This is the accepted manuscript made available via CHORUS. The article has been
published as:

High-energy neutrino follow-up search of gravitational
wave event GW150914 with ANTARES and IceCube

S. Adrián-Martínez et al. (Antares Collaboration, IceCube Collaboration, LIGO Scientific
Collaboration, and Virgo Collaboration)

Phys. Rev. D 93, 122010 — Published 23 June 2016
DOI: 10.1103/PhysRevD.93.122010

http://dx.doi.org/10.1103/PhysRevD.93.122010


High-energy Neutrino follow-up search of Gravitational Wave Event
GW150914 with ANTARES and IceCube

ANTARES Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, and Virgo Collaboration∗

We present the high-energy-neutrino follow-up observations of the first gravitational wave tran-
sient GW150914 observed by the Advanced LIGO detectors on Sept. 14th, 2015. We search for
coincident neutrino candidates within the data recorded by the IceCube and Antares neutrino de-
tectors. A possible joint detection could be used in targeted electromagnetic follow-up observations,
given the significantly better angular resolution of neutrino events compared to gravitational waves.
We find no neutrino candidates in both temporal and spatial coincidence with the gravitational wave
event. Within ±500 s of the gravitational wave event, the number of neutrino candidates detected
by IceCube and Antares were three and zero, respectively. This is consistent with the expected
atmospheric background, and none of the neutrino candidates were directionally coincident with
GW150914. We use this non-detection to constrain neutrino emission from the gravitational-wave
event.

I. INTRODUCTION

Advanced LIGO’s first observation periods [1, 2] rep-
resent a major step in probing the dynamical origin of
high-energy emission from cosmic transients [3]. The sig-
nificant improvement in gravitational wave (GW) search
sensitivity enables a comprehensive multimessenger ob-
servational effort involving partner electromagnetic ob-
servatories from radio to gamma-rays, as well as neutrino
detectors. The goals of multimessenger observations are
to gain a more complete understanding of cosmic pro-
cesses through a combination of information from dif-
ferent probes, and to increase search sensitivity over an
analysis using a single messenger [4–6].

The merger of neutron stars and black holes, and po-
tentially massive stellar core collapse with rapidly rotat-
ing cores, are expected to be significant sources of GWs
[3]. These events can result in a black hole plus accre-
tion disk system that drives a relativistic outflow [7, 8].
Energy dissipation in the outflow produces non-thermal,
high-energy radiation that is observed as gamma-ray
bursts (GRBs), and may have a �GeV neutrino com-
ponent at comparable luminosities.

Multiple detectors have been built that can search for
this high-energy neutrino signature, including the Ice-
Cube Neutrino Observatory—a cubic-kilometer facility
at the South Pole [9–11], and Antares [12–14] in the
Mediterranean sea. The construction of the KM3NeT
cubic-kilometer scale neutrino detector in the Mediter-
ranean Sea has started in December 2015 with the suc-
cessful deployment of the first detection string [15]. Ice-
Cube is planning a substantial increase in sensitivity with
near-future upgrades [16, 17]. Another facility, the Baikal
Neutrino Telescope is also planning an upgrade to cubic-
kilometer volume [18]. An astrophysical high-energy neu-
trino flux has recently been discovered by IceCube [19–
22], demonstrating the production of non-thermal high-
energy neutrinos. The specific origin of this neutrino

∗ Full author list given at the end of the article.

flux is currently unknown. Multimessenger analyses con-
straining the common sources of high-energy neutrinos
and GWs have been carried out in the past with both
Antares and IceCube [23–25].

On Sept. 14th, 2015 at 09:50:45 UTC, a highly signifi-
cant GW signal was recorded by the LIGO Hanford, WA
and Livingston, LA detectors [26]. The event, labeled
GW150914, was produced by a stellar-mass binary black
hole merger at redshift z = 0.09+0.03

−0.04. The reconstructed
mass of each black hole is ∼ 30 M�. Such a system may
produce electromagnetic emission and emit neutrinos if
the merger happens in a sufficiently baryon-dense envi-
ronment, and a black hole plus accretion disk system is
formed [27]. Current consensus is that such a scenario
is unlikely, nevertheless, there are no significant observa-
tional constraints.

Here we report the results of a neutrino follow-up
search of GW150914 using Antares and IceCube. Af-
ter brief descriptions of the GW search (Section II) and
the neutrino follow-up (Section III), we present the joint
analysis, results of the search and source constraints, and
conclusions (Section IV).

II. GRAVITATIONAL WAVE DATA ANALYSIS
AND DISCOVERY

GW150914 was initially identified by low-latency
searches for generic GW transients [28–30]. Subsequent
analysis with three independent matched-filter analyses
using models of compact binary coalescence waveforms
[31, 32] confirmed that the event was produced by the
merger of two black holes. The analyses established a
false alarm rate of less than 1 event per 203 000 years,
equivalent to a significance > 5.1σ [26]. Source parame-
ters were reconstructed using the LALInference package
[32–34], finding black-hole masses 36+5

−4 M� and 29+4
−4 M�

and luminosity distance Dgw = 410+160
−180 Mpc, where the

error ranges correspond to the range of the 90% credi-
ble interval. The duration of the signal within LIGO’s
sensitive band was 0.2 s.



2

The directional point spread function (sky map) of the
GW event was computed through the full parameter es-
timation of the signal, carried out using the LALInfer-
ence package [33, 34]. The LALInference results pre-
sented here account for calibration uncertainty in the
GW strain signal. The sky map is shown in Fig. 1.
At 90% (50%) credible level (CL), the sky map covers
590 deg2 (140 deg2).

III. HIGH-ENERGY NEUTRINO
COINCIDENCE SEARCH

High-energy neutrino observatories are primarily sen-
sitive to neutrinos with �GeV energies. IceCube and
Antares are both sensitive to through-going muons
(called track events), produced by neutrinos near the
detector, above ∼ 100 GeV. In this analysis, Antares
data include only up-going tracks for events originat-
ing from the Southern hemisphere, while IceCube data
include both up-going tracks (from the Northern hemi-
sphere) as well as down-going tracks (from the Southern
hemisphere). The energy threshold of neutrino candi-
dates increases in the Southern hemisphere for IceCube,
since downward-going atmospheric muons are not filtered
by the Earth, greatly increasing the background at lower
energies. Neutrino times of arrival are determined at µs
precision.

Since neutrino telescopes continuously take data ob-
serving the whole sky, it is possible to look back and
search for neutrino counterparts to an interesting GW
signal at any time around the GW observation.

To search for neutrinos coincident with GW150914, we
used a time window of ±500 s around the GW transient.
This search window, which was used in previous GW-
neutrino searches, is a conservative, observation-based
upper limit on the plausible emission of GWs and high-
energy neutrinos in the case of GRBs, which are thought
to be driven by a stellar-mass black hole—accretion disk
system [35]. While the relative time of arrival of GWs
and neutrinos can be informative [36–38], here we do
not use detailed temporal information beyond the ±500 s
time window.

The search for high-energy neutrino candidates
recorded by IceCube within ±500 s of GW150914 used
IceCube’s online event stream. The online event stream
implements an event selection similar to the event selec-
tion used for neutrino point source searches [39], but opti-
mized for real-time performance at the South Pole. This
event selection consists primarily of cosmic-ray-induced
background events, with an expectation per 1000 seconds
of 2.2 events in the Northern sky (atmospheric neutri-
nos), and 2.2 events in the Southern sky (high-energy
atmospheric muons). In the search window of ±500 s
centered on the GW alert time (see below), one event
was found in the Southern sky and two in the Northern
sky, which is consistent with the background expectation.
The properties of these events are listed in Table I. The

# ∆T [s] RA [h] Dec [◦] σrec
µ [◦] Erec

µ [TeV] fraction
1 +37.2 8.84 −16.6 0.35 175 12.5%
2 +163.2 11.13 12.0 1.95 1.22 26.5%
3 +311.4 −7.23 8.4 0.47 0.33 98.4%

TABLE I. Parameters of neutrino candidates identified by Ice-
Cube within the ±500 s time window around GW150914. ∆T
is the time of arrival of the neutrino candidates relative to that
of GW150914. Erec

µ is the reconstructed muon energy. σrec
µ

is the angular uncertainty of the reconstructed track direc-
tion [43]. The last column shows the fraction of background
neutrino candidates with higher reconstructed energy at the
same declination (±5◦).

neutrino candidates’ directions are shown in Fig. 1.

The muon energy in Table I is reconstructed assum-
ing a single muon is producing the event. While the
event from the Southern hemisphere has a significantly
greater reconstructed energy [40] than the other two
events, 12.5% of the background events in the same dec-
lination range in the Southern hemisphere have energies
in excess of the one observed. The intense flux of at-
mospheric muons and bundles of muons that constitute
the background for IceCube in the Southern hemisphere
gradually falls as the cosmic ray flux declines with en-
ergy [41]. The use of energy cuts to remove most of this
background is the reason that IceCube’s sensitivity in the
Southern sky is shifted to higher energies.

An additional search was performed using the high-
energy starting event selection described in [19]. No
events were found in coincidence with GW150914.

The IceCube detector also has sensitivity to outbursts
of MeV neutrinos (as occur for example in core-collapse
supernovae) via a sudden increase in the photomultiplier
rates [42]. The global photomultiplier noise rate is mon-
itored continuously, and deviations sufficient to trigger
the lowest-level of alert occur roughly once per hour. No
alert was triggered during the ±500 second time-window
around the GW candidate event.

The search for coincident neutrinos for Antares
within ±500 s of GW150914 used Antares’s online re-
construction pipeline [44]. A fast and robust algorithm
[45] selected up-going neutrino candidates with ∼mHz
rate, with atmospheric muon contamination less than
10%. In addition, to reduce the background of at-
mospheric neutrinos [46], a requirement of a minimum
reconstructed energy reduced the online event rate to
1.2 events/day. Consequently, for Antares the expected
number of neutrino candidates from the Southern sky in
a 1000 s window in the Southern sky is 0.014. We found
no neutrino events from Antares that were temporally
coincident with GW150914. This is consistent with the
expected background event rate.



3

FIG. 1. GW skymap in equatorial coordinates, showing
the reconstructed probability density contours of the GW
event at 50%, 90% and 99% CL, and the reconstructed di-
rections of high-energy neutrino candidates detected by Ice-
Cube (crosses) during a ±500 s time window around the GW
event. The neutrino directional uncertainties are < 1◦ and are
not shown. GW shading indicates the reconstructed probabil-
ity density of the GW event, darker regions corresponding to
higher probability. Neutrino numbers refer to the first column
of Table I.

IV. RESULTS

A. Joint analysis

We carried out the joint GW and neutrino search fol-
lowing the analysis developed for previous GW and neu-
trino datasets using initial GW detectors [23, 25, 35, 47].
After identifying the GW event GW150914 with the cWB
pipeline, we used reconstructed neutrino candidates to
search for temporal and directional coincidences between
GW150914 and neutrinos. We assumed that the a priori
source directional distribution is uniform. For temporal
coincidence, we searched within a ±500 s time window
around GW150914.

The relative difference in propagation time for �GeV
neutrinos and GWs (which travel at the speed of light
in general relativity) traveling to Earth from the source
is expected to be � 1 s. The relative propagation time
between neutrinos and GWs may change in alternative
gravity models [48, 49]. However, discrepancies from gen-
eral relativity could in principle be probed with a joint
GW-neutrino detection by comparing the arrival times
against the expected time frame of emission.

Directionally, we searched for overlap between the GW
sky map and the neutrino point spread functions, as-
sumed to be Gaussian with standard deviation σrec

µ (see
Table I).

The search identified no Antares neutrino candidates
that were temporally coincident with GW150914.

For IceCube, none of the three neutrino candidates
temporally coincident with GW150914 were compatible
with the GW direction at 90% CL. Additionally, the re-
constructed energy of the neutrino candidates with re-
spect to the expected background does not make them
significant. See Fig. 1 for the directional relation of

GW150914 and the IceCube neutrino candidates de-
tected within the ±500 s window. This non-detection is
consistent with our expectation from a binary black hole
merger.

To better understand the probability that the de-
tected neutrino candidates are consistent with back-
ground, we briefly consider different aspects of the data
separately. First, the number of detected neutrino can-
didates, i.e. 3 and 0 for IceCube and Antares, re-
spectively, is fully consistent with the expected back-
ground rate of 4.4 and � 1 for the two detectors, with
p-value 1 − Fpois(Nobserved ≤ 2, Nexpected = 4.4) = 0.81,
where Fpois is the Poisson cumulative distribution func-
tion. Second, for the most significant reconstructed muon
energy (Table I), 12.5% of background events will have
greater muon energy. The probability that at least one
neutrino candidate, out of 3 detected events, has an en-
ergy high enough to make it appear even less background-
like, is 1− (1− 0.125)3 ≈ 0.33. Third, with the GW sky
area 90% CL of Ωgw = 590 deg2, the probability of a
background neutrino candidate being directionally coin-
cident is Ωgw/Ωall ≈ 0.014. We expect 3Ωgw/Ωall di-
rectionally coincident neutrinos, given 3 temporal coinci-
dences. Therefore, the probability that at least one of the
3 neutrino candidates is directionally coincident with the
90% CL skymap of GW150914 is 1− (1−0.014)3 ≈ 0.04.

B. Constraints on the source

We used the non-detection of coincident neutrino can-
didates by Antares and IceCube to derive a stan-
dard frequentist neutrino spectral fluence upper limit for
GW150914 at 90% CL. Considering no spatially and tem-
porally coincident neutrino candidates, we calculated the
source fluence that on average would produce 2.3 de-
tected neutrino candidates. We carried out this analysis
as a function of source direction, and independently for
Antares and IceCube.

The obtained spectral fluence upper limits as a func-
tion of source direction are shown in Fig. 2. We con-
sidered a standard dN/dE ∝ E−2 source model, as
well as a model with a spectral cutoff at high energies:
dN/dE ∝ E−2 exp[−

√
(E/100TeV)]. The latter model

is expected for sources with exponential cutoff in the pri-
mary proton spectrum [50]. This is expected for some
galactic sources, and is also adopted here for compari-
son to previous analyses [51]. For each spectral model,
the upper limit shown in each direction of the sky is the
more stringent limit provided by one or the other de-
tector. We see in Fig. 2 that the constraint strongly
depends on the source direction, and is mostly within
E2dN/dE ∼ 10−1 − 10 GeV cm−2. Furthermore, the up-
per limits by Antares and IceCube constrain different
energy ranges in the region of the sky close to the GW
candidate. For an E−2 power-law source spectrum, 90%
of Antares signal neutrinos are in the energy range from
3 TeV to 1 PeV, whereas for IceCube at this southern



4

FIG. 2. Upper limit on the high-energy neutrino spectral
fluence (νµ + νµ) from GW150914 as a function of source
direction, assuming dN/dE ∝ E−2 (top) and dN/dE ∝
E−2 exp[−

√
(E/100TeV)] (bottom) neutrino spectra. The re-

gion surrounded by a white line shows the part of the sky in
which Antares is more sensitive (close to nadir), while on
the rest of the sky, IceCube is more sensitive. For compari-
son, the 50% CL and 90% CL contours of the GW sky map
are also shown.

declination the corresponding energy range is 200 TeV to
100 PeV.

To characterize the dependence of neutrino spectral
fluence limits on source direction, we calculate these lim-
its separately for the two distinct areas in the 90% cred-
ible region of the GW skymap. For the larger region
farther South (hereafter South region), we find upper
limits E2dN/dE = 1.2+0.25

−0.36 GeV cm−2 and E2dN/dE =

7.0+3.2
−2.0 GeV cm−2 for our two spectral models without

and with a cutoff, respectively. The error bars define the
90% confidence interval of the upper limit, showing the
level of variation within each region. The average val-
ues were obtained as geometric averages, which better
represent the upper limit values as they are distributed
over a wide numerical range. For the smaller region far-
ther North (hereafter North region), we find upper lim-
its E2dN/dE = 0.10+0.12

−0.06 GeV cm−2 and E2dN/dE =

0.55+1.79
−0.44 GeV cm−2. As expected, we see that the limits

Energy range Limit [GeV cm−2]
100 GeV – 1 TeV 150

1 TeV – 10 TeV 18
10 TeV – 100 TeV 5.1

100 TeV – 1 PeV 5.5
1 PeV – 10 PeV 2.8

10 PeV – 100 PeV 6.5
100 PeV – 1 EeV 28

TABLE II. Upper limits on neutrino spectral fluence (νµ+νµ)
from GW150914, separately for different spectral ranges, at
Dec = −70◦. We assume dN/dE ∝ E−2 within each energy
band.

are much more constraining for the North region, given
the stronger limits at the Northern hemisphere due to Ice-
Cube’s greatly improved sensitivity there. Additionally,
we see that the 90% confidence intervals for the South re-
gion, which is much more likely to contain the real source
direction than the North region, are fairly small around
the average, with the lower and higher limits only differ-
ing by about a factor of 2. The upper limits within this
area can be considered essentially uniform. We observe
a much greater variation in the North region.

To provide a more detailed picture of our constraints
on neutrino emission, we additionally calculated neutrino
fluence upper limits for different energy bands. For these
limits, we assume dN/dE ∝ E−2 within each energy
band. We focus on Dec = −70◦, which is consistent
with the most likely source direction, and also with most
of the GW sky area’s credible region. For each energy
range, we use the limit from the most sensitive detector
within that range. The obtained limits are given in Table
II.

We now convert our fluence upper limits into a con-
straint on the total energy emitted in neutrinos by the
source. To obtain this constraint, we integrate emission
within [100 GeV, 100 PeV] for each source model. The
obtained constraint will vary with respect to source di-
rection as we saw above. It will also depend on the un-
certain source distance. To account for these uncertain-
ties, we provide the range of values from the lowest to the
highest possible within the 90% confidence intervals with
respect to source direction and the 90% credible interval
with respect to source distance. For simplicity, we treat
the estimated source distance and its uncertainty inde-
pendent of the source direction. We consider both of the
distinct sky regions to provide an inclusive range. For
our two spectral models, we obtain the following upper
limit on the total energy radiated in neutrinos:

Eul
ν,tot = 5.4× 1051 – 1.3× 1054 erg (1)

E
ul(cutoff)
ν,tot = 6.6× 1051 – 3.7× 1054 erg (2)

with the first and second lines of the equation correspond-
ing to the spectral models without and with cutoff, re-
spectively. For comparison, the total energy radiated in
GWs from the source is ∼ 5× 1054 erg. This value can
also be compared to high-energy emission expected in



5

some scenarios for accreting stellar-mass black holes. For
example, typical GRB isotropic-equivalent energies are
∼ 1051 erg for long and ∼ 1049 erg for short GRBs [52].
The total energy radiated in high-energy neutrinos in the
case of GRBs can be comparable [53–57] or in some cases
much greater [58, 59] than the high-energy electromag-
netic emission. There is little reason, however, to expect
an associated GRB for a binary black hole merger (see,
nevertheless, [60]).

V. CONCLUSION

The results above represent the first concrete limit on
neutrino emission from this GW source type, and the first
neutrino follow-up of a significant GW event. With the
continued increase of Advanced LIGO-Virgo sensitivities
for the next observation periods, and the implied source
rate of 2–400 Gpc−3yr−1 in the comoving frame based
on this first detection [61], we can expect to detect a
significant number of GW sources, allowing for stacked
neutrino analyses and significantly improved constraints.
Similar analyses for the upcoming observation periods
of Advanced LIGO-Virgo will be important to provide
constraints on or to detect other joint GW and neutrino
sources.

Joint GW and neutrino searches will also be used
to improve the efficiency of electromagnetic follow-up
observations over GW-only triggers. Given the signif-
icantly more accurate direction reconstruction of neu-
trinos (∼ 1 deg2 for track events in IceCube [40, 43]
and ∼ 0.2 deg2 in Antares [62]) compared to GWs
(& 100 deg2), a joint event candidate provides a greatly
reduced sky area for follow-up observatories [63]. The de-
lay induced by the event filtering and reconstruction after
the recorded trigger time is typically 3–5 s for Antares
[44], 20–30 s for IceCube [64], and O(1 min) for LIGO-
Virgo, making data available for rapid analyses.

ACKNOWLEDGMENTS

The authors acknowledge the financial support of the
funding agencies: Centre National de la Recherche Sci-
entifique (CNRS), Commissariat à l’énergie atomique
et aux énergies alternatives (CEA), Commission Eu-
ropéenne (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),

Région Île-de-France (DIM-ACAV), Région Alsace (con-
trat CPER), Région Provence-Alpes-Côte d’Azur, Dé-
partement du Var and Ville de La Seyne-sur-Mer,
France; Bundesministerium für Bildung und Forschung
(BMBF), Germany; Istituto Nazionale di Fisica Nucle-
are (INFN), Italy; Stichting voor Fundamenteel Onder-
zoek der Materie (FOM), 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 Economı́a y Competi-
tividad (MINECO), Prometeo and Grisoĺıa programs of
Generalitat Valenciana and MultiDark, Spain; Agence
de l’Oriental and CNRST, Morocco. We also acknowl-
edge the technical support of Ifremer, AIM and Foselev
Marine for the sea operation and the CC-IN2P3 for the
computing facilities.

We acknowledge 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 Re-
search Foundation, the Grid Laboratory Of Wisconsin
(GLOW) grid infrastructure at the University of Wis-
consin - Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and Na-
tional Energy Research Scientific Computing Center,
the Louisiana Optical Network Initiative (LONI) grid
computing resources; Natural Sciences and Engineer-
ing Research Council of Canada, WestGrid and Com-
pute/Calcul Canada; Swedish Research Council, Swedish
Polar Research Secretariat, Swedish National Infrastruc-
ture for Computing (SNIC), and Knut and Alice Wal-
lenberg Foundation, Sweden; German Ministry for Ed-
ucation and Research (BMBF), Deutsche Forschungsge-
meinschaft (DFG), Helmholtz Alliance for Astroparticle
Physics (HAP), Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for
Scientific Research (FNRS-FWO), FWO Odysseus pro-
gramme, Flanders Institute to encourage scientific and
technological research in industry (IWT), Belgian Fed-
eral Science Policy Office (Belspo); University of Oxford,
United Kingdom; Marsden Fund, New Zealand; Aus-
tralian Research Council; Japan Society for Promotion
of Science (JSPS); the Swiss National Science Founda-
tion (SNSF), Switzerland; National Research Foundation
of Korea (NRF); Danish National Research Foundation,
Denmark (DNRF)

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 Tech-
nology Facilities Council (STFC) of the United King-
dom, 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 sup-
ported by the Netherlands Organisation for Scientific Re-
search, for the construction and operation of the Virgo
detector and the creation and support of the EGO consor-
tium. The authors also gratefully acknowledge research



6

support from these agencies as well as by the Council of
Scientific and Industrial Research of India, Department
of Science and Technology, India, Science & Engineer-
ing Research Board (SERB), India, Ministry of Human
Resource Development, India, the Spanish Ministerio de
Economı́a y Competitividad, the Conselleria d’Economia
i Competitivitat and Conselleria d’Educació, Cultura i
Universitats of the Govern de les Illes Balears, the Na-
tional Science Centre of Poland, the European Commis-
sion, the Royal Society, the Scottish Funding Council,
the Scottish Universities Physics Alliance, the Hungar-
ian Scientific Research Fund (OTKA), the Lyon Insti-
tute of Origins (LIO), the National Research Foundation

of Korea, Industry Canada and the Province of Ontario
through the Ministry of Economic Development and In-
novation, the Natural Science and Engineering Research
Council Canada, Canadian Institute for Advanced Re-
search, the Brazilian Ministry of Science, Technology,
and Innovation, Russian Foundation for Basic Research,
the Leverhulme Trust, the Research Corporation, Min-
istry of Science and Technology (MOST), Taiwan and
the Kavli Foundation. The authors gratefully acknowl-
edge the support of the NSF, STFC, MPS, INFN, CNRS
and the State of Niedersachsen/Germany for provision
of computational resources. This article has LIGO doc-
ument number LIGO-P1500271.

[1] J. Aasi et al., CQG 32, 074001 (2015), 1411.4547.
[2] B. P. Abbott et al., (2013), arXiv:1304.0670.
[3] I. Bartos, P. Brady, and S. Márka, CQG 30, 123001

(2013), arXiv:1212.2289.
[4] M. W. E. Smith et al., Astropart. Phys. 45, 56 (2013),

arXiv:1211.5602.
[5] S. Ando et al., Rev. Mod. Phys.85, 1401 (2013),

1203.5192.
[6] X. Fan, C. Messenger, and I. S. Heng, Astrophys. J.795,

43 (2014), 1406.1544.
[7] D. Eichler, M. Livio, T. Piran, and D. N. Schramm, Na-

ture 340, 126 (1989).
[8] S. E. Woosley, Astrophys. J.405, 273 (1993).
[9] A. Achterberg et al., Astropart. Phys. 26, 155 (2006),

astro-ph/0604450.
[10] R. Abbasi et al., Nucl. Instrum. Meth. A 601, 294 (2009).
[11] R. Abbasi et al., Nucl. Instrum. Meth. A 618, 139 (2010),

arXiv:1002.2442.
[12] M. Ageron et al., Nucl. Instrum. Meth. A 656, 11 (2011),

arXiv:1104.1607.
[13] J. A. Aguilar et al., Nuclear Instruments and Methods in

Physics Research A 570, 107 (2007), astro-ph/0610029.
[14] J. A. Aguilar et al., Nuclear Instruments and Methods in

Physics Research A 555, 132 (2005), physics/0510031.
[15] S. Adrián-Mart́ınez et al., (2016), arXiv:1601.07459.
[16] M. G. Aartsen et al., (2014), arXiv:1412.5106.
[17] M. G. Aartsen et al., (2014), arXiv:1401.2046.
[18] A. Avrorin et al., Nucl. Instrum. Meth. A 626-627, S13

(2011).
[19] M. G. Aartsen et al., Phys. Rev. Lett.113, 101101 (2014),

arXiv:1405.5303.
[20] M. G. Aartsen et al., Phys. Rev. Lett.115, 081102 (2015),

arXiv:1507.04005.
[21] M. G. Aartsen et al., Phys. Rev. D91, 022001 (2015),

arXiv:1410.1749.
[22] M. G. Aartsen et al., Astrophys. J.809, 98 (2015),

arXiv:1507.03991.
[23] I. Bartos, C. Finley, A. Corsi, and S. Márka, Phys. Rev.

Lett.107, 251101 (2011), arXiv:1108.3001.
[24] S. Adrián-Mart́ınez et al., JCAP 6, 008 (2013),

arXiv:1205.3018.
[25] M. G. Aartsen et al., Phys. Rev. D90, 102002 (2014),

arXiv:1407.1042.
[26] LIGO Scientific Collaboration and Virgo Collaboration,

B. P. Abbott et al., Phys. Rev. Lett. 116, 061102 (2016).

[27] P. Mészáros, Ann. Rev. Astron. Astroph. 40, 137 (2002),
astro-ph/0111170.

[28] S. Klimenko, I. Yakushin, A. Mercer, and G. Mitsel-
makher, CQG 25, 114029 (2008), arXiv:0802.3232.

[29] S. Klimenko et al., (2015), arXiv:1511.05999.
[30] B. Abbott et al., (2016), arXiv:1602.03843.
[31] B. Abbott et al., (2016), arXiv:1602.03839.
[32] B. Abbott et al., (2016), arXiv:1602.03840.
[33] J. Aasi et al., Phys. Rev. D88, 062001 (2013),

arXiv:1304.1775.
[34] J. Veitch et al., Phys. Rev. D91, 042003 (2015),

arXiv:1409.7215.
[35] B. Baret et al., Astropart. Phys. 35, 1 (2011),

arXiv:1101.4669.
[36] S. Razzaque, P. Mészáros, and E. Waxman, Phys. Rev.

D68, 083001 (2003), astro-ph/0303505.
[37] I. Bartos, B. Dasgupta, and S. Márka, Phys. Rev. D86,

083007 (2012), 1206.0764.
[38] I. Bartos and S. Márka, Phys. Rev. D90, 101301 (2014),

1409.1217.
[39] M. G. Aartsen et al., Astrophys. J.796, 109 (2014).
[40] M. G. Aartsen et al., J. Instrum. 9, P03009 (2014),

arXiv:1311.4767.
[41] IceCube Collaboration et al., (2015), arXiv:1506.07981.
[42] R. Abbasi et al., Astron. Astrophys. 535, A109 (2011).
[43] M. G. Aartsen et al., Phys. Rev. D89, 102004 (2014).
[44] S. Adrian-Martinez et al., (2015), arXiv:1508.01180.
[45] J. A. Aguilar et al., Astropart. Phys. 34, 652 (2011),

arXiv:1105.4116.
[46] S. Adrián-Mart́ınez et al., Eur. Phys. J. C 73, 2606

(2013).
[47] B. Baret et al., Phys. Rev. D85, 103004 (2012),

arXiv:1112.1140.
[48] U. Jacob and T. Piran, Nature Physics 3, 87 (2007),

hep-ph/0607145.
[49] B. Abbott et al., (2016), arXiv:1602.03841.
[50] A. Kappes, J. Hinton, C. Stegmann, and F. A. Aha-

ronian, Journal of Physics Conference Series 60, 243
(2007).

[51] S. Adrián-Mart́ınez et al., (2015), arXiv:1511.02149.
[52] P. Mészáros, Rep. Prog. Phys. 69, 2259 (2006), astro-

ph/0605208.
[53] P. Mészáros, (2015), arXiv:1511.01396.
[54] J. N. Bahcall and P. Mészáros, Physical Review Letters

85, 1362 (2000), hep-ph/0004019.



7

[55] I. Bartos, A. M. Beloborodov, K. Hurley, and S. Márka,
Phys. Rev. Lett.110, 241101 (2013), arXiv:1301.4232.

[56] K. Murase, K. Kashiyama, and P. Mészáros, Physical
Review Letters 111, 131102 (2013), 1301.4236.

[57] K. Murase, B. Dasgupta, and T. A. Thompson, Phys.
Rev. D89, 043012 (2014), 1303.2612.

[58] P. Mészáros and E. Waxman, Physical Review Letters
87, 171102 (2001), astro-ph/0103275.

[59] K. Murase and K. Ioka, Physical Review Letters 111,
121102 (2013), 1306.2274.

[60] V. Connaughton et al., ArXiv e-prints (2016),
1602.03920.

[61] B. Abbott et al., (2016), arXiv:1602.03842.
[62] S. Adrián-Mart́ınez et al., Astrophys. J. Lett. 786, L5

(2014).
[63] S. Nissanke, M. Kasliwal, and A. Georgieva, Astrophys.

J.767, 124 (2013), arXiv:1210.6362.
[64] M. G. Aartsen et al., (2015), arXiv:1510.05222.



Authors

S. Adrián-Mart́ınez,1 A. Albert,2 M. André,3 G. Anton,4 M. Ardid,1 J.-J. Aubert,5 T. Avgitas,6 B. Baret,6

J. Barrios-Mart́ı,7 S. Basa,8 V. Bertin,5 S. Biagi,9 R. Bormuth,10, 11 M.C. Bouwhuis,10 R. Bruijn,10, 12 J. Brunner,5

J. Busto,5 A. Capone,13, 14 L. Caramete,15 J. Carr,5 S. Celli,13, 14 T. Chiarusi,16 M. Circella,17 A. Coleiro,6

R. Coniglione,9 H. Costantini,5 P. Coyle,5 A. Creusot,6 A. Deschamps,18 G. De Bonis,13, 14 C. Distefano,9

C. Donzaud,6, 19 D. Dornic,5 D. Drouhin,2 T. Eberl,4 I. El Bojaddaini,20 D. Elsässer,21 A. Enzenhöfer,4 K. Fehn,4

I. Felis,22 L.A. Fusco,23, 16 S. Galatà,6 P. Gay,24, 25 S. Geißelsöder,4 K. Geyer,4 V. Giordano,26 A. Gleixner,4

H. Glotin,27, 28 R. Gracia-Ruiz,6 K. Graf,4 S. Hallmann,4 H. van Haren,29 A.J. Heijboer,10 Y. Hello,18 J.J.

Hernández-Rey,7 J. Hößl,4 J. Hofestädt,4 C. Hugon,30, 31 G. Illuminati,13, 14 C.W James,4 M. de Jong,10, 11 M.

Jongen,10 M. Kadler,21 O. Kalekin,4 U. Katz,4 D. Kießling,4 A. Kouchner,6, 28 M. Kreter,21 I. Kreykenbohm,32

V. Kulikovskiy,9, 33 C. Lachaud,6 R. Lahmann,4 D. Lefèvre,34 E. Leonora,26, 35 S. Loucatos,36, 6 M. Marcelin,8

A. Margiotta,23, 16 A. Marinelli,37, 38 J.A. Mart́ınez-Mora,1 A. Mathieu,5 K. Melis,12 T. Michael,10 P. Migliozzi,39

A. Moussa,20 C. Mueller,21 E. Nezri,8 G.E. Păvălaş,15 C. Pellegrino,23, 16 C. Perrina,13, 14 P. Piattelli,9 V. Popa,15

T. Pradier,40 C. Racca,2 G. Riccobene,9 K. Roensch,4 M. Saldaña,1 D. F. E. Samtleben,10, 11 M. Sanguineti,30, 31

P. Sapienza,9 J. Schnabel,4 F. Schüssler,36 T. Seitz,4 C. Sieger,4 M. Spurio,23, 16 Th. Stolarczyk,36

A. Sánchez-Losa,7, 41 M. Taiuti,30, 31 A. Trovato,9 M. Tselengidou,4 D. Turpin,5 C. Tönnis,7 B. Vallage,36, 25

C. Vallée,5 V. Van Elewyck,6 D. Vivolo,39, 42 S. Wagner,4 J. Wilms,32 J.D. Zornoza,7 and J. Zúñiga7

(The Antares Collaboration)

M. G. Aartsen,44 K. Abraham,74 M. Ackermann,91 J. Adams,58 J. A. Aguilar,54 M. Ahlers,71 M. Ahrens,81

D. Altmann,4 T. Anderson,87 I. Ansseau,54 G. Anton,4 M. Archinger,72 C. Arguelles,56 T. C. Arlen,87

J. Auffenberg,43 X. Bai,79 S. W. Barwick,68 V. Baum,72 R. Bay,49 J. J. Beatty,60, 61 J. Becker Tjus,52

K.-H. Becker,90 E. Beiser,71 S. BenZvi,88 P. Berghaus,91 D. Berley,59 E. Bernardini,91 A. Bernhard,74

D. Z. Besson,69 G. Binder,50, 49 D. Bindig,90 M. Bissok,43 E. Blaufuss,59 J. Blumenthal,43 D. J. Boersma,89

C. Bohm,81 M. Börner,63 F. Bos,52 D. Bose,83 S. Böser,72 O. Botner,89 J. Braun,71 L. Brayeur,55 H.-P. Bretz,91

N. Buzinsky,65 J. Casey,47 M. Casier,55 E. Cheung,59 D. Chirkin,71 A. Christov,66 K. Clark,84 L. Classen,4

S. Coenders,74 G. H. Collin,56 J. M. Conrad,56 D. F. Cowen,87, 86 A. H. Cruz Silva,91 J. Daughhetee,47 J. C. Davis,60

M. Day,71 J. P. A. M. de André,64 C. De Clercq,55 E. del Pino Rosendo,72 H. Dembinski,75 S. De Ridder,67

P. Desiati,71 K. D. de Vries,55 G. de Wasseige,55 M. de With,51 T. DeYoung,64 J. C. Dı́az-Vélez,71 V. di Lorenzo,72

H. Dujmovic,83 J. P. Dumm,81 M. Dunkman,87 B. Eberhardt,72 T. Ehrhardt,72 B. Eichmann,52 S. Euler,89

P. A. Evenson,75 S. Fahey,71 A. R. Fazely,48 J. Feintzeig,71 J. Felde,59 K. Filimonov,49 C. Finley,81 S. Flis,81

C.-C. Fösig,72 T. Fuchs,63 T. K. Gaisser,75 R. Gaior,57 J. Gallagher,70 L. Gerhardt,50, 49 K. Ghorbani,71 D. Gier,43

L. Gladstone,71 M. Glagla,43 T. Glüsenkamp,91 A. Goldschmidt,50 G. Golup,55 J. G. Gonzalez,75 D. Góra,91

D. Grant,65 Z. Griffith,71 C. Ha,50, 49 C. Haack,43 A. Haj Ismail,67 A. Hallgren,89 F. Halzen,71 E. Hansen,62

B. Hansmann,43 T. Hansmann,43 K. Hanson,71 D. Hebecker,51 D. Heereman,54 K. Helbing,90 R. Hellauer,59

S. Hickford,90 J. Hignight,64 G. C. Hill,44 K. D. Hoffman,59 R. Hoffmann,90 K. Holzapfel,74 A. Homeier,53

K. Hoshina,71 F. Huang,87 M. Huber,74 W. Huelsnitz,59 P. O. Hulth,81 K. Hultqvist,81 S. In,83 A. Ishihara,57

E. Jacobi,91 G. S. Japaridze,46 M. Jeong,83 K. Jero,71 B. J. P. Jones,56 M. Jurkovic,74 A. Kappes,4 T. Karg,91

A. Karle,71 U. Katz,4 M. Kauer,71, 76 A. Keivani,87 J. L. Kelley,71 J. Kemp,43 A. Kheirandish,71 M. Kim,83

T. Kintscher,91 J. Kiryluk,82 S. R. Klein,50, 49 G. Kohnen,73 R. Koirala,75 H. Kolanoski,51 R. Konietz,43 L. Köpke,72

C. Kopper,65 S. Kopper,90 D. J. Koskinen,62 M. Kowalski,51, 91 K. Krings,74 G. Kroll,72 M. Kroll,52 G. Krückl,72

J. Kunnen,55 S. Kunwar,91 N. Kurahashi,78 T. Kuwabara,57 M. Labare,67 J. L. Lanfranchi,87 M. J. Larson,62

D. Lennarz,64 M. Lesiak-Bzdak,82 M. Leuermann,43 J. Leuner,43 L. Lu,57 J. Lünemann,55 J. Madsen,80

G. Maggi,55 K. B. M. Mahn,64 M. Mandelartz,52 R. Maruyama,76 K. Mase,57 H. S. Matis,50 R. Maunu,59

F. McNally,71 K. Meagher,54 M. Medici,62 M. Meier,63 A. Meli,67 T. Menne,63 G. Merino,71 T. Meures,54

S. Miarecki,50, 49 E. Middell,91 L. Mohrmann,91 T. Montaruli,66 R. Morse,71 R. Nahnhauer,91 U. Naumann,90

G. Neer,64 H. Niederhausen,82 S. C. Nowicki,65 D. R. Nygren,50 A. Obertacke Pollmann,90 A. Olivas,59

A. Omairat,90 A. O’Murchadha,54 T. Palczewski,85 H. Pandya,75 D. V. Pankova,87 L. Paul,43 J. A. Pepper,85

C. Pérez de los Heros,89 C. Pfendner,60 D. Pieloth,63 E. Pinat,54 J. Posselt,90 P. B. Price,49 G. T. Przybylski,50

M. Quinnan,87 C. Raab,54 L. Rädel,43 M. Rameez,66 K. Rawlins,45 R. Reimann,43 M. Relich,57 E. Resconi,74

W. Rhode,63 M. Richman,78 S. Richter,71 B. Riedel,65 S. Robertson,44 M. Rongen,43 C. Rott,83 T. Ruhe,63

D. Ryckbosch,67 L. Sabbatini,71 H.-G. Sander,72 A. Sandrock,63 J. Sandroos,72 S. Sarkar,62, 77 K. Schatto,72

M. Schimp,43 P. Schlunder,63 T. Schmidt,59 S. Schoenen,43 S. Schöneberg,52 A. Schönwald,91 L. Schumacher,43



9

D. Seckel,75 S. Seunarine,80 D. Soldin,90 M. Song,59 G. M. Spiczak,80 C. Spiering,91 M. Stahlberg,43

M. Stamatikos,60 T. Stanev,75 A. Stasik,91 A. Steuer,72 T. Stezelberger,50 R. G. Stokstad,50 A. Stößl,91

R. Ström,89 N. L. Strotjohann,91 G. W. Sullivan,59 M. Sutherland,60 H. Taavola,89 I. Taboada,47 J. Tatar,50, 49

S. Ter-Antonyan,48 A. Terliuk,91 G. Tešić,87 S. Tilav,75 P. A. Toale,85 M. N. Tobin,71 S. Toscano,55 D. Tosi,71

M. Tselengidou,4 A. Turcati,74 E. Unger,89 M. Usner,91 S. Vallecorsa,66 J. Vandenbroucke,71 N. van Eijndhoven,55

S. Vanheule,67 J. van Santen,91 J. Veenkamp,74 M. Vehring,43 M. Voge,53 M. Vraeghe,67 C. Walck,81 A. Wallace,44

M. Wallraff,43 N. Wandkowsky,71 Ch. Weaver,65 C. Wendt,71 S. Westerhoff,71 B. J. Whelan,44 K. Wiebe,72

C. H. Wiebusch,43 L. Wille,71 D. R. Williams,85 L. Wills,78 H. Wissing,59 M. Wolf,81 T. R. Wood,65

K. Woschnagg,49 D. L. Xu,71 X. W. Xu,48 Y. Xu,82 J. P. Yanez,91 G. Yodh,68 S. Yoshida,57 and M. Zoll81

(The IceCube Collaboration)

B. P. Abbott,92 R. Abbott,92 T. D. Abbott,93 M. R. Abernathy,92 F. Acernese,94, 95 K. Ackley,96 C. Adams,97

T. Adams,98 P. Addesso,94 R. X. Adhikari,92 V. B. Adya,99 C. Affeldt,99 M. Agathos,100 K. Agatsuma,100

N. Aggarwal,101 O. D. Aguiar,102 L. Aiello,103, 104 A. Ain,105 P. Ajith,106 B. Allen,99, 107, 108 A. Allocca,109, 110

P. A. Altin,111 S. B. Anderson,92 W. G. Anderson,107 K. Arai,92 M. C. Araya,92 C. C. Arceneaux,112

J. S. Areeda,113 N. Arnaud,114 K. G. Arun,115 S. Ascenzi,116, 104 G. Ashton,117 M. Ast,118 S. M. Aston,97

P. Astone,119 P. Aufmuth,99 C. Aulbert,99 S. Babak,120 P. Bacon,121 M. K. M. Bader,100 P. T. Baker,122

F. Baldaccini,123, 124 G. Ballardin,125 S. W. Ballmer,126 J. C. Barayoga,92 S. E. Barclay,127 B. C. Barish,92

D. Barker,128 F. Barone,94, 95 B. Barr,127 L. Barsotti,101 M. Barsuglia,121 D. Barta,129 J. Bartlett,128

I. Bartos,130 R. Bassiri,131 A. Basti,109, 110 J. C. Batch,128 C. Baune,99 V. Bavigadda,125 M. Bazzan,132, 133

B. Behnke,120 M. Bejger,134 A. S. Bell,127 C. J. Bell,127 B. K. Berger,92 J. Bergman,128 G. Bergmann,99

C. P. L. Berry,135 D. Bersanetti,136, 137 A. Bertolini,100 J. Betzwieser,97 S. Bhagwat,126 R. Bhandare,138

I. A. Bilenko,139 G. Billingsley,92 J. Birch,97 R. Birney,140 S. Biscans,101 A. Bisht,99, 108 M. Bitossi,125 C. Biwer,126

M. A. Bizouard,114 J. K. Blackburn,92 C. D. Blair,141 D. G. Blair,141 R. M. Blair,128 S. Bloemen,142 O. Bock,99

T. P. Bodiya,101 M. Boer,143 G. Bogaert,143 C. Bogan,99 A. Bohe,120 P. Bojtos,144 C. Bond,135 F. Bondu,145

R. Bonnand,98 B. A. Boom,100 R. Bork,92 V. Boschi,109, 110 S. Bose,146, 105 Y. Bouffanais,121 A. Bozzi,125

C. Bradaschia,110 P. R. Brady,107 V. B. Braginsky,139 M. Branchesi,147, 148 J. E. Brau,149 T. Briant,150

A. Brillet,143 M. Brinkmann,99 V. Brisson,114 P. Brockill,107 A. F. Brooks,92 D. D. Brown,135 N. M. Brown,101

C. C. Buchanan,93 A. Buikema,101 T. Bulik,151 H. J. Bulten,152, 100 A. Buonanno,120, 153 D. Buskulic,98

C. Buy,121 R. L. Byer,131 L. Cadonati,154 G. Cagnoli,155, 156 C. Cahillane,92 T. Callister,92 E. Calloni,157, 95

J. B. Camp,158 K. C. Cannon,159 J. Cao,160 C. D. Capano,99 E. Capocasa,121 F. Carbognani,125 S. Caride,161

J. Casanueva Diaz,114 C. Casentini,116, 104 S. Caudill,107 F. Cavalier,114 R. Cavalieri,125 G. Cella,110 C. B. Cepeda,92

L. Cerboni Baiardi,147, 148 G. Cerretani,109, 110 E. Cesarini,116, 104 R. Chakraborty,92 T. Chalermsongsak,92

S. J. Chamberlin,162 M. Chan,127 S. Chao,163 P. Charlton,164 E. Chassande-Mottin,121 H. Y. Chen,165 Y. Chen,166

C. Cheng,163 A. Chincarini,137 A. Chiummo,125 H. S. Cho,167 M. Cho,153 J. H. Chow,111 N. Christensen,168

Q. Chu,141 S. Chua,150 S. Chung,141 G. Ciani,96 F. Clara,128 J. A. Clark,154 F. Cleva,143 E. Coccia,116, 103, 104

P.-F. Cohadon,150 A. Colla,169, 119 C. G. Collette,170 L. Cominsky,171 M. Constancio Jr.,102 A. Conte,169, 119

L. Conti,133 D. Cook,128 T. R. Corbitt,93 N. Cornish,122 A. Corsi,161 S. Cortese,125 C. A. Costa,102

M. W. Coughlin,168 S. B. Coughlin,172 J.-P. Coulon,143 S. T. Countryman,130 P. Couvares,92 E. E. Cowan,154

D. M. Coward,141 M. J. Cowart,97 D. C. Coyne,92 R. Coyne,161 K. Craig,127 J. D. E. Creighton,107 J. Cripe,93

S. G. Crowder,173 A. Cumming,127 L. Cunningham,127 E. Cuoco,125 T. Dal Canton,99 S. L. Danilishin,127

S. D’Antonio,104 K. Danzmann,108, 99 N. S. Darman,174 V. Dattilo,125 I. Dave,138 H. P. Daveloza,175 M. Davier,114

G. S. Davies,127 E. J. Daw,176 R. Day,125 D. DeBra,131 G. Debreczeni,129 J. Degallaix,156 M. De Laurentis,157, 95

W. Del Pozzo,135 T. Denker,99, 108 H. Dereli,143 V. Dergachev,92 R. T. DeRosa,97 R. De Rosa,157, 95 R. DeSalvo,177

S. Dhurandhar,105 L. Di Fiore,95 M. Di Giovanni,169, 119 A. Di Lieto,109, 110 S. Di Pace,169, 119 I. Di Palma,120, 99

A. Di Virgilio,110 G. Dojcinoski,178 V. Dolique,156 F. Donovan,101 K. L. Dooley,112 S. Doravari,97, 99 R. Douglas,127

T. P. Downes,107 M. Drago,99, 179, 180 R. W. P. Drever,92 J. C. Driggers,128 Z. Du,160 M. Ducrot,98 S. E. Dwyer,128

T. B. Edo,176 M. C. Edwards,168 A. Effler,97 H.-B. Eggenstein,99 P. Ehrens,92 J. Eichholz,96 S. S. Eikenberry,96

W. Engels,166 R. C. Essick,101 T. Etzel,92 M. Evans,101 T. M. Evans,97 R. Everett,162 M. Factourovich,130

V. Fafone,116, 104, 103 H. Fair,126 S. Fairhurst,181 X. Fan,160 Q. Fang,141 S. Farinon,137 B. Farr,165 W. M. Farr,135

M. Favata,178 M. Fays,181 H. Fehrmann,99 M. M. Fejer,131 I. Ferrante,109, 110 E. C. Ferreira,102 F. Ferrini,125

F. Fidecaro,109, 110 I. Fiori,125 D. Fiorucci,121 R. P. Fisher,126 R. Flaminio,156, 182 M. Fletcher,127 J.-D. Fournier,143

S. Franco,114 S. Frasca,169, 119 F. Frasconi,110 Z. Frei,144 A. Freise,135 R. Frey,149 V. Frey,114 T. T. Fricke,99



10

P. Fritschel,101 V. V. Frolov,97 P. Fulda,96 M. Fyffe,97 H. A. G. Gabbard,112 J. R. Gair,183 L. Gammaitoni,123, 124

S. G. Gaonkar,105 F. Garufi,157, 95 A. Gatto,121 G. Gaur,184, 185 N. Gehrels,158 G. Gemme,137 B. Gendre,143

E. Genin,125 A. Gennai,110 J. George,138 L. Gergely,186 V. Germain,98 Archisman Ghosh,106 S. Ghosh,142, 100

J. A. Giaime,93, 97 K. D. Giardina,97 A. Giazotto,110 K. Gill,187 A. Glaefke,127 E. Goetz,188 R. Goetz,96

L. Gondan,144 J. M. Gonzalez Castro,109, 110 A. Gopakumar,189 N. A. Gordon,127 M. L. Gorodetsky,139

S. E. Gossan,92 M. Gosselin,125 R. Gouaty,98 C. Graef,127 P. B. Graff,153 M. Granata,156 A. Grant,127 S. Gras,101

C. Gray,128 G. Greco,147, 148 A. C. Green,135 P. Groot,142 H. Grote,99 S. Grunewald,120 G. M. Guidi,147, 148

X. Guo,160 A. Gupta,105 M. K. Gupta,185 K. E. Gushwa,92 E. K. Gustafson,92 R. Gustafson,188 J. J. Hacker,113

B. R. Hall,146 E. D. Hall,92 G. Hammond,127 M. Haney,189 M. M. Hanke,99 J. Hanks,128 C. Hanna,162

M. D. Hannam,181 J. Hanson,97 T. Hardwick,93 J. Harms,147, 148 G. M. Harry,190 I. W. Harry,120 M. J. Hart,127

M. T. Hartman,96 C.-J. Haster,135 K. Haughian,127 A. Heidmann,150 M. C. Heintze,96, 97 H. Heitmann,143

P. Hello,114 G. Hemming,125 M. Hendry,127 I. S. Heng,127 J. Hennig,127 A. W. Heptonstall,92 M. Heurs,99, 108

S. Hild,127 D. Hoak,191 K. A. Hodge,92 D. Hofman,156 S. E. Hollitt,44 K. Holt,97 D. E. Holz,165 P. Hopkins,181

D. J. Hosken,44 J. Hough,127 E. A. Houston,127 E. J. Howell,141 Y. M. Hu,127 S. Huang,163 E. A. Huerta,192, 172

D. Huet,114 B. Hughey,187 S. Husa,193 S. H. Huttner,127 T. Huynh-Dinh,97 A. Idrisy,162 N. Indik,99

D. R. Ingram,128 R. Inta,161 H. N. Isa,127 J.-M. Isac,150 M. Isi,92 G. Islas,113 T. Isogai,101 B. R. Iyer,106

K. Izumi,128 T. Jacqmin,150 H. Jang,167 K. Jani,154 P. Jaranowski,194 S. Jawahar,195 W. W. Johnson,93

D. I. Jones,117 R. Jones,127 R. J. G. Jonker,100 L. Ju,141 Haris K,196 C. V. Kalaghatgi,115, 181 V. Kalogera,172

S. Kandhasamy,112 G. Kang,167 J. B. Kanner,92 S. Karki,149 M. Kasprzack,93, 114, 125 E. Katsavounidis,101

W. Katzman,97 S. Kaufer,108 T. Kaur,141 K. Kawabe,128 F. Kawazoe,99, 108 M. S. Kehl,159 D. Keitel,99, 193

D. B. Kelley,126 W. Kells,92 R. Kennedy,176 J. S. Key,175 A. Khalaidovski,99 F. Y. Khalili,139 I. Khan,103

S. Khan,181 Z. Khan,185 E. A. Khazanov,197 N. Kijbunchoo,128 C. Kim,167 J. Kim,198 K. Kim,199 Nam-Gyu Kim,167

Namjun Kim,131 Y.-M. Kim,198 E. J. King,44 P. J. King,128 D. L. Kinzel,97 J. S. Kissel,128 L. Kleybolte,118

S. Klimenko,96 S. M. Koehlenbeck,99 K. Kokeyama,93 S. Koley,100 V. Kondrashov,92 A. Kontos,101 M. Korobko,118

W. Z. Korth,92 I. Kowalska,151 D. B. Kozak,92 V. Kringel,99 B. Krishnan,99 C. Krueger,108 G. Kuehn,99

P. Kumar,159 L. Kuo,163 A. Kutynia,200 B. D. Lackey,126 M. Landry,128 J. Lange,201 B. Lantz,131

P. D. Lasky,202 A. Lazzarini,92 C. Lazzaro,154, 133 P. Leaci,120, 169, 119 S. Leavey,127 E. O. Lebigot,121, 160

C. H. Lee,198 H. K. Lee,199 H. M. Lee,203 K. Lee,127 A. Lenon,126 M. Leonardi,179, 180 J. R. Leong,99 N. Leroy,114

N. Letendre,98 Y. Levin,202 B. M. Levine,128 T. G. F. Li,92 A. Libson,101 T. B. Littenberg,204 N. A. Lockerbie,195

J. Logue,127 A. L. Lombardi,191 J. E. Lord,126 M. Lorenzini,103, 104 V. Loriette,205 M. Lormand,97 G. Losurdo,148

J. D. Lough,99, 108 A. P. Lundgren,99 J. Luo,168 R. Lynch,101 Y. Ma,141 T. MacDonald,131 B. Machenschalk,99

M. MacInnis,101 D. M. Macleod,93 R. M. Magee,146 M. Mageswaran,92 E. Majorana,119 I. Maksimovic,205

V. Malvezzi,116, 104 N. Man,143 I. Mandel,135 V. Mandic,173 V. Mangano,127 G. L. Mansell,111 M. Manske,107

M. Mantovani,125 F. Marchesoni,206, 124 F. Marion,98 A. S. Markosyan,131 E. Maros,92 F. Martelli,147, 148

L. Martellini,143 I. W. Martin,127 R. M. Martin,96 D. V. Martynov,92 J. N. Marx,92 K. Mason,101 A. Masserot,98

T. J. Massinger,126 M. Masso-Reid,127 F. Matichard,101 L. Matone,130 N. Mavalvala,101 N. Mazumder,146

G. Mazzolo,99 R. McCarthy,128 D. E. McClelland,111 S. McCormick,97 S. C. McGuire,207 G. McIntyre,92

J. McIver,92 D. J. McManus,111 S. T. McWilliams,192 D. Meacher,162 G. D. Meadors,120, 99 J. Meidam,100

A. Melatos,174 G. Mendell,128 D. Mendoza-Gandara,99 R. A. Mercer,107 E. Merilh,128 M. Merzougui,143

S. Meshkov,92 C. Messenger,127 C. Messick,162 P. M. Meyers,173 F. Mezzani,119, 169 H. Miao,135 C. Michel,156

H. Middleton,135 E. E. Mikhailov,208 L. Milano,157, 95 J. Miller,101 M. Millhouse,122 Y. Minenkov,104 J. Ming,120, 99

S. Mirshekari,209 C. Mishra,106 S. Mitra,105 V. P. Mitrofanov,139 G. Mitselmakher,96 R. Mittleman,101 A. Moggi,110

M. Mohan,125 S. R. P. Mohapatra,101 M. Montani,147, 148 B. C. Moore,178 C. J. Moore,210 D. Moraru,128

G. Moreno,128 S. R. Morriss,175 K. Mossavi,99 B. Mours,98 C. M. Mow-Lowry,135 C. L. Mueller,96

G. Mueller,96 A. W. Muir,181 Arunava Mukherjee,106 D. Mukherjee,107 S. Mukherjee,175 N. Mukund,105

A. Mullavey,97 J. Munch,44 D. J. Murphy,130 P. G. Murray,127 A. Mytidis,96 I. Nardecchia,116, 104

L. Naticchioni,169, 119 R. K. Nayak,211 V. Necula,96 K. Nedkova,191 G. Nelemans,142, 100 M. Neri,136, 137

A. Neunzert,188 G. Newton,127 T. T. Nguyen,111 A. B. Nielsen,99 S. Nissanke,142, 100 A. Nitz,99 F. Nocera,125

D. Nolting,97 M. E. N. Normandin,175 L. K. Nuttall,126 J. Oberling,128 E. Ochsner,107 J. O’Dell,212 E. Oelker,101

G. H. Ogin,213 J. J. Oh,214 S. H. Oh,214 F. Ohme,181 M. Oliver,193 P. Oppermann,99 Richard J. Oram,97

B. O’Reilly,97 R. O’Shaughnessy,201 D. J. Ottaway,44 R. S. Ottens,96 H. Overmier,97 B. J. Owen,161 A. Pai,196

S. A. Pai,138 J. R. Palamos,149 O. Palashov,197 C. Palomba,119 A. Pal-Singh,118 H. Pan,163 C. Pankow,172

F. Pannarale,181 B. C. Pant,138 F. Paoletti,125, 110 A. Paoli,125 M. A. Papa,120, 107, 99 H. R. Paris,131 W. Parker,97



11

D. Pascucci,127 A. Pasqualetti,125 R. Passaquieti,109, 110 D. Passuello,110 B. Patricelli,109, 110 Z. Patrick,131

B. L. Pearlstone,127 M. Pedraza,92 R. Pedurand,156 L. Pekowsky,126 A. Pele,97 S. Penn,215 A. Perreca,92

M. Phelps,127 O. Piccinni,169, 119 M. Pichot,143 F. Piergiovanni,147, 148 V. Pierro,177 G. Pillant,125 L. Pinard,156

I. M. Pinto,177 M. Pitkin,127 R. Poggiani,109, 110 P. Popolizio,125 A. Post,99 J. Powell,127 J. Prasad,105 V. Predoi,181

S. S. Premachandra,202 T. Prestegard,173 L. R. Price,92 M. Prijatelj,125 M. Principe,177 S. Privitera,120 R. Prix,99

G. A. Prodi,179, 180 L. Prokhorov,139 O. Puncken,99 M. Punturo,124 P. Puppo,119 H. Qi,107 J. Qin,141

V. Quetschke,175 E. A. Quintero,92 R. Quitzow-James,149 F. J. Raab,128 D. S. Rabeling,111 H. Radkins,128

P. Raffai,144 S. Raja,138 M. Rakhmanov,175 P. Rapagnani,169, 119 V. Raymond,120 M. Razzano,109, 110 V. Re,116

J. Read,113 C. M. Reed,128 T. Regimbau,143 L. Rei,137 S. Reid,140 D. H. Reitze,92, 96 H. Rew,208 S. D. Reyes,126

F. Ricci,169, 119 K. Riles,188 N. A. Robertson,92, 127 R. Robie,127 F. Robinet,114 A. Rocchi,104 L. Rolland,98

J. G. Rollins,92 V. J. Roma,149 J. D. Romano,175 R. Romano,94, 95 G. Romanov,208 J. H. Romie,97 S. Rowan,127

P. Ruggi,125 K. Ryan,128 S. Sachdev,92 T. Sadecki,128 L. Sadeghian,107 L. Salconi,125 M. Saleem,196 F. Salemi,99

A. Samajdar,211 L. Sammut,174, 202 E. J. Sanchez,92 V. Sandberg,128 B. Sandeen,172 J. R. Sanders,188, 126

B. Sassolas,156 B. S. Sathyaprakash,181 P. R. Saulson,126 O. Sauter,188 R. L. Savage,128 A. Sawadsky,108

P. Schale,149 R. Schilling†,99 J. Schmidt,99 P. Schmidt,92, 166 R. Schnabel,118 R. M. S. Schofield,149 E. Schreiber,99

D. Schuette,99, 108 B. F. Schutz,181, 120 J. Scott,127 S. M. Scott,111 D. Sellers,97 A. S. Sengupta,184 D. Sentenac,125

V. Sequino,116, 104 A. Sergeev,197 G. Serna,113 Y. Setyawati,142, 100 A. Sevigny,128 D. A. Shaddock,111 S. Shah,142, 100

M. S. Shahriar,172 M. Shaltev,99 Z. Shao,92 B. Shapiro,131 P. Shawhan,153 A. Sheperd,107 D. H. Shoemaker,101

D. M. Shoemaker,154 K. Siellez,143, 154 X. Siemens,107 D. Sigg,128 A. D. Silva,102 D. Simakov,99 A. Singer,92

L. P. Singer,158 A. Singh,120, 99 R. Singh,93 A. Singhal,103 A. M. Sintes,193 B. J. J. Slagmolen,111 J. R. Smith,113

N. D. Smith,92 R. J. E. Smith,92 E. J. Son,214 B. Sorazu,127 F. Sorrentino,137 T. Souradeep,105 A. K. Srivastava,185

A. Staley,130 M. Steinke,99 J. Steinlechner,127 S. Steinlechner,127 D. Steinmeyer,99, 108 B. C. Stephens,107

R. Stone,175 K. A. Strain,127 N. Straniero,156 G. Stratta,147, 148 N. A. Strauss,168 S. Strigin,139 R. Sturani,209

A. L. Stuver,97 T. Z. Summerscales,216 L. Sun,174 P. J. Sutton,181 B. L. Swinkels,125 M. Tacca,121 D. Talukder,149

D. B. Tanner,96 S. P. Tarabrin,99 A. Taracchini,120 R. Taylor,92 T. Theeg,99 M. P. Thirugnanasambandam,92

E. G. Thomas,135 M. Thomas,97 P. Thomas,128 K. A. Thorne,97 K. S. Thorne,166 E. Thrane,202 S. Tiwari,103

V. Tiwari,181 K. V. Tokmakov,195 C. Tomlinson,176 M. Tonelli,109, 110 C. V. Torres‡,217 C. I. Torrie,92

F. Travasso,123, 124 G. Traylor,97 M. C. Tringali,179, 180 L. Trozzo,218, 110 M. Tse,101 M. Turconi,143

D. Tuyenbayev,175 D. Ugolini,219 C. S. Unnikrishnan,189 A. L. Urban,107 S. A. Usman,126 H. Vahlbruch,108

G. Vajente,92 G. Valdes,175 N. van Bakel,100 M. van Beuzekom,100 J. F. J. van den Brand,152, 100

C. Van Den Broeck,100 D. C. Vander-Hyde,126, 113 L. van der Schaaf,100 J. V. van Heijningen,100 A. A. van Veggel,127

M. Vardaro,132, 133 S. Vass,92 R. Vaulin,101 A. Vecchio,135 G. Vedovato,133 J. Veitch,135 P. J. Veitch,44

K. Venkateswara,220 D. Verkindt,98 F. Vetrano,147, 148 S. Vinciguerra,135 D. J. Vine,140 J.-Y. Vinet,143 S. Vitale,101

T. Vo,126 H. Vocca,123, 124 C. Vorvick,128 D. Voss,96 W. D. Vousden,135 S. P. Vyatchanin,139 A. R. Wade,111

L. E. Wade,221 M. Wade,221 M. Walker,93 L. Wallace,92 S. Walsh,107, 99, 120 G. Wang,103 H. Wang,135 M. Wang,135

X. Wang,160 Y. Wang,141 R. L. Ward,111 J. Warner,128 M. Was,98 B. Weaver,128 L.-W. Wei,143 M. Weinert,99

A. J. Weinstein,92 R. Weiss,101 T. Welborn,97 L. Wen,141 T. Westphal,99 K. Wette,99 J. T. Whelan,201, 99

D. J. White,176 B. F. Whiting,96 R. D. Williams,92 A. R. Williamson,181 J. L. Willis,222 B. Willke,108, 99

M. H. Wimmer,99, 108 W. Winkler,99 C. C. Wipf,92 H. Wittel,99, 108 G. Woan,127 J. Worden,128 J. L. Wright,127

G. Wu,97 J. Yablon,172 W. Yam,101 H. Yamamoto,92 C. C. Yancey,153 M. J. Yap,111 H. Yu,101 M. Yvert,98

L. Zangrando,133 M. Zanolin,187 J.-P. Zendri,133 M. Zevin,172 F. Zhang,101 L. Zhang,92 M. Zhang,208 Y. Zhang,201

C. Zhao,141 M. Zhou,172 Z. Zhou,172 X. J. Zhu,141 M. E. Zucker,92, 101 S. E. Zuraw,191 and J. Zweizig92

(LIGO Scientific Collaboration and Virgo Collaboration)

†Deceased, May 2015. ‡Deceased, March 2015.
1Institut d’Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC)

- Universitat Politècnica de València. C/ Paranimf 1 , 46730 Gandia, Spain.
2GRPHE - Université de Haute Alsace - Institut universitaire de technologie de Colmar,

34 rue du Grillenbreit BP 50568 - 68008 Colmar, France
3Technical University of Catalonia, Laboratory of Applied Bioacoustics,

Rambla Exposició,08800 Vilanova i la Geltrú,Barcelona, Spain
4Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, D-91058 Erlangen, Germany

5Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, 13288 Marseille, France
6APC, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU,

Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris, France



12

7IFIC - Instituto de F́ısica Corpuscular c/ Catedraático José Beltrán, 2 E-46980 Paterna, Valencia, Spain
8LAM - Laboratoire d’Astrophysique de Marseille, Pôle de l’Étoile Site de Château-Gombert,

rue Frédéric Joliot-Curie 38, 13388 Marseille Cedex 13, France
9INFN - Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, 95123 Catania, Italy

10Nikhef, Science Park, Amsterdam, The Netherlands
11Huygens-Kamerlingh Onnes Laboratorium, Universiteit Leiden, The Netherlands

12Universiteit van Amsterdam, Instituut voor Hoge-Energie Fysica,
Science Park 105, 1098 XG Amsterdam, The Netherlands

13INFN -Sezione di Roma, P.le Aldo Moro 2, 00185 Roma, Italy
14Dipartimento di Fisica dell’Università La Sapienza, P.le Aldo Moro 2, 00185 Roma, Italy

15Institute for Space Science, RO-077125 Bucharest, Măgurele, Romania
16INFN - Sezione di Bologna, Viale Berti-Pichat 6/2, 40127 Bologna, Italy

17INFN - Sezione di Bari, Via E. Orabona 4, 70126 Bari, Italy
18Géoazur, UCA, CNRS, IRD, Observatoire de la Côte d’Azur, Sophia Antipolis, France

19Univ. Paris-Sud , 91405 Orsay Cedex, France
20University Mohammed I, Laboratory of Physics of Matter and Radiations, B.P.717, Oujda 6000, Morocco

21Institut für Theoretische Physik und Astrophysik,
Universität Würzburg, Emil-Fischer Str. 31, 97074 Würzburg, Germany

22Institut d’Investigació per a la Gestió Integrada de les Zones Costaneres (IGIC)
- Universitat Politècnica de València. C/ Paranimf 1, 46730 Gandia, Spain.

23Dipartimento di Fisica e Astronomia dell’Università, Viale Berti Pichat 6/2, 40127 Bologna, Italy
24Laboratoire de Physique Corpusculaire, Clermont Université,

Université Blaise Pascal, CNRS/IN2P3, BP 10448, F-63000 Clermont-Ferrand, France
25Also at APC, Université Paris Diderot, CNRS/IN2P3, CEA/IRFU,

Observatoire de Paris, Sorbonne Paris Cité, 75205 Paris, France
26INFN - Sezione di Catania, Viale Andrea Doria 6, 95125 Catania, Italy

27LSIS, Aix Marseille Université CNRS ENSAM LSIS UMR 7296 13397 Marseille,
France ; Université de Toulon CNRS LSIS UMR 7296 83957 La Garde, France

28Institut Universitaire de France, 75005 Paris, France
29Royal Netherlands Institute for Sea Research (NIOZ),

Landsdiep 4,1797 SZ ’t Horntje (Texel), The Netherlands
30INFN - Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy

31Dipartimento di Fisica dell’Università, Via Dodecaneso 33, 16146 Genova, Italy
32Dr. Remeis-Sternwarte and ECAP, Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany

33Moscow State University,Skobeltsyn Institute of Nuclear Physics,Leninskie gory, 119991 Moscow, Russia
34Mediterranean Institute of Oceanography (MIO), Aix-Marseille University,

13288, Marseille, Cedex 9, France; Université du Sud Toulon-Var,
83957, La Garde Cedex, France CNRS-INSU/IRD UM 110

35Dipartimento di Fisica ed Astronomia dell’Università, Viale Andrea Doria 6, 95125 Catania, Italy
36Direction des Sciences de la Matière - Institut de recherche sur les
lois fondamentales de l’Univers - Service de Physique des Particules,

CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
37INFN - Sezione di Pisa, Largo B. Pontecorvo 3, 56127 Pisa, Italy

38Dipartimento di Fisica dell’Università, Largo B. Pontecorvo 3, 56127 Pisa, Italy
39INFN -Sezione di Napoli, Via Cintia 80126 Napoli, Italy

40Université de Strasbourg, IPHC, 23 rue du Loess 67037 Strasbourg,
France - CNRS, UMR7178, 67037 Strasbourg, France

41now at INFN - Sezione di Bari, Via E. Orabona 4, 70126 Bari, Italy
42Dipartimento di Fisica dell’Università Federico II di Napoli, Via Cintia 80126, Napoli, Italy

43III. Physikalisches Institut, RWTH Aachen University, D-52056 Aachen, Germany
44University of Adelaide, Adelaide, South Australia 5005, Australia
45Dept. of Physics and Astronomy, University of Alaska Anchorage,

3211 Providence Dr., Anchorage, AK 99508, USA
46CTSPS, Clark-Atlanta University, Atlanta, GA 30314, USA
47School of Physics and Center for Relativistic Astrophysics,

Georgia Institute of Technology, Atlanta, GA 30332, USA
48Dept. of Physics, Southern University, Baton Rouge, LA 70813, USA
49Dept. of Physics, University of California, Berkeley, CA 94720, USA
50Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA

51Institut für Physik, Humboldt-Universität zu Berlin, D-12489 Berlin, Germany
52Fakultät für Physik & Astronomie, Ruhr-Universität Bochum, D-44780 Bochum, Germany

53Physikalisches Institut, Universität Bonn, Nussallee 12, D-53115 Bonn, Germany
54Université Libre de Bruxelles, Science Faculty CP230, B-1050 Brussels, Belgium



13

55Vrije Universiteit Brussel, Dienst ELEM, B-1050 Brussels, Belgium
56Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

57Dept. of Physics, Chiba University, Chiba 263-8522, Japan
58Dept. of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand

59Dept. of Physics, University of Maryland, College Park, MD 20742, USA
60Dept. of Physics and Center for Cosmology and Astro-Particle Physics,

Ohio State University, Columbus, OH 43210, USA
61Dept. of Astronomy, Ohio State University, Columbus, OH 43210, USA

62Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark
63Dept. of Physics, TU Dortmund University, D-44221 Dortmund, Germany

64Dept. of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA
65Dept. of Physics, University of Alberta, Edmonton, Alberta, Canada T6G 2E1

66Département de physique nucléaire et corpusculaire,
Université de Genève, CH-1211 Genève, Switzerland

67Dept. of Physics and Astronomy, University of Gent, B-9000 Gent, Belgium
68Dept. of Physics and Astronomy, University of California, Irvine, CA 92697, USA
69Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA

70Dept. of Astronomy, University of Wisconsin, Madison, WI 53706, USA
71Dept. of Physics and Wisconsin IceCube Particle Astrophysics Center,

University of Wisconsin, Madison, WI 53706, USA
72Institute of Physics, University of Mainz, Staudinger Weg 7, D-55099 Mainz, Germany

73Université de Mons, 7000 Mons, Belgium
74Technische Universität München, D-85748 Garching, Germany
75Bartol Research Institute and Dept. of Physics and Astronomy,

University of Delaware, Newark, DE 19716, USA
76Dept. of Physics, Yale University, New Haven, CT 06520, USA

77Dept. of Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK
78Dept. of Physics, Drexel University, 3141 Chestnut Street, Philadelphia, PA 19104, USA

79Physics Department, South Dakota School of Mines and Technology, Rapid City, SD 57701, USA
80Dept. of Physics, University of Wisconsin, River Falls, WI 54022, USA

81Oskar Klein Centre and Dept. of Physics, Stockholm University, SE-10691 Stockholm, Sweden
82Dept. of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA

83Dept. of Physics, Sungkyunkwan University, Suwon 440-746, Korea
84Dept. of Physics, University of Toronto, Toronto, Ontario, Canada, M5S 1A7

85Dept. of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA
86Dept. of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA

87Dept. of Physics, Pennsylvania State University, University Park, PA 16802, USA
88Dept. of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA

89Dept. of Physics and Astronomy, Uppsala University, Box 516, S-75120 Uppsala, Sweden
90Dept. of Physics, University of Wuppertal, D-42119 Wuppertal, Germany

91DESY, D-15735 Zeuthen, Germany
92LIGO, California Institute of Technology, Pasadena, CA 91125, USA

93Louisiana State University, Baton Rouge, LA 70803, USA
94Università di Salerno, Fisciano, I-84084 Salerno, Italy

95INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy
96University of Florida, Gainesville, FL 32611, USA

97LIGO Livingston Observatory, Livingston, LA 70754, USA
98Laboratoire d’Annecy-le-Vieux de Physique des Particules (LAPP),

Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
99Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-30167 Hannover, Germany

100Nikhef, Science Park, 1098 XG Amsterdam, Netherlands
101LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

102Instituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, Brazil
103INFN, Gran Sasso Science Institute, I-67100 L’Aquila, Italy
104INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy

105Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
106International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore 560012, India

107University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA
108Leibniz Universität Hannover, D-30167 Hannover, Germany

109Università di Pisa, I-56127 Pisa, Italy
110INFN, Sezione di Pisa, I-56127 Pisa, Italy

111Australian National University, Canberra, Australian Capital Territory 0200, Australia
112The University of Mississippi, University, MS 38677, USA

113California State University Fullerton, Fullerton, CA 92831, USA



14

114LAL, Université Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, 91400 Orsay, France
115Chennai Mathematical Institute, Chennai 603103, India
116Università di Roma Tor Vergata, I-00133 Roma, Italy

117University of Southampton, Southampton SO17 1BJ, United Kingdom
118Universität Hamburg, D-22761 Hamburg, Germany

119INFN, Sezione di Roma, I-00185 Roma, Italy
120Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, D-14476 Potsdam-Golm, Germany

121APC, AstroParticule et Cosmologie, Université Paris Diderot,
CNRS/IN2P3, CEA/Irfu, Observatoire de Paris,

Sorbonne Paris Cité, F-75205 Paris Cedex 13, France
122Montana State University, Bozeman, MT 59717, USA

123Università di Perugia, I-06123 Perugia, Italy
124INFN, Sezione di Perugia, I-06123 Perugia, Italy

125European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
126Syracuse University, Syracuse, NY 13244, USA

127SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom
128LIGO Hanford Observatory, Richland, WA 99352, USA

129Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29-33, Hungary
130Columbia University, New York, NY 10027, USA
131Stanford University, Stanford, CA 94305, USA

132Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
133INFN, Sezione di Padova, I-35131 Padova, Italy

134CAMK-PAN, 00-716 Warsaw, Poland
135University of Birmingham, Birmingham B15 2TT, United Kingdom

136Università degli Studi di Genova, I-16146 Genova, Italy
137INFN, Sezione di Genova, I-16146 Genova, Italy

138RRCAT, Indore MP 452013, India
139Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia
140SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom
141University of Western Australia, Crawley, Western Australia 6009, Australia

142Department of Astrophysics/IMAPP, Radboud University Nijmegen,
P.O. Box 9010, 6500 GL Nijmegen, Netherlands

143Artemis, Université Côte d’Azur, CNRS, Observatoire Côte d’Azur, CS 34229, Nice cedex 4, France
144MTA Eötvös University, “Lendulet” Astrophysics Research Group, Budapest 1117, Hungary
145Institut de Physique de Rennes, CNRS, Université de Rennes 1, F-35042 Rennes, France

146Washington State University, Pullman, WA 99164, USA
147Università degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
148INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy

149University of Oregon, Eugene, OR 97403, USA
150Laboratoire Kastler Brossel, UPMC-Sorbonne Universités, CNRS,

ENS-PSL Research University, Collège de France, F-75005 Paris, France
151Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland

152VU University Amsterdam, 1081 HV Amsterdam, Netherlands
153University of Maryland, College Park, MD 20742, USA

154Center for Relativistic Astrophysics and School of Physics,
Georgia Institute of Technology, Atlanta, GA 30332, USA

155Institut Lumière Matière, Université de Lyon,
Université Claude Bernard Lyon 1, UMR CNRS 5306, 69622 Villeurbanne, France

156Laboratoire des Matériaux Avancés (LMA), IN2P3/CNRS,
Université de Lyon, F-69622 Villeurbanne, Lyon, France

157Università di Napoli “Federico II,” Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy
158NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA

159Canadian Institute for Theoretical Astrophysics,
University of Toronto, Toronto, Ontario M5S 3H8, Canada

160Tsinghua University, Beijing 100084, China
161Texas Tech University, Lubbock, TX 79409, USA

162The Pennsylvania State University, University Park, PA 16802, USA
163National Tsing Hua University, Hsinchu City, 30013 Taiwan, Republic of China

164Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia
165University of Chicago, Chicago, IL 60637, USA

166Caltech CaRT, Pasadena, CA 91125, USA
167Korea Institute of Science and Technology Information, Daejeon 305-806, Korea

168Carleton College, Northfield, MN 55057, USA
169Università di Roma “La Sapienza,” I-00185 Roma, Italy



15

170University of Brussels, Brussels 1050, Belgium
171Sonoma State University, Rohnert Park, CA 94928, USA

172Northwestern University, Evanston, IL 60208, USA
173University of Minnesota, Minneapolis, MN 55455, USA

174The University of Melbourne, Parkville, Victoria 3010, Australia
175The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA

176The University of Sheffield, Sheffield S10 2TN, United Kingdom
177University of Sannio at Benevento, I-82100 Benevento,
Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
178Montclair State University, Montclair, NJ 07043, USA

179Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
180INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy

181Cardiff University, Cardiff CF24 3AA, United Kingdom
182National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

183School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom
184Indian Institute of Technology, Gandhinagar Ahmedabad Gujarat 382424, India

185Institute for Plasma Research, Bhat, Gandhinagar 382428, India
186University of Szeged, Dóm tér 9, Szeged 6720, Hungary

187Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
188University of Michigan, Ann Arbor, MI 48109, USA

189Tata Institute of Fundamental Research, Mumbai 400005, India
190American University, Washington, D.C. 20016, USA

191University of Massachusetts-Amherst, Amherst, MA 01003, USA
192West Virginia University, Morgantown, WV 26506, USA

193Universitat de les Illes Balears, IAC3—IEEC, E-07122 Palma de Mallorca, Spain
194University of Bia lystok, 15-424 Bia lystok, Poland

195SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom
196IISER-TVM, CET Campus, Trivandrum Kerala 695016, India
197Institute of Applied Physics, Nizhny Novgorod, 603950, Russia

198Pusan National University, Busan 609-735, Korea
199Hanyang University, Seoul 133-791, Korea

200NCBJ, 05-400 Świerk-Otwock, Poland
201Rochester Institute of Technology, Rochester, NY 14623, USA

202Monash University, Victoria 3800, Australia
203Seoul National University, Seoul 151-742, Korea

204University of Alabama in Huntsville, Huntsville, AL 35899, USA
205ESPCI, CNRS, F-75005 Paris, France

206Università di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy
207Southern University and A&M College, Baton Rouge, LA 70813, USA

208College of William and Mary, Williamsburg, VA 23187, USA
209Instituto de F́ısica Teórica, University Estadual Paulista/ICTP South

American Institute for Fundamental Research, São Paulo SP 01140-070, Brazil
210University of Cambridge, Cambridge CB2 1TN, United Kingdom

211IISER-Kolkata, Mohanpur, West Bengal 741252, India
212Rutherford Appleton Laboratory, HSIC, Chilton, Didcot, Oxon OX11 0QX, United Kingdom

213Whitman College, 345 Boyer Avenue, Walla Walla, WA 99362 USA
214National Institute for Mathematical Sciences, Daejeon 305-390, Korea

215Hobart and William Smith Colleges, Geneva, NY 14456, USA
216Andrews University, Berrien Springs, MI 49104, USA

21785The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
218Università di Siena, I-53100 Siena, Italy

219Trinity University, San Antonio, TX 78212, USA
220University of Washington, Seattle, WA 98195, USA

221Kenyon College, Gambier, OH 43022, USA
222Abilene Christian University, Abilene, TX 79699, USA