dataesr/scientific-paragraphs-categorization huggingface dataset:
0 23. 7 ± 2. 0 100. 0 ± 0. 0 % 100 17. 4 ± 1. 7 17. 4 ± 1. 7 100. 0 ± 0. 0 % 120 9. 5 ± 1. 3 9. 5 ± 1. 3 100. 0 ± 0. 0 % unlensed sources (grey dashed line) immediately suggests most of our sources are lensed. We can quantify this as follows. At the low fluxes, the data deviate from the model, because of the incompleteness of the HerBS sample at fluxes lower than ∼50 mJy. There are more sources than the model predicts at high fluxes, the significance of which is difficult to pin down due to the small number of sources. It is possible our sources have over-estimated 850 µm fluxes, possibly due to source confusion. However, it is important to realise that the model of  Cai et al. (2013)  is based on fitted luminosity functions. The high flux end of the luminosity function require large area surveys to be accurately fitted.
Ivison et al. (2016)inosity is calculated using the fitted photometric template The HerBS sample -SPIRE and SCUBA-2 data. The HerBS number hyperlinks to the NED database at the position of the source. The RA and DEC are the SPIRE-positions, ∆RA and ∆DEC are the SPIRE positions minus the SCUBA-2 positions. Cursive SCUBA-2 observations are classed as non-detections, as discussed in Section 3. The spectroscopic redshifts are discussed in Section 4, z phot,temp refers to the template derived in Section 4, and z phot,temp refers to the photometric redshift estimates inIvison et al. (2016). The bolometric luminosity is calculated using the fitted photometric template.
Ivison et al. (2016)IRE and SCUBA-2 data. The HerBS number hyperlinks to the NED database at the position of the source. The RA and DEC are the SPIRE-positions, ∆RA and ∆DEC are the SPIRE positions minus the SCUBA-2 positions. Cursive SCUBA-2 observations are classed as non-detections, as discussed in Section 3. The spectroscopic redshifts are discussed in Section 4, z phot,temp refers to the template derived in Section 4, and z phot,temp refers to the photometric redshift estimates inIvison et al. (2016). The bolometric luminosity is calculated using the fitted photometric template.
ACKNOWLEDGEMENTS We would like to thank our JCMT operator,  James Hoge , for his help at the full-service James Clerck Maxwell Telescope. TB, MS and SAE have received funding from the  European Union Seventh Framework Programme  ( [FP7/2007([FP7/ -2013] ] [FP&/2007-2011 ]) under grant agreement No. 607254. The  Herschel-ATLAS  is a project with Herschel, which is an  ESA  space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from  NASA. The Herschel-ATLAS website is http://www. h-atlas. org. RJI acknowledges support from  ERC  in the form of the Advanced Investigator Programme, 321302, COSMICISM. LD and SJM acknowledge support from  ERC  in the form of the Advanced Investigator Programme, 321302, COSMICISM, and the Consolidator Grant C D (ERC-2014-CoG-647939, PI H,L, Gomez ).
Within the HESPERIA Horizon 2020 project, two novel real-time tools to predict Solar Energetic Particle (SEP) events were developed. The HESPERIA UMASEP-500 tool makes real-time predictions using a lag-correlation between the soft X-ray (SXR) flux and high-energy differential proton fluxes of the GOES satellite network. We found that the use of proton data alone allowed this tool to make predictions before any Neutron Monitor (NM) station's alert. The performance of this tool for predicting Ground Level Enhancement (GLE) events for the period 2000-2016 may be summarized as follows: the probability of detection (POD) was 53. 8%, the false alarm ratio (FAR) was 30%, and the average warning time (AWT) to the first NM station's alert was 8 min. The developed HESPERIA REleASE tool makes real-time predictions of the proton flux-time profiles of 30-50 MeV protons at L1 and is based on electron intensity measurements of energies from 0.
For more information about the GLE forecast results, please consult  Núñez et al. 2017. The original purpose of the HESPERIA UMASEP-500 tool was to correlate SXR with neutron and proton data. We found that the use of proton data alone allowed this tool to make predictions before any Neutron Monitor (NM) station's alert. This satisfactory result became our operational criterion for classifying a GLE forecast as successful. We found that the correlation of SXR and neutron counter data did not trigger any hit additional to those generated using proton data alone. We also found that the use of neutron data provoked the generation of many false alarms due to some quality data problems (mainly spikes) caused by technical issues, such as problems in the neutron sensor tubes and power supplies, among others  (Souvatzoglou et al.
Numerical analysis To confirm the origin of the resonances in our noise spectrum, we calculate the mechanical eigen-frequencies of the micro-resonator using a commercial finite-element analysis software (Comsol). We simulate a 12 µm long GaAs wire, with a bottom diameter of approximately 300 nm and a tapering angle of θ = 3˚. In order to adjust the mechanical frequencies to the experimental values, we allow a 5% variation on the length of the wire (due to flux inhomogeneities over the wafer surface in the MBE chamber). To account for the observed splitting of the first flexural mode, we also introduce a small asymmetry in the QD plane. In practice, the microwire has round top diameter but an elliptic base, the consequence of a slightly anisotropic etching process (∆θ = θ x -θ y ). Fig. 9  shows the results for a 11.
Acknowledgements We acknowledge financial support from  NCCR QSIT  and  SNF  project  200020 156637. We thank  N. Lörch ,  C. Bruder ,  J. Teissier  and  S. Starosielec  for fruitful discussions;  D. Riedel ,  D. Najer ,  J. -P. Jahn  and  J. Roch  for assistance in the lab. Sample fabrication was carried out in the " Plateforme Technologique Amont " and in CEA/LETI/MINATEC/DOPT clean rooms.
White dwarfs with magnetic field strengths larger than 10 T are understood to represent more than 10% of the total population of white dwarfs. The presence of such strong magnetic fields is clearly indicated by the Zeeman triplet structure visible on absorption lines. In this work, we discuss the line broadening mechanisms and focus on the sensitivity of hydrogen lines on the magnetic field. We perform new calculations in conditions relevant to magnetized DA stellar atmospheres using models inspired from magnetic fusion plasma spectroscopy. A white dwarf spectrum from the Sloan Digital Sky Survey (SDSS) database is analyzed. An effective temperature is provided by an adjustment of the background radiation with a Planck function, and the magnetic field is inferred from absorption lines presenting a Zeeman triplet structure.
The design of a line shape model accounting for both Stark broadening and Zeeman splitting is not straightforward, because these two effects do not act as additive perturbations. Previous investigations in low-density (tokamak edge) magnetized plasma conditions have indicated an alteration of the broadening of each Zeeman component due to the change of the atomic energy level structure (degeneracy removal) in response to an external magnetic field  [7, 8]. This issue also concerns magnetized white dwarfs with spectra exhibiting Zeeman splitting. In this work, we report on the current status of the design of a line shape model accounting for Stark and Zeeman effects simultaneously, for applications to white dwarf atmosphere analysis. We perform new Stark-Zeeman line shape calculations. The applicability of spectroscopy as a diagnostic means is illustrated through the analysis of a white dwarf spectrum obtained from the Sloan Digital Sky Survey (SDSS) database.
White Dwarf Spectrum Analysis In this section, we illustrate the applicability of spectroscopy as a diagnostic means for the characterization of white dwarf atmosphere. A large amount of spectra presenting Zeeman splitting are available on the SDSS database (www. sdss. org) [1, 4]. Figure  3  shows an example of such a spectrum. We have performed a fitting of the Hα and Hβ absorption lines using an exponential attenuation model (Beer-Lambert formula) assuming a homogeneous atmosphere slab, leaving the product N 2 × L between absorber density N 2 and thickness L as an adjustable parameter. The temperature that enters the formula (through the electron collision operator and the microfield probability density function) is estimated from adjustment of the background radiation with a Planck function, assuming local thermodynamic equilibrium.
Conclusions According to observations, a significant proportion of white dwarfs have a strong magnetic field, sufficiently so that the absorption lines present a Zeeman triplet structure. In this work, we have done new calculations of Stark-Zeeman hydrogen line shapes in preparation for the development of a model. Specific issues such as the quadratic Zeeman effect need to be investigated further. The applicability of spectroscopy as a diagnostic means for magnetized white dwarf atmospheres has been illustrated through adjustments performed on a spectrum from the Sloan Digital Sky Survey (SDSS) database. It is found that line width adjustments provide an order of magnitude for the electron density and the magnetic field in the atmosphere. An extension of the work to the accounting for plasma non-homogeneity presently ongoing.
Acknowledgments: W. G. and G. P. acknowledge support from the  BASAL Centro de Astrofísica y Tecnologias Afines   PFB-06/2007. This research has received funding from the  European Research Council  under the European Union's  Horizon 2020 research and innovation program  (grant No  695099 ). PK acknowledges support from the  French Agence Nationale de la Recherche (ANR) , under grant  ANR-15-CE31-0012-01.
Acknowledgments D. L. gratefully acknowledges financial support of  Russian Science Foundation  (grant number  15-12-10004 ). NT, MP, TM, AAZ, and JLS acknowledge financial support by the  ANR   GAMBIT  project, grant  ANR-13-BS10-0014  of the  French Agence Nationale de la Recherche  and the  International project of Scientific Cooperation with Vietnam  ( CNRS PICS 6457 ). The TEM studies were conducted at the  Laboratorio de Microscopias Avanzadas, Instituto de Nanociencia de Aragon, Universidad de Zaragoza ,  Spain. Some  of the research leading to these results has received funding from the  European Union   Seventh Framework Program  under Grant Agreement  312483 ESTEEM2  ( Integrated Infrastructure Initiative -I3 ) and from the  European Union   H2020.
5 MHz for the 17 May event and at 19. 5 MHz for the 25 August event. The background occurrence probability map is based on 13 year ground-based radio observations from NDA  [Leblanc et al. , 1993, and references therein]. The white box regions were designated by  Garcia [1996]  on the basis of 39 year DAM observations at 18 to 22 MHz at the University of Florida Radio Observatory. limitation of continuous spectral data obtained during the Voyager 1 and 2 flybys of Jupiter, there is a lack of understanding of the latitudinal beaming structures of Jovian DAM radiation. The purpose of this paper is to report two concurrent DAM observations from the Juno spacecraft near Jupiter and a ground-based low-frequency radio observatory at Earth that are widely spaced in latitude over a broad frequency range of 10 to 40 MHz.
Analysis and Modeling In identifying concurrent DAM emissions with Juno and the NDA, a visual survey of Juno and NDA spectral data recorded during Juno's approach and the two 53. 5 day orbits of Jupiter (ranging from 5 May to 18 October 2016) was carried out. As a result, we found two events in which a well-defined discrete arc was measured by Juno and NDA on 17 May and 25 August 2016. Figure  1a  shows the relative positions of Jupiter, Juno, and NDA at Earth as viewed from the north pole of the Sun, while Figure  1b  summarizes the observational information concerning the Io phase and Jovian CML for the two events. It is obvious that the 17 May event intercepts the Io-A region as seen from Juno location and Io-A' for Earth's position. The 25 August event occurs in the non-Io-A source as viewed from both vantage points  [Carr et al.
, 1983; Garcia, 1996]. The two well-defined discrete arcs from the Juno and NDA spectral data are presented in time-frequency diagrams for the 17 May event in Figure  2a  and for the 25 August event in Figure  2b. The NDA's temporal resolution is fixed at 1 s for these two events. The Juno dynamic spectra are sampled with a 10 s interval for the former event and with a 1 s step for the latter event. The maximum frequency of the arcs extends to 30. 5 MHz and 27. 5 MHz, respectively, as seen by Juno and 27 MHz as seen by the NDA. The absence of the upper frequencies from NDA may be related to the extinction of radio sources at high frequency. For the lower frequencies from NDA, it may be due to the radio wave propagation through the terrestrial ionosphere or the ground-based radio reception.
In order to reconcile this problem, we introduce a contribution from the cross section of the beaming pattern as viewed from two latitudinally different observers. Nevertheless, both CDAs 1 and 2 should be corotated with the Jupiter's rotation rather than the orbital motion of Io. Another interpretation of the observational delay between Juno and NDA could be accounted for by the combination of the light travel time and a corotational lag due to the interaction between the Jovian magnetosphere and the interplanetary magnetic field (IMF). Hess et al. [2014]  showed that non-Io-related DAM arcs subcorotate with Jupiter at velocities ranging from 50% for IMF below 2 nT to 80% for IMF above 2 nT of rigid corotation. This subcorotation rate was determined by comparing dynamic spectra from NDA, Cassini, and Galileo data obtained from October to December 2000 when their observers varied in latitude from -0.
Acknowledgments The authors are indebted to all members of the  Juno mission team , especially the engineers and staff of the  Juno Waves instrument. The research at the  University of Iowa  was supported by  NASA  through contract  699041X  with the  Southwest Research Institute  and the  Theodore Dunham, Jr. grant from the  Fund for Astrophysical Research. The NDA is hosted by the  Nançay Radio Observatory / Unité Scientifique de Nançay of the Observatoire de Paris (USR 704-CNRS , supported by  Université d'Orléans, OSUC, and Région Centre in France). NDA observations are accessible online at http://www. obs-nancay. fr. Juno Waves Data used for this article are available through request to the authors and, subsequently, through the Planetary Data System.
The target frame is made of Ti or Al and has a rectangular shape (140 mm × 130 mm) with maximum thickness of 6 mm. The inner part of each target frame will be tailored for each experiment, either designed by the users or chosen among a set of available geometries. The external part will have a standard geometry to allow for mounting in the carrier frame and placement of fiducial marks and an identification mark. Targets will be characterized before the experiment. Target coordinates with respect to fiducials will be measured (using an automatic sample screening software), stored in a database and uploaded during the beamtime so that targets can be positioned in the focal spot by rastering the frame. A similar concept has been developed for the interaction area of the ELIMAIA beamline (ELI Multidisciplinary Applications of laser-Ion Acceleration, ELI-Beamlines).
Therefore a database of targets produced for previous experiments is available. The European community, on the contrary, has no coordinated strategy to access target fabrication infrastructure, and the initiative is left to the individual facilities, institutes and research groups. Some facilities, as for example the Central Laser Facility at Rutherford Appleton Laboratory (RAL) in the United Kingdom, and the PHELIX facility at GSI, Germany make their target fabrication capabilities available to the community through commercial contracts or scientific collaborations. In particular, RAL offers support to CLF users for target supply (within a given budget) thanks to an established target fabrication group. This group is involved in the whole process, from proposal evaluation and technical feasibility assessment to target delivery.
Although some groups are developing automated target processing and applying robotics to target fabrication, these capabilities are not widespread in the community. In general, surprising target fabrication capabilities and competence are available in university groups, material science laboratories and companies traditionally not considered as target suppliers. A better coordination and enhancement of those capabilities, together with the competence of experienced target fabricators, would help in creating a sustainable target supply mechanism for the upcoming facilities. In addition, user facilities should develop very basic production capabilities or, at least, adequate assembly stations, and a target database to keep track of processes and issues. Training of the next generation of target experts should be a priority for facilities and suppliers to ensure the availability of qualified experts and the continuity of laboratory operation.
Acknowledgements This summary report paper reflects the results of the discussion triggered by the EUCALL Satellite Workshop aimed at building a target network for advanced laser facilities (Dresden, August  29-31 ,  2016 , https://www. eucall. eu). The authors thank all the participants for their contribution and all of those who filled their survey on target needs and fabrication capabilities. I. P. and R. B. acknowledge support from the  European Cluster of Advanced Laser Light Sources (EUCALL)  project which has received funding from the  European Union 's  Horizon 2020 research and innovation programme  under agreement No  654220. M. O. C. , C. G. and V. L. acknowledge the support of the ELI-NP team and from  ELI-NP Phase II , a project co-financed by the  Romanian Government and European Union  through the  European Regional Development Fund -the Competitiveness Operational Programme  ( 1/07.
The MYRRHA (Multi-purpose hYbrid Research Reactor for High-tech Applications) concept is a flexible experimental lead-bismuth cooled and mixed-oxide (MOX) fueled fast spectrum facility designed to operate both in sub-critical (accelerator driven) and critical modes. One of the key issues for the safe operation of the reactor is the uncertainty assessment during the design works. The main objective of the European project CHANDA (solving CHAllenges in Nuclear DAta) Work Package 10 is to improve MYRRHA relevant nuclear data in order to reduce the reactor parameter uncertainties derived from them. In order to achieve this goal, several tasks have been undertaken. First, a sensitivity study of MYRRHA integral parameters, such as energy dependent cross sections, fission spectra and neutron multiplicities, to nuclear data has been conducted resulting in a list of MYRRHA relevant quantities (nuclides and reactions).
Introduction MYRRHA is a flexible experimental facility being designed at SCK•CEN, Mol, Belgium  [1]. It is conceived to operate both in sub-critical, or Accelerator Driven System (ADS) mode, driven by a 600 MeV linear proton accelerator, and in critical mode, as a leadbismuth cooled fast reactor. An accurate knowledge of the safety parameters (i. e. , neutron multiplication factor k eff , reactivity coefficients, etc. ) is required considering the complex neutronic design of MYRRHA  [2]. In the neutronic and safety design of the reactor, an important aspect is the uncertainty propagation and sensitivity to nuclear data; therefore, accurate and reliable nuclear data are needed for MYRRHA. The EC FP7 CHANDA project  [3] , whose acronym stands for "solving CHAllenges in Nuclear DAta", addresses the challenges in the field of nuclear data for nuclear applications.
This project will allow European scientists and institutions to improve the nuclear data needed for simulation tools in order to increase the accuracy of code assessments and consequently to better focus the design of expensive experiments. In particular, a e-mail: pablo. romojaro@externos. ciemat. es the main objective of Work Package 10 is to improve MYRRHA-relevant nuclear data in order to reduce the reactor parameter uncertainties derived from them. Within this framework, a neutron-induced nuclear data sensitivity and uncertainty (S/U) analysis of the latest MYRRHA design has been performed as a first task and a list of the most important nuclides and quantities has been obtained. As a second task, a detailed analysis of the existing experimental data and evaluations for the quantities included in the list has been carried out, investigating the impact on k e f f of quantities from different existing nuclear data libraries for different nuclides, reactions and energy regions on the MYRRHA MOX critical core model.
Bismuth and lead have been chosen as the main objects of study for improvement of nuclear data for MYRRHA since they are of vital importance and are not covered by the CIELO pilot project  [4]. New experimental data in the resonance region will be obtained at the GELINA facility. In this paper, the results of the S/U analysis for the MOX critical core are presented. An overview of the experimental data and existing evaluations for Pb and Bi is given and some issues spotted in the evaluations are discussed.
Sensitivity and uncertainty analysis MYRRHA's updated core design is described in detail in Ref. [5]. For this study a simplified model  [6] , homogenised on fuel assembly level, has been used. The layout of the core is shown in Fig. 1. The procedures included in some of the state-of-theart computer codes dedicated to reactor core analyses have been employed in this work. In particular, the calculations have been performed with the SCALE6. 2 system  [7] , in its third beta release, the MCNP6. 1 code  [8]  and the SUSD3D code  [9] , part of the XSUN-2013 system  [10]. Evaluated neutron-induced data from ENDF/B-VII. 0  [11]  have been used by SCALE and MCNP, and from ENDF/B-VII. 1  [12]  by SUSD3D. Additionally, a cylindrical geometry model of MYRRHA has been constructed to be used in the transport calculations performed by SUSD3D.
This model has been developed using equivalent concentric cylinders conserving the total mass of each material, so no further homogenization was required, and adjusting the arrangement of the cylinders in order to represent the MYRRHA critical core configuration with high-fidelity. The sensitivity analysis allows identifying the most important nuclides and reactions from the criticality safety neutronic design point of view. In Fig. 2 , the Integrated Sensitivity Coefficients (ISC) of the major contributors to k e f f uncertainty due to uncertainties in nuclear data are represented. The key quantities in MYRRHA neutronics are 239 Pu ν, 239 Pu(n,f) and 238 U(n,γ ). The ISC values are very close between codes and libraries, most of them with a relative difference smaller than 4%. However, 238 U(n,el), obtained by SUSD3D, has a difference of 51% to the value provided by SCALE, which can be attributed to omitting the implicit sensitivity contribution by SUSD3D.
Comparison of evaluated libraries for lead and bismuth Taking into account the flexibility of the MYRRHA facility in providing various irradiation environments, in addition to the list of MYRRHA-relevant isotopes and reactions presented in the previous section it is expedient to also consider the following quantities: 208 Pb(n,el) and (n,inl); and 209 Bi(n, γ ) and (n,inl). To perform the comparison, the JEFF-3. 2 [16]  library has been taken as the reference. The other considered libraries are ENDF/B-VII. 1  [11]  and JENDL-4. 0  [17]. The EXFOR database  [18]  has been used to search for experimental transmission time-of-flight (TOF) data for bismuth and lead, particularly focusing on experiments in the resolved and unresolved resonance energy ranges. The results available in EXFOR were derived from experimental data using the SAMMY code  [19] , so resolution and broadening were considered.