Search for high-mass dilepton resonances in pp collisions at √s=8 TeV with the ATLAS detector

Search for high-mass dilepton resonances in pp collisions at ffiffi s p¼8TeV with the ATLAS detector G. Aad et al.* (ATLAS Collaboration) (Received 16 May 2014; published 19 September 2014) The ATLAS detector at the Large Hadron Collider is used to search for high-mass resonances decaying to dielectron or dimuon final states. Results are presented from an analysis of proton-proton (pp) collisions at a center-of-mass energy of 8 TeV corresponding to an integrated luminosity of 20.3fb−1in the dimuon channel. A narrow resonance with Standard Model Zcouplings to fermions is excluded at 95% confidence level for masses less than 2.79 TeV in the dielectron channel, 2.53 TeV in the dimuon channel, and 2.90 TeVin the two channels combined. Limits on other model interpretations are also presented, including a grand-unification model based on the E6gauge group, Zbosons, minimal Z0models, a spin-2 graviton excitation from Randall-Sundrum models, quantum black holes, and a minimal walking technicolor model with a composite Higgs boson. DOI: 10.1103/PhysRevD.90.052005 PACS numbers: 12.60.Cn, 13.85.Qk, 14.80.Rt, 14.80.Tt I. INTRODUCTION The current energy frontier can be explored in the invariant mass spectrum of dielectron or dimuon pairs via a search for new massive resonances at the Large Hadron Collider (LHC). Such a search has been performed using the full 8 TeV center-of-mass energy proton-proton (pp) collision data set of about 20 fb−1recorded with the ATLAS detector [1] in 2012. While the Standard Model (SM) has been confirmed at the LHC, the identification of massive dilepton resonances in proton-proton collisions still constitutes one of the most promising channels in searches for new physics. It implies a fully reconstructed signal over a smooth and wellunderstood background. Models with dilepton resonances are predicted in many scenarios for new physics. Among these are grand-unification models, which are motivated by gauge unification or a restoration of the left-right symmetry violated by the weak interaction. These models predict the existence of additional neutral, spin-1 vector gauge bosons called Z0bosons, due to the existence of larger symmetry groups that break to yield the SM gauge group and additional Uð1Þgauge groups. Examples considered in this article include the Z0bosons of the E6-motivated [2,3] and minimal models [4]. Another Z0signal, the Z0 SSM,is considered due to its inherent simplicity and usefulness as a benchmark model. The sequential Standard Model (SSM) includes a Z0 SSM boson with couplings to fermions equivalent to those of the SM Zboson. Dilepton resonances are also predicted by several models motivated by solutions to the hierarchy problem of the SM, which involves the need to reconcile the very different scales of electroweak symmetry breaking and the gravitational Planck scale (MPl). The search for physics beyond the SM remains as crucial as it was prior to the discovery of the Higgs boson at the LHC [5,6], since solving the hierarchy problem is one of the primary objectives of the LHC physics program. Examples of potential signals in models that address the hierarchy problem are the Z [7–10] boson, the spin-2 graviton excitation in RandallSundrum (RS) models [11], quantum black holes (QBHs) [12], and technimesons in minimal walking technicolor (MWT) [13–16]. These, along with the Z0interpretations motivated by grand unification, are further discussed in Sec. II. To conduct the search, the dilepton invariant mass (mll) line shape is examined for a localized excess of events corresponding to a new resonance, where ll corresponds to either the dielectron or dimuon final state. This is done using signal and background templates that provide the expected yield of events in bins of mll. The methodology is fully described in Sec. XI. This search approach is advantageous because using the full shape of the distribution makes the analysis robust against uncertainties in the background model at high mass. If shape information were not used in the analysis, uncertainty in the background estimate would be more likely to mask a potential signal. The shape-based method is also more sensitive to a signal in the case of a signal with a low-mass tail arising from offshell production, which occurs due to the steeply falling parton distribution function (PDF) of the two colliding partons at large values of Bjorken x. This feature is commonly referred to as a “parton-luminosity tail,”and its size increases with the resonance width. The impact of *Full author list given at the end of the article. Published by the American Physical Society under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published articles title, journal citation, and DOI. PHYSICAL REVIEW D 90, 052005 (2014) 1550-7998=2014=90(5)=052005(30) 052005-1 © 2014 CERN, for the ATLAS Collaboration this parton-luminosity tail on the mll distribution grows as the kinematic limit is approached. The models considered here predict resonances that are narrow relative to the detector resolution. In such cases, interference effects, where they occur, are not expected to significantly alter the line shape and are thus not considered. The exception to this is the class of minimal Z0models described in Sec. II, for which large coupling strengths, and hence larger widths, are considered. In this case, interference effects are included explicitly in the analysis. The potential signals studied in this analysis vary in width and spin, and some exhibit a parton-luminosity tail while others do not. Because of this, the final results given in Sec. XII can be interpreted in the context of other models that are not directly studied here, but that predict resonances in the mll spectrum with similar signal shapes. II. DESCRIPTION AND STATUS OF THEORETICAL MODELS A detailed description of the models studied in this article is given in this section. For most models, the best previous limits from the ATLAS experiment were obtained using 5fb−1of data at ffiffiffi s p¼7TeV [17], while the exclusion results from the CMS experiment are based on 5fb−1of data at ffiffiffi s p¼7TeV and 4fb−1of data at ffiffiffi s p¼ 8TeV [18]. The data collected at 7 TeV have not been used to obtain the results presented in this paper, as doing so would not significantly extend the sensitivity of the search. Previous limits on the mass scale for QBH production are obtained from other sources, as noted in Sec. II E. For the benchmark model, previous results from ATLAS exclude a Z0 SSM boson with mass less than 2.22 TeV at 95% confidence level (C.L.), while previous results from the CMS experiment exclude a Z0 SSM boson with mass less than 2.59 TeV at 95% C.L. Direct searches at the Tevatron experiments [19,20] and indirect constraints from LEP [21–24] have resulted in limits on the Z0 SSM mass of 1.071 [20] and 1.787 TeV [25], respectively. A. E6‐motivated Z0models In the class of models based on the E6gauge group, this unified symmetry group can break to the SM in a number of different ways [2]. In many of them, E6is first broken to SOð10Þ×Uð1Þψ, with SOð10Þthen breaking either to SUð4Þ×SUð2ÞL×SUð2ÞRor SUð5Þ×Uð1Þχ. In the first of these two possibilities, a Z0 3Rcoming from SUð2ÞRor a Z0 B-L from the breaking of SUð4Þinto SUð3ÞC×Uð1ÞB-L could exist at the TeV scale. Both of these Z0bosons appear in the minimal Z0models discussed in the next section. In the SUð5Þcase, the presence of Uð1Þψand Uð1Þχ symmetries implies the existence of associated gauge bosons Z0 ψand Z0 χthat can mix. When SUð5Þis broken down to the SM, one of the Uð1Þ’s can remain unbroken down to intermediate energy scales [2,3]. Therefore, the precise model is governed by a mixing angle θE6, with the new potentially observable Z0boson defined by Z0ðθE6Þ¼Z0 ψcosθE6þZ0 χsin θE6. The value of θE6specifies the Z0boson’s coupling strength to SM fermions as well as its intrinsic width. In comparison to the benchmark Z0 SSM, which has a width of approximately 3% of its mass, the E6models predict narrower Z0signals. The Z0 ψ considered here has a width of 0.5% of its mass, and the Z0 χ has a width of 1.2% of its mass [26,27]. All other Z0signals in this model are defined by specific values of θE6ranging from 0 to π, and have widths between those of the Z0 ψ and Z0 χ. Previous results from ATLAS exclude the Z0 ψ(Z0 χ) boson with mass less than 1.79 TeV (1.97 TeV) at 95% C.L. [17], while the CMS experiment excludes a Z0 ψboson with mass less than 2.26 TeV at 95% C.L. [18]. B. Minimal Z0models In the minimal Z0models [4], the phenomenology of Z0 boson production and decay is characterized by three parameters: two effective coupling constants, gB-L and gY, and the Z0boson mass. This parametrization encompasses Z0bosons from many models, including the Z0 χ belonging to the E6-motivated model of the previous section, the Z0 3Rin a left-right symmetric model [28,29], and the Z0 B-L of the pure B-L model [30], where B (L) is the baryon (lepton) number and B-L is the conserved quantum number. The coupling parameter gB-L defines the coupling of a new Z0boson to the B-L current, while the gY parameter represents the coupling to the weak hypercharge Y. It is convenient to refer to the ratios ~ gB-L ≡gB-L=gZand ~ gY≡gY=gZ, where gZis the coupling of the SM Zboson defined by gZ¼2MZ=v. Here v¼246 GeV is the SM Higgs vacuum expectation value. To simplify further, γ0and θmin are chosen as independent parameters with the following definitions: ~ gB-L ¼γ0cosθmin,~ gY¼γ0sinθmin. The γ0parameter measures the strength of the Z0boson coupling relative to that of the SM Zboson, while θmin determines the mixing between the generators of the B-L and the weak hypercharge Y gauge groups. Specific values of γ0and θmin correspond to Z0bosons in various models, as is shown in Table Ifor the three cases mentioned in this section. TABLE I. Values for γ0and θmin in the minimal Z0models corresponding to three specific Z0bosons: Z0 B-L,Z0 χand Z0 3R. The SM weak mixing angle is denoted by θW. Z0 B-L Z0 χZ0 3R γ0ffiffi 5 8 qsin θWffiffiffiffi 41 24 qsin θW 5 ffiffiffiffi 12 psin θW cos θmin 1ffiffiffiffi 25 41 q1 ffiffi 5 p sin θmin 0−ffiffiffiffi 16 41 q−2 ffiffi 5 p G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-2 For the minimal Z0models, the width depends on γ0and θmin, and the interference with the SM Z=γprocess is included. Couplings to hypothetical right-handed neutrinos and to Wboson pairs are not included. Previous limits on the Z0mass versus couplings in the context of these models were set by the ATLAS experiment; the specific mass limit varies with γ0.Forγ0¼0.2, the range of Z0mass limits at 95% C.L. corresponding to θmin ∈½0;πis 1.1 to 2.10 TeV [17]. C. Zbosons One set of models proposes a solution to the SM hierarchy problem via the introduction of a new doublet of vector bosons: ðZ;WÞ[7–10]. These are predicted to have masses near the weak scale, motivating the search at the LHC. As a result of the tensor form of the coupling, the kinematics of the Zboson’s decay to dileptons are different from that of a Z0boson [7], and there is no interference between this and the Z=γprocess. To fix the Zboson’s coupling strength to fermions, a model with quark-lepton universality is adopted [9,10]. The gauge coupling is chosen to be the same as in the SM SUð2Þ group, and the scale of new physics is proportional to the mass of the new heavy boson. The model parameters are chosen such that the total and partial decay widths of the Ware the same as those of the charged partner of the Z0 SSM boson (W0 SSM) with the same mass. The width of the Z resonance is 3.4% of its mass [10]. Previous ATLAS results exclude a Zwith mass less than 2.20 TeV at 95% C.L. [17]. D. Graviton excitations in Randall-Sundrum models Models with extra dimensions offer an alternative solution to the mass hierarchy problem in that the higher-dimensional Planck scale can be of the order of the electroweak scale. Among them, the Randall-Sundrum model [11] postulates the existence of one warped extra dimension. Specifically, the geometry of the original RS model contains two four-dimensional branes known as the TeV brane and the Planck brane, within a five-dimensional bulk. The extra dimension in the bulk is compactified, which leads to a Kaluza-Klein tower of excited states of the graviton. The particles of the SM are confined to the TeV brane, where due to warping the apparent strength of gravity is exponentially suppressed. Gravity originates on the Planck brane; gravitons are also located on the Planck brane, but can propagate in the bulk. The RS model phenomenology is characterized by the mass of the lightest Kaluza-Klein excitation mode of the graviton known as G, and the ratio k= ¯ MPl, which defines the coupling strength of the Gto SM particles. Here kis a scale that defines the warp factor of the extra dimension and ¯ MPl ¼MPl=ffiffiffiffiffiffi 8π pis the reduced Planck mass. The Gin this model is expected to be narrow for values of k= ¯ MPl <0.2. The intrinsic width of the particle is proportional to ðk= ¯ MPlÞ2, and is 0.014% (5.8%) of the pole mass for k= ¯ MPl ¼0.01ð0.2Þ. A lower bound on k= ¯ MPl of 0.01 is theoretically preferred [31], as it limits the new physics energy scale to be of the order of TeV, and less than 10 TeV. For values above k= ¯ MPl ≈0.1the compactification radius approaches the Planck length and is less motivated on theoretical grounds [31], as this theory does not incorporate quantum gravity. The Gis produced predominantly via quark-antiquark annihilation and gluon fusion, with decays to SM fermions or bosons. While the branching ratio to dileptons is low due to the spin-2 quantum numbers of the particle, the dilepton final state is nevertheless sensitive to new spin-2 resonances due to the clean final state. Previous ATLAS results exclude a Gwith coupling k= ¯ MPl ¼0.1at 95% C.L. for masses less than 2.16 TeV [17], and the corresponding limit from CMS is 2.39 TeV [18]. E. Quantum black holes In the context of models with extra dimensions, semiclassical black holes can be formed at a collider if the available energy is well above the higher-dimensional Planck scale [32,33]. Such black holes would then decay through Hawking radiation. Quantum (or nonthermal) black holes differ from these variants in that they lack a well-defined temperature or significant entropy. This inhibits thermal decays of black holes produced at a mass scale just above the (higher-dimensional) Planck scale, which in turn limits the number of particles in the final state [12]. For two-particle final states, it is interesting to look at the quantum gravity regime, where the threshold for QBH production, Mth, lies between the higher-dimensional Planck scale, and about 5 times this value [12,34,35]. The QBH decay is governed by the yet unknown theory of quantum gravity, but it is assumed that QBHs emit with equal strength all SM particle degrees of freedom. Provided the higher-dimensional Planck scale is not higher than a few TeV, QBHs could be observed at the LHC. Production of QBHs can occur in the original RS model, and in the extra-dimensional model proposed by ArkaniHamed, Dimopoulos, and Dvali (ADD) [36]. Both scenarios are considered in the model interpretation presented here. The ADD model postulates the existence of n≥1 flat additional spatial dimensions, commonly compactified with radius R. Only gravity propagates in these extra dimensions, with SM particles confined to a fourdimensional manifold. The threshold for QBH production in the ADD model is assumed to correspond to the higherdimensional Planck scale. The analysis here was performed assuming n¼6, but the dependence of the resulting production limit on nis small. The specific model [37] used to interpret the result of this article conserves color, electric charge, and total angular SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-3 momentum. Two QBHs states with zero charge produced via q¯ qand gg have predicted branching ratios to each dilepton final state of 0.5% and 0.2%, respectively, assuming conservation of the global symmetries of lepton and baryon number. While the model parameters of Ref. [37] are considered in the context of ADD, one can take the five-dimensional ADD case to obtain an approximate RS model, which is what is used in the case of the RS model interpretation. In the RS model, the higher-dimensional Planck scale ~ Mcan be calculated from the Gmass and k= ¯ MPl as follows [12]: ~ M¼MG 3.83 ×ðk= ¯ MPlÞ2 3 ; where also here the mass threshold for QBH production Mth is assumed to be equal to the higher-dimensional Planck scale. Previous limits on the types of QBH production described in this article were set by the ATLAS experiment using final states with an energetic photon and a jet [38] as well as final states with an energetic lepton and a jet [39]. Previous limits also exist from the CMS experiment from a search dominated by multijet final states [40]. The ATLAS experiment has also set limits on the production of a different type of QBHs using dijet events [41,42]. While QBHs are not resonances, an increase in the dilepton production cross section near the black hole threshold is expected. The expected signal is therefore similar to that predicted by resonance models, and QBHs are thus referred to as resonances in the remainder of this article. F. Minimal walking technicolor Another solution to the hierarchy problem is to postulate that the Higgs boson is a composite particle, bound by a strong force called technicolor. Technicolor models use the new strong dynamics to break electroweak symmetry. These models predict the existence of new narrow technimeson resonances with masses of a few hundred GeV decaying to the dilepton final state. The interpretation used here is in the context of the minimal walking technicolor model [13–16], which predicts a composite Higgs boson having properties consistent, within current uncertainties, with the Higgs boson discovered at the LHC [5,6]. The MWT model used here is defined by the following parameters: the bare axial-vector and vector masses, MA and MV; the coupling of the spin-1 resonance to SM fermions g=~ g, where gis the coupling constant of the weak interaction and ~ gis the strength of the spin-1 resonance interaction; the Sparameter obtained using the zeroth Weinberg sum rule used to constrain MAand MV; the Higgs boson mass mH, and s, the coupling of the Higgs boson to composite spin-1 states. Here the Sparameter and sare set according to the recommendation set forth in Ref. [43]:S¼0.3and s¼0, while mH¼125 GeV is used for the Higgs boson mass. The physical mass of about 125 GeV for the Higgs boson emerges after top quark corrections are taken into account [16]. This model predicts new particles in the form of technimeson triplets: R0; 1and R0; 2. The R0 1and R0 2are produced by quark-antiquark annihilation and decay to dilepton final states via an intermediate Z=γstate. For each pair of values (MR1,~ g), the values of MR2,MA, and MVare unique. The widths and the mass difference of R1and R2 vary strongly depending on the model parameters [44].In this analysis, the model parameter ~ g¼2is used. Previous studies have shown [17] that the mll distributions obtained with ~ g¼2are representative of those for all values of ~ gand MAto which this analysis is currently sensitive. For this analysis, an mll distribution accounting for contributions from both R1and R2is used. However, the magnitude of the mass difference between the two and the characteristics of the distribution are dependent on ~ gand MA. For larger values of ~ gand small values of MA,R2is broad with a reduced amplitude, and therefore does not contribute significantly to the signal shape. Previous limits on this model were set by ATLAS on the bare axial mass, MA, in the MWT model. For a value of the coupling parameter ~ g¼2,MAvalues less than 1.57 TeV were excluded at 95% C.L. [17]. III. ATLAS DETECTOR The ATLAS detector [1] consists of an inner tracking detector system (ID) surrounded by a superconducting solenoid, electromagnetic and hadronic calorimeters, and a muon spectrometer (MS). Charged particles in the pseudorapidity1range jηj<2.5are reconstructed with the ID, which consists of layers of silicon pixel and microstrip detectors and a straw-tube transition-radiation tracker having coverage within jηj<2.0. The ID is immersed in a 2 T magnetic field provided by the solenoid. The latter is surrounded by a hermetic calorimeter that covers jηj<4.9 and provides three-dimensional reconstruction of particle showers. The electromagnetic calorimeter is a liquid argon sampling calorimeter, which uses lead absorbers for jηj<3.2and copper absorbers in the very forward region. The hadronic sampling calorimeter uses plastic scintillator tiles as the active material and iron absorbers in the region jηj<1.7. In the region 1.5<jηj<4.9, liquid argon is used as active material, with copper or/and tungsten absorbers. Outside the calorimeter, air-core toroids supply the magnetic field for the MS. There, three stations of 1ATLAS uses a right-handed coordinate system with its origin at the nominal interaction point in the center of the detector and the zaxis along the beam pipe. The xaxis points from the interaction point to the center of the LHC ring, and the yaxis points upward. Cylindrical coordinates ðr; ϕÞare used in the transverse plane, ϕbeing the azimuthal angle around the beam pipe. The pseudorapidity is defined in terms of the polar angle θ as η¼−lntanðθ=2Þ. G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-4 precision chambers allow the accurate measurement of muon track curvature in the region jηj<2.7. The majority of these precision chambers are composed of drift tubes, while cathode strip chambers provide coverage in the inner stations of the forward region for 2.0<jηj<2.7. Additional muon chambers installed between the inner and middle stations of the forward region and commissioned prior to the 2012 run improve measurements in the transition region of 1.05 <jηj<1.35 where the outer stations have no coverage. Muon triggering is possible in the range jηj<2.4, using resistive-plate chambers in the central region and thin-gap chambers in the forward region. A three-level trigger system [45] selects events to be recorded for off-line analysis. IV. DATA SAMPLE The events in the data set were collected during periods with stable beams and all relevant subsystems operational. The pp collision data recorded between April and December 2012 at ffiffiffi s p¼8TeV amount to 20.3fb−1in the dielectron channel and 20.5fb−1in the dimuon channel. In the dielectron channel, events are triggered by the presence of two energy deposits (“clusters”) in the electromagnetic calorimeter, one with transverse momentum (pT) threshold of pT>35 GeV, and the other with pT>25 GeV. The shower profiles are required to be consistent with those expected for electromagnetic showers [46]. This trigger is preferred over a dedicated dielectron trigger, which incorporates tracking information, because it is advantageous in the estimation of the data-driven background, as explained in Sec. VIII. In the dimuon channel, events are triggered by at least one of two single-muon triggers with transverse momentum thresholds of pT>24 GeV or pT>36 GeV with an additional requirement that the muon candidate be isolated (see Sec. VI) for the former case. V. SIMULATED SAMPLES Expected signal and background yields, with the exception of certain data-driven background estimates, are evaluated with simulated Monte Carlo (MC) samples and normalized using the highest-order cross-section predictions available in perturbation theory. The sample used to model the Drell-Yan (q¯ q→Z=γ→ lþl−) background is generated at next-to-leading order (NLO) using P OWHEG [47] and the CT10 PDF [48], with P YTHIA 8[49] to model parton showering and hadronization. For this and all other samples, the final-state photon radiation (FSR) is handled by P HOTOS [50], and the interaction of particles with the detector and its response are modeled using a full ATLAS detector simulation [51] based on G EANT 4[52]. The Z=γdifferential cross section with respect to mass has been calculated at next-to-next-toleading-order (NNLO) perturbative QCD (pQCD) using FEWZ [53,54] with the MSTW2008NNLO PDF [55]. The calculation includes NLO electroweak (EW) corrections beyond FSR, as well as a contribution from the irreducible, nonresonant photon-induced (PI) background, γγ →lþl−. The PI contribution is estimated using the MRST2004qed PDF [56] at leading order, by taking an average of the predictions obtained under the current and constituent quark mass schemes. Differences between the average and the individual results from those schemes are used to assign the uncertainty on this additive correction. The PI corrections were verified by SANC [57,58]. An additional small correction arises from single boson production in which the final-state charged lepton radiates a real Wor Z boson. This was estimated using M ADGRAPH 5[59], following the prescription outlined in Ref. [60]. A massdependent Kfactor used to scale the Z=γbackground samples is obtained from the ratio of the calculated NNLO pQCD cross section, with additional EW, PI, and real W=Z corrections, to the cross section from the P OWHEG sample. The values of the Kfactors as evaluated at dilepton masses of 1, 2, and 3 TeV are 1.07, 1.10, and 1.14, respectively. Other important backgrounds are due to diboson (WW, WZ, and ZZ) and top quark production. The diboson processes are generated with H ERWIG [61,62] using the CTEQ6L1 PDF [63]. The diboson cross sections are known to NLO with an uncertainty of 5%, and the values used are 57 pb (WW), 21 pb (WZ), and 7.4 pb (ZZ), as calculated with MCFM [64]. Backgrounds from t¯ tand from single top production in association with a Wboson are modeled with MC@NLO [65–67] with H ERWIG using the CT10 PDF. The t¯ tcross section is σt¯ t¼253þ13 −15 pb for a top quark mass of 172.5 GeV. This is calculated at NNLO in QCD including resummation of next-to-next-to-leading logarithmic soft gluon terms with T OP ++2.0 [68–73]. The PDF and αSuncertainties on the t¯ tcross section are calculated using the PDF4LHC prescription [74] with the MSTW2008 68% C.L. NNLO [55,75], CT10 NNLO [48,76], and NNPDF2.3 5f FFN [77] PDF error sets added in quadrature to the scale uncertainty. Varying the top quark mass by 1GeV leads to an additional systematic uncertainty of þ8and −7pb, which is also added in quadrature. The single top background in association with a Wboson has a cross section of σWt ¼22.41.5pb [78]. Given that the Wt contribution is small compared to the t¯ tcross section, an overall uncertainty of 6% is estimated on the top quark background. The simulated top quark samples are statistically limited at high invariant mass, and the expected number of events as a function of mll is therefore extrapolated into this region using fits. A number of fits to the invariant mass distribution are carried out, exploring various fit ranges as well as the two fit functions yðxÞ¼ p1xp2þp3logxand yðxÞ¼p1=ðxþp2Þp3, where yrepresents the expected yield and x¼mll. The mean and rms of these fits are used as the background contribution and its uncertainty, respectively. Background contributions from SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-5 events with jets or photons in the final state that pass the electron selection criteria are determined using the data, as explained in Sec. VIII. In the muon channel this background is negligible. In order to avoid double counting, the simulated samples in the electron channel are filtered for the presence of two electrons. An overview of the simulated MC signal and background samples is given in Table II. Simulated signal processes for the Z0models are obtained by reweighting P YTHIA 8 Drell-Yan samples to the shape of the resonance. The same technique is used for MWT signals, and the shape of the resonance is obtained using M ADGRAPH 5. A reweighting procedure is also used for Zand Gsignals, but it is applied to dedicated samples generated with C ALC HEP [79] in the case of Z, and with P YTHIA 8 in the case of G. For the QBH signals, samples are generated for each assumed energy threshold (Mth) using the QBH [80] generator. The MSTW2008LO PDF [55] is used for all signal samples, except the G, which uses the CTEQ6L PDF [63]. The ratio of the NNLO pQCD cross section calculated with FEWZ without the additional EW, PI, and real W=Z corrections to the cross section from the P YTHIA 8 sample is used to determine a mass-dependent Kfactor for the signal samples. The values of the Kfactors as evaluated at dilepton masses of 1, 2, and 3 TeVare 1.22, 1.16, and 1.16, respectively. The additional EW and real W=Z corrections are not applied to the signal samples because the dominant EW corrections depend on the Wand Zboson couplings of the new particle, and are therefore model dependent. The PI contribution is nonresonant and thus only contributes to the background. No Kfactor is applied to the leading-order Zand QBH cross sections. This is due to the different coupling of the Zto fermions, and the unknown gravitational interaction. For G,aNLO Kfactor was provided by the authors of Refs. [81–83], using CTEQ6L, which is the same PDF used in the simulation of the signal. VI. LEPTON RECONSTRUCTION Electron candidates are formed from clusters of cells reconstructed in the electromagnetic calorimeter with an associated well-reconstructed ID track. The track and the cluster must satisfy a set of identification criteria [46] that are optimized for high pile-up2conditions. These criteria require the shower profiles to be consistent with those expected for electrons and impose a minimum requirement on the amount of transition radiation. In addition, to suppress background from photon conversions, a hit in the first layer of the pixel detector is required if an active pixel layer is traversed. The electron’s energy is obtained from the calorimeter measurements and its direction from the associated track. At transverse energies (ET) relevant to this search, the calorimeter energy resolution is measured in data to be 1.2% for electrons in the central region (jηj<1.37) and 1.8% in the forward region (1.52 <jηj≤2.47)[84].For dielectron masses above 200 GeV, the mass resolution is below 2% over the entire ηrange. To suppress background from misidentified jets, isolated electrons are selected. A limit is placed on the energy corrected for transverse shower leakage and pile-up contained in a cone of radius ΔR¼0.2surrounding the electron candidate in the (η;ϕ) plane: ΔR¼ ffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi ðΔηÞ2þðΔϕÞ2 p. For the leading (highest-pT) electron candidate this energy is required to be less than 0.007 ×ETþ5.0GeV, while for the subleading electron candidate a requirement of less than 0.022 ×ETþ6.0GeV is used. These requirements have been optimized to maintain a high selection efficiency of ≈99% for each electron candidate. The difference in the isolation selection for the leading and subleading electrons takes into account the different energy losses due to bremsstrahlung. Muon tracks are first reconstructed [85,86] separately in the ID and in the MS. The two tracks are then matched and a combined fit is performed using ID and MS hits, taking into account the effects of multiple scattering and energy loss in the calorimeters. The momentum is taken from the combined fit. Each muon is required to have a minimum number of hits in each of the ID components. To obtain optimal momentum resolution, at least one selected muon is required to have at least three hits in each of three stations of the MS, or, for muons in the very forward region, at least two hits in the cathode strip chambers and at least three hits in the middle and outer MS stations. At least one hit in each of two layers of the trigger chambers is also required. These muons are referred to as three-station muons, and have pT resolution at 1 TeV ranging from 19% to 32%, depending on η. In the very forward region of the MS, the hit requirement in the inner station corresponds to at least two hits in the cathode strip chambers. In addition to three-station muons, the best remaining muon candidates in the central region of the MS (jηj<1.05) with at least five precision hits in each of the inner and outer stations are selected, and are referred to TABLE II. Overview of simulated samples used. Process Generator Parton shower PDF Drell-Yan P OWHEG P YTHIA 8.162 CT10 Diboson H ERWIG ++ 2.5.2 H ERWIG 6.520 CTEQ6L1 t¯ t,Wt MC@NLO 4.06 H ERWIG 6.520 CT10 Z0P YTHIA 8.165 P YTHIA 8.165 MSTW2008LO GP YTHIA 8.160 P YTHIA 8.160 CTEQ6L ZC ALC HEP 4.5.1 P YTHIA 8.165 MSTW2008LO MWT M ADGRAPH 5P YTHIA 8.165 MSTW2008LO QBH QBH 1.05 P YTHIA 8.165 CT10 2Multiple pp collisions occurring in the same or neighboring bunch crossings. G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-6 as two-station muons. These two-station muons are required to have at least one hit in one layer of the trigger chambers, and they have slightly worse pTresolution than the three-station muons. Residual misalignments of the muon detectors, which could cause a degradation of the momentum resolution, were studied with collision data in which the muons traversed overlapping sets of muon chambers. The effects of these misalignments and the intrinsic position resolution are included in the simulation. Muon candidates passing through chambers where the alignment quality does not allow a reliable momentum measurement at high pTare rejected. For each three-station (two-station) muon, the difference between the stand-alone momentum measurements from the ID and MS must not exceed 5 (3) times the sum in quadrature of the stand-alone uncertainties. To suppress background from cosmic rays, the muons are also required to satisfy requirements on the track impact parameters with respect to the primary vertex of the event. The impact parameter along the beam axis is required to be within 1 mm, and the transverse impact parameter is required to be within 0.2 mm. The primary vertex of the event is defined as the reconstructed vertex consistent with the beam spot position with the highest Pp2 T. The sum includes the p2 T of all tracks associated with the primary vertex. At least three associated tracks are required, each with pTabove 0.4 GeV. To reduce the background from misidentified jets, each muon is required to be isolated such that ΣpTðΔR<0.3Þ=pTðμÞ<0.05, where ΣpTðΔR<0.3Þis the scalar sum of the pTof all other tracks with pT> 1GeV within a cone of radius ΔR¼0.3around the direction of the muon. VII. EVENT SELECTION Events are required to have at least one reconstructed primary vertex. For the dielectron channel, at least two reconstructed electron candidates within jηj<2.47 are required. In each event, the leading electron and the subleading electron must satisfy ET>40 GeV and ET>30 GeV, respectively. The transition region between the central and forward regions of the calorimeters, in the range 1.37 ≤jηj≤1.52, exhibits degraded energy resolution and is therefore excluded. Because of possible charge misidentification, an opposite-charge requirement is not placed on electron candidates. Charge misidentification can occur either due to bremsstrahlung, or due to the limited momentum resolution of the ID at very high pT. The product of acceptance and efficiency (A×ϵ)is defined as the fraction of simulated candidate events that pass the dilepton event selection requirement in the mll search region 128 GeV <m ll <4500 GeV, out of those generated with a Born level dilepton mass greater than 60 GeV. Figure 1shows A×ϵas a function of the Z0 SSM pole mass for both channels. Using the described search criteria, A×ϵin the dielectron channel is found to be 71% for a Z0 SSM pole mass of 2 TeV. For low values of the Z0 SSM pole mass, A×ϵrises due to kinematic selection requirements. It drops again at high pole mass because the strong decrease of the parton luminosity at high momentum transfer enhances the relative fraction of events in the low-mass tail of the spectrum arising from off-shell Z0 SSM production. Muons passing the reconstruction criteria are required to satisfy pT>25 GeV and are used to build opposite-charge muon pairs. If two opposite-charge muons passing the three-station selection are found, they are used to make the pair and the event is said to pass the “primary dimuon selection.”If no primary dimuon candidate is found, pairs are built with one three-station muon and a two-station muon of opposite charge. Events with such pairs are said to pass the “secondary dimuon selection.”For both selections, if more than one dimuon candidate is found in an event, the one with the highest transverse momentum scalar sum is selected. In the case of a Z0 SSM of mass 2 TeV, A×ϵin the dimuon channel is estimated to be 46%, as can be seen in Fig. 1. The contribution of the primary (secondary) dimuon selection is about 42% (4%) at 2 TeV. Due to the stringent requirements placed on the number and distribution of hits required in the MS, which ensure good momentum resolution at large mll, the A×ϵfor the dimuon channel is lower compared to the dielectron channel. VIII. DATA-DRIVEN BACKGROUNDS As mentioned above, background contributions from events with jets or photons in the final state that pass the electron selection criteria are determined using the data. This includes contributions from dijet, heavy-flavor quarks, and γþjet production referred to hereafter as the dijet [TeV] SSM Z’ M 123 Efficiency×Acceptance 0 0.2 0.4 0.6 0.8 ee→Z’ μμ →Z’ SimulationATLAS = 8 TeVs FIG. 1 (color online). Product of acceptance and efficiency for the dielectron (upper distribution) and dimuon (lower distribution) selections as a function of the Z0 SSM pole mass. SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-7 background. Additional contributions are due to Wþjets processes and top quark production with Wþjets final states referred to hereafter as Wþjets background. The probability that a jet is misidentified as an electron (the “fake rate”) is determined as a function of ETand η using background-enriched data samples. These samples are recorded using several inclusive jet triggers with ET thresholds in the range 25–360 GeV. In each of these samples, the fake rate f1(f2) is calculated as the fraction of leading (subleading) electron candidates that pass the nominal electron identification and isolation requirements (“tight”), with respect to the entire sample of “loose” electron candidates. The loose candidates satisfy only a subset of the nominal electron identification criteria. However, this subset has to be stricter than the trigger requirements imposed on a single object. To avoid bias due to a real electron contribution from Wdecays or the DrellYan process, events are vetoed in the following cases: if the missing transverse momentum is larger than 25 GeV, if they contain two identified electrons satisfying strict criteria, or if they contain two electrons satisfying less strict criteria but with an invariant mass between 71 and 111 GeV. A weighted average of the fake rates obtained from the jet samples is then calculated. The values of the fake rates are around 10%. They are not strongly ETdependent, but are smaller at central pseudorapidities and increase to as high as 20% for 2.4<jηj<2.47. In addition to the fake rate, the probability r1(r2) that a real electron in the sample of loose electrons satisfies the nominal electron identification and leading (subleading) isolation requirements is used in evaluating this background. This probability is computed from MC simulation. Potential differences between data and simulated samples in lepton identification and isolation efficiencies are accounted for by applying scale factors to the simulation, which are generally close to unity. The values for r1and r2 are well above 90% for all ETand η. A system of equations is used to solve for the unknown true contribution to the background from events with one or more fake electrons. The relation between the number of true paired objects Nab, with Ea T>E b Tand a; b ∈fR; Fg, and the number of measured pairs in the triggered sample Nxy, with x; y ∈fT;Lg, can be written as 0 B B B @ NTT NTL NLT NLL 1 C C C A¼ 0 B B B @ r1r2r1f2f1r2f1f2 r1ð1−r2Þr1ð1−f2Þf1ð1−r2Þf1ð1−f2Þ ð1−r1Þr2ð1−r1Þf2ð1−f1Þr2ð1−f1Þf2 ð1−r1Þð1−r2Þð1−r1Þð1−f2Þð1−f1Þð1−r2Þð1−f1Þð1−f2Þ 1 C C C A 0 B B B @ NRR NRF NFR NFF 1 C C C A :ð1Þ The subscripts Rand Frefer to real electrons and fakes (jets), respectively. The subscript Trefers to electrons that pass the tight selection. The subscript Lcorresponds to electrons that pass the loose requirements described above but fail the tight requirements. The background is given as the part of NTT, the number of pairs where both objects are reconstructed as signal-like, originating from a pair of objects with at least one fake: NDijet&Wþjets TT ¼r1f2NRF þf1r2NFR þf1f2NFF:ð2Þ The true paired objects on the right-hand side of Eq. (2) can be expressed in terms of measurable quantities (NTT,NTL, NLT,NLL) by inverting the matrix in Eq. (1). The dijet background in the dimuon sample is evaluated from data by reversing the requirement that muons pass the track isolation requirement based on the variable ΣpTðΔR<0.3Þ=pT. The method is further described in Ref. [87]. The contribution of the dijet background in the dimuon channel is negligible, as is the background from cosmic rays. IX. SYSTEMATIC UNCERTAINTIES The treatment of systematic uncertainties in this analysis is simplified by the fact that the backgrounds are normalized to the data in the region of the Zpeak. This procedure makes the analysis insensitive to the uncertainty on the measurement of the integrated luminosity as well as other mass-independent systematic uncertainties. A mass-independent systematic error of 4% is assigned to the signal expectation due to the uncertainty on the Z=γcross section in the normalization region. This uncertainty is due to the PDF and αSuncertainties obtained from the 90% C.L. MSTW2008NNLO PDF error set, using the program VRAP [88] in order to calculate the NNLO Drell-Yan cross section in the normalization region. In addition, scale uncertainties are estimated by varying the renormalization and factorization scales simultaneously up and down by a factor of 2, also using VRAP. Mass-dependent systematic uncertainties include theoretical and experimental effects on the signal and background. These uncertainties are correlated across all mll bins in the search region. The mass-dependent theoretical uncertainties are applied to the Z=γbackground expectation only. In general, theoretical uncertainties are not applied to the signal. However, the mass dependence of the G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-8 PDF uncertainty due to acceptance variations was checked and found to be negligible. It is assumed that the experimental uncertainties are fully correlated between the signal and all types of background. In the statistical analysis, all systematic uncertainties estimated to have an impact <3% on the expected number of events for all values of mll are neglected, as they have negligible impact on the results of the search. The combined uncertainty on the Z=γbackground due to PDF (“PDF variation”) and αSis obtained from the 90% C.L. MSTW2008NNLO PDF error set, using VRAP in order to calculate the NNLO Drell-Yan cross section as a function of mll. The resulting uncertainties at dilepton masses of 2 and 3 TeV are given in Tables III and IV, respectively. An additional uncertainty is assigned to take into account potential differences between modern PDFs at the same αS¼0.117: MSTW2008NNLO, CT10NNLO, NNPDF2.3 [77], ABM11 [89], and HERAPDF1.5 [90].Of these, only the central values for ABM11 fall outside of the MSTW2008NNLO PDF’s uncertainty band. Thus, an envelope of the latter uncertainty and the ABM11 central value is formed with respect to the central value of the MSTW PDF. The 90% C.L. uncertainty from MSTW is subtracted in quadrature from this envelope, and the remaining part, which is only nonzero when the ABM11 central value is outside the MSTW2008NNLO PDF uncertainty, is quoted as “PDF choice.”Scale uncertainties are estimated by varying the renormalization and factorization scales simultaneously up and down by a factor of 2, also using VRAP. The resulting maximum variations are taken as uncertainties and are less than 3%. The uncertainty on the PI correction is taken as half the difference between the predictions obtained under the current and constituent quark mass schemes, as discussed in Sec. V. In addition, a systematic uncertainty is attributed to EW corrections for both channels, corresponding to the difference in the theoretical calculation between FEWZ and SANC. On the experimental side, a systematic effect common to both channels is due to an uncertainty of 0.65% on the beam energy [91]. The effect on the background cross section was evaluated for the dominant Z=γbackground only, and it can be as high as 5% at high dilepton masses. For the signals considered here, the effect of this uncertainty on A×ϵis negligible (<1%). In the dielectron channel, the systematic uncertainty is dominated by the determination of background contributions with jets faking electrons in the final state, mainly dijet and Wþjets processes. In order to derive this uncertainty, the method described above was altered by assuming r1¼r2¼1. This second “matrix method” leads to a simplification of the matrix in Eq. (1), but also necessitates the use of MC corrections for the identification and isolation inefficiencies of real electrons. Large corrections from MC simulation can be avoided in a third matrix method where objects in the background-enriched sample fail the requirement on the matching between track and cluster, instead of the full identification and isolation requirements. In addition to the standard background-enriched sample recorded using the jet triggers, two alternative backgroundenriched samples are obtained using a “tag and probe” technique on the jet-triggered sample and the sample triggered by electromagnetic objects. Here the choice of an electromagnetic-object trigger that is looser than a dedicated electron trigger (see Sec. IV) leads to an enlarged sample. The background-enriched sample of probes is obtained by selecting a jetlike tag and a probe with the same charge, among other requirements, in order to suppress real electron contamination. Finally, the default method and the two additional matrix methods are each used in conjunction with the default sample and the two different background-enriched samples, leading to nine different background estimates. In the mll search region, the maximum deviation of the eight alternative estimates TABLE III. Summary of systematic uncertainties on the expected numbers of events at a dilepton mass of mll ¼2TeV, where N / A indicates that the uncertainty is not applicable. Uncertainties <3% for all values of mee or mμμ are neglected in the respective statistical analysis. Dielectrons Dimuons Source (mll ¼2TeV) Signal Background Signal Background Normalization 4% N / A 4% N / A PDF variation N / A 11% N / A 12% PDF choice N / A 7% N / A 6% αs N / A 3% N / A 3% Electroweak correction N / A 2% N / A 3% Photon-induced correction N / A 3% N / A 3% Beam energy <1% 3% <1% 3% Resolution <3% <3% <3% 3% Dijet and Wþjets N / A 5% N / AN / A Total 4% 15% 4% 15% TABLE IV. Summary of systematic uncertainties on the expected numbers of events at a dilepton mass of mll ¼3TeV, where N / A indicates that the uncertainty is not applicable. Uncertainties <3% for all values of mee or mμμ are neglected in the respective statistical analysis. Dielectrons Dimuons Source (mll ¼3TeV) Signal Background Signal Background Normalization 4% N / A 4% N / A PDF variation N / A 30% N / A 17% PDF choice N / A 22% N / A 12% αs N / A 5% N / A 4% Electroweak correction N / A 4% N / A 3% Photon-induced correction N / A 6% N / A 4% Beam energy <1% 5% <1% 3% Resolution <3% <3% <3% 8% Dijet and Wþjets N / A 21% N / AN / A Total 4% 44% 4% 23% SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-9 equal to 0.1 is 2.68 TeV. Experimental limits are also set on minimal Z0models and on a minimal walking technicolor model with a composite Higgs boson. The limits set on the production threshold of quantum black holes are 3.65 TeV for the extra-dimensional model proposed by ArkaniHamed, Dimopoulos, and Dvali and 2.24 TeV for the Randall-Sundrum model. For all but those on quantum black hole production, the limits presented are the most stringent to date. ACKNOWLEDGMENTS We thank T. Hapola for implementing the minimal walking technicolor model using MADGRAPH to generate the signal and for his help with acceptance studies. The limits shown in Sec. XII were calculated using computing resources provided by the Argonne Leadership Computing Facility and the National Energy Research Scientific Computing Center. 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; BMWF 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, DNSRC, and Lundbeck Foundation, Denmark; EPLANET, ERC, and NSRF, European Union; IN2P3-CNRS, CEA-DSM/ IRFU, France; GNSF, Georgia; BMBF, DFG, HGF, MPG, and AvH Foundation, Germany; GSRT and NSRF, Greece; ISF, MINERVA, GIF, I-CORE, and Benoziyo Center, Israel; INFN, Italy; MEXT and JSPS, Japan; CNRST, Morocco; FOM and NWO, Netherlands; BRF and RCN, Norway; MNiSW and NCN, Poland; GRICES and FCT, Portugal; MNE/IFA, Romania; MES of Russia and ROSATOM, Russian Federation; JINR, MSTD, Serbia; MSSR, Slovakia; ARRS and MIZŠ, Slovenia; DST/NRF, South Africa; MINECO, Spain; SRC and Wallenberg Foundation, Sweden; SER, SNSF, and Cantons of Bern and Geneva, Switzerland; NSC, Taiwan; TAEK, Turkey; STFC, the Royal Society and Leverhulme Trust, United Kingdom; DOE and NSF, United States of America. The crucial computing support from all WLCG partners is acknowledged gratefully, in particular from CERN and the ATLAS Tier-1 facilities at TRIUMF (Canada), NDGF (Denmark, Norway, Sweden), CC-IN2P3 (France), KIT/ GridKA (Germany), INFN-CNAF (Italy), NL-T1 (Netherlands), PIC (Spain), ASGC (Taiwan), RAL (UK), and BNL (USA) and in the Tier-2 facilities worldwide. [1] ATLAS Collaboration, JINST 3, S08003 (2008). [2] D. London and J. L. Rosner, Phys. Rev. D 34, 1530 (1986). [3] P. Langacker, Rev. Mod. Phys. 81, 1199 (2009). [4] E. Salvioni, G. Villadoro, and F. Zwirner, J. High Energy Phys. 11 (2009) 068. [5] ATLAS Collaboration, Phys. Lett. B 716, 1 (2012). [6] CMS Collaboration, Phys. Lett. B 716, 30 (2012). [7] M. V. Chizhov, V. A. Bednyakov, and J. A. Budagov, Phys. At. Nucl. 71, 2096 (2008). [8] M. V. Chizhov and G. Dvali, Phys. Lett. B 703, 593 (2011). [9] M. V. Chizhov, Phys. Part. Nucl. Lett. 8, 512 (2011). [10] M. V. Chizhov, V. A. Bednyakov, and J. A. Budagov, Nuovo Cimento Soc. Ital. Fis. 33C, 343 (2010). [11] L. Randall and R. Sundrum, Phys. Rev. Lett. 83, 3370 (1999). [12] P. Meade and L. Randall, J. High Energy Phys. 05 (2008) 003. [13] F. Sannino and K. Tuominen, Phys. Rev. D 71, 051901 (2005). [14] D. D. Dietrich, F. Sannino, and K. Tuominen, Phys. Rev. D 72, 055001 (2005). [15] R. Foadi, M. T. Frandsen, T. A. Ryttov, and F. Sannino, Phys. Rev. D 76, 055005 (2007). [16] R. Foadi, M. T. Frandsen, and F. Sannino, Phys. Rev. D 87, 095001 (2013). [17] ATLAS Collaboration, J. High Energy Phys. 11 (2012) 138. [18] CMS Collaboration, Phys. Lett. B 720, 63 (2013). [19] V. M. Abazov et al. (D0 Collaboration), Phys. Lett. B 695, 88 (2011). [20] T. Aaltonen et al. (CDF Collaboration), Phys. Rev. Lett. 106, 121801 (2011). [21] G. Abbiendi et al. (The OPAL Collaboration), Eur. Phys. J. C33, 173 (2004). [22] J. Abdallah (DELPHI Collaboration), Eur. Phys. J. C 45, 589 (2006). [23] P.Achardetal. (L3Collaboration),Eur.Phys.J.C47,1(2006). [24] S. Schael et al. (ALEPH Collaboration), Eur. Phys. J. C 49, 411 (2007). [25] P. Langacker, arXiv:0911.4294. [26] M. Dittmar, A.-S. Nicollerat, and A. Djouadi, Phys. Lett. B 583, 111 (2004). [27] E. Accomando, A. Belyaev, L. Fedeli, S. F. King, and C. Shepherd-Themistocleous, Phys. Rev. D 83, 075012 (2011). [28] G. Senjanovic and R. N. Mohapatra, Phys. Rev. D 12, 1502 (1975). [29] R. N. Mohapatra and J. C. Pati, Phys. Rev. D 11, 566 (1975). [30] L. Basso, A. Belyaev, S. Moretti, and C. H. ShepherdThemistocleous, Phys. Rev. D 80, 055030 (2009). [31] H. Davoudiasl, J. L. Hewett, and T. G. Rizzo, Phys. Rev. Lett. 84, 2080 (2000). [32] D. Dimopoulos and G. Landsberg, Phys. Rev. Lett. 87, 161602 (2001). G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-16 [33] S. B. Giddings and S. Thomas, Phys. Rev. D 65, 056010 (2002). [34] D. M. Gingrich and K. Martell, Phys. Rev. D 78, 115009 (2008). [35] X. Calmet, W. Gong, and S. D. H. Hsu, Phys. Lett. B 668, 20 (2008). [36] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, Phys. Lett. B429, 263 (1998). [37] D. M. Gingrich, J. Phys. G 37, 105008 (2010). [38] ATLAS Collaboration, Phys. Lett. B 728, 562 (2014). [39] ATLAS Collaboration, Phys. Rev. Lett. 112, 091804 (2014). [40] CMS Collaboration, J. High Energy Phys. 07 (2013) 178. [41] D.-C. Dai, G. Starkman, D. Stojkovic, C. Issever, E. Rizvi, and J. Tseng, Phys. Rev. D 77, 076007 (2008). [42] ATLAS Collaboration, J. High Energy Phys. 01 (2013) 029. [43] J. R. Andersen, T. Hapola, and F. Sannino, Phys. Rev. D 85, 055017 (2012). [44] A. Belyaev, R. Foadi, M. T. Frandsen, M. Järvinen, F. Sannino, and A. Pukhov, Phys. Rev. D 79, 035006 (2009). [45] ATLAS Collaboration, Eur. Phys. J. C 72, 1849 (2012). [46] ATLAS Collaboration, Eur. Phys. J. C 74, 2941 (2014). [47] S. Alioli, P. Nason, C. Oleari, and E. Re, J. High Energy Phys. 06 (2010) 043. [48] H.-L. Lai, M. Guzzi, J. Huston, Z. Li, P. M. Nadolsky, J. Pumplin, and C.-P. Yuan, Phys. Rev. D 82, 074024 (2010). [49] T. Sjöstrand, S. Mrenna, and P. Z. Skands, Comput. Phys. Commun. 178, 852 (2008). [50] P. Golonka and Z. Wąs, Eur. Phys. J. C 45, 97 (2006). [51] ATLAS Collaboration, Eur. Phys. J. C 70, 823 (2010). [52] S. Agostinelli et al. (GEANT4 Collaboration), Nucl. Instrum. Methods Phys. Res., Sect. A 506, 250 (2003). [53] K. Melnikov and F. Petriello, Phys. Rev. D 74, 114017 (2006). [54] Y. Li and F. Petriello, Phys. Rev. D 86, 094034 (2012). [55] A. D. Martin, W. J. Stirling, R. S. Thorne, and G. Watt, Eur. Phys. J. C 63, 189 (2009). [56] A. D. Martin, R. G. Roberts, W. J. Stirling, and R. S. Thorne, Eur. Phys. J. C 39, 155 (2005). [57] D. Bardin, S. Bondarenko, P. Christova, L. Kalinovskaya, L. Rumyantsev, A. Sapronov, and W. von Schlippe, JETP Lett. 96, 285 (2012). [58] S. G. Bondarenko and A. A. Sapronov, Comput. Phys. Commun. 184, 2343 (2013). [59] J. Alwall, M. Herquet, F. Maltoni, O. Mattelaer, and T. Stelzer, J. High Energy Phys. 06 (2011) 128. [60] U. Baur, Phys. Rev. D 75, 013005 (2007). [61] G. Corcella, I. G. Knowles, G. Marchesini, S. Moretti, K. Odagiri, P. Richardson, M. H. Seymour, and B. R. Webber, J. High Energy Phys. 01 (2001) 010. [62] G. Corcella et al.,arXiv:hep-ph/0210213. [63] J. Pumplin, D. R. Stump, J. Huston, H.-L. Lai, P. Nadolsky, and W.-K. Tung, J. High Energy Phys. 07 (2002) 012. [64] J. M. Campbell and R. K. Ellis, Phys. Rev. D 60, 113006 (1999). [65] S. Frixione and B. R. Webber, J. High Energy Phys. 06 (2002) 029. [66] S. Frixione, P. Nason, and B. R. Webber, J. High Energy Phys. 08 (2003) 007. [67] S. Frixione, E. Laenen, P. Motylinski, C. White, and B. R. Webber, J. High Energy Phys. 07 (2008) 029. [68] M. Cacciari, M. Czakon, M. Mangano, A. Mitov, and P. Nason, Phys. Lett. B 710, 612 (2012). [69] P. Bärnreuther, M. Czakon, and A. Mitov, Phys. Rev. Lett. 109, 132001 (2012). [70] M. Czakon and A. Mitov, J. High Energy Phys. 12 (2012) 054. [71] M. Czakon and A. Mitov, J. High Energy Phys. 01 (2013) 080. [72] M. Czakon, P. Fiedler, and A. Mitov, Phys. Rev. Lett. 110, 252004 (2013). [73] M. Czakon and A. Mitov, arXiv:1112.5675. [74] M. Botje et al.,arXiv:1101.0538. [75] A. D. Martin, W. J. Stirling, R. S. Thorne, and G. Watt, Eur. Phys. J. C 64, 653 (2009). [76] J. Gao, M. Guzzi, J. Huston, H.-L. Lai, Z. Li, P. Nadolsky, J. Pumplin, D. Stump, and C.-P. Yuan, Phys. Rev. D 89, 033009 (2014). [77] R. Ball et al.,Nucl. Phys. B867, 244 (2013). [78] N. Kidonakis, Phys. Rev. D 82, 054018 (2010). [79] A. Belyaev, N. D. Christensen, and A. Pukhov, Comput. Phys. Commun. 184, 1729 (2013). [80] D. M. Gingrich, Comput. Phys. Commun. 181, 1917 (2010),http://qbh.hepforge.org/. [81] P. Mathews, V. Ravindran, K. Sridhar, and W. L. van Neerven, Nucl. Phys. B713, 333 (2005). [82] P. Mathews, V. Ravindran, and K. Sridhar, J. High Energy Phys. 10 (2005) 031. [83] M. C. Kumar, P. Mathews, and V. Ravindran, Eur. Phys. J. C 49, 599 (2007). [84] ATLAS Collaboration, Eur. Phys. J. C 72, 1909 (2012). [85] ATLAS Collaboration, arXiv:1404.4562. [86] ATLAS Collaboration, Report No. ATLAS-CONF-2013088, 2013, http://cds.cern.ch/record/1580207. [87] ATLAS Collaboration, Phys. Rev. Lett. 107, 272002 (2011). [88] C. Anastasiou, L. Dixon, K. Melnikov, and F. Petriello, Phys. Rev. D 69, 094008 (2004). [89] S. Alekhin, J. Blumlein, and S. Moch, Phys. Rev. D 86, 054009 (2012). [90] F. D. Aaron et al. (H1 and ZEUS Collaborations), J. High Energy Phys. 01 (2010) 109. [91] J. Wenninger, Report No. CERN-ATS-2013-040, 2013, http://cds.cern.ch/record/1546734. [92] ATLAS Collaboration, Phys. Lett. B 700, 163 (2011). [93] T. Aaltonen et al. (CDF Collaboration), Phys. Rev. Lett. 102, 091805 (2009). [94] A. Caldwell, D. Kollar, and K. Kröninger, Comput. Phys. Commun. 180, 2197 (2009). SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-17 G. Aad,84 B. Abbott,112 J. Abdallah,152 S. Abdel Khalek,116 O. Abdinov,11 R. Aben,106 B. Abi,113 M. Abolins,89 O. S. AbouZeid,159 H. Abramowicz,154 H. Abreu,153 R. Abreu,30 Y. Abulaiti,147a,147b B. S. Acharya,165a,165b,b L. Adamczyk,38a D. L. Adams,25 J. Adelman,177 S. Adomeit,99 T. Adye,130 T. Agatonovic-Jovin,13a J. A. Aguilar-Saavedra,125f,125a M. Agustoni,17 S. P. Ahlen,22 F. Ahmadov,64,c G. Aielli,134a,134b H. Akerstedt,147a,147b T. P. A. Åkesson,80 G. Akimoto,156 A. V. Akimov,95 G. L. Alberghi,20a,20b J. Albert,170 S. Albrand,55 M. J. Alconada Verzini,70 M. Aleksa,30 I. N. Aleksandrov,64 C. Alexa,26a G. Alexander,154 G. Alexandre,49 T. Alexopoulos,10 M. Alhroob,165a,165c G. Alimonti,90a L. Alio,84 J. Alison,31 B. M. M. Allbrooke,18 K. Allen,160a,d L. J. Allison,71 P. P. Allport,73 J. Almond,83 A. Aloisio,103a,103b A. Alonso,36 F. Alonso,70 C. Alpigiani,75 A. Altheimer,35 B. Alvarez Gonzalez,89 M. G. Alviggi,103a,103b K. Amako,65 Y. Amaral Coutinho,24a C. Amelung,23 D. Amidei,88 S. P. Amor Dos Santos,125a,125c A. Amorim,125a,125b S. Amoroso,48 N. Amram,154 G. Amundsen,23 C. Anastopoulos,140 L. S. Ancu,49 N. Andari,30 T. Andeen,35 C. F. Anders,58b G. Anders,30 K. J. Anderson,31 A. Andreazza,90a,90b V. Andrei,58a X. S. Anduaga,70 S. Angelidakis,9I. Angelozzi,106 P. Anger,44 A. Angerami,35 F. Anghinolfi,30 A. V. Anisenkov,108 N. Anjos,125a A. Annovi,47 A. Antonaki,9M. Antonelli,47 A. Antonov,97 J. Antos,145b F. Anulli,133a M. Aoki,65 L. Aperio Bella,18 R. Apolle,119,e G. Arabidze,89 I. Aracena,144 Y. Arai,65 J. P. Araque,125a A. T. H. Arce,45 J-F. Arguin,94 S. Argyropoulos,42 M. Arik,19a A. J. Armbruster,30 O. Arnaez,30 V. Arnal,81 H. Arnold,48 M. Arratia,28 O. Arslan,21 A. Artamonov,96 G. Artoni,23 S. Asai,156 N. Asbah,42 A. Ashkenazi,154 B. Åsman,147a,147b L. Asquith,6K. Assamagan,25 R. Astalos,145a M. Atkinson,166 N. B. Atlay,142 B. Auerbach,6K. Augsten,127 M. Aurousseau,146b G. Avolio,30 G. Azuelos,94,f Y. Azuma,156 M. A. Baak,30 C. Bacci,135a,135b H. Bachacou,137 K. Bachas,155 M. Backes,30 M. Backhaus,30 J. Backus Mayes,144 E. Badescu,26a P. Bagiacchi,133a,133b P. Bagnaia,133a,133b Y. Bai,33a T. Bain,35 J. T. Baines,130 O. K. Baker,177 S. Baker,77 P. Balek,128 F. Balli,137 E. Banas,39 Sw. Banerjee,174 A. A. E. Bannoura,176 V. Bansal,170 H. S. Bansil,18 L. Barak,173 S. P. Baranov,95 E. L. Barberio,87 D. Barberis,50a,50b M. Barbero,84 T. Barillari,100 M. Barisonzi,176 T. Barklow,144 N. Barlow,28 B. M. Barnett,130 R. M. Barnett,15 Z. Barnovska,5A. Baroncelli,135a G. Barone,49 A. J. Barr,119 F. Barreiro,81 J. Barreiro Guimarães da Costa,57 R. Bartoldus,144 A. E. Barton,71 P. Bartos,145a V. Bartsch,150 A. Bassalat,116 A. Basye,166 R. L. Bates,53 L. Batkova,145a J. R. Batley,28 M. Battaglia,138 M. Battistin,30 F. Bauer,137 H. S. Bawa,144,g T. Beau,79 P. H. Beauchemin,162 R. Beccherle,123a,123b P. Bechtle,21 H. P. Beck,17 K. Becker,176 S. Becker,99 M. Beckingham,139 C. Becot,116 A. J. Beddall,19c A. Beddall,19c S. Bedikian,177 V. A. Bednyakov,64 C. P. Bee,149 L. J. Beemster,106 T. A. Beermann,176 M. Begel,25 K. Behr,119 C. Belanger-Champagne,86 P. J. Bell,49 W. H. Bell,49 G. Bella,154 L. Bellagamba,20a A. Bellerive,29 M. Bellomo,85 K. Belotskiy,97 O. Beltramello,30 O. Benary,154 D. Benchekroun,136a K. Bendtz,147a,147b N. Benekos,166 Y. Benhammou,154 E. Benhar Noccioli,49 J. A. Benitez Garcia,160b D. P. Benjamin,45 J. R. Bensinger,23 K. Benslama,131 S. Bentvelsen,106 D. Berge,106 E. Bergeaas Kuutmann,16 N. Berger,5 F. Berghaus,170 E. Berglund,106 J. Beringer,15 C. Bernard,22 P. Bernat,77 C. Bernius,78 F. U. Bernlochner,170 T. Berry,76 P. Berta,128 C. Bertella,84 G. Bertoli,147a,147b F. Bertolucci,123a,123b D. Bertsche,112 M. I. Besana,90a G. J. Besjes,105 O. Bessidskaia,147a,147b M. F. Bessner,42 N. Besson,137 C. Betancourt,48 S. Bethke,100 W. Bhimji,46 R. M. Bianchi,124 L. Bianchini,23 M. Bianco,30 O. Biebel,99 S. P. Bieniek,77 K. Bierwagen,54 J. Biesiada,15 M. Biglietti,135a J. Bilbao De Mendizabal,49 H. Bilokon,47 M. Bindi,54 S. Binet,116 A. Bingul,19c C. Bini,133a,133b C. W. Black,151 J. E. Black,144 K. M. Black,22 D. Blackburn,139 R. E. Blair,6J.-B. Blanchard,137 T. Blazek,145a I. Bloch,42 C. Blocker,23 W. Blum,82,a U. Blumenschein,54 G. J. Bobbink,106 V. S. Bobrovnikov,108 S. S. Bocchetta,80 A. Bocci,45 C. Bock,99 C. R. Boddy,119 M. Boehler,48 J. Boek,176 T. T. Boek,176 J. A. Bogaerts,30 A. G. Bogdanchikov,108 A. Bogouch,91,a C. Bohm,147a J. Bohm,126 V. Boisvert,76 T. Bold,38a V. Boldea,26a A. S. Boldyrev,98 M. Bomben,79 M. Bona,75 M. Boonekamp,137 A. Borisov,129 G. Borissov,71 M. Borri,83 S. Borroni,42 J. Bortfeldt,99 V. Bortolotto,135a,135b K. Bos,106 D. Boscherini,20a M. Bosman,12 H. Boterenbrood,106 J. Boudreau,124 J. Bouffard,2E. V. Bouhova-Thacker,71 D. Boumediene,34 C. Bourdarios,116 N. Bousson,113 S. Boutouil,136d A. Boveia,31 J. Boyd,30 I. R. Boyko,64 I. Bozovic-Jelisavcic,13b J. Bracinik,18 A. Brandt,8G. Brandt,15 O. Brandt,58a U. Bratzler,157 B. Brau,85 J. E. Brau,115 H. M. Braun,176,a S. F. Brazzale,165a,165c B. Brelier,159 K. Brendlinger,121 A. J. Brennan,87 R. Brenner,167 S. Bressler,173 K. Bristow,146c T. M. Bristow,46 D. Britton,53 F. M. Brochu,28 I. Brock,21 R. Brock,89 C. Bromberg,89 J. Bronner,100 G. Brooijmans,35 T. Brooks,76 W. K. Brooks,32b J. Brosamer,15 E. Brost,115 G. Brown,83 J. Brown,55 P. A. Bruckman de Renstrom,39 D. Bruncko,145b R. Bruneliere,48 S. Brunet,60 A. Bruni,20a G. Bruni,20a M. Bruschi,20a L. Bryngemark,80 T. Buanes,14 Q. Buat,143 F. Bucci,49 P. Buchholz,142 R. M. Buckingham,119 A. G. Buckley,53 S. I. Buda,26a I. A. Budagov,64 F. Buehrer,48 L. Bugge,118 M. K. Bugge,118 O. Bulekov,97 A. C. Bundock,73 H. Burckhart,30 S. Burdin,73 G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-18 B. Burghgrave,107 S. Burke,130 I. Burmeister,43 E. Busato,34 D. Büscher,48 V. Büscher,82 P. Bussey,53 C. P. Buszello,167 B. Butler,57 J. M. Butler,22 A. I. Butt,3C. M. Buttar,53 J. M. Butterworth,77 P. Butti,106 W. Buttinger,28 A. Buzatu,53 M. Byszewski,10 S. Cabrera Urbán,168 D. Caforio,20a,20b O. Cakir,4a P. Calafiura,15 A. Calandri,137 G. Calderini,79 P. Calfayan,99 R. Calkins,107 L. P. Caloba,24a D. Calvet,34 S. Calvet,34 R. Camacho Toro,49 S. Camarda,42 D. Cameron,118 L. M. Caminada,15 R. Caminal Armadans,12 S. Campana,30 M. Campanelli,77 A. Campoverde,149 V. Canale,103a,103b A. Canepa,160a M. Cano Bret,75 J. Cantero,81 R. Cantrill,76 T. Cao,40 M. D. M. Capeans Garrido,30 I. Caprini,26a M. Caprini,26a M. Capua,37a,37b R. Caputo,82 R. Cardarelli,134a T. Carli,30 G. Carlino,103a L. Carminati,90a,90b S. Caron,105 E. Carquin,32a G. D. Carrillo-Montoya,146c J. R. Carter,28 J. Carvalho,125a,125c D. Casadei,77 M. P. Casado,12 M. Casolino,12 E. Castaneda-Miranda,146b A. Castelli,106 V. Castillo Gimenez,168 N. F. Castro,125a P. Catastini,57 A. Catinaccio,30 J. R. Catmore,118 A. Cattai,30 G. Cattani,134a,134b S. Caughron,89 V. Cavaliere,166 D. Cavalli,90a M. Cavalli-Sforza,12 V. Cavasinni,123a,123b F. Ceradini,135a,135b B. Cerio,45 K. Cerny,128 A. S. Cerqueira,24b A. Cerri,150 L. Cerrito,75 F. Cerutti,15 M. Cerv,30 A. Cervelli,17 S. A. Cetin,19b A. Chafaq,136a D. Chakraborty,107 I. Chalupkova,128 K. Chan,3P. Chang,166 B. Chapleau,86 J. D. Chapman,28 D. Charfeddine,116 D. G. Charlton,18 C. C. Chau,159 C. A. Chavez Barajas,150 S. Cheatham,86 A. Chegwidden,89 S. Chekanov,6S. V. Chekulaev,160a G. A. Chelkov,64 M. A. Chelstowska,88 C. Chen,63 H. Chen,25 K. Chen,149 L. Chen,33d,h S. Chen,33c X. Chen,146c Y. Chen,35 H. C. Cheng,88 Y. Cheng,31 A. Cheplakov,64 R. Cherkaoui El Moursli,136e V. Chernyatin,25,a E. Cheu,7L. Chevalier,137 V. Chiarella,47 G. Chiefari,103a,103b J. T. Childers,6 A. Chilingarov,71 G. Chiodini,72a A. S. Chisholm,18 R. T. Chislett,77 A. Chitan,26a M. V. Chizhov,64 S. Chouridou,9 B. K. B. Chow,99 D. Chromek-Burckhart,30 M. L. Chu,152 J. Chudoba,126 J. J. Chwastowski,39 L. Chytka,114 G. Ciapetti,133a,133b A. K. Ciftci,4a R. Ciftci,4a D. Cinca,62 V. Cindro,74 A. Ciocio,15 P. Cirkovic,13b Z. H. Citron,173 M. Citterio,90a M. Ciubancan,26a A. Clark,49 P. J. Clark,46 R. N. Clarke,15 W. Cleland,124 J. C. Clemens,84 C. Clement,147a,147b Y. Coadou,84 M. Cobal,165a,165c A. Coccaro,139 J. Cochran,63 L. Coffey,23 J. G. Cogan,144 J. Coggeshall,166 B. Cole,35 S. Cole,107 A. P. Colijn,106 J. Collot,55 T. Colombo,58c G. Colon,85 G. Compostella,100 P. Conde Muiño,125a,125b E. Coniavitis,167 M. C. Conidi,12 S. H. Connell,146b I. A. Connelly,76 S. M. Consonni,90a,90b V. Consorti,48 S. Constantinescu,26a C. Conta,120a,120b G. Conti,57 F. Conventi,103a,i M. Cooke,15 B. D. Cooper,77 A. M. Cooper-Sarkar,119 N. J. Cooper-Smith,76 K. Copic,15 T. Cornelissen,176 M. Corradi,20a F. Corriveau,86,j A. Corso-Radu,164 A. Cortes-Gonzalez,12 G. Cortiana,100 G. Costa,90a M. J. Costa,168 D. Costanzo,140 D. Côté,8G. Cottin,28 G. Cowan,76 B. E. Cox,83 K. Cranmer,109 G. Cree,29 S. Crépé-Renaudin,55 F. Crescioli,79 W. A. Cribbs,147a,147b M. Crispin Ortuzar,119 M. Cristinziani,21 V. Croft,105 G. Crosetti,37a,37b C.-M. Cuciuc,26a T. Cuhadar Donszelmann,140 J. Cummings,177 M. Curatolo,47 C. Cuthbert,151 H. Czirr,142 P. Czodrowski,3Z. Czyczula,177 S. D’Auria,53 M. D’Onofrio,73 M. J. Da Cunha Sargedas De Sousa,125a,125b C. Da Via,83 W. Dabrowski,38a A. Dafinca,119 T. Dai,88 O. Dale,14 F. Dallaire,94 C. Dallapiccola,85 M. Dam,36 A. C. Daniells,18 M. Dano Hoffmann,137 V. Dao,105 G. Darbo,50a S. Darmora,8 J. A. Dassoulas,42 A. Dattagupta,60 W. Davey,21 C. David,170 T. Davidek,128 E. Davies,119,e M. Davies,154 O. Davignon,79 A. R. Davison,77 P. Davison,77 Y. Davygora,58a E. Dawe,143 I. Dawson,140 R. K. Daya-Ishmukhametova,85 K. De,8 R. de Asmundis,103a S. De Castro,20a,20b S. De Cecco,79 N. De Groot,105 P. de Jong,106 H. De la Torre,81 F. De Lorenzi,63 L. De Nooij,106 D. De Pedis,133a A. De Salvo,133a U. De Sanctis,165a,165b A. De Santo,150 J. B. De Vivie De Regie,116 W. J. Dearnaley,71 R. Debbe,25 C. Debenedetti,46 B. Dechenaux,55 D. V. Dedovich,64 I. Deigaard,106 J. Del Peso,81 T. Del Prete,123a,123b F. Deliot,137 C. M. Delitzsch,49 M. Deliyergiyev,74 A. Dell’Acqua,30 L. Dell’Asta,22 M. Dell’Orso,123a,123b M. Della Pietra,103a,i D. della Volpe,49 M. Delmastro,5P. A. Delsart,55 C. Deluca,106 S. Demers,177 M. Demichev,64 A. Demilly,79 S. P. Denisov,129 D. Derendarz,39 J. E. Derkaoui,136d F. Derue,79 P. Dervan,73 K. Desch,21 C. Deterre,42 P. O. Deviveiros,106 A. Dewhurst,130 S. Dhaliwal,106 A. Di Ciaccio,134a,134b L. Di Ciaccio,5 A. Di Domenico,133a,133b C. Di Donato,103a,103b A. Di Girolamo,30 B. Di Girolamo,30 A. Di Mattia,153 B. Di Micco,135a,135b R. Di Nardo,47 A. Di Simone,48 R. Di Sipio,20a,20b D. Di Valentino,29 M. A. Diaz,32a E. B. Diehl,88 J. Dietrich,42 T. A. Dietzsch,58a S. Diglio,84 A. Dimitrievska,13a J. Dingfelder,21 C. Dionisi,133a,133b P. Dita,26a S. Dita,26a F. Dittus,30 F. Djama,84 T. Djobava,51b M. A. B. do Vale,24c A. Do Valle Wemans,125a,125g T. K. O. Doan,5D. Dobos,30 C. Doglioni,49 T. Doherty,53 T. Dohmae,156 J. Dolejsi,128 Z. Dolezal,128 B. A. Dolgoshein,97,a M. Donadelli,24d S. Donati,123a,123b P. Dondero,120a,120b J. Donini,34 J. Dopke,30 A. Doria,103a M. T. Dova,70 A. T. Doyle,53 M. Dris,10 J. Dubbert,88 S. Dube,15 E. Dubreuil,34 E. Duchovni,173 G. Duckeck,99 O. A. Ducu,26a D. Duda,176 A. Dudarev,30 F. Dudziak,63 L. Duflot,116 L. Duguid,76 M. Dührssen,30 M. Dunford,58a H. Duran Yildiz,4a M. Düren,52 A. Durglishvili,51b M. Dwuznik,38a M. Dyndal,38a J. Ebke,99 W. Edson,2N. C. Edwards,46 W. Ehrenfeld,21 T. Eifert,144 G. Eigen,14 K. Einsweiler,15 T. Ekelof,167 SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-19 M. El Kacimi,136c M. Ellert,167 S. Elles,5F. Ellinghaus,82 N. Ellis,30 J. Elmsheuser,99 M. Elsing,30 D. Emeliyanov,130 Y. Enari,156 O. C. Endner,82 M. Endo,117 R. Engelmann,149 J. Erdmann,177 A. Ereditato,17 D. Eriksson,147a G. Ernis,176 J. Ernst,2M. Ernst,25 J. Ernwein,137 D. Errede,166 S. Errede,166 E. Ertel,82 M. Escalier,116 H. Esch,43 C. Escobar,124 B. Esposito,47 A. I. Etienvre,137 E. Etzion,154 H. Evans,60 A. Ezhilov,122 L. Fabbri,20a,20b G. Facini,31 R. M. Fakhrutdinov,129 S. Falciano,133a R. J. Falla,77 J. Faltova,128 Y. Fang,33a M. Fanti,90a,90b A. Farbin,8A. Farilla,135a T. Farooque,12 S. Farrell,164 S. M. Farrington,171 P. Farthouat,30 F. Fassi,168 P. Fassnacht,30 D. Fassouliotis,9A. Favareto,50a,50b L. Fayard,116 P. Federic,145a O. L. Fedin,122,k W. Fedorko,169 M. Fehling-Kaschek,48 S. Feigl,30 L. Feligioni,84 C. Feng,33d E. J. Feng,6 H. Feng,88 A. B. Fenyuk,129 S. Fernandez Perez,30 S. Ferrag,53 J. Ferrando,53 A. Ferrari,167 P. Ferrari,106 R. Ferrari,120a D. E. Ferreira de Lima,53 A. Ferrer,168 D. Ferrere,49 C. Ferretti,88 A. Ferretto Parodi,50a,50b M. Fiascaris,31 F. Fiedler,82 A. Filipčič,74 M. Filipuzzi,42 F. Filthaut,105 M. Fincke-Keeler,170 K. D. Finelli,151 M. C. N. Fiolhais,125a,125c L. Fiorini,168 A. Firan,40 J. Fischer,176 W. C. Fisher,89 E. A. Fitzgerald,23 M. Flechl,48 I. Fleck,142 P. Fleischmann,88 S. Fleischmann,176 G. T. Fletcher,140 G. Fletcher,75 T. Flick,176 A. Floderus,80 L. R. Flores Castillo,174 A. C. Florez Bustos,160b M. J. Flowerdew,100 A. Formica,137 A. Forti,83 D. Fortin,160a D. Fournier,116 H. Fox,71 S. Fracchia,12 P. Francavilla,79 M. Franchini,20a,20b S. Franchino,30 D. Francis,30 M. Franklin,57 S. Franz,61 M. Fraternali,120a,120b S. T. French,28 C. Friedrich,42 F. Friedrich,44 D. Froidevaux,30 J. A. Frost,28 C. Fukunaga,157 E. Fullana Torregrosa,82 B. G. Fulsom,144 J. Fuster,168 C. Gabaldon,55 O. Gabizon,173 A. Gabrielli,20a,20b A. Gabrielli,133a,133b S. Gadatsch,106 S. Gadomski,49 G. Gagliardi,50a,50b P. Gagnon,60 C. Galea,105 B. Galhardo,125a,125c E. J. Gallas,119 V. Gallo,17 B. J. Gallop,130 P. Gallus,127 G. Galster,36 K. K. Gan,110 R. P. Gandrajula,62 J. Gao,33b,h Y. S. Gao,144,g F. M. Garay Walls,46 F. Garberson,177 C. García,168 J. E. García Navarro,168 M. Garcia-Sciveres,15 R. W. Gardner,31 N. Garelli,144 V. Garonne,30 C. Gatti,47 G. Gaudio,120a B. Gaur,142 L. Gauthier,94 P. Gauzzi,133a,133b I. L. Gavrilenko,95 C. Gay,169 G. Gaycken,21 E. N. Gazis,10 P. Ge,33d Z. Gecse,169 C. N. P. Gee,130 D. A. A. Geerts,106 Ch. Geich-Gimbel,21 K. Gellerstedt,147a,147b C. Gemme,50a A. Gemmell,53 M. H. Genest,55 S. Gentile,133a,133b M. George,54 S. George,76 D. Gerbaudo,164 A. Gershon,154 H. Ghazlane,136b N. Ghodbane,34 B. Giacobbe,20a S. Giagu,133a,133b V. Giangiobbe,12 P. Giannetti,123a,123b F. Gianotti,30 B. Gibbard,25 S. M. Gibson,76 M. Gilchriese,15 T. P. S. Gillam,28 D. Gillberg,30 G. Gilles,34 D. M. Gingrich,3,f N. Giokaris,9 M. P. Giordani,165a,165c R. Giordano,103a,103b F. M. Giorgi,20a F. M. Giorgi,16 P. F. Giraud,137 D. Giugni,90a C. Giuliani,48 M. Giulini,58b B. K. Gjelsten,118 S. Gkaitatzis,155 I. Gkialas,155,l L. K. Gladilin,98 C. Glasman,81 J. Glatzer,30 P. C. F. Glaysher,46 A. Glazov,42 G. L. Glonti,64 M. Goblirsch-Kolb,100 J. R. Goddard,75 J. Godfrey,143 J. Godlewski,30 C. Goeringer,82 S. Goldfarb,88 T. Golling,177 D. Golubkov,129 A. Gomes,125a,125b,125d L. S. Gomez Fajardo,42 R. Gonçalo,125a J. Goncalves Pinto Firmino Da Costa,137 L. Gonella,21 S. González de la Hoz,168 G. Gonzalez Parra,12 M. L. Gonzalez Silva,27 S. Gonzalez-Sevilla,49 L. Goossens,30 P. A. Gorbounov,96 H. A. Gordon,25 I. Gorelov,104 B. Gorini,30 E. Gorini,72a,72b A. Gorišek,74 E. Gornicki,39 A. T. Goshaw,6C. Gössling,43 M. I. Gostkin,64 M. Gouighri,136a D. Goujdami,136c M. P. Goulette,49 A. G. Goussiou,139 C. Goy,5S. Gozpinar,23 H. M. X. Grabas,137 L. Graber,54 I. Grabowska-Bold,38a P. Grafström,20a,20b K-J. Grahn,42 J. Gramling,49 E. Gramstad,118 S. Grancagnolo,16 V. Grassi,149 V. Gratchev,122 H. M. Gray,30 E. Graziani,135a O. G. Grebenyuk,122 Z. D. Greenwood,78,m K. Gregersen,77 I. M. Gregor,42 P. Grenier,144 J. Griffiths,8A. A. Grillo,138 K. Grimm,71 S. Grinstein,12,n Ph. Gris,34 Y. V. Grishkevich,98 J.-F. Grivaz,116 J. P. Grohs,44 A. Grohsjean,42 E. Gross,173 J. Grosse-Knetter,54 G. C. Grossi,134a,134b J. Groth-Jensen,173 Z. J. Grout,150 L. Guan,33b F. Guescini,49 D. Guest,177 O. Gueta,154 C. Guicheney,34 E. Guido,50a,50b T. Guillemin,116 S. Guindon,2U. Gul,53 C. Gumpert,44 J. Gunther,127 J. Guo,35 S. Gupta,119 P. Gutierrez,112 N. G. Gutierrez Ortiz,53 C. Gutschow,77 N. Guttman,154 C. Guyot,137 C. Gwenlan,119 C. B. Gwilliam,73 A. Haas,109 C. Haber,15 H. K. Hadavand,8N. Haddad,136e P. Haefner,21 S. Hageboeck,21 Z. Hajduk,39 H. Hakobyan,178 M. Haleem,42 D. Hall,119 G. Halladjian,89 K. Hamacher,176 P. Hamal,114 K. Hamano,170 M. Hamer,54 A. Hamilton,146a S. Hamilton,162 P. G. Hamnett,42 L. Han,33b K. Hanagaki,117 K. Hanawa,156 M. Hance,15 P. Hanke,58a R. Hanna,137 J. B. Hansen,36 J. D. Hansen,36 P. H. Hansen,36 K. Hara,161 A. S. Hard,174 T. Harenberg,176 S. Harkusha,91 D. Harper,88 R. D. Harrington,46 O. M. Harris,139 P. F. Harrison,171 F. Hartjes,106 S. Hasegawa,102 Y. Hasegawa,141 A. Hasib,112 S. Hassani,137 S. Haug,17 M. Hauschild,30 R. Hauser,89 M. Havranek,126 C. M. Hawkes,18 R. J. Hawkings,30 A. D. Hawkins,80 T. Hayashi,161 D. Hayden,89 C. P. Hays,119 H. S. Hayward,73 S. J. Haywood,130 S. J. Head,18 T. Heck,82 V. Hedberg,80 L. Heelan,8S. Heim,121 T. Heim,176 B. Heinemann,15 L. Heinrich,109 S. Heisterkamp,36 J. Hejbal,126 L. Helary,22 C. Heller,99 M. Heller,30 S. Hellman,147a,147b D. Hellmich,21 C. Helsens,30 J. Henderson,119 R. C. W. Henderson,71 C. Hengler,42 A. Henrichs,177 A. M. Henriques Correia,30 S. Henrot-Versille,116 C. Hensel,54 G. H. Herbert,16 Y. Hernández Jiménez,168 R. Herrberg-Schubert,16 G. Herten,48 G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-20 R. Hertenberger,99 L. Hervas,30 G. G. Hesketh,77 N. P. Hessey,106 R. Hickling,75 E. Higón-Rodriguez,168 E. Hill,170 J. C. Hill,28 K. H. Hiller,42 S. Hillert,21 S. J. Hillier,18 I. Hinchliffe,15 E. Hines,121 M. Hirose,158 D. Hirschbuehl,176 J. Hobbs,149 N. Hod,106 M. C. Hodgkinson,140 P. Hodgson,140 A. Hoecker,30 M. R. Hoeferkamp,104 J. Hoffman,40 D. Hoffmann,84 J. I. Hofmann,58a M. Hohlfeld,82 T. R. Holmes,15 T. M. Hong,121 L. Hooft van Huysduynen,109 J-Y. Hostachy,55 S. Hou,152 A. Hoummada,136a J. Howard,119 J. Howarth,42 M. Hrabovsky,114 I. Hristova,16 J. Hrivnac,116 T. Hryn’ova,5P. J. Hsu,82 S.-C. Hsu,139 D. Hu,35 X. Hu,25 Y. Huang,42 Z. Hubacek,30 F. Hubaut,84 F. Huegging,21 T. B. Huffman,119 E. W. Hughes,35 G. Hughes,71 M. Huhtinen,30 T. A. Hülsing,82 M. Hurwitz,15 N. Huseynov,64,c J. Huston,89 J. Huth,57 G. Iacobucci,49 G. Iakovidis,10 I. Ibragimov,142 L. Iconomidou-Fayard,116 E. Ideal,177 P. Iengo,103a O. Igonkina,106 T. Iizawa,172 Y. Ikegami,65 K. Ikematsu,142 M. Ikeno,65 Y. Ilchenko,31,bb D. Iliadis,155 N. Ilic,159 Y. Inamaru,66 T. Ince,100 P. Ioannou,9M. Iodice,135a K. Iordanidou,9V. Ippolito,57 A. Irles Quiles,168 C. Isaksson,167 M. Ishino,67 M. Ishitsuka,158 R. Ishmukhametov,110 C. Issever,119 S. Istin,19a J. M. Iturbe Ponce,83 R. Iuppa,134a,134b J. Ivarsson,80 W. Iwanski,39 H. Iwasaki,65 J. M. Izen,41 V. Izzo,103a B. Jackson,121 M. Jackson,73 P. Jackson,1M. R. Jaekel,30 V. Jain,2 K. Jakobs,48 S. Jakobsen,30 T. Jakoubek,126 J. Jakubek,127 D. O. Jamin,152 D. K. Jana,78 E. Jansen,77 H. Jansen,30 J. Janssen,21 M. Janus,171 G. Jarlskog,80 N. Javadov,64,c T. Javůrek,48 L. Jeanty,15 J. Jejelava,51a,o G. -Y. Jeng,151 D. Jennens,87 P. Jenni,48,p J. Jentzsch,43 C. Jeske,171 S. Jézéquel,5H. Ji,174 W. Ji,82 J. Jia,149 Y. Jiang,33b M. Jimenez Belenguer,42 S. Jin,33a A. Jinaru,26a O. Jinnouchi,158 M. D. Joergensen,36 K. E. Johansson,147a P. Johansson,140 K. A. Johns,7K. Jon-And,147a,147b G. Jones,171 R. W. L. Jones,71 T. J. Jones,73 J. Jongmanns,58a P. M. Jorge,125a,125b K. D. Joshi,83 J. Jovicevic,148 X. Ju,174 C. A. Jung,43 R. M. Jungst,30 P. Jussel,61 A. Juste Rozas,12,n M. Kaci,168 A. Kaczmarska,39 M. Kado,116 H. Kagan,110 M. Kagan,144 E. Kajomovitz,45 C. W. Kalderon,119 S. Kama,40 N. Kanaya,156 M. Kaneda,30 S. Kaneti,28 T. Kanno,158 V. A. Kantserov,97 J. Kanzaki,65 B. Kaplan,109 A. Kapliy,31 D. Kar,53 K. Karakostas,10 N. Karastathis,10 M. Karnevskiy,82 S. N. Karpov,64 K. Karthik,109 V. Kartvelishvili,71 A. N. Karyukhin,129 L. Kashif,174 G. Kasieczka,58b R. D. Kass,110 A. Kastanas,14 Y. Kataoka,156 A. Katre,49 J. Katzy,42 V. Kaushik,7K. Kawagoe,69 T. Kawamoto,156 G. Kawamura,54 S. Kazama,156 V. F. Kazanin,108 M. Y. Kazarinov,64 R. Keeler,170 R. Kehoe,40 M. Keil,54 J. S. Keller,42 J. J. Kempster,76 H. Keoshkerian,5O. Kepka,126 B. P. Kerševan,74 S. Kersten,176 K. Kessoku,156 J. Keung,159 F. Khalil-zada,11 H. Khandanyan,147a,147b A. Khanov,113 A. Khodinov,97 A. Khomich,58a T. J. Khoo,28 G. Khoriauli,21 A. Khoroshilov,176 V. Khovanskiy,96 E. Khramov,64 J. Khubua,51b H. Y. Kim,8H. Kim,147a,147b S. H. Kim,161 N. Kimura,172 O. Kind,16 B. T. King,73 M. King,168 R. S. B. King,119 S. B. King,169 J. Kirk,130 A. E. Kiryunin,100 T. Kishimoto,66 D. Kisielewska,38a F. Kiss,48 T. Kitamura,66 T. Kittelmann,124 K. Kiuchi,161 E. Kladiva,145b M. Klein,73 U. Klein,73 K. Kleinknecht,82 P. Klimek,147a,147b A. Klimentov,25 R. Klingenberg,43 J. A. Klinger,83 T. Klioutchnikova,30 P. F. Klok,105 E.-E. Kluge,58a P. Kluit,106 S. Kluth,100 E. Kneringer,61 E. B. F. G. Knoops,84 A. Knue,53 T. Kobayashi,156 M. Kobel,44 M. Kocian,144 P. Kodys,128 P. Koevesarki,21 T. Koffas,29 E. Koffeman,106 L. A. Kogan,119 S. Kohlmann,176 Z. Kohout,127 T. Kohriki,65 T. Koi,144 H. Kolanoski,16 I. Koletsou,5J. Koll,89 A. A. Komar,95,a Y. Komori,156 T. Kondo,65 N. Kondrashova,42 K. Köneke,48 A. C. König,105 S. König,82 T. Kono,65,q R. Konoplich,109,r N. Konstantinidis,77 R. Kopeliansky,153 S. Koperny,38a L. Köpke,82 A. K. Kopp,48 K. Korcyl,39 K. Kordas,155 A. Korn,77 A. A. Korol,108,s I. Korolkov,12 E. V. Korolkova,140 V. A. Korotkov,129 O. Kortner,100 S. Kortner,100 V. V. Kostyukhin,21 V. M. Kotov,64 A. Kotwal,45 C. Kourkoumelis,9V. Kouskoura,155 A. Koutsman,160a R. Kowalewski,170 T. Z. Kowalski,38a W. Kozanecki,137 A. S. Kozhin,129 V. Kral,127 V. A. Kramarenko,98 G. Kramberger,74 D. Krasnopevtsev,97 M. W. Krasny,79 A. Krasznahorkay,30 J. K. Kraus,21 A. Kravchenko,25 S. Kreiss,109 M. Kretz,58c J. Kretzschmar,73 K. Kreutzfeldt,52 P. Krieger,159 K. Kroeninger,54 H. Kroha,100 J. Kroll,121 J. Kroseberg,21 J. Krstic,13a U. Kruchonak,64 H. Krüger,21 T. Kruker,17 N. Krumnack,63 Z. V. Krumshteyn,64 A. Kruse,174 M. C. Kruse,45 M. Kruskal,22 T. Kubota,87 S. Kuday,4a S. Kuehn,48 A. Kugel,58c A. Kuhl,138 T. Kuhl,42 V. Kukhtin,64 Y. Kulchitsky,91 S. Kuleshov,32b M. Kuna,133a,133b J. Kunkle,121 A. Kupco,126 H. Kurashige,66 Y. A. Kurochkin,91 R. Kurumida,66 V. Kus,126 E. S. Kuwertz,148 M. Kuze,158 J. Kvita,114 A. La Rosa,49 L. La Rotonda,37a,37b C. Lacasta,168 F. Lacava,133a,133b J. Lacey,29 H. Lacker,16 D. Lacour,79 V. R. Lacuesta,168 E. Ladygin,64 R. Lafaye,5B. Laforge,79 T. Lagouri,177 S. Lai,48 H. Laier,58a L. Lambourne,77 S. Lammers,60 C. L. Lampen,7 W. Lampl,7E. Lançon,137 U. Landgraf,48 M. P. J. Landon,75 V. S. Lang,58a C. Lange,42 A. J. Lankford,164 F. Lanni,25 K. Lantzsch,30 S. Laplace,79 C. Lapoire,21 J. F. Laporte,137 T. Lari,90a M. Lassnig,30 P. Laurelli,47 W. Lavrijsen,15 A. T. Law,138 P. Laycock,73 B. T. Le,55 O. Le Dortz,79 E. Le Guirriec,84 E. Le Menedeu,12 T. LeCompte,6 F. Ledroit-Guillon,55 C. A. Lee,152 H. Lee,106 J. S. H. Lee,117 S. C. Lee,152 L. Lee,177 G. Lefebvre,79 M. Lefebvre,170 F. Legger,99 C. Leggett,15 A. Lehan,73 M. Lehmacher,21 G. Lehmann Miotto,30 X. Lei,7W. A. Leight,29 A. Leisos,155 SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-21 A. G. Leister,177 M. A. L. Leite,24d R. Leitner,128 D. Lellouch,173 B. Lemmer,54 K. J. C. Leney,77 T. Lenz,106 G. Lenzen,176 B. Lenzi,30 R. Leone,7K. Leonhardt,44 S. Leontsinis,10 C. Leroy,94 C. G. Lester,28 C. M. Lester,121 M. Levchenko,122 J. Levêque,5D. Levin,88 L. J. Levinson,173 M. Levy,18 A. Lewis,119 G. H. Lewis,109 A. M. Leyko,21 M. Leyton,41 B. Li,33b,t B. Li,84 H. Li,149 H. L. Li,31 L. Li,45 L. Li,33e S. Li,45 Y. Li,33c,u Z. Liang,138 H. Liao,34 B. Liberti,134a P. Lichard,30 K. Lie,166 J. Liebal,21 W. Liebig,14 C. Limbach,21 A. Limosani,87 S. C. Lin,152,v F. Linde,106 B. E. Lindquist,149 J. T. Linnemann,89 E. Lipeles,121 A. Lipniacka,14 M. Lisovyi,42 T. M. Liss,166 D. Lissauer,25 A. Lister,169 A. M. Litke,138 B. Liu,152 D. Liu,152 J. B. Liu,33b K. Liu,33b,w L. Liu,88 M. Liu,45 M. Liu,33b Y. Liu,33b M. Livan,120a,120b S. S. A. Livermore,119 A. Lleres,55 J. Llorente Merino,81 S. L. Lloyd,75 F. Lo Sterzo,152 E. Lobodzinska,42 P. Loch,7W. S. Lockman,138 T. Loddenkoetter,21 F. K. Loebinger,83 A. E. Loevschall-Jensen,36 A. Loginov,177 C. W. Loh,169 T. Lohse,16 K. Lohwasser,42 M. Lokajicek,126 V. P. Lombardo,5B. A. Long,22 J. D. Long,88 R. E. Long,71 L. Lopes,125a D. Lopez Mateos,57 B. Lopez Paredes,140 I. Lopez Paz,12 J. Lorenz,99 N. Lorenzo Martinez,60 M. Losada,163 P. Loscutoff,15 X. Lou,41 A. Lounis,116 J. Love,6 P. A. Love,71 A. J. Lowe,144,g F. Lu,33a H. J. Lubatti,139 C. Luci,133a,133b A. Lucotte,55 F. Luehring,60 W. Lukas,61 L. Luminari,133a O. Lundberg,147a,147b B. Lund-Jensen,148 M. Lungwitz,82 D. Lynn,25 R. Lysak,126 E. Lytken,80 H. Ma,25 L. L. Ma,33d G. Maccarrone,47 A. Macchiolo,100 J. Machado Miguens,125a,125b D. Macina,30 D. Madaffari,84 R. Madar,48 H. J. Maddocks,71 W. F. Mader,44 A. Madsen,167 M. Maeno,8T. Maeno,25 E. Magradze,54 K. Mahboubi,48 J. Mahlstedt,106 S. Mahmoud,73 C. Maiani,137 C. Maidantchik,24a A. Maio,125a,125b,125d S. Majewski,115 Y. Makida,65 N. Makovec,116 P. Mal,137,x B. Malaescu,79 Pa. Malecki,39 V. P. Maleev,122 F. Malek,55 U. Mallik,62 D. Malon,6C. Malone,144 S. Maltezos,10 V. M. Malyshev,108 S. Malyukov,30 J. Mamuzic,13b B. Mandelli,30 L. Mandelli,90a I. Mandić,74 R. Mandrysch,62 J. Maneira,125a,125b A. Manfredini,100 L. Manhaes de Andrade Filho,24b J. A. Manjarres Ramos,160b A. Mann,99 P. M. Manning,138 A. Manousakis-Katsikakis,9B. Mansoulie,137 R. Mantifel,86 L. Mapelli,30 L. March,168 J. F. Marchand,29 G. Marchiori,79 M. Marcisovsky,126 C. P. Marino,170 M. Marjanovic,13a C. N. Marques,125a F. Marroquim,24a S. P. Marsden,83 Z. Marshall,15 L. F. Marti,17 S. Marti-Garcia,168 B. Martin,30 B. Martin,89 T. A. Martin,171 V. J. Martin,46 B. Martin dit Latour,14 H. Martinez,137 M. Martinez,12,n S. Martin-Haugh,130 A. C. Martyniuk,77 M. Marx,139 F. Marzano,133a A. Marzin,30 L. Masetti,82 T. Mashimo,156 R. Mashinistov,95 J. Masik,83 A. L. Maslennikov,108 I. Massa,20a,20b N. Massol,5 P. Mastrandrea,149 A. Mastroberardino,37a,37b T. Masubuchi,156 T. Matsushita,66 P. Mättig,176 S. Mättig,42 J. Mattmann,82 J. Maurer,26a S. J. Maxfield,73 D. A. Maximov,108,s R. Mazini,152 L. Mazzaferro,134a,134b G. Mc Goldrick,159 S. P. Mc Kee,88 A. McCarn,88 R. L. McCarthy,149 T. G. McCarthy,29 N. A. McCubbin,130 K. W. McFarlane,56,a J. A. Mcfayden,77 G. Mchedlidze,54 S. J. McMahon,130 R. A. McPherson,170,j A. Meade,85 J. Mechnich,106 M. Medinnis,42 S. Meehan,31 S. Mehlhase,36 A. Mehta,73 K. Meier,58a C. Meineck,99 B. Meirose,80 C. Melachrinos,31 B. R. Mellado Garcia,146c F. Meloni,90a,90b A. Mengarelli,20a,20b S. Menke,100 E. Meoni,162 K. M. Mercurio,57 S. Mergelmeyer,21 N. Meric,137 P. Mermod,49 L. Merola,103a,103b C. Meroni,90a F. S. Merritt,31 H. Merritt,110 A. Messina,30,y J. Metcalfe,25 A. S. Mete,164 C. Meyer,82 C. Meyer,31 J-P. Meyer,137 J. Meyer,30 R. P. Middleton,130 S. Migas,73 L. Mijović,21 G. Mikenberg,173 M. Mikestikova,126 M. Mikuž,74 D. W. Miller,31 C. Mills,46 A. Milov,173 D. A. Milstead,147a,147b D. Milstein,173 A. A. Minaenko,129 I. A. Minashvili,64 A. I. Mincer,109 B. Mindur,38a M. Mineev,64 Y. Ming,174 L. M. Mir,12 G. Mirabelli,133a T. Mitani,172 J. Mitrevski,99 V. A. Mitsou,168 S. Mitsui,65 A. Miucci,49 P. S. Miyagawa,140 J. U. Mjörnmark,80 T. Moa,147a,147b K. Mochizuki,84 V. Moeller,28 S. Mohapatra,35 W. Mohr,48 S. Molander,147a,147b R. Moles-Valls,168 K. Mönig,42 C. Monini,55 J. Monk,36 E. Monnier,84 J. Montejo Berlingen,12 F. Monticelli,70 S. Monzani,133a,133b R. W. Moore,3A. Moraes,53 N. Morange,62 D. Moreno,82 M. Moreno Llácer,54 P. Morettini,50a M. Morgenstern,44 M. Morii,57 S. Moritz,82 A. K. Morley,148 G. Mornacchi,30 J. D. Morris,75 L. Morvaj,102 H. G. Moser,100 M. Mosidze,51b J. Moss,110 R. Mount,144 E. Mountricha,25 S. V. Mouraviev,95,a E. J. W. Moyse,85 S. Muanza,84 R. D. Mudd,18 F. Mueller,58a J. Mueller,124 K. Mueller,21 T. Mueller,28 T. Mueller,82 D. Muenstermann,49 Y. Munwes,154 J. A. Murillo Quijada,18 W. J. Murray,171,130 H. Musheghyan,54 E. Musto,153 A. G. Myagkov,129,z M. Myska,127 O. Nackenhorst,54 J. Nadal,54 K. Nagai,61 R. Nagai,158 Y. Nagai,84 K. Nagano,65 A. Nagarkar,110 Y. Nagasaka,59 M. Nagel,100 A. M. Nairz,30 Y. Nakahama,30 K. Nakamura,65 T. Nakamura,156 I. Nakano,111 H. Namasivayam,41 G. Nanava,21 R. Narayan,58b T. Nattermann,21 T. Naumann,42 G. Navarro,163 R. Nayyar,7H. A. Neal,88 P. Yu. Nechaeva,95 T. J. Neep,83 A. Negri,120a,120b G. Negri,30 M. Negrini,20a S. Nektarijevic,49 A. Nelson,164 T. K. Nelson,144 S. Nemecek,126 P. Nemethy,109 A. A. Nepomuceno,24a M. Nessi,30,aa M. S. Neubauer,166 M. Neumann,176 R. M. Neves,109 P. Nevski,25 P. R. Newman,18 D. H. Nguyen,6R. B. Nickerson,119 R. Nicolaidou,137 B. Nicquevert,30 J. Nielsen,138 N. Nikiforou,35 A. Nikiforov,16 V. Nikolaenko,129,z I. Nikolic-Audit,79 K. Nikolics,49 K. Nikolopoulos,18 P. Nilsson,8Y. Ninomiya,156 A. Nisati,133a R. Nisius,100 T. Nobe,158 L. Nodulman,6 G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-22 M. Nomachi,117 I. Nomidis,155 S. Norberg,112 M. Nordberg,30 S. Nowak,100 M. Nozaki,65 L. Nozka,114 K. Ntekas,10 G. Nunes Hanninger,87 T. Nunnemann,99 E. Nurse,77 F. Nuti,87 B. J. O’Brien,46 F. O’grady,7D. C. O’Neil,143 V. O’Shea,53 F. G. Oakham,29,f H. Oberlack,100 T. Obermann,21 J. Ocariz,79 A. Ochi,66 M. I. Ochoa,77 S. Oda,69 S. Odaka,65 H. Ogren,60 A. Oh,83 S. H. Oh,45 C. C. Ohm,30 H. Ohman,167 T. Ohshima,102 W. Okamura,117 H. Okawa,25 Y. Okumura,31 T. Okuyama,156 A. Olariu,26a A. G. Olchevski,64 S. A. Olivares Pino,46 D. Oliveira Damazio,25 E. Oliver Garcia,168 A. Olszewski,39 J. Olszowska,39 A. Onofre,125a,125e P. U. E. Onyisi,31,bb C. J. Oram,160a M. J. Oreglia,31 Y. Oren,154 D. Orestano,135a,135b N. Orlando,72a,72b C. Oropeza Barrera,53 R. S. Orr,159 B. Osculati,50a,50b R. Ospanov,121 G. Otero y Garzon,27 H. Otono,69 M. Ouchrif,136d E. A. Ouellette,170 F. Ould-Saada,118 A. Ouraou,137 K. P. Oussoren,106 Q. Ouyang,33a A. Ovcharova,15 M. Owen,83 V. E. Ozcan,19a N. Ozturk,8K. Pachal,119 A. Pacheco Pages,12 C. Padilla Aranda,12 M. Pagáčová,48 S. Pagan Griso,15 E. Paganis,140 C. Pahl,100 F. Paige,25 P. Pais,85 K. Pajchel,118 G. Palacino,160b S. Palestini,30 M. Palka,38b D. Pallin,34 A. Palma,125a,125b J. D. Palmer,18 Y. B. Pan,174 E. Panagiotopoulou,10 J. G. Panduro Vazquez,76 P. Pani,106 N. Panikashvili,88 S. Panitkin,25 D. Pantea,26a L. Paolozzi,134a,134b Th. D. Papadopoulou,10 K. Papageorgiou,155,l A. Paramonov,6D. Paredes Hernandez,34 M. A. Parker,28 F. Parodi,50a,50b J. A. Parsons,35 U. Parzefall,48 E. Pasqualucci,133a S. Passaggio,50a A. Passeri,135a F. Pastore,135a,135b,a Fr. Pastore,76 G. Pásztor,29 S. Pataraia,176 N. D. Patel,151 J. R. Pater,83 S. Patricelli,103a,103b T. Pauly,30 J. Pearce,170 M. Pedersen,118 S. Pedraza Lopez,168 R. Pedro,125a,125b S. V. Peleganchuk,108 D. Pelikan,167 H. Peng,33b B. Penning,31 J. Penwell,60 D. V. Perepelitsa,25 E. Perez Codina,160a M. T. Pérez García-Estañ,168 V. Perez Reale,35 L. Perini,90a,90b H. Pernegger,30 R. Perrino,72a R. Peschke,42 V. D. Peshekhonov,64 K. Peters,30 R. F. Y. Peters,83 B. A. Petersen,87 T. C. Petersen,36 E. Petit,42 A. Petridis,147a,147b C. Petridou,155 E. Petrolo,133a F. Petrucci,135a,135b M. Petteni,143 N. E. Pettersson,158 R. Pezoa,32b P. W. Phillips,130 G. Piacquadio,144 E. Pianori,171 A. Picazio,49 E. Piccaro,75 M. Piccinini,20a,20b R. Piegaia,27 D. T. Pignotti,110 J. E. Pilcher,31 A. D. Pilkington,77 J. Pina,125a,125b,125d M. Pinamonti,165a,165c,cc A. Pinder,119 J. L. Pinfold,3 A. Pingel,36 B. Pinto,125a S. Pires,79 M. Pitt,173 C. Pizio,90a,90b L. Plazak,145a M. -A. Pleier,25 V. Pleskot,128 E. Plotnikova,64 P. Plucinski,147a,147b S. Poddar,58a F. Podlyski,34 R. Poettgen,82 L. Poggioli,116 D. Pohl,21 M. Pohl,49 G. Polesello,120a A. Policicchio,37a,37b R. Polifka,159 A. Polini,20a C. S. Pollard,45 V. Polychronakos,25 K. Pommès,30 L. Pontecorvo,133a B. G. Pope,89 G. A. Popeneciu,26b D. S. Popovic,13a A. Poppleton,30 X. Portell Bueso,12 G. E. Pospelov,100 S. Pospisil,127 K. Potamianos,15 I. N. Potrap,64 C. J. Potter,150 C. T. Potter,115 G. Poulard,30 J. Poveda,60 V. Pozdnyakov,64 P. Pralavorio,84 A. Pranko,15 S. Prasad,30 R. Pravahan,8S. Prell,63 D. Price,83 J. Price,73 L. E. Price,6D. Prieur,124 M. Primavera,72a M. Proissl,46 K. Prokofiev,47 F. Prokoshin,32b E. Protopapadaki,137 S. Protopopescu,25 J. Proudfoot,6M. Przybycien,38a H. Przysiezniak,5E. Ptacek,115 E. Pueschel,85 D. Puldon,149 M. Purohit,25,dd P. Puzo,116 J. Qian,88 G. Qin,53 Y. Qin,83 A. Quadt,54 D. R. Quarrie,15 W. B. Quayle,165a,165b M. Queitsch-Maitland,83 D. Quilty,53 A. Qureshi,160b V. Radeka,25 V. Radescu,42 S. K. Radhakrishnan,149 P. Radloff,115 P. Rados,87 F. Ragusa,90a,90b G. Rahal,179 S. Rajagopalan,25 M. Rammensee,30 A. S. Randle-Conde,40 C. Rangel-Smith,167 K. Rao,164 F. Rauscher,99 S. Rave,82 T. C. Rave,48 T. Ravenscroft,53 M. Raymond,30 A. L. Read,118 N. P. Readioff,73 D. M. Rebuzzi,120a,120b A. Redelbach,175 G. Redlinger,25 R. Reece,138 K. Reeves,41 L. Rehnisch,16 H. Reisin,27 M. Relich,164 C. Rembser,30 H. Ren,33a Z. L. Ren,152 A. Renaud,116 M. Rescigno,133a S. Resconi,90a O. L. Rezanova,108,s P. Reznicek,128 R. Rezvani,94 R. Richter,100 M. Ridel,79 P. Rieck,16 J. Rieger,54 M. Rijssenbeek,149 A. Rimoldi,120a,120b L. Rinaldi,20a E. Ritsch,61 I. Riu,12 F. Rizatdinova,113 E. Rizvi,75 S. H. Robertson,86,j A. Robichaud-Veronneau,86 D. Robinson,28 J. E. M. Robinson,83 A. Robson,53 C. Roda,123a,123b L. Rodrigues,30 S. Roe,30 O. Røhne,118 S. Rolli,162 A. Romaniouk,97 M. Romano,20a,20b G. Romeo,27 E. Romero Adam,168 N. Rompotis,139 L. Roos,79 E. Ros,168 S. Rosati,133a K. Rosbach,49 M. Rose,76 P. L. Rosendahl,14 O. Rosenthal,142 V. Rossetti,147a,147b E. Rossi,103a,103b L. P. Rossi,50a R. Rosten,139 M. Rotaru,26a I. Roth,173 J. Rothberg,139 D. Rousseau,116 C. R. Royon,137 A. Rozanov,84 Y. Rozen,153 X. Ruan,146c F. Rubbo,12 I. Rubinskiy,42 V. I. Rud,98 C. Rudolph,44 M. S. Rudolph,159 F. Rühr,48 A. Ruiz-Martinez,30 Z. Rurikova,48 N. A. Rusakovich,64 A. Ruschke,99 J. P. Rutherfoord,7 N. Ruthmann,48 Y. F. Ryabov,122 M. Rybar,128 G. Rybkin,116 N. C. Ryder,119 A. F. Saavedra,151 S. Sacerdoti,27 A. Saddique,3 I. Sadeh,154 H. F-W. Sadrozinski,138 R. Sadykov,64 F. Safai Tehrani,133a H. Sakamoto,156 Y. Sakurai,172 G. Salamanna,75 A. Salamon,134a M. Saleem,112 D. Salek,106 P. H. Sales De Bruin,139 D. Salihagic,100 A. Salnikov,144 J. Salt,168 B. M. Salvachua Ferrando,6D. Salvatore,37a,37b F. Salvatore,150 A. Salvucci,105 A. Salzburger,30 D. Sampsonidis,155 A. Sanchez,103a,103b J. Sánchez,168 V. Sanchez Martinez,168 H. Sandaker,14 R. L. Sandbach,75 H. G. Sander,82 M. P. Sanders,99 M. Sandhoff,176 T. Sandoval,28 C. Sandoval,163 R. Sandstroem,100 D. P. C. Sankey,130 F. Sannino,ee A. Sansoni,47 C. Santoni,34 R. Santonico,134a,134b H. Santos,125a I. Santoyo Castillo,150 K. Sapp,124 A. Sapronov,64 SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-23 J. G. Saraiva,125a,125d B. Sarrazin,21 G. Sartisohn,176 O. Sasaki,65 Y. Sasaki,156 G. Sauvage,5,a E. Sauvan,5P. Savard,159,f D. O. Savu,30 C. Sawyer,119 L. Sawyer,78,m D. H. Saxon,53 J. Saxon,121 C. Sbarra,20a A. Sbrizzi,3T. Scanlon,77 D. A. Scannicchio,164 M. Scarcella,151 J. Schaarschmidt,173 P. Schacht,100 D. Schaefer,121 R. Schaefer,42 S. Schaepe,21 S. Schaetzel,58b U. Schäfer,82 A. C. Schaffer,116 D. Schaile,99 R. D. Schamberger,149 V. Scharf,58a V. A. Schegelsky,122 D. Scheirich,128 M. Schernau,164 M. I. Scherzer,35 C. Schiavi,50a,50b J. Schieck,99 C. Schillo,48 M. Schioppa,37a,37b S. Schlenker,30 E. Schmidt,48 K. Schmieden,30 C. Schmitt,82 C. Schmitt,99 S. Schmitt,58b B. Schneider,17 Y. J. Schnellbach,73 U. Schnoor,44 L. Schoeffel,137 A. Schoening,58b B. D. Schoenrock,89 A. L. S. Schorlemmer,54 M. Schott,82 D. Schouten,160a J. Schovancova,25 S. Schramm,159 M. Schreyer,175 C. Schroeder,82 N. Schuh,82 M. J. Schultens,21 H.-C. Schultz-Coulon,58a H. Schulz,16 M. Schumacher,48 B. A. Schumm,138 Ph. Schune,137 C. Schwanenberger,83 A. Schwartzman,144 Ph. Schwegler,100 Ph. Schwemling,137 R. Schwienhorst,89 J. Schwindling,137 T. Schwindt,21 M. Schwoerer,5F. G. Sciacca,17 E. Scifo,116 G. Sciolla,23 W. G. Scott,130 F. Scuri,123a,123b F. Scutti,21 J. Searcy,88 G. Sedov,42 E. Sedykh,122 S. C. Seidel,104 A. Seiden,138 F. Seifert,127 J. M. Seixas,24a G. Sekhniaidze,103a S. J. Sekula,40 K. E. Selbach,46 D. M. Seliverstov,122,a G. Sellers,73 N. Semprini-Cesari,20a,20b C. Serfon,30 L. Serin,116 L. Serkin,54 T. Serre,84 R. Seuster,160a H. Severini,112 F. Sforza,100 A. Sfyrla,30 E. Shabalina,54 M. Shamim,115 L. Y. Shan,33a R. Shang,166 J. T. Shank,22 Q. T. Shao,87 M. Shapiro,15 P. B. Shatalov,96 K. Shaw,165a,165b P. Sherwood,77 L. Shi,152,ff S. Shimizu,66 C. O. Shimmin,164 M. Shimojima,101 M. Shiyakova,64 A. Shmeleva,95 M. J. Shochet,31 D. Short,119 S. Shrestha,63 E. Shulga,97 M. A. Shupe,7 S. Shushkevich,42 P. Sicho,126 O. Sidiropoulou,155 D. Sidorov,113 A. Sidoti,133a F. Siegert,44 Dj. Sijacki,13a J. Silva,125a,125d Y. Silver,154 D. Silverstein,144 S. B. Silverstein,147a V. Simak,127 O. Simard,5Lj. Simic,13a S. Simion,116 E. Simioni,82 B. Simmons,77 R. Simoniello,90a,90b M. Simonyan,36 P. Sinervo,159 N. B. Sinev,115 V. Sipica,142 G. Siragusa,175 A. Sircar,78 A. N. Sisakyan,64,a S. Yu. Sivoklokov,98 J. Sjölin,147a,147b T. B. Sjursen,14 H. P. Skottowe,57 K. Yu. Skovpen,108 P. Skubic,112 M. Slater,18 T. Slavicek,127 K. Sliwa,162 V. Smakhtin,173 B. H. Smart,46 L. Smestad,14 S. Yu. Smirnov,97 Y. Smirnov,97 L. N. Smirnova,98,gg O. Smirnova,80 K. M. Smith,53 M. Smizanska,71 K. Smolek,127 A. A. Snesarev,95 G. Snidero,75 S. Snyder,25 R. Sobie,170,j F. Socher,44 A. Soffer,154 D. A. Soh,152,ff C. A. Solans,30 M. Solar,127 J. Solc,127 E. Yu. Soldatov,97 U. Soldevila,168 E. Solfaroli Camillocci,133a,133b A. A. Solodkov,129 A. Soloshenko,64 O. V. Solovyanov,129 V. Solovyev,122 P. Sommer,48 H. Y. Song,33b N. Soni,1A. Sood,15 A. Sopczak,127 V. Sopko,127 B. Sopko,127 V. Sorin,12 M. Sosebee,8 R. Soualah,165a,165c P. Soueid,94 A. M. Soukharev,108 D. South,42 S. Spagnolo,72a,72b F. Spanò,76 W. R. Spearman,57 R. Spighi,20a G. Spigo,30 M. Spousta,128 T. Spreitzer,159 B. Spurlock,8R. D. St. Denis,53,a S. Staerz,44 J. Stahlman,121 R. Stamen,58a E. Stanecka,39 R. W. Stanek,6C. Stanescu,135a M. Stanescu-Bellu,42 M. M. Stanitzki,42 S. Stapnes,118 E. A. Starchenko,129 J. Stark,55 P. Staroba,126 P. Starovoitov,42 R. Staszewski,39 P. Stavina,145a,a P. Steinberg,25 B. Stelzer,143 H. J. Stelzer,30 O. Stelzer-Chilton,160a H. Stenzel,52 S. Stern,100 G. A. Stewart,53 J. A. Stillings,21 M. C. Stockton,86 M. Stoebe,86 G. Stoicea,26a P. Stolte,54 S. Stonjek,100 A. R. Stradling,8A. Straessner,44 M. E. Stramaglia,17 J. Strandberg,148 S. Strandberg,147a,147b A. Strandlie,118 E. Strauss,144 M. Strauss,112 P. Strizenec,145b R. Ströhmer,175 D. M. Strom,115 R. Stroynowski,40 S. A. Stucci,17 B. Stugu,14 N. A. Styles,42 D. Su,144 J. Su,124 HS. Subramania,3R. Subramaniam,78 A. Succurro,12 Y. Sugaya,117 C. Suhr,107 M. Suk,127 V. V. Sulin,95 S. Sultansoy,4c T. Sumida,67 X. Sun,33a J. E. Sundermann,48 K. Suruliz,140 G. Susinno,37a,37b M. R. Sutton,150 Y. Suzuki,65 M. Svatos,126 S. Swedish,169 M. Swiatlowski,144 I. Sykora,145a T. Sykora,128 D. Ta,89 K. Tackmann,42 J. Taenzer,159 A. Taffard,164 R. Tafirout,160a N. Taiblum,154 Y. Takahashi,102 H. Takai,25 R. Takashima,68 H. Takeda,66 T. Takeshita,141 Y. Takubo,65 M. Talby,84 A. A. Talyshev,108,s J. Y. C. Tam,175 K. G. Tan,87 J. Tanaka,156 R. Tanaka,116 S. Tanaka,132 S. Tanaka,65 A. J. Tanasijczuk,143 K. Tani,66 N. Tannoury,21 S. Tapprogge,82 S. Tarem,153 F. Tarrade,29 G. F. Tartarelli,90a P. Tas,128 M. Tasevsky,126 T. Tashiro,67 E. Tassi,37a,37b A. Tavares Delgado,125a,125b Y. Tayalati,136d F. E. Taylor,93 G. N. Taylor,87 W. Taylor,160b F. A. Teischinger,30 M. Teixeira Dias Castanheira,75 P. Teixeira-Dias,76 K. K. Temming,48 H. Ten Kate,30 P. K. Teng,152 J. J. Teoh,117 S. Terada,65 K. Terashi,156 J. Terron,81 S. Terzo,100 M. Testa,47 R. J. Teuscher,159,j J. Therhaag,21 T. Theveneaux-Pelzer,34 J. P. Thomas,18 J. Thomas-Wilsker,76 E. N. Thompson,35 P. D. Thompson,18 P. D. Thompson,159 A. S. Thompson,53 L. A. Thomsen,36 E. Thomson,121 M. Thomson,28 W. M. Thong,87 R. P. Thun,88,a F. Tian,35 M. J. Tibbetts,15 V. O. Tikhomirov,95,hh Yu. A. Tikhonov,108,s S. Timoshenko,97 E. Tiouchichine,84 P. Tipton,177 S. Tisserant,84 T. Todorov,5S. Todorova-Nova,128 B. Toggerson,7J. Tojo,69 S. Tokár,145a K. Tokushuku,65 K. Tollefson,89 L. Tomlinson,83 M. Tomoto,102 L. Tompkins,31 K. Toms,104 N. D. Topilin,64 E. Torrence,115 H. Torres,143 E. Torró Pastor,168 J. Toth,84,ii F. Touchard,84 D. R. Tovey,140 H. L. Tran,116 T. Trefzger,175 L. Tremblet,30 A. Tricoli,30 I. M. Trigger,160a S. Trincaz-Duvoid,79 M. F. Tripiana,70 N. Triplett,25 W. Trischuk,159 B. Trocmé,55 C. Troncon,90a M. Trottier-McDonald,143 M. Trovatelli,135a,135b P. True,89 G. AAD et al. PHYSICAL REVIEW D 90, 052005 (2014) 052005-24 M. Trzebinski,39 A. Trzupek,39 C. Tsarouchas,30 J. C-L. Tseng,119 P. V. Tsiareshka,91 D. Tsionou,137 G. Tsipolitis,10 N. Tsirintanis,9S. Tsiskaridze,12 V. Tsiskaridze,48 E. G. Tskhadadze,51a I. I. Tsukerman,96 V. Tsulaia,15 S. Tsuno,65 D. Tsybychev,149 A. Tudorache,26a V. Tudorache,26a A. N. Tuna,121 S. A. Tupputi,20a,20b S. Turchikhin,98,gg D. Turecek,127 I. Turk Cakir,4d R. Turra,90a,90b P. M. Tuts,35 A. Tykhonov,74 M. Tylmad,147a,147b M. Tyndel,130 K. Uchida,21 I. Ueda,156 R. Ueno,29 M. Ughetto,84 M. Ugland,14 M. Uhlenbrock,21 F. Ukegawa,161 G. Unal,30 A. Undrus,25 G. Unel,164 F. C. Ungaro,48 Y. Unno,65 D. Urbaniec,35 P. Urquijo,21 G. Usai,8A. Usanova,61 L. Vacavant,84 V. Vacek,127 B. Vachon,86 N. Valencic,106 S. Valentinetti,20a,20b A. Valero,168 L. Valery,34 S. Valkar,128 E. Valladolid Gallego,168 S. Vallecorsa,49 J. A. Valls Ferrer,168 P. C. Van Der Deijl,106 R. van der Geer,106 H. van der Graaf,106 R. Van Der Leeuw,106 D. van der Ster,30 N. van Eldik,30 P. van Gemmeren,6J. Van Nieuwkoop,143 I. van Vulpen,106 M. C. van Woerden,30 M. Vanadia,133a,133b W. Vandelli,30 R. Vanguri,121 A. Vaniachine,6P. Vankov,42 F. Vannucci,79 G. Vardanyan,178 R. Vari,133a E. W. Varnes,7 T. Varol,85 D. Varouchas,79 A. Vartapetian,8K. E. Varvell,151 F. Vazeille,34 T. Vazquez Schroeder,54 J. Veatch,7 F. Veloso,125a,125c S. Veneziano,133a A. Ventura,72a,72b D. Ventura,85 M. Venturi,170 N. Venturi,159 A. Venturini,23 V. Vercesi,120a M. Verducci,139 W. Verkerke,106 J. C. Vermeulen,106 A. Vest,44 M. C. Vetterli,143,f O. Viazlo,80 I. Vichou,166 T. Vickey,146c,jj O. E. Vickey Boeriu,146c G. H. A. Viehhauser,119 S. Viel,169 R. Vigne,30 M. Villa,20a,20b M. Villaplana Perez,90a,90b E. Vilucchi,47 M. G. Vincter,29 V. B. Vinogradov,64 J. Virzi,15 I. Vivarelli,150 F. Vives Vaque,3 S. Vlachos,10 D. Vladoiu,99 M. Vlasak,127 A. Vogel,21 M. Vogel,32a P. Vokac,127 G. Volpi,123a,123b M. Volpi,87 H. von der Schmitt,100 H. von Radziewski,48 E. von Toerne,21 V. Vorobel,128 K. Vorobev,97 M. Vos,168 R. Voss,30 J. H. Vossebeld,73 N. Vranjes,137 M. Vranjes Milosavljevic,106 V. Vrba,126 M. Vreeswijk,106 T. Vu Anh,48 R. Vuillermet,30 I. Vukotic,31 Z. Vykydal,127 W. Wagner,176 P. Wagner,21 H. Wahlberg,70 S. Wahrmund,44 J. Wakabayashi,102 J. Walder,71 R. Walker,99 W. Walkowiak,142 R. Wall,177 P. Waller,73 B. Walsh,177 C. Wang,152,kk C. Wang,45 F. Wang,174 H. Wang,15 H. Wang,40 J. Wang,42 J. Wang,33a K. Wang,86 R. Wang,104 S. M. Wang,152 T. Wang,21 X. Wang,177 C. Wanotayaroj,115 A. Warburton,86 C. P. Ward,28 D. R. Wardrope,77 M. Warsinsky,48 A. Washbrook,46 C. Wasicki,42 I. Watanabe,66 P. M. Watkins,18 A. T. Watson,18 I. J. Watson,151 M. F. Watson,18 G. Watts,139 S. Watts,83 B. M. Waugh,77 S. Webb,83 M. S. Weber,17 S. W. Weber,175 J. S. Webster,31 A. R. Weidberg,119 P. Weigell,100 B. Weinert,60 J. Weingarten,54 C. Weiser,48 H. Weits,106 P. S. Wells,30 T. Wenaus,25 D. Wendland,16 Z. Weng,152,ff T. Wengler,30 S. Wenig,30 N. Wermes,21 M. Werner,48 P. Werner,30 M. Wessels,58a J. Wetter,162 K. Whalen,29 A. White,8M. J. White,1R. White,32b S. White,123a,123b D. Whiteson,164 D. Wicke,176 F. J. Wickens,130 W. Wiedenmann,174 M. Wielers,130 P. Wienemann,21 C. Wiglesworth,36 L. A. M. Wiik-Fuchs,21 P. A. Wijeratne,77 A. Wildauer,100 M. A. Wildt,42,ll H. G. Wilkens,30 J. Z. Will,99 H. H. Williams,121 S. Williams,28 C. Willis,89 S. Willocq,85 J. A. Wilson,18 A. Wilson,88 I. Wingerter-Seez,5F. Winklmeier,115 B. T. Winter,21 M. Wittgen,144 T. Wittig,43 J. Wittkowski,99 S. J. Wollstadt,82 M. W. Wolter,39 H. Wolters,125a,125c B. K. Wosiek,39 J. Wotschack,30 M. J. Woudstra,83 K. W. Wozniak,39 M. Wright,53 M. Wu,55 S. L. Wu,174 X. Wu,49 Y. Wu,88 E. Wulf,35 T. R. Wyatt,83 B. M. Wynne,46 S. Xella,36 M. Xiao,137 D. Xu,33a L. Xu,33b,mm B. Yabsley,151 S. Yacoob,146b,nn M. Yamada,65 H. Yamaguchi,156 Y. Yamaguchi,156 A. Yamamoto,65 K. Yamamoto,63 S. Yamamoto,156 T. Yamamura,156 T. Yamanaka,156 K. Yamauchi,102 Y. Yamazaki,66 Z. Yan,22 H. Yang,33e H. Yang,174 U. K. Yang,83 Y. Yang,110 S. Yanush,92 L. Yao,33a W-M. Yao,15 Y. Yasu,65 E. Yatsenko,42 K. H. Yau Wong,21 J. Ye,40 S. Ye,25 I. Yeletskikh,64 A. L. Yen,57 E. Yildirim,42 M. Yilmaz,4b R. Yoosoofmiya,124 K. Yorita,172 R. Yoshida,6K. Yoshihara,156 C. Young,144 C. J. S. Young,30 S. Youssef,22 D. R. Yu,15 J. Yu,8J. M. Yu,88 J. Yu,113 L. Yuan,66 A. Yurkewicz,107 B. Zabinski,39 R. Zaidan,62 A. M. Zaitsev,129,z A. Zaman,149 S. Zambito,23 L. Zanello,133a,133b D. Zanzi,100 C. Zeitnitz,176 M. Zeman,127 A. Zemla,38a K. Zengel,23 O. Zenin,129 T. Ženiš,145a D. Zerwas,116 G. Zevi della Porta,57 D. Zhang,88 F. Zhang,174 H. Zhang,89 J. Zhang,6L. Zhang,152 X. Zhang,33d Z. Zhang,116 Z. Zhao,33b A. Zhemchugov,64 J. Zhong,119 B. Zhou,88 L. Zhou,35 N. Zhou,164 C. G. Zhu,33d H. Zhu,33a J. Zhu,88 Y. Zhu,33b X. Zhuang,33a A. Zibell,175 D. Zieminska,60 N. I. Zimine,64 C. Zimmermann,82 R. Zimmermann,21 S. Zimmermann,21 S. Zimmermann,48 Z. Zinonos,54 M. Zinser,82 M. Ziolkowski,142 G. Zobernig,174 A. Zoccoli,20a,20b M. zur Nedden,16 G. Zurzolo,103a,103b V. Zutshi107 and L. Zwalinski30 (ATLAS Collaboration) 1Department of Physics, University of Adelaide, Adelaide, Australia 2Physics Department, SUNY Albany, Albany, New York, USA 3Department of Physics, University of Alberta, Edmonton Albeta, Canada 4aDepartment of Physics, Ankara University, Ankara, Turkey SEARCH FOR HIGH-MASS DILEPTON RESONANCES IN …PHYSICAL REVIEW D 90, 052005 (2014) 052005-25