dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements We would like to thank  Ewine van Dishoeck  for her useful insights and suggestions. Publisher's Note Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations. Open Access This article is licensed under a Creative Commons Attribution 4. 0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder.
The SOLPS-ITER code suite is used worldwide for plasma edge modeling, the interpretation of experiments, as well as for the design of the ITER divertor. The numerical scheme of the plasma solver of the code, B2. 5, is based on the assumption of perfectly orthogonal grids in the poloidal plane, aligned with the magnetic field, while in practice grids are often strongly distorted to match divertor target shapes. Neglecting these grid distortion leads to qualitatively and quantitatively incorrect results for fluid neutral simulations, and may affect results in cold (detached) divertors even when using kinetic neutral simulations. In this contribution, we present the first results of a newly implemented 9-point stencil in B2. 5 to properly handle misaligned grids. The new scheme is then applied to fluid neutral simulations of a well-diagnosed and previously modeled Alcator C-Mod discharge.
Introduction The SOLPS code suite has been used as the workhorse for the design of the ITER divertor  [1]. The latest version of the code, SOLPS-ITER  [2, 3] , is based on an up-to-date version of EIRENE and includes the advanced fluid drifts model from SOLPS5. 2. One of the ongoing developments of the code aims at enabling the use of grids extending up to the vessel wall. In this contribution, we report on a part of this effort that involves improving the discretization of the underlying plasma equations. Presently, the plasma solver in the code, B2. 5, assumes perfectly orthogonal grids in the poloidal plane, aligned with the magnetic field. However, such grids are not compatible with the strongly shaped divertor targets in most current machines, and as foreseen on ITER. Therefore, in practice the grids are only aligned with the magnetic surfaces, but radial lines may be far from orthogonal to the field.
PoS(ICRC2019)871 Follow-up of ANTARES neutrino alerts D. Dornic also had optical follow-ups with TAROT and ROTSE telescopes. No optical transient were identified in the error box of the two neutrinos. Transient or strongly variable radio sources consistent with the neutrino positions are looked for using MWA archival data at frequencies between 118 and 182 MHz, taken 20 days prior to, at the same time as, and up to a year after the neutrino triggers. As no radio counterparts are detected, 5σ upper limits have been computed for low-frequency radio emission of ∼10 37 erg s -1 for progenitors at 20 Mpc. If the neutrino sources are instead not in nearby galaxies, but originate in binary neutron star coalescences, the limits constrain the progenitors to be at z ≥ 0. 2. The analyses of the two others neutrino alerts are in progress.
Acknowledgements This work was supported by recurrent funding from the  Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA)  and specific fundings through the  CAR-NOT program  ( LETI institute, ABCDE grant ). Authors wish to thank  Lee Bernick  ( MIT-Giant exchange student program ) for the bacteria experiments and  Pierre Marcoux  ( LETI-CEA ) for the fluorescent E. coli cultures.
15 ± 0. 05 pc all along its length  (André et al. 2016) , within ∼50% of the typical inner filament width observed with Herschel in nearby clouds  (Arzoumanian et al. 2019). NGC 6334 is a very active star-forming region at a distance d ∼ 1. 7 kpc, which contains 150 OB stars and more than 2000 young stellar objects  (Persi & Tapia 2008; Russeil et al. 2013; Willis et al. 2013; Tigé et al. 2017) , for a total gas mass of ∼2. 2×10 5 M. Here, thanks to the high angular resolution and sensitivity of Atacama Large Millimeter Array (ALMA) data at 3 mm, we investigate the density and velocity sub-structure of the massive NGC 6334 filament and compare the results with those obtained for nearby, lower-mass star-forming filaments. The paper is organized as follows. In Sect. 2, we describe our ALMA observations of NGC 6334 in both the N 2 H + (1-0), HC 3 N(10-9), HC 5 N(36-35), CH 3 CCH(6 0 -5 0 ), H 2 CS(3 1,2 -2 1,1 ) lines and the 3.
The complex gain calibration was carried out using the quasar J1713-3418 with the 12m array and the quasar J1717-3342 with ACA. Absolute flux calibration was achieved by ob-serving two solar system objects (Callisto and Titan) with the 12m array and planets (Mars and Neptune) with ACA. Calibration and data reduction were performed with the Common Astronomy Software Application (CASA) package (version 4. 5. 3 for 12m data calibration and imaging, version 4. 6. 0 for 7m data calibration). For imaging, we adopted the Briggs weighting scheme with a robust parameter of 0. 5, as a good compromise between maximizing angular resolution and sensitivity to extended structures. The resulting synthesized beam sizes (∼3 , corresponding to 0. 025 pc) and rms noise levels for each line and the continuum are summarized in Table  1.
Although contamination of the 3. 1 mm continuum data by free-free emission is an issue, compact sources robustly detected in both 3. 1 mm continuum and N 2 H + emission are unlikely to be affected. We estimated the mass (M tot ) of each compact continuum source, under the assumption that all of the 3. 1 mm continuum emission arises from dust and that the emission is optically thin. The mass was obtained from the integrated 3. 1 mm flux density S tot 3. 1mm derived from two-dimensional Gaussian fitting in the 12m+7m continuum image 3  using the formula: where d, κ 3. 1mm , and B 3. 1mm (T d ) are the distance to the target, the dust opacity (per unit mass of gas + dust), and the Planck function at dust temperature T d , respectively. We adopted the same dust opacity law as the Herschel Gould Belt survey team, namely κ λ = 0.
3  and Sect. 4. 1). In the following, we therefore regard these 26 compact 3. 1 mm continuum sources as dense cores. Extraction of velocity-coherent fiber-like features with getfilaments. We extracted filamentary structures from the ALMA N 2 H + data cube after subtraction of compact N 2 H + emission using the getfilaments algorithm (e. g. , Men'shchikov 2013). Each N 2 H + velocity channel map was decomposed into a set of spatially-filtered single-scale images from small (3 ) to large (16 ) scales. At each scale, the algorithm separated filamentary structures and compact sources, and extracted significant filamentary structures in the source-subtracted image component. All extracted filamentary structures were merged into a single image per velocity channel map. We selected only filamentary structures whose >90% pixels along the crest were detected above the > 3σ level in each channel.
As the velocity resolution of our ALMA N 2 H + data (0. 2 km s -1 , that is, less than the isothermal sound speed in the cloud) should be sufficient to resolve the velocity width of the filament, we also imposed that a selected filamentary structure should be detected in at least two consecutive velocity channels. By comparing velocity-channel maps, we therefore associated filamentary structures with matching spatial distributions among channels (see Appendix D). Our procedure is similar to that used by  Hacar et al. (2013)  to trace velocity-coherent structures in data cubes, in the sense that both methods work in position-position-velocity (PPV) space 5. In this way, we identified five distinct fiber-like structures, labeled F-1 to F-5, whose crests are displayed in Fig. 4  and Fig. 5. Examples of individual N 2 H + (HFS 1) spectra across the two main fiber-like structures F-1 and F-2 are shown in Fig.
Due to the lower effective sensitivity of the H 2 CS(3 1,2 -2 1,1 ) data, the NGC 6334 filament is broken up into two segments in H 2 CS. The H 2 CS filamentary structures coincide with the northern and southern parts of the filamentary structures traced in other lines. Owing to the lower line intensities and/or lower spectral resolution of our data in HC 3 N, HC 5 N, CH 3 CCH, and H 2 CS, we could not carry out as detailed a PPV analysis in these lines as in N 2 H +.
2015). In both NGC 6334 and Aquila, cores were extracted from the data using the same algorithm getsources. For easier comparison, the Aquila CMF was renormalized to have a peak value comparable to that of the NGC 6334 CMF. All error bars correspond to √ N counting statistics. The magenta vertical dashed line indicates the estimated 90% completeness level (2. 6 M ) of our ALMA 3. 2 mm census of dense cores in the NGC 6334 filament. The blue vertical dashed line marks the 90% completeness level of the Aquila CMF (0. 2M ). (The blue shaded area reflects uncertainties associated with the uncertain classification of starless cores as bound or unbound objects. ) scribe the collapse of an isothermal filament under the effect of self-gravity (e. g  Inutsuka & Miyama 1992 , 1997). With a typical inner width of 0.
These two distinct fragmentation scales are suggestive of two fragmentation modes: a cylindrical mode corresponding to groups of cores, and a spherical, Jeans-like mode corresponding to cores within groups. 5. We also identified five fiber-like, velocity-coherent substructures within the filament by applying the getfilaments algorithm to the ALMA N 2 H + (1-0) data cube. The typical length of these fiber-like structures is 0. 5 pc and the projected velocity difference between them is ∼ 0. 8 km s -1. Only two or three of these five velocity-coherent features are well aligned with the NGC 6334 filament and may represent genuine, intertwined fiber sub-structures. The other two detected velocity-coherent features may rather trace accretion flows onto the main filament. 6. With the important exception of the typical core mass (which is here an order of magnitude higher), the fragmentation properties and velocity structure of the massive ( > ∼ 500 M /pc) filament in NGC 6334 are remarkably similar to the properties observed by  Hacar et al.
Acknowledgements. This paper makes use of the following ALMA data: ADS/JAO. ALMA# 2015. 1. 01404. S. ALMA is a partnership of  ESO  (representing its member states),  NSF (USA)  and  NINS (Japan) , together with  NRC (Canada) , NSC  and  ASIAA (Taiwan) , and  KASI (Republic of Korea) , in cooperation with the  Republic of Chile. The Joint ALMA Observatory is operated by  ESO ,  AUI/NRAO  and  NAOJ. This work was supported by the  ANR-11-BS56-010  project " STARFICH " and the  European Research Council  under the European Union's  Seventh Framework Programme  ( ERC Advanced Grant  Agreement no. 291294 -'ORISTARS' ). YS also received support from the  ANR  project  NIKA2SKY  (grant agreement  ANR-15-CE31-0017 ). This work was supported by  NAOJ ALMA   Scientific Research Grant Numbers   2017-04A.
(8) In the following, we assume a flat prior on H 0 within [20,140] km s -1 Mpc -1 , unless otherwise stated. This is a very broad prior, covering a range much larger than current estimates of H 0. This choice was made as a compromise between the following aspects: i) a result which is mostly informed by the LVC and DES data rather than by external constraints, ii) a result which can be compared with the first standard siren estimate, and iii) a complete galaxy sample which contains most of the stellar mass within the localization volume, to minimize the chance of missing the real host galaxy. As explained in more detail in §4, the redshift cut is related to the H 0 prior range, and in order to explore higher values of H 0 , one needs to include higher redshift galaxies, and make a higher luminosity cut to preserve the volume limited sample.
2018). Future dark siren measurements will require complete galaxy catalogs. A wide field galaxy catalog with a DES-like depth is currently available only for ∼ 1/8 of the sky. However, DES can be complemented with other datasets taken with DECam (such as the Blanco Imaging of the Southern Sky, BLISS, and the Dark Energy Camera Legacy Survey, DECals), to cover the whole Southern sky to a good depth (r ∼ 23. 4, 5σ depth). An even deeper survey with more precise photo-z's, such as the Large Synoptic Survey Telescope (LSST; LSST Dark Energy Science Collaboration 2012), would be of great value for further improving these constraints. At the expected level of precision from hundreds of events (< 10%), systematics will play an important role. In future work, we plan to incorporate systematic uncertainties in our simulated data studies, in order to prepare for precision cosmology analyses on real data.
Based in part on observations at  Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory , which is operated by the  Association of Universities for Research in Astronomy (AURA)  under a cooperative agreement with the  National Science Foundation. The DES Data Management System is supported by the  NSF  under Grant Numbers  AST-1138766  and  AST-1536171. The DES participants from Spanish institutions are partially supported by  MINECO  under grants  AYA2015-71825 ,  ESP2015-88861 ,  FPA2015-68048 , and  Centro de Excelencia   SEV-2016-0588 ,  SEV-2016-0597  and  MDM-2015-0509. Research leading to these results has received funding from the  ERC  under the  EU's 7 th Framework Programme including  grants  ERC 240672 ,  291329  and  306478. We acknowledge support from the  Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) , through project number  CE110001020.
Additional support for Advanced LIGO was provided by the  Australian Research Council. The authors gratefully acknowledge the  Italian Istituto Nazionale di Fisica Nucleare (INFN) , the  French Centre National de la Recherche Scientifique (CNRS)  and the  Foundation for Fundamental Research on Matter  supported by the  Netherlands Organisation for Scientific Research , for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the  Council of Scientific and Industrial Research of India , the  Department of Science and Technology, India , the  Science & Engineering Research Board (SERB), India , the  Ministry of Human Resource Development, India , the  Spanish Agencia Estatal de Investigación , the  Vicepresidència i Conselleria d'Innovació ,  Recerca i Turisme  and the  Conselleria d'Educació i Universitat del Govern de les Illes Balears , the  Conselleria d'Educació, Investigació, Cultura i Esport de la Generalitat Valenciana , the  National Science Centre of Poland , the  Swiss National Science Foundation (SNSF) , the  Russian Foundation for Basic Research , the  Russian Science Foundation , the  European Commission , the  European Regional Development Funds (ERDF) , the  Royal Society , the  Scottish Funding Council , the  Scottish Universities Physics Alliance , the  Hungarian Scientific Research Fund (OTKA) , the  Lyon Institute of Origins (LIO) , the  Paris Île-de-France Region , the  National Research, Development and Innovation Office Hungary (NKFIH) , the  National Research Foundation of Korea, Industry Canada  and the  Province of Ontario  through the  Ministry of Economic Development and Innovation , the  Natural Science and Engineering Research Council Canada , the  Canadian Institute for Advanced Research , the  Brazilian Ministry of Science, Technology, Innovations , and Communications, the  International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR) , the  Research Grants Council of Hong Kong , the  National Natural Science Foundation of China (NSFC) , the  Leverhulme Trust , the  Research Corporation , the  Ministry of Science and Technology (MOST), Taiwan  and the  Kavli Foundation.
The first five quantities are calculated in the CM frame. The neural network training is performed with simulated signal and qq events. Signal and background samples are generated with the EvtGen program  [16] ; for signal we assume a uniform decay in phase space. A GEANT-based  [17]  simulation is used to model the detector response. We require the neural network output (C NB ) to be greater than -0. 2 to substantially reduce the continuum background. For both decays, the relative signal efficiency due to this requirement is approximately 91% and the achieved continuum suppression is close to 84%. The remainder of the C NB distribution strongly peaks near 1. 0 for signal, making it challenging to model it analytically. However, its transformed variable C ′ NB = ln C NB -C NB,min C NB,max -C NB , (2) where C NB,min = -0.
We thank the  KEKB group  for the excellent operation of the accelerator; the  KEK cryogenics group  for the efficient operation of the solenoid; and the  KEK computer group , and the  Pacific Northwest National Laboratory (PNNL) Environmental Molecular Sciences Laboratory (EMSL) computing group  for strong computing support; and the  National Institute of Informatics , and  Science Information NETwork 5  ( SINET5 ) for valuable network support. We acknowledge support from the  Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan , the  Japan Society for the Promotion of Science (JSPS) , and the  Tau-Lepton Physics Research Center of Nagoya University ; the  Australian Research Council  including grants  DP180102629 ,  DP170102389 ,  DP170102204 ,  DP150103061 ,  FT130100303 ;  Austrian Science Fund  under Grant No.
P  26794-N20 ; the  National Natural Science Foundation of China  under Contracts No. 11435013 , No. 11475187 , No. 11521505 , No. 11575017 , No. 11675166 , No. 11705209 ;  Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS) , Grant No. QYZDJ-SSW-SLH011 ; the  CAS Center for Excellence in Particle Physics (CCEPP) ; the  Shanghai Pujiang Program  under Grant No. 18PJ1401000 ; the  Ministry of Education, Youth and Sports of the Czech Republic  under Contract No. LTT17020 ; the  Carl Zeiss Foundation , the  Deutsche Forschungsgemeinschaft , the  Excellence Cluster Universe , and the  VolkswagenStiftung ; the  Department of Science and Technology of India ; the  Istituto Nazionale di Fisica Nucleare of Italy; National Research Foundation (NRF)  of  Korea  Grants No. 2015H1A2A1033649 , No.
Measurements. The scanning tunneling spectroscopy measurements were performed in-situ in a home-made apparatus at a base temperature of 320 mK and in ultrahigh vacuum in the low 10 -11 mbar range. Mechanically sharpened Pt/Ir tips were used. The bias voltage was applied to the sample with respect to the tip. Typical set-point parameters for topography are 20 pA at V = -50 mV. Typical set-point parameters for spectroscopy are 120 pA at V = -5 mV. The electron temperature was estimated to be 350 mK. The tunneling conductance curves dI/dV were numerically differentiated from raw I(V ) experimental data. Each conductance map is extracted from a set of data consisting of spectroscopic I(V ) curves measured at each point of a 220×220 grid, acquired simultaneously with the topographic image. Each I(V ) curve contains 700 energy points in the [-0.
Results: The population included 106 children (6. 5%) aged <2 years, 815 (50. 0%) aged 2 to <12 years and 710 (43. 5%) aged 12 to <18 years, with a mean (AE SD) age of 10. 2 (AE 4. 9) years. Central nervous system exploration was the most frequent MRI type (80. 4%) and main risk factors were any stage of renal insufficiency (9. 8%) and allergies (5. 2%). Only one AE (vomiting) that was deemed doubtfully related to gadoterate meglumine was observed. No suspicions of NSF were reported. Good to very good image quality was obtained for 98. 4% of pediatric patients and diagnosis was established in 99. 6% of cases. Conclusion: This study confirmed the good safety profile of gadoterate meglumine in routine practice in a large pediatric population. The study is registered on https://clinicaltrials.
Methods. We observe "Jupiter as an exoplanet" by dividing a LOFAR observation of Jupiter by a down-scaling factor and adding this observation to beam-formed data of the "sky background". Then we run this artificial dataset through our total intensity (Stokes-I) and circular polarization (Stokes-V) processing and post-processing pipelines and determine up to which down-scaling factor Jupiter is still detected in the dataset. Results. We find that exoplanetary radio bursts can be detected at 5 pc if the circularly polarized flux is 10 5 times stronger than the typical level of Jupiter's radio bursts during active emission events (∼ 4 × 10 5 Jy). Equivalently, circularly polarized radio bursts can be detected up to a distance of 20 pc (encompassing the known exoplanets 55 Cnc, Tau Boötis, and Upsilon Andromedae) assuming the level of emission is 10 5 times stronger than the peak flux of Jupiter's decametric burst emission (∼ 6 × 10 6 Jy).
The reason for this is that the upper limit depends on the detection method. In this work, we present a detection tool that integrates the processing steps described in  Turner et al. 2017 (RFI-mitigation, normal- ization by the time-frequency (t-f) response function, t-f integration) and a series of sensitive observables based on the work of  Vasylieva (2015). In order to test, validate, and quantify the sensitivity reached with this tool, we apply it to a LOFAR observation of Jupiter's magnetospheric radio emission in which the signal from Jupiter is attenuated. The idea is simple: we observe Jupiter, divide its signal by a fixed factor before adding it to an observation of "sky background", thereby creating an artificial dataset best described as "Jupiter as an exoplanet". We then run our pipeline and check whether the (attenuated) radio signal from Jupiter is detected.
1c  and 1d. While most of the analysis was done using Obs #2 for the "sky background", we also used two other dates of observations with two OFF-beams to verify our results. The third dataset was taken on February 26, 2017 from 01:16 to 04:16 UT (hereafter Obs #3) and was pointed at the same OFF-beam positions as Obs #2. This date had far worse RFI conditions than Obs #2 and also had noticeable large-scale scintillation due to a disturbed ionosphere. The fourth dataset was taken on September 28, 2016 from 23:00 to 04:00 UT (hereafter Obs #4; Table  1 ). Obs #4 was comparable in quality to Obs #2 (no large scale scintillation patterns) and RFI conditions but was pointed at a different part of the sky.
Note that equations (  2 ) and (3) can be used to add the signal (of Jupiter or other) observed with one telescope in a given frequency range to the background recorded with another telescope in another frequency range, as long as the SEFD of the two telescopes in their respective spectral ranges are known. Equations (4) and (  5 ) are the application for the considered LOFAR-LBA observations. The Jupiter signal thus transferred retains its absolute intensity (e. g. in Jy). For step (ii) we use an observation of Jupiter simultaneously taken to the LOFAR one, carried out at the NDA. For this observation, the NDA observes simultaneously in right-hand (RH) and left-hand (LH) circular polarizations from 10 to 40 MHz in 400 spectral channels at a time resolution of 1 second. Hourly calibration sequences on noise sources of known flux density are embedded in the data and allow us to calibrate the observations in absolute flux density (Jy), with an accuracy ∼ 20%.