of 17
D
RAFT VERSION
J
ULY
27, 2016
Preprint typeset using L
A
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UPPER LIMITS ON THE RATES OF BINARY NEUTRON STAR AND NEUTRON-STAR–BLACK-HOLE MERGERS
FROM ADVANCED LIGO’S FIRST OBSERVING RUN
B. P. A
BBOTT
,
1
R. A
BBOTT
,
1
T. D. A
BBOTT
,
2
M. R. A
BERNATHY
,
3
F. A
CERNESE
,
4,5
K. A
CKLEY
,
6
C. A
DAMS
,
7
T. A
DAMS
,
8
P. A
DDESSO
,
9
R. X. A
DHIKARI
,
1
V. B. A
DYA
,
10
C. A
FFELDT
,
10
M. A
GATHOS
,
11
K. A
GATSUMA
,
11
N. A
GGARWAL
,
12
O. D. A
GUIAR
,
13
L. A
IELLO
,
14,15
A. A
IN
,
16
P. A
JITH
,
17
B. A
LLEN
,
10,18,19
A. A
LLOCCA
,
20,21
P. A. A
LTIN
,
22
S. B. A
NDERSON
,
1
W. G. A
NDERSON
,
18
K. A
RAI
,
1
M. C. A
RAYA
,
1
C. C. A
RCENEAUX
,
23
J. S. A
REEDA
,
24
N. A
RNAUD
,
25
K. G. A
RUN
,
26
S. A
SCENZI
,
27,15
G. A
SHTON
,
28
M. A
ST
,
29
S. M. A
STON
,
7
P. A
STONE
,
30
P. A
UFMUTH
,
19
C. A
ULBERT
,
10
S. B
ABAK
,
31
P. B
ACON
,
32
M. K. M. B
ADER
,
11
P. T. B
AKER
,
33
F. B
ALDACCINI
,
34,35
G. B
ALLARDIN
,
36
S. W. B
ALLMER
,
37
J. C. B
ARAYOGA
,
1
S. E. B
ARCLAY
,
38
B. C. B
ARISH
,
1
D. B
ARKER
,
39
F. B
ARONE
,
4,5
B. B
ARR
,
38
L. B
ARSOTTI
,
12
M. B
ARSUGLIA
,
32
D. B
ARTA
,
40
J. B
ARTLETT
,
39
I. B
ARTOS
,
41
R. B
ASSIRI
,
42
A. B
ASTI
,
20,21
J. C. B
ATCH
,
39
C. B
AUNE
,
10
V. B
AVIGADDA
,
36
M. B
AZZAN
,
43,44
M. B
EJGER
,
45
A. S. B
ELL
,
38
B. K. B
ERGER
,
1
G. B
ERGMANN
,
10
C. P. L. B
ERRY
,
46
D. B
ERSANETTI
,
47,48
A. B
ERTOLINI
,
11
J. B
ETZWIESER
,
7
S. B
HAGWAT
,
37
R. B
HANDARE
,
49
I. A. B
ILENKO
,
50
G. B
ILLINGSLEY
,
1
J. B
IRCH
,
7
R. B
IRNEY
,
51
S. B
ISCANS
,
12
A. B
ISHT
,
10,19
M. B
ITOSSI
,
36
C. B
IWER
,
37
M. A. B
IZOUARD
,
25
J. K. B
LACKBURN
,
1
C. D. B
LAIR
,
52
D. G. B
LAIR
,
52
R. M. B
LAIR
,
39
S. B
LOEMEN
,
53
O. B
OCK
,
10
M. B
OER
,
54
G. B
OGAERT
,
54
C. B
OGAN
,
10
A. B
OHE
,
31
C. B
OND
,
46
F. B
ONDU
,
55
R. B
ONNAND
,
8
B. A. B
OOM
,
11
R. B
ORK
,
1
V. B
OSCHI
,
20,21
S. B
OSE
,
56,16
Y. B
OUFFANAIS
,
32
A. B
OZZI
,
36
C. B
RADASCHIA
,
21
P. R. B
RADY
,
18
V. B. B
RAGINSKY
,
50
M. B
RANCHESI
,
57,58
J. E. B
RAU
,
59
T. B
RIANT
,
60
A. B
RILLET
,
54
M. B
RINKMANN
,
10
V. B
RISSON
,
25
P. B
ROCKILL
,
18
J. E. B
ROIDA
,
61
A. F. B
ROOKS
,
1
D. A. B
ROWN
,
37
D. D. B
ROWN
,
46
N. M. B
ROWN
,
12
S. B
RUNETT
,
1
C. C. B
UCHANAN
,
2
A. B
UIKEMA
,
12
T. B
ULIK
,
62
H. J. B
ULTEN
,
63,11
A. B
UONANNO
,
31,64
D. B
USKULIC
,
8
C. B
UY
,
32
R. L. B
YER
,
42
M. C
ABERO
,
10
L. C
ADONATI
,
65
G. C
AGNOLI
,
66,67
C. C
AHILLANE
,
1
J. C
ALDER
́
ON
B
USTILLO
,
65
T. C
ALLISTER
,
1
E. C
ALLONI
,
68,5
J. B. C
AMP
,
69
K. C. C
ANNON
,
70
J. C
AO
,
71
C. D. C
APANO
,
10
E. C
APOCASA
,
32
F. C
ARBOGNANI
,
36
S. C
ARIDE
,
72
J. C
ASANUEVA
D
IAZ
,
25
C. C
ASENTINI
,
27,15
S. C
AUDILL
,
18
M. C
AVAGLI
`
A
,
23
F. C
AVALIER
,
25
R. C
AVALIERI
,
36
G. C
ELLA
,
21
C. B. C
EPEDA
,
1
L. C
ERBONI
B
AIARDI
,
57,58
G. C
ERRETANI
,
20,21
E. C
ESARINI
,
27,15
S. J. C
HAMBERLIN
,
73
M. C
HAN
,
38
S. C
HAO
,
74
P. C
HARLTON
,
75
E. C
HASSANDE
-M
OTTIN
,
32
B. D. C
HEESEBORO
,
76
H. Y. C
HEN
,
77
Y. C
HEN
,
78
C. C
HENG
,
74
A. C
HINCARINI
,
48
A. C
HIUMMO
,
36
H. S. C
HO
,
79
M. C
HO
,
64
J. H. C
HOW
,
22
N. C
HRISTENSEN
,
61
Q. C
HU
,
52
S. C
HUA
,
60
S. C
HUNG
,
52
G. C
IANI
,
6
F. C
LARA
,
39
J. A. C
LARK
,
65
F. C
LEVA
,
54
E. C
OCCIA
,
27,14
P.-F. C
OHADON
,
60
A. C
OLLA
,
80,30
C. G. C
OLLETTE
,
81
L. C
OMINSKY
,
82
M. C
ONSTANCIO
J
R
.,
13
A. C
ONTE
,
80,30
L. C
ONTI
,
44
D. C
OOK
,
39
T. R. C
ORBITT
,
2
N. C
ORNISH
,
33
A. C
ORSI
,
72
S. C
ORTESE
,
36
C. A. C
OSTA
,
13
M. W. C
OUGHLIN
,
61
S. B. C
OUGHLIN
,
83
J.-P. C
OULON
,
54
S. T. C
OUNTRYMAN
,
41
P. C
OUVARES
,
1
E. E. C
OWAN
,
65
D. M. C
OWARD
,
52
M. J. C
OWART
,
7
D. C. C
OYNE
,
1
R. C
OYNE
,
72
K. C
RAIG
,
38
J. D. E. C
REIGHTON
,
18
J. C
RIPE
,
2
S. G. C
ROWDER
,
84
A. C
UMMING
,
38
L. C
UNNINGHAM
,
38
E. C
UOCO
,
36
T. D
AL
C
ANTON
,
10
S. L. D
ANILISHIN
,
38
S. D’A
NTONIO
,
15
K. D
ANZMANN
,
19,10
N. S. D
ARMAN
,
85
A. D
ASGUPTA
,
86
C. F. D
A
S
ILVA
C
OSTA
,
6
V. D
ATTILO
,
36
I. D
AVE
,
49
M. D
AVIER
,
25
G. S. D
AVIES
,
38
E. J. D
AW
,
87
R. D
AY
,
36
S. D
E
,
37
D. D
E
B
RA
,
42
G. D
EBRECZENI
,
40
J. D
EGALLAIX
,
66
M. D
E
L
AURENTIS
,
68,5
S. D
EL
́
EGLISE
,
60
W. D
EL
P
OZZO
,
46
T. D
ENKER
,
10
T. D
ENT
,
10
V. D
ERGACHEV
,
1
R. D
E
R
OSA
,
68,5
R. T. D
E
R
OSA
,
7
R. D
E
S
ALVO
,
9
R. C. D
EVINE
,
76
S. D
HURANDHAR
,
16
M. C. D
́
IAZ
,
88
L. D
I
F
IORE
,
5
M. D
I
G
IOVANNI
,
89,90
T. D
I
G
IROLAMO
,
68,5
A. D
I
L
IETO
,
20,21
S. D
I
P
ACE
,
80,30
I. D
I
P
ALMA
,
31,80,30
A. D
I
V
IRGILIO
,
21
V. D
OLIQUE
,
66
F. D
ONOVAN
,
12
K. L. D
OOLEY
,
23
S. D
ORAVARI
,
10
R. D
OUGLAS
,
38
T. P. D
OWNES
,
18
M. D
RAGO
,
10
R. W. P. D
REVER
,
1
J. C. D
RIGGERS
,
39
M. D
UCROT
,
8
S. E. D
WYER
,
39
T. B. E
DO
,
87
M. C. E
DWARDS
,
61
A. E
FFLER
,
7
H.-B. E
GGENSTEIN
,
10
P. E
HRENS
,
1
J. E
ICHHOLZ
,
6,1
S. S. E
IKENBERRY
,
6
W. E
NGELS
,
78
R. C. E
SSICK
,
12
T. E
TZEL
,
1
M. E
VANS
,
12
T. M. E
VANS
,
7
R. E
VERETT
,
73
M. F
ACTOUROVICH
,
41
V. F
AFONE
,
27,15
H. F
AIR
,
37
S. F
AIRHURST
,
91
X. F
AN
,
71
Q. F
ANG
,
52
S. F
ARINON
,
48
B. F
ARR
,
77
W. M. F
ARR
,
46
M. F
AVATA
,
92
M. F
AYS
,
91
H. F
EHRMANN
,
10
M. M. F
EJER
,
42
E. F
ENYVESI
,
93
I. F
ERRANTE
,
20,21
E. C. F
ERREIRA
,
13
F. F
ERRINI
,
36
F. F
IDECARO
,
20,21
I. F
IORI
,
36
D. F
IORUCCI
,
32
R. P. F
ISHER
,
37
R. F
LAMINIO
,
66,94
M. F
LETCHER
,
38
J.-D. F
OURNIER
,
54
S. F
RASCA
,
80,30
F. F
RASCONI
,
21
Z. F
REI
,
93
A. F
REISE
,
46
R. F
REY
,
59
V. F
REY
,
25
P. F
RITSCHEL
,
12
V. V. F
ROLOV
,
7
P. F
ULDA
,
6
M. F
YFFE
,
7
H. A. G. G
ABBARD
,
23
J. R. G
AIR
,
95
L. G
AMMAITONI
,
34
S. G. G
AONKAR
,
16
F. G
ARUFI
,
68,5
G. G
AUR
,
96,86
N. G
EHRELS
,
69
G. G
EMME
,
48
P. G
ENG
,
88
E. G
ENIN
,
36
A. G
ENNAI
,
21
J. G
EORGE
,
49
L. G
ERGELY
,
97
V. G
ERMAIN
,
8
A
BHIRUP
G
HOSH
,
17
A
RCHISMAN
G
HOSH
,
17
S. G
HOSH
,
53,11
J. A. G
IAIME
,
2,7
K. D. G
IARDINA
,
7
A. G
IAZOTTO
,
21
K. G
ILL
,
98
A. G
LAEFKE
,
38
E. G
OETZ
,
39
R. G
OETZ
,
6
L. G
ONDAN
,
93
G. G
ONZ
́
ALEZ
,
2
J. M. G
ONZALEZ
C
ASTRO
,
20,21
A. G
OPAKUMAR
,
99
N. A. G
ORDON
,
38
M. L. G
ORODETSKY
,
50
S. E. G
OSSAN
,
1
M. G
OSSELIN
,
36
R. G
OUATY
,
8
A. G
RADO
,
100,5
C. G
RAEF
,
38
P. B. G
RAFF
,
64
M. G
RANATA
,
66
A. G
RANT
,
38
S. G
RAS
,
12
C. G
RAY
,
39
G. G
RECO
,
57,58
A. C. G
REEN
,
46
P. G
ROOT
,
53
H. G
ROTE
,
10
S. G
RUNEWALD
,
31
G. M. G
UIDI
,
57,58
X. G
UO
,
71
A. G
UPTA
,
16
M. K. G
UPTA
,
86
K. E. G
USHWA
,
1
E. K. G
USTAFSON
,
1
R. G
USTAFSON
,
101
J. J. H
ACKER
,
24
B. R. H
ALL
,
56
E. D. H
ALL
,
1
G. H
AMMOND
,
38
M. H
ANEY
,
99
M. M. H
ANKE
,
10
J. H
ANKS
,
39
C. H
ANNA
,
73
M. D. H
ANNAM
,
91
J. H
ANSON
,
7
T. H
ARDWICK
,
2
J. H
ARMS
,
57,58
G. M. H
ARRY
,
3
I. W. H
ARRY
,
31
M. J. H
ART
,
38
M. T. H
ARTMAN
,
6
C.-J. H
ASTER
,
46
K. H
AUGHIAN
,
38
A. H
EIDMANN
,
60
M. C. H
EINTZE
,
7
H. H
EITMANN
,
54
P. H
ELLO
,
25
G. H
EMMING
,
36
M. H
ENDRY
,
38
I. S. H
ENG
,
38
J. H
ENNIG
,
38
J. H
ENRY
,
102
A. W. H
EPTONSTALL
,
1
M. H
EURS
,
10,19
S. H
ILD
,
38
D. H
OAK
,
36
D. H
OFMAN
,
66
K. H
OLT
,
7
D. E. H
OLZ
,
77
P. H
OPKINS
,
91
J. H
OUGH
,
38
E. A. H
OUSTON
,
38
E. J. H
OWELL
,
52
Y. M. H
U
,
10
S. H
UANG
,
74
E. A. H
UERTA
,
103
D. H
UET
,
25
B. H
UGHEY
,
98
S. H
USA
,
104
S. H. H
UTTNER
,
38
T. H
UYNH
-D
INH
,
7
N. I
NDIK
,
10
D. R. I
NGRAM
,
39
R. I
NTA
,
72
H. N. I
SA
,
38
J.-M. I
SAC
,
60
M. I
SI
,
1
T. I
SOGAI
,
12
B. R. I
YER
,
17
K. I
ZUMI
,
39
T. J
ACQMIN
,
60
H. J
ANG
,
79
K. J
ANI
,
65
P. J
ARANOWSKI
,
105
S. J
AWAHAR
,
106
L. J
IAN
,
52
F. J
IM
́
ENEZ
-F
ORTEZA
,
104
W. W. J
OHNSON
,
2
D. I. J
ONES
,
28
R. J
ONES
,
38
R. J. G. J
ONKER
,
11
L. J
U
,
52
H
ARIS
K,
107
C. V. K
ALAGHATGI
,
91
V. K
ALOGERA
,
83
S. K
ANDHASAMY
,
23
G. K
ANG
,
79
J. B. K
ANNER
,
1
S. J. K
APADIA
,
10
S. K
ARKI
,
59
K. S. K
ARVINEN
,
10
M. K
ASPRZACK
,
36,2
E. K
ATSAVOUNIDIS
,
12
W. K
ATZMAN
,
7
S. K
AUFER
,
19
T. K
AUR
,
52
K. K
AWABE
,
39
F. K
́
EF
́
ELIAN
,
54
M. S. K
EHL
,
108
D. K
EITEL
,
104
D. B. K
ELLEY
,
37
W. K
ELLS
,
1
R. K
ENNEDY
,
87
J. S. K
EY
,
88
F. Y. K
HALILI
,
50
I. K
HAN
,
14
S. K
HAN
,
91
Z. K
HAN
,
86
E. A. K
HAZANOV
,
109
N. K
IJBUNCHOO
,
39
C
HI
-W
OONG
K
IM
,
79
C
HUNGLEE
K
IM
,
79
J. K
IM
,
110
K. K
IM
,
111
N. K
IM
,
42
W. K
IM
,
112
Y.-M. K
IM
,
110
S. J. K
IMBRELL
,
65
E. J. K
ING
,
112
P. J. K
ING
,
39
J. S. K
ISSEL
,
39
B. K
LEIN
,
83
L. K
LEYBOLTE
,
29
S. K
LIMENKO
,
6
S. M. K
OEHLENBECK
,
10
S. K
OLEY
,
11
V. K
ONDRASHOV
,
1
A. K
ONTOS
,
12
M. K
OROBKO
,
29
W. Z. K
ORTH
,
1
I. K
OWALSKA
,
62
D. B. K
OZAK
,
1
V. K
RINGEL
,
10
B. K
RISHNAN
,
10
A. K
R
́
OLAK
,
113,114
C. K
RUEGER
,
19
G. K
UEHN
,
10
P. K
UMAR
,
108
R. K
UMAR
,
86
L. K
UO
,
74
A. K
UTYNIA
,
113
B. D. L
ACKEY
,
37
M. L
ANDRY
,
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arXiv:1607.07456v1 [astro-ph.HE] 25 Jul 2016
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1
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32,71
C. H. L
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110
H. K. L
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91
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37
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14,15
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120
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12
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30
I. M
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120
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84
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1
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12
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80,30
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12
L. M
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12
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73
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11
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85
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18
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83
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6
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53,11
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128
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129
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129
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91
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104
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10
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J. O
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7
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EILLY
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7
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HAUGHNESSY
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102
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112
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72
A. P
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107
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49
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109
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30
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74
C. P
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83
F. P
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91
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49
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36
M. A. P
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31,18,10
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W. P
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7
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38
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36
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21
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38
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1
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A. P
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7
S. P
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131
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1
L. M. P
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83
M. P
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38
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80,30
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54
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57,58
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9
G. P
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36
L. P
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66
I. M. P
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9
M. P
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38
M. P
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18
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20,21
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36
A. P
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10
J. P
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38
J. P
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16
V. P
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91
T. P
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84
L. R. P
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1
M. P
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10,36
M. P
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9
S. P
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31
R. P
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10
G. A. P
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89,90
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50
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10
M. P
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35
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30
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31
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18
J. Q
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52
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115
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88
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1
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59
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39
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22
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39
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93
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49
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49
M. R
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88
P. R
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80,30
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31
M. R
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20,21
V. R
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27
J. R
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24
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54
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48
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51
D. H. R
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1,6
H. R
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101
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102
N. A. R
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,
1,38
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38
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25
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15
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J. G. R
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123
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7
D. R
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38
A. R
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10
P. R
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36
K. R
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39
S. S
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1
T. S
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,
39
L. S
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,
18
M. S
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133
L. S
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36
M. S
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107
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10
A. S
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126
L. S
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115
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1
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39
B. S
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83
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37
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66
B. S. S
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91
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37
O. E. S. S
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101
R. L. S
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A. S
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19
P. S
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59
R. S
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10
J. S
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10
P. S
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1,78
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29
R. M. S. S
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59
A. S
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29
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10
D. S
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10,19
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91,31
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38
S. M. S
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22
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7
A. S. S
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96
D. S
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36
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27,15
A. S
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109
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53,11
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22
T. S
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39
M. S. S
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83
M. S
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10
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64
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18
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12
D. M. S
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18
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1
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69
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31,10,19
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2
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14
A. M. S
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104
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48
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86
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41
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10
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18
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88
K. A. S
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38
N. S
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66
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61
S. S
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50
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A. L. S
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7
T. Z. S
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L. S
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85
S. S
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86
P. J. S
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91
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M. J. S
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98
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59
D. B. T
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6
M. T
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97
S. P. T
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10
A. T
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31
R. T
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1
T. T
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10
M. P. T
HIRUGNANASAMBANDAM
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1
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7
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K. A. T
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K. T
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C. T
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C. V. T
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88
C. I. T
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1
D. T
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D. T
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23
M. C. T
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J.-P. Z
ENDRI
,
44
M. Z
EVIN
,
83
L. Z
HANG
,
1
M. Z
HANG
,
123
Y. Z
HANG
,
102
C. Z
HAO
,
52
M. Z
HOU
,
83
Z. Z
HOU
,
83
X. J. Z
HU
,
52
M. E. Z
UCKER
,
1,12
S. E. Z
URAW
,
119
AND
J. Z
WEIZIG
1
Deceased, March 2016.
Deceased, May 2015.
Deceased, March 2015.
(LIGO Scientific Collaboration and Virgo Collaboration)
(Dated: July 27, 2016)
3
1
LIGO, California Institute of Technology, Pasadena, CA 91125, USA
2
Louisiana State University, Baton Rouge, LA 70803, USA
3
American University, Washington, D.C. 20016, USA
4
Universit
`
a di Salerno, Fisciano, I-84084 Salerno, Italy
5
INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy
6
University of Florida, Gainesville, FL 32611, USA
7
LIGO Livingston Observatory, Livingston, LA 70754, USA
8
Laboratoire d’Annecy-le-Vieux de Physique des Particules (LAPP), Universit
́
e Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France
9
University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy
10
Albert-Einstein-Institut, Max-Planck-Institut f
̈
ur Gravitationsphysik, D-30167 Hannover, Germany
11
Nikhef, Science Park, 1098 XG Amsterdam, The Netherlands
12
LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
13
Instituto Nacional de Pesquisas Espaciais, 12227-010 S
̃
ao Jos
́
e dos Campos, S
̃
ao Paulo, Brazil
14
INFN, Gran Sasso Science Institute, I-67100 L’Aquila, Italy
15
INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy
16
Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India
17
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore 560012, India
18
University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA
19
Leibniz Universit
̈
at Hannover, D-30167 Hannover, Germany
20
Universit
`
a di Pisa, I-56127 Pisa, Italy
21
INFN, Sezione di Pisa, I-56127 Pisa, Italy
22
Australian National University, Canberra, Australian Capital Territory 0200, Australia
23
The University of Mississippi, University, MS 38677, USA
24
California State University Fullerton, Fullerton, CA 92831, USA
25
LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit
́
e Paris-Saclay, Orsay, France
26
Chennai Mathematical Institute, Chennai 603103, India
27
Universit
`
a di Roma Tor Vergata, I-00133 Roma, Italy
28
University of Southampton, Southampton SO17 1BJ, United Kingdom
29
Universit
̈
at Hamburg, D-22761 Hamburg, Germany
30
INFN, Sezione di Roma, I-00185 Roma, Italy
31
Albert-Einstein-Institut, Max-Planck-Institut f
̈
ur Gravitationsphysik, D-14476 Potsdam-Golm, Germany
32
APC, AstroParticule et Cosmologie, Universit
́
e Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cit
́
e, F-75205 Paris Cedex 13,
France
33
Montana State University, Bozeman, MT 59717, USA
34
Universit
`
a di Perugia, I-06123 Perugia, Italy
35
INFN, Sezione di Perugia, I-06123 Perugia, Italy
36
European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy
37
Syracuse University, Syracuse, NY 13244, USA
38
SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom
39
LIGO Hanford Observatory, Richland, WA 99352, USA
40
Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Mikl
́
os
́
ut 29-33, Hungary
41
Columbia University, New York, NY 10027, USA
42
Stanford University, Stanford, CA 94305, USA
43
Universit
`
a di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy
44
INFN, Sezione di Padova, I-35131 Padova, Italy
45
CAMK-PAN, 00-716 Warsaw, Poland
46
University of Birmingham, Birmingham B15 2TT, United Kingdom
47
Universit
`
a degli Studi di Genova, I-16146 Genova, Italy
48
INFN, Sezione di Genova, I-16146 Genova, Italy
49
RRCAT, Indore MP 452013, India
50
Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia
4
51
SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom
52
University of Western Australia, Crawley, Western Australia 6009, Australia
53
Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands
54
Artemis, Universit
́
e C
ˆ
ote d’Azur, CNRS, Observatoire C
ˆ
ote d’Azur, CS 34229, Nice cedex 4, France
55
Institut de Physique de Rennes, CNRS, Universit
́
e de Rennes 1, F-35042 Rennes, France
56
Washington State University, Pullman, WA 99164, USA
57
Universit
`
a degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy
58
INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy
59
University of Oregon, Eugene, OR 97403, USA
60
Laboratoire Kastler Brossel, UPMC-Sorbonne Universit
́
es, CNRS, ENS-PSL Research University, Coll
`
ege de France, F-75005 Paris, France
61
Carleton College, Northfield, MN 55057, USA
62
Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland
63
VU University Amsterdam, 1081 HV Amsterdam, The Netherlands
64
University of Maryland, College Park, MD 20742, USA
65
Center for Relativistic Astrophysics and School of Physics, Georgia Institute of Technology, Atlanta, GA 30332, USA
66
Laboratoire des Mat
́
eriaux Avanc
́
es (LMA), CNRS/IN2P3, F-69622 Villeurbanne, France
67
Universit
́
e Claude Bernard Lyon 1, F-69622 Villeurbanne, France
68
Universit
`
a di Napoli “Federico II,” Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy
69
NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
70
RESCEU, University of Tokyo, Tokyo, 113-0033, Japan.
71
Tsinghua University, Beijing 100084, China
72
Texas Tech University, Lubbock, TX 79409, USA
73
The Pennsylvania State University, University Park, PA 16802, USA
74
National Tsing Hua University, Hsinchu City, 30013 Taiwan, Republic of China
75
Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia
76
West Virginia University, Morgantown, WV 26506, USA
77
University of Chicago, Chicago, IL 60637, USA
78
Caltech CaRT, Pasadena, CA 91125, USA
79
Korea Institute of Science and Technology Information, Daejeon 305-806, Korea
80
Universit
`
a di Roma “La Sapienza,” I-00185 Roma, Italy
81
University of Brussels, Brussels 1050, Belgium
82
Sonoma State University, Rohnert Park, CA 94928, USA
83
Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL 60208, USA
84
University of Minnesota, Minneapolis, MN 55455, USA
85
The University of Melbourne, Parkville, Victoria 3010, Australia
86
Institute for Plasma Research, Bhat, Gandhinagar 382428, India
87
The University of Sheffield, Sheffield S10 2TN, United Kingdom
88
The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA
89
Universit
`
a di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy
90
INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy
91
Cardiff University, Cardiff CF24 3AA, United Kingdom
92
Montclair State University, Montclair, NJ 07043, USA
93
MTA E
̈
otv
̈
os University, “Lendulet” Astrophysics Research Group, Budapest 1117, Hungary
94
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
95
School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom
96
Indian Institute of Technology, Gandhinagar Ahmedabad Gujarat 382424, India
97
University of Szeged, D
́
om t
́
er 9, Szeged 6720, Hungary
98
Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA
99
Tata Institute of Fundamental Research, Mumbai 400005, India
100
INAF, Osservatorio Astronomico di Capodimonte, I-80131, Napoli, Italy
101
University of Michigan, Ann Arbor, MI 48109, USA
5
102
Rochester Institute of Technology, Rochester, NY 14623, USA
103
NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
104
Universitat de les Illes Balears, IAC3—IEEC, E-07122 Palma de Mallorca, Spain
105
University of Białystok, 15-424 Białystok, Poland
106
SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom
107
IISER-TVM, CET Campus, Trivandrum Kerala 695016, India
108
Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada
109
Institute of Applied Physics, Nizhny Novgorod, 603950, Russia
110
Pusan National University, Busan 609-735, Korea
111
Hanyang University, Seoul 133-791, Korea
112
University of Adelaide, Adelaide, South Australia 5005, Australia
113
NCBJ, 05-400
́
Swierk-Otwock, Poland
114
IM-PAN, 00-956 Warsaw, Poland
115
Monash University, Victoria 3800, Australia
116
Seoul National University, Seoul 151-742, Korea
117
The Chinese University of Hong Kong, Shatin, NT, Hong Kong
118
University of Alabama in Huntsville, Huntsville, AL 35899, USA
119
University of Massachusetts-Amherst, Amherst, MA 01003, USA
120
ESPCI, CNRS, F-75005 Paris, France
121
Universit
`
a di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy
122
Southern University and A&M College, Baton Rouge, LA 70813, USA
123
College of William and Mary, Williamsburg, VA 23187, USA
124
Instituto de F
́
ısica Te
́
orica, University Estadual Paulista/ICTP South American Institute for Fundamental Research, S
̃
ao Paulo SP 01140-070, Brazil
125
University of Cambridge, Cambridge CB2 1TN, United Kingdom
126
IISER-Kolkata, Mohanpur, West Bengal 741252, India
127
Rutherford Appleton Laboratory, HSIC, Chilton, Didcot, Oxon OX11 0QX, United Kingdom
128
Whitman College, 345 Boyer Avenue, Walla Walla, WA 99362 USA
129
National Institute for Mathematical Sciences, Daejeon 305-390, Korea
130
Universit
́
e de Lyon, F-69361 Lyon, France
131
Hobart and William Smith Colleges, Geneva, NY 14456, USA
132
Janusz Gil Institute of Astronomy, University of Zielona G
́
ora, 65-265 Zielona G
́
ora, Poland
133
King’s College London, University of London, London WC2R 2LS, United Kingdom
134
Andrews University, Berrien Springs, MI 49104, USA
135
Universit
`
a di Siena, I-53100 Siena, Italy
136
Trinity University, San Antonio, TX 78212, USA
137
University of Washington, Seattle, WA 98195, USA
138
Kenyon College, Gambier, OH 43022, USA
139
Abilene Christian University, Abilene, TX 79699, USA
ABSTRACT
We report here the non-detection of gravitational waves from the merger of binary neutron star systems and
neutron-star–black-hole systems during the first observing run of Advanced LIGO. In particular we searched for
gravitational wave signals from binary neutron star systems with component masses
[
1
,
3
]
M
and component
dimensionless spins
<
0
.
05. We also searched for neutron-star–black-hole systems with the same neutron star
parameters, black hole mass
[
2
,
99
]
M
and no restriction on the black hole spin magnitude. We assess the
sensitivity of the two LIGO detectors to these systems, and find that they could have detected the merger of
binary neutron star systems with component mass distributions of 1
.
35
±
0
.
13
M
at a volume-weighted average
distance of
70 Mpc, and for neutron-star–black-hole systems with neutron star masses of 1
.
4
M
and black
hole masses of at least 5
M
, a volume-weighted average distance of at least
110 Mpc. From this we constrain
with 90% confidence the merger rate to be less than 12,600 Gpc
3
yr
1
for binary-neutron star systems and
less than 3,600 Gpc
3
yr
1
for neutron-star–black-hole systems. We discuss the astrophysical implications
of these results, which we find to be in tension with only the most optimistic predictions. However, we find
6
that if no detection of neutron-star binary mergers is made in the next two Advanced LIGO and Advanced
Virgo observing runs we would place significant constraints on the merger rates. Finally, assuming a rate
of 10
+
20
7
Gpc
3
yr
1
short gamma ray bursts beamed towards the Earth and assuming that all short gamma-
ray bursts have binary-neutron-star (neutron-star–black-hole) progenitors we can use our 90% confidence rate
upper limits to constrain the beaming angle of the gamma-ray burst to be greater than 2
.
3
+
1
.
7
1
.
1
(4
.
3
+
3
.
1
1
.
9
).
1.
INTRODUCTION
Between September 12, 2015 and January 19, 2016 the
two advanced Laser Interferometer Gravitational Wave Ob-
servatory (LIGO) detectors conducted their first observing
period (O1). During O1, two high-mass binary black-hole
(BBH) events were identified with high confidence (
>
5
σ
):
GW150914 (Abbott
et al.
2016a) and GW151226 (Abbott
et al.
2016b). A third signal, LVT151012, was also identi-
fied with 1
.
7
σ
confidence (Abbott
et al.
2016c,d) In all three
cases the component masses are confidently constrained to be
above the 3
.
2
M
upper mass limit of neutron-stars (NSs) set
by theoretical considerations (Rhoades and Ruffini 1974; Ab-
bott
et al.
2016e). The details of these observations, investiga-
tions about the properties of the observed BBH mergers, and
the astrophysical implications are explored in (Abbott
et al.
2016e,f,g,h,c,i).
The search methods that successfully observed these BBH
mergers also target other types of compact binary coales-
cences, specifically the inspiral and merger of binary neutron-
star (BNS) systems and neutron-star–black-hole (NSBH) sys-
tems. Such systems were considered among the most promis-
ing candidates for an observation in O1. For example, a sim-
ple calculation prior to the start of O1 predicted 0.0005 - 4
detections of BNS signals during O1 (Aasi
et al.
2016).
In this paper we report on the search for BNS and NSBH
mergers in O1. We have searched for BNS systems with com-
ponent masses
[
1
,
3
]
M
, component dimensionless spins
<
0
.
05 and spin orientations aligned or anti-aligned with the
orbital angular momentum. We have searched for NSBH
systems with neutron star mass
[
1
,
3
]
M
, black-hole (BH)
mass
[
2
,
99
]
M
neutron star dimensionless spin magnitude
<
0
.
05, BH dimensionless spin magnitude
<
0
.
99 and both
spins aligned or anti-aligned with the orbital angular momen-
tum. No observation of either BNS or NSBH mergers was
made in O1. We explore the astrophysical implications of this
result, placing upper limits on the rates of such merger events
in the local Universe that are roughly an order of magnitude
smaller than those obtained with data from Initial LIGO and
Initial Virgo (Abbott
et al.
2009; Acernese
et al.
2008; Abadie
et al.
2012a). We compare these updated rate limits to current
predictions of BNS and NSBH merger rates and explore how
the non-detection of BNS and NSBH systems in O1 can be
used to explore possible constraints of the opening angle of
the radiation cone of short gamma-ray bursts (GRBs), assum-
ing that short GRB progenitors are BNS or NSBH mergers.
The layout of this paper is as follows. In
§
2 we describe the
motivation for our search parameter space. In
§
3 we briefly
describe the search methodology, then describe the results of
the search in
§
4. We then discuss the constraints that can
be placed on the rates of BNS and NSBH mergers in
§
5 and
the astrophysical implications of the rates in
§
6. Finally, we
conclude in
§
7.
2.
SOURCE CONSIDERATIONS
There are currently thousands of known NSs, most de-
tected as pulsars (Hobbs
et al.
; Manchester
et al.
2005). Of
these,
70 are found in binary systems and allow estimates
of the NS mass (Ott
et al.
; Lattimer 2012; Ozel and Freire
2016). Published mass estimates range from 1
.
0
±
0
.
17
M
(Falanga
et al.
2015) to 2
.
74
±
0
.
21
M
(Freire
et al.
2008)
although there is some uncertainty in some of these measure-
ments. Considering only precise mass measurements from
these observations one can set a lower bound on the max-
imum possible neutron star mass of 2
.
01
±
0
.
04
M
(Anto-
niadis
et al.
2013) and theoretical considerations set an up-
per bound on the maximum possible neutron star mass of
2
.
9–3
.
2
M
(Rhoades and Ruffini 1974; Kalogera and Baym
1996). The standard formation scenario of core-collapse su-
pernovae restricts the birth masses of neutron stars to be above
1
.
1–1
.
6
M
(Ozel
et al.
2012; Lattimer 2012; Kiziltan
et al.
2013).
Eight candidate BNS systems allow mass measurements
for individual components, giving a much narrower mass
distribution (Lorimer 2008). Masses are reported between
1
.
0
M
and 1
.
49
M
(Ott
et al.
; Ozel and Freire 2016), and
are consistent with an underlying mass distribution of
(
1
.
35
±
0
.
13
)
M
(Kiziltan
et al.
2010). These observational measure-
ments assume masses are greater than 0
.
9
M
.
The fastest spinning pulsar observed so far rotates with a
frequency of 716 Hz (Hessels
et al.
2006). This corresponds
to a dimensionless spin
χ
=
c
|
S
|
/
Gm
2
of roughly 0.4, where
m
is the object’s mass and
S
is the angular momentum.
1
Such
rapid rotation rates likely require the NS to have been spun up
through mass-transfer from its companion. The fastest spin-
ning pulsar in a confirmed BNS system has a spin frequency
of 44 Hz (Kramer and Wex 2009), implying that dimension-
less spins for NS in BNS systems are
0
.
04 (Brown
et al.
2012). However, recycled NS can have larger spins, and the
potential BNS pulsar J1807-2500B (Lynch
et al.
2012) has a
spin of 4.19 ms, giving a dimensionless spin of up to
0
.
2.
2
1
Assuming a mass of 1
.
4
M
and a moment of inertia
=
J
/
of 1
.
5
×
10
45
g cm
2
; the exact moment of inertia is dependent on the unknown NS
equation-of-state (Lattimer 2012).
2
Calculated with a pulsar mass of 1
.
37
M
and a high moment of inertia,
2
×
10
45
g cm
2
.