dataesr/scientific-paragraphs-categorization huggingface dataset:
Statistical analysis The m distributions are scrutinised for a resonant or non-resonant new physics excess using two methods and are used to set limits on resonant and non-resonant new physics models, as well as on generic resonances. Tabulated values of all the observed results, along with their uncertainties, are also provided in the Durham HEP database [53]. The signal search and limit setting rely on a likelihood function, dependent on the parameter of interest, such as the signal cross-section, signal strength, coupling constant or the contact interaction scale. The likelihood function also depends on nuisance parameters which describe the systematic uncertainties. In this analysis the data are assumed to be Poisson-distributed in each bin of the m distribution and the likelihood is constructed as a product of individual bin likelihoods.
The modes of marginalised posteriors of the nuisance parameters from the MCMC method are used to construct the SM prediction. The negative logarithm of the smallest p-value is the BH statistic. The BH statistic is then interpreted as a global p-value utilising simulated experiments where, in each simulated experiment, simulated data is generated from SM background model. The dielectron and dimuon channels are tested separately. A search for Z χ signals as well as generic Z signals with widths from 1% to 12% is performed utilising the log-likelihood ratio (LLR) test described in Ref. [56]. This second approach is specifically sensitive to narrow Z -like signals, and is thus complementary to the more general BH approach. To perform the LLR search, the Histfactory  [57]  package is used together with the RooStats  [58]  and RooFit  [59]  packages.
Conclusion The ATLAS detector at the LHC has been used to search for both resonant and non-resonant new phenomena in the dilepton invariant mass spectrum above the Z boson's pole. The search is conducted with 36. 1 fb -1 of pp collision data at √ s = 13 TeV, recorded during 2015 and 2016. The highest invariant mass event is found at 2. 90 TeV in the dielectron channel, and 1. 99 TeV in the dimuon channel. The observed dilepton invariant mass spectrum is consistent with the Standard Model prediction, within systematic and statistical uncertainties. Among a choice of different models, the data are interpreted in terms of resonant spin-1 Z gauge boson production and non-resonant qq contact interactions. For the resonant interpretation, upper limits are set on the cross-section times branching ratio for a spin-1 Z gauge boson.
Expected and observed event yields in the dimuon channel, directly corresponding to the non-linear binning presented in Figure3(b). The expected yield is given up to at most 4 digit precision. 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. In addition, individual groups and members have received support from BCKDF, the Canada Council, CANARIE, CRC, Compute Canada, FQRNT, and the Ontario Innovation Trust, Canada; EPLANET, ERC, ERDF, FP7, Horizon 2020 and Marie Sklodowska-Curie Actions, European Union; Investissements d'Avenir Labex and Idex, ANR, Région Auvergne and Fondation Partager le Savoir, France; DFG and AvH Foundation, Germany; Herakleitos, Thales and Aristeia programmes co-financed by EU-ESF and the Greek NSRF; BSF, GIF and Minerva, Israel; BRF, Norway; CERCA Programme Generalitat de Catalunya, Generalitat Valenciana, Spain; the Royal Society and Leverhulme Trust, United Kingdom.
Acknowledgements We thank  CERN  for the very successful operation of the LHC, as well as the support staff from our institutions without whom ATLAS could not be operated efficiently. We acknowledge the support of  ANPCyT , Argentina; YerPhI, Armenia;  ARC, Australia ;  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-DSM/IRFU , France; SRNSF, 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,.
ACKNOWLEDGMENTS. We thank  Fundacao de Amparo  a  Pesquisa do Estado de Sao Paulo (FAPESP)  (Grant  2013/07276-1 ),  Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) , and  Conselho Nacional de Desenvolvimento Científico e Tecnol ógico (CNPq)  (Grant  PVE 400228/2014-9 ) for financial support. We appreciate discussions with  P. Courteille  and the technical assistance provided by  E. Henn  and  G. Roati. M. S. H. also acknowledges a  Senior Visiting Professorship  granted by  CAPES.
Note that our solution is dealiased following the 3/2 rule. The code is efficiently parallelized using MPI (Message Passing Interface) and we use up to 2,048 processors for the highest resolution considered in this study. The entire cylindrical domain is discretized using 53,760 elements and a spectral order of N = 11. The element distribution is denser close to the external and bottom boundaries. This, in addition to the Gauss-Lobatto-Legendre point distribution close to the element boundaries, ensures an appropriate resolution of the Ekman boundary layers with approximately six grid points to describe them in all cases. The vertical extent of the cylindrical domain is stretched so that the upper boundary matches to the analytical paraboloid shape that depends on the rotation rate and on the gravitational acceleration.
Acknowledgements This work was supported by the  French Agence Nationale pour la Recherche  (Grant No. ANR-13-JS05-0004-01 ) and by the  Aix-Marseille University Foundation  (A *  MIDEX  project No. ANR-11-IDEX-0001-02 ). J. A. 's sabbatical in Marseille was supported by  S. A. Kremen , by the invited professor programmes of  Ecole Centrale Marseille and Aix-Marseille University , and by the  Labex MEC  (grant  ANR-11-LABX-0092 ). We also acknowledge support from IDRIS for computational time on Turing (Project No. 100508 ) and from the  HPC resources of Aix-Marseille University  (project  Equip@Meso  No. ANR-10-EQPX-29-01  of the  programme Investissements d' Avenir ).
Follow-up of alerts from IceCube On April 27th, 2016, at 05:52:32 UT, IceCube recorded an event fulfilling the HESE criteria and issued an alert soon afterwards. The neutrino has been reconstructed to originate from RA = 16h 02m 16s, Dec = 9. 34 deg with an uncertainty of 36 (radius, 90% containment) and a total charge deposited within the detector of about 18900 photoelectrons. Visibility and weather constrains delayed H. E. S. S. observations of the identified region to April 29th, 2016 around 21:07 UTC. The observations were taken with an average zenith angle of around 50 deg, the resulting energy threshold, defined as the energy where the acceptance is 10% of its maximum value, is 350 GeV. Analyzing the total dataset of 1. 7 h effective livetime, the significance map shown in Fig. 2  has been obtained.
Follow-up of alerts from ANTARES A dedicated direct link between the ANTARES online reconstruction and alert emission system TAToO  [9]  and the H. E. S. S. alert system allows for rapid exchanges of alerts between the two experiments. The performance of this approach has been illustrated by an alert received on January 30, 2017. On 00:39:12 ANTARES recorded a single, high-energy neutrino. The data transfer to the shore station, their filtering, the event reconstruction triggered a VoEvent notice to be emitted to partner observatories at 00:39:25. The alert was received at the H. E. S. S. site triggering automatic follow-up observations which were started at 00:39:44, i. e. only 32 seconds after the neutrino event. About one hour of H. E. S. S. observations could be obtained immediately following the alert before the direction moved outside the visibility window (cf.
Fig. 5 ). Searches for transient gamma-ray emission on various timescales is in progress. Another 30min of data was taken during the night after the alert (2017-01-31 19:29 UT) in order to search for afterglow and/or delayed or emission. A preliminary analysis using monoscopic data from the 28m telescope and time integrating the full dataset did not reveal any significant gamma-ray emission. The significance map of the region around the reconstructed neutrino direction is shown in Fig. 5.
Acknowledgments The support of the  Namibian authorities and of the University of Namibia  in facilitating the construction and operation of H. E. S. S. is gratefully acknowledged, as is the support by the  German Ministry for Education and Research (BMBF) , the  Max Planck Society , the  German Research Foundation (DFG) , the  French Ministry for Research , the  CNRS-IN2P3  and the  Astroparticle Interdisciplinary Programme of the CNRS , the  U. K. Science and Technology Facilities Council (STFC) , the  IPNP of the Charles University , the  Czech Science Foundation , the  Polish Ministry of Science and Higher Education , the  South African Department of Science and Technology and National Research Foundation , the  University of Namibia , the  Innsbruck University , the  Austrian Science Fund (FWF) , and the  Austrian Federal Ministry for Science, Research and Economy , and by the  University of Adelaide  and the  Australian Research Council.
Powder X-ray diffraction The structural analysis was based on X-ray powder diffraction. Diffraction data were collected in a 2h range from 10 to 120 with a step interval of 0. 014 using a Philips PW 3040 (h-h) diffractometer (k Coka ). The nuclear structure was refined using the Rietveld method through the FullProf software  (Houchati et al. , 2012).
2. Description of the structure T 0 -phase La 1. 8 Pr 0. 2 CuO 4 samples were obtained from the above ''pseudo-S'' phase La 1. 8 Pr 0. 2 CuO 3. 5 samples by being heated under an oxygen flow at relatively low temperatures. X-ray diffraction analysis revealed that when the sample was Table  1  Crystallographic data and interatomic distance of the compound La 1. 8 Pr 0. 2 CuO 3. 5. heated in the temperature range of 300 to 500 °C and then cooled to room temperature in air, the sample showed T 0 rather than T structure of the La 1. 8 Pr 0. 2 CuO 4 starting material. The X-ray diffraction pattern of T 0 -phase La 1. 8 Pr 0. 2 CuO 4 is shown in Fig. 7. All the peaks can be indexed on the basis of the tetragonal lattice (I4/mmm), the experimental profile can be refined with good agreement factors with the structural model of the T 0 -phase (Table  2 ).
Acknowledgments We acknowledge funding from the  ANR  project  SuperRing  ( ANR-15-CE30-0012-02 ). J. J. thanks  Studienstiftung des deutschen Volkes  for financial support. The DMRG simulations were run by J. J. and M. R. on the Mogon cluster of the  JGU  (made available by the  CSM and AHRP) , with a code based on a flexible Abelian Symmetric Tensor Networks Library, developed in collaboration with the group of  S. Montangero  at the  University of Ulm.
Observations, data reduction, and radial-velocity variation High-resolution spectra of CS 29497-004 were obtained with UVES at VLT-UT2 during October-December 2002 and July-August 2003. A total of 22 exposures were obtained with the BLUE346 setting, and six with the BLUE437 setting. In both cases Image Slicer #2 was used, yielding a nominal resolving power of R = λ/∆λ = 75 000. The total useful wavelength range covered by these two settings is 3050-4980 Å in the rest frame of the star. The observations are summarized in Table  2. The individual pipeline-reduced spectra were first corrected for geocentric radial-velocity shifts, determined by measuring Notes. λ refers to the combined useful wavelength range (in the rest frame of the star) of all N individual exposures, and t is the total integration time.
Model atmospheres The model atmospheres used in this analysis are the same as those used in the analysis of the r-II star CS 31082-001  (Cayrel et al. 2001; Hill et al. 2002)  and the VMP/EMP giants in the First Stars project  (Cayrel et al. 2004 ). The models are interpolated in a grid of OSMARCS models computed between 2000 and 2002 by B. Plez, using the latest version of the MARCS code. The MARCS code was originally developed by  Gustafsson et al. (1975) , and updated and improved over the years by  Plez (1992) ,  Edvardsson et al. (1993) ,  Asplund et al. (1997), and Gustafsson et al. (2008). The abundance measurements themselves were carried out using the suite of programs Turbospectrum  (Alvarez & Plez 1998) , either through an equivalent-width analysis, or direct comparison (and χ 2 minimisation) between the observed and synthetic spectra.
Line data The linelist adopted to determine abundances in this paper is the same as the one used in  Hill et al. (2002)  and  Cayrel et al. (2004) , with the exception of a number of neutron-capture elements for which improved atomic data has appeared in recent years, thanks to the efforts of atomic physicists (e. g. ,  Lawler et al. 2001a Lawler et al. ,c, 2004 Lawler et al. , 2006 Lawler et al. , 2007;; Nilsson et al. 2002a,b). The neutron-capture element linelist is given in Table  B. 1, together with the references for transition probabilities and hyperfine structure coefficients, where appropriate. The atomic linelist used for the spectrum synthesis was assembled using the VALD database  (Kupka et al. 1999 (Kupka et al. , 2000)) ; oscillator strengths and/or hyperfine structures were updated for specific lines.
Acknowledgements. We are grateful to the  ESO  staff at Paranal and Garching for obtaining the observations and reducing the data, respectively. N. C. expresses his gratitude to the  Observatoire Paris-Meudon  for hospitality shown to him during a 1-month visit during which most of this paper was written. He acknowledges support by  Sonderforschungsbereich SFB 881  " The Milky Way System " (subproject  A4 ) of the  German Research Foundation (DFG). T. C. B. acknowledges partial support for this work from grants  PHY 02-16783 ,  PHY 08-22648 ;  Physics Frontier Center/Joint Institute for Nuclear Astrophysics  (JINA), and  PHY   14-30152 ;  Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE ), awarded by the  US National Science Foundation. P. S. B. is a Research Fellow of the  Royal Swedish Academy of Sciences  supported by a grant from the  Knut and Alice Wallenberg Foundation.
Depending on the wind conditions, the payload will stay in sight of the telescopes for few hours approximately. The lock-in technique and the high signal to noise ratio from the source allow short integration times, so such a flight duration is enough to calibrate the instruments and generate beam maps. POLOCALC total consumption will be less than 25 W. For ground use either a lead battery pack or lithium battery pack are suitable, while for the flight we will make use of high capacity lithium battery packs, that can easily provide 150 -200 Wh/kg. The balloon payload only requires a light, low consumption telemetry to relay tracking data for the ground antennas' auto-pointing and to allow access for all the telescopes that need to track the source. Drone flights will also be used to test telescopes tracking systems.
This suppressed error level is negligible for current experiments targeting r = 0. 01 and future experiments like CMB-S4 that will target r = 0. 001. Primordial B-mode signals (dashed), the gravitational lensing B-mode signal (dash-dot), and the EE signal (green) are plotted for reference in the left panel. In the following sections we present the expected scientific impact of POLOCALC, which can be preliminarily evaluated by simulating CMB data with noise properties that match those expected from current (Advanced ACTPol) and near future (CMB-S3) experimental configurations. The posterior distributions are then obtained by performing a Markov Chain Monte Carlo analysis employing the public COSMOMC package  (Lewis et al. , 2002)  and an exact likelihood approach  (Perotto et al. , 2006).
METHODS III-N on Silicon growth was realized via MOCVD using a single chamber closed coupled showerhead equipment manufactured by AIXTRON capable of fully automated handling of 200 mm wafers. Au free process integration was carried out using CEA-LETI's CMOS facilities on the basis of a process flow comprised of approximately 80 technological steps. Electrical characterization was performed by the use of a Tesla 300 mm semi-automatic prober and an Agilent B1505A power device analyzer. All numerical calculations were performed on specifically developed scripts and were double checked using various commercial and open source coding environments.
We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger (BBH) event GW170104. No candidate electromagnetic counterparts was detected by either GBM or LAT. A detailed analysis of the GBM and LAT data over timescales from seconds to days covering the LIGO localization region is presented. The resulting flux upper bound from the GBM is (5. 2-9. 4)×10 -  erg cm -2 s -1 in the 10-1000 keV range and from the LAT is (0. 2-13)×10 -9 erg cm -2 s -1 in the 0. 1-1 GeV range. We also describe the improvements to our automated pipelines and analysis techniques for searching for and characterizing the potential electromagnetic counterparts for future gravitational wave events from Advanced LIGO/VIRGO.
GBM Signal Searches An automatic, ground-based search of the GBM CTTE data for sGRBs is currently running promptly after the data are downlinked. This search, which we refer to here as the un-targeted search, is similar to the flight software algorithms that GBM uses for triggering on GRBs, which look for simultaneous excesses in two GBM NaI detectors. This search currently rebins the CTTE data into time series with 18 bin widths from 64 ms to 30. 72 s and four phase offsets for each bin width. These time series are created for four different energy ranges that were optimized for finding weak triggered sGRBs: nominally 30-500 keV, 50-500 keV, 100-500 keV and 100 keV-1 MeV. The background estimation is performed via cubic spline fitting and intervals of data are removed from consideration if the background fit deviates significantly from the observed background.
The LAT signal searches Several automatic programs search for transient events over a wide range of timescales in the LAT data. The Fermi automatic science processing (ASP) pipeline and the Fermi All-sky Variability Analysis (FAVA) 3  are used to search for excess emission on hour-to-week long timescales. The ASP pipeline performs a blind search for sources on all-sky count maps constructed from the event data acquired on 6 and 24 hr timescales. Candidate flaring sources are then fit using a standard likelihood analysis with the model including nearby known sources and the Galactic and isotropic diffuse contributions. These candidate sources are then characterized and matched to known sources, allowing for the detection of flaring cataloged sources as well as new unassociated sources. FAVA is a blind photometric analysis in which a grid of regions covering the entire sky is searched over 24 hr and 1 week timescales for deviations from the expected flux based on the observed long-term mission-averaged emission  (Ackermann et al.
2013). This allows the FAVA search to be independent of any model of the gamma-ray sky, and therefore complementary to the standard likelihood analyses. As described in  Ackermann et al. (2016) ;  Racusin et al. (2017)  and, more specifically, in  Vianello et al. (2017) , we have designed specific methods for the follow-up searches in the LAT data of EM counterparts to GW events. The fixed time window search and the adaptive time window search are two of these custom search methods that we run on the LIGO localization maps. In the first case, we search for high-energy gamma-ray emission on a set of fixed time windows (≈ 10ks long) around the LIGO trigger. For each time window, we select all the pixels 4 that were observable by the LAT within the 90% containment of the LIGO localization map and perform an independent likelihood analysis in an 8 • radius region of interest (ROI).
While no conventional model predicts EM counterparts for these sources, our observations are important in two respects: a. ) We improve and test the search algorithms in anticipation of GW events where we do expect an EM counterpart (e. g. , a binary merger with at least one NS component). b. ) We provide flux upper bound constraints for the unexpected scenario where BBH mergers are accompanied by gamma rays. The Fermi -GBM collaboration acknowledges support for GBM development, operations and data analysis from NASA in the United States and BMWi/DLR in Germany. The Fermi -LAT Collaboration acknowledges support for LAT development, operation and data analysis from NASA and DOE (United States), CEA/Irfu and IN2P3/CNRS (France), ASI and INFN (Italy), MEXT, KEK, and JAXA (Japan), and the K. A.
For each of the seventeen sources that do not have their maximum flux within the 10 arcsecond circle around the SPIRE position, that do have a signal-to-noise greater than 3, we decreased the size of the searching box to find the peak in flux. Of these seventeen sources, seven sources have fluxes within 10 arc seconds from the Figure 2. This flowchart shows the data reduction steps schematically, starting from the raw data files at the top, working to the reduced cutouts at the bottom. The intricacies are detailed in the data reduction section. For each observation, two sets of timeslices are cleaned and processed through the iterative mapmaker, and these resulting maps are subtracted to provide a jackknife estimate of the noise. A fake source is injected to estimate peak attenuation due to the filtering process, and allows us to create a PSF for the final matched filter step.
The overlay graph inside Figure  3  shows a strong correlation for most points around the centre, however all other nondetections appear uniformly scattered, making an even distribution likely. We know from  Negrello et al. (2007)  that there is a risk that several of these sources are blazar contaminations. In order to find these contaminants, we plot their flux ratios in Figure  4. The top panel shows the flux ratios based on just Herschel fluxes. We plot S 500µm /S 250µm versus S 350µm /S 250µm. The sources that lie very close to a known blazar (within 10 arc seconds) in the NASA Extragalactic Database (NED) (black circles) lie in the same region as the high-redshift HerBS sources (gray triangles, blue squares and red circles). We also plot the track for the template we derive in Section 4 through the diagram as the redshift changes (black line and circles).
(2010). The large χ 2 values in Table  5  imply that a single template is not actually a good representation of the data. We fit our template to 22 galaxies, each with 4 data points, except one source where we only fitted the three SPIRE fluxes, as its SCUBA-2 flux remained undetected. The free parameters in our model are the template parameters (3 or 4) and the amplitudes for each galaxy (22, eq. 5). The expected χ 2 values for the two models, on the assumption that they are a good representation of the data, are therefore χ 2 Best-f it ≈ N data -N param -1 ≈ 4 × 22 -22 -4 -1 ≈ 61, χ 2 Fixed-β ≈ N data -N param -1 ≈ 4 × 22 -22 -3 -1 ≈ 62. However, we observe χ 2 -values of ∼812, indicating that our sources are poorly modelled by a single galaxy template. We tested the photometric redshift estimates of the templates using the same sources we used to derive the best-fit template.