dataesr/scientific-paragraphs-categorization huggingface dataset:
The difference between the observed and predicted numbers of e ± e ± events is used as a scale factor to account for the modeling in the simulation. The observed number of events in the data is determined by fitting the Z boson mass peak. The predicted number of events is determined by weighting the OS2 events with the value W p. The scale factors and their associated statistical uncertainties in the barrel and endcap regions are found to be 0. 80 ± 0. 03 and 0. 87 ± 0. 03, respectively. To validate the combined sign mismeasurement probability and scale factors in the data, a control sample of Z → e ± e ∓ events is again selected, as described above, but here requiring that one electron is found in the endcap and the other, in the barrel region. The difference in the predicted and observed numbers of e ± e ± events in this sample is 12%.
Acknowledgments We congratulate our colleagues in the CERN accelerator departments for the excellent performance of the LHC and thank the technical and administrative staffs at  CERN  and at other  CMS institutes  for their contributions to the success of the CMS effort. In addition, we gratefully acknowledge the computing centers and personnel of the Worldwide LHC Computing Grid for delivering so effectively the computing infrastructure essential to our analyses. Finally, we acknowledge the enduring support for the construction and operation of the LHC and the CMS detector provided by the following funding agencies: the  Austrian Federal Ministry of Science, Research and Economy  and the  Austrian Science Fund ; the  Belgian Fonds de la Recherche Scientifique , and  Fonds voor Wetenschappelijk Onderzoek ; the  Brazilian Funding Agencies (CNPq, CAPES ,  FAPERJ ,  FAPERGS , and  FAPESP) ; the  Bulgarian Ministry of Education and Science ; CERN; the  Chinese Academy of Sciences, Ministry of Science and Technology, and Na-Desarrollo Regional, Spain ; the  Ministry of Science, Technology and Research, Sri Lanka ; the  Swiss Funding Agencies (ETH Board, ETH Zurich, PSI, SNF, UniZH ,  Canton Zurich , and SER); the  Ministry of Science and Technology, Taipei ; the  Thailand Center of Excellence in Physics , the  Institute for the Promotion of Teaching Science and Technology of Thailand, Special Task Force for Activating Research and the National Science and Technology Development Agency of Thailand ; the  Scientific and Technical Research Council of Turkey , and  Turkish Atomic Energy Authority ; the  National Academy of Sciences of Ukraine, and State Fund for Fundamental Researches, Ukraine ; the  Science and Technology Facilities Council , UK; the  US Department of Energy , and the  US National Science Foundation.
Individuals have received support from the  Marie-Curie program  and the  European Research Council and Horizon 2020  Grant, contract No. 675440  ( European Union ); the  Leventis Foundation ; the A. P. Sloan Foundation; the  Alexander von Humboldt Foundation ; the  Belgian Federal Science Policy Office ; the  Fonds pour la Formation à la Recherche dans l'Industrie et dans l'Agriculture (FRIA-Belgium) ; the  Agentschap voor Innovatie door Wetenschap en Technologie  ( IWT-Belgium ); the  F. R. S. -FNRS  and  FWO (Belgium)  under the  "Excellence of Science -EOS" -be. h project n. 30820817; the  Ministry of Education, Youth and Sports (MEYS)  of the Czech Republic; the  Lend ület ("Momentum") Program  and the  János Bolyai Research Scholarship of the Hungarian Academy of Sciences , the  New National Excellence Program ÚNKP , the  NKFIA  research grants  123842 ,  123959 ,  124845 ,  124850  and  125105  (Hungary); the  Council of Scientific and Industrial Research, India ; the  HOMING PLUS program  of the  Foundation for Polish Science , cofinanced from  European Union, Regional Development Fund , the  Mobility Plus program of the Ministry of Science and Higher Education , the  National Science Center (Poland) , contracts Harmonia  2014/14/M/ST2/00428 ,  Opus 2014/13/B/ST2/02543 ,  2014/15/B/ST2/03998 , and  2015/19/B/ST2/02861 , Sonata-bis  2012/07/E/ST2/01406 ; the  National Priorities Research Program  by  Qatar National Research Fund ; the  Programa de Excelencia María de Maeztu , and the  Programa Severo Ochoa del Principado de Asturias ; the Thalis and Aristeia programs cofinanced by  EU-ESF , and the  Greek NSRF ; the  Rachadapisek Sompot Fund for Postdoctoral Fellowship, Chulalongkorn University , and the  Chulalongkorn Academic into Its 2nd Century Project Advancement Project (Thailand) ; the  Welch Foundation , contract  C-1845 ; and the  Weston Havens Foundation (USA).
1% according to the ExAC Browser of Broad Institute (21) and 1,000 Genomes  (22)  databases. Subsequent filtering steps sorted out variants following the autosomal recessive inheritance model as well as their functional impact (i. e. , non-sense, affecting the canonical splice-site regions or non-synonymous) and the prediction of Polyphen  (23)  and SIFT (24) bioinformatics tools. Filtering about 43,500 variants in each sample led to the identification of two different ESCO2 (NG_008117. 1) homozygous alterations in the probands: c. 1131+1G>A in intron 6 of patient 1 and c. 417del in exon 3 of patient 2 [sequence variants were termed according to HGVS recommendations (25)]. Sanger sequencing confirmed the biallelic pathogenic alterations in the probands and the carrier status of their parents (Figures  1L, S ) and of the elder brother of patient 1.
The splice donor variant c. 1131+1G>A has a MAF < 0. 01 and has been previously reported  (13, (26) (27) (28)  while the c. 417del is absent from public databases, has not been described to date and has been submitted to LOVD database (https://databases. lovd. nl/shared/ genes/ESCO2). The final diagnosis of Roberts syndrome was done in both cases. Moreover, C-banding chromosome analysis of patient 1 showed the premature centromere separation and heterochromatin repulsion known to be pathognomonic for RBS (Figure  1M ).
This piezoelectric actuator is mounted on the same mechanical system as the source. Rotation of the system makes it possible to turn the beam towards the detector. A dual stage micro-channel plate fluorescent screen assembly (F2225-21P from Hamamatsu) detects single low-energy electrons from 10 to 1000 eV. We recently showed that in counting mode, this apparatus enhances the resolution of a low-energy electron microscope  36. In the present experiment, this mode is used both to determine the electron charge and to show the particle-wave duality. This detector is placed 86 cm away from the source. Images and films of the fluorescent screen are recorded using a cooled CCD camera (Model C4742-95 from Hamamatsu). Here, a counting mode record is directly obtained from the integrated software HiPic from Hamamatsu: the stain produced by the impact of one electron is reduced to one pixel, and each impact counts as 1.
2 W water immersion objective. Atto488-labeled DOPE lipids were excited by an argon ion laser with a wavelength of 488 nm, and their emission in the range from 500 to 550 nm was detected with the QUASAR detection unit. For irradiation of the photo-oxidizer erythrosine, we used the microscope-attached mercury lamp (HXP 120 C, FSet43wf). Image analysis was performed with the software ImageJ. ■ ASSOCIATED CONTENT * S Supporting Information The Supporting Information is available free of charge on the ACS Publications website at DOI: 10. 1021/acsomega. 9b00912. Swelling ratios and polymer fractions of the PNIPAAm hydrogel versus illumination energy dose; CLSM images of GUVs, formed on homogenous PNIPAAm hydrogel films; scheme of the PNIPAAm terpolymer synthetic route (PDF).
A final polishing step was applied using a mixture of colloidal silica suspension with a mean particle size of 0. 04 µm and 10 % H2O2. Incremental loading of the specimen was performed using a displacement rate of 0. 02 mm min -1. The crosshead displacement is measured using a linear variable differential transformer position transducer. The engineering strain is derived from the displacement data after a machine stiffness correction using a reference Young's modulus of 115 GPa. In order to characterize the surface of the specimen at different deformation stages, the crosshead displacement was stopped after reaching targeted stress values. The engineering stress -strain conditions corresponding to arrests of the crosshead displacement are plotted on figure  2a. The characterization of the crystallographic orientations in the region of interest was performed at each stop using EBSD.
The microscope is operated under a 25 kV tension and a probe current of about 5 nA is used. Kikkuchi diffraction patterns are acquired with a 5 x 5 binning (128 x 96 pixels) and indexed using a standard Hough transform-based automated processing at a rate of 200 points per second. A 0. 4 µm hexagonal step was applied for a scan duration of 30 minutes at each loading step. Operating deformation systems were first identified using a slip traces analysis at each loading step. Forward-scattered electron (FSD) micrographs are used for the slip trace detection. A FSD map of the region of interest at the 970 MPa step is shown in figure  2b. The orientation of experimental and theoretical slip traces as calculated using the EBSD data are compared. 0001 , 101 0 and 101 1 slip planes are presently considered.
25). Indeed, activation of a slip system with a Schmid factor lower than 0. 25 is very unlikely  [9, [34] [35] [36]. An apparent critical resolved shear stress (CRSS) value was estimated for each successful basal or prismatic slip system identification. Assuming a global stress state, the apparent CRSS value was calculated as the product of the Schmid factor and the average of the remote stress applied before and after slip trace appearance. Apparent CRSS values and associated standard deviations were finally averaged over both basal and prismatic slip systems. This procedure, which relies on a homogeneous stress assumption, neglects stress heterogeneities. However, a prior study revealed that the bias introduced is limited if a statistical approach is applied  [37]. In order to study lattice rotations at the nodule / colony scale, pre-processing of the raw crystallographic orientation data was performed using OIM analysis software.
The following steps are applied. (i) Data points with a confidence index below 0. 1 were dismissed in order to rule out unreliable data points. (ii) Separate nodules / colonies were identified using a 2° misorientation criterion. (iii) The average crystallographic orientations of the 34 nodules and the 21 colonies considered in the present study were computed. The resulting Euler angles ( , , ) were then processed using an in-house Matlab code in order to calculate the lattice rotation relative to the initial lattice orientation. The crystalline orientation at step i is expressed in the specimen frame using the rotation matrix , defined as follows  (3). , = cos cos -sin sin cos -sin cos -cos sin cos sin sin cos sin + sin cos cos -sin sin + cos cos cos -cos sin sin sin cos sin cos ' The lattice rotation between step j and step i is described using the rotation matrix ∆ ,) given in equation  (4).
The resulting values are plotted against the macroscopic plastic strain in figure  6. The average angles of rotation associated with the operation of basal slip are slightly higher than the average angles of rotation associated with the operation of prismatic slip. For instance, under an applied stress of 970 MPa, the angles are 0. 75 ° for prismatic slip and 0. 82 ° for basal slip. A linear regression was applied to both datasets. Regression coefficients about 0. 966 and 0. 990 were obtained for basal and prismatic slip respectively. These values, which are very close to 1, indicate a good fit to the data. A slope of 46 ° was obtained for the subset of colonies associated with the operation of basal slip while a slope of 43 ° was obtained for the subset of colonies associated with the operation of prismatic slip.
Results The spectra of z g , R g and n SD in minimum bias pp collisions were corrected using a 2D-Bayesian unfolding approach to correct for detector effects. The detector effects were studied using GEANT3 on simulated PYTHIA jet events. The results for the pp collisions are presented in the range 40 ≤ p ch T,jet < 60 GeV/c  [13]. Due to a lack of pp statistics at the Pb-Pb collision energy of √ s NN = 2. 76 TeV and the good agreement observed between pp data and PYTHIA at √ s= 7 TeV, PYTHIA events at √ s= 2. 76 TeV were used as the vacuum reference for the Pb-Pb data. In Pb-Pb collisions the measurements of z g and n SD were made in the range 80 ≤ p ch,rec T,jet < 120 GeV/c to avoid contamination from combinatorial background and compared to a smeared reference generated by embedding PYTHIA jets into 0-10% central Pb-Pb events.
Second, also due to this huge gravitational pull, metals are sinked in the deep interiors of white dwarf envelopes, precluding from associating a metallicity value to these objects. Finally, the number of white dwarfs identified in volume-limited samples is rather small. Fortunately, the advent of large data surveys such as Gaia has dramatically increased the number of known white dwarfs, thus providing statistically significant large complete samples. This fact, together with the potential of white dwarfs as cosmochronometers, opens the door to use these objects as reliable tracers of the dynamic Galactic evolution. In this Letter we aim to put into manifest the Hercules stream signature in the population of white dwarfs of the local neighborhood. Additionally, we aim to identify those white dwarfs belonging to the Hercules stream and to derive a first approach to their age distribution.
The Gaia DR2 white dwarf 100 pc sample The second data release of the Gaia mission has provided an unprecedented wealth of accurate astrometric and photometric information. In particular, nearly 260, 000 objects have been identified as white dwarf candidates  (Gentile Fusillo et al. 2019 ) up to a few kpc from the Sun. Moreover, Jiménez-Esteban et al. (  2018 ) claimed that the largest and nearly complete Gaia white dwarf sample extends up to 100 pc from the Sun and contains close to 18, 000 objects. For this sample, and by means of applying innovative techniques based on a Random Forest machine learning algorithm,  Torres et al. (2019)  have been able to classify the white dwarf population into its different Galactic components: thin and thick-disk and stellar halo. The final classified sample contains 12,227 thin-disk, 1,410 thick-disk and nearly 100 halo white dwarf candidates.
Conclusions We have revealed the imprint of the Hercules stream in the space velocity of white dwarfs in the solar neighborhood. In particular, we analyzed the recent Gaia white dwarf population, which presents a valuable wealth of accurate photometric and astrometric data and a nearly complete sample within 100 pc. The analysis of the white dwarf UV plane puts into manifest an overden-Fig. 3. Age distribution for each of the three Hercules sub-stream identified in this work and for all of them considered together (right panel). The sub-stream Her b presents a maximum at around 4 Gyr with an extended long tail up to very old ages. Her a is similar, but with a less clear peak. Sub-stream Her c appears as a more uniform distribution between 2 and 10 Gyr. Also plotted as red lines are analytical normal fits for Her a and c and a log-normal fit for Her c and the entire distribution.
The product of the cross section and branching fraction is therefore approximated to be about 8 fb for all m a 1 values considered in this analysis. The present search for the exotic a 1 particle in the µ + µ -bb final state is sensitive to the mass range of 20 ≤ m a 1 ≤ 62. 5 GeV. The sensitivity of the search largely decreases towards m a 1 ≈ 20 GeV and lower because a 1 gets boosted and the two b quark jets tend to merge  [26]. The upper bound is imposed by the Higgs boson mass. The analysis is performed using the protonproton collision data at 13 TeV collected with the CMS detector during 2016, corresponding to an integrated luminosity of 35. 9 fb -1. Though the signal selection is optimised for the h → a 1 a 1 → µ + µ -bb process, decays of h → a 1 a 1 → µ + µ -τ -τ + can contribute to the selected sample if hadronically decaying τ leptons are misidentified as b quark jets.
The reference cross section for the Drell-Yan process is computed using FEWZ 3. 1  [30]  at next-to-next-to-leading order. The top quark samples, tt and single top quark production, are produced with POWHEG2. 0  [31] [32] [33] [34]  at next-to-leading order (NLO). Backgrounds from diboson (WW, WZ, ZZ) production are generated at NLO with the same program and settings as that of the Drell-Yan samples. The only exception is the W W process that is generated at LO. The set of parton distribution functions (PDFs) is NLO NNPDF3. 0 for NLO samples, and LO NNPDF3. 0 for LO samples  [35]. For all samples, PYTHIA 8. 212  [36]  with tune CUETP8M1  [37, 38]  is used for the modelling of the parton showering and fragmentation. The full CMS detector simulation based on GEANT4  [39]  is implemented for all generated event samples.
Results The analysis yields no significant excess of events over the SM background prediction. Figure  4  shows the m µµ distribution in the data of all categories together with the best fit output for the background model, including uncertainties. The upper limit on σ h B(h → a 1 a 1 → µ + µ -bb ) is obtained at 95% CL using the CL s criterion  [57, 58]  and an asymptotic approximation to the distribution of the profiled likelihood ratio test statistic  [59]. Assuming the SM cross sections for the Higgs boson production processes within the theoretical uncertainties, an upper limit is placed on B(h → a 1 a 1 → µ + µ -bb ) using the same procedure. Limits are evaluated as a function of m a 1. The observed and expected limits are illustrated in Fig. 5  for both cases. Dominant systematic uncertainties are those associated with the b jet identification, followed by the modelling of parton shower and fragmentation.
Individuals have received support from the  Marie-Curie  programme and the  European Research Council and Horizon 2020  Grant, contract No. 675440  ( European Union ); the  Leventis Foundation ; the A. P. Sloan Foundation; the  Alexander von Humboldt Foundation ; the  Belgian Federal Science Policy Office ; the  Fonds pour la Formation à la Recherche dans l'Industrie et dans l'Agriculture (FRIA-Belgium) ; the  Agentschap voor Innovatie door Wetenschap en Technologie  ( IWT-Belgium ); the  F. R. S. -FNRS  and  FWO (Belgium)  under the  "Excellence of Science -EOS" -be. h project n. 30820817; the  Ministry of Education, Youth and Sports (MEYS)  of the Czech Republic; the  Lend ület ("Momentum") Programme  and the  János Bolyai Research Scholarship of the Hungarian Academy of Sciences , the  New National Excellence Program ÚNKP , the  NKFIA  research grants  123842 ,  123959 ,  124845 ,  124850 , and  125105  (Hungary); the  Council of Science and Industrial Research, India ; the  HOMING PLUS programme of the Foundation for Polish Science , cofinanced from  European Union, Regional Development Fund , the  Mobility Plus programme of the Ministry of Science and Higher Education , the  National Science Center (Poland) , contracts Harmonia  2014/14/M/ST2/00428 ,  Opus 2014/13/B/ST2/02543 ,  2014/15/B/ST2/03998 , and  2015/19/B/ST2/02861 , Sonata-bis  2012/07/E/ST2/01406 ; the  National Priorities Research Program  by  Qatar National Research Fund ; the  Programa Estatal de Fomento de la Investigaci ón Científica y Técnica de Excelencia María de Maeztu , grant  MDM-2015-0509  and the  Programa Severo Ochoa del Principado de Asturias ; the Thalis and Aristeia programmes cofinanced by  EU-ESF  and the  Greek NSRF ; the  Rachadapisek Sompot Fund for Postdoctoral Fellowship, Chulalongkorn University  and the  Chulalongkorn Academic into Its 2nd Century Project Advancement Project (Thailand) ; the  Welch Foundation , contract  C-1845 ; and the  Weston Havens Foundation (USA).
Search for the Radio Pulsar at Parkes On 2018 September 14 th we observed the point-like source for 2700 seconds using the Directors Time of the ATNF Parkes radio telescope in NSW, Australia. The central beam of the multibeam receiver was used and data were recorded using the Parkes Digital Filterbank (PDFB) systems. We used a 2-bit sampling and a sampling time of 64 microsecond with 512 frequency channels over 256 MHz bandwidth (centred at 1369 MHz). The pulsar searching software package PRESTO  (Ransom 2001 ) was used to carry out RFI zapping and masking, de-dispersion and searches of periodic signals. We searched for dispersion measures (DMs) of up to 1000 cm -3 pc, but found no convincing candidates with a S/N greater than 8. For a pulse period of 10 ms and DM of 200 cm -3 pc and assuming a pulse duty cycle of 10 percent, our observations provide a flux density limit of 0.
DISCUSSION We explore two possible scenarios for the nature of this object. Namely: (i) A PWN associated with DEM S5: This is supported by (a) the detection of a radio point source coincident with the hard X-ray point source (PWN/pulsar composite), (b) an X-ray spectrum consistent with a power law with photon index typical as seen from PWN/pulsar spectra and the stability of the X-ray flux, (c) the radio spectral indices and (d) shocked IR emission. In the case of PWNe, the extent of the radio emission is generally greater than that in X-rays because of the longer cooling time of radio-emitting electrons. The radio emission may therefore trace the path of the PWN from the centre of the SNR as indicated by the current radio data of DEM S5 at 2100 MHz (Fig. 6 ). The detection of the cometary morphology in radio indicates a large kick velocity of the pulsar at birth.
ACKNOWLEDGEMENTS The  Australian Compact Array  and the  Australian SKA Pathfinder (ASKAP)  are part of the Australian Telescope which is funded by the  Commonwealth of Australia  for operation as National Facility managed by  CSIRO. This paper includes archived data obtained through the  Australia Telescope Online Archive  (http://atoa. atnf. csiro. au). We used the karma and miriad software packages developed by the  ATNF. Operation of ASKAP  is funded by the  Australian Government  with support from the  National Collaborative Research Infrastructure Strategy. ASKAP uses the resources of the  Pawsey Supercomputing Centre. Establishment of ASKAP , the  Murchison Radio-astronomy Observatory  and the  Pawsey Supercomputing Centre are initiatives of the Australian Government , with support from the  Government of Western Australia  and the  Science and Indus-try Endowment Fund.
We acknowledge the  Wajarri Yamatji people  as the traditional owners of the Observatory site. M. S. acknowledges support by the  Deutsche Forschungsgemeinschaft (DFG)  through the  Heisenberg research grant   SA 2131/4-1  and the  Heisenberg professor grant   SA 2131/5-1. This work is part of project No. 176005 , 'Emission nebulae: structure and evolution', supported by the  Ministry of Education, Science, and Technological Development of the Republic of Serbia. Parts of this research were conducted with support of  Australian Research Council   Centre of Excellence for All Sky Astrophysics in 3 Dimensions  ( ASTRO 3D ), through project number  CE170100013. The authors would like to thank the anonymous referee for a constructive report and useful comments.