Search for a Structure in the B0sπ± Invariant Mass Spectrum with the ATLAS Experiment

Search for a Structure in the B0 sπInvariant Mass Spectrum with the ATLAS Experiment M. Aaboud et al.* (ATLAS Collaboration) (Received 8 February 2018; revised manuscript received 29 March 2018; published 18 May 2018) A search for the narrow structure, Xð5568Þ, reported by the D0 Collaboration in the decay sequence X→B0 sπ,B0 s→J=ψϕ, is presented. The analysis is based on a data sample recorded with the ATLAS detector at the LHC corresponding to 4.9fb−1of pp collisions at 7 TeV and 19.5fb−1at 8 TeV. No significant signal was found. Upper limits on the number of signal events, with properties corresponding to those reported by D0, and on the Xproduction rate relative to B0 smesons, ρX, were determined at 95% confidence level. The results are NðXÞ<382 and ρX<0.015 for B0 smesons with transverse momenta above 10 GeV, and NðXÞ<356 and ρX<0.016 for transverse momenta above 15 GeV. Limits are also set for potential B0 sπresonances in the mass range 5550 to 5700 MeV. DOI: 10.1103/PhysRevLett.120.202007 The D0 Collaboration reported evidence of a narrow structure, Xð5568Þ, in the decay X→B0 sπwith B0 s→ J=ψϕ in proton-antiproton collisions at a center-of-mass energy of ffiffiffi s p¼1.96 TeV at the Tevatron collider [1]. The structure was interpreted as a tetraquark with four different quark flavors: b,s,u, and d. The mass and natural width of this state were fitted to be m¼5567.82.9ðstatÞþ0.9 −1.9ðsystÞ and Γ¼21.96.4ðstatÞþ5.0 −2.5ðsystÞMeV, respectively, and the signal significance is 5.1σ. The ratio ρXof the yield of Xð5568Þto the yield of the B0 smeson for a transverse momentum range 10 <p TðB0 sÞ<30 GeV was measured to be 0.086 0.019ðstatÞ0.014ðsystÞ. The result initiated a discussion of the nature of the new state and prospects for observation of other tetraquark hadrons [2–6]. Recently, the D0 Collaboration reported further evidence for the resonance Xð5568Þ[7] in the decay sequence X→B0 sπ,B0 s→μ∓νDs,Ds→ϕπ, which is consistent with their previous measurement [1]. However, searches for Xð5568Þin decays to B0 sπ,B0 s→ J=ψϕ performed by the LHCb [8] and CMS [9] Collaborations in proton-proton (pp) collisions at the LHC and by the CDF Collaboration [10] at the Tevatron, revealed no signal. The upper limits ρX< 0.024 [LHCb, pTðB0 sÞ>10 GeV], ρX<0.011 [CMS, pTðB0 sÞ>10 GeV] and ρX<0.010 [CMS, pTðB0 sÞ> 15 GeV] at 95% confidence level (C.L.) were determined within the acceptances of the LHCb and CMS experiments. CDF set an upper limit ρX<0.067 at 95% C.L. within a kinematic range similar to that of D0 [1]. In this Letter, a search for the Xð5568Þstate by the ATLAS experiment at the LHC is presented (B0 srefers to both the B0 sand ¯ B0 smesons). The B0 smesons are reconstructed in their decays to J=ψðμþμ−ÞϕðKþK−Þ. The analysis is based on a combined sample of pp collision data at ffiffiffi s p¼7and 8 TeV corresponding to integrated luminosities of 4.9 and 19.5fb−1, respectively. The ATLAS detector [11] covers nearly the entire solid angle around the collision point with layers of tracking detectors, calorimeters, and muon chambers. The muon and tracking systems are of particular importance in the reconstruction of B mesons. The inner tracking detector (ID) consists of a silicon pixel detector, a silicon microstrip detector and a transition radiation tracker. The muon spectrometer (MS) surrounds the calorimeters and consists of three large superconducting toroids with eight coils each, a system of tracking chambers, and detectors for triggering. To study the detector response, to estimate backgrounds, and to model systematic effects, 12 ×106Monte Carlo (MC) simulated B0 s→J=ψϕ and 1×106B0 sπevents were generated using P ythia 8.183 [12,13] tuned with ATLAS data [14]. Multiple overlaid proton-proton collisions (pileup) were simulated with P ythia soft QCD processes. The detector response was simulated using the ATLAS simulation framework [15] based on GEANT 4[16]. The MC events were weighted to reproduce the same pileup and trigger conditions as in the data. As in the D0 analysis [1], the B0 sπresonance was generated using the Breit-Wigner (BW) parametrization appropriate for an S-wave two-body decay near threshold: *Full author list given at the end of the Letter. Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3. PHYSICAL REVIEW LETTERS 120, 202007 (2018) 0031-9007=18=120(20)=202007(19) 202007-1 © 2018 CERN, for the ATLAS Collaboration FBW(mðB0 sπÞ;m X;ΓX) ¼mðB0 sπÞmXΓ(mðB0 sπÞ;ΓX) (m2 X−m2ðB0 sπÞ)2þm2 XΓ2(mðB0 sπÞ;ΓX);ð1Þ where mðB0 sπÞis the invariant mass of the B0 sπ candidate and mXand ΓXare the mass and the natural width of the resonance. The mass-dependent width is Γ(mðB0 sπÞ;ΓX)¼ΓX×ðq1=q0Þ, where q1and q0are the magnitudes of the three-vector momenta of the B0 s meson in the rest frame of the B0 sπsystem at the invariant masses equal to mðB0 sπÞand mX, respectively. The mass and the width were set to mX¼5567.8MeV and ΓX¼21.9MeV, as reported in Ref. [1]. The events were selected by the dimuon triggers [17] based on identification of a J=ψ→μþμ−decay, with pTthresholds of either 4 or 6 GeV, with both symmetric, (4, 4) or (6, 6) GeV, and asymmetric, (4,6) GeV, combinations. In addition, each event must contain at least one reconstructed primary vertex (PV), formed from at least six ID tracks. The selection of J=ψand ϕ→KþK−candidates is identical to the one described in detail in Ref. [18]. Candidates for B0 s→J=ψϕ decays are selected by fitting the tracks for each combination of J=ψ→μþμ−and ϕ→KþK−to a common vertex. The fit is further constrained by fixing the invariant mass of the two muon tracks to the J=ψmass [19]. A quadruplet of tracks is accepted for further analysis if the vertex fit has a χ2=d:o:f:<3. For each B0 smeson candidate the proper decay time tis extracted using the method described in Ref. [18]. Events with t> 0.2 ps are selected to reduce the background from the events with a J=ψ produced directly in the pp collision. If there is more than one accepted B0 scandidate in the event, the candidate with the lowest χ2=d:o:f:of the vertex fit is selected. For the selected events the average number of proton-proton interactions per bunch crossing is 21, necessitating a choice of the best candidate for the PV at which the B0 smeson is produced. The variable used is the three-dimensional impact parameter d0, which is calculated as the distance between the line extrapolated from the reconstructed B0 s meson vertex in the direction of the B0 smomentum, and each PV candidate. The chosen PV is the one with the smallest d0. Using MC simulation it was shown that the fraction of B0 scandidates that are assigned the wrong PV is less than 1% [18] and that the corresponding effect on the results is negligible. Finally, a requirement that the B0 s transverse momentum is greater than 10 GeV is applied. Figure 1shows the reconstructed J=ψKþK−mass distribution and the result of an extended unbinned maximumlikelihood fit in the range (5150–5650) MeV, in which the signal is modeled by a sum of two Gaussian distributions and an exponential function is used to model the combinatorial background. The observed signal width is consistent with MC simulation. The fitted B0 smass is mfitðB0 sÞ¼5366.60.1ðstatÞMeV, in agreement with the world average value 5366.89 0.19 MeV [19]. For further investigation, only candidates with a reconstructed mass in the signal region 5346.6–5386.6 MeV are included, which gives NðB0 sÞ¼52750 280 ðstatÞcandidates. The B0 sπcandidates are constructed by combining each of the tracks forming the selected PV with the selected B0 s candidate. Tracks that were already used to reconstruct the B0 scandidate and tracks identified as leptons (eor μ) are excluded, as well as tracks with transverse momentum pT<500 MeV. This pTselection was chosen to maximize the ratio of the B0 sπsignal to the background, based on MC simulation. Assigning the pion mass hypothesis to the tracks that pass these selection criteria, the mass mðB0 sπÞ is calculated as mðJ=ψKKπÞ−mðJ=ψKKÞþmfitðB0 sÞ, where mfitðB0 sÞ¼5366.6MeV. On average there are 1.8 B0 sπcandidates in each selected event and all are retained for the analysis. A systematic study has shown that the effect on the results due to multiple candidates is negligible. The mass distribution of B0 sπcandidates is fitted using an extended unbinned maximum-likelihood method. The probability density function (PDF) for the background component is defined as a threshold function: Fbck(mðB0 sπÞ)¼mðB0 sπÞ−mthr na × expX 4 i¼1 pimðB0 sπÞ−mthr ni; ð2Þ where mthr ¼mfitðB0 sÞþmπand n,a, and piare free parameters of the fit. The background PDF was tested using ) [MeV] - K + KψJ/(m 5200 5300 5400 5500 5600 Events / 5 MeV 0 1000 2000 3000 4000 5000 6000 7000 8000 9000 Data Signal (S) Background (B) Fit(S+B) ATLAS -1 =7 TeV, 4.9 fbs -1 =8 TeV, 19.5 fbs FIG. 1. The invariant mass distribution for B0 s→J=ψϕ candidates satisfying the selection criteria. Data are shown as points and results of fits to signal (dashed), background (dotted), and the total fit (solid) are shown as lines. The two outer (red) shaded bands and the central (green) shaded band represent the mass sidebands and the signal region of B0 smeson candidates, respectively. PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-2 events with no real B0 sπcandidates from two categories. The first background sample contains data events where B0 sπcandidates are formed using “fake”B0 smesons from the mass sidebands, shown in Fig. 1by red shaded bands, defined as 5150 <mðJ=ψKþK−Þ<5210 MeV and 5510 <mðJ=ψKþK−Þ<5650 MeV. The second background sample is modeled using MC events containing only B0 smesons not originating from the B0 sπsignal, tuned to reproduce the B0 stransverse momentum distribution in data. In these events the B0 smeson is combined with each of the tracks originating from the selected PV. The first sample is normalized to the fitted number of B0 sbackground events in the B0 smass signal region 5346.6–5386.6 MeV, while the second sample is normalized to the fitted number of B0 s signal events in the same region. The sum of these two distributions is consistent with the distribution of the data. ThefunctioninEq.(2) describes both background distributions as well as their sum within uncertainties. The signal PDF Fsig(mðB0 sπÞ)is defined as a convolution of an Swave Breit-Wigner PDF, defined in Eq. (1), and the detector resolution represented by a Gaussian function with a width that is calculated individually for each B0 sπcandidate from the tracking and vertexing error matrices. Using MC and data samples, it has been verified that the per candidate mass resolutions are the same for the B0 sπsignal and for the background events passing the selection criteria. The average resolution for the B0 sπsignal, with the mass and width corresponding to those of the structure reported by the D0 Collaboration (mX¼5567.8MeV and ΓX¼21.9MeV), is 3.2 MeV. The full probability function used is F(mðB0 sπÞ)¼NðXÞFsig(mðB0 sπÞ) þ½Ncan −NðXÞFbck(mðB0 sπÞ);ð3Þ where NðXÞis the number of signal events and Ncan is the number of all selected B0 sπcandidates. The signal mass and width are fixed to the central values reported by the D0 Collaboration. Following other experiments, fits are performed for two subsets of B0 sπcandidates, first with pTðB0 sÞ>10 GeV and second with pTðB0 sÞ>15 GeV. The results of the fits are shown in Fig. 2and summarized in Table I. No significant Xð5568Þsignal is observed. Additional selections such as cuts on the angle between the momenta of the B0 sand πcandidates were investigated and did not produce evidence of a signal. These were found to introduce peaking background so are not included in the analysis. The yields NðXÞand NðB0 sÞobtained from the fits areusedtoevaluatetheXproduction rate relative to B0 s, within the ATLAS acceptance, using the formula ρX≡σðpp →XþanythingÞ×BðX→B0 sπÞ σðpp →B0 sþanythingÞ ¼NðXÞ NðB0 sÞ×1 ϵrelðXÞ;ð4Þ where σrepresents the production cross section for each of the particles, within the ATLAS acceptance, and the relative efficiency ϵrelðXÞ¼ϵðXÞ=ϵðB0 sÞis the selection efficiency for the state X, decaying to B0 sπ,relativetothatfortheB0 s meson and accounts for the reconstruction and selection FIG. 2. Results of the fit to the B0 sπmass distribution for candidates with pTðB0 sÞ>10 GeV (left) and pTðB0 sÞ>15 GeV (right). The bottom panels show the difference between each data point and the fit divided by the statistical uncertainty of that point. TABLE I. Yields of B0 sand Xð5568Þcandidates obtained from the fits to the B0 sand B0 sπcandidate mass distributions, with statistical uncertainties. The values given for NðB0 sÞare those inside the B0 ssignal window. The reported values for Xð5568Þare obtained from the fits with signal mass and width parameters fixed to those reported by the D0 Collaboration. The relative efficiencies ϵrelðXÞand their uncertainties are described in the text. NðB0 sÞ=103pTðB0 sÞ>10 GeV 52.75 0.28 pTðB0 sÞ>15 GeV 43.46 0.24 NðXÞpTðB0 sÞ>10 GeV 60 140 pTðB0 sÞ>15 GeV −30 150 ϵrelðXÞpTðB0 sÞ>10 GeV 0.53 0.09 pTðB0 sÞ>15 GeV 0.60 0.10 PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-3 efficiency of the companion pion, including the soft pion acceptance. The relative efficiency, ϵrelðXÞ, was determined using MC simulation of events containing X→B0 sπand B0 s decays. In the ratio, the acceptance of the B0 sdecay cancels, so the value to be determined is the pion reconstruction efficiency for B0 sπevents in which the B0 smeson satisfies acceptance, reconstruction, and selection criteria. Based on MC events, ϵrelðXÞis determined as a function of pTðB0 sÞand of mðB0 sπÞ. Using an MC-based function, the acceptance is determined individually for each B0 sπcandidate, based on its measured values of pTðB0 sÞand mðB0 sπÞ. The acceptance ratio, ϵrelðXÞ,is calculated as an average over the events included in the mðB0 sπÞinterval within which the search for a resonance is performed. The width of this interval is defined by a BW function convolved with the mass resolution function, with the start and end points of the range chosen to include 99% of the signal events. The uncertainty of ϵrelðXÞis calculated by varying the fitted parameters of the MCbased function used to describe the acceptance as a function of pTðB0 sÞwithin their uncertainties. Small variations of this function due to the pseudorapidity of the B0 swere investigated and are included in the systematic uncertainties. The error also includes the uncertainty in the number of data events used in the average and the statistical uncertainty in the pTðB0 sÞdistribution of these events. The error in the pion reconstruction efficiency, arising from uncertainties in the amount of ID material, is found to have a negligible effect on ρX. As no significant signal is observed, corresponding to the properties of the Xð5568Þas reported by Ref. [1], upper limits are determined for the number of B0 sπsignal events, NðXÞ, and for the relative production rate, ρX. These are calculated using the asymptotic approximation from the profile likelihood formalism [20] based on the CLsfrequentist method [21]. To establish the limit on the number of B0 sπsignal events, the PDF models for signal and background, defined respectively by Eqs. (1) and (2), are used as inputs to the CLsmethod. Without systematic uncertainties, the extracted upper limits at 95% C.L. are NðXÞ<264 for pTðB0 sÞ>10 GeV and NðXÞ<213 for pTðB0 sÞ>15 GeV. Systematic uncertainties affecting these limits are included in the determination of NðXÞ. To obtain results that can be compared to the state Xð5568Þ reported by the D0 Collaboration, systematic uncertainties are assigned by varying the values of mXand ΓXindependently within Gaussian constraints, with uncertainties equal to those quoted in Ref. [1]. The default model of the Xresonance, which is assumed to be spinless, is changed to a BW P-wave resonance. To include the systematic uncertainty due to the modeling of the background, the default PDF of Eq. (2) is replaced by a seventh-order Chebyshev polynomial, allowing more free parameters in the fit. For the detector resolution, the default per-candidate mass resolution model is replaced by the sum of three Gaussian functions with a common mean. The parameters used are determined from the B0 sπMC sample. Using these alternative models, upper limits that include systematic uncertainties are extracted, leading to values NðXÞ<382 for pTðB0 sÞ>10 GeV and NðXÞ<356 for pTðB0 sÞ>15 GeV. To extract the upper limits on ρX additional systematic uncertainties are included. The calculation of ρXalso depends on the precision of extracting the number of B0 ssignal events and the relative efficiency ϵrelðXÞ. To include these uncertainties, the central values and the uncertainties of the number of B0 ssignal events and ϵrelðXÞare used to construct Gaussian constraints, which are included as additional inputs to the CLsmethod. Both the statistical and systematic uncertainties are included after being summed in quadrature. For the B0 ssignal, the default fit model of two Gaussian functions is changed to a triple Gaussian function and the change in the result is taken as a systematic uncertainty. The uncertainty due to the proper decay time requirement t> 0.2 ps was estimated by varying it within the time resolution and found to be negligible. The resulting upper limits at 95% C.L. are ρX<0.015 for pTðB0 sÞ>10 GeV and ρX<0.016 for pTðB0 sÞ>15 GeV. A hypothesis test is performed for the presence of a B0 sπ peak for every 5 MeV step in its mass from 5550 to 5700 MeV, assuming a resonant state as described by Eq. (1), with a BW width of 21.9 MeV [1] and pTðB0 sÞ> 10 GeV. For each B0 sπmass tested, ϵrelðXÞis calculated using the same method as for Xð5568Þ. The values of ϵrelðXÞvary from 0.50 to 0.55 in the search interval. The upper limit of ρXat 95% C.L. is determined for each tested FIG. 3. Upper limits on ρXat 95% C.L. (black squares connected by line) at different masses of a hypothetical resonant state Xdecaying to B0 sπ, for events with pTðB0 sÞ>10 GeV. A BW width of 21.96.4ðstatÞþ5.0 −2.5ðsystÞMeV is assumed, as reported by D0. The values include systematic uncertainties. The expected 95% C.L. upper limits (central black dot-dashed line) with 1σ(green) and 2σ(yellow) uncertainty bands on ρX are shown as a function of the assumed resonance mass. PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-4 mass. The same systematic uncertainties as in the determination of ρXfor the state Xð5568Þare included, with the exception of the Xð5568Þmass uncertainty. The median expected upper limit at 95% C.L. as a function of the B0 sπ mass is also determined with 1σand 2σerror bands. The results are shown in Fig. 3. In conclusion, a search for a new state Xð5568Þdecaying to B0 sπ, with properties as reported by the D0 Collaboration, was performed by the ATLAS experiment at the LHC, using 4.9fb−1of pp collision data at 7 TeVand 19.5fb−1at 8 TeV. No significant signal was found. Within the acceptance in which this analysis is performed, upper limits on the number of signal events, NðXÞ, and on the X production rate relative to B0 smesons, were determined at 95% C.L., resulting in NðXÞ<382 and ρX<0.015 for pTðB0 sÞ>10 GeV, and NðXÞ<356 and ρX<0.016 for pTðB0 sÞ>15 GeV. Limits are also set for potential B0 sπ resonances in the mass range from 5550 to 5700 MeV. Across the full range, the upper limit set on ρXat 95% C.L. varies between 0.010 and 0.018, and does not exceed the 1σerror band from the expected limit. We thank CERN for the very successful operation of the LHC, as well as the support staff from our institutions without whom ATLAS could not be operated efficiently. We acknowledge the support of ANPCyT, Argentina; YerPhI, Armenia; ARC, Australia; BMWFW and FWF, Austria; ANAS, Azerbaijan; SSTC, Belarus; CNPq and FAPESP, Brazil; NSERC, NRC and CFI, Canada; CERN; CONICYT, Chile; CAS, MOST and NSFC, China; COLCIENCIAS, Colombia; MSMT CR, MPO CR and VSC CR, Czech Republic; DNRF and DNSRC, Denmark; IN2P3-CNRS, CEA-DRF/IRFU, France; SRNSFG, Georgia; BMBF, HGF, and MPG, Germany; GSRT, Greece; RGC, Hong Kong SAR, China; ISF, I-CORE and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; NWO, Netherlands; RCN, Norway; MNiSW and NCN, Poland; FCT, Portugal; MNE/IFA, Romania; MES of Russia and NRC KI, Russian Federation; JINR; MESTD, Serbia; MSSR, Slovakia; ARRS and MIZŠ, Slovenia; DST/NRF, South Africa; MINECO, Spain; SRC and Wallenberg Foundation, Sweden; SERI, SNSF and Cantons of Bern and Geneva, Switzerland; MOST, Taiwan; TAEK, Turkey; STFC, United Kingdom; DOE and NSF, USA. In addition, individual groups and members have received support from BCKDF, the Canada Council, CANARIE, CRC, Compute Canada, FQRNT, and the Ontario Innovation Trust, Canada; EPLANET, ERC, ERDF, FP7, Horizon 2020 and Marie Skłodowska-Curie Actions, European Union; Investissements d’Avenir Labex and Idex, ANR, R´egion Auvergne and Fondation Partager le Savoir, France; DFG and AvH Foundation, Germany; Herakleitos, Thales and Aristeia programmes co-financed by EU-ESF and the Greek NSRF; BSF, GIF and Minerva, Israel; BRF, Norway; CERCA Programme Generalitat de Catalunya, Generalitat Valenciana, Spain; the Royal Society and Leverhulme Trust, United Kingdom. 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Gagliardi,53a,53b L. G. Gagnon,97 C. Galea,108 B. Galhardo,128a,128c E. J. Gallas,122 B. J. Gallop,133 P. Gallus,130 G. Galster,39 K. K. Gan,113 S. Ganguly,175 Y. Gao,77 Y. S. Gao,145,h F. M. Garay Walls,34a C. García,170 J. E. García Navarro,170 J. A. García Pascual,35a M. Garcia-Sciveres,16 R. W. Gardner,33 N. Garelli,145 V. Garonne,121 K. Gasnikova,45 C. Gatti,50 A. Gaudiello,53a,53b G. Gaudio,123a I. L. Gavrilenko,98 C. Gay,171 G. Gaycken,23 E. N. Gazis,10 C. N. P. Gee,133 J. Geisen,58 M. Geisen,86 M. P. Geisler,60a K. Gellerstedt,148a,148b C. Gemme,53a M. H. Genest,57 C. Geng,92 S. Gentile,134a,134b C. Gentsos,156 S. George,80 D. Gerbaudo,13 G. Geßner,46 S. Ghasemi,143 M. Ghneimat,23 B. Giacobbe,22a S. Giagu,134a,134b N. Giangiacomi,22a,22b P. Giannetti,126a S. M. Gibson,80 M. Gignac,171 M. Gilchriese,16 D. Gillberg,31 G. Gilles,177 D. M. Gingrich,3,e M. P. Giordani,167a,167c F. M. Giorgi,22a P. F. Giraud,138 P. Giromini,59 G. Giugliarelli,167a,167c D. Giugni,94a F. Giuli,122 M. Giulini,60b B. K. Gjelsten,121 S. Gkaitatzis,156 I. Gkialas,9,t E. L. Gkougkousis,13 P. Gkountoumis,10 L. K. Gladilin,101 C. Glasman,85 J. Glatzer,13 P. C. F. Glaysher,45 A. Glazov,45 M. Goblirsch-Kolb,25 J. Godlewski,42 S. Goldfarb,91 T. Golling,52 D. Golubkov,132 A. Gomes,128a,128b,128d R. Gonçalo,128a R. Goncalves Gama,26a J. Goncalves Pinto Firmino Da Costa,138 G. Gonella,51 L. Gonella,19 A. Gongadze,68 F. Gonnella,19 J. L. Gonski,59 S. González de la Hoz,170 S. Gonzalez-Sevilla,52 L. Goossens,32 P. A. Gorbounov,99 H. A. Gordon,27 B. Gorini,32 E. Gorini,76a,76b A. Gorišek,78 A. T. Goshaw,48 C. Gössling,46 M. I. Gostkin,68 C. A. Gottardo,23 C. R. Goudet,119 D. Goujdami,137c A. G. Goussiou,140 N. Govender,147b,u C. Goy,5E. Gozani,154 I. Grabowska-Bold,41a P. O. J. Gradin,168 E. C. Graham,77 J. Gramling,166 E. Gramstad,121 S. Grancagnolo,17 V. Gratchev,125 P. M. Gravila,28f C. Gray,56 H. M. Gray,16 Z. D. Greenwood,82,v C. Grefe,23 K. Gregersen,81 I. M. Gregor,45 P. Grenier,145 K. Grevtsov,5J. Griffiths,8A. A. Grillo,139 K. Grimm,75 S. Grinstein,13,w Ph. Gris,37 J.-F. Grivaz,119 S. Groh,86 E. Gross,175 J. Grosse-Knetter,58 G. C. Grossi,82 Z. J. Grout,81 A. Grummer,107 L. Guan,92 W. Guan,176 J. Guenther,32 F. Guescini,163a D. Guest,166 O. Gueta,155 R. Gugel,51 B. Gui,113 E. Guido,53a,53b T. Guillemin,5S. Guindon,32 U. Gul,56 C. Gumpert,32 J. Guo,36b W. Guo,92 Y. Guo,36c,x R. Gupta,43 S. Gurbuz,20a G. Gustavino,115 B. J. Gutelman,154 P. Gutierrez,115 N. G. Gutierrez Ortiz,81 C. Gutschow,81 C. Guyot,138 M. P. Guzik,41a C. Gwenlan,122 C. B. Gwilliam,77 A. Haas,112 C. Haber,16 H. K. Hadavand,8N. Haddad,137e A. Hadef,88 S. Hageböck,23 M. Hagihara,164 H. Hakobyan,180,a M. Haleem,45 J. Haley,116 G. Halladjian,93 G. D. Hallewell,88 K. Hamacher,177 P. Hamal,117 K. Hamano,172 A. Hamilton,147a G. N. Hamity,141 P. G. Hamnett,45 K. Han,36c,y L. Han,36c S. Han,35a,35d K. Hanagaki,69,z M. Hance,139 D. M. Handl,102 B. Haney,124 R. Hankache,83 P. Hanke,60a J. B. Hansen,39 J. D. Hansen,39 M. C. Hansen,23 P. H. Hansen,39 K. Hara,164 A. S. Hard,176 T. Harenberg,177 F. Hariri,119 S. Harkusha,95 PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-8 P. F. Harrison,173 N. M. Hartmann,102 Y. Hasegawa,142 A. Hasib,49 S. Hassani,138 S. Haug,18 R. Hauser,93 L. Hauswald,47 L. B. Havener,38 M. Havranek,130 C. M. Hawkes,19 R. J. Hawkings,32 D. Hayden,93 C. P. Hays,122 J. M. Hays,79 H. S. Hayward,77 S. J. Haywood,133 T. Heck,86 V. Hedberg,84 L. Heelan,8S. Heer,23 K. K. Heidegger,51 S. Heim,45 T. Heim,16 B. Heinemann,45,aa J. J. Heinrich,102 L. Heinrich,112 C. Heinz,55 J. Hejbal,129 L. Helary,32 A. Held,171 S. Hellman,148a,148b C. Helsens,32 R. C. W. Henderson,75 Y. Heng,176 S. Henkelmann,171 A. M. Henriques Correia,32 S. Henrot-Versille,119 G. H. Herbert,17 H. Herde,25 V. Herget,178 Y. Hernández Jim´enez,147c H. Herr,86 G. Herten,51 R. Hertenberger,102 L. Hervas,32 T. C. Herwig,124 G. G. Hesketh,81 N. P. Hessey,163a J. W. Hetherly,43 S. Higashino,69 E. Higón-Rodriguez,170 K. Hildebrand,33 E. Hill,172 J. C. Hill,30 K. H. Hiller,45 S. J. Hillier,19 M. Hils,47 I. Hinchliffe,16 M. Hirose,51 D. Hirschbuehl,177 B. Hiti,78 O. Hladik,129 D. R. Hlaluku,147c X. Hoad,49 J. Hobbs,150 N. Hod,163a M. C. Hodgkinson,141 P. Hodgson,141 A. Hoecker,32 M. R. Hoeferkamp,107 F. Hoenig,102 D. Hohn,23 T. R. Holmes,33 M. Holzbock,102 M. Homann,46 S. Honda,164 T. Honda,69 T. M. Hong,127 B. H. Hooberman,169 W. H. Hopkins,118 Y. Horii,105 A. J. Horton,144 J-Y. Hostachy,57 A. Hostiuc,140 S. Hou,153 A. Hoummada,137a J. Howarth,87 J. Hoya,74 M. Hrabovsky,117 J. Hrdinka,32 I. Hristova,17 J. Hrivnac,119 T. Hryn’ova,5A. Hrynevich,96 P. J. Hsu,63 S.-C. Hsu,140 Q. Hu,27 S. Hu,36b Y. Huang,35a Z. Hubacek,130 F. Hubaut,88 F. Huegging,23 T. B. Huffman,122 E. W. Hughes,38 M. Huhtinen,32 R. F. H. Hunter,31 P. Huo,150 A. M. Hupe,31 N. Huseynov,68,c J. Huston,93 J. Huth,59 R. Hyneman,92 G. Iacobucci,52 G. Iakovidis,27 I. Ibragimov,143 L. Iconomidou-Fayard,119 Z. Idrissi,137e P. Iengo,32 O. Igonkina,109,bb T. Iizawa,174 Y. Ikegami,69 M. Ikeno,69 Y. Ilchenko,11,cc D. Iliadis,156 N. Ilic,145 F. Iltzsche,47 G. Introzzi,123a,123b P. Ioannou,9,a M. Iodice,136a K. Iordanidou,38 V. Ippolito,59 M. F. Isacson,168 N. Ishijima,120 M. Ishino,157 M. Ishitsuka,159 C. Issever,122 S. Istin,20a F. Ito,164 J. M. Iturbe Ponce,62a R. Iuppa,162a,162b H. Iwasaki,69 J. M. Izen,44 V. Izzo,106a S. Jabbar,3P. Jackson,1 R. M. Jacobs,23 V. Jain,2G. Jakel,177 K. B. Jakobi,86 K. Jakobs,51 S. Jakobsen,65 T. Jakoubek,129 D. O. Jamin,116 D. K. Jana,82 R. Jansky,52 J. Janssen,23 M. Janus,58 P. A. Janus,41a G. Jarlskog,84 N. Javadov,68,c T. Javůrek,51 M. Javurkova,51 F. Jeanneau,138 L. Jeanty,16 J. Jejelava,54a,dd A. Jelinskas,173 P. Jenni,51,ee C. Jeske,173 S. J´ez´equel,5H. Ji,176 J. Jia,150 H. Jiang,67 Y. Jiang,36c Z. Jiang,145 S. Jiggins,81 J. Jimenez Pena,170 S. Jin,35b A. Jinaru,28b O. Jinnouchi,159 H. Jivan,147c P. Johansson,141 K. A. Johns,7C. A. Johnson,64 W. J. Johnson,140 K. Jon-And,148a,148b R. W. L. Jones,75 S. D. Jones,151 S. Jones,7T. J. Jones,77 J. Jongmanns,60a P. M. Jorge,128a,128b J. Jovicevic,163a X. Ju,176 A. Juste Rozas,13,w A. Kaczmarska,42 M. Kado,119 H. Kagan,113 M. Kagan,145 S. J. Kahn,88 T. Kaji,174 E. Kajomovitz,154 C. W. Kalderon,84 A. Kaluza,86 S. Kama,43 A. Kamenshchikov,132 L. Kanjir,78 Y. Kano,157 V. A. Kantserov,100 J. Kanzaki,69 B. Kaplan,112 L. S. Kaplan,176 D. Kar,147c K. Karakostas,10 N. Karastathis,10 M. J. Kareem,163b E. Karentzos,10 S. N. Karpov,68 Z. M. Karpova,68 V. Kartvelishvili,75 A. N. Karyukhin,132 K. Kasahara,164 L. Kashif,176 R. D. Kass,113 A. Kastanas,149 Y. Kataoka,157 C. Kato,157 A. Katre,52 J. Katzy,45 K. Kawade,70 K. Kawagoe,73 T. Kawamoto,157 G. Kawamura,58 E. F. Kay,77 V. F. Kazanin,111,d R. Keeler,172 R. Kehoe,43 J. S. Keller,31 E. Kellermann,84 J. J. Kempster,80 J Kendrick,19 H. Keoshkerian,161 O. Kepka,129 B. P. Kerševan,78 S. Kersten,177 R. A. Keyes,90 M. Khader,169 F. Khalil-zada,12 A. Khanov,116 A. G. Kharlamov,111,d T. Kharlamova,111,d A. Khodinov,160 T. J. Khoo,52 V. Khovanskiy,99,a E. Khramov,68 J. Khubua,54b,ff S. Kido,70 M. Kiehn,52 C. R. Kilby,80 H. Y. Kim,8S. H. Kim,164 Y. K. Kim,33 N. Kimura,167a,167c O. M. Kind,17 B. T. King,77 D. Kirchmeier,47 J. Kirk,133 A. E. Kiryunin,103 T. Kishimoto,157 D. Kisielewska,41a V. Kitali,45 O. Kivernyk,5E. Kladiva,146b T. Klapdor-Kleingrothaus,51 M. H. Klein,92 M. Klein,77 U. Klein,77 K. Kleinknecht,86 P. Klimek,110 A. Klimentov,27 R. Klingenberg,46,a T. Klingl,23 T. Klioutchnikova,32 F. F. Klitzner,102 E.-E. Kluge,60a P. Kluit,109 S. Kluth,103 E. Kneringer,65 E. B. F. G. Knoops,88 A. Knue,51 A. Kobayashi,157 D. Kobayashi,73 T. Kobayashi,157 M. Kobel,47 M. Kocian,145 P. Kodys,131 T. Koffas,31 E. Koffeman,109 N. M. Köhler,103 T. Koi,145 M. Kolb,60b I. Koletsou,5 T. Kondo,69 N. Kondrashova,36b K. Köneke,51 A. C. König,108 T. Kono,69,gg R. Konoplich,112,hh N. Konstantinidis,81 B. Konya,84 R. Kopeliansky,64 S. Koperny,41a K. Korcyl,42 K. Kordas,156 A. Korn,81 I. Korolkov,13 E. V. Korolkova,141 O. Kortner,103 S. Kortner,103 T. Kosek,131 V. V. Kostyukhin,23 A. Kotwal,48 A. Koulouris,10 A. Kourkoumeli-Charalampidi,123a,123b C. Kourkoumelis,9E. Kourlitis,141 V. Kouskoura,27 A. B. Kowalewska,42 R. Kowalewski,172 T. Z. Kowalski,41a C. Kozakai,157 W. Kozanecki,138 A. S. Kozhin,132 V. A. Kramarenko,101 G. Kramberger,78 D. Krasnopevtsev,100 M. W. Krasny,83 A. Krasznahorkay,32 D. Krauss,103 J. A. Kremer,41a J. Kretzschmar,77 K. Kreutzfeldt,55 P. Krieger,161 K. Krizka,16 K. Kroeninger,46 H. Kroha,103 J. Kroll,129 J. Kroll,124 J. Kroseberg,23 J. Krstic,14 U. Kruchonak,68 H. Krüger,23 N. Krumnack,67 M. C. Kruse,48 T. Kubota,91 H. Kucuk,81 S. Kuday,4b J. T. Kuechler,177 S. Kuehn,32 A. Kugel,60a F. Kuger,178 T. Kuhl,45 V. Kukhtin,68 R. Kukla,88 Y. Kulchitsky,95 S. Kuleshov,34b Y. P. Kulinich,169 M. Kuna,11 T. Kunigo,71 A. Kupco,129 T. Kupfer,46 O. Kuprash,155 H. Kurashige,70 PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-9 79School of Physics and Astronomy, Queen Mary University of London, London, United Kingdom 80Department of Physics, Royal Holloway University of London, Surrey, United Kingdom 81Department of Physics and Astronomy, University College London, London, United Kingdom 82Louisiana Tech University, Ruston, Louisiana, USA 83Laboratoire de Physique Nucl´eaire et de Hautes Energies, UPMC and Universit´e Paris-Diderot and CNRS/IN2P3, Paris, France 84Fysiska institutionen, Lunds universitet, Lund, Sweden 85Departamento de Fisica Teorica C-15, Universidad Autonoma de Madrid, Madrid, Spain 86Institut für Physik, Universität Mainz, Mainz, Germany 87School of Physics and Astronomy, University of Manchester, Manchester, United Kingdom 88CPPM, Aix-Marseille Universit´e and CNRS/IN2P3, Marseille, France 89Department of Physics, University of Massachusetts, Amherst, Massachusetts, USA 90Department of Physics, McGill University, Montreal, Quebec, Canada 91School of Physics, University of Melbourne, Victoria, Australia 92Department of Physics, The University of Michigan, Ann Arbor, Michigan, USA 93Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan, USA 94aINFN Sezione di Milano, Italy 94bDipartimento di Fisica, Universit`a di Milano, Milano, Italy 95B.I. Stepanov Institute of Physics, National Academy of Sciences of Belarus, Minsk, Republic of Belarus 96Research Institute for Nuclear Problems of Byelorussian State University, Minsk, Republic of Belarus 97Group of Particle Physics, University of Montreal, Montreal, Quebec, Canada 98P.N. Lebedev Physical Institute of the Russian Academy of Sciences, Moscow, Russia 99Institute for Theoretical and Experimental Physics (ITEP), Moscow, Russia 100National Research Nuclear University MEPhI, Moscow, Russia 101D.V. Skobeltsyn Institute of Nuclear Physics, M.V. Lomonosov Moscow State University, Moscow, Russia 102Fakultät für Physik, Ludwig-Maximilians-Universität München, München, Germany 103Max-Planck-Institut für Physik (Werner-Heisenberg-Institut), München, Germany 104Nagasaki Institute of Applied Science, Nagasaki, Japan 105Graduate School of Science and Kobayashi-Maskawa Institute, Nagoya University, Nagoya, Japan 106aINFN Sezione di Napoli, Italy 106bDipartimento di Fisica, Universit`a di Napoli, Napoli, Italy 107Department of Physics and Astronomy, University of New Mexico, Albuquerque, New Mexico, USA 108Institute for Mathematics, Astrophysics and Particle Physics, Radboud University Nijmegen/Nikhef, Nijmegen, Netherlands 109Nikhef National Institute for Subatomic Physics and University of Amsterdam, Amsterdam, Netherlands 110Department of Physics, Northern Illinois University, DeKalb, Illinois, USA 111Budker Institute of Nuclear Physics, SB RAS, Novosibirsk, Russia 112Department of Physics, New York University, New York, New York, USA 113The Ohio State University, Columbus, Ohio, USA 114Faculty of Science, Okayama University, Okayama, Japan 115Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, Oklahoma, USA 116Department of Physics, Oklahoma State University, Stillwater, Oklahoma, USA 117Palacký University, RCPTM, Olomouc, Czech Republic 118Center for High Energy Physics, University of Oregon, Eugene, Oregon, USA 119LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit´e Paris-Saclay, Orsay, France 120Graduate School of Science, Osaka University, Osaka, Japan 121Department of Physics, University of Oslo, Oslo, Norway 122Department of Physics, Oxford University, Oxford, United Kingdom 123aINFN Sezione di Pavia, Italy 123bDipartimento di Fisica, Universit`a di Pavia, Pavia, Italy 124Department of Physics, University of Pennsylvania, Philadelphia, Pennsylvania, USA 125National Research Centre “Kurchatov Institute”B.P. Konstantinov Petersburg Nuclear Physics Institute, St. Petersburg, Russia 126aINFN Sezione di Pisa, Italy 126bDipartimento di Fisica E. Fermi, Universit`a di Pisa, Pisa, Italy 127Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania, USA 128aLaboratório de Instrumentação e Física Experimental de Partículas - LIP, Lisboa, Portugal 128bFaculdade de Ciências, Universidade de Lisboa, Lisboa, Portugal 128cDepartment of Physics, University of Coimbra, Coimbra, Portugal 128dCentro de Física Nuclear da Universidade de Lisboa, Lisboa, Portugal 128eDepartamento de Fisica, Universidade do Minho, Braga, Portugal 128fDepartamento de Fisica Teorica y del Cosmos, Universidad de Granada, Granada, Portugal 128gDep Fisica and CEFITEC of Faculdade de Ciencias e Tecnologia, Universidade Nova de Lisboa, Caparica, Portugal PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-16 129Institute of Physics, Academy of Sciences of the Czech Republic, Praha, Czech Republic 130Czech Technical University in Prague, Praha, Czech Republic 131Charles University, Faculty of Mathematics and Physics, Prague, Czech Republic 132State Research Center Institute for High Energy Physics (Protvino), NRC KI, Russia 133Particle Physics Department, Rutherford Appleton Laboratory, Didcot, United Kingdom 134aINFN Sezione di Roma, Italy 134bDipartimento di Fisica, Sapienza Universit`a di Roma, Roma, Italy 135aINFN Sezione di Roma Tor Vergata, Italy 135bDipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy 136aINFN Sezione di Roma Tre, Italy 136bDipartimento di Matematica e Fisica, Universit`a Roma Tre, Roma, Italy 137aFacult´e des Sciences Ain Chock, R´eseau Universitaire de Physique des Hautes Energies - Universit´e Hassan II, Casablanca, Morocco 137bCentre National de l’Energie des Sciences Techniques Nucleaires, Rabat, Morocco 137cFacult´e des Sciences Semlalia, Universit´e Cadi Ayyad, LPHEA-Marrakech, Morocco 137dFacult´e des Sciences, Universit´e Mohamed Premier and LPTPM, Oujda, Morocco 137eFacult´e des sciences, Universit´e Mohammed V, Rabat, Morocco 138DSM/IRFU (Institut de Recherches sur les Lois Fondamentales de l’Univers), CEA Saclay (Commissariat `al’Energie Atomique et aux Energies Alternatives), Gif-sur-Yvette, France 139Santa Cruz Institute for Particle Physics, University of California Santa Cruz, Santa Cruz, California, USA 140Department of Physics, University of Washington, Seattle, Washington, USA 141Department of Physics and Astronomy, University of Sheffield, Sheffield, United Kingdom 142Department of Physics, Shinshu University, Nagano, Japan 143Department Physik, Universität Siegen, Siegen, Germany 144Department of Physics, Simon Fraser University, Burnaby, British Columbia, Canada 145SLAC National Accelerator Laboratory, Stanford, California, USA 146aFaculty of Mathematics, Physics & Informatics, Comenius University, Bratislava, Slovak Republic 146bDepartment of Subnuclear Physics, Institute of Experimental Physics of the Slovak Academy of Sciences, Kosice, Slovak Republic 147aDepartment of Physics, University of Cape Town, Cape Town, South Africa 147bDepartment of Physics, University of Johannesburg, Johannesburg, South Africa 147cSchool of Physics, University of the Witwatersrand, Johannesburg, South Africa 148aDepartment of Physics, Stockholm University, Sweden 148bThe Oskar Klein Centre, Stockholm, Sweden 149Physics Department, Royal Institute of Technology, Stockholm, Sweden 150Departments of Physics & Astronomy and Chemistry, Stony Brook University, Stony Brook, New York, USA 151Department of Physics and Astronomy, University of Sussex, Brighton, United Kingdom 152School of Physics, University of Sydney, Sydney, Australia 153Institute of Physics, Academia Sinica, Taipei, Taiwan 154Department of Physics, Technion: Israel Institute of Technology, Haifa, Israel 155Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel 156Department of Physics, Aristotle University of Thessaloniki, Thessaloniki, Greece 157International Center for Elementary Particle Physics and Department of Physics, The University of Tokyo, Tokyo, Japan 158Graduate School of Science and Technology, Tokyo Metropolitan University, Tokyo, Japan 159Department of Physics, Tokyo Institute of Technology, Tokyo, Japan 160Tomsk State University, Tomsk, Russia 161Department of Physics, University of Toronto, Toronto, Ontario, Canada 162aINFN-TIFPA, Italy 162bUniversity of Trento, Trento, Italy 163aTRIUMF, Vancouver, British Columbia, Canada 163bDepartment of Physics and Astronomy, York University, Toronto, Ontario, Canada 164Faculty of Pure and Applied Sciences, and Center for Integrated Research in Fundamental Science and Engineering, University of Tsukuba, Tsukuba, Japan 165Department of Physics and Astronomy, Tufts University, Medford, Massachusetts, USA 166Department of Physics and Astronomy, University of California Irvine, Irvine, California, USA 167aINFN Gruppo Collegato di Udine, Sezione di Trieste, Udine, Italy 167bICTP, Trieste, Italy 167cDipartimento di Chimica, Fisica e Ambiente, Universit`a di Udine, Udine, Italy 168Department of Physics and Astronomy, University of Uppsala, Uppsala, Sweden 169Department of Physics, University of Illinois, Urbana, Illinois, USA 170Instituto de Fisica Corpuscular (IFIC), Centro Mixto Universidad de Valencia - CSIC, Spain PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-17 171Department of Physics, University of British Columbia, Vancouver, British Columbia, Canada 172Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia, Canada 173Department of Physics, University of Warwick, Coventry, United Kingdom 174Waseda University, Tokyo, Japan 175Department of Particle Physics, The Weizmann Institute of Science, Rehovot, Israel 176Department of Physics, University of Wisconsin, Madison, Wisconsin, USA 177Fakultät für Mathematik und Naturwissenschaften, Fachgruppe Physik, Bergische Universität Wuppertal, Wuppertal, Germany 178Fakultät für Physik und Astronomie, Julius-Maximilians-Universität, Würzburg, Germany 179Department of Physics, Yale University, New Haven, Connecticut, USA 180Yerevan Physics Institute, Yerevan, Armenia 181Centre de Calcul de l’Institut National de Physique Nucl´eaire et de Physique des Particules (IN2P3), Villeurbanne, France 182Academia Sinica Grid Computing, Institute of Physics, Academia Sinica, Taipei, Taiwan aDeceased. bAlso at Department of Physics, King’s College London, London, United Kingdom. cAlso at Institute of Physics, Azerbaijan Academy of Sciences, Baku, Azerbaijan. dAlso at Novosibirsk State University, Novosibirsk, Russia. eAlso at TRIUMF, Vancouver, British Columbia, Canada. fAlso at Department of Physics & Astronomy, University of Louisville, Louisville, KY, USA. gAlso at Physics Department, An-Najah National University, Nablus, Palestine. hAlso at Department of Physics, California State University, Fresno, CA, USA. iAlso at Department of Physics, University of Fribourg, Fribourg, Switzerland. jAlso at II Physikalisches Institut, Georg-August-Universität, Göttingen, Germany. kAlso at Departament de Fisica de la Universitat Autonoma de Barcelona, Barcelona, Spain. lAlso at Tomsk State University, Tomsk, and Moscow Institute of Physics and Technology State University, Dolgoprudny, Russia. mAlso at The Collaborative Innovation Center of Quantum Matter (CICQM), Beijing, China. nAlso at Universita di Napoli Parthenope, Napoli, Italy. oAlso at Institute of Particle Physics (IPP), Canada. pAlso at Horia Hulubei National Institute of Physics and Nuclear Engineering, Bucharest, Romania. qAlso at CPPM, Aix-Marseille Universit´e and CNRS/IN2P3, Marseille, France. rAlso at Department of Physics, St. Petersburg State Polytechnical University, St. Petersburg, Russia. sAlso at Borough of Manhattan Community College, City University of New York, New York City, NY, USA. tAlso at Department of Financial and Management Engineering, University of the Aegean, Chios, Greece. uAlso at Centre for High Performance Computing, CSIR Campus, Rosebank, Cape Town, South Africa. vAlso at Louisiana Tech University, Ruston, LA, USA. wAlso at Institucio Catalana de Recerca i Estudis Avancats, ICREA, Barcelona, Spain. xAlso at Department of Physics, The University of Michigan, Ann Arbor, MI, USA. yAlso at LAL, Univ. Paris-Sud, CNRS/IN2P3, Universit´e Paris-Saclay, Orsay, France. zAlso at Graduate School of Science, Osaka University, Osaka, Japan. aaAlso at Fakultät für Mathematik und Physik, Albert-Ludwigs-Universität, Freiburg, Germany. bbAlso at Institute for Mathematics, Astrophysics and Particle Physics, Radboud University Nijmegen/Nikhef, Nijmegen, Netherlands. ccAlso at Department of Physics, The University of Texas at Austin, Austin, TX, USA. ddAlso at Institute of Theoretical Physics, Ilia State University, Tbilisi, Georgia. eeAlso at CERN, Geneva, Switzerland. ffAlso at Georgian Technical University (GTU), Tbilisi, Georgia. ggAlso at Ochadai Academic Production, Ochanomizu University, Tokyo, Japan. hhAlso at Manhattan College, New York, NY, USA. iiAlso at The City College of New York, New York, NY, USA. jjAlso at Departamento de Fisica Teorica y del Cosmos, Universidad de Granada, Granada, Portugal. kkAlso at Department of Physics, California State University, Sacramento, CA, USA. llAlso at Moscow Institute of Physics and Technology State University, Dolgoprudny, Russia. mmAlso at Departement de Physique Nucleaire et Corpusculaire, Universit´e de Gen`eve, Geneva, Switzerland. nnAlso at Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Barcelona, Spain. ooAlso at School of Physics, Sun Yat-sen University, Guangzhou, China. ppAlso at Institute for Nuclear Research and Nuclear Energy (INRNE) of the Bulgarian Academy of Sciences, Sofia, Bulgaria. qqAlso at Faculty of Physics, M. V. Lomonosov Moscow State University, Moscow, Russia. rrAlso at National Research Nuclear University MEPhI, Moscow, Russia. ssAlso at Department of Physics, Stanford University, Stanford, CA, USA. ttAlso at Institute for Particle and Nuclear Physics, Wigner Research Centre for Physics, Budapest, Hungary. PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-18 uuAlso at Giresun University, Faculty of Engineering, Turkey. vvAlso at Department of Physics, Nanjing University, Jiangsu, China. wwAlso at Institute of Physics, Academia Sinica, Taipei, Taiwan. xxAlso at University of Malaya, Department of Physics, Kuala Lumpur, Malaysia. PHYSICAL REVIEW LETTERS 120, 202007 (2018) 202007-19