dataesr/scientific-paragraphs-categorization huggingface dataset:
Discussion We generated a nomogram aimed at predicting PG overdose based on early predictors calculated on the planning CT dataset and on a CT performed in the first week of treatment. In total, 14 of the 16 patients with a calculated mean PG overdose of 2. 5Gy were identified by the nomogram. All patients with a PG overdose >2. 5Gy were identified. Weekly replanning of these 14 targeted patients enabled the mean PG dose to be decreased by 3. 9Gy compared to the cumulated delivered dose, corresponding to an 8 % decrease in the estimated absolute xerostomia risk. Due to anatomical variations occurring during the course of IMRT, some PGs can receive doses exceeding the planned dose (overdose). In an attempt to prevent this, ART is designed to take these anatomical variations into account by generating one or several new plannings.
Acknowledgments This collaborative effort was supported by the  European Science Foundation  through the  Research Networking Program : Thunderstorm effects on the atmosphere-ionosphere system (TEA-IS). Z. B. acknowledges support from the  Czech Science Foundation  Research Projects No. 15-04023S  and No. LO1411  ( NPU I ) funded by the  Ministry of Education, Youth and Sports of the Czech Republic. This work has been done partially within the  LABEX Plas@par  project and has received financial state aid managed by the  Agence Nationale de la Recherche  as part of the  programme "Investissements d'avenir"  under the reference  ANR-11-IDEX-0004-02. The authors also acknowledge helpful discussions with  S Celestin  and  N Lehtinen  and are grateful to  S Biagi  for access to the cross-sectional database used in the code MAGBOLTZ.
We report results from simultaneous radio and X-ray observations of PSR B0611+22 which is known to exhibit bursting in its single-pulse emission. The pulse phase of the bursts vary with radio frequency. The bursts are correlated in 327/150 MHz datasets while they are anti-correlated, with bursts at one frequency associated with normal emission at the other, in 820/150 MHz datasets. Also, the flux density of this pulsar is lower than expected at 327 MHz assuming a power law. We attribute this unusual behaviour to the pulsar itself rather than absorption by external astrophysical sources. Using this dataset over an extensive frequency range, we show that the bursting phenomenon in this pulsar exhibits temporal variance over a span of few hours. We also show that the bursting is quasi-periodic over the observed band.
OBSERVATIONS All observations were carried out on MJD 56756. PSR B0611+22 was observed at three different radio frequencies including 327 MHz (Arecibo Observatory), 820 MHz (Green Bank Telescope) and 150 MHz (International LOFAR station-Nançay, France). The observation configurations for the radio telescopes are given in Table  1. The data were recorded and converted into multi-channel filterbank format before being written out to disk. Then, the data were incoherently dedispersed using PRESTO 1  at the pulsar DM of 96 pc cm -3 to remove the dispersion delay of incoming radio waves due to the interstellar medium. For the LOFAR (FR606) data, coherent dedispersion was carried out using DSPSR 2  (van  Straten et al. 2011). Simultaneously, the pulsar was observed by XMM-Newton. The XMM-Newton observations used the photon imaging camera (EPIC)  (Strüder et al.
We applied the same smoothing to each dataset to give them comparable resolution. To ensure time alignment, we removed dispersion delay for each telescope using infinite frequency as the reference. The timeseries for each dataset were barycentered to remove any time delays due to different locations of the telescopes. By doing this, we were able to obtain snippets of datasets where we could study the bursting behaviour simultaneously at different radio frequencies. Figure  5  clearly shows enhanced emission to study broadband correlations. The emission exhibits a change in its behaviour going from 820/150 MHz observations to 327/150 MHz observations. The direction of phase shift during bursting is different at 327 and 820 MHz when compared to their corresponding 150 MHz datasets. The correlation in 327/150 MHz and the anti-correlation in 820/150 MHz of the bursting is evident in Fig.
4  which shows the cross-correlations between the two frequencies. Fig. 4  reveals a slight offset in the maximum of the 327/150 MHz (∼60 bins) and the minimum of the 820/150 MHz (∼50 bins) plot from the zero lag. Since the offsets are comparable to the kernel width used to smooth the datasets along the time axis, they are insignificant and most likely not intrinsic to this phenomena. We divided the time series into sections with no bursting and where bursting was clearly evident. The sections were selected visually from the smoothed data. From these sections, average profiles were created by summing the energies over the phase bins where the pulsed emission was seen. The profiles clearly bring out the difference in the behaviour of bursting at both frequencies. The profile for the bursting pulses is phase shifted in pulse longitude at the two frequencies as reported by  Seymour et al.
To calibrate the observed flux, we have used software described in detail by  Kondratiev et al. (2016). The software produces flux density scaling factor using Eq 1 for each pulse and frequency channel. In order to properly estimate G and Tsys, the software makes use of the Hamaker beam model  (Hamaker 2006)  and mscorpol 3 by Tobia Carozzi to calculate Jones matrices of the HBA antenna response for 3 https://github. com/2baOrNot2ba/mscorpol a given frequency and sky coordinates. The HBA antenna temperature, TA, is derived from CasA measurements done by  Wijnholds & van Cappellen (2011). The background sky temperature, T sky , is taken from a sky map at 408 MHz by  Haslam et al. (1982) , scaled to the HBA frequency as ν -2. 55  (Lawson et al. 1987). The error on the flux density calculation is 50% and can be attributed to e.
Broadband flux density modulation To quantify the variation in the detected flux from the pulsar, we estimated the modulation index at different frequen-   cies. Modulation index is a measure of pulse to pulse intensity fluctuation. To derive the intrinsic modulation indices (mint) we used the method described in  Kramer et al. (2003). First, we estimated the flux of each of the observations. Since we did not have calibrator observations, we used the radiometer equation  (Lorimer et al. 2012 ) to obtain flux densities at different frequencies. Then, we normalized the time series by a 200 s running median to correct the pulsar signal for any possible effects of interstellar scintillation. Finally, the datasets were re-scaled to be consistent with the initial average flux density. For every observation, we integrated individual pulses to obtain the average pulse profile and calculated its flux density (see Table  2 ).
After correcting the datasets for the effects of interstellar scintillation, for each one, we calculated the intrinsic modulation index m 2 int = (S -S ) 2 S 2 , (2) where, S is the mean flux density and S is the measured flux density of a single pulse. We compared our results with results for other pulsars  (Bartel et al. 1980; Kramer et al. 2003). It is clearly seen that mint decreases with frequency until a certain "cut off" frequency and rises again (see Fig. 8 ). Our results are consistent with other pulsars where a similar trend is observed  (Maron et al. 2013).
X-ray flux upper limits We observed PSR B0611+22 for 33 ks using XMM Newton. We observed the pulsar using both PN CCD and MOS camera mounted on the telescope. We did not detect the pulsar but obtained an upper limit on the X-ray flux using the method described in  Lorimer et al. (2012). We obtained an upper limit on the count rate of ∼ 5×10 - 4  counts s -1 at 99% confidence level. Then, assuming a nonthermal emission from the pulsar with a photon index Γ ≈ 2  (Pavlov et al. 2009 ) and using the publicly available software WEBPIMMS 4 , we obtained a limit on the unabsorbed X-ray flux, F unabs 0. 3-8 keV of∼2. 7 × 10 -15 ergs cm -2 s -1 assuming a neutral hydrogen column density NH of 3. 1 × 10 21 cm -2 , estimated using 10% ionization fraction. The obtained upper limit is less than the flux reported for PSR B0943+10 (Hermsen 2013) using the same non-thermal Figure  7.
Though PSR B0611+22 seems to be a mode changing pulsar, the frequency dependence of the mode change is not explained by current mode changing models and observations  (Rankin 1983). Kern (2000)  claims that phase offset in the bursting profile occurs due to the periodic existence of a conal component along with the core component. Though the model is able to explain the slight increase in the width of the pulse profile in bursting mode, it fails to account for the different direction of phase offset at different frequencies. The observations presented here suggest that the spectral indices of the two components are different. Therefore, if the components preserve their phase, this manifests itself as an anti-correlation in the two simultaneous datasets We intend to do follow-up observations with a wider frequency coverage before making any claims on the model of emission of this pulsar.
CONCLUSIONS We have carried out a detailed analysis of simultaneous radio and X-ray observations of pulsar PSR B0611+22. The multi-frequency data reveal a wealth of information about the emission characteristics of this pulsar. The bursting behaviour varied across the radio band with a quasi-periodic characteristic at all frequencies. The 327/150 MHz and 820/150 MHz simultaneous observations show an anticorrelation in bursting. We leave modeling this unusual behaviour to a later paper. Future polarimetric studies of both modes will help in discerning the emission physics of this pulsar. Moreover, we obtained a flux density spectrum from the radio observations of this pulsar. The spectrum shows a turnover at higher frequencies. We considered free-free thermal absorption by the surrounding ISM as a possible explanation but such model cannot explain the flux density at 150 MHz.
ACKNOWLEDGEMENTS We thank our referee for useful comments that greatly improved the manuscript. This work was supported by a  NASA XMM-Newton  grant (award no. 74279 ). We thank  West Virginia University  for its financial support of GBT operations, which enabled some of the observations for this project. We thank the staff of LOFAR station, Nançay, France for the observations. The financial assistance of the South African  SKA  project ( SKA SA ) towards this research is hereby acknowledged. Opinions expressed and conclusions arrived at are those of the authors and are not necessarily to be attributed to the SKA SA.
Summary The HST and its suite of instruments have inevitably set the standard for UV and visible astronomy from space. Conceived as a general-purpose observatory, it has been able to study a wide variety of scientific goals by providing diffraction-limited imaging and spectroscopy from low to high resolution across a wavelength range from the far UV to the near-infrared. In its current configuration, the telescope has an efficient capability that continues to deliver exciting new discoveries. However, the exploration of exoplanetary systems will require a factor of 30 to 50 increase in effective area with respect to HST and reach the best possible angular (<10 mas). Such a capability will also produce a revolution in the study of astrophysical disks and jets. Furthermore, the implementation of a few carefully selected instruments will allow collection of the data needed to understand the physics behind planet formation, planetary atmospheric stability and evolution, the interaction between the components of planetary systems and the census of the metallic compounds.
Purified N 2 was then introduced in a static mass spectrometer where masses 28 and 29 were analysed on a Faraday cup detector and masses 29 and 30 were counted on an electron multiplier  (Humbert et al. , 2000). Potential CO contamination, checked with the measured 29/30 ratio, was found to be always negligible. The abundances of nitrogen and the 15 N/ 14 N ratios were then computed from the data and from runs with our in-house N 2 standard (purified atmospheric N 2 ). Blanks were found to be less than 0. 1 % of the signals for all runs. Errors on the isotopic ratios are computed from the standard deviation of in-house N 2 standard runs and from the internal precision of the respective sample runs. Nitrogen metal/silicate partition coefficients D N metal/silicate were calculated according to D N metal/silicate = C N metal /C N silicate , where C N metal and C N silicate are the nitrogen concentrations in the liquid Fe-rich metal and silicate melt, respectively.
Acknowledgments We thank  Daniel Baumann ,  Micha Berkooz ,  Ulf Danielsson ,  Emilian Dudas ,  Anatoly Dymarsky ,  Mariana Graña ,  Stanislav Kuperstein ,  Emil Martinec ,  Stefano Massai ,  Praxitelis Ntokos ,  Giulio Pasini ,  Joe Polchinski ,  Andrea Puhm ,  Rodolfo Russo , and  Thomas Van Riet  for useful discussions. This work was supported by the  John Templeton Foundation  Grant  48222. The work of I. B. was also supported by the  ERC   Starting Grant 240210 String-QCD-BH , and by a grant from the  Foundational Questions Institute (FQXi) Fund , a donor advised fund of the  Silicon Valley Community Foundation  on the basis of proposal FQXi- RFP3-1321  (this grant was administered by  Theiss Research). The work of J. B. and D. T. was also supported by the  CEA Eurotalents program.
This list is far from being exhaustive, and this type of data is ever less frequently considered by its owners to be personal. The rights to access personal data, required by the simple smartphone 'app' of a public transport provider (i. e. RATP Paris, version 2014), are food for thought on the erosion of the notion of ''private life''. In order to take advantage of a service as simple as the suggestion of subway itineraries, the user must authorise access to the status and identifier of the telephone, to its GPS position, to its address book, to data storage (reading and writing), to all networks, and must authorise the creation or suppression of user accounts, control of the telephone's vibrator and sleepmode system, as well as its synchronisation parameters. In this context, it is not surprising that the question of behavioural and societal prediction has become one of the new Eldorados of the digital economy.
), the NSA has created a hitherto unimaginable database on the state of human activities, which is updated almost in real time. This database, together with the methods that will be developed to harness its information, perhaps embody the ultimate horizon of what an ''external'' viewpoint of our societies could be. The extent of the NSA's spying activities created a shock, since it indiscriminately reduced to ashes any notion of private life for both American residents and the rest of the world. However, the most perturbing fact is perhaps that the means used by the NSA appear to be disproportionate, or even inadequate, in view of their justification. The latter states that it requires all of these data in order to prevent a second September 11. In order to find a needle in a haystack, access to the entire haystack would be required.
g. , at the target entrance or close to the end of the ion path). The collimator was made of a tungsten alloy with a 4-mm slit opening and, when applicable, the shielding consisted of lead blocks. Two setups were considered. The data of the first setup (setup 1) were collected by means of a LYSO detector, while in the second one (setup 2), the LYSO and LaBr 3 detectors were used. A schema of setups 1 and 2 can be observed in Figures  1  and 2 , respectively. In order to select the prompt gammas from the extensive background, the time-of-flight (TOF) technique was used in conjunction with a VME-based acquisition system with NIM modules and discrete logic and analogic electronics. The TOF windows applied during the analysis were always sufficiently large to include all the visible prompt-gamma events.
The TOF stop signal was given by the high-frequency (HF) signal of the cyclotron running in pulsed mode. The stop signal was actually provided by a discriminator converting the HF signal into a digital logic one whose frequency was divided by a factor of ~5 with respect to the HF frequency to cope with the time-to-amplitude (TAC) module limitations. The TOF spectra measured in these conditions correspond therefore to ~5 periods of the HF signal. The circular beam spot was around 5 mm sigma at isocenter, considering a Gaussian spatial beam distribution  (18). Energy thresholds were also applied to the data in order to reduce the background component. The energies considered were obtained after calibration with gamma sources. Therefore, it is an absorbed gamma-equivalent energy but, for the sake of simplicity, it will be simply referred to as energy.
Comparison between Experimental and Simulated Data The Geant4 benchmarking included two endpoints, arguably the two most relevant ones: yields and information correlated with the ion range. The former has an impact on, for example, camera optimization, while the latter plays a major role in a monitoring scenario. The yields were assessed using the reference model and comparing its outcomes with the experimental data. The discrepancy was then evaluated by computing the average relative difference between selected simulated and experimental data points. The rationale for such a selection was the need to avoid high-gradient signal regions since they could have a significant and misleading impact on the calculation of the relative difference due to spatial uncertainties. Therefore, the points considered were between 20 mm (to avoid the entrance of the target positioned at 0 mm -see, e.
ACKNOWLEDGMENTS The present work was performed in the framework of  FP7-ENTERVISION network  (Grant Agreement number  264552 ),  FP7-ENVISION programme  (Grant Agreement number  241851 ),  LabEx PRIMES   ANR-11-LABX-0063/ANR-11-IDEX-0007 ,  ETOILE's research programme (PRRH)  at  Université Claude Bernard Lyon 1 (UCBL) , and  France Hadron  ( ANR-11-INBS-0007 ). We would also like to acknowledge  IBA  for providing the nozzle details of the system installed at the clinical facility WPE,  Essen  and for hosting the experiment there. Finally, we gratefully acknowledge  IN2P3 Computing Center (CNRS)  for providing a significant amount of the computing resources and services needed for this work.
Computation of nonadiabatic couplings between excited states is described in the next section. To analyze the distortions of thymine's ring during dynamics, we computed the Cremer-Pople parameters  [26]  and classified them into conformations according to Boeyens' scheme  [39]. All ADC(2) computations were done with TURBOMOLE  [40]. Spectrum and dynamics were computed with the NEWTON-X/TURBOMOLE interface  [41, 42]. Intersection point optimizations were done with an in-house modified version of CIOpt program  [43]. Cremer-Pople parameters were obtained using the PLATON program  [44].
Acknowledgments:  Ljiljana Stojanović ,  Shuming Bai , and  Mario Barbatti  thank the support of the  Aix-Marseille Initiative d'Excellence (A*MIDEX ) grant (No. ANR-11-IDEX-0001-02 ) funded by the  French Government "Investissements d'Avenir" program  supervised by the  Agence Nationale de la Recherche. This work was granted access to the  HPC resources of Aix-Marseille Université  financed by the project  Equip@Meso  ( ANR-10-EQPX-29-01 ) also within the  "Investissements d'Avenir" program. Artur F. Izmaylov  acknowledges funding from a  Sloan Research Fellowship  and the  Natural Sciences and Engineering Research Council of Canada (NSERC)  through the  Discovery Grants Program.
Acknowledgments -We would like to thank  Michele Caselle ,  Beatrice Conti ,  Davide Fioravanti ,  Ferdinando Gliozzi ,  Simone Piscaglia  for useful discussions, and especially  Sergei Dubovsky ,  Victor Gorbenko ,  Marco Meineri  and  Davide Vadacchino  for clarifying discussions on issues related to effective string theories. We are also very grateful to  Fedor Smirnov  and  Sasha Zamolodchikov  for comments and encouragement at various points, and for sharing with us a copy of their paper " On space of integrable quantum field theories " [52] before publication. The research leading to these results has received funding from the  People Programme  ( Marie Curie Actions ) of the European Unions Seventh Framework Programme FP7/2007-2013/ under REA Grant Agreement No 317089 (GATIS), and was partially supported by  INFN  grant  FTECP  and the  UniTo-SanPaolo  research grant Nr  TO-Call3-2012-0088  " Modern Applications of String Theory " (MAST).
Acknowledgments This work has been supported by  ESI GROUP  through the ECN-ESI Chair on advanced modeling and simulation of materials, structures and processes as well as by the  Spanish Ministry of Economy and Competitiveness  through Grants Number  CICYT DPI2014-51844-C2-1-R  and  DPI2015-72365-EXP  and by the  Regional Government of Aragon  and the  European Social Fund , Research Group  T88.
After washing in water, the samples were left to dry in air. They were imaged using a Zeiss AxioZ2 microscope (using Metafer Isis software) to obtain visible light and optical fluorescence images for reference and correlation with the X-ray results. For X-ray imaging, several silicon nitride membranes were prepared with the same sample material. The resulting samples were found to contain a large number of intact nuclei, but also chromosome spreads and individual chromosomes from burst nuclei. Some of the membrane-bound samples were stained with platinum blue  (Wanner & Formanek, 1995) , at 5 mM for 30 min and washed in water. No significant differences were found in the X-ray phase contrast images; however, the Pt X-ray fluorescence M-line-signal was found to strongly interfere with the fitting of the X-ray fluorescence spectra due to overlap with the P K-lines.
Acknowledgements This work was supported by a  BBSRC   Professorial Fellowship   BB/H022597/1  ' Diamond Professorial Fellowship  for imaging chromosomes by coherent X-ray diffraction'. Additional support came from  EPSRC  grant  EP/I022562/1 , 'Phase modulation technology for X-ray imaging'. We thank  ESRF  for beam time and hospitality during the measurements in the framework of proposal ls2399. Work at  Brookhaven National Laboratory  was supported by the  US Department of Energy, Office of Science, Office of Basic Energy Sciences , under Contract  DE-SC00112704.
Introduction Identification of jets originating from b-quark fragmentation (b-tagging) plays an important role in physics programs at the LHC. In particular, it is essential for many physics analyses such as property measurements of the top quark, searches for the Higgs boson decaying to a b-quark pair (H → b b), and searches for new physics phenomena which are expected to have b-quark(s) in their final state. In this proceedings article, we report the current status of b-tagging performance in the ATLAS experiment  [1]  at the LHC. The tagging efficiencies of b-, c-, and lightjets 1 are measured using data collected by the ATLAS experiment during the LHC Run 1. In the following sections, the term "7 (8) TeV dataset" is used to refer to the dataset corresponding to an integrated luminosity of 4.
6 (20. 3) fb -1 collected in the year 2011 (2012) at a center-of-mass energy of 7 (8) TeV. The b-tagging algorithms are reviewed in section 2. Novel methods to derive the tagging efficiency of band c-jets from data, a process referred to as calibration, are presented in sections 3 and 4. Updated calibrations using 1 Light-jet is defined as a jet corresponding to neither b-, c-, nor τ-jets. the 8 TeV dataset of cand light-jets are reported in sections 5 and 6.