dataesr/scientific-paragraphs-categorization huggingface dataset:
Events selected for this analysis are triggered by a J/ψ → µ + µ -decay, where the J/ψ meson is required at the software level to be consistent with coming from the decay of a B 0 meson by use either of IP requirements or detachment of the J/ψ meson decay vertex from the primary vertex (PV). In the simulation, pp collisions are generated using Pythia  [10]  with a specific LHCb configuration  [11]. Decays of hadronic particles are described by EvtGen  [12] , in which final state radiation is generated using Photos  [13]. The interaction of the generated particles with the detector and its response are implemented using the Geant4 toolkit  [14, 15]  as described in Ref. [16]. 3 Decay amplitude formalism.
We find that f 0 (980) production is much smaller than predicted for tetraquarks, which we rule out at the 8 standard deviation level using the model of Ref. [2]. Concern has been expressed  [33]  that if the f 0 (980) were a tetraquark state the measurement of the mixingdependent CP -violating phase in the decay B 0 s → J/ψ f 0 (980) could be affected due to additional decay mechanisms. Our result here alleviates this potential source of error. centres are supported by IN2P3 (France), KIT and BMBF (Germany), INFN (Italy), NWO and SURF (The Netherlands), PIC (Spain), GridPP (United Kingdom). We are indebted to the communities behind the multiple open source software packages on which we depend. We are also thankful for the computing resources and the access to software R&D tools provided by Yandex LLC (Russia).
Acknowledgements We express our gratitude to our colleagues in the CERN accelerator departments for the excellent performance of the LHC. We thank the technical and administrative staff at the LHCb institutes. We acknowledge support from  CERN  and from the national agencies:  CAPES ,  CNPq ,  FAPERJ  and  FINEP (Brazil) ;  NSFC (China) ;  CNRS/IN2P3  and  Region Auvergne (France) ;  BMBF ,  DFG ,  HGF  and  MPG (Germany) ;  SFI (Ireland) ;  INFN (Italy) ;  FOM  and  NWO  (The Netherlands); SCSR (Poland);  MEN/IFA (Romania) ;  MinES, Rosatom ,  RFBR  and  NRC "Kurchatov Institute" (Russia) ;  MinECo, XuntaGal and GENCAT (Spain) ;  SNSF  and  SER (Switzerland) ;  NASU (Ukraine) ;  STFC  and the  Royal Society  ( United Kingdom );  NSF (USA). We also acknowledge the support received from  EPLANET ,  Marie Curie Actions  and the  ERC  under  FP7.
Acknowledgments This work was supported partially by the  Spanish national company  for radioactive waste ENRESA, through the  CIEMAT-ENRESA agreements on "Transmutación de residuos radiactivos de alta actividad ", the  Spanish Plan Nacional de IþD þi de Física de Partículas  (project  FPA2008-04972-C03-01 ), the  Spanish Ministerio de Ciencia e Innovación  through the  CONSOLIDER CSD 2007-00042  project and the  European Union 's  Seventh Framework Programme  under grant agreement no  262010.
RESULTS We here analyze the EPIC data of the XMM-Newton Large Program of observations of SN 1006 (together with older XMM-Newton archive observations). The data and the reduction process are described in detail in  Miceli et al. (2012 Miceli et al. ( , 2013b)). The interstellar environment around SN 1006 was studied by using the HI observations presented in D02. The radio data were obtained using the Australia Telescope Compact Array and combined with single dish data from Parkes telescope (we refer to D02 for further information).
ACKNOWLEDGEMENTS S. R. is grateful to  J. Cardy  for useful discussions, and to  H. W. Diehl  for informing him about Refs. [42][43][44]. We thank the organizers and participants for the stimulating environment at the "Back to the Bootstrap 3" conference at  CERN. The work of S. E. was supported by the  French ANR  Contract No. 05-BLAN-NT09-573739 , the  ERC Advanced  Grant No. 226371  and the ITN program PITN-GA-2009-237920. M. P. is supported by  DOE  Grant No. DE-SC0010010-Task A. D. P. thanks the  Galileo Galilei Institute for Theoretical Physics  and the  INFN  for hospitality and partial support during the completion of this work. The work of S. R. is supported in part by the  European Program "Unification in the LHC Era ", contract  PITN-GA-2009-237920  (UNILHC). The work of D. S. D.
Acknowledgments The successful installation, commissioning, and operation of the  Pierre Auger Observatory  would not have been possible without the strong commitment and effort from the technical and administrative staff in Malarg üe. G. Curci was supported by the  Italian Space Agency (ASI)  in the frame of  PRIMES  project. We are very grateful to the following agencies and organizations for financial support:  Comisi ón Nacional de Energía At ómica, Fundaci ón Antorchas, Gobierno De La Provincia de Mendoza, Municipalidad de Malarg üe, NDM Holdings  and  Valle Las Le  ñas, in gratitude for their continuing cooperation over land access, Argentina; the  Australian Research Council ;  Conselho Nacional de Desenvolvimento Científico e Tecnol ógico (CNPq) ,  Financiadora de Estudos e Projetos (FINEP) ,  Fundacão de Amparo à Pesquisa do Estado de Rio de Janeiro (FAPERJ) ,  São Paulo Research Foundation (FAPESP)  Grants # 2010/07359-6 , # 1999/05404-3 ,  Ministério de Ciência e Tecnologia (MCT) , Brazil; AVCR, MSMT-CR LG13007,  7AMB12AR013 ,  MSM0021620859 , and  TACR TA01010517  ,  Czech Republic ;  Centre de Calcul IN2P3/CNRS ,  Centre National de la Recherche Scientifique (CNRS) ,  Conseil Régional Ile-de-France ,  Département Physique Nucléaire et Corpusculaire  ( PNC-IN2P3/CNRS ),  Département Sciences de l'Univers (SDU-INSU/CNRS ), France;  Bundesministerium f ür Bildung und Forschung (BMBF) ,  Deutsche Forschungsgemeinschaft (DFG) ,  Finanzministerium Baden-W ürttemberg, Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF) ,  Ministerium f ür Wissenschaft und Forschung ,  Nordrhein-Westfalen, Ministerium f ür Wissenschaft, Forschung und Kunst, Baden-W ürttemberg, Germany ;  Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR) ,  Gran Sasso Center for Astroparticle Physics (CFA) ,  CETEMPS Center of Excellence, Italy ;  Consejo Nacional de Ciencia y Tecnología (CONACYT) ,  Mexico ;  Ministerie van Onderwijs, Cultuur en Wetenschap ,  Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) ,  Stichting voor Fundamenteel Onderzoek der Materie (FOM) ,  Netherlands ;  Ministry of Science and Higher Education , Grant Nos.
Calorimetric denaturation curve Differential scanning calorimetry (DSC) studies were performed using a Seratam Micro DSC III calorimeter. Samples cut from A-form DNA fiber films were hermetically sealed in a Hastelloy sample tube, and the calorimetry measurements were made relative to an empty tube. Measurements were made for a variety of heating rates between 0. 6 and 1. 2 K min -1 , with the data showing no discernible difference between ramp rates. Comparison between the melting profile of A-DNA films obtained by calorimetry (dashed-dotted line) and the theoretical profile given by fitting with the modified PBD model (thick red line) for a sequence of 40 000 base pairs extracted from a salmon sequence listed in the GenBank  [23]. For comparison the thin (black) full line shows the specific heat of a B-DNA film, made of Li-DNA humidified under 92% relative humidity.
( 4 ) high c 2 2 gnd In these expressions I designates the integrated intensity of each peak, Γ its width in units of Å -1 , and Q c the position of its center. The experimental resolution was measured using a silicon Bragg peak. The measurements were used to parameterize the instrument resolution for all Q and the DNA data were fitted by model expressions convoluted with the expression for the resolution. Examples of the fits are shown in figure  3. We applied certain constraints to the variables in order to have robust and systematic fits, which are particularly problematic when close to the melting temperature where the signal-to-noise is small. The widths of the three high-Q peaks were constrained to be equal, defined as Γ high. We justify this by noting that the three peaks are close together in Q and that their widths, as confirmed by close inspection of the calculation in figure  2 , are very similar.
The data at 300 K were then fitted. The resulting values of Q c were then fixed for all temperatures. The fitted values for I at 300 K were used to calculate the I I low ratios for the three high-Q peaks, where I low is the integrated intensity of the low-Q peak, and these ratios were fixed for all subsequent fits. We justify this by noting that the Bragg peaks come from closed regions of DNA. The spatial correlation length may change, but the integrated intensities will be a result of the number of scattering centers in the closed regions. Their ratios will not vary substantially with temperature. The number of free parameters to fit the temperature-dependent data thus reduces to three: I T ( ) low ; Γ T ( ) high ; and the width of the low-Q peak, Γ T ( ) low. Figure  4  shows I T I ( ) (300 K) low low along with the variation of the fraction of undenatured DNA determined by calorimetry.
The stacking interactions were chosen to properly describe the melting profile of our DNA sample, as determined by calorimetry. Figure  1  shows a comparison of the experimental melting profile with the theoretical profile calculated with the modified PBD model. Some fine structure is observed in the calculated profile due to the finite number of base pairs used for the calculation. The experimental data were obtained from a sample with billions of base pairs, while the PBD model used a segment of 40 000 base pairs from the sequence of one salmon gene. The melting profile is, of course, sequence dependent, and we expect that the fine structure in the calculation would average out if we could perform the calculation for a much larger DNA segment. Nevertheless, the model gives a denaturation profile which is very close to the calorimetric profile.
Section 4 focuses on the method used to compute the various efficiencies. The data and simulation samples used in this work are given in Section 5 together with the main triggers that enabled the event collection. Section 6 reports on the identification efficiency measurement, presenting the background evaluation and the results obtained with the tag-and-probe technique. A similar methodology, but using a subset of the samples available for the identification efficiency measurement, is used to extract the efficiency of the electron reconstruction described in Section 7. The study of the probability to mismeasure the charge of an electron is presented in Section 8. The summary of the work is given in Section 9.
The 2011 data and simulation samples The data recorded during the 2011 proton-proton collision run at 7 TeV are subdivided into several periods corresponding to the changing conditions of the detector, including the energy thresholds of the primary triggers, as well as the instantaneous luminosity of the LHC. Monte Carlo samples are generated to mimic the same period granularity. In order to reproduce the pile-up effects observed in the data, additional inelastic proton-proton interactions in the form of simulated Pythia  [16]  minimum-bias events are included in the Monte Carlo simulation.
Samples All data collected by the ATLAS detector undergo careful scrutiny to ensure the quality of the recorded information. In particular, data used for the efficiency measurements are filtered requiring that all detector subsystems needed in the analysis (calorimeters and tracking detectors) are operating nominally. Several detector defects had minor impacts on the quality of the 2011 data set. The total integrated luminosity used for the measurement presented in this paper is L = 4. 7 fb -1  [17]. Samples of simulated Z → ee, W → eν, and J/ψ → ee decays are used to benchmark the expected electron reconstruction and identification performance. The primary Z → ee and W → eν MC samples are generated with Powheg version r1556  [18, 19, 20, 21]  and parton showering is accomplished using Pythia version 6.
425. The J/ψ samples are generated using the same version of Pythia. All generators are interfaced to Photos version 3. 0  [22]  to simulate the effect of final-state QED radiation. The generated event samples are passed through a detailed ATLAS detector simulation  [23]  using GEANT4  [24]. The MC events are reconstructed using the same software suite as used for the data. Because background subtraction is not performed on the MC signal samples when assessing the expected electron efficiency, generator-level information is used to select electrons originating only from Z → ee, W → eν, or J/ψ → ee decays. Correction factors are applied to the simulation to account for known discrepancies with the data. These include corrections in the form of event weights applied to the simulated events to match the average interaction rate per bunch crossing and the width of the beam-spot in the z-direction, both as measured in the 2011 data set.
Z → ee channel: The baseline sample of Z → ee events is modified by using alternative selection criteria defining the tag electrons. Three m ee windows (80-100, 70-100 and 75-105 GeV) are used to extract the signal events. Moreover, the size and composition of the background are varied by modifying the reverse requirements used to generate the templates. As an example, the curves "Bkg template 1 and 2" in The invariant mass for pairs where the probe satisfies the tight criteria is also shown. (c) Invariant mass distribution for the J/ψ → ee sample in the short-lifetime range. The purple curve corresponds to the measured background with same-sign (SS) pairs, the dashed green line shows the opposite-sign (OS) background, the blue curve indicates the extracted signal and the red line is the fit to data taking into account signal, background, and ψ(2S) (not shown in the figure) contributions.
For E T > 20 GeV, the uncertainties are shown in the 50 η bins available using the fine granularity. The total uncertainties are dominated by the statistical component. The systematic uncertainties are dominated by the uncorrelated component, which is largely due to the difference of the two Z → ee methods and thus affected by limited statistics of the different data samples employed for the background-subtraction procedures. Breit-Wigner function with fixed Z width  [26]  to model the signal, and a Landau function to model the background. The S/B ratio is ∼ 7 and ∼ 5 in the EMEC and the FCal, respectively. After background subtraction, a total of 192,000 and 76,000 probes remain in the two regions. Variations of the tag requirements are performed, which change the S/B ratio by up to a factor of two.
It then follows that the centralelectron reconstruction efficiency as measured in data reflects the performance of the track reconstruction and the track-cluster matching procedure. Efficiency values are measured for three event samples: all reconstructed electron candidates; electron candidates satisfying in addition a requirement on the quality of the matching track; this is to match the probe definition of the J/ψ → ee selection used in the electron identification efficiency measurement; electron candidates with a good track and satisfying in addition the requirement on the hadronic leakage R had defined by the loose identification criteria; this is to match the probe definition of the W → eν and Z → ee selections. For this measurement, only one of the channels available to the identification efficiency measurement, a Z → ee sample, can be used.
Background evaluation The electron background contribution is estimated using a methodology similar to that employed for the identification efficiency measurements discussed in Section 6. 1. 2, based on the electron-positron invariant mass. The background cluster-pair invariant mass template is obtained from data by reversing identification requirements on the probe object and then normalising the distribution to the background-dominated clusterpair invariant mass distribution in the 110-250 GeV region. When measuring the reconstruction efficiency alone, the probe electrons of the background template are required to fail at least two of the requirements defining the loose identification, with the exception of those associated with the track quality, and to satisfy the anti-isolation requirement E cone T (0.
Reconstruction efficiency and systematics The reconstruction efficiency as a function of pseudorapidity for all three event selections is shown in Fig-  ure  17 in E T bins ranging from 15 to 50 GeV. In the lowest E T bin, a coarser η binning is used to cope with the smaller data sample, and still ensure that the total uncertainty is equally shared between statistical and systematic sources. The systematic uncertainties are assessed by varying parameters in the fitting procedure and measuring the global systematic uncertainty as the RMS of the distribution of the results obtained with each configuration. These variations include identification quality of the tag electron, the invariant-mass range used to select the signal events, the template shape used for electrons, and the sideband fit range for the photon background evaluation.
Acknowledgements 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, MIN-ERVA, 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 MIZ Š, 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.
Acknowledgements The authors thankfully acknowledge the computer resources, technical expertise and assistance provided by the  Barcelona Supercomputing Center -Centro Nacional de Supercomputación  for the projects  QCM-2009-1-0014 ,  QCM-2008-3-0012  and  QCM-2008-2-0010. The research institution  INSTM  is also acknowledged by M. M. , who is also thankful for the resources given by the  Cybersar Project managed by the "Consorzio COSMOLAB ". E. G. acknowledges financial support from the  Direcció General de Recerca de la Generalitat de Catalunya  (Grant  2009SGR-1003 ) and from the  Ministerio de Ministerio de Economía y Cometitividad (MINECO) of Spain  (Grant  FIS2012-39443-C02-01 ). I. S. acknowledges the  HPC-EUROPA 2 project  (project n. 228398) for the support of the  European Commision -Capacities Area -Research Infrastructures , which allowed him to visit the group of M.
Acknowledgements J. P. P. acknowledges the support given by the  International Relativistic Astrophysics PhD Program  through the  Erasmus Mundus Grant   2011-1640  from  EACEA of the European Commission. H. J. M. C. acknowledges the  ICRANet Coordinating Headquarters in Pescara, Italy , for hospitality, and the support by the  International Cooperation Program CAPES-ICRANet  through the  Sabbatical Grant   0153-14-1 , financed by  CAPES -Brazilian Federal Agency for Support and Evaluation of Graduate Education within the Ministry of Education of Brazil. We thank the anonymous referee for the comments and suggestions which helped us to improved the presentation of the results of this research.
Selection criteria are applied to reject background candidates that fake Z → µ + µ -decays: the impact parameter of each track with respect to the closest primary vertex must be less than 100 µm, and the sum of the energies measured in the ECAL and HCAL associated to each track has to be less than 0. 5 times the track momentum measured in the tracking system. The χ 2 -probability of the track fit is required to be larger than 1 % for both tracks. Figure  1  shows the invariant mass distribution of the selected candidates for the two beam configurations together with the predictions from simulation. There is a good agreement between data and simulation. In total, eleven candidates are selected in the forward sample and four in the backward sample. The rapidity distributions of the Z candidates are shown in Fig.
2007 ). The first observation was displaced by -0. 5 • in declination and started at a zenith angle of 31. 7 • , reaching a final position of 34. 6 • (mean value of 32. 7 • ) with a deadtime-corrected livetime of 1576 s. For the second observation (displaced 0. 5 • in declination), the zenith angle range was 34. 1-37. 3 • (mean value of 36. 1 • ). It started at 03:45:23 UT and had a livetime of 1574 s. All data were taken during good weather conditions with good hardware status of all four telescopes. The data calibration, image cleaning, Hillas moment calculation  (Hillas 1996 ) and event reconstruction is done as described in  Aharonian et al. (2006a)  with the standard H. E. S. S. analysis software 2. In this reference, three different selection cuts (standard, hard, loose) to reject background caused by cosmic-ray showers are described, suited for different source scenarios.
Results The results of the analysis of the H. E. S. S. data taken for GRB 100621A are shown in Table  1. No excess is observed using the total data set. In order to search for emission on shorter time scales and closer to t 0 a further analysis was done on each observation separately and on the events corresponding to the first 300 s of the first observation. Shorter time scales are not possible because the number of events in the on-region would become too low to estimate the significance. No significant excess is found here either. The result for the total dataset has also been crosschecked with an independent calibration and analysis of the data  (Becherini et al. 2011). Upper limits on the number of excess events are calculated using the method of  Rolke et al. (2005). These upper limits are converted to integral flux upper limits using the H.
Summary In this paper, the analysis of the H. E. S. S. data on GRB 100621A is presented. A significant excess has neither been observed in the total data set, nor on shorter time scales closer to the prompt emission. This constrains the possibility of a temporallyextended emission in the form of an additional hard power law like it has been observed by Fermi-LAT in previous bright bursts. A component as strong as in GRB 130427A is not compatible with the H. E. S. S. measurements. GRB 100621A is one of the brightest X-ray sources detected by Swift with a very bright X-ray afterglow. The H. E. S. S. observations started during the shallow decline of the X-ray light curve and the upper limits on the energy output during that time are comparable to the level of the X-ray emission. The ratio between the X-ray and VHE flux is constrained to be greater than 0.