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Wagner, A, Drout, MR, Eifler, TF, Estrada, J, Evrard, AE, Fernandez, E, Finley, DA, Flaugher, B, Foley, RJ, Fong, W-F, Fosalba, P, Fox, DB, Frieman, J, Fryer, CL, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, Herner, K, Honscheid, K, James, DJ, Johnson, MD, Johnson, MWG, Karliner, I, Kasen, D, Kent, S, Kessler, R, Kim, AG, Kind, MC, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Margutti, R, Marriner, J, Martini, P, Matheson, T, Melchior, P, Metzger, BD, Miller, CJ, Miquel, R, Neilsen, E, Nichol, RC, Nord, B, Nugent, P, Ogando, R, Petravick, D, Plazas, AA, Quataert, E, Roe, N, Romer, AK, Roodman, A, Rosell, AC, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Sheldon, E, Smith, N, Smith, RC, Soares-Santos, M, Sobreira, F, Stebbins, A, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Thomas, RC, Tucker, DL, Vikram, V, Walker, AR, Wechsler, RH, Wester, W, Yanny, B, Zhang, Y, Zuntz, J, Survey, FTDE, Connaughton, TDECGW-EMCV, Burns, E, Goldstein, A, Briggs, MS, Zhang, B-B, Hui, CM, Jenke, P, Wilson-Hodge, CA, Bhat, PN, Bissaldi, E, Cleveland, W, Fitzpatrick, G, Giles, MM, Gibby, MH, Greiner, J, Kienlin, AV, Kippen, RM, McBreen, S, Mailyan, B, Meegan, CA, Paciesas, WS, Preece, RD, Roberts, O, Sparke, L, Stanbro, M, Toelge, K, Veres, P, Yu, H-F, Blackburn, L, Ackermann, FTFGBMCM, Ajello, M, Albert, A, Anderson, B, Atwood, WB, Axelsson, M, Baldini, L, Barbiellini, G, Bastieri, D, Bellazzini, R, Bissaldi, E, Blandford, RD, Bloom, ED, Bonino, R, Bottacini, E, Brandt, TJ, Bruel, P, Buson, S, Caliandro, GA, Cameron, RA, Caragiulo, M, Caraveo, PA, Cavazzuti, E, Charles, E, Chekhtman, A, Chiang, J, Chiaro, G, Ciprini, S, Cohen-Tanugi, J, Cominsky, LR, Costanza, F, Cuoco, A, D'Ammando, F, Palma, FD, Desiante, R, Digel, SW, Lalla, ND, Mauro, MD, Venere, LD, Domínguez, A, Drell, PS, Dubois, R, Favuzzi, C, Ferrara, EC, Franckowiak, A, Fukazawa, Y, Funk, S, Fusco, P, Gargano, F, Gasparrini, D, Giglietto, N, Giommi, P, Giordano, F, Giroletti, M, Glanzman, T, Godfrey, G, Gomez-Vargas, GA, Green, D, Grenier, IA, Grove, JE, Guiriec, S, Hadasch, D, Harding, AK, Hays, E, Hewitt, JW, Hill, AB, Horan, D, Jogler, T, Jóhannesson, G, Johnson, AS, Kensei, S, Kocevski, D, Kuss, M, Mura, GL, Larsson, S, Latronico, L, Li, J, Li, L, Longo, F, Loparco, F, Lovellette, MN, Lubrano, P, Magill, J, Maldera, S, Manfreda, A, Marelli, M, Mayer, M, Mazziotta, MN, McEnery, JE, Meyer, M, Michelson, PF, Mirabal, N, Mizuno, T, Moiseev, AA, Monzani, ME, Moretti, E, Morselli, A, Moskalenko, IV, Negro, M, Nuss, E, Ohsugi, T, Omodei, N, Orienti, M, Orlando, E, Ormes, JF, Paneque, D, Perkins, JS, Pesce-Rollins, M, Piron, F, Pivato, G, Porter, TA, Racusin, JL, Rainò, S, Rando, R, Razzaque, S, Reimer, A, Reimer, O, Salvetti, D, Parkinson, PMS, Sgrò, C, Simone, D, Siskind, EJ, Spada, F, Spandre, G, Spinelli, P, Suson, DJ, Tajima, H, Thayer, JB, Thompson, DJ, Tibaldo, L, Torres, DF, Troja, E, Uchiyama, Y, Venters, TM, Vianello, G, Wood, KS, Wood, M, Zhu, S, Zimmer, S, Brocato, FTFLATCE, Cappellaro, E, Covino, S, Grado, A, Nicastro, L, Palazzi, E, Pian, E, Amati, L, Antonelli, LA, Capaccioli, M, D'Avanzo, P, D'Elia, V, Getman,

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F, Giuffrida, G, Iannicola, G, Limatola, L, Lisi, M, Marinoni, S, Marrese, P, Melandri, A, Piranomonte, S, Possenti, A, Pulone, L, Rossi, A, Stamerra, A, Stella, L, Testa, V, Tomasella, L, Yang, S, TeAm, FTGWI, Bazzano, A, Bozzo, E, Brandt, S, Courvoisier, TJ-L, Ferrigno, C, Hanlon, L, Kuulkers, E, Laurent, P, Mereghetti, S, Roques, JP, Savchenko, V, Ubertini, P, Kasliwal, FTINTEGRALCMM, Singer, LP, Cao, Y, Duggan, G, Kulkarni, SR, Bhalerao, V, Miller, AA, Barlow, T, Bellm, E, Manulis, I, Rana, J, Laher, R, Masci, F, Surace, J, Rebbapragada, U, Cook, D, Sistine, AV, Sesar, B, Perley, D, Ferreti, R, Prince, T, Kendrick, R, Horesh, A, Factory, FTIPT, Hurley, CK, Golenetskii, SV, Aptekar, RL, Frederiks, DD, Svinkin, DS, Rau, A, Kienlin, AV, Zhang, X, Smith, DM, Cline, T, Krimm, H, Abe, FTINF, Doi, M, Fujisawa, K, Kawabata, KS, Morokuma, T, Motohara, K, Tanaka, M, Ohta, K, Yanagisawa, K, Yoshida, M, Baltay, FTJ-GEMCC, Bersier, D, Bode, MF, Collins, CA, Copperwheat, CM, Darnley, MJ, Galloway, DK, Gomboc, A, Kobayashi, S, Mazzali, PA, Mundell, CG, Piascik, AS, Pollacco, D, Steele, IA, Ulaczyk, K, Jonker, PG, Rowlinson, A, Stappers, BW, Wijers, RAMJ, Array, FTLF, Lipunov, CV, Gorbovskoy, E, Tyurina, N, Kornilov, V, Balanutsa, P, Kuznetsov, A, Buckley, D, Rebolo, R, Serra-Ricart, M, Israelian, G, Budnev, NM, Gress, O, Ivanov, K, Poleshuk, V, Tlatov, A, Yurkov, V, Kawai, FTMASTERCN, Serino, M, Negoro, H, Nakahira, S, Mihara, T, Tomida, H, Ueno, S, Tsunemi, H, Matsuoka, M, Croft, FTMAXICS, Feng, L, Franzen, TMO, Gaensler, BM, Johnston-Hollitt, M, Kaplan, DL, Morales, MF, Tingay, SJ, Wayth, RB, Williams, A, Array, FTMW-F, Smartt, CSJ, Chambers, KC, Smith, KW, Huber, ME, Young, DR, Wright, DE, Coughlin, M, Schultz, A, Denneau, L, Flewelling, H, Magnier, EA, Primak, N, Rest, A, Sherstyuk, A, Stalder, B, Stubbs, CW, Tonry, J, Waters, C, Willman, M, for, TP-SCFOE, Campbell, H, Kotak, R, Sollerman, J, Smith, M, Dennefeld, M, Anderson, JP, Botticella, MT, Chen, T-W, Valle, MD, Elias-Rosa, N, Fraser, M, Inserra, C, Kankare, E, Kupfer, T, Harmanen, J, Galbany, L, Guillou, LL, Lyman, JD, Maguire, K, Mitra, A, Nicholl, M, Razza, A, Terreran, G, Valenti, S, Gal-Yam, A, Ćwiek, FTPESSTOCA, Ćwiok, M, Mankiewicz, L, Opiela, R, Zaremba, M, Żarnecki, AF, Scalzo, FTPOTSCRA, Schmidt, BP, Wolf, C, Yuan, F, Evans, FTSCPA, Kennea, JA, Burrows, DN, Campana, S, Cenko, SB, Giommi, P, Marshall, FE, Nousek, J, O'Brien, P, Osborne, JP, Palmer, D, Perri, M, Racusin, J, Siegel, M, Tagliaferri, G, Klotz, FTSCA, Turpin, D, Laugier, R, TAROT, FT, Zadko, , Observatory, AN, Beroiz, CCM, Peñuela, T, Macri, LM, Oelkers, RJ, Lambas, DG, Vrech, R, Cabral, J, Colazo, C, Dominguez, M, Sanchez, B, Gurovich, S, Lares, M, Marshall, JL, DePoy, DL, Padilla, N, Pereyra, NA, Benacquista, M, Key, JS, Tanvir, FTTOROSCNR, Wiersema, K, Levan, AJ, Steeghs, D, Hjorth, J, Fynbo, JPU, Malesani, D, Milvang-Jensen, B, Watson, D, Greiner, J, Irwin, M, Fernandez, CG, McMahon, RG, Banerji, M, Gonzalez-Solares, E, Schulze, S, Postigo, ADU, Thoene, CC, Cano, Z, Rosswog, S and Collaboration, FTVISTA

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Localization and broadband follow-up of the gravitational-wave transient GW150914

http://researchonline.ljmu.ac.uk/id/eprint/3076/

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Abbott, BP, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, RX, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, B, Allocca, A, Altin, PA, Anderson, SB, Anderson, WG, Arai, K, Araya, MC, Arceneaux, CC, Areeda, JS, Arnaud, N, Arun, KG,

THE ASTROPHYSICAL JOURNAL LETTERS, IN PRESSPreprint typeset using LATEX style AASTeX6 v. 1.0

LOCALIZATION AND BROADBAND FOLLOW-UP OF THE GRAVITATIONAL-WAVE TRANSIENT GW150914

THE LIGO SCIENTIFIC COLLABORATION AND THE VIRGO COLLABORATION,THE AUSTRALIAN SQUARE KILOMETER ARRAY PATHFINDER (ASKAP) COLLABORATION, THE BOOTES COLLABORATION,

THE DARK ENERGY SURVEY AND THE DARK ENERGY CAMERA GW-EM COLLABORATIONS, THE Fermi GBM COLLABORATION,THE Fermi LAT COLLABORATION, THE GRAVITATIONAL WAVE INAF TEAM (GRAWITA), THE INTEGRAL COLLABORATION,

THE INTERMEDIATE PALOMAR TRANSIENT FACTORY (IPTF) COLLABORATION, THE INTERPLANETARY NETWORK,THE J-GEM COLLABORATION, THE LA SILLA–QUEST SURVEY, THE LIVERPOOL TELESCOPE COLLABORATION,

THE LOW FREQUENCY ARRAY (LOFAR) COLLABORATION, THE MASTER COLLABORATION, THE MAXI COLLABORATION,THE MURCHISON WIDE-FIELD ARRAY (MWA) COLLABORATION, THE PAN-STARRS COLLABORATION,

THE PESSTO COLLABORATION, THE PI OF THE SKY COLLABORATION, THE SKYMAPPER COLLABORATION,THE Swift COLLABORATION, THE TAROT, ZADKO, ALGERIAN NATIONAL OBSERVATORY, AND C2PU COLLABORATION,

THE TOROS COLLABORATION, AND THE VISTA COLLABORATION

See the end matter for the full list of authors.

(Received 2016 February 29; Accepted 2016 April 26)

ABSTRACT

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser InterferometerGravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designatedG184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, prelim-inary estimates of the time, significance, and sky location of the event were shared with 63 teams of observerscovering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facil-ities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization ofthe first observed compact binary merger. We summarize the follow-up observations reported by 25 teams viaprivate Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GWsky localization coverage, the timeline and depth of the observations. As this event turned out to be a binaryblack hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, thisfirst broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone andhighlights the broad capabilities of the transient astronomy community and the observing strategies that havebeen developed to pursue neutron star binary merger events. Detailed investigations of the EM data and resultsof the EM follow-up campaign are being disseminated in papers by the individual teams.Keywords: gravitational waves; methods: observational

1. INTRODUCTION

In 2015 September, the Advanced Laser Interferom-eter Gravitational-wave Observatory (LIGO; Aasi et al.2015) made the first direct detection of an astrophysicalgravitational-wave (GW) signal that turned out to be froma binary black hole (BBH) merger. The LIGO Hanfordand Livingston sites are the first two nodes of a growingglobal network of highly sensitive GW facilities, soon toinclude Advanced Virgo (Acernese et al. 2015), KAGRA,and LIGO–India. Some of the most promising astrophysicalsources of GWs are also expected to produce broadband elec-tromagnetic (EM) emission and neutrinos. This has createdexciting new opportunities for joint broadband EM observa-tions and multi-messenger astronomy.

In a compact binary coalescence (CBC) event, a tight binarycomprised of two neutron stars (NSs), two black holes (BHs),

lsc-spokesperson@ligo.orgvirgo-spokesperson@ego-gw.eu

or a NS and a BH experiences a runaway orbital decay dueto gravitational radiation. In a binary including at least oneNS— a binary neutron star (BNS) or neutron star–black hole(NSBH) merger—we expect EM signatures due to energeticoutflows at different timescales and wavelengths. If a rela-tivistic jet forms, we may observe a prompt short gamma-rayburst (GRB) lasting on the order of one second or less, fol-lowed by X-ray, optical, and radio afterglows of hours to daysduration (e.g., Eichler et al. 1989; Narayan et al. 1992; Nakar2007; Berger 2014; Fong et al. 2015). Rapid neutron capturein the sub-relativistic ejecta (e.g., Lattimer & Schramm 1976)is hypothesized to produce a kilonova or macronova, an op-tical and near-infrared signal lasting hours to weeks (e.g., Li& Paczynski 1998). Eventually, we may observe a radio blastwave from this sub-relativistic outflow, detectable for monthsto years (e.g., Nakar & Piran 2011). Furthermore, several sec-onds prior to or tens of minutes after merger, we may seea coherent radio burst lasting milliseconds (e.g., Hansen &Lyutikov 2001; Zhang 2014). In short, a NS binary can pro-

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duce EM radiation over a wide range of wavelengths and timescales. On the other hand, in the case of a stellar-mass BBH,the current consensus is that no significant EM counterpartemission is expected except for those in highly improbableenvironments pervaded by large ambient magnetic fields orbaryon densities.

The first campaign to find EM counterparts triggered bylow-latency GW event candidates was carried out with the ini-tial LIGO and Virgo detectors and several EM astronomy fa-cilities in 2009 and 2010 (Abadie et al. 2012a,b; Evans et al.2012; Aasi et al. 2014). In preparing for Advanced detec-tor operations, the LIGO and Virgo collaborations workedwith the broader astronomy community to set up an evolvedand greatly expanded EM follow-up program.1 Seventy-four groups with access to ground- and space-based facili-ties joined, of which 63 were operational during AdvancedLIGO’s first observing run (O1). Details of the 2009 to 2010EM follow campaign and changes for O1 are given in Sec-tion 1 of the Supplement (Abbott et al. 2016g).

After years of construction and commissioning, the Ad-vanced LIGO detectors at Livingston, Louisiana, and Han-ford, Washington, began observing in 2015 September withabout 3.5 times the distance reach (> 40 times the sensitivevolume) of the earlier detectors. A strong GW event was iden-tified shortly after the pre-run calibration process was com-pleted. Deep analysis of this event, initially called G184098and later given the name GW150914, is presented in Abbottet al. (2016c) and companion papers referenced therein. Inthis paper we describe the initial low-latency analysis andevent candidate selection (Section 2), the rapid determina-tion of likely sky localization (Section 3), and the follow-up EM observations carried out by partner facilities (Sec-tions 4 and 5). For analyses of those observations, we referthe reader to the now-public Gamma-ray Coordinates Net-work (GCN) circulars2 and to a number of recent papers.We end with a brief discussion of EM counterpart detectionprospects for future events.

2. DATA ANALYSIS AND DISCOVERY

As configured for O1, four low-latency pipelines contin-ually search for transient signals that are coincident in thetwo detectors within the 10 ms light travel time separatingthem. Coherent WaveBurst (cWB; Klimenko et al. 2016) andOmicron+LALInference Burst (oLIB; Lynch et al. 2015) bothsearch for unmodeled GW bursts (Abbott et al. 2016d). GST-LAL (Cannon et al. 2012; Messick et al. 2016) and Multi-Band Template Analysis (MBTA; Adams et al. 2015) searchspecifically for NS binary mergers using matched filtering.Because CBC waveforms can be precisely computed fromgeneral relativity, GSTLAL and MBTA are more sensitive to

1 See program description and participation information at http://www.ligo.org/scientists/GWEMalerts.php.

2 All circulars related to GW150914 are collected at http://gcn.gsfc.nasa.gov/other/GW150914.gcn3

CBC signals than the burst search pipelines are. All four de-tection pipelines report candidates within a few minutes ofdata acquisition.

LIGO conducted a series of engineering runs throughoutAdvanced LIGO’s construction and commissioning to pre-pare to collect and analyze data in a stable configuration. Theeighth engineering run (ER8) began on 2015 August 17 at15:00 and critical software was frozen by August 30.3 Therest of ER8 was to be used to calibrate the detectors, to carryout diagnostic studies, to practice maintaining a high coin-cident duty cycle, and to train and tune the data analysispipelines. Calibration was complete by September 12 and O1was scheduled to begin on September 18. On 2015 Septem-ber 14, cWB reported a burst candidate to have occurred at09:50:45 with a network signal-to-noise ratio (S/N) of 23.45and an estimated false alarm rate (FAR) < 0.371 yr−1 basedon the available (limited at that time) data statistics. Also,oLIB reported a candidate with consistent timing and S/N.No candidates were reported at this time by the low-latencyGSTLAL and MBTA pipelines, ruling out a BNS or NSBHmerger.

Although the candidate occurred before O1 officially be-gan, the LIGO and Virgo collaborations decided to send analert to partner facilites because the preliminary FAR esti-mate satisfied our planned alert threshold of 1 month−1. Al-though we had not planned to disseminate real-time GCN no-tices before the formal start of O1, most of the computinginfrastructure was in place. Basic data quality checks weredone within hours of GW150914; both interferometers werestable and the data stream was free of artifacts (Abbott et al.2016a). A cWB sky map was available 17 minutes after thedata were recorded, and a LALInference Burst (LIB) sky mapwas available after 14 hr. After extra data integrity checks andan update to the GCN server software, these two sky mapswere communicated to observing partners in a GCN circu-lar nearly two days after the event occurred (GCN 18330).Mass estimates were not released in this initial circular, andobservers may have assumed the event was associated with aBNS system or a GW burst (e.g., from a nearby core-collapsesupernova; SN). The knowledge that GW150914 was consis-tent with a BBH inspiral and merger was only shared later onOctober 3 (GCN 18388). Figure 1 shows the chronology ofthe GW detection alerts and follow-up observations.

The data were re-analyzed offline with two independentmatched-filter searches using a template bank that includesboth NS binary and BBH mergers. The waveform was con-firmed to be consistent with a BBH merger and this informa-tion was shared with observers about three weeks after theevent (GCN 18388). The FAR was evaluated with the datacollected through 20 October, reported to be less than 1 in100 years (GCN 18851; Abbott et al. 2016b), and ultimatelydetermined to be much lower. The final results of the offline

3 All dates and times are in UT.

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 3

100 101 102

t− tmerger (days)

Initial GWBurst Recovery

InitialGCN Circular

Updated GCN Circular(identified as BBH candidate)

Finalsky map

Fermi GBM, LAT, MAXI,IPN, INTEGRAL (archival)

SwiftXRT

SwiftXRT

Fermi LAT,MAXI

BOOTES-3 MASTER Swift UVOT, SkyMapper, MASTER, TOROS, TAROT, VST, iPTF, Keck,Pan-STARRS1, KWFC, QUEST, DECam, LT, P200, Pi of the Sky, PESSTO, UH

Pan-STARRS1VST TOROS

VISTA

MWA ASKAP,LOFAR

ASKAP,MWA

VLA,LOFAR

VLA,LOFAR VLA

Figure 1. Timeline of observations of GW150914, separated by band and relative to the time of the GW trigger. The top row showsGW information releases. The bottom four rows show high-energy, optical, near-infrared, and radio observations, respectively.Optical spectroscopy and narrow-field radio observations are indicated with darker tick marks and boldface text. Table 1 reportsmore detailed information on the times of observations made with each instrument.

search are reported in Abbott et al. (2016c).

3. SKY MAPS

We produce and disseminate probability sky maps using asequence of algorithms with increasing accuracy and compu-tational cost. Here, we compare four location estimates: theprompt cWB and LIB localizations that were initially sharedwith observing partners plus the rapid BAYESTAR localiza-tion and the final localization from LALInference. All fourare shown in Fig. 2.

cWB performs a constrained maximum likelihood estimateof the reconstructed signal on a sky grid (Klimenko et al.2016) weighted by the detectors’ antenna patterns (Essicket al. 2015) and makes minimal assumptions about the wave-form morphology. With two detectors, this amounts to re-stricting the signal to only one of two orthogonal GW polar-izations throughout most of the sky. LIB performs Bayesianinference assuming the signal is a sinusoidally modulatedGaussian (Lynch et al. 2015). While this assumption may notperfectly match the data, it is flexible enough to produce reli-able localizations for a wide variety of waveforms, includingBBH inspiral-merger-ringdown signals (Essick et al. 2015).BAYESTAR produces sky maps by triangulating the times,amplitudes, and phases on arrival supplied by all the CBCpipelines (Singer & Price 2016). BAYESTAR was not avail-able promptly because the low-latency CBC searches werenot configured for BBHs; the localization presented here isderived from the offline CBC search. LALInference performsfull forward modeling of the data using a parameterized CBCwaveform which allows for BH spins and detector calibra-tion uncertainties (Veitch et al. 2015). It is the most accuratemethod for CBC signals but takes the most time due to thehigh dimensionality. We present the same LALInference mapas Abbott et al. (2016e), with a spline interpolation proce-

dure to include the potential effects of calibration uncertain-ties. The BAYESTAR and LALInference maps were sharedwith observers on 2016 January 13 (GCN 18858), at the con-clusion of the O1 run. Since GW150914 is a CBC event, weconsider the LALInference map to be the most accurate, au-thoritative, and final localization for this event. This map hasa 90% credible region with area 630 deg2.

All of the sky maps agree qualitatively, favoring a broad,long section of arc in the southern hemisphere and to a lesserextent a shorter section of nearly the same arc near the equa-tor. While the majority of LIB’s probability is concentratedin the southern hemisphere, a non-trivial fraction of the 90%confidence region extends into the northern hemisphere. TheLALInference sky map shows much less support in the north-ern hemisphere which is likely associated with the strongerconstraints available with full CBC waveforms. The cWB lo-calization also supports an isolated hot spot near α ∼ 9h, δ ∼5◦, where the detector responses make it possible to indepen-dently measure two polarization components. In this region,cWB considers signals not constrained to have the ellipticalpolarization expected from a compact binary merger.

Quantitative comparisons of the four sky maps can be foundin section 2 of the Supplement (Abbott et al. 2016g). Themain feature in all of the maps is an annulus with polar an-gle θHL determined by the arrival time difference ∆tHL be-tween the two detectors. However, refinements are possibledue to phase as well as amplitude consistency and the mildlydirectional antenna patterns of the LIGO detectors (Kasli-wal & Nissanke 2014; Singer et al. 2014). In particular, thedetectors’ antenna patterns dominate the modulation aroundthe ring for un-modeled reconstructions through a correlationwith the inferred distance of the source (Essick et al. 2015).As shown in Fig. 2, the algorithms all infer polar angles thatare consistent at the 1σ level.

4

∆tHL, θHLcWB

LIBBAYESTAR

LALInference

4h

8h

12h

16h

20h24h

7.7ms

7.1ms

6.4ms

40° 45° 50°

Figure 2. Comparison of different GW sky maps, showing the 90% credible level contours for each algorithm. This is anorthographic projection centered on the centroid of the LIB localization. The inset shows the distribution of the polar angle θHL

(equivalently, the arrival time difference ∆tHL).

4. FOLLOW-UP OBSERVATIONS

Twenty-five participating teams of observers responded tothe GW alert to mobilize satellites and ground-based tele-scopes spanning 19 orders of magnitude in EM wavelength.Observations and archival analysis started shortly after thecandidate was announced, two days after the event wasrecorded. Most facilities followed tiling strategies based onthe cWB and LIB sky maps. Some groups, considering the

possibility of a NS merger or core-collapse SN, selected fieldsbased on the areal density of nearby galaxies or targeted theLarge Magellanic Cloud (LMC) (e.g., Annis et al. 2016). Hadthe BBH nature of the signal been promptly available, mostgroups would not have favored local galaxies because LIGO’srange for BBH mergers is many times larger than that forBNSs. Fig. 3 displays the footprints of all reported obser-vations. The campaign is summarized in Table 1 in terms of

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 5

Sun

Moon

GWradio

optical/IRX-ray

γ-ray (all-sky)

4h

8h

12h

16h

20h24h

Figure 3. Footprints of observations in comparison with the 50% and 90% credible levels of the initially distributed GW local-ization maps. Radio fields are shaded in red, optical/infrared fields are in green, and the XRT fields are indicated by the bluecircles. The all-sky Fermi GBM, LAT, INTEGRAL SPI-ACS, and MAXI observations are not shown. Where fields overlap, theshading is darker. The initial cWB localization is shown as thin black contour lines and the LIB localization as thick black lines.The inset highlights the Swift observations consisting of a hexagonal grid and a selection of the a posteriori most highly rankedgalaxies. The Schlegel et al. (1998) reddening map is shown in the background to represent the Galactic plane. The projection isthe same as in Fig. 2.

instruments, depth, time, and sky coverage. Some optical can-didate counterparts were followed up spectroscopically and inthe radio band as summarized in Table 2. The overall EMfollow-up of GW150914 consisting of broad-band tiled ob-

servations and observations to characterize candidate coun-terparts are described in detail in Sections 3 through 5 of theSupplement (Abbott et al. 2016g).

Findings from these follow-up observations have been re-

6

ported in several papers. A weak transient signal was foundin Fermi GBM data 0.4 s after the time of GW150914 (Con-naughton et al. 2016), but no corresponding signal was foundin the INTEGRAL SPI–ACS instrument (Savchenko et al.2016) or AGILE (Tavani et al. 2016). No GRB-like after-glow was found in X-rays with Swift XRT (Evans et al. 2016)or MAXI (N. Kawai et al., in preparation), in UV/opticalwith Swift UVOT (Evans et al. 2016), or at GeV energieswith Fermi LAT (Ackermann et al. 2016). Tiled observationswith wide-field optical instruments listed in Table 1 foundmany transients, but spectroscopy with the instruments listedin Table 2 along with further photometry showed that none ofthem were associated with GW150914 (Kasliwal et al. 2016;Smartt et al. 2016; Soares-Santos et al. 2016; Morokuma et al.2016). Annis et al. (2016) used DECam to search for a miss-ing supergiant in the LMC, which would have been evidencefor the collapse of a massive star that could have producedGWs, but failed to produce a typical core-collapse SN.

5. COVERAGE

Using the GW data alone, we can only constrain the posi-tion of the source on the sky to an area of ≈600 deg2 (90%confidence). The inferred redshift is z = 0.09+0.03

−0.04, corre-sponding to a luminosity distance of 410+160

−180 Mpc (Abbottet al. 2016e).

Table 1 lists the area tiled by each facility and the probabil-ity contained within those tiles, calculated with respect to thelocalization methods described in Section 3.

By far the most complete coverage of the area is at the high-est energies. The INTEGRAL SPI–ACS provided the largesteffective area in the 75 keV–1 MeV range, albeit with signifi-cantly varying detection efficiency. Owing to its nearly omni-directional response, it had a full coverage of the GW proba-bility map (GCN 18354; Savchenko et al. 2016). Fermi GBMcaptured 75% of the localization at the time of the GW triggerand the entire area by 25 minutes after (GCN 18339). FermiLAT observations started 4200 s after the trigger and the entirelocalization continued to be observed every three hours.

Coverage in X-rays is complete down to 10−9 erg cm−2 s−1

with the MAXI observations, but relatively sparse atfainter flux, with the Swift XRT tiles spanning about5 deg2 and enclosing a probability of ∼0.3% in the energyrange 0.3–10 keV to a depth of 10−13–10−11 erg cm−2 s−1

(GCNs 18331, 18346).Optical facilities together tiled about 900 deg2 and cap-

tured a containment probability of over 50% of the initialLIB sky map and slightly less for the final LALInference skymap that was available after the observations were completed.The depth varies widely among these facilities. MASTERand Pan-STARRS1 covered the most area with their observa-tions, while large areas also were covered by the intermedi-ate Palomar Transient Factory (iPTF), Dark Energy Camera(DECam), VLT Survey Telescope (VST@ESO; E. Brocato etal. 2016, in preparation), and La Silla–QUEST. The contained

probability of the initial sky maps is dominated by MASTER,DECam, Pan-STARRS1, La Silla–QUEST, and VST@ESO,while the final sky map is contained best by MASTER,DECam and VST@ESO. Relatively small area and containedprobability were covered by facilities that targeted nearbygalaxies. The only wide-field near-infrared facility, the Vis-ible and Infrared Survey Telescope (VISTA@ESO), covered70 deg2 and captured a containment probability of 8% of thefinal LALInference sky map.

The radio coverage is also extensive, with a contained prob-ability of 86%, dominated by Murchison Widefield Array(MWA) in the 118 MHz band (GCN 18345).

Table 2 lists the observations done by large telescope spec-trographs and a radio facility to follow-up candidate opti-cal counterparts. Deep photometry, broadband observations,and spectroscopy identified the majority of the candidates tobe normal population type Ia and type II SNe, with a fewdwarf novae and active galactic nuclei (AGNs) that are allvery likely unrelated to GW150914. Candidate classifica-tion, comparison of redshift with the GW distance, and useof source age are crucial constraints to rule candidates inand out. Detailed discussions of candidate selection, spec-troscopic and broadband follow-up are presented in survey-specific publications about iPTF candidates (Kasliwal et al.2016) and about PESSTO follow-up of Pan-STARRS1 candi-dates (Smartt et al. 2016).

6. SENSITIVITY

The third column of Table 1 summarizes the depth of thefollow-up program. We provide limiting flux, flux density, ormagnitude for the different facilities. We emphasize that theselimits only apply to the fraction of the sky contours that havebeen followed up. For example, the MWA fields have an 86%chance of containing the source’s sky location and provide noconstraints on sky locations representing the remaining 14%.

Because the follow-up program was primarily designed tosearch for counterparts to BNS and NSBH mergers, it is in-teresting to note that the observational campaign would haveprovided powerful constraints on such a system. A BNS co-alescence could have been detected by LIGO during O1 at adistance of ∼ 70 Mpc, averaged over sky position and orienta-tions (Martynov et al. 2016). A short GRB afterglow similarto those that have been observed by Swift XRT would havebeen detectable at that distance. Re-scaling the observed X-ray fluxes of short GRBs at 11 hr after the event would yieldfluxes in the range 2×10−11 to 6×10−8 erg cm−2 s−1 (Berger2014). Kilonova emission from a BNS merger at that distancewould reach a peak apparent magnitude of 17–24 within aweek or two after the merger (e.g., Metzger et al. 2010; Barnes& Kasen 2013; Tanaka & Hotokezaka 2013; Grossman et al.2014). This range overlaps with the depth reached in the op-tical and near-IR bands. Finally, this BNS system might pro-duce radio emission from tens of µJy to tens of mJy (e.g.,Hotokezaka & Piran 2015) with different timescales spanning

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 7

Table 1. Summary of Tiled Observations

Facility/ Area Contained Probability (%)Instrument Banda Depthb Timec (deg2) cWB LIB BSTRd LALInf GCN

Gamma-ray

Fermi LAT 20 MeV– 1.7 × 10−9 (every — 100 100 100 100 18709300 GeV 3 hr)

Fermi GBM 8 keV–40 MeV 0.7–5 × 10−7 (archival) — 100 100 100 100 18339(0.1–1 MeV)

INTEGRAL 75 keV–1 MeV 1.3 × 10−7 (archival) — 100 100 100 100 18354IPN 15 keV–10 MeV 1 × 10−7 (archival) — 100 100 100 100 —

X-ray

MAXI/GSC 2–20 keV 1 × 10−9 (archival) 17900 95 89 92 84 19013Swift XRT 0.3–10 keV 5 × 10−13 (gal.) 2.3, 1, 1 0.6 0.03 0.18 0.04 0.05 18331

2–4 × 10−12 (LMC) 3.4, 1, 1 4.1 1.2 1.9 0.16 0.26 18346

Opticale

DECam i, z i < 22.5, z < 21.5 3.9, 5, 22 100 38 14 14 11 18344, 18350iPTF R R < 20.4 3.1, 3, 1 130 2.8 2.5 0.0 0.2 18337KWFC i i < 18.8 3.4, 1, 1 24 0.0 1.2 0.0 0.1 18361MASTER C < 19.9 -1.1, 7, 7 710 50 36 55 50 18333, 18390, 18903, 19021Pan-STARRS1 i i < 19.2 − 20.8 3.2, 21, 42 430 28 29 2.0 4.2 18335, 18343, 18362, 18394La Silla– g, r r < 21 3.8, 5, 0.1 80 23 16 6.2 5.7 18347

QUESTSkyMapper i, v i < 19.1, v < 17.1 2.4, 2, 3 30 9.1 7.9 1.5 1.9 18349Swift UVOT u u < 19.8 (gal.) 2.3, 1, 1 3 0.7 1.0 0.1 0.1 18331

u u < 18.8 (LMC) 3.4, 1, 1 18346TAROT C R < 18 2.8, 5, 14 30 15 3.5 1.6 1.9 18332, 18348TOROS C r < 21 2.5, 7, 90 0.6 0.03 0.0 0.0 0.0 18338VST@ESO r r < 22.4 2.9, 6, 50 90 29 10 14 10 18336, 18397

Near Infrared

VISTA@ESO Y, J,KS J < 20.7 4.8, 1, 7 70 15 6.4 10 8.0 18353

Radio

ASKAP 863.5 MHz 5–15 mJy 7.5, 2, 6 270 82 28 44 27 18363, 18655LOFAR 145 MHz 12.5 mJy 6.8, 3, 90 100 27 1.3 0.0 0.1 18364, 18424, 18690MWA 118 MHz 200 mJy 3.5, 2, 8 2800 97 72 86 86 18345aBand: photon energy, optical or near-infrared filter (or C for clear unfiltered light), wavelength range, or central frequency.bDepth: gamma/X-ray limiting flux in erg cm−2 s−1; 5σ optical/IR limiting magnitude (AB); and 5σ radio limiting spectral flux density in

mJy. The reported values correspond to the faintest flux/magnitude of detectable sources in the images.cElapsed time in days between start of observations and the time of GW150914 (2015 September 14 09:50:45), number of repeated observations

of the same area, and total observation period in days.dBAYESTAR.eSearches for bright optical transients were also done by BOOTES-3 and Pi of the Sky. Details are given in the Supplement (Abbott et al.

2016g).

8

Table 2. Summary of Follow-up Observations

Spectroscopic Follow-up

Instrument No. of Candidates Discovery Survey Epochs λ (A) ∆λa (A) GCNKeckII+DEIMOS 8 iPTF 1 4650 − 9600 3.5 18337, 18341LT+SPRAT 1 Pan-STARRS1 1 4500 − 7500 18 18370, 18371NTT+EFOSC2 10 QUEST/Pan-STARRS1 1 3650 − 9250 18 18359, 18395P200+DBSP 1 Pan-STARRS1 1 3200 − 9000 4 − 8 18372UH2.2m+SNIFS 9 Pan-STARRS1 1 3200 − 10000 4 − 6 —

Radio Follow-upInstrument No. of Candidates Discovery Survey Epochs Freq. (GHz) Lim. Fluxb (uJy) GCNVLA 1 iPTF 3 6 . 50 18420, 18474, 18914

aFull width at half maximum resolution.b 5σ, 2 GHz nominal bandwidth, ≈ 20 min on-source.

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 9

weeks to years. Tables 1 and 2 show that the radio obser-vations from wide-field facilities were sensitive to mJy fluxdensities at low frequencies where fainter sources with longertimescales are expected, while the narrow-field VLA was sen-sitive to well localized radio transients down to µJy flux den-sities at frequencies above a few GHz.

7. CONCLUSIONS

GW150914 is consistent with the inspiral and merger oftwo BHs of masses 36+5

−4 and 29+4−4 M�, respectively, result-

ing in the formation of a final BH of mass 62+4−4 M� (Ab-

bott et al. 2016c). In classical general relativity, a vacuumBBH merger does not produce any EM or particle emissionwhatsoever. Whereas supermassive BBHs in galactic cen-ters may appear as dual AGNs or have other distinctive EMsignatures due to interactions with gas or magnetic fields,stellar BBH systems are not expected to possess detectableEM counterparts. The background gas densities and mag-netic field strengths should therefore be typical of the inter-stellar medium, which are many orders of magnitude smallerthan the environments of EM bright supermassive BBHs. Al-though GW150914 is loud in GWs and expected to be absentin all EM bands, thorough follow-up observations were pur-sued to check for EM emission. Future EM follow-ups of GWsources will shed light on the presence or absence of firm EMcounterparts and astrophysical processes that may trigger EMemission from these systems.

The EM campaign following GW150914 successfullydemonstrates the capability of the observing partners to coverlarge swaths of the sky localization area, to identify candi-dates, and to activate larger telescopes for photometric andspectroscopic characterization within a few days of an event.We note that the information about the source’s BBH na-ture and updated sky maps were sent out 20 days and fourmonths after the event, respectively. This resulted in some in-struments covering much less of the probability region or tothe required depth of GW150914 than they may have plannedfor. We expect future alerts to be issued within tens of min-utes with more information about the signal type and morerapid updates of the maps. The follow-up efforts would havebeen sensitive to a wide range of emission expected from BNSor NSBH mergers. However, the widely variable sensitiv-ity reached across the sky localization area continues to bea challenge for an EM counterpart search.

The number of galaxies (with luminosities L > 0.1L?;Blanton et al. 2003) within the comoving volume of 10−2

Gpc3 corresponding to the 90% credible area of the LALIn-ference sky map and within the 90% confidence interval dis-tance is ∼ 105. Such a number makes it impossible to identifythe host galaxy in the absence of an EM counterpart detection.The presence of a third GW detector such as Virgo would haveimproved the sky localization of GW150914 to a few tens ofsquare degrees both for the unmodeled and CBC searches.The future addition of more GW detectors to the global net-

work (Abbott et al. 2016f) will significantly improve the effi-ciency of searches for EM counterparts.

In summary, we have described the EM follow-up programcarried out for the first GW source detected by AdvancedLIGO. Within two days of the initial tentative detection ofGW150914, a GCN circular was sent to EM follow-up part-ners alerting them to the event and providing them with ini-tial sky maps. Twenty-five EM observing teams mobilizedtheir resources, and over the ensuing three months observa-tions were performed with a diverse array of facilities overa broad wavelength range (from radio to γ-ray). Findingsfrom those observations are being disseminated in other pa-pers. The localization and broadband follow-up of this GWevent constitutes an important first step in a new era of gravi-tational wave multi-messenger astronomy.

See the Supplement (Abbott et al. 2016g) for a full listof acknowledgements. This is LIGO document LIGO-P1500227-v12.

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AUTHORS

B. P. ABBOTT1, R. ABBOTT1, T. D. ABBOTT2, M. R. ABERNATHY1, F. ACERNESE3,4, K. ACKLEY5, C. ADAMS6,T. ADAMS7, P. ADDESSO3, R. X. ADHIKARI1, V. B. ADYA8, C. AFFELDT8, M. AGATHOS9, K. AGATSUMA9,

N. AGGARWAL10, O. D. AGUIAR11, L. AIELLO12,13, A. AIN14, P. AJITH15, B. ALLEN8,16,17, A. ALLOCCA18,19,P. A. ALTIN20, S. B. ANDERSON1, W. G. ANDERSON16, K. ARAI1, M. C. ARAYA1, C. C. ARCENEAUX21, J. S. AREEDA22,

N. ARNAUD23, K. G. ARUN24, S. ASCENZI25,13, G. ASHTON26, M. AST27, S. M. ASTON6, P. ASTONE28, P. AUFMUTH8,C. AULBERT8, S. BABAK29, P. BACON30, M. K. M. BADER9, P. T. BAKER31, F. BALDACCINI32,33, G. BALLARDIN34,S. W. BALLMER35, J. C. BARAYOGA1, S. E. BARCLAY36, B. C. BARISH1, D. BARKER37, F. BARONE3,4, B. BARR36,

L. BARSOTTI10, M. BARSUGLIA30, D. BARTA38, S. BARTHELMY39, J. BARTLETT37, I. BARTOS40, R. BASSIRI41,A. BASTI18,19, J. C. BATCH37, C. BAUNE8, V. BAVIGADDA34, M. BAZZAN42,43, B. BEHNKE29, M. BEJGER44,

A. S. BELL36, C. J. BELL36, B. K. BERGER1, J. BERGMAN37, G. BERGMANN8, C. P. L. BERRY45, D. BERSANETTI46,47,A. BERTOLINI9, J. BETZWIESER6, S. BHAGWAT35, R. BHANDARE48, I. A. BILENKO49, G. BILLINGSLEY1, J. BIRCH6,

R. BIRNEY50, S. BISCANS10, A. BISHT8,17, M. BITOSSI34, C. BIWER35, M. A. BIZOUARD23, J. K. BLACKBURN1,C. D. BLAIR51, D. G. BLAIR51, R. M. BLAIR37, S. BLOEMEN52, O. BOCK8, T. P. BODIYA10, M. BOER53, G. BOGAERT53,

C. BOGAN8, A. BOHE29, P. BOJTOS54, C. BOND45, F. BONDU55, R. BONNAND7, B. A. BOOM9, R. BORK1, V. BOSCHI18,19,S. BOSE56,14, Y. BOUFFANAIS30, A. BOZZI34, C. BRADASCHIA19, P. R. BRADY16, V. B. BRAGINSKY49,

M. BRANCHESI57,58, J. E. BRAU59, T. BRIANT60, A. BRILLET53, M. BRINKMANN8, V. BRISSON23, P. BROCKILL16,A. F. BROOKS1, D. A. BROWN35, D. D. BROWN45, N. M. BROWN10, C. C. BUCHANAN2, A. BUIKEMA10, T. BULIK61,H. J. BULTEN62,9, A. BUONANNO29,63, D. BUSKULIC7, C. BUY30, R. L. BYER41, L. CADONATI64, G. CAGNOLI65,66,C. CAHILLANE1, J. C. BUSTILLO67,64, T. CALLISTER1, E. CALLONI68,4, J. B. CAMP39, K. C. CANNON69, J. CAO70,

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 11

C. D. CAPANO8, E. CAPOCASA30, F. CARBOGNANI34, S. CARIDE71, J. C. DIAZ23, C. CASENTINI25,13, S. CAUDILL16,M. CAVAGLIA21, F. CAVALIER23, R. CAVALIERI34, G. CELLA19, C. B. CEPEDA1, L. C. BAIARDI57,58, G. CERRETANI18,19,

E. CESARINI25,13, R. CHAKRABORTY1, T. CHALERMSONGSAK1, S. J. CHAMBERLIN72, M. CHAN36, S. CHAO73,P. CHARLTON74, E. CHASSANDE-MOTTIN30, H. Y. CHEN75, Y. CHEN76, C. CHENG73, A. CHINCARINI47, A. CHIUMMO34,H. S. CHO77, M. CHO63, J. H. CHOW20, N. CHRISTENSEN78, Q. CHU51, S. CHUA60, S. CHUNG51, G. CIANI5, F. CLARA37,J. A. CLARK64, F. CLEVA53, E. COCCIA25,12,13, P.-F. COHADON60, A. COLLA79,28, C. G. COLLETTE80, L. COMINSKY81,

M. CONSTANCIO JR.11, A. CONTE79,28, L. CONTI43, D. COOK37, T. R. CORBITT2, N. CORNISH31, A. CORSI71,S. CORTESE34, C. A. COSTA11, M. W. COUGHLIN78, S. B. COUGHLIN82, J.-P. COULON53, S. T. COUNTRYMAN40,

P. COUVARES1, E. E. COWAN64, D. M. COWARD51, M. J. COWART6, D. C. COYNE1, R. COYNE71, K. CRAIG36,J. D. E. CREIGHTON16, J. CRIPE2, S. G. CROWDER83, A. CUMMING36, L. CUNNINGHAM36, E. CUOCO34,

T. DAL CANTON8, S. L. DANILISHIN36, S. D’ANTONIO13, K. DANZMANN17,8, N. S. DARMAN84, V. DATTILO34,I. DAVE48, H. P. DAVELOZA85, M. DAVIER23, G. S. DAVIES36, E. J. DAW86, R. DAY34, D. DEBRA41, G. DEBRECZENI38,J. DEGALLAIX66, M. DE LAURENTIS68,4, S. DELEGLISE60, W. DEL POZZO45, T. DENKER8,17, T. DENT8, H. DERELI53,V. DERGACHEV1, R. T. DEROSA6, R. DE ROSA68,4, R. DESALVO87, S. DHURANDHAR14, M. C. D IAZ85, L. DI FIORE4,

M. DI GIOVANNI79,28, A. DI LIETO18,19, S. DI PACE79,28, I. DI PALMA29,8, A. DI VIRGILIO19, G. DOJCINOSKI88,V. DOLIQUE66, F. DONOVAN10, K. L. DOOLEY21, S. DORAVARI6,8, R. DOUGLAS36, T. P. DOWNES16, M. DRAGO8,89,90,

R. W. P. DREVER1, J. C. DRIGGERS37, Z. DU70, M. DUCROT7, S. E. DWYER37, T. B. EDO86, M. C. EDWARDS78,A. EFFLER6, H.-B. EGGENSTEIN8, P. EHRENS1, J. EICHHOLZ5, S. S. EIKENBERRY5, W. ENGELS76, R. C. ESSICK10,

T. ETZEL1, M. EVANS10, T. M. EVANS6, R. EVERETT72, M. FACTOUROVICH40, V. FAFONE25,13,12, H. FAIR35,S. FAIRHURST91, X. FAN70, Q. FANG51, S. FARINON47, B. FARR75, W. M. FARR45, M. FAVATA88, M. FAYS91,

H. FEHRMANN8, M. M. FEJER41, I. FERRANTE18,19, E. C. FERREIRA11, F. FERRINI34, F. FIDECARO18,19, I. FIORI34,D. FIORUCCI30, R. P. FISHER35, R. FLAMINIO66,92, M. FLETCHER36, J.-D. FOURNIER53, S. FRANCO23, S. FRASCA79,28,

F. FRASCONI19, Z. FREI54, A. FREISE45, R. FREY59, V. FREY23, T. T. FRICKE8, P. FRITSCHEL10, V. V. FROLOV6,P. FULDA5, M. FYFFE6, H. A. G. GABBARD21, J. R. GAIR93, L. GAMMAITONI32,33, S. G. GAONKAR14, F. GARUFI68,4,

A. GATTO30, G. GAUR94,95, N. GEHRELS39, G. GEMME47, B. GENDRE53, E. GENIN34, A. GENNAI19, J. GEORGE48,L. GERGELY96, V. GERMAIN7, A. GHOSH15, S. GHOSH52,9, J. A. GIAIME2,6, K. D. GIARDINA6, A. GIAZOTTO19,

K. GILL97, A. GLAEFKE36, E. GOETZ98, R. GOETZ5, L. GONDAN54, G. GONZALEZ2, J. M. G. CASTRO18,19,A. GOPAKUMAR99, N. A. GORDON36, M. L. GORODETSKY49, S. E. GOSSAN1, M. GOSSELIN34, R. GOUATY7,

C. GRAEF36, P. B. GRAFF63, M. GRANATA66, A. GRANT36, S. GRAS10, C. GRAY37, G. GRECO57,58, A. C. GREEN45,P. GROOT52, H. GROTE8, S. GRUNEWALD29, G. M. GUIDI57,58, X. GUO70, A. GUPTA14, M. K. GUPTA95, K. E. GUSHWA1,

E. K. GUSTAFSON1, R. GUSTAFSON98, J. J. HACKER22, B. R. HALL56, E. D. HALL1, G. HAMMOND36, M. HANEY99,M. M. HANKE8, J. HANKS37, C. HANNA72, M. D. HANNAM91, J. HANSON6, T. HARDWICK2, K. HARIS100, J. HARMS57,58,G. M. HARRY101, I. W. HARRY29, M. J. HART36, M. T. HARTMAN5, C.-J. HASTER45, K. HAUGHIAN36, A. HEIDMANN60,

M. C. HEINTZE5,6, H. HEITMANN53, P. HELLO23, G. HEMMING34, M. HENDRY36, I. S. HENG36, J. HENNIG36,A. W. HEPTONSTALL1, M. HEURS8,17, S. HILD36, D. HOAK102, K. A. HODGE1, D. HOFMAN66, S. E. HOLLITT103,

K. HOLT6, D. E. HOLZ75, P. HOPKINS91, D. J. HOSKEN103, J. HOUGH36, E. A. HOUSTON36, E. J. HOWELL51, Y. M. HU36,S. HUANG73, E. A. HUERTA104,82, D. HUET23, B. HUGHEY97, S. HUSA67, S. H. HUTTNER36, T. HUYNH-DINH6,

A. IDRISY72, N. INDIK8, D. R. INGRAM37, R. INTA71, H. N. ISA36, J.-M. ISAC60, M. ISI1, G. ISLAS22, T. ISOGAI10,B. R. IYER15, K. IZUMI37, T. JACQMIN60, H. JANG77, K. JANI64, P. JARANOWSKI105, S. JAWAHAR106,F. JIMENEZ-FORTEZA67, W. W. JOHNSON2, D. I. JONES26, R. JONES36, R. J. G. JONKER9, L. JU51,

C. V. KALAGHATGI24,91, V. KALOGERA82, S. KANDHASAMY21, G. KANG77, J. B. KANNER1, S. KARKI59,M. KASPRZACK2,23,34, E. KATSAVOUNIDIS10, W. KATZMAN6, S. KAUFER17, T. KAUR51, K. KAWABE37, F. KAWAZOE8,17,

F. KEFELIAN53, M. S. KEHL69, D. KEITEL8,67, D. B. KELLEY35, W. KELLS1, R. KENNEDY86, J. S. KEY85,A. KHALAIDOVSKI8, F. Y. KHALILI49, I. KHAN12, S. KHAN91, Z. KHAN95, E. A. KHAZANOV107, N. KIJBUNCHOO37,

C. KIM77, J. KIM108, K. KIM109, N. KIM77, N. KIM41, Y.-M. KIM108, E. J. KING103, P. J. KING37, D. L. KINZEL6,J. S. KISSEL37, L. KLEYBOLTE27, S. KLIMENKO5, S. M. KOEHLENBECK8, K. KOKEYAMA2, S. KOLEY9,

V. KONDRASHOV1, A. KONTOS10, M. KOROBKO27, W. Z. KORTH1, I. KOWALSKA61, D. B. KOZAK1, V. KRINGEL8,A. KROLAK110,111, C. KRUEGER17, G. KUEHN8, P. KUMAR69, L. KUO73, A. KUTYNIA110, B. D. LACKEY35,

M. LANDRY37, J. LANGE112, B. LANTZ41, P. D. LASKY113, A. LAZZARINI1, C. LAZZARO64,43, P. LEACI29,79,28,S. LEAVEY36, E. O. LEBIGOT30,70, C. H. LEE108, H. K. LEE109, H. M. LEE114, K. LEE36, A. LENON35, M. LEONARDI89,90,

J. R. LEONG8, N. LEROY23, N. LETENDRE7, Y. LEVIN113, B. M. LEVINE37, T. G. F. LI1, A. LIBSON10,T. B. LITTENBERG115, N. A. LOCKERBIE106, J. LOGUE36, A. L. LOMBARDI102, J. E. LORD35, M. LORENZINI12,13,

V. LORIETTE116, M. LORMAND6, G. LOSURDO58, J. D. LOUGH8,17, H. LUCK17,8, A. P. LUNDGREN8, J. LUO78,R. LYNCH10, Y. MA51, T. MACDONALD41, B. MACHENSCHALK8, M. MACINNIS10, D. M. MACLEOD2,

12

F. MAGANA-SANDOVAL35, R. M. MAGEE56, M. MAGESWARAN1, E. MAJORANA28, I. MAKSIMOVIC116,V. MALVEZZI25,13, N. MAN53, I. MANDEL45, V. MANDIC83, V. MANGANO36, G. L. MANSELL20, M. MANSKE16,

M. MANTOVANI34, F. MARCHESONI117,33, F. MARION7, S. MARKA40, Z. MARKA40, A. S. MARKOSYAN41, E. MAROS1,F. MARTELLI57,58, L. MARTELLINI53, I. W. MARTIN36, R. M. MARTIN5, D. V. MARTYNOV1, J. N. MARX1, K. MASON10,

A. MASSEROT7, T. J. MASSINGER35, M. MASSO-REID36, F. MATICHARD10, L. MATONE40, N. MAVALVALA10,N. MAZUMDER56, G. MAZZOLO8, R. MCCARTHY37, D. E. MCCLELLAND20, S. MCCORMICK6, S. C. MCGUIRE118,

G. MCINTYRE1, J. MCIVER1, D. J. MCMANUS20, S. T. MCWILLIAMS104, D. MEACHER72, G. D. MEADORS29,8,J. MEIDAM9, A. MELATOS84, G. MENDELL37, D. MENDOZA-GANDARA8, R. A. MERCER16, E. MERILH37,

M. MERZOUGUI53, S. MESHKOV1, C. MESSENGER36, C. MESSICK72, P. M. MEYERS83, F. MEZZANI28,79, H. MIAO45,C. MICHEL66, H. MIDDLETON45, E. E. MIKHAILOV119, L. MILANO68,4, J. MILLER10, M. MILLHOUSE31, Y. MINENKOV13,

J. MING29,8, S. MIRSHEKARI120, C. MISHRA15, S. MITRA14, V. P. MITROFANOV49, G. MITSELMAKHER5,R. MITTLEMAN10, A. MOGGI19, M. MOHAN34, S. R. P. MOHAPATRA10, M. MONTANI57,58, B. C. MOORE88,

C. J. MOORE121, D. MORARU37, G. MORENO37, S. R. MORRISS85, K. MOSSAVI8, B. MOURS7, C. M. MOW-LOWRY45,C. L. MUELLER5, G. MUELLER5, A. W. MUIR91, A. MUKHERJEE15, D. MUKHERJEE16, S. MUKHERJEE85, N. MUKUND14,

A. MULLAVEY6, J. MUNCH103, D. J. MURPHY40, P. G. MURRAY36, A. MYTIDIS5, I. NARDECCHIA25,13,L. NATICCHIONI79,28, R. K. NAYAK122, V. NECULA5, K. NEDKOVA102, G. NELEMANS52,9, M. NERI46,47, A. NEUNZERT98,

G. NEWTON36, T. T. NGUYEN20, A. B. NIELSEN8, S. NISSANKE52,9, A. NITZ8, F. NOCERA34, D. NOLTING6,M. E. N. NORMANDIN85, L. K. NUTTALL35, J. OBERLING37, E. OCHSNER16, J. O’DELL123, E. OELKER10, G. H. OGIN124,

J. J. OH125, S. H. OH125, F. OHME91, M. OLIVER67, P. OPPERMANN8, R. J. ORAM6, B. O’REILLY6,R. O’SHAUGHNESSY112, D. J. OTTAWAY103, R. S. OTTENS5, H. OVERMIER6, B. J. OWEN71, A. PAI100, S. A. PAI48,

J. R. PALAMOS59, O. PALASHOV107, N. PALLIYAGURU71, C. PALOMBA28, A. PAL-SINGH27, H. PAN73, C. PANKOW82,F. PANNARALE91, B. C. PANT48, F. PAOLETTI34,19, A. PAOLI34, M. A. PAPA29,16,8, H. R. PARIS41, W. PARKER6,D. PASCUCCI36, A. PASQUALETTI34, R. PASSAQUIETI18,19, D. PASSUELLO19, B. PATRICELLI18,19, Z. PATRICK41,B. L. PEARLSTONE36, M. PEDRAZA1, R. PEDURAND66, L. PEKOWSKY35, A. PELE6, S. PENN126, A. PERRECA1,M. PHELPS36, O. PICCINNI79,28, M. PICHOT53, F. PIERGIOVANNI57,58, V. PIERRO87, G. PILLANT34, L. PINARD66,

I. M. PINTO87, M. PITKIN36, R. POGGIANI18,19, P. POPOLIZIO34, A. POST8, J. POWELL36, J. PRASAD14, V. PREDOI91,S. S. PREMACHANDRA113, T. PRESTEGARD83, L. R. PRICE1, M. PRIJATELJ34, M. PRINCIPE87, S. PRIVITERA29,

G. A. PRODI89,90, L. PROKHOROV49, O. PUNCKEN8, M. PUNTURO33, P. PUPPO28, M. PURRER29, H. QI16, J. QIN51,V. QUETSCHKE85, E. A. QUINTERO1, R. QUITZOW-JAMES59, F. J. RAAB37, D. S. RABELING20, H. RADKINS37,

P. RAFFAI54, S. RAJA48, M. RAKHMANOV85, P. RAPAGNANI79,28, V. RAYMOND29, M. RAZZANO18,19, V. RE25, J. READ22,C. M. REED37, T. REGIMBAU53, L. REI47, S. REID50, D. H. REITZE1,5, H. REW119, S. D. REYES35, F. RICCI79,28,

K. RILES98, N. A. ROBERTSON1,36, R. ROBIE36, F. ROBINET23, A. ROCCHI13, L. ROLLAND7, J. G. ROLLINS1,V. J. ROMA59, R. ROMANO3,4, G. ROMANOV119, J. H. ROMIE6, D. ROSINSKA127,44, S. ROWAN36, A. RUDIGER8,

P. RUGGI34, K. RYAN37, S. SACHDEV1, T. SADECKI37, L. SADEGHIAN16, L. SALCONI34, M. SALEEM100, F. SALEMI8,A. SAMAJDAR122, L. SAMMUT84,113, E. J. SANCHEZ1, V. SANDBERG37, B. SANDEEN82, J. R. SANDERS98,35,

B. SASSOLAS66, B. S. SATHYAPRAKASH91, P. R. SAULSON35, O. SAUTER98, R. L. SAVAGE37, A. SAWADSKY17,P. SCHALE59, R. SCHILLING†8, J. SCHMIDT8, P. SCHMIDT1,76, R. SCHNABEL27, R. M. S. SCHOFIELD59,

A. SCHONBECK27, E. SCHREIBER8, D. SCHUETTE8,17, B. F. SCHUTZ91,29, J. SCOTT36, S. M. SCOTT20, D. SELLERS6,D. SENTENAC34, V. SEQUINO25,13, A. SERGEEV107, G. SERNA22, Y. SETYAWATI52,9, A. SEVIGNY37, D. A. SHADDOCK20,

S. SHAH52,9, M. S. SHAHRIAR82, M. SHALTEV8, Z. SHAO1, B. SHAPIRO41, P. SHAWHAN63, A. SHEPERD16,D. H. SHOEMAKER10, D. M. SHOEMAKER64, K. SIELLEZ53,64, X. SIEMENS16, D. SIGG37, A. D. SILVA11, D. SIMAKOV8,

A. SINGER1, A. SINGH29,8, R. SINGH2, A. SINGHAL12, A. M. SINTES67, B. J. J. SLAGMOLEN20, J. R. SMITH22,N. D. SMITH1, R. J. E. SMITH1, E. J. SON125, B. SORAZU36, F. SORRENTINO47, T. SOURADEEP14, A. K. SRIVASTAVA95,

A. STALEY40, M. STEINKE8, J. STEINLECHNER36, S. STEINLECHNER36, D. STEINMEYER8,17, B. C. STEPHENS16,R. STONE85, K. A. STRAIN36, N. STRANIERO66, G. STRATTA57,58, N. A. STRAUSS78, S. STRIGIN49, R. STURANI120,A. L. STUVER6, T. Z. SUMMERSCALES128, L. SUN84, P. J. SUTTON91, B. L. SWINKELS34, M. J. SZCZEPANCZYK97,

M. TACCA30, D. TALUKDER59, D. B. TANNER5, M. TAPAI96, S. P. TARABRIN8, A. TARACCHINI29, R. TAYLOR1,T. THEEG8, M. P. THIRUGNANASAMBANDAM1, E. G. THOMAS45, M. THOMAS6, P. THOMAS37, K. A. THORNE6,

K. S. THORNE76, E. THRANE113, S. TIWARI12, V. TIWARI91, K. V. TOKMAKOV106, C. TOMLINSON86, M. TONELLI18,19,C. V. TORRES‡85, C. I. TORRIE1, D. TOYRA45, F. TRAVASSO32,33, G. TRAYLOR6, D. TRIFIRO21, M. C. TRINGALI89,90,

L. TROZZO129,19, M. TSE10, M. TURCONI53, D. TUYENBAYEV85, D. UGOLINI130, C. S. UNNIKRISHNAN99,A. L. URBAN16, S. A. USMAN35, H. VAHLBRUCH17, G. VAJENTE1, G. VALDES85, N. VAN BAKEL9, M. VAN BEUZEKOM9,

J. F. J. VAN DEN BRAND62,9, C. VAN DEN BROECK9, D. C. VANDER-HYDE35,22, L. VAN DER SCHAAF9,J. V. VAN HEIJNINGEN9, A. A. VAN VEGGEL36, M. VARDARO42,43, S. VASS1, M. VASUTH38, R. VAULIN10, A. VECCHIO45,

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 13

G. VEDOVATO43, J. VEITCH45, P. J. VEITCH103, K. VENKATESWARA131, D. VERKINDT7, F. VETRANO57,58,A. VICERE57,58, S. VINCIGUERRA45, D. J. VINE50, J.-Y. VINET53, S. VITALE10, T. VO35, H. VOCCA32,33, C. VORVICK37,

D. VOSS5, W. D. VOUSDEN45, S. P. VYATCHANIN49, A. R. WADE20, L. E. WADE132, M. WADE132, M. WALKER2,L. WALLACE1, S. WALSH16,8,29, G. WANG12, H. WANG45, M. WANG45, X. WANG70, Y. WANG51, R. L. WARD20,

J. WARNER37, M. WAS7, B. WEAVER37, L.-W. WEI53, M. WEINERT8, A. J. WEINSTEIN1, R. WEISS10, T. WELBORN6,L. WEN51, P. WESSELS8, T. WESTPHAL8, K. WETTE8, J. T. WHELAN112,8, D. J. WHITE86, B. F. WHITING5,

R. D. WILLIAMS1, A. R. WILLIAMSON91, J. L. WILLIS133, B. WILLKE17,8, M. H. WIMMER8,17, W. WINKLER8,C. C. WIPF1, H. WITTEL8,17, G. WOAN36, J. WORDEN37, J. L. WRIGHT36, G. WU6, J. YABLON82, W. YAM10,H. YAMAMOTO1, C. C. YANCEY63, M. J. YAP20, H. YU10, M. YVERT7, A. ZADROZNY110, L. ZANGRANDO43,

M. ZANOLIN97, J.-P. ZENDRI43, M. ZEVIN82, F. ZHANG10, L. ZHANG1, M. ZHANG119, Y. ZHANG112, C. ZHAO51,M. ZHOU82, Z. ZHOU82, X. J. ZHU51, M. E. ZUCKER1,10, S. E. ZURAW102, J. ZWEIZIG1

The LIGO Scientific Collaboration and the Virgo Collaboration

J. ALLISON134,135, K. BANNISTER134,135, M. E. BELL134,135, S. CHATTERJEE136, A. P. CHIPPENDALE134,P. G. EDWARDS134, L. HARVEY-SMITH134, IAN HEYWOOD134,137, A. HOTAN138, B. INDERMUEHLE134, J. MARVIL134,D. MCCONNELL134, T. MURPHY139,135, A. POPPING140,135, J. REYNOLDS134, R. J. SAULT84,134, M. A. VORONKOV134,

M. T. WHITING134

The Australian Square Kilometer Array Pathfinder (ASKAP) Collaboration

A. J. CASTRO-TIRADO141,142, R. CUNNIFFE141, M. JELINEK143, J. C. TELLO141, S. R. OATES141, Y.-D. HU141,P. KUBANEK144, S. GUZIY145, A. CASTELLON146, A. GARCIA-CEREZO142, V. F. MUNOZ142, C. PEREZ DEL PULGAR142,

S. CASTILLO-CARRION147, J. M. CASTRO CERON148, R. HUDEC143,149, M. D. CABALLERO-GARCIA150, P. PATA149,S. VITEK149, J. A. ADAME151, S. KONIG151, F. RENDON141,151, T. DE J. MATEO SANGUINO152,

R. FERNANDEZ-MUNOZ153, P. C. YOCK154, N. RATTENBURY154, W. H. ALLEN155, R. QUEREL156, S. JEONG141,157,I. H. PARK157, J. BAI158, CH. CUI159, Y. FAN158, CH. WANG158, D. HIRIART160, W. H. LEE161, A. CLARET141,

R. SANCHEZ-RAMIREZ141, S. B. PANDEY162, T. MEDIAVILLA163, L. SABAU-GRAZIATI164

The BOOTES Collaboration

T. M. C. ABBOTT165, F. B. ABDALLA166,137, S. ALLAM167, J. ANNIS167, R. ARMSTRONG168, A. BENOIT-LEVY169,166,170,E. BERGER171, R. A. BERNSTEIN172, E. BERTIN169,170, D. BROUT173, E. BUCKLEY-GEER167, D. L. BURKE174,175,

D. CAPOZZI176, J. CARRETERO177,178, F. J. CASTANDER177, R. CHORNOCK179, P. S. COWPERTHWAITE171, M. CROCCE177,C. E. CUNHA174, C. B. D’ANDREA176,26, L. N. DA COSTA180,181, S. DESAI182,183, H. T. DIEHL167, J. P. DIETRICH182,183,

Z. DOCTOR184, A. DRLICA-WAGNER167, M. R. DROUT171, T. F. EIFLER173,185, J. ESTRADA167, A. E. EVRARD98,E. FERNANDEZ178, D. A. FINLEY167, B. FLAUGHER167, R. J. FOLEY186,187, W.-F. FONG188, P. FOSALBA177, D. B. FOX189,

J. FRIEMAN167,184, C. L. FRYER190, E. GAZTANAGA177, D. W. GERDES191, D. A. GOLDSTEIN192,193, D. GRUEN174,175,R. A. GRUENDL186,194, G. GUTIERREZ167, K. HERNER167, K. HONSCHEID195,196, D. J. JAMES165, M. D. JOHNSON194,

M. W. G. JOHNSON194, I. KARLINER187, D. KASEN197,193, S. KENT167, R. KESSLER184, A. G. KIM193, M. C. KIND186,194,K. KUEHN198, N. KUROPATKIN167, O. LAHAV166, T. S. LI199, M. LIMA200,180, H. LIN167, M. A. G. MAIA180,181,R. MARGUTTI201, J. MARRINER167, P. MARTINI195,202, T. MATHESON203, P. MELCHIOR168, B. D. METZGER204,

C. J. MILLER205,191, R. MIQUEL206,178, E. NEILSEN167, R. C. NICHOL176, B. NORD167, P. NUGENT193, R. OGANDO180,181,D. PETRAVICK194, A. A. PLAZAS185, E. QUATAERT207, N. ROE193, A. K. ROMER208, A. ROODMAN174,175,

A. C. ROSELL180,181, E. S. RYKOFF174,175, M. SAKO173, E. SANCHEZ209, V. SCARPINE167, R. SCHINDLER175,M. SCHUBNELL191, D. SCOLNIC184, I. SEVILLA-NOARBE209,186, E. SHELDON210, N. SMITH188, R. C. SMITH165,

M. SOARES-SANTOS167, F. SOBREIRA180, A. STEBBINS167, E. SUCHYTA173, M. E. C. SWANSON194, G. TARLE191,J. THALER187, D. THOMAS176, R. C. THOMAS193, D. L. TUCKER167, V. VIKRAM211, A. R. WALKER165,

R. H. WECHSLER41,174,175, W. WESTER167, B. YANNY167, Y. ZHANG98, J. ZUNTZ212

The Dark Energy Survey and the Dark Energy Camera GW-EM Collaborations

V. CONNAUGHTON213, E. BURNS214, A. GOLDSTEIN215,216, M. S. BRIGGS217, B.-B. ZHANG218,219, C. M. HUI216,P. JENKE218, C. A. WILSON-HODGE216, P. N. BHAT218, E. BISSALDI220, W. CLEVELAND213, G. FITZPATRICK218,

M. M. GILES221, M. H. GIBBY221, J. GREINER222, A. VON KIENLIN222, R. M. KIPPEN223, S. MCBREEN224,B. MAILYAN218, C. A. MEEGAN218, W. S. PACIESAS213, R. D. PREECE217, O. ROBERTS224, L. SPARKE225,

M. STANBRO214, K. TOELGE222, P. VERES218, H.-F. YU222,226, L. BLACKBURN171

The Fermi GBM Collaboration

14

M. ACKERMANN227, M. AJELLO228, A. ALBERT229, B. ANDERSON230,231, W. B. ATWOOD232, M. AXELSSON233,234,L. BALDINI235,229, G. BARBIELLINI236,237, D. BASTIERI238,239, R. BELLAZZINI240, E. BISSALDI241, R. D. BLANDFORD229,

E. D. BLOOM229, R. BONINO242,243, E. BOTTACINI229, T. J. BRANDT244, P. BRUEL245, S. BUSON244,246,247,G. A. CALIANDRO229,248, R. A. CAMERON229, M. CARAGIULO249,241, P. A. CARAVEO250, E. CAVAZZUTI251,E. CHARLES229, A. CHEKHTMAN252, J. CHIANG229, G. CHIARO239, S. CIPRINI251,253, J. COHEN-TANUGI254,

L. R. COMINSKY255, F. COSTANZA241, A. CUOCO242,243, F. D’AMMANDO256,257, F. DE PALMA241,258, R. DESIANTE259,242,S. W. DIGEL229, N. DI LALLA240, M. DI MAURO229, L. DI VENERE249,241, A. DOMINGUEZ228, P. S. DRELL229,

R. DUBOIS229, C. FAVUZZI249,241, E. C. FERRARA244, A. FRANCKOWIAK229, Y. FUKAZAWA260, S. FUNK261,P. FUSCO249,241, F. GARGANO241, D. GASPARRINI251,253, N. GIGLIETTO249,241, P. GIOMMI251, F. GIORDANO249,241,

M. GIROLETTI256, T. GLANZMAN229, G. GODFREY229, G. A. GOMEZ-VARGAS262,13, D. GREEN263,244, I. A. GRENIER264,J. E. GROVE265, S. GUIRIEC244,266, D. HADASCH267, A. K. HARDING244, E. HAYS244, J.W. HEWITT268, A. B. HILL269,229,

D. HORAN245, T. JOGLER229, G. JOHANNESSON270, A. S. JOHNSON229, S. KENSEI260, D. KOCEVSKI244, M. KUSS240,G. LA MURA239,267, S. LARSSON233,231, L. LATRONICO242, J. LI271, L. LI233,231, F. LONGO236,237, F. LOPARCO249,241,

M. N. LOVELLETTE265, P. LUBRANO253, J. MAGILL263, S. MALDERA242, A. MANFREDA240, M. MARELLI250,M. MAYER227, M. N. MAZZIOTTA241, J. E. MCENERY244,263,272, M. MEYER230,231, P. F. MICHELSON229,

N. MIRABAL244,266, T. MIZUNO273, A. A. MOISEEV247,263, M. E. MONZANI229, E. MORETTI274, A. MORSELLI13,I. V. MOSKALENKO229, M. NEGRO242,243, E. NUSS254, T. OHSUGI273, N. OMODEI229, M. ORIENTI256, E. ORLANDO229,

J. F. ORMES275, D. PANEQUE274,229, J. S. PERKINS244, M. PESCE-ROLLINS240,229, F. PIRON254, G. PIVATO240,T. A. PORTER229, J. L. RACUSIN244, S. RAINO249,241, R. RANDO238,239, S. RAZZAQUE276, A. REIMER267,229,

O. REIMER267,229, D. SALVETTI250, P. M. SAZ PARKINSON232,277,278, C. SGRO240, D. SIMONE241, E. J. SISKIND279,F. SPADA240, G. SPANDRE240, P. SPINELLI249,241, D. J. SUSON280, H. TAJIMA281,229, J. B. THAYER229,

D. J. THOMPSON244, L. TIBALDO282, D. F. TORRES271,283, E. TROJA244,263, Y. UCHIYAMA284, T. M. VENTERS244,G. VIANELLO229, K. S. WOOD265, M. WOOD229, S. ZHU263, S. ZIMMER230,231

The Fermi LAT Collaboration

E. BROCATO285, E. CAPPELLARO286, S. COVINO287, A. GRADO288, L. NICASTRO289, E. PALAZZI289, E. PIAN289,290,L. AMATI289, L. A. ANTONELLI285,291, M. CAPACCIOLI292, P. D’AVANZO287, V. D’ELIA285,291, F. GETMAN288,G. GIUFFRIDA285,291, G. IANNICOLA285, L. LIMATOLA288, M. LISI285, S. MARINONI285,291, P. MARRESE285,286,

A. MELANDRI287, S. PIRANOMONTE285, A. POSSENTI293, L. PULONE285, A. ROSSI289, A. STAMERRA290,294,L. STELLA285, V. TESTA285, L. TOMASELLA286, S. YANG286

The GRAvitational Wave Inaf TeAm (GRAWITA)

A. BAZZANO295, E. BOZZO296, S. BRANDT297, T. J.-L. COURVOISIER296, C. FERRIGNO296, L. HANLON298,E. KUULKERS299, P. LAURENT300, S. MEREGHETTI301, J. P. ROQUES302, V. SAVCHENKO303, P. UBERTINI295

The INTEGRAL Collaboration

M. M. KASLIWAL304, L. P. SINGER39,215, Y. CAO304, G. DUGGAN304, S. R. KULKARNI304, V. BHALERAO14,A. A. MILLER185,304,305, T. BARLOW304, E. BELLM304, I. MANULIS306, J. RANA14, R. LAHER307, F. MASCI307,

J. SURACE307, U. REBBAPRAGADA185, D. COOK304, A. VAN SISTINE16, B. SESAR308, D. PERLEY309, R. FERRETI310,T. PRINCE304, R. KENDRICK311, A. HORESH306

The Intermediate Palomar Transient Factory (iPTF) Collaboration

K. HURLEY312, S. V. GOLENETSKII313, R. L. APTEKAR313, D. D. FREDERIKS313, D. S. SVINKIN313, A. RAU222,A. VON KIENLIN222, X. ZHANG222, D. M. SMITH232, T. CLINE39,314, H. KRIMM247,315

The InterPlanetary Network

F. ABE316, M. DOI317, K. FUJISAWA318, K. S. KAWABATA319, T. MOROKUMA317, K. MOTOHARA317, M. TANAKA320,K. OHTA321, K. YANAGISAWA322, M. YOSHIDA319

The J-GEM Collaboration

C. BALTAY323, D. RABINOWITZ323, N. ELLMAN323, S. ROSTAMI323

The La Silla–QUEST Survey

D. F. BERSIER324, M. F. BODE324, C. A. COLLINS324, C. M. COPPERWHEAT324, M. J. DARNLEY324,D. K. GALLOWAY325,326, A. GOMBOC327,328, S. KOBAYASHI324, P. MAZZALI324, C. G. MUNDELL329, A. S. PIASCIK324,

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 15

DON POLLACCO330, I. A. STEELE324, K. ULACZYK330

The Liverpool Telescope Collaboration

J.W. BRODERICK331, R.P. FENDER332, P.G. JONKER333,52, A. ROWLINSON331,334,135, B.W. STAPPERS212,R.A.M.J. WIJERS334

The Low Frequency Array (LOFAR) Collaboration

V. LIPUNOV335, E. GORBOVSKOY335, N. TYURINA335, V. KORNILOV335, P. BALANUTSA335, A. KUZNETSOV335,D. BUCKLEY336, R. REBOLO337, M. SERRA-RICART337, G. ISRAELIAN337, N. M. BUDNEV338, O. GRESS338,

K. IVANOV338, V. POLESHUK338, A. TLATOV339, V. YURKOV340

The MASTER Collaboration

N. KAWAI341, M. SERINO342, H. NEGORO343, S. NAKAHIRA344, T. MIHARA342, H. TOMIDA345, S. UENO345,H. TSUNEMI346, M. MATSUOKA342

The MAXI Collaboration

S. CROFT347,348, L. FENG349, T. M. O. FRANZEN350, B. M. GAENSLER351,139,135, M. JOHNSTON-HOLLITT352,D. L. KAPLAN16, M. F. MORALES131, S. J. TINGAY350,135,353, R. B. WAYTH350,135, A. WILLIAMS350

The Murchison Wide-field Array (MWA) Collaboration

S. J. SMARTT354, K. C. CHAMBERS355, K. W. SMITH354, M. E. HUBER355, D. R. YOUNG354, D. E. WRIGHT354,A. SCHULTZ355, L. DENNEAU355, H. FLEWELLING355, E. A. MAGNIER355, N. PRIMAK355, A. REST356, A. SHERSTYUK355,

B. STALDER355, C. W. STUBBS357, J. TONRY355, C. WATERS355, M. WILLMAN355

The Pan-STARRS Collaboration

F. OLIVARES E.358,359, H. CAMPBELL360, R. KOTAK354, J. SOLLERMAN310, M. SMITH26, M. DENNEFELD361,J. P. ANDERSON362, M. T. BOTTICELLA288, T.-W. CHEN222, M. D. VALLE288, N. ELIAS-ROSA286, M. FRASER360,

C. INSERRA354, E. KANKARE354, T. KUPFER304, J. HARMANEN363, L. GALBANY358,364, L. LE GUILLOU365,366,J. D. LYMAN330, K. MAGUIRE354, A. MITRA366, M. NICHOLL171, A. RAZZA358,364, G. TERRERAN286,354,

S. VALENTI367,368, A. GAL-YAM369

The PESSTO Collaboration

A. CWIEK110, M. CWIOK370, L. MANKIEWICZ371, R. OPIELA371, M. ZAREMBA370, A. F. ZARNECKI370

The Pi of the Sky Collaboration

C. A. ONKEN20,135, R. A. SCALZO20,135, B. P. SCHMIDT20,135, C. WOLF20,135, F. YUAN20,135

The SkyMapper Collaboration

P. A. EVANS372, J. A. KENNEA72, D. N. BURROWS72, S. CAMPANA287, S. B. CENKO39,373, P. GIOMMI291,F. E. MARSHALL39, J. NOUSEK72, P. O’BRIEN372, J. P. OSBORNE372, D. PALMER374, M. PERRI291,285, M. SIEGEL72,

G. TAGLIAFERRI287

The Swift Collaboration

A. KLOTZ375, D. TURPIN375, R. LAUGIER53

The TAROT, Zadko, Algerian National Observatory, and C2PU Collaboration

M. BEROIZ85,376, T. PENUELA85,183, L. M. MACRI377, R. J. OELKERS377, D. G. LAMBAS378, R. VRECH378, J. CABRAL378,C. COLAZO378, M. DOMINGUEZ378, B. SANCHEZ378, S. GUROVICH378, M. LARES378, J. L. MARSHALL377,

D. L. DEPOY377, N. PADILLA379, N. A. PEREYRA85, M. BENACQUISTA85

The TOROS Collaboration

N. R. TANVIR372, K. WIERSEMA372, A. J. LEVAN330, D. STEEGHS330, J. HJORTH309, J. P. U. FYNBO309, D. MALESANI309,B. MILVANG-JENSEN309, D. WATSON309, M. IRWIN360, C. G. FERNANDEZ360, R. G. MCMAHON360, M. BANERJI360,

E. GONZALEZ-SOLARES360, S. SCHULZE379,358, A. DE U. POSTIGO380,309, C. C. THOENE380, Z. CANO381, S. ROSSWOG310

The VISTA Collaboration

16

1LIGO, California Institute of Technology, Pasadena, CA 91125, USA2Louisiana State University, Baton Rouge, LA 70803, USA

3Universita di Salerno, Fisciano, I-84084 Salerno, Italy4INFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy

5University of Florida, Gainesville, FL 32611, USA6LIGO Livingston Observatory, Livingston, LA 70754, USA

7Laboratoire d’Annecy-le-Vieux de Physique des Particules (LAPP), Universite Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy-le-Vieux, France8Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik, D-30167 Hannover, Germany

9Nikhef, Science Park, 1098 XG Amsterdam, The Netherlands10LIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USA

11Instituto Nacional de Pesquisas Espaciais, 12227-010 Sao Jose dos Campos, SP, Brazil12INFN, Gran Sasso Science Institute, I-67100 L’Aquila, Italy

13Istituto Nazionale di Fisica Nucleare, Sezione di Roma “Tor Vergata,” I-00133 Roma, Italy14Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India

15International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bangalore 560012, India16University of Wisconsin-Milwaukee, Milwaukee, WI 53201, USA

17Leibniz Universitat Hannover, D-30167 Hannover, Germany18Universita di Pisa, I-56127 Pisa, Italy

19INFN, Sezione di Pisa, I-56127 Pisa, Italy20Australian National University, Canberra, Australian Capital Territory 0200, Australia

21The University of Mississippi, University, MS 38677, USA22California State University Fullerton, Fullerton, CA 92831, USA

23LAL, Univ. Paris-Sud, CNRS/IN2P3, Universite Paris-Saclay, Orsay, France24Chennai Mathematical Institute, Chennai, India

25Universita di Roma “Tor Vergata,” I-00133 Roma, Italy26School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK

27Universitat Hamburg, D-22761 Hamburg, Germany28INFN, Sezione di Roma, I-00185 Roma, Italy

29Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik, D-14476 Potsdam-Golm, Germany30APC, AstroParticule et Cosmologie, Universite Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cite, F-75205 Paris Cedex 13,

France31Montana State University, Bozeman, MT 59717, USA

32Universita di Perugia, I-06123 Perugia, Italy33INFN, Sezione di Perugia, I-06123 Perugia, Italy

34European Gravitational Observatory (EGO), I-56021 Cascina, Pisa, Italy35Syracuse University, Syracuse, NY 13244, USA

36SUPA, University of Glasgow, Glasgow G12 8QQ, United Kingdom37LIGO Hanford Observatory, Richland, WA 99352, USA

38Wigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklos ut 29-33, Hungary39NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA

40Columbia University, New York, NY 10027, USA41Stanford University, Stanford, CA 94305, USA

42Universita di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, Italy43INFN, Sezione di Padova, I-35131 Padova, Italy

44CAMK-PAN, 00-716 Warsaw, Poland45University of Birmingham, Birmingham B15 2TT, United Kingdom

46Universita degli Studi di Genova, I-16146 Genova, Italy47INFN, Sezione di Genova, I-16146 Genova, Italy

48RRCAT, Indore MP 452013, India49Faculty of Physics, Lomonosov Moscow State University, Moscow 119991, Russia

50SUPA, University of the West of Scotland, Paisley PA1 2BE, United Kingdom51University of Western Australia, Crawley, Western Australia 6009, Australia

52Department of Astrophysics/IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands53Artemis, Universite Cote d’Azur, CNRS, Observatoire Cote d’Azur, CS 34229, Nice cedex 4, France

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 17

54MTA Eotvos University, “Lendulet” Astrophysics Research Group, Budapest 1117, Hungary55Institut de Physique de Rennes, CNRS, Universite de Rennes 1, F-35042 Rennes, France

56Washington State University, Pullman, WA 99164, USA57Universita degli Studi di Urbino “Carlo Bo,” I-61029 Urbino, Italy58INFN, Sezione di Firenze, I-50019 Sesto Fiorentino, Firenze, Italy

59University of Oregon, Eugene, OR 97403, USA60Laboratoire Kastler Brossel, UPMC-Sorbonne Universites, CNRS, ENS-PSL Research University, College de France, F-75005 Paris, France

61Astronomical Observatory Warsaw University, 00-478 Warsaw, Poland62VU University Amsterdam, 1081 HV Amsterdam, The Netherlands

63University of Maryland, College Park, MD 20742, USA64Center for Relativistic Astrophysics and School of Physics, Georgia Institute of Technology, Atlanta, GA 30332, USA

65Institut Lumiere Matiere, Universite de Lyon, Universite Claude Bernard Lyon 1, UMR CNRS 5306, F-69622 Villeurbanne, France66Laboratoire des Materiaux Avances (LMA), IN2P3/CNRS, Universite de Lyon, F-69622 Villeurbanne, Lyon, France

67Universitat de les Illes Balears, IAC3—IEEC, E-07122 Palma de Mallorca, Spain68Universita di Napoli ’Federico II’, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, Italy

69Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada70Tsinghua University, Beijing 100084, China

71Texas Tech University, Lubbock, TX 79409, USA72The Pennsylvania State University, University Park, PA 16802, USA73National Tsing Hua University, Hsinchu City, 30013, Taiwan R.O.C.

74Charles Sturt University, Wagga Wagga, New South Wales 2678, Australia75University of Chicago, Chicago, IL 60637, USA

76Caltech CaRT, Pasadena, CA 91125, USA77Korea Institute of Science and Technology Information, Daejeon 305-806, Korea

78Carleton College, Northfield, MN 55057, USA79Universita di Roma “La Sapienza,” I-00185 Roma, Italy

80University of Brussels, Brussels B-1050, Belgium81Sonoma State University, Rohnert Park, CA 94928, USA

82Northwestern University, Evanston, IL 60208, USA83University of Minnesota, Minneapolis, MN 55455, USA

84The University of Melbourne, Parkville, Victoria 3010, Australia85The University of Texas Rio Grande Valley, Brownsville, TX 78520, USA

86The University of Sheffield, Sheffield S10 2TN, United Kingdom87University of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, Italy

88Montclair State University, Montclair, NJ 07043, USA89Universita di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, Italy

90INFN, Trento Institute for Fundamental Physics and Applications, I-38123 Povo, Trento, Italy91Cardiff University, Cardiff CF24 3AA, United Kingdom

92National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan93School of Mathematics, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom

94Indian Institute of Technology, Gandhinagar, Ahmedabad, Gujarat 382424, India95Institute for Plasma Research, Bhat, Gandhinagar 382428, India

96University of Szeged, Dom ter 9, Szeged 6720, Hungary97Embry-Riddle Aeronautical University, Prescott, AZ 86301, USA

98University of Michigan, Ann Arbor, MI 48109, USA99Tata Institute of Fundamental Research, Mumbai 400005, India100IISER-TVM, CET Campus, Trivandrum Kerala 695016, India

101American University, Washington, D.C. 20016, USA102University of Massachusetts-Amherst, Amherst, MA 01003, USA103University of Adelaide, Adelaide, South Australia 5005, Australia

104West Virginia University, Morgantown, WV 26506, USA105University of Białystok, 15-424 Białystok, Poland

106SUPA, University of Strathclyde, Glasgow G1 1XQ, United Kingdom107Institute of Applied Physics, Nizhny Novgorod, 603950, Russia

18

108Pusan National University, Busan 609-735, Korea109Hanyang University, Seoul 133-791, Korea

110NCBJ, 05-400 Swierk-Otwock, Poland111IM-PAN, 00-956 Warsaw, Poland

112Rochester Institute of Technology, Rochester, NY 14623, USA113Monash University, Victoria 3800, Australia

114Seoul National University, Seoul 151-742, Korea115University of Alabama in Huntsville, Huntsville, AL 35899, USA

116ESPCI, CNRS, F-75005 Paris, France117Universita di Camerino, Dipartimento di Fisica, I-62032 Camerino, Italy118Southern University and A&M College, Baton Rouge, LA 70813, USA

119College of William and Mary, Williamsburg, VA 23187, USA120Instituto de Fısica Teorica, University Estadual Paulista/ICTP South American Institute for Fundamental Research, Sao Paulo SP 01140-070, Brazil

121University of Cambridge, Cambridge CB2 1TN, United Kingdom122IISER-Kolkata, Mohanpur, West Bengal 741252, India

123Rutherford Appleton Laboratory, HSIC, Chilton, Didcot, Oxon OX11 0QX, United Kingdom124Whitman College, 345 Boyer Ave, Walla Walla, WA 99362 USA

125National Institute for Mathematical Sciences, Daejeon 305-390, Korea126Hobart and William Smith Colleges, Geneva, NY 14456, USA

127Janusz Gil Institute of Astronomy, University of Zielona Gora, 65-265 Zielona Gora, Poland128Andrews University, Berrien Springs, MI 49104, USA

129Universita di Siena, I-53100 Siena, Italy130Trinity University, San Antonio, TX 78212, USA

131University of Washington, Seattle, WA 98195, USA132Kenyon College, Gambier, OH 43022, USA

133Abilene Christian University, Abilene, TX 79699, USA134CSIRO Astronomy and Space Science, PO Box 76, Epping NSW 1710, Australia

135ARC Centre of Excellence for All-sky Astrophysics (CAASTRO)136Cornell Center for Astrophysics and Planetary Science, Ithaca, NY 14853, USA

137Department of Physics and Electronics, Rhodes University, PO Box 94, Grahamstown, 6140, South Africa138CSIRO Astronomy and Space Science, 26 Dick Perry Avenue, Technology Park, Kensington WA 6151, Australia

139Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006, Australia140International Centre for Radio Astronomy Research (ICRAR), The University of Western Australia, M468, 35 Stirling Highway, Crawley, Perth, WA, 6009,

Australia141Instituto de Astrofısica de Andalucıa (IAA-CSIC), P.O. Box 03004, E-18080 Granada, Spain

142Departamento de Ingenierıa de Sistemas y Automatica, Escuela de Ingenierıas, Universidad de Malaga, Unidad Asociada al CSIC, Dr. Pedro Ortiz Ramos,

E-29071 Malaga, Spain143Astronomical Institute, Academy of Sciences of the Czech Republic 251 65 Ondrejov, Czech Republic

144Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, 182 21 Praha 8, Czech Republic145Nikolaev National University, Nikolska str. 24, 54030 Nikolaev, Ukraine

146Facultad de Ciencias, Universidad de Malaga, Bulevard Louis Pasteur, E-29010 Malaga, Spain147Ensenanza Virtual y Laboratorios Tecnologicos, Universidad de Malaga, Jimenez Fraud 10, E-29071 Malaga, Spain

148ISDEFE for the SMOS FOS (ESA-ESAC), E-28692 Villanueva de la Canada (Madrid), Spain149Czech Technical University, Faculty of Electrical Engineering, Dep. of Radioelectronics, Technicka 2 166 27 Praha, Czech Republic

150Astronomical Institute of the Academy of Sciences, Bocnı II 1401, CZ-14100 Praha 4, Czech Republic151Estacion de Sondeos Atmosfericos (ESAt) de El Arenosillo (CEDEA-INTA), E-21130 Mazagon, Huelva, Spain

152Departamento de Ingenierıa Electronica, Sistemas Informaticos y Automatica, Universidad de Huelva, E.T.S.I. de La Rabida, E-21819 Palos de la Frontera

(Huelva), Spain153Instituto de Hortofruticultura Subtropical y Mediterranea La Mayora (IHSM/UMA-CSIC), E-29750 Algarrobo Costa (Malaga), Spain

154Department of Physics, University of Auckland, Private Bag 92019, New Zealand155Vintage Lane Observatory, RD3, 7273 Blenheim, New Zealand

156National Institute of Water and Atmospheric Research (NIWA), Lauder, New Zealand157Department of Physics, Sungkyunkwan University (SKKU), Suwon, Korea158Yunnan Astronomical Observatory, CAS, Kunming 650011, Yunnan, China

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 19

159National Astronomical Observatory, Chinese Academy of Sciences, Beijing 100012, China160Instituto de Astronomıa, Universidad Nacional Autonoma de Mexico, 22800 Ensenada, Baja California, Mexico

161Instituto de Astronomıa, Universidad Nacional Autonoma de Mexico, Apdo Postal 70-264, Cd. Universitaria, 04510 Mexico DF, Mexico162Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital-263 002, India

163Escuela Politecnica Superior, Universidad de Cadiz, Avda. Ramon Puyol, E-11202 Algeciras (Cadiz), Spain164Division de Ciencias del Espacio, Instituto Nacional de Tecnica Aerospacial (INTA), E-28850 Torrejon de Ardoz (Madrid), Spain

165Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile166Department of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UK

167Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA168Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA

169CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France170Sorbonne Universites, UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014, Paris, France

171Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, United States172Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101, USA

173Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA174Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA

175SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA176Institute of Cosmology & Gravitation, University of Portsmouth, Portsmouth, PO1 3FX, UK

177Institut de Ciencies de l’Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, E-08193 Bellaterra, Barcelona, Spain178Institut de Fısica d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona) Spain

179Astrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USA180Laboratorio Interinstitucional de e-Astronomia—LIneA, Rua Gal. Jose Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil

182Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Germany183Ludwig Maximillian Universitat Munich, Faculty of Physics, Schellingstrasse 4, D-80799 Munich, Germany

184Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA185Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA

186Department of Astronomy, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA187Department of Physics, University of Illinois, 1110 W. Green St., Urbana, IL 61801, USA

188University of Arizona, Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA189Department of Astronomy & Astrophysics, Center for Particle & Gravitational Astrophysics, and Center for Theoretical & Observational Cosmology,

Pennsylvania State University, University Park, PA 16802, USA190CCS Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA

191Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA192Department of Astronomy, University of California, Berkeley, 501 Campbell Hall, Berkeley, CA 94720, USA

193Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA194National Center for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA

195Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA196Department of Physics, The Ohio State University, Columbus, OH 43210, USA

197Departments of Physics and Astronomy, University of California, Berkeley, CA, USA198Australian Astronomical Observatory, North Ryde, NSW 2113, Australia

199George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M

University, College Station, TX 77843, USA200Departamento de Fısica Matematica, Instituto de Fısica, Universidade de Sao Paulo, CP 66318, CEP 05314-970, Sao Paulo, SP, Brazil

201Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA202Department of Astronomy, The Ohio State University, Columbus, OH 43210, USA

203National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA204Columbia Astrophysics Laboratory, Pupin Hall, New York, NY, 10027,USA

205Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA206Institucio Catalana de Recerca i Estudis Avancats, E-08010 Barcelona, Spain

207Department of Astronomy & Theoretical Astrophysics Center, University of California, Berkeley, CA 94720-3411, USA208Department of Physics and Astronomy, Pevensey Building, University of Sussex, Brighton, BN1 9QH, UK

209Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas (CIEMAT), Madrid, Spain210Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA

211Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA

20

212Jodrell Bank Center for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester, M13 9PL, UK213Universities Space Research Association, 320 Sparkman Dr. Huntsville, AL 35806, USA

214Physics Dept, University of Alabama in Huntsville, 320 Sparkman Dr., Huntsville, AL 35899, USA215NASA Postdoctoral Program Fellow

216Astrophysics Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USA217Dept. of Space Science, University of Alabama in Huntsville, 320 Sparkman Dr., Huntsville, AL 35899, USA

218CSPAR, University of Alabama in Huntsville, 320 Sparkman Dr., Huntsville, AL 35899, USA219Instituto de Astrofısica de Andaluca (IAA-CSIC), P.O. Box 03004, E-18080 Granada, Spain

220Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy221Jacobs Technology, Inc., Huntsville, AL, USA

222Max-Planck-Institut fur Extraterrestrische Physik, Giessenbachstraße 1, D-85748, Garching, Germany223Los Alamos National Laboratory, NM 87545, USA

224School of Physics, University College Dublin, Belfield, Stillorgan Road, Dublin 4, Ireland225NASA Headquarters, Washington DC, USA

226Excellence Cluster Universe, Technische Universitat Munchen, Boltzmannstr. 2, D-85748, Garching, Germany227Deutsches Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

228Department of Physics and Astronomy, Clemson University, Kinard Lab of Physics, Clemson, SC 29634-0978, USA229W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National

Accelerator Laboratory, Stanford University, Stanford, CA 94305, USA230Department of Physics, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden

231The Oskar Klein Centre for Cosmoparticle Physics, AlbaNova, SE-106 91 Stockholm, Sweden232Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz,

Santa Cruz, CA 95064, USA233Department of Physics, KTH Royal Institute of Technology, AlbaNova, SE-106 91 Stockholm, Sweden

234Tokyo Metropolitan University, Department of Physics, Minami-osawa 1-1, Hachioji, Tokyo 192-0397, Japan235Universita di Pisa and Istituto Nazionale di Fisica Nucleare, Sezione di Pisa I-56127 Pisa, Italy

236Istituto Nazionale di Fisica Nucleare, Sezione di Trieste, I-34127 Trieste, Italy237Dipartimento di Fisica, Universita di Trieste, I-34127 Trieste, Italy

238Istituto Nazionale di Fisica Nucleare, Sezione di Padova, I-35131 Padova, Italy239Dipartimento di Fisica e Astronomia “G. Galilei”, Universita di Padova, I-35131 Padova, Italy

240Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I-56127 Pisa, Italy241Istituto Nazionale di Fisica Nucleare, Sezione di Bari, I-70126 Bari, Italy

242Istituto Nazionale di Fisica Nucleare, Sezione di Torino, I-10125 Torino, Italy243Dipartimento di Fisica Generale “Amadeo Avogadro” , Universita degli Studi di Torino, I-10125 Torino, Italy

244NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA245Laboratoire Leprince-Ringuet, Ecole polytechnique, CNRS/IN2P3, Palaiseau, France

246Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County, Baltimore, MD 21250, USA247Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

248Consorzio Interuniversitario per la Fisica Spaziale (CIFS), I-10133 Torino, Italy249Dipartimento di Fisica “M. Merlin” dell’Universita e del Politecnico di Bari, I-70126 Bari, Italy

250INAF—Istituto di Astrofisica Spaziale e Fisica Cosmica, I-20133 Milano, Italy251Agenzia Spaziale Italiana (ASI) Science Data Center, I-00133 Roma, Italy

252College of Science, George Mason University, Fairfax, VA 22030, resident at Naval Research Laboratory, Washington, DC 20375, USA253Istituto Nazionale di Fisica Nucleare, Sezione di Perugia, I-06123 Perugia, Italy

254Laboratoire Univers et Particules de Montpellier, Universite Montpellier, CNRS/IN2P3, Montpellier, France255Department of Physics and Astronomy, Sonoma State University, Rohnert Park, CA 94928-3609, USA

256INAF Istituto di Radioastronomia, I-40129 Bologna, Italy257Dipartimento di Astronomia, Universita di Bologna, I-40127 Bologna, Italy

258Universita Telematica Pegaso, Piazza Trieste e Trento, 48, I-80132 Napoli, Italy259Universita di Udine, I-33100 Udine, Italy

260Department of Physical Sciences, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan261Erlangen Centre for Astroparticle Physics, D-91058 Erlangen, Germany

262Instituto de Astrofısica, Facultad de Fısica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile263Department of Physics and Department of Astronomy, University of Maryland, College Park, MD 20742, USA

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 21

264Laboratoire AIM, CEA-IRFU/CNRS/Universite Paris Diderot, Service d’Astrophysique, CEA Saclay, F-91191 Gif sur Yvette, France265Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA

266NASA Postdoctoral Program Fellow, USA267Institut fur Astro- und Teilchenphysik and Institut fur Theoretische Physik, Leopold-Franzens-Universitat Innsbruck, A-6020 Innsbruck, Austria

268University of North Florida, Department of Physics, 1 UNF Drive, Jacksonville, FL 32224 , USA269School of Physics and Astronomy, University of Southampton, Highfield, Southampton, SO17 1BJ, UK

270Science Institute, University of Iceland, IS-107 Reykjavik, Iceland271Institute of Space Sciences (IEEC-CSIC), Campus UAB, E-08193 Barcelona, Spain

272email: Julie.E.McEnery@nasa.gov273Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

274Max-Planck-Institut fur Physik, D-80805 Munchen, Germany275Department of Physics and Astronomy, University of Denver, Denver, CO 80208, USA

276Department of Physics, University of Johannesburg, PO Box 524, Auckland Park 2006, South Africa277Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong, China

278The University of Hong Kong, Laboratory for Space Research, Hong Kong, China279NYCB Real-Time Computing Inc., Lattingtown, NY 11560-1025, USA

280Department of Chemistry and Physics, Purdue University Calumet, Hammond, IN 46323-2094, USA281Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan

282Max-Planck-Institut fur Kernphysik, D-69029 Heidelberg, Germany283Institucio Catalana de Recerca i Estudis Avancats (ICREA), Barcelona, Spain

284Department of Physics, 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501, Japan285INAF—Osservatorio Astronomico di Roma, via Frascati 33, I-00078 Monte Porzio Catone (RM), Italy

286INAF—Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I-35122 Padova, Italy287INAF—Osservatorio Astronomico di Brera, via E. Bianchi 46, I-23807 Merate, Italy

288INAF—Osservatorio Astronomico di Capodimonte, salita Moiariello 16, I-80131 Napoli, Italy289INAF—Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129 Bologna, Italy

290Scuola Normale Superiore, Piazza dei Cavalieri, 7, I-56126 Pisa, Italy291ASI-Science Data Center, via dl Politecnico s.n.c., I-00133 Roma, Italy

292Dip. di Fisica Ettore Pancini, University of Naples Federico II, C.U. Monte Sant’Angelo, Via Cinthia, I-80126, Napoli, Italy293INAF—ORA—Osservatorio Astronomico di Cagliari, Via della Scienza n. 5, I-09047 Selargius (CA), Italy

294INAF—Osservatorio Astronomico di Torino, Strada Osservatorio 20, I-10025, Pino Torinese (To), Italy295INAF—Institute for Space Astrophysics and Planetology, Via Fosso del Cavaliere 100, I-00133 Rome, Italy296ISDC, Department of astronomy, University of Geneva, chemin d’Ecogia, 16 CH-1290 Versoix, Switzerland

297DTU Space—National Space Institute Elektrovej—Building 327 DK-2800 Kongens Lyngby Denmark298Space Science Group, School of Physics, University College Dublin, Belfield, Dublin 4, Ireland

299European Space Astronomy Centre (ESA/ESAC), Science Operations Department, E-28691, Villanueva de la Ca nada, Madrid, Spain300APC, AstroParticule et Cosmologie, Universite Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cite, 10 rue Alice Domont et

Leonie Duquet, F-75205 Paris Cedex 13, France301INAF, IASF-Milano, via E.Bassini 15, I-20133 Milano, Italy

302Universite Toulouse; UPS-OMP; CNRS; IRAP; 9 Av. Roche, BP 44346, F-31028 Toulouse, France303Francois Arago Centre, APC, Universite Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris,, Sorbonne Paris Cite, 10 rue Alice Domon et Leonie

Duquet, 75205 Paris Cedex 13, France304Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA

305Hubble Fellow306Department of Particle Physics and Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel307Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA

308Max Planck Institute for Astronomy, Knigstuhl 17, D-69117 Heidelberg, Germany309Dark Cosmology Centre, Niels Bohr Institute, Juliane Maries Vej 30, Copenhagen , DK-2100, Denmark

310Department of Astronomy and the Oskar Klein Centre, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden311Lockheed Martin Space Systems Company, Palo Alto, CA 94304

312University of California, Berkeley, Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720-7450, USA313Ioffe Physical Technical Institute, Politekhnicheskaya 26, St. Petersburg, 194021, Russia

314Emeritus315Universities Space Research Association, 7178 Columbia Gateway Drive, Columbia, MD 21046 USA

22

316Institute for Space-Earth Environmental Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan317Institute of Astronomy, Graduate School of Science, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan

318The Research Institute for Time Studies, Yamaguchi University, Yamaguchi, Yamaguchi 753-8511, Japan319Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan

320Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan321Department of Astronomy, Kyoto University, Kyoto, Kyoto 606-8502, Japan

322Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Asakuchi, Okayama 719-0232, Japan323Physics Department, Yale University, New Haven, CT 06520, USA

324Astrophysics Research Institue, Liverpool JMU, Liverpool L3 5RF, UK325Monash Centre for Astrophysics (MoCA), Monash University, Clayton VIC 3800, Australia

326School of Physics & Astronomy, Monash University, Clayton VIC 3800, Australia327University of Nova Gorica, Vipavska 13, 5000 Nova Gorica, Slovenia

328Faculty of Mathematics and Physics, University of Ljubljana, Jadranska 19, 1000 Ljubljana, Slovenia329Department of Physics, University of Bath, BA2 7AY, UK

330University of Warwick, Department of Physics, Gibbet Hill Road, Coventry, CV4 7AL, UK331ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands

332Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK333SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, the Netherlands

334Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands335Lomonosov Moscow State University, Sternberg Astronomical Institute, 13, Universitetskiy prospekt, Moscow, 119234, Russia

336South African Astronomical Observatory, PO Box 9, 7935 Observatory , Cape Town, South Africa337The Instituto de Astrofisica de Canarias, Calle Via Lactea, s/n, E-38200 La Laguna, Tenerife, Spain

338Applied Physics Institute, Irkutsk State University, 20, Gagarin blvd,, Irkutsk, 664003, Russia339Kislovodsk Solar Station of the Main (Pulkovo) Observatory RAS, P.O.Box 45, ul. Gagarina 100, Kislovodsk, 357700, Russia

340Blagoveschensk State Pedagogical University, Lenin str., 104, Amur Region, Blagoveschensk, 675000, Russia341Department of Physics, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8851, Japan

342MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan343Department of Physics, Nihon University, 1-8-14 Kanda-Surugadai, Chiyoda-ku, Tokyo 101-8308, Japan

344JEM Mission Operations and Integration Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba,

Ibaraki 305-8505, Japan345Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa

252-5210, Japan346Department of Earth and Space Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, Japan

347University of California, Berkeley, Astronomy Dept., 501 Campbell Hall #3411, Berkeley, CA 94720, USA348Eureka Scientific, Inc., 2452 Delmer Street Suite 100, Oakland, CA 94602, USA

349Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA350International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia

351Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, Canada352School of Chemical & Physical Sciences, Victoria University of Wellington, PO Box 600, Wellington 6140, New Zealand

353Osservatorio di Radio Astronomia, Istituto Nazionale di Astrofisica, Bologna, I-40123, Italy354Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK

355Institute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USA356Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

357Department of Physics, Harvard University, Cambridge, MA 02138, USA358Millennium Institute of Astrophysics, Casilla 36D, Santiago, Chile

359Departamento de Ciencias Fisicas, Universidad Andres Bello, Avda. Republica 252, Santiago, Chile360Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

361Institut d’Astrophysique de Paris, CNRS, and Universite Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014, Paris, France362European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile

363Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vaialantie 20, FI-21500 Piikkio, Finland364Departamento de Astronomia, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile

365Sorbonne Universites, UPMC Univ. Paris 06, UMR 7585, LPNHE, F-75005, Paris, France366CNRS, UMR 7585, Laboratoire de Physique Nucleaire et des Hautes Energies, 4 place Jussieu, F-75005 Paris, France

367Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA

LOCALIZATION AND BROADBAND FOLLOW-UP OF GW150914 23

368Department of Physics, University of California Santa Barbara, Santa Barbara, CA 93106, USA369Benoziyo Center for Astrophysics, Weizmann Institute of Science, 76100 Rehovot, Israel

370Faculty of Physics, University of Warsaw, 02-093 Warszawa, Poland371Center for Theoretical Physics of the Polish Academy of Sciences, 02-668 Warszawa, Poland

372Department of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK373Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA

374Los Alamos National Laboratory, B244, Los Alamos, NM, 87545, USA375L’Institut de Recherche en Astrophysique et Planetologie, CNRS UMR 5277/UPS, 14 avenue Edouard Belin, F-31400 Toulouse, France

376University of Texas at San Antonio, San Antonio, TX, USA377Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, 4242 TAMU, College Station,

TX 77843, USA378Universidad Nacional de Cordoba, IATE, Laprida 854, Cordoba, Argentina

379Instituto de Astrofısica, Pontificia Universidad Catolica de Chile, Av. Vicuna Mackenna 4860, Santiago, Chile380Instituto de Astrofısica de Andalucıa, Consejo Superior de Investigaciones Cientıficas, Glorieta de la Astronomıa s/n, E-18008 Granada, Spain

381Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, 107 Reykjavik, Iceland