Search for intermediate mass black hole binaries in the first and second observing runs of the Advanced LIGO and Virgo network

(1)

DRAFT-V16

runs of the Advanced LIGO and Virgo network

B. P. Abbott,1 _{R. Abbott,}1_{T. D. Abbott,}2 _{S. Abraham,}3_{F. Acernese,}4, 5 _{K. Ackley,}6 _{A. Adams,}7 _{C. Adams,}8

R. X. Adhikari,1 _{V. B. Adya,}9 _{C. Affeldt,}10, 11 _{M. Agathos,}12, 13 _{K. Agatsuma,}14 _{N. Aggarwal,}15 _{O. D. Aguiar,}16

L. Aiello,17, 18 _{A. Ain,}3_{P. Ajith,}19_{G. Allen,}20 _{A. Allocca,}21, 22 _{M. A. Aloy,}23 _{P. A. Altin,}9 _{A. Amato,}24 _{S. Anand,}1

A. Ananyeva,1 _{S. B. Anderson,}1 _{W. G. Anderson,}25 _{S. V. Angelova,}26 _{S. Antier,}27 _{S. Appert,}1 _{K. Arai,}1

M. C. Araya,1 _{J. S. Areeda,}28 _{M. Ar`ene,}27 _{N. Arnaud,}29, 30 _{S. M. Aronson,}31 _{K. G. Arun,}32_{S. Ascenzi,}17, 33

G. Ashton,6 _{S. M. Aston,}8 _{P. Astone,}34_{F. Aubin,}35 _{P. Aufmuth,}11_{K. AultONeal,}36 _{C. Austin,}2_{V. Avendano,}37

A. Avila-Alvarez,28_{S. Babak,}27_{P. Bacon,}27_{F. Badaracco,}17, 18_{M. K. M. Bader,}38_{S. Bae,}39_{A. M. Baer,}7 _{J. Baird,}27

P. T. Baker,40 _{F. Baldaccini,}41, 42 _{G. Ballardin,}30 _{S. W. Ballmer,}43 _{A. Bals,}36_{S. Banagiri,}44 _{J. C. Barayoga,}1

C. Barbieri,45, 46 _{S. E. Barclay,}47 _{B. C. Barish,}1 _{D. Barker,}48 _{K. Barkett,}49_{S. Barnum,}15 _{F. Barone,}50, 5 _{B. Barr,}47

L. Barsotti,15_{M. Barsuglia,}27 _{D. Barta,}51 _{J. Bartlett,}48 _{I. Bartos,}31_{R. Bassiri,}52 _{A. Basti,}21, 22 _{M. Bawaj,}53, 42

J. C. Bayley,47 _{M. Bazzan,}54, 55 _{B. B´ecsy,}56 _{M. Bejger,}27, 57 _{I. Belahcene,}29 _{A. S. Bell,}47 _{D. Beniwal,}58

M. G. Benjamin,36 _{B. K. Berger,}52 _{G. Bergmann,}10, 11 _{S. Bernuzzi,}12 _{C. P. L. Berry,}59 _{D. Bersanetti,}60

A. Bertolini,38 _{J. Betzwieser,}8 _{R. Bhandare,}61 _{J. Bidler,}28 _{E. Biggs,}25_{I. A. Bilenko,}62_{S. A. Bilgili,}40_{G. Billingsley,}1

R. Birney,26 _{O. Birnholtz,}63 _{S. Biscans,}1, 15 _{M. Bischi,}64, 65 _{S. Biscoveanu,}15 _{A. Bisht,}11 _{M. Bitossi,}30, 22

M. A. Bizouard,66 _{J. K. Blackburn,}1 _{J. Blackman,}49 _{C. D. Blair,}8 _{D. G. Blair,}67 _{R. M. Blair,}48_{S. Bloemen,}68

F. Bobba,69, 70 _{N. Bode,}10, 11 _{M. Boer,}66 _{Y. Boetzel,}71_{G. Bogaert,}66 _{F. Bondu,}72 _{R. Bonnand,}35 _{P. Booker,}10, 11

B. A. Boom,38 _{R. Bork,}1 _{V. Boschi,}30 _{S. Bose,}3 _{V. Bossilkov,}67 _{J. Bosveld,}67_{Y. Bouffanais,}54, 55 _{A. Bozzi,}30

C. Bradaschia,22 _{P. R. Brady,}25 _{A. Bramley,}8 _{M. Branchesi,}17, 18 _{J. E. Brau,}73 _{M. Breschi,}12 _{T. Briant,}74

J. H. Briggs,47 _{F. Brighenti,}64, 65 _{A. Brillet,}66 _{M. Brinkmann,}10, 11 _{P. Brockill,}25 _{A. F. Brooks,}1 _{J. Brooks,}30

D. D. Brown,58 _{S. Brunett,}1 _{A. Buikema,}15 _{T. Bulik,}75 _{H. J. Bulten,}76, 38 _{A. Buonanno,}77, 78 _{D. Buskulic,}35

C. Buy,27 _{R. L. Byer,}52 _{M. Cabero,}10, 11 _{L. Cadonati,}79 _{G. Cagnoli,}80 _{C. Cahillane,}1 _{J. Calder´on Bustillo,}6

T. A. Callister,1 _{E. Calloni,}81, 5 _{J. B. Camp,}82_{W. A. Campbell,}6_{M. Canepa,}83, 60 _{K. C. Cannon,}84 _{H. Cao,}58

J. Cao,85 _{G. Carapella,}69, 70 _{F. Carbognani,}30 _{S. Caride,}86_{M. F. Carney,}59 _{G. Carullo,}21, 22 _{J. Casanueva Diaz,}22

C. Casentini,87, 33 _{S. Caudill,}38_{M. Cavagli`}_a,88, 89 _{F. Cavalier,}29 _{R. Cavalieri,}30 _{G. Cella,}22 _{P. Cerd´a-Dur´an,}23

E. Cesarini,90, 33 _{O. Chaibi,}66 _{K. Chakravarti,}3 _{S. J. Chamberlin,}91 _{M. Chan,}47 _{S. Chao,}92 _{P. Charlton,}93

E. A. Chase,59_{E. Chassande-Mottin,}27 _{D. Chatterjee,}25 _{M. Chaturvedi,}61 _{K. Chatziioannou,}94 _{B. D. Cheeseboro,}40

H. Y. Chen,95 _{X. Chen,}67 _{Y. Chen,}49 _{H.-P. Cheng,}31 _{C. K. Cheong,}96 _{H. Y. Chia,}31 _{F. Chiadini,}97, 70

A. Chincarini,60 _{A. Chiummo,}30 _{G. Cho,}98 _{H. S. Cho,}99_{M. Cho,}78 _{N. Christensen,}100, 66 _{Q. Chu,}67 _{S. Chua,}74

K. W. Chung,96 _{S. Chung,}67 _{G. Ciani,}54, 55 _{M. Cie´slar,}57 _{A. A. Ciobanu,}58 _{R. Ciolfi,}101, 55 _{F. Cipriano,}66

A. Cirone,83, 60 _{F. Clara,}48_{J. A. Clark,}79 _{P. Clearwater,}102_{F. Cleva,}66 _{E. Coccia,}17, 18 _{P.-F. Cohadon,}74_{D. Cohen,}29

M. Colleoni,103 _{C. G. Collette,}104 _{C. Collins,}14 _{M. Colpi,}45, 46 _{L. R. Cominsky,}105 _{M. Constancio Jr.,}16 _{L. Conti,}55

S. J. Cooper,14_{P. Corban,}8 _{T. R. Corbitt,}2 _{I. Cordero-Carri´on,}106 _{S. Corezzi,}41, 42 _{K. R. Corley,}107_{N. Cornish,}56

D. Corre,29 _{A. Corsi,}86 _{S. Cortese,}30 _{C. A. Costa,}16 _{R. Cotesta,}77 _{M. W. Coughlin,}1 _{S. B. Coughlin,}108, 59

J.-P. Coulon,66 _{S. T. Countryman,}107 _{P. Couvares,}1 _{P. B. Covas,}103_{E. E. Cowan,}79_{D. M. Coward,}67 _{M. J. Cowart,}8

D. C. Coyne,1 _{R. Coyne,}109_{J. D. E. Creighton,}25_{T. D. Creighton,}110 _{J. Cripe,}2 _{M. Croquette,}74 _{S. G. Crowder,}111

T. J. Cullen,2 _{A. Cumming,}47 _{L. Cunningham,}47 _{E. Cuoco,}30 _{T. Dal Canton,}82 _{G. D´alya,}112 _{B. D’Angelo,}83, 60

S. L. Danilishin,10, 11 _{S. D’Antonio,}33 _{K. Danzmann,}11, 10 _{A. Dasgupta,}113 _{C. F. Da Silva Costa,}31

L. E. H. Datrier,47 _{V. Dattilo,}30 _{I. Dave,}61 _{M. Davier,}29 _{D. Davis,}43 _{E. J. Daw,}114 _{D. DeBra,}52_{M. Deenadayalan,}3

J. Degallaix,24 _{M. De Laurentis,}81, 5 _{S. Del´eglise,}74 _{W. Del Pozzo,}21, 22 _{L. M. DeMarchi,}59 _{N. Demos,}15

T. Dent,115 _{R. De Pietri,}116, 117 _{R. De Rosa,}81, 5 _{C. De Rossi,}24, 30 _{R. DeSalvo,}118 _{O. de Varona,}10, 11

S. Dhurandhar,3 _{M. C. D´ıaz,}110 _{T. Dietrich,}38 _{L. Di Fiore,}5 _{C. DiFronzo,}14 _{C. Di Giorgio,}69, 70 _{F. Di Giovanni,}23

M. Di Giovanni,119, 120 _{T. Di Girolamo,}81, 5 _{A. Di Lieto,}21, 22 _{B. Ding,}104_{S. Di Pace,}121, 34 _{I. Di Palma,}121, 34

F. Di Renzo,21, 22 _{A. K. Divakarla,}31 _{A. Dmitriev,}14_{Z. Doctor,}95 _{F. Donovan,}15 _{K. L. Dooley,}108, 88 _{S. Doravari,}3

I. Dorrington,108 _{T. P. Downes,}25 _{M. Drago,}17, 18 _{J. C. Driggers,}48 _{Z. Du,}85 _{J.-G. Ducoin,}29 _{P. Dupej,}47

O. Durante,69, 70 _{S. E. Dwyer,}48 _{P. J. Easter,}6 _{G. Eddolls,}47 _{T. B. Edo,}114 _{A. Effler,}8 _{P. Ehrens,}1 _{J. Eichholz,}9

S. S. Eikenberry,31 _{M. Eisenmann,}35 _{R. A. Eisenstein,}15_{L. Errico,}81, 5 _{R. C. Essick,}95_{H. Estelles,}103 _{D. Estevez,}35

Z. B. Etienne,40_{T. Etzel,}1 _{M. Evans,}15 _{T. M. Evans,}8 _{V. Fafone,}87, 33, 17 _{S. Fairhurst,}108 _{X. Fan,}85_{S. Farinon,}60

B. Farr,73_{W. M. Farr,}14 _{E. J. Fauchon-Jones,}108 _{M. Favata,}37 _{M. Fays,}114 _{M. Fazio,}122 _{C. Fee,}123 _{J. Feicht,}1

M. M. Fejer,52 _{F. Feng,}27 _{D. L. Ferguson,}79 _{A. Fernandez-Galiana,}15 _{I. Ferrante,}21, 22 _{E. C. Ferreira,}16

(2)

DRAFT-V16

R. Fittipaldi,124, 70 _{M. Fitz-Axen,}44 _{V. Fiumara,}125, 70 _{R. Flaminio,}35, 126 _{M. Fletcher,}47 _{E. Floden,}44 _{E. Flynn,}28

H. Fong,84 _{J. A. Font,}23, 127 _{P. W. F. Forsyth,}9 _{J.-D. Fournier,}66 _{Francisco Hernandez Vivanco,}6 _{S. Frasca,}121, 34

F. Frasconi,22_{Z. Frei,}112 _{A. Freise,}14 _{R. Frey,}73 _{V. Frey,}29 _{P. Fritschel,}15_{V. V. Frolov,}8 _{G. Fronz`e,}128_{P. Fulda,}31

M. Fyffe,8 _{H. A. Gabbard,}47 _{B. U. Gadre,}77 _{S. M. Gaebel,}14 _{J. R. Gair,}129_{L. Gammaitoni,}41_{S. G. Gaonkar,}3

C. Garc´ıa-Quir´os,103 _{F. Garufi,}81, 5 _{B. Gateley,}48 _{S. Gaudio,}36 _{G. Gaur,}130_{V. Gayathri,}131_{G. Gemme,}60_{E. Genin,}30

A. Gennai,22 _{D. George,}20 _{J. George,}61 _{L. Gergely,}132 _{S. Ghonge,}79 _{Abhirup Ghosh,}77 _{Archisman Ghosh,}38

S. Ghosh,25 _{B. Giacomazzo,}119, 120 _{J. A. Giaime,}2, 8 _{K. D. Giardina,}8 _{D. R. Gibson,}133_{K. Gill,}107_{L. Glover,}134

J. Gniesmer,135 _{P. Godwin,}91 _{E. Goetz,}48 _{R. Goetz,}31 _{B. Goncharov,}6 _{G. Gonz´}_alez,2 _{J. M. Gonzalez Castro,}21, 22

A. Gopakumar,136 _{S. E. Gossan,}1 _{M. Gosselin,}30, 21, 22 _{R. Gouaty,}35 _{B. Grace,}9 _{A. Grado,}137, 5 _{M. Granata,}24

A. Grant,47 _{S. Gras,}15 _{P. Grassia,}1 _{C. Gray,}48 _{R. Gray,}47 _{G. Greco,}64, 65 _{A. C. Green,}31 _{R. Green,}108

E. M. Gretarsson,36 _{A. Grimaldi,}119, 120 _{S. J. Grimm,}17, 18 _{P. Groot,}68_{H. Grote,}108 _{S. Grunewald,}77 _{P. Gruning,}29

G. M. Guidi,64, 65 _{H. K. Gulati,}113 _{Y. Guo,}38 _{A. Gupta,}91 _{Anchal Gupta,}1 _{P. Gupta,}38 _{E. K. Gustafson,}1

R. Gustafson,138_{L. Haegel,}103 _{O. Halim,}18, 17 _{B. R. Hall,}139 _{E. D. Hall,}15 _{E. Z. Hamilton,}108 _{G. Hammond,}47

M. Haney,71 _{M. M. Hanke,}10, 11 _{J. Hanks,}48_{C. Hanna,}91 _{M. D. Hannam,}108 _{O. A. Hannuksela,}96 _{T. J. Hansen,}36

J. Hanson,8_{T. Harder,}66 _{T. Hardwick,}2_{K. Haris,}19_{J. Harms,}17, 18 _{G. M. Harry,}140_{I. W. Harry,}141_{R. K. Hasskew,}8

C. J. Haster,15 _{K. Haughian,}47 _{F. J. Hayes,}47 _{J. Healy,}63 _{A. Heidmann,}74 _{M. C. Heintze,}8 _{H. Heitmann,}66

F. Hellman,142 _{P. Hello,}29 _{G. Hemming,}30 _{M. Hendry,}47 _{I. S. Heng,}47 _{J. Hennig,}10, 11 _{M. Heurs,}10, 11 _{S. Hild,}47

T. Hinderer,143, 38, 144 _{S. Hochheim,}10, 11 _{D. Hofman,}24_{A. M. Holgado,}20_{N. A. Holland,}9 _{K. Holt,}8 _{D. E. Holz,}95

P. Hopkins,108_{C. Horst,}25_{J. Hough,}47 _{E. J. Howell,}67 _{C. G. Hoy,}108 _{Y. Huang,}15 _{M. T. H¨}_ubner,6 _{E. A. Huerta,}20

D. Huet,29 _{B. Hughey,}36 _{V. Hui,}35_{S. Husa,}103 _{S. H. Huttner,}47 _{T. Huynh-Dinh,}8 _{B. Idzkowski,}75 _{A. Iess,}87, 33

H. Inchauspe,31_{C. Ingram,}58 _{R. Inta,}86_{G. Intini,}121, 34 _{B. Irwin,}123 _{H. N. Isa,}47_{J.-M. Isac,}74_{M. Isi,}15_{B. R. Iyer,}19

T. Jacqmin,74 _{S. J. Jadhav,}145 _{K. Jani,}79 _{N. N. Janthalur,}145 _{P. Jaranowski,}146 _{D. Jariwala,}31 _{A. C. Jenkins,}147

J. Jiang,31 _{G. R. Johns,}7 _{D. S. Johnson,}20 _{A. W. Jones,}14 _{D. I. Jones,}148 _{J. D. Jones,}48 _{R. Jones,}47

R. J. G. Jonker,38 _{L. Ju,}67 _{J. Junker,}10, 11 _{C. V. Kalaghatgi,}108 _{V. Kalogera,}59 _{B. Kamai,}1 _{S. Kandhasamy,}3

G. Kang,39 _{J. B. Kanner,}1 _{S. J. Kapadia,}25 _{S. Karki,}73 _{R. Kashyap,}19 _{M. Kasprzack,}1 _{S. Katsanevas,}30

E. Katsavounidis,15 _{W. Katzman,}8 _{S. Kaufer,}11_{K. Kawabe,}48 _{N. V. Keerthana,}3 _{F. K´ef´elian,}66_{D. Keitel,}141

R. Kennedy,114 _{J. S. Key,}149 _{F. Y. Khalili,}62_{B. Khamesra,}79 _{I. Khan,}17, 33 _{S. Khan,}10, 11 _{E. A. Khazanov,}150

N. Khetan,17, 18 _{M. Khursheed,}61_{N. Kijbunchoo,}9 _{Chunglee Kim,}151 _{G. J. Kim,}79 _{J. C. Kim,}152_{K. Kim,}96

W. Kim,58 _{W. S. Kim,}153 _{Y.-M. Kim,}154 _{C. Kimball,}59 _{P. J. King,}48 _{M. Kinley-Hanlon,}47 _{R. Kirchhoff,}10, 11

J. S. Kissel,48_{L. Kleybolte,}135_{J. H. Klika,}25_{S. Klimenko,}31 _{T. D. Knowles,}40_{P. Koch,}10, 11 _{S. M. Koehlenbeck,}10, 11

G. Koekoek,38, 155 _{S. Koley,}38 _{V. Kondrashov,}1 _{A. Kontos,}156 _{N. Koper,}10, 11 _{M. Korobko,}135 _{W. Z. Korth,}1

M. Kovalam,67_{D. B. Kozak,}1 _{C. Kr¨amer,}10, 11 _{V. Kringel,}10, 11 _{N. Krishnendu,}32_{A. Kr´olak,}157, 158 _{N. Krupinski,}25

G. Kuehn,10, 11 _{A. Kumar,}145 _{P. Kumar,}159 _{Rahul Kumar,}48 _{Rakesh Kumar,}113 _{L. Kuo,}92 _{A. Kutynia,}157

S. Kwang,25 _{B. D. Lackey,}77 _{D. Laghi,}21, 22 _{P. Laguna,}79 _{K. H. Lai,}96 _{T. L. Lam,}96 _{M. Landry,}48 _{B. B. Lane,}15

R. N. Lang,160 _{J. Lange,}63 _{B. Lantz,}52 _{R. K. Lanza,}15 _{A. Lartaux-Vollard,}29 _{P. D. Lasky,}6 _{M. Laxen,}8

A. Lazzarini,1 _{C. Lazzaro,}55 _{P. Leaci,}121, 34 _{S. Leavey,}10, 11 _{Y. K. Lecoeuche,}48 _{C. H. Lee,}99 _{H. K. Lee,}161

H. M. Lee,162 _{H. W. Lee,}152 _{J. Lee,}98 _{K. Lee,}47 _{J. Lehmann,}10, 11 _{A. K. Lenon,}40 _{N. Leroy,}29 _{N. Letendre,}35

Y. Levin,6 _{A. Li,}96 _{J. Li,}85 _{K. J. L. Li,}96 _{T. G. F. Li,}96 _{X. Li,}49 _{F. Lin,}6 _{F. Linde,}163, 38 _{S. D. Linker,}134

T. B. Littenberg,164 _{J. Liu,}67 _{X. Liu,}25 _{M. Llorens-Monteagudo,}23_{R. K. L. Lo,}96, 1 _{L. T. London,}15 _{A. Longo,}165, 166

M. Lorenzini,17, 18 _{V. Loriette,}167 _{M. Lormand,}8 _{G. Losurdo,}22_{J. D. Lough,}10, 11 _{C. O. Lousto,}63_{G. Lovelace,}28

M. E. Lower,168 _{H. L¨}_uck,11, 10 _{D. Lumaca,}87, 33 _{A. P. Lundgren,}141_{R. Lynch,}15_{Y. Ma,}49 _{R. Macas,}108 _{S. Macfoy,}26

M. MacInnis,15 _{D. M. Macleod,}108 _{A. Macquet,}66 _{I. Maga˜}_{na Hernandez,}25_{F. Maga˜}_na-Sandoval,31 _{R. M. Magee,}91

E. Majorana,34_{I. Maksimovic,}167_{A. Malik,}61 _{N. Man,}66 _{V. Mandic,}44 _{V. Mangano,}47, 121, 34 _{G. L. Mansell,}48, 15

M. Manske,25 _{M. Mantovani,}30 _{M. Mapelli,}54, 55 _{F. Marchesoni,}53, 42 _{F. Marion,}35_{S. M´arka,}107 _{Z. M´arka,}107

C. Markakis,20 _{A. S. Markosyan,}52_{A. Markowitz,}1 _{E. Maros,}1 _{A. Marquina,}106 _{S. Marsat,}27 _{F. Martelli,}64, 65

I. W. Martin,47_{R. M. Martin,}37_{V. Martinez,}80_{D. V. Martynov,}14 _{H. Masalehdan,}135 _{K. Mason,}15 _{E. Massera,}114

A. Masserot,35 _{T. J. Massinger,}1 _{M. Masso-Reid,}47 _{S. Mastrogiovanni,}27 _{A. Matas,}77 _{F. Matichard,}1, 15

L. Matone,107 _{N. Mavalvala,}15 _{J. J. McCann,}67 _{R. McCarthy,}48 _{D. E. McClelland,}9 _{S. McCormick,}8

L. McCuller,15 _{S. C. McGuire,}169 _{C. McIsaac,}141_{J. McIver,}1 _{D. J. McManus,}9 _{T. McRae,}9 _{S. T. McWilliams,}40

D. Meacher,25 _{G. D. Meadors,}6 _{M. Mehmet,}10, 11 _{A. K. Mehta,}19 _{J. Meidam,}38 _{E. Mejuto Villa,}118, 70

A. Melatos,102 _{G. Mendell,}48 _{R. A. Mercer,}25 _{L. Mereni,}24 _{K. Merfeld,}73 _{E. L. Merilh,}48 _{M. Merzougui,}66

S. Meshkov,1 _{C. Messenger,}47_{C. Messick,}91 _{F. Messina,}45, 46 _{R. Metzdorff,}74 _{P. M. Meyers,}102 _{F. Meylahn,}10, 11

(3)

DRAFT-V16

J. C. Mills,108 _{M. C. Milovich-Goff,}134 _{O. Minazzoli,}66, 170 _{Y. Minenkov,}33 _{A. Mishkin,}31 _{C. Mishra,}171

T. Mistry,114 _{S. Mitra,}3 _{V. P. Mitrofanov,}62 _{G. Mitselmakher,}31 _{R. Mittleman,}15 _{G. Mo,}100 _{D. Moffa,}123

K. Mogushi,88 _{S. R. P. Mohapatra,}15 _{M. Molina-Ruiz,}142 _{M. Mondin,}134 _{M. Montani,}64, 65 _{C. J. Moore,}14

D. Moraru,48 _{F. Morawski,}57_{G. Moreno,}48 _{S. Morisaki,}84 _{B. Mours,}35 _{C. M. Mow-Lowry,}14 _{F. Muciaccia,}121, 34

Arunava Mukherjee,10, 11 _{D. Mukherjee,}25 _{S. Mukherjee,}110 _{Subroto Mukherjee,}113 _{N. Mukund,}10, 11, 3_{A. Mullavey,}8

J. Munch,58 _{E. A. Mu˜}_niz,43 _{M. Muratore,}36 _{P. G. Murray,}47 _{A. Nagar,}90, 128, 172 _{I. Nardecchia,}87, 33

L. Naticchioni,121, 34 _{R. K. Nayak,}173 _{B. F. Neil,}67 _{J. Neilson,}118, 70 _{G. Nelemans,}68, 38 _{T. J. N. Nelson,}8

M. Nery,10, 11 _{A. Neunzert,}138 _{L. Nevin,}1 _{K. Y. Ng,}15 _{S. Ng,}58 _{C. Nguyen,}27 _{P. Nguyen,}73 _{D. Nichols,}143, 38

S. A. Nichols,2 _{S. Nissanke,}143, 38_{F. Nocera,}30 _{C. North,}108_{L. K. Nuttall,}141_{M. Obergaulinger,}23, 174 _{J. Oberling,}48

B. D. O’Brien,31 _{G. Oganesyan,}17, 18 _{G. H. Ogin,}175 _{J. J. Oh,}153 _{S. H. Oh,}153 _{F. Ohme,}10, 11 _{H. Ohta,}84

M. A. Okada,16_{M. Oliver,}103_{P. Oppermann,}10, 11_{Richard J. Oram,}8_{B. O’Reilly,}8_{R. G. Ormiston,}44_{L. F. Ortega,}31

R. O’Shaughnessy,63 _{S. Ossokine,}77 _{D. J. Ottaway,}58 _{H. Overmier,}8 _{B. J. Owen,}86_{A. E. Pace,}91 _{G. Pagano,}21, 22

M. A. Page,67 _{G. Pagliaroli,}17, 18 _{A. Pai,}131 _{S. A. Pai,}61 _{J. R. Palamos,}73 _{O. Palashov,}150_{C. Palomba,}34 _{H. Pan,}92

P. K. Panda,145 _{P. T. H. Pang,}96, 38 _{C. Pankow,}59 _{F. Pannarale,}121, 34 _{B. C. Pant,}61 _{F. Paoletti,}22 _{A. Paoli,}30

A. Parida,3_{W. Parker,}8, 169 _{D. Pascucci,}47, 38 _{A. Pasqualetti,}30 _{R. Passaquieti,}21, 22 _{D. Passuello,}22 _{M. Patil,}158

B. Patricelli,21, 22_{E. Payne,}6 _{B. L. Pearlstone,}47 _{T. C. Pechsiri,}31 _{A. J. Pedersen,}43 _{M. Pedraza,}1_{R. Pedurand,}24, 176

A. Pele,8 _{S. Penn,}177 _{A. Perego,}119, 120 _{C. J. Perez,}48 _{C. P´erigois,}35 _{A. Perreca,}119, 120 _{J. Petermann,}135

H. P. Pfeiffer,77 _{M. Phelps,}10, 11 _{K. S. Phukon,}3 _{O. J. Piccinni,}121, 34 _{M. Pichot,}66 _{F. Piergiovanni,}64, 65

V. Pierro,118, 70 _{G. Pillant,}30 _{L. Pinard,}24 _{I. M. Pinto,}118, 70, 90 _{M. Pirello,}48 _{M. Pitkin,}47 _{W. Plastino,}165, 166

R. Poggiani,21, 22 _{D. Y. T. Pong,}96_{S. Ponrathnam,}3 _{P. Popolizio,}30 _{E. K. Porter,}27 _{J. Powell,}168 _{A. K. Prajapati,}113

J. Prasad,3_{K. Prasai,}52 _{R. Prasanna,}145 _{G. Pratten,}103 _{T. Prestegard,}25 _{M. Principe,}118, 90, 70 _{G. A. Prodi,}119, 120

L. Prokhorov,14 _{M. Punturo,}42_{P. Puppo,}34_{M. P¨}_urrer,77 _{H. Qi,}108_{V. Quetschke,}110_{P. J. Quinonez,}36 _{F. J. Raab,}48

G. Raaijmakers,143, 38 _{H. Radkins,}48 _{N. Radulesco,}66 _{P. Raffai,}112 _{S. Raja,}61_{C. Rajan,}61 _{B. Rajbhandari,}86

M. Rakhmanov,110 _{K. E. Ramirez,}110 _{A. Ramos-Buades,}103 _{Javed Rana,}3 _{K. Rao,}59 _{P. Rapagnani,}121, 34

V. Raymond,108 _{M. Razzano,}21, 22 _{J. Read,}28 _{T. Regimbau,}35 _{L. Rei,}60 _{S. Reid,}26 _{D. H. Reitze,}1, 31

P. Rettegno,128, 178 _{F. Ricci,}121, 34_{C. J. Richardson,}36_{J. W. Richardson,}1_{P. M. Ricker,}20_{G. Riemenschneider,}178, 128

K. Riles,138_{M. Rizzo,}59 _{N. A. Robertson,}1, 47 _{F. Robinet,}29 _{A. Rocchi,}33_{L. Rolland,}35_{J. G. Rollins,}1 _{V. J. Roma,}73

M. Romanelli,72 _{R. Romano,}4, 5 _{C. L. Romel,}48_{J. H. Romie,}8 _{C. A. Rose,}25_{D. Rose,}28 _{K. Rose,}123 _{D. Rosi´}_nska,75

S. G. Rosofsky,20 _{M. P. Ross,}179 _{S. Rowan,}47 _{A. R¨}_udiger,10, 11,∗ _{P. Ruggi,}30_{G. Rutins,}133 _{K. Ryan,}48_{S. Sachdev,}91

T. Sadecki,48 _{M. Sakellariadou,}147_{O. S. Salafia,}180, 45, 46 _{L. Salconi,}30_{M. Saleem,}32 _{A. Samajdar,}38 _{L. Sammut,}6

E. J. Sanchez,1 _{L. E. Sanchez,}1 _{N. Sanchis-Gual,}181 _{J. R. Sanders,}182 _{K. A. Santiago,}37 _{E. Santos,}66 _{N. Sarin,}6

B. Sassolas,24 _{B. S. Sathyaprakash,}91, 108 _{O. Sauter,}138, 35 _{R. L. Savage,}48_{P. Schale,}73 _{M. Scheel,}49 _{J. Scheuer,}59

P. Schmidt,14, 68 _{R. Schnabel,}135 _{R. M. S. Schofield,}73 _{A. Sch¨onbeck,}135 _{E. Schreiber,}10, 11 _{B. W. Schulte,}10, 11

B. F. Schutz,108 _{J. Scott,}47_{S. M. Scott,}9 _{E. Seidel,}20_{D. Sellers,}8 _{A. S. Sengupta,}183 _{N. Sennett,}77 _{D. Sentenac,}30

V. Sequino,60_{A. Sergeev,}150 _{Y. Setyawati,}10, 11 _{D. A. Shaddock,}9 _{T. Shaffer,}48 _{M. S. Shahriar,}59 _{M. B. Shaner,}134

A. Sharma,17, 18 _{P. Sharma,}61 _{P. Shawhan,}78 _{H. Shen,}20 _{R. Shink,}184 _{D. H. Shoemaker,}15_{D. M. Shoemaker,}79

K. Shukla,142 _{S. ShyamSundar,}61 _{K. Siellez,}79 _{M. Sieniawska,}57 _{D. Sigg,}48 _{L. P. Singer,}82_{D. Singh,}91 _{N. Singh,}75

A. Singhal,17, 34 _{A. M. Sintes,}103 _{S. Sitmukhambetov,}110 _{V. Skliris,}108 _{B. J. J. Slagmolen,}9 _{T. J. Slaven-Blair,}67

J. R. Smith,28 _{R. J. E. Smith,}6 _{S. Somala,}185 _{E. J. Son,}153 _{S. Soni,}2 _{B. Sorazu,}47 _{F. Sorrentino,}60_{T. Souradeep,}3

E. Sowell,86 _{A. P. Spencer,}47 _{M. Spera,}54, 55 _{A. K. Srivastava,}113 _{V. Srivastava,}43 _{K. Staats,}59_{C. Stachie,}66

M. Standke,10, 11 _{D. A. Steer,}27 _{M. Steinke,}10, 11 _{J. Steinlechner,}135, 47 _{S. Steinlechner,}135_{D. Steinmeyer,}10, 11

S. P. Stevenson,168 _{D. Stocks,}52 _{R. Stone,}110 _{D. J. Stops,}14 _{K. A. Strain,}47 _{G. Stratta,}186, 65 _{S. E. Strigin,}62

A. Strunk,48 _{R. Sturani,}187 _{A. L. Stuver,}188 _{V. Sudhir,}15 _{T. Z. Summerscales,}189 _{L. Sun,}1 _{S. Sunil,}113 _{A. Sur,}57

J. Suresh,84 _{P. J. Sutton,}108 _{B. L. Swinkels,}38 _{M. J. Szczepa´}_nczyk,36_{M. Tacca,}38 _{S. C. Tait,}47 _{C. Talbot,}6

D. B. Tanner,31 _{D. Tao,}1 _{M. T´apai,}132_{A. Tapia,}28 _{J. D. Tasson,}100 _{R. Taylor,}1 _{R. Tenorio,}103 _{L. Terkowski,}135

M. Thomas,8 _{P. Thomas,}48 _{S. R. Thondapu,}61 _{K. A. Thorne,}8 _{E. Thrane,}6 _{Shubhanshu Tiwari,}119, 120

Srishti Tiwari,136 _{V. Tiwari,}108 _{K. Toland,}47 _{M. Tonelli,}21, 22 _{Z. Tornasi,}47 _{A. Torres-Forn´e,}190 _{C. I. Torrie,}1

D. T¨oyr¨a,14 _{F. Travasso,}30, 42 _{G. Traylor,}8 _{M. C. Tringali,}75 _{A. Tripathee,}138 _{A. Trovato,}27 _{L. Trozzo,}191, 22

K. W. Tsang,38 _{M. Tse,}15 _{R. Tso,}49 _{L. Tsukada,}84 _{D. Tsuna,}84 _{T. Tsutsui,}84 _{D. Tuyenbayev,}110_{K. Ueno,}84

D. Ugolini,192 _{C. S. Unnikrishnan,}136_{A. L. Urban,}2 _{S. A. Usman,}95_{H. Vahlbruch,}11 _{G. Vajente,}1 _{G. Valdes,}2

M. Valentini,119, 120 _{N. van Bakel,}38 _{M. van Beuzekom,}38 _{J. F. J. van den Brand,}76, 38 _{C. Van Den Broeck,}38, 193

D. C. Vander-Hyde,43 _{L. van der Schaaf,}38 _{J. V. VanHeijningen,}67 _{A. A. van Veggel,}47 _{M. Vardaro,}54, 55

(4)

DRAFT-V16

G. Venugopalan,1 _{D. Verkindt,}35 _{F. Vetrano,}64, 65 _{A. Vicer´e,}64, 65 _{A. D. Viets,}25 _{S. Vinciguerra,}14 _{D. J. Vine,}133

J.-Y. Vinet,66 _{S. Vitale,}15_{T. Vo,}43 _{H. Vocca,}41, 42 _{C. Vorvick,}48 _{S. P. Vyatchanin,}62 _{A. R. Wade,}1 _{L. E. Wade,}123

M. Wade,123 _{R. Walet,}38 _{M. Walker,}28 _{L. Wallace,}1 _{S. Walsh,}25 _{H. Wang,}14 _{J. Z. Wang,}138 _{S. Wang,}20

W. H. Wang,110 _{Y. F. Wang,}96_{R. L. Ward,}9 _{Z. A. Warden,}36 _{J. Warner,}48 _{M. Was,}35_{J. Watchi,}104_{B. Weaver,}48

L.-W. Wei,10, 11 _{M. Weinert,}10, 11 _{A. J. Weinstein,}1 _{R. Weiss,}15 _{F. Wellmann,}10, 11 _{L. Wen,}67 _{E. K. Wessel,}20

P. Weßels,10, 11 _{J. W. Westhouse,}36 _{K. Wette,}9 _{J. T. Whelan,}63 _{B. F. Whiting,}31 _{C. Whittle,}15 _{D. M. Wilken,}10, 11

D. Williams,47 _{A. R. Williamson,}143, 38_{J. L. Willis,}1 _{B. Willke,}11, 10 _{W. Winkler,}10, 11 _{C. C. Wipf,}1 _{H. Wittel,}10, 11

G. Woan,47 _{J. Woehler,}10, 11 _{J. K. Wofford,}63 _{J. L. Wright,}47 _{D. S. Wu,}10, 11 _{D. M. Wysocki,}63 _{S. Xiao,}1 _{R. Xu,}111

H. Yamamoto,1 _{C. C. Yancey,}78_{L. Yang,}122 _{Y. Yang,}31 _{Z. Yang,}44 _{M. J. Yap,}9 _{M. Yazback,}31 _{D. W. Yeeles,}108

A. Yoon,7 _{Hang Yu,}15 _{Haocun Yu,}15 _{S. H. R. Yuen,}96 _{A. K. Zadro˙zny,}110 _{A. Zadro˙zny,}157 _{M. Zanolin,}36

T. Zelenova,30_{J.-P. Zendri,}55 _{M. Zevin,}59 _{J. Zhang,}67 _{L. Zhang,}1 _{T. Zhang,}47 _{C. Zhao,}67 _{G. Zhao,}104_{M. Zhou,}59

Z. Zhou,59 _{X. J. Zhu,}6_{A. B. Zimmerman,}194 _{M. E. Zucker,}1, 15 _{J. Zweizig,}1_{F. Salemi,}195_{and M. A. Papa}196, 197, 195

(The LIGO Scientific Collaboration and the Virgo Collaboration) 1_{LIGO, California Institute of Technology, Pasadena, CA 91125, USA}

2_{Louisiana State University, Baton Rouge, LA 70803, USA}

3_{Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India} 4

Dipartimento di Farmacia, Universit`a di Salerno, I-84084 Fisciano, Salerno, Italy 5_{INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy} 6_{OzGrav, School of Physics & Astronomy, Monash University, Clayton 3800, Victoria, Australia}

7_{Christopher Newport University, Newport News, VA 23606, USA} 8_{LIGO Livingston Observatory, Livingston, LA 70754, USA}

9_{OzGrav, Australian National University, Canberra, Australian Capital Territory 0200, Australia} 10_{Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany}

11_{Leibniz Universit¨}_{at Hannover, D-30167 Hannover, Germany}

12_{Theoretisch-Physikalisches Institut, Friedrich-Schiller-Universit¨}_{at Jena, D-07743 Jena, Germany} 13_{University of Cambridge, Cambridge CB2 1TN, United Kingdom}

14_{University of Birmingham, Birmingham B15 2TT, United Kingdom} 15_{LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA}

16_{Instituto Nacional de Pesquisas Espaciais, 12227-010 S˜}_{ao Jos´}_{e dos Campos, S˜}_{ao Paulo, Brazil} 17_{Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy}

18

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

19_{International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, India} 20_{NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA}

21_Universit`_{a di Pisa, I-56127 Pisa, Italy} 22_{INFN, Sezione di Pisa, I-56127 Pisa, Italy} 23

Departamento de Astronom´ıa y Astrof´ısica, Universitat de Val`encia, E-46100 Burjassot, Val`encia, Spain 24_{Laboratoire des Mat´}_{eriaux Avanc´}_{es (LMA), CNRS/IN2P3, F-69622 Villeurbanne, France}

25_{University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA} 26_{SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom}

27_{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 28_{California State University Fullerton, Fullerton, CA 92831, USA}

29_{LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit´}_{e Paris-Saclay, F-91898 Orsay, France} 30_{European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy}

31_{University of Florida, Gainesville, FL 32611, USA} 32_{Chennai Mathematical Institute, Chennai 603103, India} 33_{INFN, Sezione di Roma Tor Vergata, I-00133 Roma, Italy}

34_{INFN, Sezione di Roma, I-00185 Roma, Italy}

35_{Laboratoire d’Annecy de Physique des Particules (LAPP), Univ. Grenoble Alpes,}

Universit´e Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy, France 36_{Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA}

37_{Montclair State University, Montclair, NJ 07043, USA} 38_{Nikhef, Science Park 105, 1098 XG Amsterdam, The Netherlands}

39_{Korea Institute of Science and Technology Information, Daejeon 34141, South Korea} 40_{West Virginia University, Morgantown, WV 26506, USA}

41_Universit`_{a di Perugia, I-06123 Perugia, Italy} 42_{INFN, Sezione di Perugia, I-06123 Perugia, Italy}

(5)

DRAFT-V16

46_{INFN, Sezione di Milano-Bicocca, I-20126 Milano, Italy} 47_{SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom}

48_{LIGO Hanford Observatory, Richland, WA 99352, USA} 49_{Caltech CaRT, Pasadena, CA 91125, USA} 50

Dipartimento di Medicina, Chirurgia e Odontoiatria “Scuola Medica Salernitana, ” Universit`a di Salerno, I-84081 Baronissi, Salerno, Italy

51_{Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Mikl´}_{os ´}_{ut 29-33, Hungary} 52_{Stanford University, Stanford, CA 94305, USA}

53_Universit`_{a di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy} 54_Universit`_{a di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy}

55_{INFN, Sezione di Padova, I-35131 Padova, Italy} 56_{Montana State University, Bozeman, MT 59717, USA}

57_{Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, Poland} 58_{OzGrav, University of Adelaide, Adelaide, South Australia 5005, Australia}

59

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

60_{INFN, Sezione di Genova, I-16146 Genova, Italy} 61_{RRCAT, Indore, Madhya Pradesh 452013, India}

62_{Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia} 63_{Rochester Institute of Technology, Rochester, NY 14623, USA}

64_Universit`_{a degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy} 65_{INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy}

66_{Artemis, Universit´}_{e Cˆ}_{ote d’Azur, Observatoire Cˆ}_{ote d’Azur,}

CNRS, CS 34229, F-06304 Nice Cedex 4, France 67

OzGrav, University of Western Australia, Crawley, Western Australia 6009, Australia 68_{Department of Astrophysics/IMAPP, Radboud University Nijmegen,}

P.O. Box 9010, 6500 GL Nijmegen, The Netherlands

69_{Dipartimento di Fisica “E.R. Caianiello,” Universit`}_{a di Salerno, I-84084 Fisciano, Salerno, Italy} 70_{INFN, Sezione di Napoli, Gruppo Collegato di Salerno,}

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

71_{Physik-Institut, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland} 72

Univ Rennes, CNRS, Institut FOTON - UMR6082, F-3500 Rennes, France 73_{University of Oregon, Eugene, OR 97403, USA}

74_{Laboratoire Kastler Brossel, Sorbonne Universit´}_{e, CNRS,}

ENS-Universit´e PSL, Coll`ege de France, F-75005 Paris, France 75_{Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland}

76_{VU University Amsterdam, 1081 HV Amsterdam, The Netherlands}

77_{Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany} 78_{University of Maryland, College Park, MD 20742, USA}

79_{School of Physics, Georgia Institute of Technology, Atlanta, GA 30332, USA} 80_Universit´_{e de Lyon, Universit´}_{e Claude Bernard Lyon 1,}

CNRS, Institut Lumi`ere Mati`ere, F-69622 Villeurbanne, France

81_Universit`_{a di Napoli “Federico II,” Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy} 82_{NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA}

83_{Dipartimento di Fisica, Universit`}_{a degli Studi di Genova, I-16146 Genova, Italy} 84_{RESCEU, University of Tokyo, Tokyo, 113-0033, Japan.}

85_{Tsinghua University, Beijing 100084, China} 86_{Texas Tech University, Lubbock, TX 79409, USA} 87_Universit`_{a di Roma Tor Vergata, I-00133 Roma, Italy} 88_{The University of Mississippi, University, MS 38677, USA} 89_{Missouri University of Science and Technology, Rolla, MO 65409, USA} 90

Museo Storico della Fisica e Centro Studi e Ricerche “Enrico Fermi,” I-00184 Roma, Italy 91_{The Pennsylvania State University, University Park, PA 16802, USA}

92_{National Tsing Hua University, Hsinchu City, 30013 Taiwan, Republic of China} 93_{Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia}

94_{Canadian Institute for Theoretical Astrophysics,}

University of Toronto, Toronto, Ontario M5S 3H8, Canada 95_{University of Chicago, Chicago, IL 60637, USA} 96

The Chinese University of Hong Kong, Shatin, NT, Hong Kong 97_{Dipartimento di Ingegneria Industriale (DIIN),}

Universit`a di Salerno, I-84084 Fisciano, Salerno, Italy 98

Seoul National University, Seoul 08826, South Korea 99_{Pusan National University, Busan 46241, South Korea}

(6)

DRAFT-V16

101_{INAF, Osservatorio Astronomico di Padova, I-35122 Padova, Italy} 102_{OzGrav, University of Melbourne, Parkville, Victoria 3010, Australia} 103_{Universitat de les Illes Balears, IAC3—IEEC, E-07122 Palma de Mallorca, Spain}

104_Universit´_{e Libre de Bruxelles, Brussels 1050, Belgium} 105

Sonoma State University, Rohnert Park, CA 94928, USA 106

Departamento de Matemáticas, Universitat de València, E-46100 Burjassot, València, Spain 107_{Columbia University, New York, NY 10027, USA}

108_{Cardiff University, Cardiff CF24 3AA, United Kingdom} 109_{University of Rhode Island, Kingston, RI 02881, USA}

110_{The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA} 111_{Bellevue College, Bellevue, WA 98007, USA}

112_{MTA-ELTE Astrophysics Research Group, Institute of Physics, E¨}_otv¨_{os University, Budapest 1117, Hungary} 113_{Institute for Plasma Research, Bhat, Gandhinagar 382428, India}

114_{The University of Sheffield, Sheffield S10 2TN, United Kingdom} 115_{IGFAE, Campus Sur, Universidade de Santiago de Compostela, 15782 Spain}

116_{Dipartimento di Scienze Matematiche, Fisiche e Informatiche, Universit`}_{a di Parma, I-43124 Parma, Italy} 117_{INFN, Sezione di Milano Bicocca, Gruppo Collegato di Parma, I-43124 Parma, Italy}

118_{Dipartimento di Ingegneria, Universit`}_{a del Sannio, I-82100 Benevento, Italy} 119_Universit`_{a di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy}

120_{INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy} 121_Universit`_{a di Roma “La Sapienza,” I-00185 Roma, Italy}

122_{Colorado State University, Fort Collins, CO 80523, USA} 123_{Kenyon College, Gambier, OH 43022, USA}

124_{CNR-SPIN, c/o Universit`}_{a di Salerno, I-84084 Fisciano, Salerno, Italy} 125_{Scuola di Ingegneria, Universit`}_{a della Basilicata, I-85100 Potenza, Italy}

126_{National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan} 127_{Observatori Astron`}_{omic, Universitat de Val`}_{encia, E-46980 Paterna, Val`}_{encia, Spain}

128_{INFN Sezione di Torino, I-10125 Torino, Italy}

129_{School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom} 130

Institute Of Advanced Research, Gandhinagar 382426, India 131

Indian Institute of Technology Bombay, Powai, Mumbai 400 076, India 132

University of Szeged, D´om t´er 9, Szeged 6720, Hungary

133_{SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom}

134_{California State University, Los Angeles, 5151 State University Dr, Los Angeles, CA 90032, USA} 135_Universit¨_{at Hamburg, D-22761 Hamburg, Germany}

136_{Tata Institute of Fundamental Research, Mumbai 400005, India} 137_{INAF, Osservatorio Astronomico di Capodimonte, I-80131 Napoli, Italy}

138_{University of Michigan, Ann Arbor, MI 48109, USA} 139_{Washington State University, Pullman, WA 99164, USA}

140_{American University, Washington, D.C. 20016, USA} 141_{University of Portsmouth, Portsmouth, PO1 3FX, United Kingdom}

142_{University of California, Berkeley, CA 94720, USA}

143_{GRAPPA, Anton Pannekoek Institute for Astronomy and Institute for High-Energy Physics,}

University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 144_{Delta Institute for Theoretical Physics, Science Park 904, 1090 GL Amsterdam, The Netherlands}

145_{Directorate of Construction, Services & Estate Management, Mumbai 400094 India} 146_{University of Bia lystok, 15-424 Bia lystok, Poland}

147

King’s College London, University of London, London WC2R 2LS, United Kingdom 148

University of Southampton, Southampton SO17 1BJ, United Kingdom 149

University of Washington Bothell, Bothell, WA 98011, USA 150_{Institute of Applied Physics, Nizhny Novgorod, 603950, Russia}

151_{Ewha Womans University, Seoul 03760, South Korea} 152_{Inje University Gimhae, South Gyeongsang 50834, South Korea} 153_{National Institute for Mathematical Sciences, Daejeon 34047, South Korea} 154_{Ulsan National Institute of Science and Technology, Ulsan 44919, South Korea}

155_{Maastricht University, P.O. Box 616, 6200 MD Maastricht, The Netherlands} 156_{Bard College, 30 Campus Rd, Annandale-On-Hudson, NY 12504, USA}

157_{NCBJ, 05-400 ´}_{Swierk-Otwock, Poland}

158_{Institute of Mathematics, Polish Academy of Sciences, 00656 Warsaw, Poland} 159_{Cornell University, Ithaca, NY 14850, USA}

160_{Hillsdale College, Hillsdale, MI 49242, USA} 161_{Hanyang University, Seoul 04763, South Korea}

(7)

DRAFT-V16

163_{Institute for High-Energy Physics, University of Amsterdam,}

Science Park 904, 1098 XH Amsterdam, The Netherlands 164_{NASA Marshall Space Flight Center, Huntsville, AL 35811, USA}

165_{Dipartimento di Matematica e Fisica, Universit`}_{a degli Studi Roma Tre, I-00146 Roma, Italy} 166_{INFN, Sezione di Roma Tre, I-00146 Roma, Italy}

167_{ESPCI, CNRS, F-75005 Paris, France}

168_{OzGrav, Swinburne University of Technology, Hawthorn VIC 3122, Australia} 169

Southern University and A&M College, Baton Rouge, LA 70813, USA 170_{Centre Scientifique de Monaco, 8 quai Antoine Ier, MC-98000, Monaco}

171_{Indian Institute of Technology Madras, Chennai 600036, India} 172_{Institut des Hautes Etudes Scientifiques, F-91440 Bures-sur-Yvette, France}

173_{IISER-Kolkata, Mohanpur, West Bengal 741252, India} 174_{Institut f¨}_{ur Kernphysik, Theoriezentrum, 64289 Darmstadt, Germany} 175_{Whitman College, 345 Boyer Avenue, Walla Walla, WA 99362 USA}

176_Universit´_{e de Lyon, F-69361 Lyon, France}

177_{Hobart and William Smith Colleges, Geneva, NY 14456, USA} 178_{Dipartimento di Fisica, Universit`}_{a degli Studi di Torino, I-10125 Torino, Italy}

179_{University of Washington, Seattle, WA 98195, USA}

180_{INAF, Osservatorio Astronomico di Brera sede di Merate, I-23807 Merate, Lecco, Italy} 181_{Centro de Astrof´ısica e Gravita}_×_c_˜_ao₍_{CEN T RA}₎_,

DepartamentodeF´ısica, InstitutoSuperiorTecnico, U niversidadedeLisboa,´ 1049−001Lisboa, P ortugal

182_{Marquette University, 11420 W. Clybourn St., Milwaukee, WI 53233, USA} 183_{Indian Institute of Technology, Gandhinagar Ahmedabad Gujarat 382424, India}

184_Universit´_{e de Montr´}_{eal/Polytechnique, Montreal, Quebec H3T 1J4, Canada} 185_{Indian Institute of Technology Hyderabad, Sangareddy, Khandi, Telangana 502285, India}

186_{INAF, Osservatorio di Astrofisica e Scienza dello Spazio, I-40129 Bologna, Italy}

187_{International Institute of Physics, Universidade Federal do Rio Grande do Norte, Natal RN 59078-970, Brazil} 188_{Villanova University, 800 Lancaster Ave, Villanova, PA 19085, USA}

189_{Andrews University, Berrien Springs, MI 49104, USA}

190_{Max Planck Institute for Gravitationalphysik (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany} 191_Universit`_{a di Siena, I-53100 Siena, Italy}

192_{Trinity University, San Antonio, TX 78212, USA} 193_{Van Swinderen Institute for Particle Physics and Gravity,}

University of Groningen, Nijenborgh 4, 9747 AG Groningen, The Netherlands 194_{Department of Physics, University of Texas, Austin, TX 78712, USA}

195_{Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, Germany} 196

Max Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, Germany 197_{University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA}

(Dated: June 18, 2019)

Gravitational wave astronomy has been firmly established with the detection of gravitational

1

waves from the merger of ten stellar mass binary black holes and a neutron star binary. This paper

2

reports on the all-sky search for gravitational waves from intermediate mass black hole binaries in

3

the first and second observing runs of the Advanced LIGO and Virgo network. The search uses

4

three independent algorithms: two based on matched filtering of the data with waveform templates

5

of gravitational wave signals from compact binaries, and a third, model-independent algorithm that

6

employs no signal model for the incoming signal. No intermediate mass black hole binary event

7

was detected in this search. Consequently, we place upper limits on the merger rate density for a

8

family of intermediate mass black hole binaries. In particular, we choose sources with total masses

9

M =m1+m2 ∈[120,800] M and mass ratios q =m2/m1 ∈[0.1,1.0]. For the first time, this

10

calculation is done using numerical relativity waveforms (which include higher modes) as models of

11

the real emitted signal. We place a most stringent upper limit of 0.20 Gpc−3_yr−1 _{(in co-moving}

12

units at the 90% confidence level) for equal-mass binaries with individual massesm1,2 = 100 M

13

and dimensionless spinsχ1,2= 0.8 aligned with the orbital angular momentum of the binary. This

14

improves by a factor of∼5 that reported after Advanced LIGO’s first observing run.

15

PACS numbers: 04.80.Nn, 07.05.Kf, 95.55.Ym

∗_{Deceased, July 2018.}

I. INTRODUCTION

The first two observing runs of Advanced LIGO and

16

Virgo (O1 and O2 respectively) have significantly

en-17

hanced our understanding of black hole (BH) binaries in

(8)

DRAFT-V16

the universe. Gravitational waves (GWs) from 10 binary

19

black hole mergers with total mass between 18.6+3.1

−0.7M

20

and 85.1+15−10..69 M were detected during these two

ob-21

serving runs [1–8]. These observations have revealed a

22

new population of heavy stellar mass BH components of

23

up to 50 M, for which we had no earlier

electromag-24

netic observational evidence [8, 9]. This finding limit is

25

consistent with the formation of heavier BHs from core

26

collapse being prevented by a mechanism known as

pul-27

sational pair-instability supernovae (PISN) [10–13].

Ac-28

cording to this idea, stars with helium core mass in the

29

range ∼ 32−64M undergo pulsational pair

instabil-30

ity leaving behind remnants of .65M. Stars with

he-31

lium core mass in the range_∼64₋135M undergo pair

32

instability and leave no remnant, while stars with

he-33

lium mass & 135Modot are thought to directly collapse

34

to intermediate-mass black holes.

35

Intermediate mass black holes (IMBHs) are BHs

heav-36

ier than stellar mass BHs but lighter than

supermas-37

sive black holes (SMBHs), which places them roughly

38

in the range of 102

−105 _M

[14, 15]. Currently there

39

is only indirect observational evidence. Observations

in-40

clude probing the mass of the central BH in galaxies as

41

well as massive star clusters with direct kinematical

mea-42

surements which has led to recent claims for the presence

43

of IMBHs [16–18]. Other observations come from the

ex-44

trapolation of several scaling relations between the mass

45

of the central SMBH and their host galaxies [19] to the

46

mass range of globular clusters [20, 21]. In this way,

sev-47

eral clusters have been found to be good candidates for

48

having IMBHs in their centers [22–24]. If present, IMBHs

49

would heat up the cores of these clusters, strongly

influ-50

encing the distribution of the stars in the cluster and

51

their dynamics, leaving a characteristic imprint in the

52

surface brightness profile, as well as in the mass-to-light

53

ratio [25]. Controversy exists regarding the

interpreta-54

tion of these observations, as some of them can also be

55

explained by a high concentration of stellar-mass BHs

56

or the presence of binaries[22–24, 26]. Empirical mass

57

scaling relations of quasi-periodic oscillations [27] in

lu-58

minous X-Ray sources have also provided evidence for

59

IMBH [28]. Finally, IMBHs have been proposed as

can-60

didates to explain ultra-luminous X-Ray (ULX) sources

61

in nearby galaxies, which are brighter than the

accret-62

ing X-ray sources with stellar mass BHs [29, 30].

How-63

ever, neutron stars or stellar-mass black holes emitting

64

above their Eddington luminosity could also account for

65

such observations. In summary, no definitive evidence of

66

IMBHs has yet been obtained.

67

The possible astrophysical formation channels of

68

IMBHs remain uncertain. Proposed channels include the

69

direct collapse of massive first generation, low metallicity

70

Population III stars [31–34] and mergers of stellar mass

71

BHs in globular clusters [36] and multiple collisions of

72

stars in dense young star clusters [18, 35, 37–39], among

73

others [40]. Further, some astrophysical scenarios [14]

in-74

dicate that SMBHs in galactic centers might be formed

75

from hierarchical mergers of IMBHs [15, 41]. The

di-76

rect observation of IMBHs with gravitational waves could

77

strengthen the possible evolutionary link between

stel-78

lar mass BHs and SMBHs. Finally, observing an IMBH

79

population would help to understand details of the

pul-80

sational pair-instability supernovae mechanism.

81

The GW observation of a coalescing binary

consist-82

ing of at least one IMBH component or resulting in an

83

IMBH remnant, which we will term an IMBHB, could

84

provide the first definitive confirmation of the existence of

85

IMBHs. In fact, IMBHBs are the sources that would emit

86

the most gravitational-wave energy in the LIGO-Virgo

87

frequency band, potentially making them detectable to

88

distances (and redshifts) beyond that of any other

LIGO-89

Virgo source [42]. Even in the absence of a detection,

90

a search for IMBHBs provides stringent constraints on

91

their merger rate density, which has implications for

po-92

tential IMBHB and SMBH formation channels.

93

IMBHs are not only interesting from an

astrophysi-94

cal point of view, they are also excellent laboratories

95

to test general relativity in the strong field regime [43–

96

46]. Their large masses would lead to strong merger

97

and ringdown signals in the Advanced LIGO-Virgo

fre-98

quency band. Therefore, higher modes might be visible in

99

IMBHB signals because those modes are especially strong

100

in the merger and ringdown stages. The observation of

101

multimodal merger and ringdown signals is paramount

102

to understanding fundamental properties of general

rela-103

tivity, such as the no-hair theorem [47–50] and BH kick

104

measurements [51–53].

105

The first search for GWs from IMBHBs was carried out

106

in the data from initial LIGO and initial Virgo

(2005-107

2010) [54, 55]. Owing to the large masses of

IMB-108

HBs, such systems are expected to merge at low

fre-109

quencies where the initial detectors were less sensitive

110

due to the presence of several noise sources, such as

111

suspension noise, thermal noise and optical cavity

con-112

trol noise. As a result, the those detectors were

sen-113

sitive to only the merger and ringdown phases of the

114

IMBHB systems. Initial IMBHB analyses applied either

115

the model-independent time-frequency searches [56] or

116

ringdown searches. No IMBHB merger was detected in

117

these searches.

118

Because of the improved low-frequency sensitivities

119

of the Advanced LIGO and Advanced Virgo

detec-120

tors [57, 58], IMBHB signals are visible in band for a

121

longer period of time, which increases the effectiveness

122

of modeled searches that use more than just the

ring-123

down portion of an IMBHB’s waveform. Ref. [42]

re-124

ports results from a combined search for IMBHBs that

125

used two independent search algorithms: a

matched-126

filter analysis, called GstLAL [59–61], which uses the

127

inspiral, merger, and ringdown portions of the IMBHB

128

waveform and the model-independent analysis coherent

129

WaveBurst (cWB) [56]. No IMBHBs were found by

130

these searches, and upper limits on the merger rate

den-131

sity for 12 targeted IMBHB sources with total mass

be-132

tween 120 M−600 M and mass ratios down to 1/10

133

were obtained. The most stringent upper limit on the

(9)

DRAFT-V16

merger rate density from this combined analysis was

135

0.93 Gpc−3 yr−1 _{for binaries consisting of two 100 M}

136

BHs with dimensionless spin magnitude 0.8 aligned with

137

the system’s orbital angular momentum.

138

All upper limits on the IMBHB merger rate reported

139

in past searches [42, 54, 55] were obtained using models

140

for the GW signal that include only the dominant

radiat-141

ing mode, namely (`, m) = (2,±2), of the GW emission

142

[62]. However, it has been shown that higher modes

con-143

tribute more substantially to signals emitted by heavy

144

binaries. This impact increases as the system becomes

145

more asymmetric in mass [63, 64], as the spin of the BHs

146

becomes more negative [65, 66], and as the precession in

147

the binary becomes stronger [67]. As a consequence, the

148

omission of higher modes leads in general to more

con-149

servative upper limits on the IMBHB merger rate [68].

150

In this work, we improve on past studies in two distinct

151

ways. We use numerical relativity (NR) simulations with

152

higher modes to model GW signals from IMBHBs for

153

computing upper limit estimates. Additionally, our

com-154

bined analysis now includes the matched-filter search

Py-155

CBC [69, 70] in addition to GstLAL and cWB. Because

156

of these novelties, we have, in addition to analyzing the

157

O2 data set, reanalyzed the O1 data set and report here

158

combined upper limits for the O1 and O2 observing runs.

159

In this paper, we report upper limits on the merger rate

160

density of 17 targeted (non-precessing) IMBHB sources.

161

Our most stringent upper limit is 0.20 Gpc−3 yr−1 _for

162

equal-mass binaries with component spins aligned with

163

the orbital angular momentum of the system and

dimen-164

sionless magnitudesχ1,2= 0.8.

165

The rest of this paper is organized as follows. In Sec. II

166

we describe the data set, outline the individual search

al-167

gorithms that make up the combined search, and report

168

our search’s null detection of IMBHBs. In Sec. III we

169

describe the NR simulations that we use to compute

up-170

per limits on IMBHB merger rates report these for the

171

case of 17 IMBHB sources. We draw final conclusions in

172

Sec. IV.

173

II. IMBHB SEARCH IN O1 AND O2 DATA

174

A. Data Summary

175

This analysis was carried out using O1 and O2 data

176

sets from the two LIGO (Livingston and Hanford)

de-177

tectors and Virgo. We have used the final calibration,

178

which was produced after the conclusion of the run,

in-179

cluding compensation for frequency-dependent

fluctua-180

tions in the calibration [71–73]. Well identified sources

181

of noise have also been subtracted from the strain data

182

as explained in Refs. [73, 74]. The maximum calibration

183

uncertainty across the frequency band of [10-5,000] Hz for

184

the two LIGO detectors is∼10% in amplitude and∼5

185

degrees in phase for O1 and∼4% in amplitude and∼3

186

degrees in phase for O2 [7, 71]. For Virgo we consider an

187

uncertainty of 5.1% in amplitude and 2.3 degrees in phase

188

[73]. After removing data with significant instrumental

189

disturbance, we use 48.6 days and 118.0 days of joint

190

Hanford-Livingston data from the O1 and O2 observing

191

runs respectively. The Virgo detector joined the LIGO

192

detectors during the last∼15 days of O2, which provided

193

with an additional 4.0 days of coincident data with either

194

of Hanford-Virgo or Livingston-Virgo network. The data

195

from O1 and O2 was divided into 9 and 21 blocks

respec-196

tively with coincident time ranging from 4.7₋7.0 days.

197

For more details, see Ref. [8].

198

B. Search algorithms

199

We combine the two matched-filter searches, namely

200

GstLAL [59–61, 75] and PyCBC [69, 70], and one

model-201

independent analysis, cWB [76], into a single IMBHB

202

search. The two model-based matched filtering

analy-203

ses use a bank of templates made of pre-computed

com-204

pact binary merger GW waveforms. Matched filter based

205

analyses are optimal to extract known signals from

sta-206

tionary, Gaussian noise [77]. However, the templates we

207

use are limited to non-eccentric, aligned-spin systems.

208

They contain only the dominant waveform mode of the

209

GW emission and omit higher modes [64, 78].

Addi-210

tionally, Advanced LIGO and Virgo data are known to

211

contain a large number of short noise transients [79],

212

which can mimic short GW signals like those emitted by

213

IMBHBs. While matched-filter searches use several

tech-214

niques to discriminate between noisy transients and real

215

GW events [61, 80, 81], they are known to lose significant

216

efficiency when looking for short signals like those from

217

IMBHBs. Therefore, the IMBHB search is carried out

218

jointly with an analysis that can identify short-duration

219

GW signals without a model for the morphology of the

220

GW waveform. In this search, all three analyses use O1

221

and O2 Advanced LIGO data. However, because of the

222

incomparable sensitivities between the Advanced LIGO

223

detector and Advanced Virgo detector, only the GstLAL

224

analysis uses Virgo data, as is done in Ref. [8].

225

1. Modeled analyses

226

The matched-filter analyses GstLAL and PyCBC use

227

templates that span the parameter space of neutron stars,

228

stellar-mass BHs, and IMBHs. In this study, we use the

229

same two searches reported in Ref. [8] to calculate upper

230

limits on the merger rate density of IMBHBs.

231

The matched-filter signal-to-noise ratio (SNR) time

se-232

ries is computed for every template. Triggers are

pro-233

duced when the SNR time series surpasses a

predeter-234

mined threshold, where clusters of triggers are trimmed

235

by maximizing the SNR within small time windows. In

236

addition, a signal consistency veto [61, 81, 82] is

calcu-237

lated for each trigger. A list of GW candidates is

con-238

structed from triggers generated by common templates

239

that are coincident in time across more than one

(10)

DRAFT-V16

tor, where the coincidence window takes into account the

241

travel time between detectors. Next, a ranking statistic

242

is calculated for each candidate that estimates a

likeli-243

hood ratio that the candidate would be observed in the

244

presence of a GW compared to a pure-noise expectation.

245

Finally, a p-value1 _P _{is determined by comparing the}

246

value of its ranking statistic to that of triggers coming

247

from background noise in the data. A detailed

descrip-248

tion of the GstLAL and PyCBC pipelines can be found

249

in Refs. [59–61, 75] and [69, 70], respectively;

addition-250

ally, details outlining how candidates are ranked across

251

observing runs can be found in Ref. [8].

252

The GstLAL analysis uses the template bank described

253

in Ref. [83]. The region of this bank that overlaps the

254

IMBHB parameter space, which starts at a total mass

255

of 100 M, reaches up to a total mass of 400 M in

256

the detector frame and covers mass ratios in the range

257

of 1/98 < q < 1. The waveforms used are a

reduced-258

order-model of the SEOBNRv4 approximant [84]. The

259

spin of these templates are either aligned or anti-aligned

260

with the orbital angular momentum of the system with

261

dimensionless magnitudes less than 0.999.

262

The PyCBC analysis uses the template bank described

263

in Ref. [85]. The region of this bank that overlaps the

264

IMBHB parameter space reaches up to a total mass

265

of 500 M in the detector frame, excluding templates

266

with duration below 0.15 s, and covers the range of

267

1/98< q < 1. The waveforms used are also a

reduced-268

order-model of the SEOBNRv4 approximant, and the

269

aligned or anti-aligned dimensionless spin magnitudes are

270

less than 0.998.

271

2. Un-modeled analysis

272

Coherent WaveBurst (cWB) is the GW transient

de-273

tection algorithm designed to look for unmodeled

short-274

duration GW transients in the multi-detector data from

275

interferometric GW detector networks. Designed to

oper-276

ate without a specific waveform model, cWB identifies

co-277

incident excess power in the wavelet time-frequency

rep-278

resentations of the detector strain data [86], for signal

fre-279

quencies up to 1 kHz and durations up to a few seconds.

280

The search identifies events that are coherent in multiple

281

detectors and reconstructs the source sky location and

282

signal waveforms by using the constrained maximum

like-283

lihood method [76]. The cWB detection statistic is based

284

on the coherent energyEc obtained by cross-correlating

285

the signal waveforms reconstructed in multiple detectors.

286

It is proportional to the network SNR and used to rank

287

the events found by cWB.

288

To improve the robustness of the algorithm against

289

non-stationary detector noise, cWB uses

signal-290

independent vetoes, which reduce the high rate of the

291

1 _{The probability that noise would produce a trigger at least as}

significant as the observed candidate.

initial excess power triggers. The primary veto cut is on

292

the network correlation coefficient cc = Ec/(Ec +En),

293

whereEnis the residual noise energy estimated after the

294

reconstructed signal is subtracted from the data.

Typi-295

cally, for a GW signalcc≈1 and for instrumental glitches

296

cc 1. Therefore, candidate events with cc < 0.7 are

297

rejected as potential glitches.

298

To improve the detection efficiency of IMBHBs as well

299

as to reduce the false alarm rates (FARs), the cWB

anal-300

ysis employs additional selection cuts based on the

na-301

ture of IMBHB signals. IMBHB signals have two distinct

302

features in the time-frequency representation. First, the

303

signal frequencies lie below 250 Hz. We use this to

ex-304

clude all the non-IMBHB events in the search, including

305

noise events. Secondly, the inspiral signal duration in

306

the detector band is relatively short, which leads to

rel-307

atively low SNR in the inspiral phase as compared to

308

the merger and ringdown phases. In the cWB

frame-309

work, chirp mass (_M= (m1 m2)3/5M−1/5) is estimated

310

using the frequency evolution of a signal’s inspiral.

How-311

ever, in the case of low SNRs, we cannot accurately

esti-312

mate the chirp mass of the binary [87]; still, we use this

313

framework to introduce additional cuts on the estimated

314

chirp mass to reject non-IMBHB signals. The

simula-315

tion studies show that IMBHB signals are recovered with

316

|M|>10 M which we use in this search. 2 We apply

317

this selection cut to reduce the noise background when

318

producing the candidate events.

319

For estimation of the statistical significance of the

can-320

didate event, each event is ranked against a sample of

321

background triggers obtained by repeating the analysis

322

on time-shifted data [1]. To exclude astrophysical events

323

from the background sample, the time shifts are selected

324

to be much longer (1 second or more) than the expected

325

signal time delay between the detectors. By using

differ-326

ent time shifts, a sample of background events equivalent

327

to approximately 500 years of background data is

accu-328

mulated for each of the 30 blocks of data. The cWB

can-329

didate events that survived the cWB selection criteria,

330

are assigned a FAR given by the rate of the

correspond-331

ing background events with the coherent network SNR

332

value larger than that of the candidate event.

333

C. Combined search

334

Each of our three algorithms produces its own list of

335

GW candidates, characterized by GPS time, FAR and

336

associated p-value P. These three lists are then

com-337

bined into a common single list of candidates. To avoid

338

counting candidates more than once, candidates within a

339

time window of 100 ms across different lists are assumed

340

to be the same. To account for the use of three search

341

2_Negative _M _{values correspond to frequencies decreasing with}