dataesr/scientific-paragraphs-categorization huggingface dataset:
1 days). No hard X-ray or gamma-ray signal above the background was found. By taking advantage of the full sensitivity and wide FoV of the combination of the IBIS, SPI, and JEM-X instruments, we provide a stringent upper limit over a broad energy range, from 3 keV up to 8 MeV. The INTEGRAL upper limits above 80 keV are tighter than those set by any other instrument and constrain the isotropic-equivalent luminosity of the soft gammaray afterglow to less than 1. 4×10 43 erg s -1 (80-300 keV), assuming a distance of 40 Mpc to the source Our data exclude the possibility that a short-or a long-lasting bright hard X-ray and/or soft gamma-ray phase of activity followed GRB 170817A/GW170817. With these results, we show that INTEGRAL continues to play a key role in the rapidly emerging multi-messenger field by constraining both the prompt and delayed gamma-ray emission associated with compact object mergers.
Acknowledgements This work is based on observations with INTEGRAL, an  ESA  project with instruments and science data center funded by  ESA  member states (especially the PI countries:  Denmark, France, Germany, Italy, Switzerland, Spain ), and with the participation of Russia and the  USA. The IN-TEGRAL  SPI  project has been completed under the responsibility and leadership of  CNES. The SPI-ACS detector system has been provided by  MPE Garching/Germany. The SPI team is grateful to  ASI, CEA ,  CNES ,  DLR ,  ESA ,  INTA ,  NASA  and  OSTC  for their support. The Italian INTE-GRAL team acknowledges the support of  ASI/INAF  agreement n. 2013-025-R. 1. RD and AvK acknowledge the German INTEGRAL support through  DLR  grant  50 OG 1101. AL and RS acknowledge the support from the  Russian Science Foundation  (grant  14-22-00271 ).
AD is funded by  Spanish MINECO/FEDER  grant  ESP2015-65712-C5-1-R. Some of the results in this paper have been derived using the HEALPix [68] package. We are grateful  VirtualData  from  LABEX P2IO  for enabling access to the StratusLab academic cloud. We acknowledge the continuous support by the  INTEGRAL Users Group  and the exceptionally efficient support by the teams at  ESAC  and  ESOC  for the scheduling of the targeted follow-up observations.
In such a way, each configuration has its own set of wavefunctions. The latests are determined in a single-configuration approximation. One peculiarity of the code is that it does not rely on the "isolated atom" picture, but on a realistic atom-in-plasma modelling (equation of state). Relativistic effects are taken into account in the Pauli approximation. The DLA (Detailed Line Accounting) part of the spectrum is performed using an adapted version of the RCG routine from Cowan's suite of atomicstructure and spectra codes  [20]. The RCG source code was used for decades by spectroscopists, it has many available options and is well documented. In SCO-RCG, criteria are defined to select transition arrays that can be treated line-by-line. The data required for the calculation of the detailed transition arrays (Slater, spin-orbit and dipolar integrals) are obtained from SCO, providing in this way a consistent description of the plasma screening effects on the wavefunctions.
One observes that ATOMIC "full" and ATOMIC n5 agree within 20 % and that, in all cases, ATOMIC n5 values are smaller than those of ATOMIC "full". SCO-RCG, which is not limited to n ≤ 5, is generally closer to ATOMIC "full" than to ATOMIC n5 (see Fig. 8 , left and right, as well as tables 1 and 2)  [41] , which is consistent with the fact that configuration interaction plays a less important role than state completeness in the present case. The values of OP (Opacity Project)  [42, 43] , are usually lower. The Opacity Project, an international collaboration of about 25 scientists from 6 countries, started in response to a plea  [3]. The atomic data are available in the database TOPbase  [44]  and the monochromatic opacities and Rosseland mean opacities are available at the OPServer  [45]  at the Ohio Supercomputer Center.
Acknowledgements The work is partially supported by the  Marie Skłodowska-Curie Research, Innovation Staff Exchange  Project  H2020-MSCA-RISE-2014  no. 644260  "INTELUM". The Ukrainian and French teams also acknowledge the support from  Ukrainian-French   PICS  project between  CNRS  (Project no. 6598 ) and  National Academy of Sciences of Ukraine  ( ProjectF1-2016 ).
LTE models are also much simpler for numer ical realization and, in principle, may be implemented by means of ready-to-use specialized software such as Plasimo  [4]  or the Equilibrium DC Discharge (sub)module of the Plasma module of COMSOL Multiphysics ®. It is therefore highly desirable to develop a self-consistent joining of a numerical model of LTE bulk plasma with a cathode. The importance of this subject has been realized long ago and many attempts have been made; e. g. [5] [6] [7] [8] [9] [10] [11] [12]. However, there is still no universally accepted approach. In fact, many researchers do not consider the physics of plasma-electrode interaction and employ the LTE equations right to the electrode surfaces. One of the problems of such an approach is an unrealistically high resistance of the near-electrode plasma, which requires some or other numerical cut-off; e.
After that, one finds the additive constant in the distribution of electrostatic potential in the cathode by applying equation  (11)  on the axis of symmetry, and thus the arc voltage. The solution is complete for the arc current I being considered. Note that equation  (11)  has been satisfied only at one point of the cathode surface (on the axis of symmetry). This is a price to be paid for simplifying the procedure by assuming U constant. However, the modelling results show that ϕ (LTE)  does not vary much on the cathode surface inside the arc attachment; the voltage drop inside the cathode is small, meaning that ϕ (s) varies little as well; hence, the residual in equation (  11 ) is not large. Commercial software COMSOL Multiphysics (version 5. 2) is used for numerical calculations. The 'Heat transfer in solids' and 'Electrical currents' modules are used for solving the equations in the electrodes.
Acknowledgments The work at  Université d'Orléans  was supported by  Zodiac aerospace  and the work at  Universidade da Madeira  was supported by  FCT-Fundação para a Ciência e a Tecnologia of Portugal  through the project  Pest-OE/UID/FIS/50010/2013. The authors thank  Yann Cressault  for providing data on some transport coefficients of the plasma.
To that end, further development of intersecting brane models beyond simple torus geometries, as e. g. in  [52] , is crucial for a connection to string cosmology. for helpful discussions before the first version, and G. Bossard, M. Graña, K. Krasnov, R. Minasian, B. Pioline, G. Policastro, H. Samtleben and D. Tsimpis for useful comments that improved this draft towards its revised version. The work of D. A. is part of the Einstein Research Project "Gravitation and High Energy Physics", funded by the Einstein Foundation Berlin. The work of J. B. is supported by John Templeton Foundation Grant 48222, and the CEA Eurotalents program.
Introduction In the last decade, the space photometry missions CoRoT and Kepler have provided us with a wealth of precise seismic data for a large number of stars. This revolution is now allowing us to carry out precise seismic modelling for these stars and to test the physical inputs of our stellar models. As a by-product of this modelling, asteroseismology also delivers precise and accurate fundamental parameters, which are essential to other fields such as galactic archeology or exoplanetology. Amongst the observed targets, the Kepler Legacy sample contains the dwarfs that have the best frequency sets within the Kepler data (See  [5]  for the presentation of the dataset and  [6]  for forward modeling results of the Kepler Legacy sample). As such, they can be seen as benchmark stars to test our inputs of stellar models and the efficiency of seismic modelling.
This is a strong argument in favor of a significant anisotropy along that particular axis. It is worth noting that thermal variation of magnetization measurement performed along the three crystallographic directions also indicates a slightly higher magnetization along b (not shown). To figure out quantitatively the nature of the Dy 3+ anisotropy, numerical ab-initio calculations (including 4f electronic correlation and spin-orbit interaction) have been performed, on an embedded DyO 5 fragment. We used the CASSCF code of the MOLCAS package  22  for the orbital and correlation calculations, the EPCISO code  23  for the spin-orbit calculation and a home made code for the anisotropy and magnetic moments calculation from the ab-initio results. We find that the low energy crystal field states of the Dy 3+ ions are formed by a doublet.
To identify the signal, we compared the data with the spectra published for similar materials, YMn 2 O 5 and TbMn 2 O 5 in refs  25  and 26 respectively. Indeed, we observe features clearly reminiscent of the spin wave branches reported in these two compounds. The spin wave energies were determined based on a simple fit assuming a standard Gaussian profile on top of a constant background. A flat feature at about 6. 5 meV may also correspond to a signal (see 7B and C). Actuallly, owing to the experimental set up, this energy region corresponds to small scattering angles, hence a region where the contamination due to the incident beam may become significant especially when considering long counting times. The feature at 6. 5 meV is likely due to this effect, and thus not relevant.
Acknowledgements Authors gratefully acknowledge LLB and  ILL  for beam-time allowance. We also acknowledge  V. Simonet  for her careful reading of the manuscript and  F. Damay  for fruitful discussions. This work was financially supported by the  ANR   Dymage 13-BS04-0013. This work has also benefited from  LabEx PALM's Investissements d' Avenir programme  ( ANR-10-LABX-0039-PALM ).
Emission line selected objects We also searched for emission lines directly in the data cubes to identify objects. We adopted the software ORIGIN (detectiOn and extRactIon of Galaxy emIssion liNes;  Mary et al. in prep. )  to perform blind detections. The ORIGIN software uses a matched filter in threedimensional data to detect signals by correlating with a set of spectral templates. It first uses a principal component analysis (PCA) to remove continuum emission. A matched filter is then applied to the continuum removed data cube and the P-value test is used to assign a detection probability to each emission line candidate. When the test gives a high probability, a narrowband image is created using the raw data cube to further test the significance of the line. The line is only considered to be a real detected line when it survives the narrowband image test.
Finally, the spatial position of each detected line is estimated by spatial deconvolution. For more details on the procedures and parame-ters used for the detections in udf-10 and the mosaic, we refer to Paper I. In udf-10 and the mosaic, 306 and 1251 emission line objects were detected with ORIGIN, respectively. In addition to ORIGIN, we also used the MUSELET software 4  to test our blind search for line emitters in the Mosaic field. The MUSELET software is a SExtractor-based detection tool, which identifies line emission sources in continuum-subtracted narrowband images of a cube. The narrowband images are produced by collapsing (weighted average) the closest 5 wavelength planes (6. 25Å) and subtracting a median continuum from the closest 20 wavelength planes (25Å) on each of the blue and red sides of the narrowband regions.
By comparing the UVUDF sources and ORIGIN detections with the raw MUSELET catalogs of emission line sources in the mosaic, MUSELET only detects 60% of the objects which ORIGIN detects, but it finds 16 additional sources. The lower detection rate and small number of additional detections of MUSELET strengthens our choice of ORIGIN as the primary line detection software for the analyses of these fields. All of the sources detected only by MUSELET are also included in the analyses of this work and the released catalogs.
Redshift determination We adopted a semi-automatic method for the redshift identification. For the continuum selected galaxies, we used the redshift fitting software MARZ  (Hinton et al. 2016). The redshift determination of MARZ is based on a modified version of the AUTOZ cross-correlation algorithm  (Baldry et al. 2014). From a userdefined input list of spectral templates, it automatically finds the best-fit template to the input spectrum and determines the redshift. If the resulting redshift is not ideal, then the user can also update it interactively in the same window. We used the peak position of the most significant detected feature to define redshift, including Lyα. The Lyα peak emission may not represent the systemic redshift due to radiation transfer effects of the resonant Lyα line in bulk motion of neutral hydrogen gas  (Hashimoto et al.
We also implement a feature to show images in the panel on the right. Leclercq et al. 2017 ). However, this results in an increased scatter for faint emission lines. For the detected emission lines with S/N > 3, the line flux and its uncertainty are provided along with the measured redshift in the released catalog (Appendix A). We used the spectral line fitting software PLATEFIT  (Tremonti et al. 2004; Brinchmann et al. 2008)  to simultaneously fit all of the emission lines falling within the spectral range. This tool first uses a set of model template spectra from  Bruzual & Charlot (2003)  with stellar spectra from MILES  (Sánchez-Blázquez et al. 2006)  to fit the continuum of the observed spectrum at a predefined redshift with strong emission lines masked. After subtracting the fitted continuum from the observed spectrum, a single Gaussian profile is fitted to each expected emission line in velocity space.
The velocity offset (the velocity shift relative to the redshift of the galaxy) and velocity dispersion of all of the emission lines are tied to be the same. See Tremonti et al. (2004)  for a more detailed description of the software. The velocity offset is limited to vary within ±300 km s -1. For emission line galaxies, we used the velocity offset output from PLATEFIT to refine the original (input) redshift. The calculation of the velocity offset includes Lyα when it is detected. The typical velocity offset is about 10 km s -1 on average. When the original redshift is obtained directly from MARZ's cross-correlation, we do not expect the offset to be significant, but it can be larger when the redshift identifiers manually estimate the redshift. As described above, PLATEFIT fits single Gaussian functions to the emission lines.
The rest of the objects can be visually identified in the images, but they are not detected by SExtractor 6   (Bertin & Arnouts 1996). In order to measure continuum fluxes (or upper limits) of these objects, we used NoiseChisel 7 , which is an image analysis software employing a noise-based detection concept  (Akhlaghi & Ichikawa 2015). It is run independently on each of the HST images and the largest (from all the filters) object closer than 0. 30 to the position reported by ORIGIN/MUSELET is taken as representing the pixels associated with it to create a segmentation map for each object. We are able to associate a NoiseChisel segmentation map for 76% of the objects only found by ORIGIN/MUSELET. However, for the rest of the objects, no NoiseChisel segmentation map (in any of the HST broadband images) can be found within 0.
Based on the redshift analysis in our deepest survey field udf-10, we tried to find the best combination of the two extraction methods to maximize the efficiency of redshift identifications. As shown in Figure  9 , for the objects with redshift determined, 85 out of 98 objects at z < 3 (CONFID ≥ 2), mostly [O ii] emitters, have F775W ≤ 27 mag (see also Figure  10 ). While the majority at z > 3 are fainter than 27 mag, 106 out of 155 objects (70%) in this redshift range are detected by line emission directly in the data cube with ORIGIN. In addition, all of the absorption galaxies, which ORIGIN cannot detect, are brighter than 26. 1 mag. We simulated expected [O ii] line fluxes to investigate the sudden reduction of [O ii] emitters fainter than 27 mag visible in Figure  10. With the spectral energy distribution (SED) fitting code FAST 8  (Kriek et al.
Acknowledgements. The authors are grateful for useful suggestions by the referee that improved the manuscript. We thank  Laure Piqueras  for her support with analysis and observation software. This work is supported by the  ERC  advanced grant  339659-MUSICOS  ( R. Bacon ). JB acknowledges support by  Fundação para a Ciência e a Tecnologia (FCT)  through national funds ( UID/FIS/04434/2013 ) and by  FEDER  through  COMPETE2020  ( POCI-01-0145-FEDER-007672 ) and was in part supported by  FCT through Investigador FCT  contract  IF/01654/2014/CP1215/CT0003. JR and BC acknowledge support from the  ERC  starting grant  336736-CALENDS. TC acknowledges support of the ANR FOGHAR  ( ANR-13-BS05-0010-02 ), the  OCEVU Labex  ( ANR-11-LABX-0060 ), and the A* MIDEX  project ( ANR-11-IDEX-0001-02 ) funded by the " Investissements d'avenir" French government program  managed by the  ANR.
The Large Volume Detector (LVD) is a 1 kton liquid scintillator detector located at Laboratori Nazionali del Gran Sasso, Italy, at the average depth of 3600 m w. e. The experiment has been continuously taking data since June 1992. The muon dataset collected by LVD over 25 years (from 1992 to 2016) consists of 5. 5 • 10 7 events, being the largest ever provided by a single detector underground. The analysis of the global time series shows a modulation of muon flux underground with period of T = (365. 1 ± 0. 2) days, an amplitude of 1. 5% and a maximum at the beginning of July. A clear correlation with atmospheric temperature variations is present, with a measured coefficient of α T = 0. 93 ± 0. 02. This is in agreement with the expected value at LVD depth and with the value measured by other experiments in the same underground site.
LVD Muon Data Muons are identified in LVD through the time coincidence of signals with an energy release E ≥ 10 MeV in two or more counters within a time window of 175 ns, which is large enough to include the time jitter of the PMT's transit time. Data selection is performed via the standard quality cuts that have been defined in the search for neutrino burst  [9]. Additionaly, the muon-like events associated to the CNGS (CERN Neutrino to Gran Sasso  [10] ) neutrino beam in the period  [2006] [2007] [2008] [2009] [2010] [2011] [2012]  have been excluded if in coincidence with the time of the beam spills inside a time window of [-10 : +20. 5]µs, being 10. 5µs the spill duration. The resulting dataset consists of 5. 5 • 10 7 muons for a total livetime of 8403 days. The measured daily muon rate is shown in figure  5  and it is mainly affected by the different detector configurations over the time, as shown in figure  3.
Results The daily muon flux of figure  7  has been fitted with a sinusoidal function I µ (t) = I 0 µ + ∆I µ cos( 2π T (t -ϕ )) (6. 1) obtaining a period of T = (365. 1 ± 0. 2) d, which is compatible with what expected from the yearly temperature modulation. The amplitude ∆I µ and the phase ϕ of the modulation can be better evaluated by projecting and averaging the 25 years dataset into one single year, as shown in figure  8. We assume that there is not a long term modulation lying under the first armonic and we neglect the short time variations. We use again the fit function in 6. 1, but fixing T = 365 d, and including systematic errors of muon flux values. We obtain ∆I µ = (5. 2 ± 0. 3) • 10 -6 m -2 s -1 (∼ 1. 5%) and a phase ϕ = (187 ± 3) d (corresponding to the beginning of July). From the daily muon flux (fig.
Acknowledgements We would like to thank  Ulf Danielsson ,  Giuseppe Dibitetto ,  Mariana Graña ,  Fernando Marchesano ,  Washington Taylor , and  Angel Uranga  for interesting discussions. The work of I. B. and J. B. was supported by the  John Templeton Foundation  Grant  48222  and by the  ANR grant Black-dS-String. The work of J. B. was also supported by the  CEA Eurotalents program. The work of R. S. was supported by the  ERC Advanced Grant SPLE  under contract  ERC-2012-ADG-20120216-320421. In our calculations we have used SymPy [33] and we would like to thank the developers.
Acknowledgements: We would like to thank  T. Kontos ,  V. Juricic ,  S. Q. Shen  and  X. R. Wang  for useful comments. This work is supported by  Agence Nationale de la Recherche LabEx  grant  ENS-ICFP  ( ANR-10-LABX-0010/ANR-10-IDEX-0001-02 PSL ) and by the  Austrian Science Fund , Project SFB  F2504-N17  IRON. TP acknowledges support from the  Mahidol Wittayanusorn Scholarship  and the  Franco-Thai Scholarship.
Thomas Schäfer: Transport Properties of Strongly Correlated Fluids Experiments at RHIC and the LHC have shown that quark gluon plasma behaves as a nearly perfect fluid. This means that the shear viscosity to entropy density ratio η/s of the plasma is close to the limits thought to be set by quantum mechanics  [6]. Holographic dualities have provided a theoretical The lines show a hydrodynamic analysis performed using η/s = 0. 2  [11]. Right panel: Hydrodynamic fit to the expansion data of Cao et al. [12] , from  [13]. The data correspond to three different temperatures that are significantly above the critical temperature, and the fit was used to verify the validity of kinetic theory in the high temperature regime. example of a nearly perfect fluid  [7] , but we do not know whether the physical mechanism for perfect fluidity in AdS/CFT is relevant to QCD.
Acknowledgments: This work was supported in parts by the  US Department of Energy  grant  DE-FG02-03ER41260  (TS), the  Federal Target Program for Research and Development in Priority Areas of Development of the Russian Scientific and Technological Complex  for 2014-2020, Contract  14. 584. 21. 0017  (AM), and the  US Department of Energy  under Contracts No. DE-FG-88ER40388  and  DE-AC02-98CH10886 (DK).
We suggest that this discrepancy is because previous measurements were made by single point sensors permanently located close to the stationary stylus specimen. This means that continued emission from the moving surface after the contact has passed (i. e. "afteremission"  [27] ), was not be detected. Conversely, in this experiment, emission from the whole of the wear track is recorded. Fig. 2  (c) shows the average emission verses time for the scratch test on the oxidised Al specimen. This shows large emission peaks however no baseline emission or after emission is observed. The emission from this specimen, which we attribute to the fracture of the oxide layer, can be observed in greater detail in Fig. 2(d). Fig. 3  displays the same average phosphor-screen intensity data in Fig. 2 , but this time plotted against the cycle number and In addition to providing spatially averaged data, the phosphor screen images can be viewed individually as the examples in Fig.
Four-body decays require five independent variables to fully represent the phase space. Consequently, binned analyses will have a trade-off between minimising the number of bins, in order to maximise the number of events per bin, and retaining sensitivity to the interference between all contributing resonances. The measurement presented here includes data collected in 2012, resulting in a signal sample that is about three times larger than in the previous LHCb analysis. The method exploited here, known as the energy test, is an unbinned technique, which is advantageous in the analysis of multibody decays. The energy test was applied for the first time to search for CP violation in decays of D 0 → π -π + π 0  [5] ; here we present its first application to four-body decays. The energy test is used to assess the compatibility of the observed data with CP symmetry.