Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10−23/Hz−−−√ was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30  M⊙ could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914

Search for high-energy neutrinos from gravitational wave event GW151226 and candidate LVT151012 with ANTARES and IceCube

The Advanced LIGO observatories detected gravitational waves from two binary black hole mergers during their first observation run (O1). We present a high-energy neutrino follow-up search for the second gravitational wave event, GW151226, as well as for gravitational wave candidate LVT151012. We find two and four neutrino candidates detected by IceCube, and one and zero detected by Antares, within ±500 s around the respective gravitational wave signals, consistent with the expected background rate. None of these neutrino candidates are found to be directionally coincident with GW151226 or LVT151012. We use nondetection to constrain isotropic-equivalent high-energy neutrino emission from GW151226, adopting the GW event's 3D localization, to less than 2×1051-2×1054 erg. © 2017 American Physical Society

Directional Limits on Persistent Gravitational Waves from Advanced LIGO's First Observing Run

We employ gravitational-wave radiometry to map the stochastic gravitational wave background expected from a variety of contributing mechanisms and test the assumption of isotropy using data from the Advanced Laser Interferometer Gravitational Wave Observatory's (aLIGO) first observing run. We also search for persistent gravitational waves from point sources with only minimal assumptions over the 20-1726 Hz frequency band. Finding no evidence of gravitational waves from either point sources or a stochastic background, we set limits at 90% confidence. For broadband point sources, we report upper limits on the gravitational wave energy flux per unit frequency in the range Fα,Θ(f)<(0.1-56)×10-8 erg cm-2 s-1 Hz-1(f/25 Hz)α-1 depending on the sky location Θ and the spectral power index α. For extended sources, we report upper limits on the fractional gravitational wave energy density required to close the Universe of Ω(f,Θ)<(0.39-7.6)×10-8 sr-1(f/25 Hz)α depending on Θ and α. Directed searches for narrowband gravitational waves from astrophysically interesting objects (Scorpius X-1, Supernova 1987 A, and the Galactic Center) yield median frequency-dependent limits on strain amplitude of h0<(6.7,5.5, and 7.0)×10-25, respectively, at the most sensitive detector frequencies between 130-175 Hz. This represents a mean improvement of a factor of 2 across the band compared to previous searches of this kind for these sky locations, considering the different quantities of strain constrained in each case. © 2017 Published by the American Physical Society

First Search for Gravitational Waves from Known Pulsars with Advanced LIGO

We present the result of searches for gravitational waves from 200 pulsars using data from the first observing run of the Advanced LIGO detectors. We find no significant evidence for a gravitational-wave signal from any of these pulsars, but we are able to set the most constraining upper limits yet on their gravitational-wave amplitudes and ellipticities. For eight of these pulsars, our upper limits give bounds that are improvements over the indirect spin-down limit values. For another 32, we are within a factor of 10 of the spin-down limit, and it is likely that some of these will be reachable in future runs of the advanced detector. Taken as a whole, these new results improve on previous limits by more than a factor of two

Effects of waveform model systematics on the interpretation of GW150914

PAPER Effects of waveform model systematics on the interpretation of GW150914 B P Abbott1, R Abbott1, T D Abbott2, M R Abernathy3, F Acernese4,5, K Ackley6, C Adams7, T Adams8, P Addesso9,144, R X Adhikari1, V B Adya10, C Affeldt10, M Agathos11, K Agatsuma11, N Aggarwal12, O D Aguiar13, L Aiello14,15, A Ain16, P Ajith17, B Allen10,18,19, A Allocca20,21, P A Altin22, A Ananyeva1, S B Anderson1, W G Anderson18, S Appert1, K Arai1, M C Araya1, J S Areeda23, N Arnaud24, K G Arun25, S Ascenzi15,26, G Ashton10, M Ast27, S M Aston7, P Astone28, P Aufmuth19, C Aulbert10, A Avila-Alvarez23, S Babak29, P Bacon30, M K M Bader11, P T Baker31, F Baldaccini32,33, G Ballardin34, S W Ballmer35, J C Barayoga1, S E Barclay36, B C Barish1, D Barker37, F Barone4,5, B Barr36, L Barsotti12, M Barsuglia30, D Barta38, J Bartlett37, I Bartos39, R Bassiri40, A Basti20,21, J C Batch37, C Baune10, V Bavigadda34, M Bazzan41,42, C Beer10, M Bejger43, I Belahcene24, M Belgin44, A S Bell36, B K Berger1, G Bergmann10, C P L Berry45, D Bersanetti46,47, A Bertolini11, J Betzwieser7, S Bhagwat35, R Bhandare48, I A Bilenko49, G Billingsley1, C R Billman6, J Birch7, R Birney50, O Birnholtz10, S Biscans1,12, A Bisht19, M Bitossi34, C Biwer35, M A Bizouard24, J K Blackburn1, J Blackman51, C D Blair52, D G Blair52, R M Blair37, S Bloemen53, O Bock10, M Boer54, G Bogaert54, A Bohe29, F Bondu55, R Bonnand8, B A Boom11, R Bork1, V Boschi20,21, S Bose16,56, Y Bouffanais30, A Bozzi34, C Bradaschia21, P R Brady18, V B Braginsky49,145, M Branchesi57,58, J E Brau59, T Briant60, A Brillet54, M Brinkmann10, V Brisson24, P Brockill18, J E Broida61, A F Brooks1, D A Brown35, D D Brown45, N M Brown12, S Brunett1, C C Buchanan2, A Buikema12, T Bulik62, H J Bulten11,63, A Buonanno29,64, D Buskulic8, C Buy30, R L Byer40, M Cabero10, L Cadonati44, G Cagnoli65,66, C Cahillane1, J Calderón Bustillo44, T A Callister1, E Calloni5,67, J B Camp68, K C Cannon69, H Cao70, J Cao71, C D Capano10, E Capocasa30, F Carbognani34, S Caride72, J Casanueva Diaz24, C Casentini15,26, S Caudill18, M Cavaglià73, F Cavalier24, R Cavalieri34, G Cella21, C B Cepeda1, L Cerboni Baiardi57,58, G Cerretani20,21, E Cesarini15,26, S J Chamberlin74, M Chan36, S Chao75, P Charlton76, E Chassande-Mottin30, B D Cheeseboro31, H Y Chen77, Y Chen51, H-P Cheng6, A Chincarini47, A Chiummo34, T Chmiel78, H S Cho79, M Cho64, J H Chow22, N Christensen61, Q Chu52, A J K Chua80, S Chua60, S Chung52, G Ciani6, F Clara37, J A Clark44, F Cleva54, C Cocchieri73, E Coccia14,15, P-F Cohadon60, A Colla28,81, C G Collette82, L Cominsky83, M Constancio Jr13, L Conti42, S J Cooper45, T R Corbitt2, N Cornish84, A Corsi72, S Cortese34, C A Costa13, M W Coughlin61, S B Coughlin85, J-P Coulon54, S T Countryman39, P Couvares1, P B Covas86, E E Cowan44, D M Coward52, M J Cowart7, D C Coyne1, R Coyne72, J D E Creighton18, T D Creighton87, J Cripe2, S G Crowder88, T J Cullen23, A Cumming36, L Cunningham36, E Cuoco34, T Dal Canton68, S L Danilishin36, S D'Antonio15, K Danzmann10,19, A Dasgupta89, C F Da Silva Costa6, V Dattilo34, I Dave48, M Davier24, G S Davies36, D Davis35, E J Daw90, B Day44, R Day34, S De35, D DeBra40, G Debreczeni38, J Degallaix65, M De Laurentis5,67, S Deléglise60, W Del Pozzo45, T Denker10, T Dent10, V Dergachev29, R De Rosa5,67, R T DeRosa7, R DeSalvo91, J Devenson50, R C Devine31, S Dhurandhar16, M C Díaz87, L Di Fiore5, M Di Giovanni92,93, T Di Girolamo5,67, A Di Lieto20,21, S Di Pace28,81, I Di Palma28,29,81, A Di Virgilio21, Z Doctor77, V Dolique65, F Donovan12, K L Dooley73, S Doravari10, I Dorrington94, R Douglas36, M Dovale Álvarez45, T P Downes18, M Drago10, R W P Drever1,146, J C Driggers37, Z Du71, M Ducrot8, S E Dwyer37, T B Edo90, M C Edwards61, A Effler7, H-B Eggenstein10, P Ehrens1, J Eichholz1, S S Eikenberry6, R A Eisenstein12, R C Essick12, Z Etienne31, T Etzel1, M Evans12, T M Evans7, R Everett74, M Factourovich39, V Fafone14,15,26, H Fair35, S Fairhurst94, X Fan71, S Farinon47, B Farr77, W M Farr45, E J Fauchon-Jones94, M Favata95, M Fays94, H Fehrmann10, M M Fejer40, A Fernández Galiana12, I Ferrante20,21, E C Ferreira13, F Ferrini34, F Fidecaro20,21, I Fiori34, D Fiorucci30, R P Fisher35, R Flaminio65,96, M Fletcher36, H Fong97, S S Forsyth44, J-D Fournier54, S Frasca28,81, F Frasconi21, Z Frei98, A Freise45, R Frey59, V Frey24, E M Fries1, P Fritschel12, V V Frolov7, P Fulda6,68, M Fyffe7, H Gabbard10, B U Gadre16, S M Gaebel45, J R Gair99, L Gammaitoni32, S G Gaonkar16, F Garufi5,67, G Gaur100, V Gayathri101, N Gehrels68, G Gemme47, E Genin34, A Gennai21, J George48, L Gergely102, V Germain8, S Ghonge17, Abhirup Ghosh17, Archisman Ghosh11,17, S Ghosh11,53, J A Giaime2,7, K D Giardina7, A Giazotto21, K Gill103, A Glaefke36, E Goetz10, R Goetz6, L Gondan98, G González2, J M Gonzalez Castro20,21, A Gopakumar104, M L Gorodetsky49, S E Gossan1, M Gosselin34, R Gouaty8, A Grado5,105, C Graef36, M Granata65, A Grant36, S Gras12, C Gray37, G Greco57,58, A C Green45, P Groot53, H Grote10, S Grunewald29, G M Guidi57,58, X Guo71, A Gupta16, M K Gupta89, K E Gushwa1, E K Gustafson1, R Gustafson106, J J Hacker23, B R Hall56, E D Hall1, G Hammond36, M Haney104, M M Hanke10, J Hanks37, C Hanna74, M D Hannam94, J Hanson7, T Hardwick2, J Harms57,58, G M Harry3, I W Harry29, M J Hart36, M T Hartman6, C-J Haster45,97, K Haughian36, J Healy107, A Heidmann60, M C Heintze7, H Heitmann54, P Hello24, G Hemming34, M Hendry36, I S Heng36, J Hennig36, J Henry107, A W Heptonstall1, M Heurs10,19, S Hild36, D Hoak34, D Hofman65, K Holt7, D E Holz77, P Hopkins94, J Hough36, E A Houston36, E J Howell52, Y M Hu10, E A Huerta108, D Huet24, B Hughey103, S Husa86, S H Huttner36, T Huynh-Dinh7, N Indik10, D R Ingram37, R Inta72, H N Isa36, J-M Isac60, M Isi1, T Isogai12, B R Iyer17, K Izumi37, T Jacqmin60, K Jani44, P Jaranowski109, S Jawahar110, F Jiménez-Forteza86, W W Johnson2, D I Jones111, R Jones36, R J G Jonker11, L Ju52, J Junker10, C V Kalaghatgi94, V Kalogera85, S Kandhasamy73, G Kang79, J B Kanner1, S Karki59, K S Karvinen10, M Kasprzack2, E Katsavounidis12, W Katzman7, S Kaufer19, T Kaur52, K Kawabe37, F Kéfélian54, D Keitel86, D B Kelley35, R Kennedy90, J S Key112, F Y Khalili49, I Khan14, S Khan94, Z Khan89, E A Khazanov113, N Kijbunchoo37, Chunglee Kim114, J C Kim115, Whansun Kim116, W Kim70, Y-M Kim114,117, S J Kimbrell44, E J King70, P J King37, R Kirchhoff10, J S Kissel37, B Klein85, L Kleybolte27, S Klimenko6, P Koch10, S M Koehlenbeck10, S Koley11, V Kondrashov1, A Kontos12, M Korobko27, W Z Korth1, I Kowalska62, D B Kozak1, C Krämer10, V Kringel10, B Krishnan10, A Królak118,119, G Kuehn10, P Kumar97, R Kumar89, L Kuo75, A Kutynia118, B D Lackey29,35, M Landry37, R N Lang18, J Lange107, B Lantz40, R K Lanza12, A Lartaux-Vollard24, P D Lasky120, M Laxen7, A Lazzarini1, C Lazzaro42, P Leaci28,81, S Leavey36, E O Lebigot30, C H Lee117, H K Lee121, H M Lee114, K Lee36, J Lehmann10, A Lenon31, M Leonardi92,93, J R Leong10, N Leroy24, N Letendre8, Y Levin120, T G F Li122, A Libson12, T B Littenberg123, J Liu52, N A Lockerbie110, A L Lombardi44, L T London94, J E Lord35, M Lorenzini14,15, V Loriette124, M Lormand7, G Losurdo21, J D Lough10,19, G Lovelace23, H Lück10,19, A P Lundgren10, R Lynch12, Y Ma51, S Macfoy50, B Machenschalk10, M MacInnis12, D M Macleod2, F Magaña-Sandoval35, E Majorana28, I Maksimovic124, V Malvezzi15,26, N Man54, V Mandic125, V Mangano36, G L Mansell22, M Manske18, M Mantovani34, F Marchesoni33,126, F Marion8, S Márka39, Z Márka39, A S Markosyan40, E Maros1, F Martelli57,58, L Martellini54, I W Martin36, D V Martynov12, K Mason12, A Masserot8, T J Massinger1, M Masso-Reid36, S Mastrogiovanni28,81, F Matichard1,12, L Matone39, N Mavalvala12, N Mazumder56, R McCarthy37, D E McClelland22, S McCormick7, C McGrath18, S C McGuire127, G McIntyre1, J McIver1, D J McManus22, T McRae22, S T McWilliams31, D Meacher54,74, G D Meadors10,29, J Meidam11, A Melatos128, G Mendell37, D Mendoza-Gandara10, R A Mercer18, E L Merilh37, M Merzougui54, S Meshkov1, C Messenger36, C Messick74, R Metzdorff60, P M Meyers125, F Mezzani28,81, H Miao45, C Michel65, H Middleton45, E E Mikhailov129, L Milano5,67, A L Miller6,28,81, A Miller85, B B Miller85, J Miller12, M Millhouse84, Y Minenkov15, J Ming29, S Mirshekari130, C Mishra17, S Mitra16, V P Mitrofanov49, G Mitselmakher6, R Mittleman12, A Moggi21, M Mohan34, S R P Mohapatra12, M Montani57,58, B C Moore95, C J Moore80, D Moraru37, G Moreno37, S R Morriss87, B Mours8, C M Mow-Lowry45, G Mueller6, A W Muir94, Arunava Mukherjee17, D Mukherjee18, S Mukherjee87, N Mukund16, A Mullavey7, J Munch70, E A M Muniz23, P G Murray36, A Mytidis6, K Napier44, I Nardecchia15,26, L Naticchioni28,81, G Nelemans11,53, T J N Nelson7, M Neri46,47, M Nery10, A Neunzert106, J M Newport3, G Newton36, T T Nguyen22, A B Nielsen10, S Nissanke11,53, A Nitz10, A Noack10, F Nocera34, D Nolting7, M E N Normandin87, L K Nuttall35, J Oberling37, E Ochsner18, E Oelker12, G H Ogin131, J J Oh116, S H Oh116, F Ohme10,94, M Oliver86, P Oppermann10, Richard J Oram7, B O'Reilly7, R O'Shaughnessy107, D J Ottaway70, H Overmier7, B J Owen72, A E Pace74, J Page123, A Pai101, S A Pai48, J R Palamos59, O Palashov113, C Palomba28, A Pal-Singh27, H Pan75, C Pankow85, F Pannarale94, B C Pant48, F Paoletti21,34, A Paoli34, M A Papa10,18,29, H R Paris40, W Parker7, D Pascucci36, A Pasqualetti34, R Passaquieti20,21, D Passuello21, B Patricelli20,21, B L Pearlstone36, M Pedraza1, R Pedurand65,132, L Pekowsky35, A Pele7, S Penn133, C J Perez37, A Perreca1, L M Perri85, H P Pfeiffer97, M Phelps36, O J Piccinni28,81, M Pichot54, F Piergiovanni57,58, V Pierro9, G Pillant34, L Pinard65, I M Pinto9, M Pitkin36, M Poe18, R Poggiani20,21, P Popolizio34, A Post10, J Powell36, J Prasad16, J W W Pratt103, V Predoi94, T Prestegard18,125, M Prijatelj10,34, M Principe9, S Privitera29, G A Prodi92,93, L G Prokhorov49, O Puncken10, M Punturo33, P Puppo28, M Pürrer29, H Qi18, J Qin52, S Qiu120, V Quetschke87, E A Quintero1, R Quitzow-James59, F J Raab37, D S Rabeling22, H Radkins37, P Raffai98, S Raja48, C Rajan48, M Rakhmanov87, P Rapagnani28,81, V Raymond29, M Razzano20,21, V Re26, J Read23, T Regimbau54, L Rei47, S Reid50, D H Reitze1,6, H Rew129, S D Reyes35, E Rhoades103, F Ricci28,81, K Riles106, M Rizzo107, N A Robertson1,36, R Robie36, F Robinet24, A Rocchi15, L Rolland8, J G Rollins1, V J Roma59, J D Romano87, R Romano4,5, J H Romie7, D Rosińska43,134, S Rowan36, A Rüdiger10, P Ruggi34, K Ryan37, S Sachdev1, T Sadecki37, L Sadeghian18, M Sakellariadou135, L Salconi34, M Saleem101, F Salemi10, A Samajdar136, L Sammut120, L M Sampson85, E J Sanchez1, V Sandberg37, J R Sanders35, B Sassolas65, B S Sathyaprakash74,94, P R Saulson35, O Sauter106, R L Savage37, A Sawadsky19, P Schale59, J Scheuer85, E Schmidt103, J Schmidt10, P Schmidt1,51, R Schnabel27, R M S Schofield59, A Schönbeck27, E Schreiber10, D Schuette10,19, B F Schutz29,94, S G Schwalbe103, J Scott36, S M Scott22, D Sellers7, A S Sengupta137, D Sentenac34, V Sequino15,26, A Sergeev113, Y Setyawati11,53, D A Shaddock22, T J Shaffer37, M S Shahriar85, B Shapiro40, P Shawhan64, A Sheperd18, D H Shoemaker12, D M Shoemaker44, K Siellez44, X Siemens18, M Sieniawska43, D Sigg37, A D Silva13, A Singer1, L P Singer68, A Singh10,19,29, R Singh2, A Singhal14, A M Sintes86, B J J Slagmolen22, B Smith7, J R Smith23, R J E Smith1, E J Son116, B Sorazu36, F Sorrentino47, T Souradeep16, A P Spencer36, A K Srivastava89, A Staley39, M Steinke10, J Steinlechner36, S Steinlechner27,36, D Steinmeyer10,19, B C Stephens18, S P Stevenson45, R Stone87, K A Strain36, N Straniero65, G Stratta57,58, S E Strigin49, R Sturani130, A L Stuver7, T Z Summerscales138, L Sun128, S Sunil89, P J Sutton94, B L Swinkels34, M J Szczepańczyk103, M Tacca30, D Talukder59, D B Tanner6, M Tápai102, A Taracchini29, R Taylor1, T Theeg10, E G Thomas45, M Thomas7, P Thomas37, K A Thorne7, E Thrane120, T Tippens44, S Tiwari14,93, V Tiwari94, K V Tokmakov110, K Toland36, C Tomlinson90, M Tonelli20,21, Z Tornasi36, C I Torrie1, D Töyrä45, F Travasso32,33, G Traylor7, D Trifirò73, J Trinastic6, M C Tringali92,93, L Trozzo21,139, M Tse12, R Tso1, M Turconi54, D Tuyenbayev87, D Ugolini140, C S Unnikrishnan104, A L Urban1, S A Usman94, H Vahlbruch19, G Vajente1, G Valdes87, N van Bakel11, M van Beuzekom11, J F J van den Brand11,63, C Van Den Broeck11, D C Vander-Hyde35, L van der Schaaf11, J V van Heijningen11, A A van Veggel36, M Vardaro41,42, V Varma51, S Vass1, M Vasúth38, A Vecchio45, G Vedovato42, J Veitch45, P J Veitch70, K Venkateswara141, G Venugopalan1, D Verkindt8, F Vetrano57,58, A Viceré57,58, A D Viets18, S Vinciguerra45, D J Vine50, J-Y Vinet54, S Vitale12, T Vo35, H Vocca32,33, C Vorvick37, D V Voss6, W D Vousden45, S P Vyatchanin49, A R Wade1, L E Wade78, M Wade78, M Walker2, L Wallace1, S Walsh10,29, G Wang14,58, H Wang45, M Wang45, Y Wang52, R L Ward22, J Warner37, M Was8, J Watchi82, B Weaver37, L-W Wei54, M Weinert10, A J Weinstein1, R Weiss12, L Wen52, P Weßels10, T Westphal10, K Wette10, J T Whelan107, B F Whiting6, C Whittle120, D Williams36, R D Williams1, A R Williamson94, J L Willis142, B Willke10,19, M H Wimmer10,19, W Winkler10, C C Wipf1, H Wittel10,19, G Woan36, J Woehler10, J Worden37, J L Wright36, D S Wu10, G Wu7, W Yam12, H Yamamoto1, C C Yancey64, M J Yap22, Hang Yu12, Haocun Yu12, M Yvert8, A Zadrożny118, L Zangrando42, M Zanolin103, J-P Zendri42, M Zevin85, L Zhang1, M Zhang129, T Zhang36, Y Zhang107, C Zhao52, M Zhou85, Z Zhou85, S J Zhu10,29, X J Zhu52, M E Zucker1,12, J Zweizig1 (LIGO Scientific Collaboration, Virgo Collaboration), M Boyle143, T Chu97, D Hemberger51, I Hinder29, L E Kidder143, S Ossokine29, M Scheel51, B Szilagyi51, S Teukolsky143 and A Vano Vinuales94 Hide full author list Published 12 April 2017 • © 2017 IOP Publishing Ltd Classical and Quantum Gravity, Volume 34, Number 10 Focus Issue: Gravitational Waves Article PDF Figures References Citations PDF 258 Total downloads Cited by 1 articles Article has an altmetric score of 3 Turn on MathJax Get permission to re-use this article Share this article Article information Abstract Parameter estimates of GW150914 were obtained using Bayesian inference, based on three semi-analytic waveform models for binary black hole coalescences. These waveform models differ from each other in their treatment of black hole spins, and all three models make some simplifying assumptions, notably to neglect sub-dominant waveform harmonic modes and orbital eccentricity. Furthermore, while the models are calibrated to agree with waveforms obtained by full numerical solutions of Einstein's equations, any such calibration is accurate only to some non-zero tolerance and is limited by the accuracy of the underlying phenomenology, availability, quality, and parameter-space coverage of numerical simulations. This paper complements the original analyses of GW150914 with an investigation of the effects of possible systematic errors in the waveform models on estimates of its source parameters. To test for systematic errors we repeat the original Bayesian analysis on mock signals from numerical simulations of a series of binary configurations with parameters similar to those found for GW150914. Overall, we find no evidence for a systematic bias relative to the statistical error of the original parameter recovery of GW150914 due to modeling approximations or modeling inaccuracies. However, parameter biases are found to occur for some configurations disfavored by the data of GW150914: for binaries inclined edge-on to the detector over a small range of choices of polarization angles, and also for eccentricities greater than ~0.05. For signals with higher signal-to-noise ratio than GW150914, or in other regions of the binary parameter space (lower masses, larger mass ratios, or higher spins), we expect that systematic errors in current waveform models may impact gravitational-wave measurements, making more accurate models desirable for future observations

All-sky search for long-duration gravitational wave transients in the first Advanced LIGO observing run

We present the results of a search for long-duration gravitational wave transients in the data of the LIGO Hanford and LIGO Livingston second generation detectors between September 2015 and January 2016 , with a total observational time of 49 d. The search targets gravitational wave transients of 10 – 500 s duration in a frequency band of 24 – 2048 Hz, with minimal assumptions about the signal waveform, polarization, source direction, or time of occurrence. No significant events were observed. As a result we set 90% confidence upper limits on the rate of long-duration gravitational wave transients for different types of gravitational wave signals. We also show that the search is sensitive to sources in the Galaxy emitting at least ∼ 10 − 8 M c 2 in gravitational waves

All-sky search for short gravitational-wave bursts in the first Advanced LIGO run

We present the results from an all-sky search for short-duration gravitational waves in the data of the first run of the Advanced LIGO detectors between September 2015 and January 2016. The search algorithms use minimal assumptions on the signal morphology, so they are sensitive to a wide range of sources emitting gravitational waves. The analyses target transient signals with duration ranging from milliseconds to seconds over the frequency band of 32 to 4096 Hz. The first observed gravitational-wave event, GW150914, has been detected with high confidence in this search; the other known gravitational-wave event, GW151226, falls below the search’s sensitivity. Besides GW150914, all of the search results are consistent with the expected rate of accidental noise coincidences. Finally, we estimate rate-density limits for a broad range of non-binary-black-hole transient gravitational-wave sources as a function of their gravitational radiation emission energy and their characteristic frequency. These rate-density upper limits are stricter than those previously published by an order of magnitude