for cascades. During the ±500 s time window, no events passed this event selection from anywhere in the sky.

A combined analysis of the IceCube through-going track selection and the starting-event selection allows upper limits to be placed on the neutrino fluence from GW170817 between the energies of 1 TeV and 1 EeV, as shown in Figure 2. In the central range from 10 TeV to 100 PeV, the upper limit for an $E^{-2}$ power-law spectral fluence is $F(E) = 0.19(E/\text{GeV})^{-2} \text{ GeV}^{-1} \text{ cm}^{-2}$.

Both the through-going track selection and the starting-event selection were applied to data collected in the 14 day period following the time of GW170817. Because of IceCube's location at the South Pole and 99.88% on-time during the 14 day period, the exposure to the source location is continuous and unvaried. No spatially and temporally coincident events were seen in either selection during this follow-up period. The resulting upper limits are presented in Figure 2. At most energies these are unchanged from the short time window. At the lowest energies, where most background events occur, the analysis effectively requires stricter criteria for a coincident event than were required in the short time window; the limits are correspondingly higher. In the central range from 10 TeV to
<figure><img src="image_5.png" /><figcaption>**Figure 2.** Upper limits (at 90% confidence level) on the neutrino spectral fluence from GW170817 during a ±500 s window centered on the GW trigger time (top panel), and a 14 day window following the GW trigger (bottom panel). For each experiment, limits are calculated separately for each energy decade, assuming a spectral fluence $F(E) = F_{up} \times [E/\text{GeV}]^{-2}$ in that decade only. Also shown are predictions by neutrino emission models. In the upper plot, models from Kimura et al. (2017) for both extended emission (EE) and prompt emission are scaled to a distance of 40 Mpc and shown for the case of the on-axis viewing angle ($\theta_{obs} \lesssim \theta_j$) and selected off-axis angles to indicate the dependence on this parameter. The shown off-axis angles are measured in excess of the jet opening half-angle $\theta_j$. GW data and the redshift of the host galaxy constrain the viewing angle to $\theta_{obs} \in [0^\circ, 36^\circ]$ (see Section 3). In the lower plot, models from Fang & Metzger (2017) are scaled to a distance of 40 Mpc. All fluences are shown as the per the flavor sum of neutrino and anti-neutrino fluence, assuming equal fluence in all flavors, as expected for standard neutrino oscillation parameters.</figcaption></figure>

100 PeV, the upper limit on an $E^{-2}$ power-law spectral fluence is $F(E) = 0.23 \times (E/\text{GeV})^{-2} \text{ GeV}^{-1} \text{ cm}^{-2}$.

The IceCube detector is also sensitive to outbursts of MeV neutrinos via a simultaneous increase in all photomultiplier signal rates. A neutrino burst signal from a galactic core-collapse supernova would be detected with high precision (Abbasi et al. 2011). The detector global dark rate is monitored continuously, the influence of cosmic-ray muons is removed, and low-level triggers are formed when deviations from the nominal rate exceed pre-defined levels. No alert was triggered during the ±500 s time window around the GW candidate. This is consistent with our expectations for cosmic events such as core-collapse supernovae or compact binary mergers that are significantly farther away than Galactic distances.

## 2.3. Pierre Auger Observatory

With the surface detector (SD) of the Pierre Auger Observatory in Malargüe, Argentina (Aab et al. 2015b), air showers induced by ultra-high-energy (UHE) neutrinos can be

identified for energies above ~10¹⁷ eV in the more numerous background of UHE cosmic rays (Aab et al. 2015a). The SD consists of 1660 water-Cherenkov stations spread over an area of ~3000 km² following a triangular arrangement of 1.5 km grid spacing (Aab et al. 2015b). The signals produced by the passage of shower particles through the SD detectors are recorded as time traces in 25 ns intervals.

Cosmic rays interact shortly after entering the atmosphere and induce extensive air showers. For highly inclined directions their electromagnetic component gets absorbed due to the large grammage of atmosphere from the first interaction point to the ground. As a consequence, the shower front at ground level is dominated by muons that induce sharp time traces in the water-Cherenkov stations. On the contrary, showers induced by downward-going neutrinos at large zenith angles can start their development deep in the atmosphere producing traces that spread over longer times. These showers have a considerable fraction of electrons and photons that undergo more interactions than muons in the atmosphere, spreading more in time as they pass through the detector. This is also the case for Earth-skimming showers, mainly induced by tau neutrinos ($\nu_\tau$) that traverse horizontally below the Earth's crust, and interact near the exit point inducing a tau lepton that escapes the Earth and decays in flight in the atmosphere above the SD.

Dedicated and efficient selection criteria based on the different time profiles of the signals detected in showers created by hadronic and neutrino primaries, enable the search for Earth-skimming as well as downward-going neutrino-induced showers (Aab et al. 2015a). Deeply starting downward-going showers initiated by neutrinos of any flavor can be efficiently identified for zenith angles of 60° < $\theta$ < 90° (Aab et al. 2015a). For the Earth-skimming channel typically only $\nu_\tau$-induced showers with zenith angles 90° < $\theta$ < 95° can trigger the SD. This is the most sensitive channel to UHE neutrinos, mainly due to the larger grammage and higher density of the target (the Earth) where neutrinos are converted and where tau leptons can travel tens of kilometers (Aab et al. 2015a). The angular resolution of the Auger SD for inclined showers is better than 2°5, improving significantly as the number of triggered stations increases (Bonifazi & Pierre Auger Collaboration 2009).

Auger performed a search for UHE neutrinos with its SD in a time window of ±500 s centered at the merger time of GW170817 (Abbott et al. 2017c), as well as in a 14 day period after it (Murase et al. 2009; Gao et al. 2013; Fang & Metzger 2017).

The sensitivity to UHE neutrinos in Auger is limited to large zenith angles, so that at each instant they can be efficiently detected only from a specific fraction of the sky (Abreu et al. 2012; Aab et al. 2016). Remarkably, the position of the optical counterpart in NGC 4993 (Abbott et al. 2017c; Coulter et al. 2017b, 2017a) is visible from Auger in the field of view of the Earth-skimming channel during the whole ±500 s window as shown in Figure 1. In this time period, the source of GW170817 transits from $\theta \sim 93^\circ$3 to $\theta \sim 90^\circ$4 as seen from the center of the array. The performance of the Auger SD array (regularly monitored every minute) is very stable in the ±500 s window around GW170817, with an average number of active stations amounting to ~95.8 ± 0.1% of the 1660 stations of the SD array.
No inclined showers passing the Earth-skimming selection (neutrino candidates) were found in the time window ±500 s around the trigger time of GW170817. The estimated number of background events from cosmic rays in a 1000 s period is ~6.3 × 10⁻⁷ for the cuts applied in the Earth-skimming analysis (Aab et al. 2015a).

The absence of candidates in the ±500 s window allows us to constrain the fluence in UHE neutrinos from GW170817, assuming they are emitted steadily in this interval and with an $E^{-2}$ spectrum (Aab et al. 2016). Single-flavor differential limits to the spectral fluence are shown in Figure 2, in bins of one decade in energy. The sensitivity of the observatory is largest in the energy bin around 10¹⁸ eV. The single-flavor upper limit to the spectral fluence is $F(E) = 0.77(E/\text{GeV})^{-2} \text{GeV}^{-1} \text{cm}^{-2}$ over the energy range from 10¹⁷ eV to 2.5 × 10¹⁹ eV.

In the 14 day search period, as the Earth rotates, the position of NGC 4993 transits through the field of view of the Earth-skimming and downward-going channels. As seen from the Pierre Auger Observatory, the zenith angle of the optical counterpart oscillates daily between $\theta \sim 11^\circ$ and $\theta \sim 121^\circ$. The source is visible in the Earth-skimming channel for ~4% of the day and in the downward-going channel for ~10.5% (~11.1%) in the zenith angle range $60^\circ < \theta < 75^\circ$ ($75^\circ < \theta < 90^\circ$). No neutrino candidates were identified in the two-week search period. Single-flavor differential limits to the spectral fluence are shown in Figure 2. The corresponding upper limit to the spectral fluence is $F(E) = 25(E/\text{GeV})^{-2} \text{GeV}^{-1} \text{cm}^{-2}$ over the same energy interval as for the ±500 s time window, where the difference is due to the relatively long periods of time when the source of GW170817 is not visible in the inclined directions.

### 3. Discussion

The nature of high-energy emission from the binary merger and its aftermath is not yet clear. We compared the expected spectral fluence for different emission scenarios to our observational upper limits to probe the properties of the merger and its aftermath. Here, we briefly outline the relevant information from electromagnetic observations and present our results for the different emission scenarios.

The merger occurred at a distance of ~40 Mpc, which is the distance of its host galaxy NGC 4993, identified through electromagnetic observations (Abbott et al. 2017c; Coulter et al. 2017a, 2017b). The prompt gamma-ray emission from the source, GRB 170817A, had an observed isotropic-equivalent energy of $E_{iso} \approx 4 \times 10^{46}$ erg, as recorded by Fermi-GBM (Abbott et al. 2017a). This is orders of magnitude below typical observed short GRB energies (Berger 2014; Abbott et al. 2017a).

Prompt gamma-ray emission in at least some short GRBs is followed by a weaker, extended emission that can last for hundreds of seconds (Norris & Bonnell 2006; Kimura et al. 2017). Fermi-GBM did not detect a temporally extended emission following GRB 170817A, placing a constraint of ~2 × 10⁴⁶ erg s⁻¹ for a 10 s long emission period over 1 keV–10 MeV (Abbott et al. 2017a), significantly below typical luminosities observed for extended emission.

The very faint gamma-ray emission, along with its observed, delayed afterglow, are consistent with a typical short GRB viewed off-axis (Fong et al. 2017; Fraija et al. 2017; Granot et al. 2017; Haggard et al. 2017; Hallinan et al. 2017; Ioka & Nakamura 2017; Kim et al. 2017; Margutti et al. 2017; Murguia-Berthier et al. 2017; Troja et al. 2017). A GRB is

viewed off-axis if its viewing angle $\theta_{obs}$, defined as the angle between the jet axis and the line of sight, is greater than the jet opening half-angle $\theta_j$ (Granot et al. 2002). The viewing angle inferred from the data is $\theta_{obs} \gtrsim 20^\circ$, while typical opening half-angles for short GRBs are within $\theta_j \approx 3^\circ–10^\circ$ (Berger 2014).

GW data combined with the measured redshift of the host galaxy further provide constraints on $\theta_{obs}$. Here, we assume that the jet axis is aligned with the binary's total angular momentum vector. Adopting the Hubble constant from cosmic microwave background measurements by the Planck satellite (Ade et al. 2016), these data are consistent with $\theta_{obs} = 0$, but also allow for a misalignment of $\theta_{obs} \le 28^\circ$ at a 90% credible level. Adopting the Hubble constant from Type Ia supernova measurements (Riess et al. 2016) gives a similar result with maximum misalignment of $\theta_{obs} \le 36^\circ$ at a 90% credible level (Abbott et al. 2017d).

Considering this off-axis scenario, we examined the expected high-energy neutrino emission from a typical GRB observed at different viewing angles. The most promising neutrino-production mechanism from GRBs is related to the extended gamma emission, due to its relatively low Lorentz factor resulting in high meson production efficiency (Kimura et al. 2017). In Figure 2, we compared our observational constraints with the expected neutrino fluence from the GRB's extended emission. For the on-axis (i.e., $\theta_{obs} \lesssim \theta_j$) spectral fluence $F_{on}$, we assumed the results of Kimura et al. (2017), rescaled to 40 Mpc. We approximated the observed off-axis spectral fluence, $F_{off}(E)$, for these models using $F_{off}(E) = \eta F_{on}(E/\eta)$, where the scaling factor $\eta = \delta(\theta_{obs})/\delta(0)$ accounts for different Doppler factors $\delta(\theta_{obs}) = [\Gamma(1 - \beta \cos(\theta_{obs} - \theta_j))]^{-1}$ (Granot et al. 2002).

For comparison, we also examined the expected neutrino flux associated with the prompt GRB emission (e.g., Moharana et al. 2016; Kimura et al. 2017). This emission phase is less favorable for neutrino production than the extended emission. We see in Figure 2 that prompt emission from a single merger event is unlikely to produce a detected neutrino for the considered observatories, even if viewed on-axis.

Another proposed explanation for the faintness of gamma-ray emission is the interaction of the GRB jet with ejecta material from the merger (Gottlieb et al. 2017; Kasliwal et al. 2017; Piro & Kollmeier 2017). Energy deposition by the jet into the neutron star ejecta can form a cocoon that expands outwards at mildly relativistic speeds over a wide opening angle. Faint gamma-ray emission is then expected during the breakout of this cocoon from the outer tail of the ejecta (Gottlieb et al. 2017).

High-energy neutrino production in this scenario may significantly exceed the observed gamma-ray emission as neutrinos can escape through the ejecta even before it becomes transparent to gamma-rays. This scenario resembles that of a jet burrowing through the stellar envelope in a core-collapse event (Mészáros and Waxman 2001; Razzaque et al. 2003; Bartos et al. 2012; Murase & Ioka 2013). Nevertheless, if the observed gamma-rays come from the outbreak of a wide cocoon, it is less likely that the relativistic jet, which is more narrowly beamed than the cocoon outbreak, also pointed toward Earth.

We further considered an additional neutrino-production mechanism related to ejecta material from the merger. If a rapidly rotating neutron star forms in the merger and does not immediately collapse into a black hole, it can power a relativistic wind with its rotational energy, which may be responsible for the sometimes observed extended emission
(Metzger et al. 2008). Optically thick ejecta from the merger can attenuate the gamma-ray flux, while allowing the escape of high-energy neutrinos. Additionally, it may trap some of the wind energy until it expands and becomes transparent. This process can convert some of the wind energy to high-energy particles, producing a *long-term* neutrino radiation that can last for days (Murase et al. 2009; Gao et al. 2013; Fang & Metzger 2017). The properties of ejecta material around the merger can be characterized from its kilonova/macronova emission.

Considering the possibility that the relative weakness of gamma-ray emission from GRB 170817A may be partly due to attenuation by the ejecta, we compared our neutrino constraints to neutrino emission expected for typical GRB parameters. For the prompt and extended emissions, we used the results of Kimura et al. (2017) and compared these to our constraints for the relevant ±500 s time window. For extended emission we considered source parameters corresponding to both optimistic and moderate scenarios in Table 1 of Kimura et al. (2017). For emission on even longer timescales, we compared our constraints for the 14 day time window with the relevant results of Fang & Metzger (2017), namely, emission from approximately 0.3 to 3 days and from 3 to 30 days following the merger. Predictions based on fiducial emission models and neutrino constraints are shown in Figure 2. We found that our limits would constrain the optimistic extended-emission scenario for a typical GRB at ~40 Mpc, viewed at zero viewing angle.

## 4. Conclusion

We searched for high-energy neutrinos from the first binary neutron star merger detected through GWs, GW170817, in the energy band of [~$10^{11}$ eV, ~$10^{20}$ eV] using the ANTARES, IceCube, and Pierre Auger Observatories, as well as for MeV neutrinos with IceCube. This marks an unprecedented joint effort of experiments sensitive to high-energy neutrinos. We have observed no significant neutrino counterpart within a ±500 s window, nor in the subsequent 14 days. The three detectors complement each other in the energy bands in which they are most sensitive (see Figure 2).

This non-detection is consistent with our expectations from a typical GRB observed off-axis, or with a low-luminosity GRB. Optimistic scenarios for on-axis gamma-attenuated emission are constrained by the present non-detection.

While the location of this source was nearly ideal for Auger, it was well above the horizon for IceCube and ANTARES for prompt observations. This limited the sensitivity of the latter two detectors, particularly below ~100 TeV. For source locations near, or below the horizon, a factor of ~10 increase in fluence sensitivity to prompt emission from an $E^{-2}$ neutrino spectrum is expected.

With the discovery of a nearby binary neutron star merger, the ongoing enhancement of detector sensitivity (Abbott et al. 2016) and the growing network of GW detectors (Iyer et al. 2011; Aso et al. 2013), we can expect that several binary neutron star mergers will be observed in the near future. Not only will this allow stacking analyses of neutrino emission, but it will also bring about sources with favorable orientation and direction.

The ANTARES, IceCube, and Pierre Auger Collaborations are planning to continue the rapid search for neutrino candidates from identified GW sources. A coincident neutrino, with a typical position uncertainty of ~1 deg$^2$ could significantly

improve the fast localization of joint events compared to the GW-only case. In addition, the first joint GW and high-energy neutrino discovery might thereby be known to the wider astronomy community within minutes after the event, opening a rich field of multi-messenger astronomy with particle, electromagnetic, and gravitational waves combined.

(ANTARES) The ANTARES authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Commission Européenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A\*MIDEX project (ANR-11-IDEX-0001-02), Région Île-de-France (DIM-ACAV), Région Alsace (contrat CPER), Région Provence-Alpes-Côte d'Azur, Département du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium für Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Economía y Compañitividad (MINECO); Plan Estatal de Investigación (refs. FPA2015-65150-C3-1-P, -2-P, and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisolía programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM, and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.

(IceCube) The IceCube collaboration acknowledges the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin—Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Initiative and Networking Fund of the Helmholtz Association, Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark.
(Auger) The successful installation, commissioning, and operation of the Pierre Auger Observatory would not have been possible without the strong commitment and effort from the technical and administrative staff in Malargüe. We are very grateful to the following agencies and organizations for financial support:

Argentina—Comisión Nacional de Energía Atómica; Agencia Nacional de Promoción Científica y Tecnológica (ANPCyT); Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET); Gobierno de la Provincia de Mendoza; Municipalidad de Malargüe; NDM Holdings and Valle Las Leñas; in gratitude for their continuing cooperation over land access; Australia—the Australian Research Council; Brazil—Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq); Financiadora de Estudos y Proyectos (FINEP); Fundação de Amparo à Pesquisa do Estado de Rio de Janeiro (FAPERJ); São Paulo Research Foundation (FAPESP) grant Nos. 2010/07359-6 and 1999/05404-3; Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC); Czech Republic—grant No. MSMT CR LG15014, LO1305, LM2015038 and CZ.02.1.01/0.0/0.0/16_013/0001402; France—Centre de Calcul IN2P3/CNRS; Centre National de la Recherche Scientifique (CNRS); Conseil Régional Ile-de-France; Département Physique Nucléaire et Corpusculaire (PNC-IN2P3/CNRS); Département Sciences de l'Univers (SDU-INSU/CNRS); Institut Lagrange de Paris (ILP) grant No. LABEX ANR-10-LABX-63 within the Investissements d'Avenir Programme grant No. ANR-11-IDEX-0004-02; Germany—Bundesministerium für Bildung und Forschung (BMBF); Deutsche Forschungsgemeinschaft (DFG); Finanzministerium Baden-Württemberg; Helmholtz Alliance for Astroparticle Physics (HAP); Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF); Ministerium für Innovation, Wissenschaft und Forschung des Landes Nordrhein-Westfalen; Ministerium für Wissenschaft, Forschung und Kunst des Landes Baden-Württemberg; Italy—Istituto Nazionale di Fisica Nucleare (INFN); Istituto Nazionale di Astrofisica (INAF); Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR); CETEMPS Center of Excellence; Ministero degli Affari Esteri (MAE); Mexico—Consejo Nacional de Ciencia y Tecnología (CONACYT) No. 167733; Universidad Nacional Autónoma de México (UNAM); PAPIIT DGAPA-UNAM; The Netherlands—Ministerie van Onderwijs, Cultuur en Wetenschap; Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); Stichting voor Fundamenteel Onderzoek der Materie (FOM); Poland—National Centre for Research and Development, grant Nos. ERA-NET-ASPERA/01/11 and ERA-NET-ASPERA/02/11; National Science Centre, grant Nos. 2013/08/M/ST9/00322, 2013/08/M/ST9/00728 and HARMONIA 5–2013/10/M/ST9/00062, UMO-2016/22/M/ST9/00198; Portugal—Portuguese national funds and FEDER funds within Programa Operacional Factores de Competitividade through Fundação para a Ciência e a Tecnologia (COMPETE); Romania—Romanian Authority for Scientific Research ANCS; CNDI-UEFISCDI partnership projects grant Nos. 20/2012 and 194/2012 and PN 16 42 01 02; Slovenia—Slovenian Research Agency; Spain—Comunidad de Madrid; Fondo Europeo de Desarrollo Regional (FEDER) funds; Ministerio de Economía y Competitividad; Xunta de Galicia; European Community 7th Framework Program grant No. FP7-PEOPLE-2012-IEF-328826; USA—Department of Energy, Contract Nos. DE-AC02-07CH11359, DE-FR02-04ER41300, DE-FG02-99ER41107 and DE-SC0011689; National Science Foundation, grant No. 0450696; The Grainger Foundation; Marie

Curie-IRSES/EPLANET; European Particle Physics Latin American Network; European Union 7th Framework Program, grant No. PIRSES-2009-GA-246806; European Union's Horizon 2020 research and innovation programme (grant No. 646623); and UNESCO.

(LIGO and Virgo) The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidencia i Conselleria d'Innovació Recerca i Turisme and the Conselleria d'Educació i Universitat del Govern de les Illes Balears, the Conselleria d'Educació Investigació Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research, Development and Innovation Office Hungary (NKFI), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources.

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K. Clark⁷⁶, L. Classen⁷⁷, S. Coenders⁷⁸, G. H. Collin⁵⁶, J. M. Conrad⁵⁶, D. F. Cowen⁵⁵,⁷⁹, R. Cross⁶⁷, M. Day⁷⁴,
J. P. A. M. de André⁸⁰, C. De Clercq⁷⁵, J. J. DeLaunay⁵⁵, H. Dembinski⁸¹, S. De Ridder⁸², P. Desiati⁷⁴, K. D. de Vries⁷⁵,
G. de Wasseige<sup>75</sup>, M. de With<sup>83</sup>, T. DeYoung<sup>80</sup>, J. C. Díaz-Vélez<sup>74</sup>, V. di Lorenzo<sup>61</sup>, H. Dujmovic<sup>72</sup>, J. P. Dumm<sup>51</sup>, M. Dunkman<sup>55</sup>, E. Dvorak<sup>58</sup>, B. Eberhardt<sup>61</sup>, T. Ehrhardt<sup>61</sup>, B. Eichmann<sup>65</sup>, P. Eller<sup>55</sup>, P. A. Evenson<sup>81</sup>, S. Fahey<sup>74</sup>, A. R. Fazely<sup>84</sup>, J. Felde<sup>68</sup>, K. Filimonov<sup>62</sup>, C. Finley<sup>51</sup>, S. Flis<sup>51</sup>, A. Franckowiak<sup>47</sup>, E. Friedman<sup>68</sup>, T. Fuchs<sup>71</sup>, T. K. Gaisser<sup>81</sup>, J. Gallagher<sup>85</sup>, L. Gerhardt<sup>70</sup>, K. Ghorbani<sup>74</sup>, W. Giang<sup>59</sup>, T. Glauch<sup>57</sup>, T. Glüsenkamp<sup>53</sup>, A. Goldschmidt<sup>70</sup>, J. G. Gonzalez<sup>81</sup>, D. Grant<sup>59</sup>, Z. Griffith<sup>74</sup>, C. Haack<sup>57</sup>, A. Hallgren<sup>73</sup>, F. Halzen<sup>74</sup>, K. Hanson<sup>74</sup>, D. Hebecker<sup>83</sup>, D. Heereman<sup>49</sup>, K. Helbing<sup>66</sup>, R. Hellauer<sup>68</sup>, S. Hickford<sup>66</sup>, J. Hignight<sup>80</sup>, G. C. Hill<sup>46</sup>, K. D. Hoffman<sup>68</sup>, R. Hoffmann<sup>66</sup>, B. Hokanson-Fasig<sup>74</sup>, K. Hoshina<sup>74,86</sup>, F. Huang<sup>55</sup>, M. Huber<sup>78</sup>, K. Hultqvist<sup>51</sup>, M. Hünnefeld<sup>71</sup>, S. In<sup>72</sup>, A. Ishihara<sup>87</sup>, E. Jacobi<sup>47</sup>, G. S. Japaridze<sup>88</sup>, M. Jeong<sup>72</sup>, K. Jero<sup>74</sup>, B. J. P. Jones<sup>89</sup>, P. Kalaczynski<sup>57</sup>, W. Kang<sup>72</sup>, A. Kappes<sup>77</sup>, T. Karg<sup>47</sup>, A. Karle<sup>74</sup>, U. Katz<sup>53</sup>, M. Kauer<sup>74</sup>, A. Keivani<sup>55</sup>, J. L. Kelley<sup>74</sup>, A. Kheirandish<sup>74</sup>, J. Kim<sup>72</sup>, M. Kim<sup>87</sup>, T. Kintscher<sup>47</sup>, J. Kiryluk<sup>90</sup>, T. Kittler<sup>53</sup>, S. R. Klein<sup>62,70</sup>, G. Kohnen<sup>91</sup>, R. Koirala<sup>81</sup>, H. Kolanoski<sup>83</sup>, L. Köpke<sup>61</sup>, C. Kopper<sup>59</sup>, S. Kopper<sup>92</sup>, J. P. Koschinsky<sup>57</sup>, D. J. Koskinen<sup>50</sup>, M. Kowalski<sup>47,83</sup>, K. Krings<sup>78</sup>, M. Kroll<sup>65</sup>, G. Krück<sup>61</sup>, J. Kunnen<sup>75</sup>, S. Kunwar<sup>47</sup>, N. Kurahashi<sup>93</sup>, T. Kuwabara<sup>87</sup>, A. Kyriacou<sup>46</sup>, M. Labare<sup>82</sup>, J. L. Lanfranchi<sup>55</sup>, M. J. Larson<sup>50</sup>, F. Lauber<sup>66</sup>, M. Lesiak-Bzdak<sup>90</sup>, M. Leuermann<sup>57</sup>, Q. R. Liu<sup>74</sup>, L. Lu<sup>87</sup>, J. Lünemann<sup>75</sup>, W. Luszczak<sup>74</sup>, J. Madsen<sup>94</sup>, G. Maggi<sup>75</sup>, K. B. M. Mahn<sup>80</sup>, S. Mancina<sup>74</sup>, R. Maruyama<sup>95</sup>, K. Mase<sup>87</sup>, R. Maunu<sup>68</sup>, F. McNally<sup>74</sup>, K. Meagher<sup>49</sup>, M. Medici<sup>50</sup>, M. Meier<sup>71</sup>, T. Menne<sup>71</sup>, G. Merino<sup>74</sup>, T. Meures<sup>49</sup>, S. Miarecki<sup>62,70</sup>, J. Micallef<sup>80</sup>, G. Momente<sup>61</sup>, T. Montaruli<sup>52</sup>, R. W. Moore<sup>59</sup>, M. Moulai<sup>56</sup>, R. Nahnhauer<sup>47</sup>, P. Nakarmi<sup>92</sup>, U. Naumann<sup>66</sup>, G. Neer<sup>80</sup>, H. Niederhausen<sup>90</sup>, S. C. Nowicki<sup>59</sup>, D. R. Nygren<sup>70</sup>, A. Obertacke Pollmann<sup>66</sup>, A. Olivas<sup>68</sup>, A. O'Murchadha<sup>49</sup>, T. Palczewski<sup>62,70</sup>, H. Pandya<sup>81</sup>, D. V. Pankova<sup>55</sup>, P. Peiffer<sup>61</sup>, J. A. Pepper<sup>92</sup>, C. Pérez de los Heros<sup>73</sup>, D. Pieloth<sup>71</sup>, E. Pinat<sup>49</sup>, M. Plum<sup>54</sup>, D. Pranav<sup>96</sup>, P. B. Price<sup>62</sup>, G. T. Przybylski<sup>70</sup>, C. Raab<sup>49</sup>, L. Rädel<sup>57</sup>, M. Rameez<sup>50</sup>, K. Rawlins<sup>97</sup>, I. C. Rea<sup>78</sup>, R. Reimann<sup>57</sup>, B. Relethford<sup>93</sup>, M. Relich<sup>87</sup>, E. Resconi<sup>78</sup>, W. Rhode<sup>71</sup>, M. Richman<sup>93</sup>, S. Robertson<sup>46</sup>, M. Rongen<sup>57</sup>, C. Rott<sup>72</sup>, T. Ruhe<sup>71</sup>, D. Ryckbosch<sup>82</sup>, D. Rysewyk<sup>80</sup>, T. Sälzer<sup>57</sup>, S. E. Sanchez Herrera<sup>59</sup>, A. Sandrock<sup>71</sup>, J. Sandroos<sup>61</sup>, M. Santander<sup>92</sup>, S. Sarkar<sup>50,98</sup>, S. Sarkar<sup>59</sup>, K. Satalecka<sup>47</sup>, P. Schlunder<sup>71</sup>, T. Schmidt<sup>68</sup>, A. Schneider<sup>74</sup>, S. Schoenen<sup>57</sup>, S. Schöneberg<sup>65</sup>, L. Schumacher<sup>57</sup>, D. Seckel<sup>81</sup>, S. Seunarine<sup>94</sup>, J. Soedingrekso<sup>71</sup>, D. Soldin<sup>66</sup>, M. Song<sup>68</sup>, G. M. Spiczak<sup>94</sup>, C. Spiering<sup>47</sup>, J. Stachurska<sup>47</sup>, M. Stamatikos<sup>63</sup>, T. Stanev<sup>81</sup>, A. Stasik<sup>47</sup>, J. Stettner<sup>57</sup>, A. Steuer<sup>61</sup>, T. Stezelberger<sup>70</sup>, R. G. Stokstad<sup>70</sup>, A. Stößl<sup>87</sup>, N. L. Strotjohann<sup>47</sup>, T. Stuttard<sup>50</sup>, G. W. Sullivan<sup>68</sup>, M. Sutherland<sup>63</sup>, I. Taboada<sup>96</sup>, J. Tatar<sup>62,70</sup>, F. Tenholt<sup>65</sup>, S. Ter-Antonyan<sup>84</sup>, A. Terliuk<sup>47</sup>, G. Tešić<sup>55</sup>, S. Tilav<sup>81</sup>, P. A. Toale<sup>92</sup>, M. N. Tobin<sup>74</sup>, S. Toscano<sup>75</sup>, D. Tosi<sup>74</sup>, M. Tselengidou<sup>53</sup>, C. F. Tung<sup>96</sup>, A. Turcati<sup>78</sup>, C. F. Turley<sup>55</sup>, B. Ty<sup>74</sup>, E. Unger<sup>73</sup>, M. Usner<sup>47</sup>, J. Vandenbroucke<sup>74</sup>, W. Van Driessche<sup>82</sup>, N. van Eijndhoven<sup>75</sup>, S. Vanheule<sup>82</sup>, J. van Santen<sup>47</sup>, M. Vehring<sup>57</sup>, E. Vogel<sup>57</sup>, M. Vraeghe<sup>82</sup>, C. Walck<sup>51</sup>, A. Wallace<sup>46</sup>, M. Wallraff<sup>57</sup>, F. D. Wandler<sup>59</sup>, N. Wandkowsky<sup>74</sup>, A. Waza<sup>57</sup>, C. Weaver<sup>59</sup>, M. J. Weiss<sup>55</sup>, C. Wendt<sup>74</sup>, J. Werthebach<sup>71</sup>, S. Westerhoff<sup>74</sup>, B. J. Whelan<sup>46</sup>, K. Wiebe<sup>61</sup>, C. H. Wiebusch<sup>57</sup>, L. Wille<sup>74</sup>, D. R. Williams<sup>92</sup>, L. Wills<sup>93</sup>, M. Wolf<sup>74</sup>, J. Wood<sup>74</sup>, T. R. Wood<sup>59</sup>, E. Woolsey<sup>59</sup>, K. Woschnagg<sup>62</sup>, D. L. Xu<sup>74</sup>, X. W. Xu<sup>84</sup>, Y. Xu<sup>90</sup>, J. P. Yanez<sup>59</sup>, G. Yodh<sup>60</sup>, S. Yoshida<sup>87</sup>, T. Yuan<sup>74</sup>, M. Zoll<sup>51</sup>

(IceCube Collaboration)

A. Aab<sup>99</sup>, P. Abreu<sup>100</sup>, M. Aglietta<sup>101,102</sup>, I. F. M. Albuquerque<sup>103</sup>, J. M. Albury<sup>104</sup>, I. Allekotte<sup>105</sup>, A. Almela<sup>106,107</sup>, J. Alvarez Castillo<sup>108</sup>, J. Alvarez-Muñiz<sup>109</sup>, G. A. Anastasi<sup>110,111</sup>, L. Anchordoqui<sup>112</sup>, B. Andrada<sup>106</sup>, S. Andringa<sup>100</sup>, C. Aramo<sup>113</sup>, N. Arsene<sup>114</sup>, H. Asorey<sup>105,115</sup>, P. Assis<sup>100</sup>, G. Avila<sup>116,117</sup>, A. M. Badescu<sup>118</sup>, A. Balaceanu<sup>119</sup>, F. Barbato<sup>120</sup>, R. J. Barreira Luz<sup>100</sup>, J. J. Beatty<sup>121</sup>, K. H. Becker<sup>122</sup>, J. A. Bellido<sup>104</sup>, C. Berat<sup>123</sup>, M. E. Bertaina<sup>102,124</sup>, X. Bertou<sup>105</sup>, P. L. Biermann<sup>125</sup>, J. Biteau<sup>126</sup>, S. G. Blaess<sup>104</sup>, A. Blanco<sup>100</sup>, J. Blazek<sup>127</sup>, C. Bleve<sup>128,129</sup>, M. Boháčová<sup>127</sup>, C. Bonifazi<sup>130</sup>, N. Borodai<sup>131</sup>, A. M. Botti<sup>106,132</sup>, J. Brack<sup>133</sup>, I. Brancus<sup>119</sup>, T. Bretz<sup>134</sup>, A. Bridgeman<sup>135</sup>, F. L. Briechle<sup>134</sup>, P. Buchholz<sup>136</sup>, A. Bueno<sup>137</sup>, S. Buitink<sup>99</sup>, M. Buscemi<sup>138,139</sup>, K. S. Caballero-Mora<sup>140</sup>, L. Caccianiga<sup>141</sup>, A. Cancio<sup>106,107</sup>, F. Canfora<sup>99</sup>, R. Caruso<sup>138,139</sup>, A. Castellina<sup>101,102</sup>, F. Catalani<sup>142</sup>, G. Cataldi<sup>129</sup>, L. Cazon<sup>100</sup>, A. G. Chavez<sup>143</sup>, J. A. Chinellato<sup>144</sup>, J. Chudoba<sup>127</sup>, R. W. Clay<sup>104</sup>, A. C. Cobos Cerutti<sup>145</sup>, R. Colalillo<sup>113,120</sup>, A. Coleman<sup>146</sup>, L. Collica<sup>102</sup>, M. R. Coluccia<sup>128,129</sup>, R. Conceição<sup>100</sup>, G. Consolati<sup>147,148</sup>, F. Contreras<sup>116,117</sup>, M. J. Cooper<sup>104</sup>, S. Coutu<sup>146</sup>, C. E. Covault<sup>149</sup>, J. Cronin<sup>150,357</sup>, S. D'Amico<sup>129,151</sup>, B. Daniel<sup>144</sup>, S. Dasso<sup>152,153</sup>, K. Daumiller<sup>132</sup>, B. R. Dawson<sup>104</sup>, J. A. Day<sup>104</sup>, R. M. de Almeida<sup>154</sup>, S. J. de Jong<sup>99,155</sup>, G. De Mauro<sup>99</sup>, J. R. T. de Mello Neto<sup>130,156</sup>, I. De Mitri<sup>128,129</sup>, J. de Oliveira<sup>154</sup>, V. de Souza<sup>157</sup>, J. Debatin<sup>135</sup>, O. Deligny<sup>126</sup>, M. L. Díaz Castro<sup>144</sup>, F. Diogo<sup>100</sup>, C. Dobrigkeit<sup>144</sup>, J. C. D'Olivo<sup>108</sup>, Q. Dorosti<sup>136</sup>, R. C. dos Anjos<sup>158</sup>, M. T. Dova<sup>159</sup>, A. Dundovic<sup>160</sup>, J. Ebr<sup>127</sup>, R. Engel<sup>132</sup>, M. Erdmann<sup>134</sup>, M. Erfani<sup>136</sup>, C. O. Escobar<sup>161</sup>, J. Espadanal<sup>100</sup>, A. Etchegoyen<sup>106,107</sup>, H. Falcke<sup>99,155,162</sup>, J. Farmer<sup>150</sup>, G. Farrar<sup>163</sup>, A. C. Fauth<sup>144</sup>, N. Fazzini<sup>161</sup>, F. Feldbusch<sup>164</sup>, F. Fenu<sup>102,124</sup>, B. Fick<sup>165</sup>, J. M. Figueira<sup>106</sup>, A. Filipčič<sup>166,167</sup>, M. M. Freire<sup>168</sup>, T. Fujii<sup>150</sup>, A. Fuster<sup>106,107</sup>, R. Gaïor<sup>169</sup>, B. García<sup>145</sup>, F. Gate<sup>170</sup>, H. Gemmeke<sup>164</sup>, A. Gherghel-Lascu<sup>119</sup>, P. L. Ghia<sup>126</sup>, U. Giaccari<sup>130,171</sup>, M. Giammarchi<sup>147</sup>, M. Giller<sup>172</sup>, D. Glas<sup>173</sup>, C. Glaser<sup>134</sup>, G. Golup<sup>105</sup>, M. Gómez Berisso<sup>105</sup>, P. F. Gómez Vitale<sup>116,117</sup>, N. González<sup>106,132</sup>, A. Gorgi<sup>101,102</sup>, M. Gottowik<sup>122</sup>, A. F. Grillo<sup>111,358</sup>, T. D. Grubb<sup>104</sup>, F. Guarino<sup>113,120</sup>, G. P. Guedes<sup>174</sup>, R. Halliday<sup>149</sup>, M. R. Hampel<sup>106</sup>, P. Hansen<sup>159</sup>, D. Harari<sup>105</sup>, T. A. Harrison<sup>104</sup>, V. M. Harvey<sup>104</sup>, A. Haungs<sup>132</sup>, T. Hebbeker<sup>134</sup>, D. Heck<sup>132</sup>, P. Heimann<sup>136</sup>, A. E. Herve<sup>135</sup>, G. C. Hill<sup>104</sup>, C. Hojvat<sup>161</sup>, E. Holt<sup>106,132</sup>, P. Homola<sup>131</sup>, J. R. Hörandel<sup>99,155</sup>, P. Horvath<sup>175</sup>, M. Hrabovsky<sup>175</sup>, T. Huege<sup>132</sup>, J. Hulsman<sup>106,132</sup>, A. Insolia<sup>138,139</sup>, P. G. Isar<sup>114</sup>, I. Jandt<sup>122</sup>, J. A. Johnsen<sup>176</sup>, M. Josebachuili<sup>106</sup>, J. Jurysek<sup>127</sup>, A. Kääpä<sup>122</sup>, K. H. Kampert<sup>122</sup>, B. Keilhauer<sup>132</sup>, N. Kemmerich<sup>103</sup>, J. Kemp<sup>134</sup>, R. M. Kieckhafer<sup>165</sup>, H. O. Klages<sup>132</sup>, M. Kleifges<sup>164</sup>, J. Kleinfeller<sup>116</sup>, R. Krause<sup>134</sup>, N. Krohm<sup>122</sup>, D. Kuempel<sup>122</sup>, G. Kukec Mezek<sup>167</sup>, N. Kunka<sup>164</sup>, A. Kuotb Awad<sup>135</sup>, B. L. Lago<sup>177</sup>
D. LaHurd<sup>149</sup>, R. G. Lang<sup>157</sup>, M. Lauscher<sup>134</sup>, R. Legumina<sup>172</sup>, M. A. Leigui de Oliveira<sup>178</sup>, A. Letessier-Selvon<sup>169</sup>, I. Lhenry-Yvon<sup>126</sup>, K. Link<sup>135</sup>, D. Lo Presti<sup>138,139</sup>, L. Lopes<sup>100</sup>, R. López<sup>179</sup>, A. López Casado<sup>109</sup>, R. Lorek<sup>149</sup>, Q. Luce<sup>126</sup>, A. Lucero<sup>106</sup>, M. Malacari<sup>150</sup>, M. Mallamaci<sup>141,147</sup>, D. Mandat<sup>127</sup>, P. Mantsch<sup>161</sup>, A. G. Mariazzi<sup>159</sup>, I. C. Mariş<sup>180</sup>, G. Marsella<sup>128,129</sup>, D. Martello<sup>128,129</sup>, H. Martinez<sup>181</sup>, O. Martínez Bravo<sup>179</sup>, J. J. Masías Meza<sup>153</sup>, H. J. Mathes<sup>132</sup>, S. Mathys<sup>122</sup>, J. Matthews<sup>182</sup>, G. Matthiae<sup>183,184</sup>, E. Mayotte<sup>122</sup>, P. O. Mazur<sup>161</sup>, C. Medina<sup>176</sup>, G. Medina-Tanco<sup>108</sup>, D. Melo<sup>106</sup>, A. 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Parra<sup>179</sup>, T. Paul<sup>112</sup>, M. Pech<sup>127</sup>, F. Pedreira<sup>109</sup>, J. Pekala<sup>131</sup>, R. Pelayo<sup>188</sup>, J. Peña-Rodriguez<sup>115</sup>, L. A. S. Pereira<sup>144</sup>, M. Perlin<sup>106</sup>, L. Perrone<sup>128,129</sup>, C. Peters<sup>134</sup>, S. Petrera<sup>110,111</sup>, J. Phuntsok<sup>146</sup>, T. Pierog<sup>132</sup>, M. Pimenta<sup>100</sup>, V. Pirronello<sup>138,139</sup>, M. Platino<sup>106</sup>, M. Plum<sup>134</sup>, J. Poh<sup>150</sup>, C. Porowski<sup>131</sup>, R. R. Prado<sup>157</sup>, P. Privitera<sup>150</sup>, M. Prouza<sup>127</sup>, E. J. Quel<sup>187</sup>, S. Querchfeld<sup>122</sup>, S. Quinn<sup>149</sup>, R. Ramos-Pollan<sup>115</sup>, J. Rautenberg<sup>122</sup>, D. Ravignani<sup>106</sup>, J. Ridky<sup>127</sup>, F. Riehn<sup>100</sup>, M. Risse<sup>136</sup>, P. Ristori<sup>187</sup>, V. Rizi<sup>111,189</sup>, W. Rodrigues de Carvalho<sup>103</sup>, G. Rodriguez Fernandez<sup>183,184</sup>, J. Rodriguez Rojo<sup>116</sup>, M. J. Roncoroni<sup>106</sup>, M. Roth<sup>132</sup>, E. Roulet<sup>105</sup>, A. C. Rovero<sup>152</sup>, P. Ruehl<sup>136</sup>, S. J. Safli<sup>104</sup>, A. Saftoiu<sup>119</sup>, F. Salamida<sup>111,189</sup>, H. Salazar<sup>179</sup>, A. Saleh<sup>167</sup>, G. Salina<sup>184</sup>, F. Sánchez<sup>106</sup>, P. Sanchez-Lucas<sup>137</sup>, E. M. Santos<sup>103</sup>, E. Santos<sup>127</sup>, F. Sarazin<sup>176</sup>, R. Sarmento<sup>100</sup>, C. Sarmiento-Cano<sup>106</sup>, R. Sato<sup>116</sup>, M. Schauer<sup>122</sup>, V. Scherini<sup>129</sup>, H. Schieler<sup>132</sup>, M. Schimp<sup>122</sup>, D. Schmidt<sup>106,132</sup>, O. Scholten<sup>190,191</sup>, P. Schovánek<sup>127</sup>, F. G. Schröder<sup>132</sup>, S. Schröder<sup>122</sup>, A. Schulz<sup>135</sup>, J. Schumacher<sup>134</sup>, S. J. Sciutto<sup>159</sup>, A. Segreto<sup>139,192</sup>, A. Shadkam<sup>182</sup>, R. C. Shellard<sup>171</sup>, G. Sigl<sup>160</sup>, G. Silli<sup>106,132</sup>, R. Šmída<sup>132</sup>, G. R. Snow<sup>193</sup>, P. Sommers<sup>146</sup>, S. Sonntag<sup>136</sup>, J. F. Soriano<sup>112</sup>, R. Squartini<sup>116</sup>, D. Stanca<sup>119</sup>, S. Stanič<sup>167</sup>, J. Stasielak<sup>131</sup>, P. Stassi<sup>123</sup>, M. Stolpovskiy<sup>123</sup>, F. Strafella<sup>128,129</sup>, A. Streich<sup>135</sup>, F. Suarez<sup>106,107</sup>, M. Suarez Durán<sup>115</sup>, T. Sudholz<sup>104</sup>, T. Suomijärvi<sup>126</sup>, A. D. Supanitsky<sup>152</sup>, J. Šupík<sup>175</sup>, J. Swain<sup>194</sup>, Z. Szadkowski<sup>173</sup>, A. Taboada<sup>132</sup>, O. A. Taborda<sup>105</sup>, C. Timmermans<sup>99,155</sup>, C. J. Todero Peixoto<sup>142</sup>, L. Tomankova<sup>132</sup>, B. Tomé<sup>100</sup>, G. Torralba Elipe<sup>109</sup>, P. Travnicek<sup>127</sup>, M. Trini<sup>167</sup>, M. Tueros<sup>159</sup>, R. Ulrich<sup>132</sup>, M. Unger<sup>132</sup>, M. Urban<sup>134</sup>, J. F. Valdés Galicia<sup>108</sup>, I. Valiño<sup>109</sup>, L. Valore<sup>113,120</sup>, G. van Aar<sup>99</sup>, P. van Bodegom<sup>104</sup>, A. M. van den Berg<sup>190</sup>, A. van Vliet<sup>99</sup>, E. Varela<sup>179</sup>, B. Vargas Cárdenas<sup>108</sup>, R. A. Vázquez<sup>109</sup>, D. Veberič<sup>132</sup>, C. Ventura<sup>156</sup>, I. D. Vergara Quispe<sup>159</sup>, V. Verzi<sup>184</sup>, J. Vicha<sup>127</sup>, L. Villaseñor<sup>143</sup>, S. Vorobiov<sup>167</sup>, H. Wahlberg<sup>159</sup>, O. Wainberg<sup>106,107</sup>, D. Walz<sup>134</sup>, A. A. Watson<sup>195</sup>, M. Weber<sup>164</sup>, A. Weindl<sup>132</sup>, M. Wiedeński<sup>173</sup>, L. Wiencke<sup>176</sup>, H. Wilczyński<sup>131</sup>, M. Wirtz<sup>134</sup>, D. Wittkowski<sup>122</sup>, B. Wundheiler<sup>106</sup>, L. Yang<sup>167</sup>, A. Yushkov<sup>127</sup>, E. Zas<sup>109</sup>, D. Zavrtanik<sup>166,167</sup>, M. Zavrtanik<sup>166,167</sup>, A. Zepeda<sup>181</sup>, B. Zimmermann<sup>164</sup>, M. Ziolkowski<sup>136</sup>, Z. Zong<sup>126</sup>, F. Zuccarello<sup>138,139</sup>, (The Pierre Auger Collaboration) B. P. Abbott<sup>196</sup>, R. Abbott<sup>196</sup>, T. D. Abbott<sup>197</sup>, F. Acernese<sup>198,199</sup>, K. Ackley<sup>200,201</sup>, C. Adams<sup>202</sup>, T. Adams<sup>203</sup>, P. Addesso<sup>204</sup>, R. X. Adhikari<sup>196</sup>, V. B. Adya<sup>205</sup>, C. Affeldt<sup>205</sup>, M. Afrough<sup>206</sup>, B. Agarwal<sup>207</sup>, M. Agathos<sup>208</sup>, K. Agatsuma<sup>209</sup>, N. Aggarwal<sup>210</sup>, O. D. Aguiar<sup>211</sup>, L. Aiello<sup>212,213</sup>, A. Ain<sup>214</sup>, P. Ajith<sup>215</sup>, B. Allen<sup>205,216,217</sup>, G. Allen<sup>207</sup>, A. Allocca<sup>218,219</sup>, P. A. Altin<sup>220</sup>, A. Amato<sup>221</sup>, A. Ananyeva<sup>196</sup>, S. B. Anderson<sup>196</sup>, W. G. Anderson<sup>216</sup>, S. V. Angelova<sup>222</sup>, S. Antier<sup>223</sup>, S. Appert<sup>196</sup>, K. Arai<sup>196</sup>, M. C. Araya<sup>196</sup>, J. S. Areeda<sup>224</sup>, N. Arnaud<sup>223,225</sup>, K. G. Arun<sup>226</sup>, S. Ascenzi<sup>227,228</sup>, G. Ashton<sup>205</sup>, M. Ast<sup>229</sup>, S. M. Aston<sup>202</sup>, P. Astone<sup>230</sup>, D. V. Atallah<sup>231</sup>, P. Aufmuth<sup>217</sup>, C. Aulbert<sup>205</sup>, K. Ault<sup>202</sup>, C. Austin<sup>197</sup>, A. Avila-Alvarez<sup>224</sup>, S. Babak<sup>233</sup>, P. Bacon<sup>234</sup>, M. K. M. Bader<sup>209</sup>, S. Bae<sup>235</sup>, P. T. Baker<sup>236</sup>, F. Baldaccini<sup>237,238</sup>, G. Ballardin<sup>225</sup>, S. W. Ballmer<sup>239</sup>, S. Banagiri<sup>240</sup>, J. C. Barayoga<sup>196</sup>, S. E. Barclay<sup>241</sup>, B. C. Barish<sup>196</sup>, D. Barker<sup>242</sup>, K. Barkett<sup>243</sup>, F. Barone<sup>198,199</sup>, B. Barr<sup>241</sup>, L. Barsotti<sup>210</sup>, M. Barsuglia<sup>234</sup>, D. Barta<sup>244</sup>, J. Bartlett<sup>242</sup>, I. Bartos<sup>200,245</sup>, R. Bassiri<sup>246</sup>, A. Basti<sup>218,219</sup>, J. C. Batch<sup>242</sup>, M. Bawaj<sup>238,247</sup>, J. C. Bayley<sup>241</sup>, M. Bazzan<sup>248,249</sup>, B. Bécsy<sup>250</sup>, C. Beer<sup>205</sup>, M. Bejger<sup>251</sup>, I. Belahcene<sup>223</sup>, A. S. Bell<sup>241</sup>, B. K. Berger<sup>196</sup>, G. Bergmann<sup>205</sup>, J. J. Bero<sup>252</sup>, C. P. L. Berry<sup>253</sup>, D. Bersanetti<sup>254</sup>, A. Bertolini<sup>209</sup>, J. Betzwieser<sup>202</sup>, S. Bhagwat<sup>239</sup>, R. Bhandare<sup>255</sup>, I. A. Bilenko<sup>256</sup>, G. Billingsley<sup>196</sup>, C. R. Billman<sup>200</sup>, J. Birch<sup>202</sup>, R. Birney<sup>257</sup>, O. Birnholtz<sup>205</sup>, S. Biscans<sup>196,210</sup>, S. Biscoveanu<sup>201,258</sup>, A. Bisht<sup>217</sup>, M. Bitossi<sup>219,225</sup>, C. Biwer<sup>239</sup>, M. A. Bizouard<sup>223</sup>, J. K. Blackburn<sup>196</sup>, J. Blackman<sup>243</sup>, C. D. Blair<sup>196,259</sup>, D. G. Blair<sup>259</sup>, R. M. Blair<sup>242</sup>, S. Bloemen<sup>260</sup>, O. Bock<sup>205</sup>, N. Bode<sup>205</sup>, M. Boer<sup>261</sup>, G. Bogaert<sup>261</sup>, A. Bohe<sup>233</sup>, F. Bondu<sup>262</sup>, E. Bonilla<sup>246</sup>, R. Bonnand<sup>203</sup>, B. A. Boom<sup>209</sup>, R. Bork<sup>196</sup>, V. Boschi<sup>219,225</sup>, S. Bose<sup>214,263</sup>, K. Bossie<sup>202</sup>, Y. Bouffanais<sup>234</sup>, A. Bozzi<sup>225</sup>, C. Bradaschia<sup>219</sup>, P. R. Brady<sup>216</sup>, M. Branchesi<sup>212,213</sup>, J. E. Brau<sup>264</sup>, T. Briant<sup>265</sup>, A. Brillet<sup>261</sup>, M. Brinkmann<sup>205</sup>, V. Brisson<sup>223</sup>, P. Brockill<sup>216</sup>, J. E. Broida<sup>266</sup>, A. F. Brooks<sup>196</sup>, D. A. Brown<sup>239</sup>, D. D. Brown<sup>267</sup>, S. Brunett<sup>196</sup>, C. C. Buchanan<sup>197</sup>, A. Buikema<sup>210</sup>, T. Bulik<sup>268</sup>, H. J. Bulten<sup>209,269</sup>, A. Buonanno<sup>233,270</sup>, D. Buskulic<sup>203</sup>, C. Buy<sup>234</sup>, R. L. Byer<sup>246</sup>, M. Cabero<sup>205</sup>, L. Cadonati<sup>271</sup>, G. Cagnoli<sup>221,272</sup>, C. Cahillane<sup>196</sup>, J. Calderón Bustillo<sup>271</sup>, T. A. Callister<sup>196</sup>, E. Calloni<sup>199,273</sup>, J. B. Camp<sup>274</sup>, M. Canepa<sup>254,275</sup>, P. Canizares<sup>260</sup>, K. C. Cannon<sup>276</sup>, H. Cao<sup>267</sup>, J. Cao<sup>277</sup>, C. D. Capano<sup>205</sup>, E. Capocasa<sup>234</sup>, F. Carbognani<sup>225</sup>, S. Caride<sup>278</sup>, M. F. Carney<sup>279</sup>, J. Casanueva Diaz<sup>223</sup>, C. Casentini<sup>227,228</sup>, S. Caudill<sup>209,216</sup>, M. Cavaglià<sup>206</sup>, F. Cavalier<sup>223</sup>, R. Cavalieri<sup>225</sup>, G. Cella<sup>219</sup>, C. B. Cepeda<sup>196</sup>, P. Cerdá-Durán<sup>280</sup>, G. Cerretani<sup>218,219</sup>, E. Cesarini<sup>228,281</sup>, S. J. Chamberlin<sup>258</sup>, M. Chan<sup>241</sup>, S. Chao<sup>282</sup>, P. Charlton<sup>283</sup>, E. Chase<sup>284</sup>, E. Chassande-Mottin<sup>234</sup>, D. Chatterjee<sup>216</sup>, B. D. Cheeseboro<sup>236</sup>, H. Y. Chen<sup>285</sup>, X. Chen<sup>259</sup>, Y. Chen<sup>243</sup>, H.-P. Cheng<sup>200</sup>, H. Chia<sup>200</sup>, A. Chincarini<sup>254</sup>, A. Chiummo<sup>225</sup>,
T. Chmiel²⁷⁹, H. S. Cho²⁸⁶, M. Cho²⁷⁰, J. H. Chow²²⁰, N. Christensen²⁶¹,²⁶⁶, Q. Chu²⁵⁹, A. J. K. Chua²⁰⁸, S. Chua²⁶⁵, A. K. W. Chung²⁸⁷, S. Chung²⁵⁹, G. Ciani²⁰⁰,²⁴⁸,²⁴⁹, R. Ciofi²⁸⁸,²⁸⁹, C. E. Cirelli²⁴⁶, A. Cirone²⁵⁴,²⁷⁵, F. Clara²⁴², J. A. Clark²⁷¹, P. Clearwater²⁹⁰, F. Cleva²⁶¹, C. Cocchieri²⁶⁰, E. Coccia²¹²,²¹³, P.-F. Cohadon²⁶⁵, D. Cohen²²³, A. Colla²³⁰,²⁹¹, C. G. Collette²⁹², L. R. Cominsky²⁹³, M. Constancio, Jr.²¹¹, L. Conti²⁴⁹, S. J. Cooper²⁵³, P. Corban²⁰², T. R. Corbitt¹⁹⁷, I. Cordero-Carrión²⁹⁴, K. R. Corley²⁴⁵, N. Cornish²⁹⁵, A. Corsi²⁷⁸, S. Cortese²²⁵, C. A. Costa²¹¹, M. W. Coughlin¹⁹⁶,²⁶⁶, S. B. Coughlin²⁸⁴, J.-P. Coulon²⁶¹, S. T. Countryman²⁴⁵, P. Couvares¹⁹⁶, P. B. Covas²⁹⁶, E. E. Cowan²⁷¹, D. M. Coward²⁵⁹, M. J. Cowart²⁰², D. C. Coyne¹⁹⁶, R. Coyne²⁷⁸, J. D. E. Creighton²¹⁶, T. D. Creighton²⁹⁷, J. Cripe¹⁹⁷, S. G. Crowder²⁹⁸, T. J. Cullen¹⁹⁷,²²⁴, A. Cumming²⁴¹, L. Cunningham²⁴¹, E. Cuoco²²⁵, T. Dal Canton²⁷⁴, G. Dálya²⁵⁰, S. L. Danilishin²⁰⁵,²¹⁷, S. D'Antonio²²⁸, K. Danzmann²⁰⁵,²¹⁷, A. Dasgupta²⁹⁹, C. F. Da Silva Costa²⁰⁰, V. Dattilo²²⁵, I. Dave²⁵⁵, M. Davier²²³, D. Davis²³⁹, E. J. Daw³⁰⁰, B. Day²⁷¹, S. De²³⁹, D. DeBra²⁴⁶, J. Degallaix²²¹, M. De Laurentis¹⁹⁹,²¹², S. Deléglise²⁶⁵, W. Del Pozzo²¹⁸,²¹⁹,²⁵³, N. Demos²¹⁰, T. Denker²⁰⁵, T. Dent²⁰⁵, R. De Pietri³⁰¹,³⁰², V. Dergachev²³³, R. De Rosa¹⁹⁹,²⁷³, R. T. DeRosa²⁰², C. De Rossi²²¹,²²⁵, R. DeSalvo³⁰³, O. de Varona²⁰⁵, J. Devenson²²², S. Dhurandhar²¹⁴, M. C. Díaz²⁹⁷, L. Di Fiore¹⁹⁹, M. Di Giovanni²⁸⁹,³⁰⁴, T. Di Girolamo¹⁹⁹,²⁴⁵,²⁷³, A. Di Lieto²¹⁸,²¹⁹, S. Di Pace²³⁰,²⁹¹, I. Di Palma²³⁰,²⁹¹, F. Di Renzo²¹⁸,²¹⁹, Z. Doctor²⁸⁵, V. Dolique²²¹, F. Donovan²¹⁰, K. L. Dooley²⁰⁶, S. Doravari²⁰⁵, I. Dorrington²³¹, R. Douglas²⁴¹, M. Dovale Álvarez²⁵³, T. P. Downes²¹⁶, M. Drago²⁰⁵, C. Dreissigacker²⁰⁵, J. C. Driggers²⁴², Z. Du²⁷⁷, M. Ducrot²⁰³, P. Dupej²⁴¹, S. E. Dwyer²⁴², T. B. Edo³⁰⁰, M. C. Edwards²⁶⁶, A. Effler²⁰², H.-B. Eggenstein²⁰⁵,²³³, P. Ehrens¹⁹⁶, J. Eichholz¹⁹⁶, S. S. Eikenberry²⁰⁰, R. A. Eisenstein²¹⁰, R. C. Essick²¹⁰, D. Estevez²⁰³, Z. B. Etienne²³⁶, T. Etzel¹⁹⁶, M. Evans²¹⁰, T. M. Evans²⁰², M. Factourovich²⁴⁵, V. Fafone²¹²,²²⁷,²²⁸, H. Fair²³⁹, S. Fairhurst²³¹, X. Fan²⁷⁷, S. Farinon²⁵⁴, B. Farr²⁸⁵, W. M. Farr²⁵³, E. J. Fauchon-Jones²³¹, M. Favata³⁰⁵, M. Fays²³¹, C. Fee²⁷⁹, H. Fehrmann²⁰⁵, J. Feicht¹⁹⁶, M. M. Fejer²⁴⁶, A. Fernandez-Galiana²¹⁰, I. Ferrante²¹⁸,²¹⁹, E. C. Ferreira²¹¹, F. Ferrini²²⁵, F. Fidecaro²¹⁸,²¹⁹, D. Finstad²³⁹, I. Fiori²²⁵, D. Fiorucci²³⁴, M. Fishbach²⁸⁵, R. P. Fisher²³⁹, M. Fitz-Axen²⁴⁰, R. Flaminio²²¹,²³⁰, M. Fletcher²⁴¹, H. Fong³⁰⁷, J. A. Font²⁸⁰,³⁰⁸, P. W. F. Forsyth²²⁰, S. S. Forsyth²⁷¹, J.-D. Fournier²⁶¹, S. Frasca²³⁰,²⁹¹, F. Frasconi²¹⁹, Z. Frei²⁵⁰, A. Freise²⁵³, R. Frey²⁶⁴, V. Frey²²³, E. M. Fries¹⁹⁶, P. Fritschel²¹⁰, V. V. Frolov²⁰², P. Fulda²⁰⁰, M. Fyffe²⁰², H. Gabbard²⁴¹, B. U. Gadre²¹⁴, S. M. Gaebel²⁵³, J. R. Gair³⁰⁹, L. Gammaitoni²³⁷, M. R. Ganija²⁶⁷, S. G. Gaonkar²¹⁴, C. Garcia-Quiros²⁹⁶, F. Garufi¹⁹⁹,²⁷³, B. Gateley²⁴², S. Gaudio²³², G. Gaur³¹⁰, V. Gayathri³¹¹, N. Gehrels²⁷⁴,³⁵⁸, G. Gemme²⁵⁴, E. Genin²²⁵, A. Gennai²¹⁹, D. George²⁰⁷, J. George²⁵⁵, L. Gergely³¹², V. Germain²⁰³, S. Ghonge²⁷¹, Abhirup Ghosh²¹⁵, Archisman Ghosh²⁰⁹,²¹⁵, S. Ghosh²⁰⁹,²¹⁶,²⁶⁰, J. A. Giaime¹⁹⁷,²⁰², K. D. Giardina²⁰², A. Giazotto²¹⁹, K. Gill²³², L. Glover³⁰³, E. Goetz³¹³, R. Goetz²⁰⁰, S. Gomes²³¹, B. Goncharov²⁰¹, G. González¹⁹⁷, J. M. Gonzalez Castro²¹⁸,²¹⁹, A. Gopakumar³¹⁴, M. L. Gorodetsky²⁵⁶, S. E. Gossan¹⁹⁶, M. Gosselin²²⁵, R. Gouaty²⁰³, A. Grado¹⁹⁹,³¹⁵, C. Graef²⁴¹, M. Granata²²¹, A. Grant²⁴¹, S. Gras²¹⁰, C. Gray²⁴², G. Greco³¹⁶,³¹⁷, A. C. Green²⁵³, E. M. Gretarsson²³², P. Groot²⁶⁰, H. Grote²⁵⁰, S. Grunewald²³³, P. Gruning²²³, G. M. Guidi³¹⁶,³¹⁷, X. Guo²⁷⁷, A. Gupta²⁵⁸, M. K. Gupta²⁹⁹, K. E. Gushwa¹⁹⁶, E. K. Gustafson¹⁹⁶, R. Gustafson³¹³, O. Halim²¹²,²¹³, B. R. Hall²⁶³, E. D. Hall²¹⁰, E. Z. Hamilton²³¹, G. Hammond²⁴¹, M. Haney³¹⁸, M. M. Hanke²⁵⁰, J. Hanks²⁴², C. Hanna²⁵⁸, M. D. Hannam²³¹, O. A. Hannuksela²⁸⁷, J. Hanson²⁰², T. Hardwick¹⁹⁷, J. Harms²¹²,²¹³, G. M. Harry³¹⁹, I. W. Harry²³³, M. J. Hart²⁴¹, C.-J. Haster³⁰⁷, K. Haughian²⁴¹, J. Healy²⁵², A. Heidmann²⁶⁵, M. C. Heintze²⁰², H. Heitmann²⁶¹, P. Hello²²³, G. Hemming²²⁵, M. Hendry²⁴¹, I. S. Heng²⁴¹, J. Hennig²⁴¹, A. W. Heptonstall¹⁹⁶, M. Heurs²⁵⁰,²¹⁷, S. Hild²⁴¹, T. Hinderer²⁶⁰, D. Hoak²²⁵, D. Hofman²²¹, K. Holt²⁰², D. E. Holz²⁸⁵, P. Hopkins²³¹, C. Horst²¹⁶, J. Hough²⁴¹, E. A. Houston²⁴¹, E. J. Howell²⁵⁹, A. Hreibi²⁶¹, Y. M. Hu²⁵⁰, E. A. Huerta²⁰⁷, D. Huet²²³, B. Hughey²³², S. Husa²⁹⁶, S. H. Huttner²⁴¹, T. Huynh-Dinh²⁰², N. Indik²⁰⁵, R. Inta²⁷⁸, G. Intini²³⁰,²⁹¹, H. N. Isa²⁴¹, J.-M. Isac²⁶⁵, M. Isi¹⁹⁶, B. R. Iyer²¹⁵, K. Izumi²⁴², T. Jacqmin²⁶⁵, K. Jani²⁷¹, P. Jaranowski³²⁰, S. Jawahar²⁵⁷, F. Jiménez-Forteza²⁹⁶, W. W. Johnson¹⁹⁷, D. I. Jones³²¹, R. Jones²⁴¹, R. J. G. Jonker²⁰⁹, L. Ju²⁵⁹, J. Junker²⁰⁵, C. V. Kalaghatgi²³¹, V. Kalogera²⁸⁴, B. Kamai¹⁹⁶, S. Kandhasamy²⁰², G. Kang²³⁵, J. B. Kanner¹⁹⁶, S. J. Kapadia²¹⁶, S. Karki²⁶⁴, K. S. Karvinen²⁰⁵, M. Kasprzack¹⁹⁷, M. Katolik²⁰⁷, E. Katsavounidis²¹⁰, W. Katzman²⁰², S. Kaufer²¹⁷, K. Kawabe²⁴², F. Kéfélian²⁶¹, D. Keitel²⁴¹, A. J. Kemball²⁰⁷, R. Kennedy³⁰⁰, C. Kent²³¹, J. S. Key³²², F. Y. Khalili²⁵⁶, I. Khan²¹²,²²⁸, S. Khan²⁰⁵, Z. Khan²⁹⁹, E. A. Khazanov³²³, N. Kijbunchoo²²⁰, Chunglee Kim³²⁴, J. C. Kim³²⁵, K. Kim²⁸⁷, W. Kim²⁶⁷, W. S. Kim³²⁶, Y.-M. Kim²⁸⁶, S. J. Kimbrell²⁷¹, E. J. King²⁶⁷, P. J. King²⁴², M. Kinley-Hanlon³¹⁹, R. Kirchhoff²⁰⁵, J. S. Kissel²⁴², L. Kleybolte²²⁹, S. Klimenko²⁰⁰, T. D. Knowles²³⁶, P. Koch²⁰⁵, S. M. Koehlenbeck²⁰⁵, S. Koley²⁰⁹, V. Kondrashov¹⁹⁶, A. Kontos²¹⁰, M. Korobko²²⁹, W. Z. Korth¹⁹⁶, I. Kowalska²⁶⁸, D. B. Kozak¹⁹⁶, C. Krämer²⁰⁵, V. Kringel²⁰⁵, B. Krishnan²⁰⁵, A. Królak³²⁷,³²⁸, G. Kuehn²⁰⁵, P. Kumar³⁰⁷, R. Kumar²⁹⁹, S. Kumar²¹⁵, L. Kuo²⁸², A. Kutynia³²⁷, S. Kwang²¹⁶, B. D. Lackey²³³, K. H. Lai²⁸⁷, M. Landry²⁴², R. N. Lang³²⁹, J. Lange²⁵², B. Lantz²⁴⁶, R. K. Lanza²¹⁰, A. Lartaux-Vollard²²³, P. D. Lasky²⁰¹, M. Laxen²⁰², A. Lazzarini¹⁹⁶, C. Lazzaro²⁴⁹, P. Leaci²³⁰,²⁹¹, S. Leavey²⁴¹, C. H. Lee²⁸⁶, H. K. Lee³³⁰, H. M. Lee³³¹, H. W. Lee³²⁵, K. Lee²⁴¹, J. Lehmann²⁵⁰, A. Lenon²³⁶, M. Leonardi²⁸⁹,³⁰⁴, N. Leroy²²³, N. Letendre²⁰³, Y. Levin²⁰¹, T. G. F. Li²⁸⁷, S. D. Linker³⁰³, T. B. Littenberg³³², J. Liu²⁵⁹, R. K. L. Lo²⁸⁷, N. A. Lockerbie²⁵⁷, L. T. London²³¹, J. E. Lord²³⁹, M. Lorenzini²¹²,²¹³, V. Loriette³³³, M. Lormand²⁰², G. Losurdo²¹⁹, J. D. Lough²⁰⁵, C. O. Lousto²⁵², G. Lovelace²²⁴, H. Lück²⁰⁵,²¹⁷, D. Lumaca²²⁷,²²⁸, A. P. Lundgren²⁰⁵, R. Lynch²¹⁰, Y. Ma²⁴³, R. Macas²³¹, S. Macfoy²²², B. Machenschalk²⁰⁵, M. MacInnis²¹⁰, D. M. Macleod²³¹, I. Magaña Hernandez²¹⁶, F. Magaña-Sandoval²³⁹, L. Magaña Zertuche²³⁹, R. M. Magee²⁵⁸, E. Majorana²³⁰, I. Maksimovic³³³, N. Man²⁶¹, V. Mandic²⁴⁰, V. Mangano²⁴¹, G. L. Mansell²²⁰, M. Manske²¹⁶,²²⁰, M. Mantovani²²⁵, F. Marchesoni²³⁸,²⁴⁷, F. Marion²⁰³, S. Márka²⁴⁵,
Z. Márka²⁴⁵, C. Markakis²⁰⁷, A. S. Markosyan²⁴⁶, A. Markowitz¹⁹⁶, E. Maros¹⁹⁶, A. Marquina²⁹⁴, F. Martelli³¹⁶,³¹⁷, L. Martellini²⁶¹, I. W. Martin²⁴¹, R. M. Martin³⁰⁵, D. V. Martynov²¹⁰, K. Mason²¹⁰, E. Massera³⁰⁰, A. Masserot²⁰³, T. J. Massinger¹⁹⁶, M. Masso-Reid²⁴¹, S. Mastrogiovanni²³⁰,²⁹¹, A. Matas²⁴⁰, F. Matichard¹⁹⁶,²¹⁰, L. Matone²⁴⁵, N. Mavalvala²¹⁰, N. Mazumder²⁶³, R. McCarthy²⁴², D. E. McClelland²²⁰, S. McCormick²⁰², L. McCuller²¹⁰, S. C. McGuire³³⁴, G. McIntyre¹⁹⁶, J. McIver¹⁹⁶, D. J. McManus²²⁰, L. McNeill²⁰¹, T. McRae²²⁰, S. T. McWilliams²³⁶, D. Meacher²⁵⁸, G. D. Meadors²⁰⁵,²³³, M. Mehmet²⁰⁵, J. Meidam²⁰⁹, E. Mejuto-Villa²⁰⁴, A. Melatos²⁹⁰, G. Mendell²⁴², R. A. Mercer²¹⁶, E. L. Merilh²⁴², M. Merzouguï²⁶¹, S. Meshkov¹⁹⁶, C. Messenger²⁴¹, C. Messick²⁵⁸, R. Metzdorff²⁶⁵, P. M. Meyers²⁴⁰, H. Miao²⁵³, C. Michel²²¹, H. Middleton²⁵³, E. E. Mikhailov³³⁵, L. Milano¹⁹⁹,²⁷³, A. L. Miller²⁰⁰,²³⁰,²⁹¹, B. B. Miller²⁸⁴, J. Miller²¹⁰, M. Millhouse²⁹⁵, M. C. Milovich-Goff³⁰³, O. Minazzoli²⁶¹,³³⁶, Y. Minenkov²²⁸, J. Ming²³³, C. Mishra³³⁷, S. Mitra²¹⁴, V. P. Mitrofanov²⁵⁶, G. Mitselmakher²⁰⁰, R. Mittleman²¹⁰, D. Moffa²⁷⁹, A. Moggi²¹⁹, K. Mogushi²⁰⁶, M. Mohan²²⁵, S. R. P. Mohapatra²¹⁰, M. Montani³¹⁶,³¹⁷, C. J. Moore²⁰⁸, D. Moraru²⁴², G. Moreno²⁴², S. R. Morriss²⁹⁷, B. Mours²⁰³, C. M. Mow-Lowry²⁵³, G. Mueller²⁰⁰, A. W. Muir²³¹, Arunava Mukherjee²⁰⁵, D. Mukherjee²¹⁶, S. Mukherjee²⁹⁷, N. Mukund²¹⁴, A. Mullavey²⁰², J. Munch²⁶⁷, E. A. Muñiz²³⁹, M. Muratore²³², P. G. Murray²⁴¹, K. Napier²⁷¹, I. Nardecchia²²⁷,²²⁸, L. Naticchioni²³⁰,²⁹¹, R. K. Nayak³³⁸, J. Neilson³⁰³, G. Nelemans²⁰⁹,²⁶⁰, T. J. N. Nelson²⁰², M. Nery²⁰⁵, A. Neunzert³¹³, L. Nevin¹⁹⁶, J. M. Newport³¹⁹, G. Newton²⁴¹,³⁵⁹, K. K. Y. Ng²⁸⁷, T. T. Nguyen²²⁰, D. Nichols²⁶⁰, A. B. Nielsen²⁰⁵, S. Nissanke²⁰⁹,²⁶⁰, A. Nitz²⁰⁵, A. Noack²⁰⁵, F. Nocera²²⁵, D. Nolting²⁰², C. North²³¹, L. K. Nuttall²³¹, J. Oberling²⁴², G. D. O'Dea³⁰³, G. H. Ogin³³⁹, J. J. Oh³²⁶, S. H. Oh³²⁶, F. Ohme²⁰⁵, M. A. Okada²¹¹, M. Oliver²⁹⁶, P. Oppermann²⁰⁵, Richard J. Oram²⁰², B. O'Reilly²⁰², R. Ormiston²⁴⁰, L. F. Ortega²⁰⁰, R. O'Shaughnessy²⁵², S. Ossokine²³³, D. J. Ottaway²⁶⁷, H. Overmier²⁰², B. J. Owen²⁷⁸, A. E. Pace²⁵⁸, J. Page³³², M. A. Page²⁵⁹, A. Pai³¹¹,³⁴⁰, S. A. Pai²⁵⁵, J. R. Palamos²⁶⁴, O. Palashov³²³, C. Palomba²³⁰, A. Pal-Singh²²⁹, Howard Pan²⁸², Huang-Wei Pan²⁸², B. Pang²⁴³, P. T. H. Pang²⁸⁷, C. Pankow²⁸⁴, F. Pannarale²³¹, B. C. Pant²⁵⁵, F. Paoletti²¹⁹, A. Paoli²²⁵, M. A. Papa²⁰⁵,²¹⁶,²³³, A. Parida²¹⁴, W. Parker²⁰², D. Pascucci²⁴¹, A. Pasqualetti²²⁵, R. Passaquietti²¹⁸,²¹⁹, D. Passuello²¹⁹, M. Patil³²⁸, B. Patricelli²¹⁹,³⁴¹, B. L. Pearlstone²⁴¹, M. Pedraza¹⁹⁶, R. Pedurand²²¹,³⁴², L. Pekowsky²³⁹, A. Pele²⁰², S. Penn³⁴³, C. J. Perez²⁴², A. Perreca¹⁹⁶,²⁸⁹,³⁰⁴, L. M. Perri²⁸⁴, H. P. Pfeiffer²³³,³⁰⁷, M. Phelps²⁴¹, O. J. Piccinni²³⁰,²⁹¹, M. Pichot²⁶¹, F. Piergiovanni³¹⁶,³¹⁷, V. Pierro²⁰⁴, G. Pillant²²⁵, L. Pinard²²¹, I. M. Pinto²⁰⁴, M. Pirello²⁴², M. Pitkin²⁴¹, M. Poe²¹⁶, R. Poggiani²¹⁸,²¹⁹, P. Popolizio²²⁵, E. K. Porter²³⁴, A. Post²⁰⁵, J. Powell²⁴¹,³⁴⁴, J. Prasad²¹⁴, J. W. W. Pratt²³², G. Pratten²⁹⁶, V. Predoi²³¹, T. Prestegard²¹⁶, M. Prijatelj²⁰⁵, M. Principe²⁰⁴, S. Privitera²³³, G. A. Prodi²⁸⁹,³⁰⁴, L. G. Prokhorov²⁵⁶, O. Puncken²⁰⁵, M. Punturo²³⁸, P. Puppo²³⁰, M. Pürrer²³³, H. Qi²¹⁶, V. Quetschke²⁹⁷, E. A. Quintero¹⁹⁶, R. Quitzow-James²⁶⁴, F. J. Raab²⁴², D. S. Rabeling²²⁰, H. Radkins²⁴², P. Raffai²⁵⁰, S. Raja²⁵⁵, C. Rajan²⁵⁵, B. Rajbhandari²⁷⁸, M. Rakhmanov²⁹⁷, K. E. Ramirez²⁹⁷, A. Ramos-Buades²⁹⁶, P. Rapagnani²³⁰,²⁹¹, V. Raymond²³³, M. Razzano²¹⁸,²¹⁹, J. Read²²⁴, T. Regimbau²⁶¹, L. Rei²⁵⁴, S. Reid²⁵⁷, D. H. Reitze¹⁹⁶,²⁰⁰, W. Ren²⁰⁷, S. D. Reyes²³⁹, F. Ricci²³⁰,²⁹¹, P. M. Ricker²⁰⁷, S. Rieger²⁰⁵, K. Riles³¹³, M. Rizzo²²⁵, N. A. Robertson¹⁹⁶,²⁴¹, R. Robie²⁴¹, F. Robinet²²³, A. Rocchi²²⁸, L. Rolland²⁰³, J. G. Rollins¹⁹⁶, V. J. Roma²⁶⁴, R. Romano¹⁹⁸,¹⁹⁹, C. L. Romel²⁴², J. H. Romie²⁰², D. Rosińska²⁵¹,³⁴⁵, M. P. Ross³⁴⁶, S. Rowan²⁴¹, A. Rüdiger²⁰⁵, P. Ruggi²²⁵, G. Rutins²²², K. Ryan²⁴², S. Sachdev¹⁹⁶, T. Sadecki²⁴², L. Sadeghian²¹⁶, M. Sakellariadou³⁴⁷, L. Salconi²²⁵, M. Saleem³¹¹, F. Salemi²⁰⁵, A. Samajdar³³⁸, L. Sammut²⁰¹, L. M. Sampson²⁸⁴, E. J. Sanchez¹⁹⁶, L. E. Sanchez¹⁹⁶, N. Sanchis-Gual²⁸⁰, V. Sandberg²⁴², J. R. Sanders²³⁹, B. Sassolas²²¹, P. R. Saulson²³⁹, O. Sauter³¹³, R. L. Savage²⁴², A. Sawadsky²²⁹, P. Schale²⁶⁴, M. Scheel²⁴³, J. Scheuer²⁸⁴, J. Schmidt²⁰⁵, P. Schmidt¹⁹⁶,²⁶⁰, R. Schnabel²²⁹, R. M. S. Schofield²⁶⁴, A. Schönbeck²²⁹, E. Schreiber²⁰⁵, D. Schuette²⁰⁵,²¹⁷, B. W. Schulte²⁰⁵, B. F. Schutz²⁰⁵,²³¹, S. G. Schwalbe²³², J. Scott²⁴¹, S. M. Scott²²⁰, E. Seidel²⁰⁷, D. Sellers²⁰², A. Sengupta³⁴⁸, D. Sentenac²²⁵, V. Sequino²¹²,²²⁷,²²⁸, A. Sergeev³²³, D. A. Shaddock²²⁰, T. J. Shaffer²⁴², A. A. Shah³³², M. S. Shahriar²⁸⁴, M. B. Shaner³⁰³, L. Shao²³³, B. Shapiro²⁴⁶, P. Shawhan²⁷⁰, A. Sheperd²¹⁶, D. H. Shoemaker²¹⁰, D. M. Shoemaker²⁷¹, K. Siellez²⁷¹, X. Siemens²¹⁶, M. Sieniawska²⁵¹, D. Sigg²⁴², A. D. Silva²¹¹, L. P. Singer²⁷⁴, A. Singh²⁰⁵,²¹⁷,²³³, A. Singhal²¹²,²³⁰, A. M. Sintes²⁹⁶, B. J. J. Slagmolen²²⁰, B. Smith²⁰², J. R. Smith²²⁴, R. J. E. Smith¹⁹⁶,²⁰¹, S. Somala³⁴⁹, E. J. Son³²⁶, J. A. Sonnenberg²¹⁶, B. Sorazu²⁴¹, F. Sorrentino²⁵⁴, T. Souradeep²¹⁴, A. P. Spencer²⁴¹, A. K. Srivastava²⁹⁹, K. Staats²³², A. Staley²⁴⁵, M. Steinke²⁰⁵, J. Steinlechner²²⁹,²⁴¹, S. Steinlechner²²⁹, D. Steinmeyer²⁰⁵, S. P. Stevenson²⁵³,³⁴⁴, R. Stone²⁹⁷, D. J. Stops²⁵³, K. A. Strain²⁴¹, G. Stratta³¹⁶,³¹⁷, S. E. Strigin²⁵⁶, A. Strunk²⁴², R. Sturani³⁵⁰, A. L. Stuver²⁰², T. Z. Summerscales³⁵¹, L. Sun²⁹⁰, S. Sunil²⁹⁹, J. Suresh²¹⁴, P. J. Sutton²³¹, B. L. Swinkels²²⁵, M. J. Szczepańczyk²³², M. Tacca²⁰⁹, S. C. Tait²⁴¹, C. Talbot²⁰¹, D. Talukder²⁶⁴, D. B. Tanner²⁰⁰, M. Tápai³¹², A. Taracchini²³³, J. D. Tasson²⁶⁶, J. A. Taylor³³², R. Taylor¹⁹⁶, S. V. Tewari³⁴³, T. Theeg²⁰⁵, F. Thies²⁰⁵, E. G. Thomas²⁵³, M. Thomas²⁰², P. Thomas²⁴², K. A. Thorne²⁰², E. Thrane²⁰¹, S. Tiwari²¹²,²⁸⁹, V. Tiwari²³¹, K. V. Tokmakov²⁵⁷, K. Toland²⁴¹, M. Tonelli²¹⁸,²¹⁹, Z. Tornasi²⁴¹, A. Torres-Forné²⁸⁰, C. I. Torrie¹⁹⁶, D. Töyrä²⁵³, F. Travasso²²⁵,²³⁸, G. Traylor²⁰², J. Trinastic²⁰⁰, M. C. Tringali²⁸⁹,³⁰⁴, L. Trozzo²¹⁹,³⁵², K. W. Tsang²⁰⁹, M. Tse²¹⁰, R. Tso¹⁹⁶, L. Tsukada²⁷⁶, D. Tsuna²⁷⁶, D. Tuyenbayev²⁹⁷, K. Ueno²¹⁶, D. Ugolini³⁵³, C. S. Unnikrishnan³¹⁴, A. L. Urban¹⁹⁶, S. A. Usman²³¹, H. Vahlbruch²¹⁷, G. Vajente¹⁹⁶, G. Valdes¹⁹⁷, N. van Bakel²⁰⁹, M. van Beuzekom²⁰⁹, J. F. J. van den Brand²⁰⁹,²⁶⁹, C. Van Den Broeck²⁰⁹,³⁵⁴, D. C. Vander-Hyde²³⁹, L. van der Schaaf²⁰⁹, J. V. van Heijningen²⁰⁹, A. A. van Veggel²⁴¹, M. Vardaro²⁴⁸,²⁴⁹, V. Varma²⁴³, S. Vass¹⁹⁶, M. Vasúth²⁴⁴, A. Vecchio²⁵³, G. Vedovato²⁴⁹, J. Veitch²⁴¹, P. J. Veitch²⁶⁷, K. Venkateswara³⁴⁶, G. Venugopalan¹⁹⁶, D. Verkindt²⁰³, F. Vetrano³¹⁶,³¹⁷, A. Vicere³¹⁶,³¹⁷, A. D. Viets²¹⁶, S. Vinciguerra²⁵³, D. J. Vine²²², J.-Y. Vinet²⁶¹, S. Vitale²¹⁰, T. Vo²³⁹, H. Vocca²³⁷,²³⁸, C. Vorvick²⁴², S. P. Vyatchanin²⁵⁶, A. R. Wade¹⁹⁶,
L. E. Wade²⁷⁹, M. Wade²⁷⁹, R. Walet²⁰⁹, M. Walker²²⁴, L. Wallace¹⁹⁶, S. Walsh²⁰⁵,²¹⁶,²³³, G. Wang²¹²,³¹⁷, H. Wang²⁵³, J. Z. Wang²⁵⁸, W. H. Wang²⁹⁷, Y. F. Wang²⁸⁷, R. L. Ward²²⁰, J. Warner²⁴², M. Was²⁰³, J. Watchi²⁹², B. Weaver²⁴², L.-W. Wei²⁰⁵,²¹⁷, M. Weinert²⁰⁵, A. J. Weinstein¹⁹⁶, R. Weiss²¹⁰, L. Wen²⁵⁹, E. K. Wessel²⁰⁷, P. Weßels²⁰⁵, J. Westerweck²⁰⁵, T. Westphal²⁰⁵, K. Wette²²⁰, J. T. Whelan²⁵², B. F. Whiting²⁰⁰, C. Whittle²⁰¹, D. Wilken²⁰⁵, D. Williams²⁴¹, R. D. Williams¹⁹⁶, A. R. Williamson²⁶⁰, J. L. Willis¹⁹⁶,³⁵⁵, B. Willke²⁰⁵,²¹⁷, M. H. Wimmer²⁰⁵, W. Winkler²⁰⁵, C. C. Wipf¹⁹⁶, H. Wittel²⁰⁵,²¹⁷, G. Woan²⁴¹, J. Woehler²⁰⁵, J. Wofford²⁵², K. W. K. Wong²⁸⁷, J. Worden²⁴², J. L. Wright²⁴¹, D. S. Wu²⁰⁵, D. M. Wysocki²⁵², S. Xiao¹⁹⁶, H. Yamamoto¹⁹⁶, C. C. Yancey²⁷⁰, L. Yang³⁵⁶, M. J. Yap²²⁰, M. Yazback²⁰⁰, Hang Yu²¹⁰, Haocun Yu²¹⁰, M. Yvert²⁰³, A. Zadrożny³²⁷, M. Zanolin²³², T. Zelenova²²⁵, J.-P. Zendri²⁴⁹, M. Zevin²⁸⁴, L. Zhang¹⁹⁶, M. Zhang³³⁵, T. Zhang²⁴¹, Y.-H. Zhang²⁵², C. Zhao²⁵⁹, M. Zhou²⁸⁴, Z. Zhou²⁸⁴, S. J. Zhu²⁰⁵,²³³, X. J. Zhu²⁰¹, M. E. Zucker¹⁹⁶,²¹⁰, J. Zweizig¹⁹⁶, and (LIGO Scientific Collaboration and Virgo Collaboration)

¹ GRPHE—Université de Haute Alsace—Institut universitaire de technologie de Colmar, 34 rue du Grillenbreit BP F-50568-68008 Colmar, France

² Technical University of Catalonia, Laboratory of Applied Bioacoustics, Rambla Exposició, E-08800 Vilanova i la Geltrú, Barcelona, Spain

³ INFN—Sezione di Genova, Via Dodecaneso 33, I-16146 Genova, Italy

⁴ Institut d'Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC)—Universitat Politècnica de València. C/Paranimf 1, E-46730 Gandia, Spain

⁵ Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France

⁶ APC, Univ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, Sorbonne Paris Cité, France

⁷ IFIC—Instituto de Física Corpuscular (CSIC—Universitat de València) c/ Catedrático José Beltrán, 2 E-46980 Paterna, Valencia, Spain

⁸ LAM—Laboratoire d'Astrophysique de Marseille, Pôle de l'Étoile Site de Château-Gombert, rue Frédéric Joliot-Curie 38, F-13388 Marseille Cedex 13, France

⁹ National Center for Energy Sciences and Nuclear Techniques, B.P.1382, R.P.10001 Rabat, Morocco

¹⁰ INFN—Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, I-95123 Catania, Italy

¹¹ Nikhef, Science Park, Amsterdam, The Netherlands

¹² Huygens-Kamerlingh Onnes Laboratorium, Universiteit Leiden, The Netherlands

¹³ Institute of Space Science, RO-077125 Bucharest, Măgurele, Romania

¹⁴ Universiteit van Amsterdam, Instituut voor Hoge-Energie Fysica, Science Park 105, 1098 XG Amsterdam, The Netherlands

¹⁵ INFN—Sezione di Roma, P.le Aldo Moro 2, I-00185 Roma, Italy

¹⁶ Dipartimento di Fisica dell'Università La Sapienza, P.le Aldo Moro 2, I-00185 Roma, Italy

¹⁷ Gran Sasso Science Institute, Viale Francesco Crispi 7, I-00167 L'Aquila, Italy

¹⁸ University Mohammed V in Rabat, Faculty of Sciences, 4 av. Ibn Battouta, B.P. 1014, R.P. 10000 Rabat, Morocco

¹⁹ INFN—Sezione di Bologna, Viale Berti-Pichat 6/2, I-40127 Bologna, Italy

²⁰ INFN—Sezione di Bari, Via E. Orabona 4, I-70126 Bari, Italy

²¹ Department of Computer Architecture and Technology/CITIC, University of Granada, E-18071 Granada, Spain

²² Géoazur, UCA, CNRS, IRD, Observatoire de la Côte d'Azur, Sophia Antipolis, France

²³ Dipartimento di Fisica dell'Università, Via Dodecaneso 33, I-16146 Genova, Italy

²⁴ Université Paris-Sud, F-91405 Orsay Cedex, France

²⁵ Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D-91058 Erlangen, Germany

²⁶ University Mohammed I, Laboratory of Physics of Matter and Radiations, B.P.717, Oujda 6000, Morocco

²⁷ Institut für Theoretische Physik und Astrophysik, Universität Würzburg, Emil-Fischer Str. 31, D-97074 Würzburg, Germany

²⁸ Dipartimento di Fisica e Astronomia dell'Università, Viale Berti Pichat 6/2, I-40127 Bologna, Italy

²⁹ Laboratoire de Physique Corpusculaire, Clermont Université, Université Blaise Pascal, CNRS/IN2P3, BP 10448, F-63000 Clermont-Ferrand, France

³⁰ INFN—Sezione di Catania, Viale Andrea Doria 6, I-95125 Catania, Italy

³¹ 31, Aix Marseille Université CNRS ENSAM LSIS UMR 7296 13397 Marseille, France; Université de Toulon CNRS LSIS UMR 7296, F-83957 La Garde, France

³² Institut Universitaire de France, F-75005 Paris, France

³³ Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France

³⁴ Royal Netherlands Institute of Sea Research (NIOZ) and Utrecht University, Landsdip 4, 1797 SZ 't Horntje (Texel), the Netherlands

³⁵ Dr. Remeis-Sternwarte and ECAP, Friedrich-Alexander-Universität Erlangen-Nürnberg, Sternwartstr. 7, D-96049, Germany

³⁶ Moscow State University, Skobeltsyn Institute of Nuclear Physics, Leninskie gory, 119991 Moscow, Russia

³⁷ Mediterranean Institute of Oceanography (MIO), Aix-Marseille University, 13288, Marseille, Cedex 9, France; Université du Sud Toulon-Var, CNRS-INSU/IRD UM 110, F-83957, La Garde Cedex, France

³⁸ Dipartimento di Fisica ed Astronomia dell'Università, Viale Andrea Doria 6, I-95125 Catania, Italy

³⁹ Direction des Sciences de la Matière—Institut de recherche sur les lois fondamentales de l'Univers—Service de Physique des Particules, CEA Saclay, F-91191 Gif-sur-Yvette Cedex, France

⁴⁰ INFN—Sezione di Pisa, Largo B. Pontecorvo 3, I-56127 Pisa, Italy

⁴¹ Dipartimento di Fisica dell'Università, Largo B. Pontecorvo 3, I-56127 Pisa, Italy

⁴² INFN—Sezione di Napoli, Via Cintia I-80126 Napoli, Italy

⁴³ Dipartimento di Fisica dell'Università Federico II di Napoli, Via Cintia I-80126, Napoli, Italy

⁴⁴ Dipartimento di Física Teórica y del Cosmos & C.A.F.P.E., University of Granada, E-18071 Granada, Spain

⁴⁵ Dr. Remeis-Sternwarte and ECAP, Friedrich-Alexander-Universität Erlangen-Nürnberg, Sternwartstr. 7, D-96049 Bamberg, Germany

⁴⁶ Department of Physics, University of Adelaide, Adelaide, SA 5005, Australia

⁴⁷ DESY, D-15738 Zeuthen, Germany

⁴⁸ Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand

⁴⁹ Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium

⁵⁰ Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark

⁵¹ Oskar Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden

⁵² Département de physique nucléaire et corpusculaire, Université de Genève, CH-1211 Genève, Switzerland

⁵³ Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany

⁵⁴ Department of Physics, Marquette University, Milwaukee, WI, 53201, USA

⁵⁵ Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA

⁵⁶ Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

⁵⁷ III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany

⁵⁸ Physics Department, South Dakota School of Mines and Technology, Rapid City, SD 57701, USA
⁵⁹ Department of Physics, University of Alberta, Edmonton, AB T6G 2E1, Canada

⁶⁰ Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA

⁶¹ Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany

⁶² Department of Physics, University of California, Berkeley, CA 94720, USA

⁶³ Department of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA

⁶⁴ Department of Astronomy, Ohio State University, Columbus, OH 43210, USA

⁶⁵ Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany

⁶⁶ Department of Physics, University of Wuppertal, D-42119 Wuppertal, Germany

⁶⁷ Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA

⁶⁸ Department of Physics, University of Maryland, College Park, MD 20742, USA

⁶⁹ Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA

⁷⁰ Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA

⁷¹ Department of Physics, TU Dortmund University, D-44221 Dortmund, Germany

⁷² Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea

⁷³ Department of Physics and Astronomy, Uppsala University, Box 516, SE-75120 Uppsala, Sweden

⁷⁴ Department of Physics and Wisconsin IceCube Particle Astrophysics Center, University of Wisconsin–Madison, Madison, WI 53706, USA

⁷⁵ Vrije Universiteit Brussel (VUB), Dienst ELEM, B-1050 Brussels, Belgium

⁷⁶ SNOLAB, 1039 Regional Road 24, Creighton Mine 9, Lively, ON P3Y 1N2, Canada

⁷⁷ Institut für Kernphysik, Westfälische Wilhelms-Universität Münster, D-48149 Münster, Germany

⁷⁸ Physik-department, Technische Universität München, D-85748 Garching, Germany

⁷⁹ Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA

⁸⁰ Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA

⁸¹ Bartol Research Institute and Dept. of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA

⁸² Department of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium

⁸³ Institut für Physik, Humboldt-Universität zu Berlin, D-12489 Berlin, Germany

⁸⁴ Department of Physics, Southern University, Baton Rouge, LA 70813, USA

⁸⁵ Department of Astronomy, University of Wisconsin–Madison, Madison, WI 53706, USA

⁸⁶ Earthquake Research Institute, University of Tokyo, Bunkyo, Tokyo 113-0032, Japan

⁸⁷ Department of Physics and Institute for Global Prominent Research, Chiba University, Chiba 263-8522, Japan

⁸⁸ CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA

⁸⁹ Department of Physics, University of Texas at Arlington, 502 Yates Street, Science Hall Rm 108, Box 19059, Arlington, TX 76019, USA

⁹⁰ Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA

⁹¹ Université de Mons, B-7000 Mons, Belgium

⁹² Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA

⁹³ Department of Physics, Drexel University, 1341 Chestnut Street, Philadelphia, PA 19104, USA

⁹⁴ Department of Physics, University of Wisconsin, River Falls, WI 54022, USA

⁹⁵ Department of Physics, Yale University, New Haven, CT 06520, USA

⁹⁶ School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA

⁹⁷ Department of Physics and Astronomy, University of Alaska Anchorage, 3211 Providence Drive, Anchorage, AK 99508, USA

⁹⁸ Department of Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK

⁹⁹ IMAPP, Radboud University Nijmegen, Nijmegen, The Netherlands

¹⁰⁰ Laboratório de Instrumentação e Física Experimental de Partículas—LIP and Instituto Superior Técnico—IST, Universidade de Lisboa—UL, Lisboa, Portugal

¹⁰¹ Observatorio Astrofísico di Torino (INAF), Torino, Italy

¹⁰² INFN, Sezione di Torino, Torino, Italy

¹⁰³ Universidade de São Paulo, Instituto de Física, São Paulo, SP, Brazil

¹⁰⁴ University of Adelaide, Adelaide, SA, Australia

¹⁰⁵ Centro Atómico Bariloche and Instituto Balseiro (CNEA-UNCuyo-CONICET), San Carlos de Bariloche, Argentina

¹⁰⁶ Instituto de Tecnologías en Deteción y Astropartículas (CNEA, CONICET, UNSAM), Buenos Aires, Argentina

¹⁰⁷ Universidad Tecnológica Nacional, Facultad Regional Buenos Aires, Buenos Aires, Argentina

¹⁰⁸ Universidad Nacional Autónoma de México, México, D.F., México

¹⁰⁹ Universidad de Santiago de Compostela, Santiago de Compostela, Spain

¹¹⁰ Gran Sasso Science Institute (INFN), L’Aquila, Italy

¹¹¹ INFN Laboratori Nazionali del Gran Sasso, Assergi (L’Aquila), Italy

¹¹² Department of Physics and Astronomy, Lehman College, City University of New York, New York, NY, USA

¹¹³ INFN, Sezione di Napoli, Napoli, Italy

¹¹⁴ Institute of Space Science, Bucharest-Magurele, Romania

¹¹⁵ Universidad Industrial de Santander, Bucaramanga, Colombia

¹¹⁶ Observatorio Pierre Auger, Malargüe, Argentina

¹¹⁷ Observatorio Pierre Auger and Comisión Nacional de Energía Atómica, Malargüe, Argentina

¹¹⁸ University Politehnică of Bucharest, Bucharest, Romania

¹¹⁹ “Horia Hulubei” National Institute for Physics and Nuclear Engineering, Bucharest-Magurele, Romania

¹²⁰ Università di Napoli “Federico II”, Dipartimento di Fisica “Ettore Pancini,” Napoli, Italy

¹²¹ Ohio State University, Columbus, OH, USA

¹²² Bergische Universität Wuppertal, Department of Physics, Wuppertal, Germany

¹²³ Laboratoire de Physique Subatomique et de Cosmolgie (LPSC), Université Grenoble-Alpes, CNRS/IN2P3, Grenoble, France

¹²⁴ Università Torino, Dipartimento di Fisica, Torino, Italy

¹²⁵ Max-Planck-Institut für Radioastronomie, Bonn, Germany

¹²⁶ Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud, Univ. Paris/Saclay, CNRS-IN2P3, Orsay, France

¹²⁷ Institute of Physics of the Czech Academy of Sciences, Prague, Czech Republic

¹²⁸ Università del Salento, Dipartimento di Matematica e Fisica “E. De Giorgi,” Lecce, Italy

¹²⁹ INFN, Sezione di Lecce, Lecce, Italy

¹³⁰ Universidade Federal do Rio de Janeiro, Instituto de Física, Rio de Janeiro, RJ, Brazil

¹³¹ Institute of Nuclear Physics PAN, Krakow, Poland

¹³² Karlsruhe Institute of Technology, Institut für Kernphysik, Karlsruhe, Germany
¹³³ Colorado State University, Fort Collins, CO, USA

¹³⁴ RWTH Aachen University, III. Physikalisches Institut A, Aachen, Germany

¹³⁵ Karlsruhe Institute of Technology, Institut für Experimentelle Kernphysik (IEKP), Karlsruhe, Germany

¹³⁶ Universität Siegen, Fachbereich 7 Physik—Experimentelle Teilchenphysik, Siegen, Germany

¹³⁷ Universidad de Granada and C.A.F.P.E., Granada, Spain

¹³⁸ Università di Catania, Dipartimento di Fisica e Astronomia, Catania, Italy

¹³⁹ INFN, Sezione di Catania, Catania, Italy

¹⁴⁰ Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, México

¹⁴¹ Università di Milano, Dipartimento di Fisica, Milano, Italy

¹⁴² Universidade de São Paulo, Escola de Engenharia de Lorena, Lorena, SP, Brazil

¹⁴³ Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Michoacán, México

¹⁴⁴ Universidad Estadual de Campinas, IFGW, Campinas, SP, Brazil

¹⁴⁵ Instituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET, UNSAM), and Universidad Tecnológica Nacional—Facultad Regional Mendoza (CONICET/CNEA), Mendoza, Argentina

¹⁴⁶ Pennsylvania State University, University Park, PA, USA

¹⁴⁷ INFN, Sezione di Milano, Milano, Italy

¹⁴⁸ Politecnico di Milano, Dipartimento di Scienze e Tecnologie Aerospaziali, Milano, Italy

¹⁴⁹ Case Western Reserve University, Cleveland, OH, USA

¹⁵⁰ University of Chicago, Enrico Fermi Institute, Chicago, IL, USA

¹⁵¹ Università del Salento, Dipartimento di Ingegneria, Lecce, Italy

¹⁵² Instituto de Astronomía y Física del Espacio (IAFE, CONICET-UBA), Buenos Aires, Argentina

¹⁵³ Departamento de Física and Departamento de Ciencias de la Atmósfera y los Océanos, FCEyN, Universidad de Buenos Aires and CONICET, Buenos Aires, Argentina

¹⁵⁴ Universidade Federal Fluminense, EEIMVR, Volta Redonda, RJ, Brazil

¹⁵⁵ Nationaal Instituut voor Kernfysica en Hoge Energie Fysica (NIKHEF), Science Park, Amsterdam, The Netherlands

¹⁵⁶ Universidade Federal do Rio de Janeiro (UFRJ), Observatório do Valongo, Rio de Janeiro, RJ, Brazil

¹⁵⁷ Universidade de São Paulo, Instituto de Física de São Carlos, São Carlos, SP, Brazil

¹⁵⁸ Universidade Federal do Paraná, Setor Palotina, Palotina, Brazil

¹⁵⁹ IFLP, Universidad Nacional de La Plata and CONICET, La Plata, Argentina

¹⁶⁰ Università Hamburg, II. Institut für Theoretische Physik, Hamburg, Germany

¹⁶¹ Fermi National Accelerator Laboratory, USA

¹⁶² Stichting Astronomisch Onderzoek in Nederland (ASTRON), Dwingeloo, The Netherlands

¹⁶³ New York University, New York, NY, USA

¹⁶⁴ Karlsruhe Institute of Technology, Institut für Prozessdatenverarbeitung und Elektronik, Karlsruhe, Germany

¹⁶⁵ Michigan Technological University, Houghton, MI, USA

¹⁶⁶ Experimental Particle Physics Department, J. Stefan Institute, Ljubljana, Slovenia

¹⁶⁷ Center for Astrophysics and Cosmology (CAC), University of Nova Gorica, Nova Gorica, Slovenia

¹⁶⁸ Instituto de Física de Rosario (IFIR)—CONICET/U.N.R. and Facultad de Ciencias Bioquímicas y Farmacéuticas U.N.R., Rosario, Argentina

¹⁶⁹ Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), Universités Paris 6 et Paris 7, CNRS-IN2P3, Paris, France

¹⁷⁰ SUBATECH, École des Mines de Nantes, CNRS-IN2P3, Université de Nantes, France

¹⁷¹ Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, RJ, Brazil

¹⁷² University of Łódź, Faculty of Astrophysics, Łódź, Poland

¹⁷³ University of Łódź, Faculty of High-Energy Astrophysics, Łódź, Poland

¹⁷⁴ Universidade Estadual de Feira de Santana, Feira de Santana, Brazil

¹⁷⁵ Palacky University, RCPTM, Olomouc, Czech Republic

¹⁷⁶ Colorado School of Mines, Golden, CO, USA

¹⁷⁷ Centro Federal de Educação Tecnológica Celso Suckow da Fonseca, Nova Friburgo, Brazil

¹⁷⁸ Universidade Federal do ABC, Santo André, SP, Brazil

¹⁷⁹ Benemérita Universidad Autónoma de Puebla, Puebla, México

¹⁸⁰ Université Libre de Bruxelles (ULB), Brussels, Belgium

¹⁸¹ Centro de Investigación y de Estudios Avanzados del IPN (CINVESTAV), México, D.F., México

¹⁸² Louisiana State University, Baton Rouge, LA, USA

¹⁸³ Università di Roma “Tor Vergata”, Dipartimento di Fisica, Roma, Italy

¹⁸⁴ INFN, Sezione di Roma “Tor Vergata,” Roma, Italy

¹⁸⁵ Universidade Federal de Alpenas, Brasília, Brazil

¹⁸⁶ Charles University, Faculty of Mathematics and Physics, Institute of Particle and Nuclear Physics, Prague, Czech Republic

¹⁸⁷ Centro de Investigaciones en Láseres y Aplicaciones, CITEDEF and CONICET, Villa Martelli, Argentina

¹⁸⁸ Unidad Profesional Interdisciplinaria en Ingeniería y Tecnologías Avanzadas del Instituto Politécnico Nacional (UPIITA-IPN), México, D.F., México

¹⁸⁹ Università dell’Aquila, Dipartimento di Scienze Fisiche e Chimiche, L’Aquila, Italy

¹⁹⁰ KVI—Center for Advanced Radiation Technology, University of Groningen, Groningen, The Netherlands

¹⁹¹ Vrije Universiteit Brussels, Brussels, Belgium

¹⁹² INAF—Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Palermo, Italy

¹⁹³ University of Nebraska, Lincoln, NE, USA

¹⁹⁴ Northeastern University, Boston, MA, USA

¹⁹⁵ School of Physics and Astronomy, University of Leeds, Leeds, UK

¹⁹⁶ LIGO, California Institute of Technology, Pasadena, CA 91125, USA

¹⁹⁷ Louisiana State University, Baton Rouge, LA 70803, USA

¹⁹⁸ Università di Salerno, Fisciano, I-84084 Salerno, Italy

¹⁹⁹ INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy

²⁰⁰ University of Florida, Gainesville, FL 32611, USA

²⁰¹ OzGrav, School of Physics & Astronomy, Monash University, Clayton, VIC 3800, Australia

²⁰² LIGO Livingston Observatory, Livingston, LA 70754, USA

²⁰³ Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy, France

²⁰⁴ University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
205 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany

206 The University of Mississippi, University, MS 38677, USA

207 NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA

208 University of Cambridge, Cambridge CB2 1TN, UK

209 Nikhef, Science Park, 1098 XG Amsterdam, The Netherlands

210 LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

211 Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil

212 Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy

213 INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy

214 Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India

215 International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India

216 University of Wisconsin–Milwaukee, Milwaukee, WI 53201, USA

217 Leibniz Universität Hannover, D-30167 Hannover, Germany

218 Università di Pisa, I-56127 Pisa, Italy

219 INFN, Sezione di Pisa, I-56127 Pisa, Italy

220 OzGrav, Australian National University, Canberra, ACT 0200, Australia

221 Laboratoire des Matériaux Avancés (LMA), CNRS/IN2P3, F-69622 Villeurbanne, France

222 SUPA, University of the West of Scotland, Paisley PA1 2BE, UK

223 LAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, F-91898 Orsay, France

224 California State University Fullerton, Fullerton, CA 92831, USA

225 European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy

226 Chennai Mathematical Institute, Chennai 603103, India

227 Università di Roma Tor Vergata, I-00133 Roma, Italy

228 INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy

229 Universität Hamburg, D-22761 Hamburg, Germany

230 INFN, Sezione di Roma, I-00185 Roma, Italy

231 Cardiff University, Cardiff CF24 3AA, UK

232 Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA

233 Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany

234 APC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, France

235 Korea Institute of Science and Technology Information, Daejeon 34141, Korea

236 West Virginia University, Morgantown, WV 26506, USA

237 Università di Perugia, I-06123 Perugia, Italy

238 INFN, Sezione di Perugia, I-06123 Perugia, Italy

239 Syracuse University, Syracuse, NY 13244, USA

240 University of Minnesota, Minneapolis, MN 55455, USA

241 SUPA, University of Glasgow, Glasgow G12 8QQ, UK

242 LIGO Hanford Observatory, Richland, WA 99352, USA

243 Caltech CaRT, Pasadena, CA 91125, USA

244 Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29–33, Hungary

245 Columbia University, New York, NY 10027, USA

246 Stanford University, Stanford, CA 94305, USA

247 Università di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy

248 Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy

249 INFN, Sezione di Padova, I-35131 Padova, Italy

250 Institute of Physics, Eötvös University, Pázmány P. s. 1/A, Budapest 1117, Hungary

251 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland

252 Rochester Institute of Technology, Rochester, NY 14623, USA

253 University of Birmingham, Birmingham B15 2TT, UK

254 INFN, Sezione di Genova, I-16146 Genova, Italy

255 RRCAT, Indore MP 452013, India

256 Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia

257 SUPA, University of Strathclyde, Glasgow G1 1XQ, UK

258 The Pennsylvania State University, University Park, PA 16802, USA

259 OzGrav, University of Western Australia, Crawley, WA 6009, Australia

260 Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands

261 Artemis, Université Côte d'Azur, Observatoire Côte d'Azur, CNRS, CS 34229, F-06304 Nice Cedex 1, France

262 Institut FOTON, CNRS, Université de Rennes 1, F-35042 Rennes, France

263 Washington State University, Pullman, WA 99164, USA

264 University of Oregon, Eugene, OR 97403, USA

265 Laboratoire Kastler Brossel, UPMC-Sorbonne Universités, CNRS, ENS-PSL Research University, Collège de France, F-75005 Paris, France

266 Carleton College, Northfield, MN 55057, USA

267 OzGrav, University of Adelaide, Adelaide, SA 5005, Australia

268 Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland

269 VU University Amsterdam, 1081 HV Amsterdam, The Netherlands

270 University of Maryland, College Park, MD 20742, USA

271 Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA 30332, USA

272 Université Claude Bernard Lyon 1, F-69622 Villeurbanne, France

273 Università di Napoli “Federico II,” Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy

274 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

275 Dipartimento di Fisica, Università degli Studi di Genova, I-16146 Genova, Italy

276 RESCEU, University of Tokyo, Tokyo, 113-0033, Japan

277 Tsinghua University, Beijing 100084, China
278 Texas Tech University, Lubbock, TX 79409, USA

279 Kenyon College, Gambier, OH 43022, USA

280 Departamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, Spain

281 Museo Storico della Fisica e Centro Studi e Ricerche Enrico Fermi, I-00184 Roma, Italy

282 National Tsing Hua University, Hsinchu City, 30013 Taiwan, Republic of China

283 Charles Sturt University, Wagga Wagga, NSW 2678, Australia

284 Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60208, USA

285 University of Chicago, Chicago, IL 60637, USA

286 Pusan National University, Busan 46241, Korea

287 The Chinese University of Hong Kong, Shatin, NT, Hong Kong

288 INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy

289 INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy

290 OzGrav, University of Melbourne, Parkville, VIC 3010, Australia

291 Università di Roma “La Sapienza,” I-00185 Roma, Italy

292 Université Libre de Bruxelles, Brussels 1050, Belgium

293 Sonoma State University, Rohnert Park, CA 94928, USA

294 Departamento de Matemáticas, Universitat de València, E-46100 Burjassot, València, Spain

295 Montana State University, Bozeman, MT 59717, USA

296 Universitat de les Illes Balears, IAC3—IEEC, E-07122 Palma de Mallorca, Spain

297 The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA

298 Bellevue College, Bellevue, WA 98007, USA

299 Institute for Plasma Research, Bhat, Gandhinagar 382428, India

300 The University of Sheffield, Sheffield S10 2TN, UK

301 Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Università di Parma, I-43124 Parma, Italy

302 INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy

303 California State University, Los Angeles, 5151 State University Drive, Los Angeles, CA 90032, USA

304 Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy

305 Montclair State University, Montclair, NJ 07043, USA

306 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

307 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada

308 Observatori Astronòmiche, Universitat de València, E-46980 Paterna, València, Spain

309 School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, UK

310 University and Institute of Advanced Research, Koba Institutional Area, Gandhinagar Gujarat 382007, India

311 IISER-TVM, CET Campus, Trivandrum Kerala 695016, India

312 University of Szeged, Döm tér 9, Szeged 6720, Hungary

313 University of Michigan, Ann Arbor, MI 48109, USA

314 Tata Institute of Fundamental Research, Mumbai 400005, India

315 INAF, Osservatorio Astronomico di Capodimonte, I-80131, Napoli, Italy

316 Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy

317 INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy

318 Physik-Institut, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland

319 American University, Washington, DC 20016, USA

320 University of Białystok, 15-424 Białystok, Poland

321 University of Southampton, Southampton SO17 1BJ, UK

322 University of Washington Bothell, 18115 Campus Way NE, Bothell, WA 98011, USA

323 Institute of Applied Physics, Nizhny Novgorod, 603950, Russia

324 Korea Astronomy and Space Science Institute, Daejeon 34055, Korea

325 Inje University Gimhae, South Gyeongsang 50834, Korea

326 National Institute for Mathematical Sciences, Daejeon 34047, Korea

327 NCBJ, 05-400 Świerk-Otwock, Poland

328 Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland

329 Hillsdale College, Hillsdale, MI 49242, USA

330 Hanyang University, Seoul 04763, Korea

331 Seoul National University, Seoul 08826, Korea

332 NASA Marshall Space Flight Center, Huntsville, AL 35811, USA

333 ESPCI, CNRS, F-75005 Paris, France

334 Southern University and A&M College, Baton Rouge, LA 70813, USA

335 College of William and Mary, Williamsburg, VA 23187, USA

336 Centre Scientifique de Monaco, 8 quai Antoine Ier, MC-98000, Monaco

337 Indian Institute of Technology Madras, Chennai 600036, India

338 IISER-Kolkata, Mohanpur, West Bengal 741252, India

339 Whitman College, 345 Boyer Avenue, Walla Walla, WA 99362 USA

340 Indian Institute of Technology Bombay, Powai, Mumbai, Maharashtra 400076, India

341 Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, Italy

342 Université de Lyon, F-69361 Lyon, France

343 Hobart and William Smith Colleges, Geneva, NY 14456, USA

344 OzGrav, Swinburne University of Technology, Hawthorn, VIC 3122, Australia

345 Janusz Gil Institute of Astronomy, University of Zielona Góra, 65-265 Zielona Góra, Poland

346 University of Washington, Seattle, WA 98195, USA

347 King's College London, University of London, London WC2R 2LS, UK

348 Indian Institute of Technology, Gandhinagar Ahmedabad Gujarat 382424, India

349 Indian Institute of Technology Hyderabad, Sangareddy, Khandi, Telangana 502285, India

350 International Institute of Physics, Universidade Federal do Rio Grande do Norte, Natal RN 59078-970, Brazil

351 Andrews University, Berrien Springs, MI 49104, USA
352 Università di Siena, I-53100 Siena, Italy

353 Trinity University, San Antonio, TX 78212, USA

354 Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Nijenborgh 4, 9747 AG Groningen, The Netherlands

355 Abilene Christian University, Abilene, TX 79699, USA

356 Colorado State University, Fort Collins, CO 80523, USA

357 Deceased, 2016 August.

358 Deceased, 2017 February.

359 Deceased, 2016 December.