dataesr/scientific-paragraphs-categorization huggingface dataset:
(  1 ), described in Section 6. 2] with the parameters determined from a fit to the observed m γ R γ R spectra in collision data. For each simulated sample of the benchmark scenario, with different values of m a and m X , separate tests are performed for an increasing number of injected signal events. The average of the number of events determined from the fit to multiple pseudo-datasets and the number inserted should be identical in an ideal case, and the difference between these two numbers is taken as a systematic uncertainty in the signal mass shape modeling. The fraction, f , of signal events that appear in the low-∆E category is parametrized as a function of the mass parameters m X and m a of the benchmark signal scenario, to have a continuous model for all the masses considered in the results.
Conclusion A search for pairs of highly collimated groupings of photons-photon-jets-that are identified as single, photonlike energy clusters in the EM calorimeter of the ATLAS detector at the LHC is presented. Data from proton-proton collisions at a center-of-mass energy of 13 TeV collected in 2015 and 2016, corresponding to an integrated luminosity of 36. 7 fb -1 , are used. Pairs of photon-jets can arise, for example, as the final-state decay products of a new high-mass resonance decaying via new light resonances into highly collimated groupings of photons. Candidate photon-jet events are initially selected with a loose diphoton trigger and then potential photon-jets are selected using a combination of variables that model EM shower development. Sensitivity to photon-jets is then increased by categorizing reconstructed photons by one of those shower shape variables and narrow resonances are searched for in the resulting mass distributions of two reconstructed photons.
In addition to the calculated upper limits for this benchmark signal scenario, the results, including the evaluation of the observed upper limits, are provided in HepData  [40]  in a largely model-independent way, to enable reinterpretation in the context of other signal models containing highly collimated photon-jets of low or high photon multiplicity. [40] ATLAS Collaboration, A search for pairs of highly collimated photon-jets in pp collisions at √ s = 13 TeV with the ATLAS detector. HEPData, Phys. Rev. (2018), : https://doi. org/10. 17182/hepdata. 85728. [41] ATLAS Collaboration, ATLAS Computing Acknowledgements, ATL-GEN-PUB-2016-002, : https://cds. cern. ch/record/2202407.
Acknowledgments We thank  CERN  for the very successful operation of the LHC, as well as the support staff from our institutions without whom ATLAS could not be operated efficiently. We acknowledge the support of  ANPCyT , Argentina; YerPhI, Armenia;  ARC, Australia ;  BMWFW  and  FWF , Austria; ANAS, Azerbaijan; SSTC, Belarus;  CNPq  and  FAPESP, Brazil ;  NSERC ,  NRC  and  CFI ,  Canada ; CERN; CONICYT, Chile; CAS,  MOST  and  NSFC, China ;  COLCIENCIAS, Colombia; MSMT CR, MPO CR  and  VSC CR, Czech Republic ;  DNRF  and  DNSRC, Denmark ;  IN2P3-CNRS ,  CEA-DRF/IRFU , France; SRNSFG, Georgia; BMBF,  HGF , and  MPG, Germany ;  GSRT, Greece; RGC, Hong Kong SAR, China ;  ISF, I-CORE  and  Benoziyo Center , Israel; INFN, Italy;  MEXT  and  JSPS, Japan ; CNRST, Morocco; NWO, Netherlands; RCN, Norway;  MNiSW  and  NCN , Poland; FCT, Portugal; MNE/IFA, Romania;  MES of Russia  and  NRC KI , Russian Federation; JINR; MESTD, Serbia; MSSR, Slovakia; ARRS and MIZŠ, Slovenia; DST/NRF, South Africa; MINECO, Spain;  SRC and Wallenberg Foundation, Sweden ;  SERI ,  SNSF  and  Cantons of Bern and Geneva, Switzerland; MOST, Taiwan ;  TAEK, Turkey; STFC, United Kingdom ;  DOE  and  NSF ,  United States of America.
These findings not only provide a key missing link for collisionless shock research but also contribute to understanding physics in other The red shaded region marks a large difference in the shock ramp between C3 and C4. The structure in (B) is evidence that the shock ramp substructure varies over electron scales, because features in this dataset are dictated by the inter-spacecraft separation of 7 km. We have marked the spatial length scales of the ramp and the substructure (see the Materials and Methods section for how these lengths were derived). (C to E) Hodograms derived from the application of minimum variance analysis to the magnetic field differences in the shock frame. The variations appear elliptically polarized and propagate almost parallel to the shock normal, consistent with whistler waves on the predicted scales of the GC model of shock front reformation  (17)  (see the Materials and Methods section for technical details of the hodograms).
Acknowledgments Funding: M. A. B. and S. N. W. are grateful to the  STFC  (grant  ST/N002865/1 ). A. P. D. and T. I. P. were funded by the  Academy of Finland  (grant nos. 288472  and  267073/2013 ). Y. V. K. was supported by the  Swedish Research Council  (grant no. 2016-05507 ). V. K. acknowledges the financial support from  CNES  through the grant " Stereo S-Waves & Wind Invited Scientist. "M. G. was supported in part by the  Israel Science Foundation  (grant no. 368/14 ). C. T. R. was supported through  NASA's Magnetospheric Multiscale mission. A. P. D. was supported by the  Swedish Civil Contingencies Agency (MSB)  (grant no. 2016-2102 ). C. C. acknowledges the  Cluster FGM  (grant no. ST/P003427/1 ) from  UKSA/STFC. N. G. acknowledges financial support from  NASA  grant  80NSSC17K0015  and  NSF  grant  1663770.
e. , the full region labeled DECaLS in Figure  1 ). The goal is to complete this survey in the 2019A semester. The Legacy Surveys program also makes use of other DECam grz data within the DESI footprint, as those data become public. The most significant of these other data sets is from the Dark Energy Survey, which includes a 1,130 deg 2 contiguous area in the SGC footprint of the Legacy Surveys. DECaLS is therefore not re-observing that area, and is instead making use of the DES raw data as they become public. Data from the early DECam science verification period have a number of problematic features, and are not currently included in the reductions or data releases from the Legacy Surveys.
DATA REDUCTION AND CALIBRATIONS All data from the Legacy Surveys are first processed at NOAO/Tucson through the NOAO Community Pipelines ("CPs"). Each instrument and telescope combination has its own CP that takes raw data as an input and provides detrended and calibrated data products. The NOAO Pipeline Scientist and architect is co-author F. Valdes, who is responsible for the development and continued operation of the CPs. The CPs include algorithms and code (from a variety of sources, the key ones being code developed by DES Data Management, the TERAPIX suite, and IRAF;  Valdes et al. (2014) ;  Bertin & Arnouts (1996) ;  Bertin (2011) ;  Bertin et al. (2002) ;  Tody (1986) ) which are modified and packaged for the needs of the NOAO environment and characteristics of the different instruments.
Data products delivered to the NOAO Science Archive include flux calibrated images (i. e. , individual images with and without distortion corrections applied, and image stacks), bad data masks, and weight maps. The three cameras used by the Legacy Surveys (i. e. , DECam, Mosaic-3, and 90Prime) each have their own CP. The basic steps of each CP are summarized in Table  5. Detailed technical descriptions of each CP are in preparation 9   (Valdes et al. 2014 , describes an early version of DECam CP). The CP for the DECaLS data evolved from the Dark Energy Survey pipeline such that it has algorithms and code from several sources. The key sources are code developed by DES Data Management, the TERAPIX suite, and IRAF  (Valdes et al. 2014; Bertin & Arnouts 1996; Bertin 2011; Bertin et al. 2002; Tody 1986 ).
Astrometric Calibration The NOAO CP reductions of all Legacy Survey imaging data derive a world coordinate system (WCS), a function mapping pixel coordinates to celestial coordinates. The function (TPV: tangent plane projection with polynomial distortions 10  ) is determined for each CCD by least square fitting to the pixel centroids of detected sources with known coordinates in a reference catalog. For the astrometric solution, the pixel centroids of reference stars are computed using intensity weighted means using Source Extractor  (Bertin & Arnouts 1996)  in the DECam CP, and using the ACE package in IRAF  (Valdes 2001; Tody 1986 ) in the Mosaic-3 and 90Prime CPs. The final source positions in the catalogs are computed using the Tractor, as described in section 8. The reference coordinates were from the 2MASS catalog  (Skrutskie et al.
The mid-infrared photometry for each optically-detected source is then determined by forcing the location and shape of the model, convolving with the WISE PSF and fitting to the WISE stacked image. This "forced photometry" approach allows us to deblend any confused WISE sources by using the higher-spatial-resolution optical data, but also limits the Legacy Surveys catalogs to only contain WISE photometry for sources that are detected at optical wavelengths. The procedure described produces object positions, fluxes and colors that are consistently measured across the three Legacy Surveys. Figure  7  shows examples of how The Tractor is being applied to the Legacy Surveys. The footprint of the Legacy Surveys is divided into "bricks" of size 0. 25 • ×0. 25 • , and a model of the sky within each brick is computed using all CCDs that contribute data within that brick.
The three sets of vertical panels show: the grz image data for a brick; the rendered The Tractor model; and the residual image (i. e. , datamodel). While most of the faint sources are well fit by the parametric models we used for the Legacy Surveys, more significant residuals are seen associated with very extended galaxies and the halos of bright, saturated stars. The Tractor and our source detection algorithms do result in the catalog containing a small fraction of spurious sources. These are primarily due to inadequately masked particle events or satellite trails, single-exposure detections of transient sources (primarily asteroids), and sources identified in the extended scattered light halos or diffraction spikes associated with bright stars, or in the diffuse emission associated with large galaxies.
However, we are also able to measure the fluxes of significantly fainter objects, as well as study collections of objects that are blended in the WISE images but that are resolved in the optical images. The increased level of source counts in the force-photometered data observed at bright WISE magnitudes (i. e. , W 1 16 mag) in the right panel of figure  8  is due to sources detected in the vicinity of bright stars or galaxies; ≈50% of these sources are real objects, Readers can explore the data, models and residual images in more detail using the Legacy Surveys Imagine sky viewer at http://legacysurvey. org/viewer and the remaining are spurious detections due to the halos or diffraction spikes around bright stars or the poorly-modeled extended light of galaxies. All are located near other brighter targets, which is why they are compromised.
We are currently working on improving the models for future data releases. Figure  9  compares a traditional optical-infrared color-color diagram, based on matching sources between catalogs at different wavelengths, to the photometry derived from our WISE forced photometry, which requires no such matching. This demonstrates how The Tractor greatly increases the access to mid-infrared photometry for targets fainter than the AllWISE catalog detection limits, albeit with increased scatter. We have verified the reliability of the forced photometry detections and measurements by comparing The Tractor catalog results with those from deep Spitzer data in the COSMOS field (i. e. , the S-COSMOS catalog from  Sanders et al. 2007). Defining reliability as the fraction of Spitzer sources recovered, we find that the reliability is ≥95% for sources with W1 or W2 signal-to-noise ratios of ≥ 5, corresponding to 21.
We have implemented an automated observing strategy for all surveys, where observing conditions are monitored in near-real time and exposure times are modified and target field selection is optimized on-the-fly to ensure that each individual observation reaches the required depth. This strategy ensures that the ground-based surveys produce datasets that are as uniform as possible. The data are pipeline processed using the NOAO Community Pipelines, and catalogs are then generated from the imaging data using an inference-based forward modeling approach known as The Tractor, implemented at NERSC. All the imaging data, source catalogs, and code from the Legacy Surveys are publicly available: the raw and pipeline-processed optical imaging data are made public as soon as they are available in the NOAO Archive and catalogs from the project are released approximately twice each year.
This research used resources of the  National Energy Research Scientific Computing Center , a  DOE Office of Science User Facility  supported by the  Office of Science of the U. S. Department of Energy  under Contract No. DE-AC02-05CH11231. The research leading to these results has received funding from the  European Research Council  under the  European Union 's  Seventh Framework Programme  ( FP/2007-2013 ) / ERC Grant Agreement n. 320964  (WDTracer). J. Moustakas  gratefully acknowledges support from the  National Science Foundation  grant  AST-1616414. A. Dey  thanks the  Radcliffe Institute for Advanced Study  for their generous support during the year these surveys were initiated. A. Dey ,  D. J. Schlegel , and  D. Lang  thank the  Aspen Center for Physics , which is supported by  National Science Foundation  grant  PHY-1066293 , for their hospitality and support during summer 2015 during which part of this work was conducted.
As detailed in the bottom row of the figure, there is a clear amplitude asymmetry due to the blocking of dead DM actuators. This odd amplitude component A odd , combined with the even phase θ even that cancels the effect of the asymmetry in the dark holes, results in the real focal-plane electric field that will be used to probe even pupil-plane phase aberrations. Approximately 3. 5 % of the focal plane power is in the real electric field and therefore available to sense even phase aberrations. Simulations are performed with the HCIPy package  (Por et al. 2018 ), an open-source software for high-contrast imaging simulations that is available on GitHub 1. The simulations are monochromatic (λ=1550 nm). They sample the pupil-plane with 256×256 pixels and use the Fraunhofer approximation to propagate the electric field to the focal-plane, which is sampled with 150×150 pixels for 3 pixels per λ/D.
SCExAO The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument  (Jovanovic et al. 2015 ) is a high-contrast imaging instrument at the Subaru Telescope. It operates downstream of the AO188 system (Minowa et al. 2010), which gives an initial, loworder correction. SCExAO drives a 2000-actuator deformable mirror (DM) based on wavefront measurements from a pyramid wavefront sensor (PYWFS) in the optical -NIR (600-900 nm) that can run at 3. 5 kHz, but most often runs at 2 kHz. There are 45 actuators across the pupil, giving the system the ability to correct out to 22. 5λ/D. The real-time control of SCExAO is handled by the compute and control for adaptive optics (cacao) package  (Guyon et al. 2018). Cacao allows for NCPA corrections to be handled by a separate DM channel, where the software automatically sends offsets to the PYWFS.
Acknowledgements. The authors thank the referee for comments on the manuscript that significantly improved the presentation of the work. The authors warmly thank  S. Y. Haffert  and  E. H. Por  for useful discussion on focal-plane wavefront sensing. The research of  Steven P. Bos ,  David S. Doelman , and  Frans Snik  leading to these results has received funding from the  European Research Council  under  ERC Starting Grant  agreement  678194  (FALCONER). The development of SCExAO was supported by the  JSPS  ( Grant-in-Aid for Research # 23340051 , # 26220704 , # 23103002 ), the  Astrobiology Center (ABC)  of the  National Institutes of Natural Sciences, Japan , the  Mt Cuba Foundation  and the directors contingency fund at Subaru Telescope. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community.
Introduction The search for heavy charged long-lived particles presented in this paper is based on a data sample of 36. 1 fb -1 of proton-proton (pp) collisions at √ s = 13 TeV collected in 2015 and 2016. It utilizes observables related to large ionization energy loss (dE/dx) and time of flight (ToF), which are signatures of heavy charged particles traveling significantly slower than the speed of light. The mass of the particles is estimated using the dE/dx (m dE/dx ) or ToF (m ToF ) measurements together with the reconstructed momentum. The background is estimated in a purely data-driven manner, and multiple signal regions are defined to address the different possible signatures of heavy long-lived particles (LLPs) that reach at least the ATLAS hadronic calorimeter, which corresponds to decay lengths of a few meters.
Typically, the energy deposit in the calorimeters is less than 10 GeV. All simulated events included a modeling of contributions from pileup by overlaying minimum-bias pp interactions from the same (in-time pileup) and nearby (out-of-time pileup) bunch crossings simulated in P 8 (version 8. 186) and EvtGen (version 1. 2. 0) with the A2  [51]  tune and MSTW2008LO [52] PDF set. The simulated events were reconstructed using the same software used for collision data, and were reweighted so that the distribution of the number of collisions per bunch crossing matched that of the data.
The ANTARES detector is an abyssal undersea neutrino telescope in the Mediterranean Sea. The search for point-like neutrino sources is one of the main goals of ANTARES, so a reliable way to evaluate the detector angular resolution and pointing accuracy is needed. In a previous analysis, the deficit in the atmospheric muon flux in the direction of the Moon induced by absorption of cosmic rays was investigated. It has allowed the estimation of the angular resolution and of the pointing accuracy of the detector. In this work the same approach was applied to measure the Sun shadow effect. This analysis is based on the ANTARES data taken in the interval between 2008 -2015. According to Monte Carlo simulation the expected statistical significance of the analysis is 2. 9σ.
Introduction The ANTARES undersea neutrino telescope is currently in operation for more than 10 years  [1]. The main goal of the telescope is to detect neutrino point-like sources, so it is critically important to correctly estimate the angular resolution and the pointing accuracy of the telescope. One of the methods to evaluate the angular resolution is based on the detection of the so-called "Moon and Sun shadow". The shadow is the atmospheric muon flux deficit in the region around the celestial object due to its absorption of primary cosmic rays. A similar measurement has been performed by several Collaborations: CYGNUS  [2] , TIBET  [3] , CASA  [4] , MACRO  [5] , SOUDAN  [6]  , ARGO  [7]  and also IceCube  [8]. The measurement of the Moon shadow with ANTARES was published in  [9]. In this proceeding we report the preliminary results of the Sun shadow analysis using the ANTARES 2008-2015 data sample, corresponding to a total live-time of around 2800 days.
Sun-shadow 1D profile distribution and angular resolution estimation The reconstructed events from the 2008-2015 ANTARES data sample have been selected with the optimized cuts described above and the muon density close to the Sun region is derived. The events were binned using concentric rings around the Sun centre up to an angular distance of 10 • with bin size of 0. 4 •. The muon density versus the distance from the Sun is presented in Fig. 3. The muon deficit is clearly visible close to the nominal Sun position. For the estimation of the angular resolution, the Sun shadowing effect is assumed to follow a Gaussian distribution with standard deviation σ res , which is the detector angular resolution itself  [9]. A similar approach has already been followed by  [5, 8]. The number of expected events is evaluated by fitting the distribution in Fig.
Conclusions In this work the analysis of the Sun shadow effect was performed based on the 2008-2015 ANTARES data sample, corresponding to a total live-time of around 2800 days. The expected value of the statistical significance for the ANTARES Sun shadow analysis is 2. 9σ. The data sample shows a clear deficit in the region close to the nominal Sun position and the estimated detector angular resolution for atmospheric downward-going muons is σ res = 0. 99 • ± 0. 34 •. The angular resolution value is compatible to the Moon shadow analysis result at 1σ level. A larger statistical significance for the Sun shadow will be possible by increasing the data sample with events from the latest reconstructed runs (up to 2017). With such an improved statistics the study of the detector pointing performance will be then more effective obtaining the 68%, 90% and 95% CL contours of the Sun Shadow in the field of view around the expected direction of the Sun.
Introduction The joint production of three vector bosons is a rare process in the Standard Model (SM). Studies of triboson production can test the non-Abelian gauge structure of the SM theory and any deviations from the SM prediction would provide hints of new physics at higher energy scales  [1] [2] [3] [4]. Triboson production has been studied at the Large Hadron Collider (LHC) using proton-proton (pp) collision data taken at √ s = 8 TeV for processes such as γγγ  [5] , W γγ  [6, 7] , Zγγ  [7, 8] , WW γ and W Zγ  [9, 10] , and WWW  [11]. This letter presents the first evidence for the joint production of three massive vector bosons in pp collisions using the dataset collected with the ATLAS detector between 2015 and 2017 at √ s = 13 TeV. At leading order (LO) in quantum chromodynamics (QCD), the production of three massive vector bosons (VVV, with V = W, Z) can proceed via the radiation of each vector boson from a fermion, from an associated boson production with an intermediate boson (W, Z/γ * or H) decaying into two vector bosons, or from a quartic gauge coupling vertex.
Conclusion In conclusion, a search for the joint production of three massive vector bosons (W or Z) in proton-proton collisions using 79. 8 fb -1 of data at √ s = 13 TeV collected by the ATLAS detector at the LHC, is presented. Events with two, three or four reconstructed electrons or muons are analysed. Evidence for the production of three massive vector bosons is observed with a combined significance of 4. 1 standard deviations, where the expectation is 3. 1 standard deviations. The measured production cross sections are σ WWW = 0. 65 The crucial computing support from all WLCG partners is acknowledged gratefully, in particular from CERN, 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), the Tier-2 facilities worldwide and large non-WLCG resource providers.