dataesr/scientific-paragraphs-categorization huggingface dataset:
Considering that the percentage of children who were infected with EVD during the 2014-2015 epidemic in West Africa was 16% and these children had a higher case fatality rate than adults  [13] , the results from this trial will provide important information to guide the vaccination of children in future epidemics such as the one ongoing in DRC where children are being vaccinated. Whether the different vaccination approaches are able to confer durable antibody responses after vaccination remains an important question and currently limited data exist to address this question. The PREV AC and PREVAC-UP trials will evaluate the durability of immune responses with follow-up of the participants up to 60 months after vaccination. These data will provide important information when considering a preventive vaccination strategy for at-risk populations, including health-care and front-line workers who may face ongoing exposure to cases over repeated outbreaks.
Funding This research was supported in part by the  National Institutes of Health (NIH)  and by  Institut national de la santé et de la recherche médicale (Inserm)  and by the  London School of Hygiene and Tropical Medicine (LSHTM). Funding was provided in part by  NIAID  under  NCI  contract  HHSN261201500003I  through the  Frederick National Laboratory for Cancer Research. The content of this publication does not necessarily reflect the views or policies of the  Department of Health and Human Services , nor does mention of trade names, commercial products, or organizations imply endorsement by the  US Government. This project has received funding from the  Innovative Medicines Initiative 2 Joint Undertaking  under grant agreement No  115854. This Joint Undertaking receives support from the  European Union 's  Horizon 2020 research  and.
The Clinical Problem Coronary heart disease (CHD) is one of the leading causes of death in many countries, as it is estimated that each minute, a myocardial infarction (MI)-related death occurs  [1]. Other than first or recurrent symptomatic CHD registered as hospitalized MI or cardiacrelated deaths, about 20% of events still remain silent  [2, 3]. Each year, scientifical societies estimate 515,000 new attacks and 205,000 recurrent attacks, with an average first presentation age of 64. 9 years for men and 72. 3 years for women  [2, [4] [5] [6]. Data from the Framingham Heart Study (FH) revealed that CHD constitutes more than half of all cardiovascular events in the aged population  [2, 3]. Fortunately, early reperfusion strategies (percutaneous coronary intervention, PCI) and the decline in ST-elevation myocardial infarction (STEMI) presentation (from 133 to 50 cases per 100,000 person/years) have reduced CHD-associated mortality rates.
Acknowledgment: The authors are grateful for the scientific and technical support from the  Australian Centre for Microscopy and Microanalysis (ACMM)  as well as the  Microscopy Australia node at the University of Sydney. Thanks  Dr Xianghai An  from the  University of Sydney  for the fruitful discussion on the mechanical behaviour of materials. We are grateful for A/Prof. John Daniels , and PhD candidates  Fan Ji  and  Tongzheng Xin  from the  University of New South Wales  for helpful discussions regarding oxygen vacancies in perovskite oxides, and  Dr. Jun Luo  from  TRS Technologies  for providing single crystal samples. Thanks  Prof. Gustau Catalan  from  Catalan Institute of Nanoscience and Nanotechnology (ICN2 ) for the discussion of flexoelectricity. This work was supported by the  Australian Federal Government  through the  Next Generation Technologies Fund , and the  DST Strategic Research Initiative in Advanced Materials and Sensors.
A. Magnetization measurement The magnetic hysteresis loop was measured for (I)-(V) to investigate a reduction in the saturation magnetization as decreasing Fe thickness. The data were normalized with the volume of the Fe layers, where the "magnetically dead" part, 1. 1 nm per bilayer, estimated by the PNR analysis, was subtracted from the nominal Fe thickness given by the sputtering rate. (II) and (III) kept the same saturation magnetization as (I) as shown in Fig. 3(a). In addition, H c became smaller with decreasing Ge thickness. H c and μ i were 1. 5 kA/m and 2:6 Â 10 2 for (I), whereas 0. 24 kA/m and 1:6 Â 10 3 for (III). A thinner Fe layer of (IV) resulted in a reduction in the saturation magnetization. (V) with the thinnest Fe layer was not ferromagnetic at 300 K. The magnetization of the samples in an external field of 8.
ACKNOWLEDGMENTS The authors acknowledge the  J-PARC MLF  for providing the beam time and support (Proposal Nos. 2018B0191 ,  2019A0057 ,  2020A0192 , and  2020B0196 ). R. M. thanks  Mr. M. Akiyama  ( Interface Co. Ltd. ) for support with the multilayer deposition. The field-cooled magnetization was measured by using a SQUID magnetometer at the  Comprehensive Research Organization for Science and Society (CROSS) user laboratories. The technical assistance for the field-cooled magnetization measurement provided by  Dr. M. Ishikado  ( CROSS ) is gratefully acknowledged. This research was supported in part by the  JSPS KAKENHI  (Grant No. 19K12647 ).
ACKNOWLEDGMENTS This research has been supported by the  Spanish Ministry of Science, Innovation and Universities  through grants " Juan de la Cierva -Incorporación "  IJC2018-037897-I  and  PID2019-111436RB-C22 , by the  Agència Valenciana de la Innovació  through grants  INNVA1/2020/92  and  INNCON/2021/8 , and by the project  HYPERMETA  funded under the program Étoiles Montantes of the  Région Pays de la Loire. R. D. M. -H acknowledges support from  Colciencias Scholarship program  No. 727-2015.
To provide a population representative of the general French adult population, proportional quotas were used based on sex, age, socioeconomic status, and regional distribution (as described in Table  1 ) according to data previously published by INSEE. Collected data were obtained via the Internet from a random selection of 2036 French Internet users over 18 years old who agreed to participate. An Internet questionnaire was completed by each participant, but if contact was lost or the questionnaire was not totally completed, another participant with similar characteristics (sex, age, socioeconomic status, and regional distribution) was selected. No missing data were allowed, and respondents had to answer all questions. However, before answering the questionnaire, each respondent was informed of the nature of the survey, that their anonymity would be respected, and that collected information would not allow identification.
5 Interestingly, stabilization is currently being observed. Few data on allergies in the French population are available. A recent study assessed the risk of allergic disease among 714 children of the Paris birth cohort, consisting of 3840 full-term and healthy singletons born from parents living in Paris or nearby suburbs. 6 In this study, a profile of early and transient sensitization to foods that increased the risk of asthma later in childhood was identified (4. 9%). Children strongly sensitized to house dust mites at 8 to 9 years of age (9. 0%) had the highest risks of asthma and allergic rhinitis. Finally, the sensitization profile for timothy grass pollen at 8/9 years of age (5. 3%) was related to respiratory allergic diseases, as was early onset and a persistent sensitization profile (4.
LC-MS studies and data analysis The quantification of ITZ and OH-ITZ (the major active metabolite of ITZ in humans  (Heykants et al. , 1989)  as well as in rats  (Yoo et al. , 2000) ) was performed for all plasma samples. For the bioanalytics, a Waters e2695 Separation Module coupled to a Waters ACQ-QDA Detector was used. MS-measurements were performed with a capillary voltage of 0. 8 kV and a cone voltage of 15 V. A Waters XBridge® Shield RP18 column (3. 5 μm, 2. 1 mm × 100 mm, 130 Å) was installed and the column temperature set to 30 • C. Non-isocratic conditions were applied to measure the ITZ and OH-ITZ plasma concentrations precisely. The compositions of the mobile phases and the non-isocratic conditions are described in Tables  2  and 3. For detection, the positive ion electrospray ionization mode was used.
Data analysis The maximum plasma concentration (c max ) and the associated time t max were determined directly from the plasma concentration profiles. The determination of the area under the curve (AUC) of the plasma concentration profiles were estimated by trapezoidal integration to the last sampling point (24 h). The evaluation of the bioavailability was performed by using the sum of the AUCs of ITZ and OH-ITZ (AUC sum ). The statistical comparison of c max and AUC ITZ were accomplished with a one-way analysis of variance (ANOVA) and post hoc Tukey's multiple comparison test. P values of <0. 05 were considered as statistically significant.
Declaration of Competing Interest This work was funded by Nisso Chemical Europe GmbH. University of Bonn and Nisso Chemical Europe GmbH participated in study design, research, interpretation of data, writing, data collection, analysis, reviewing, and approving the publication. Edmont Stoyanov is an employee of Nisso Chemical Europe GmbH and does not own stocks on Nippon Soda Ltd. Rafael Bachmaier, Marius Monschke, Anna K. Krome and Thilo Faber are PhD students and Karl G. Wagner and Alf Lamprecht are professors at the University of Bonn. Yann Pellequer is an employee of the University of Franche-Comté in Besancon. They have no additional conflicts of interest to report.
Data and Methodology The data studied in this paper are radar data at Roissy-Charles-de-Gaulles airport (CDG) from the French Air Navigation Service Provider (DSNA); Among all airports whose operations are assigned to DSNA, CDG was chosen because it was the only airport that maintained sufficient traffic during the Covid outbreak to obtain statistically representative results. The data was collected during two time periods: a reference period before COVID-19 from 01 to 31 May 2019 (accounting for 21 895 landings), and a study period under COVID-19 from 16 March to 20 April 2020 (accounting for 4 583 landings). The reference period covering May 1st to May 31st was the available period that best respected the seasonality studied during the COVID-19 period. The data contains landing trajectories (longitude, latitude, altitude, ground speed, vertical speed) as well as meta-information such as aircraft type, airline, and the runway used.
Introduction Photometry and spectroscopy provide critical information on type II supernova (SN). They characterize, for example, the timescale over which the energy stored in the ejecta is released, the color of the escaping radiation, the level of ionization of the spectrum formation region, and the composition of the ejecta. Such data do not, however, provide direct constraints on the geometry of the explosion. Lacking spatially resolved observations for type II-Plateau (II-P) SNe, spectropolarimetry is the best technique to provide constraints on the morphology of SN ejecta, especially at early times  (Shapiro & Sutherland 1982). The polarization is linear, caused by scattering with free electrons, and is typically less than 1% in the continuum  (Wang & Wheeler 2008). The current spectropolarimetric dataset of type II SNe is limited to 10-20 objects, mostly because of the scarcity of nearby events.
Although intimately associated with ejecta asymmetry,  Dessart & Hillier (2011)  suggest that the polarization peak at the onset of the nebular phase is caused by a radiative transfer effect as the ejecta turns optically thin,  A&A 651, A19 (2021)  while its subsequent evolution reflects the drop in ejecta optical depth. Chornock et al. (2010)  presented spectropolarimetric observations for a few more type II SNe, confirming the general trend observed for SN 2004dj. It thus appears that type II SNe typically show a temporal increase in continuum polarization through the photospheric phase, reaching a maximum at the onset of the nebular phase, and subsequently dropping. To supplement this dataset, we initiated a VLT-FORS spectropolarimetric program in 2008. Over a number of years, we gathered multiepoch high quality observations for SNe 2008bk, 2012aw, and 2013ej, as well as a more sparse dataset for a few additional objects.
Although this dataset has been presented in a terse format previously  (Leonard et al. 2012 (Leonard et al. , 2015)) , we are now in a position to present the observations in more detail, and with modeling results. We start in this paper with SN 2012aw. In the next section, we summarize the results from the polarization modeling of  Dessart & Hillier (2011). Section 3 presents the numerical approach used for the present study, which is also presented in detail in  Hillier & Dessart (in prep. ). As in  Dessart & Hillier (2011) , we adopt a 2D axisymmetric ejectum but we now model the polarized spectrum for the whole optical range rather than focus on isolated lines and the overlapping continuum. In Sect. 4, we present the spectropolarimetric observations of SN 2012aw that we collected with VLT-FORS while Sect.
1D-X1 SN2012aw Fig. 1. Multiepoch spectral comparison between SN 2012aw and our reference 1D CMFGEN model 1D-X1 (see  Sect. 3. 1). The data correspond to the observed total flux for SN 2012aw obtained with VLT-FORS in spectropolarimetric mode. The model is redshifted, reddened, and then normalized to the observed flux at 7000 Å. The V-band brightness offset, calculated from the observed photometry  (Bose et al. 2013 ; corrected for distance and extinction) and the model photometry, is given for each epoch and is typically on the order of 0. 1 mag. This model is named x1p5 in  Hillier & Dessart (2019)  and is our best match model for SN 2012aw. Hillier  & Dessart 2019 ) and corresponds to a 15 M zero age main sequence star, exploded to yield an ejecta kinetic energy of 1. 2 × 10 51 erg, an ejecta mass of 12.
12 M , and a 56 Ni mass of 0. 056 M. Figure  1  illustrates the agreement in the optical range (the data are from our spectropolarimetric VLT-FORS program) between model 1D-X1 and SN 2012aw, and also the fact that the model is within about 0. 1 mag of the observed V band magnitude throughout the high brightness phase (there is a similar offset at nebular times; see  Hillier & Dessart 2019). This agreement suggests that a spherical ejecta model yields a satisfactory match to the photometric and spectroscopic observations of SN 2012aw. The deviations from spherical symmetry that we introduce must therefore remain small enough not to deteriorate the agreement between observations and the results for model 1D-X1.
The VLT-FORS dataset We obtained seven epochs of spectropolarimetry of the Type II-P supernova SN 2012aw using the European Southern Observatory's Very Large Telescope (VLT) at Cerro Paranal in Chile  (Appenzeller et al. 1998)   2. All observations were made with the FOcal Reducer and low dispersion Spectrograph (FORS2), mounted at the Cassegrain focus of the Antu (UT1) telescope. The data sample days 16-120 following the date of explosion (16. 09 March, 2012 UT) estimated by  Bose et al. (2013). Details of the observational epochs, instrumental setup, exposure times, and observational conditions are given in Table  2. The data are presented in Fig. 5. Each complete observational sequence consisted of four separate exposures with the half-wave retarder plate positioned at each of 0, 45, 22.
1990; Berdyugin et al. 1995)  at every epoch, and always found it to be null to within 0. 05%. For each epoch, the normalized Stokes q and u parameters derived from all complete observational sequences were 4 http://www. eso. org/instruments/fors/inst/pola. html combined according to their statistical weights, with new uncertainties calculated. We then removed the interstellar polarization derived in Sect. 4. 2, removed a redshift of 778 km s -1 (de  Vaucouleurs et al. 1991, via NED) , rebinned to 5 Å bin -1 , and created a final, rest-frame dataset with a wavelength range of 4350-9150 Å. We also computed results binned to 15, 25, 50 and 100 Å bin -1 for presentation purposes. To generate the total flux spectrum for each epoch, a final correction for telluric absorption bands  (Wade & Horne 1988 ) was made.
To illustrate the continuum polarization as a function of time we show in the left panel of Fig. 6  the normalized Stokes q and u measurements for all seven epochs in three spectral regions devoid of strong lines around 6000, 7000, and 8000 Å. All measurements lie in a single quadrant of the (q, u) plane, and to first order lie along a straight line. The biggest departure from a straight line occurs for the data at 120 d. The offset is significant, although the data at this epoch also has the worst signal-tonoise ratio. If SN 2012aw were axisymmetric all polarization data would lie along a straight line in the (q, u) plane, and, in the absence of interstellar polarization, would pass through the origin. The presence of a dominant axis in the data sets indicates that SN 2012aw must possess a strong degree of axial symmetry.
This is done to put most of the observed polarization in q. The rotated fluxes are then given by q rot = q cos(2θ rot ) + u sin(2θ rot ) (  6 ) and u rot = -q sin(2θ rot ) + u cos(2θ rot ). ( 7 ) The data of SN 2012aw, corrected for interstellar polarization, yield an observed polarization angle of 118 deg in the plane of the sky. However, we choose to rotate the Stokes vectors by the angle orthogonal to this -that is, of 28 deg -in order to produce a sign of the rotated Stokes vectors that agrees with the models, for ease of comparison (rotating through an angle 90 deg different simply changes the sign of the polarization). With this rotation, the bulk of the polarization is now in q, and u is generally close to zero. This works with only modest success at early times when the polarization level is low, but it seems suitable for epochs four and later, as shown in the next section.
Finally, the bottom panel shows the percentage polarization P for both the observation (black) and the model (colors other than black). The model results are sometimes shown for all inclinations. The inclination of zero degree yields zero polarization. The other inclinations are spaced uniformly every 11. 25 deg, colored from blue to red (colorblind rainbow colormap) as the inclination is increased. Compared with the simulations presented in  Dessart & Hillier (2011) , the present simulations provide the total and polarized flux spectrum over the entire optical range. We explicitly account for line overlap or blanketing and can directly compare to the optical VLT-FORS spectropolarimetric data that we collected for SN 2012aw. 1 )), corresponding to a density contrast at a given radius of 1.
Results with the latitudinal density scaling at early times The observed polarization of SN 2012aw at the corresponding epoch differs in a number of ways from the model predictions. It is greater at redder wavelengths, although at this epoch the polarization is quite low, and only about 0. 2% at 7000 Å, thus significantly lower than the maximum value obtained with the models discussed above (about 0. 6%). Observations also reveal a sizable change in polarization across Hβ and Hα, but not other lines (perhaps because the data are too noisy). While Hβ and Hα in the models also show polarization, the structure does not match the observations. In q the model shows an enhanced polarization in the P Cygni absorption component (not seen in the observations), and the polarization absorption trough is offset from that observed.
Results with the latitudinal stretching at early times For an asymmetric ejecta resulting from a radial stretching of the 1D CMFGEN model 1D-X1 (see Sect. For SN 2012aw, we correct for the instrumental polarization, for the interstellar polarization and redshift (as well as reddening for F I ). The observed normalized Stokes parameters have been rotated by 28 deg (see  Sect. 4. 3). The ordinate range is the same for q rot and u rot. A binning of 25 Å is used for q rot , u rot , and P, while a binning of 5 Å is used for F I. As described in the caption to Fig. 5 , a representative 1σ uncertainty in the polarization was calculated, and is shown in the bottom panels. The polarization displayed in the bottom panels for the SN 2012aw data is the "traditional polarization", as defined in the caption to Fig.
0), the model P rises to a maximum of 0. 6% in the largely line-free region between Fe II 5169 Å and Hα. The observed polarization of SN 2012aw at the corresponding epoch differs in a number of ways from the model predictions. It is greater at redder wavelengths, although at this epoch the polarization is quite low, and only about 0. 2% at 7000 Å, thus significantly lower than the maximum value obtained with the models discussed above (about 0. 6%). Observations also reveal a sizable change in polarization across Hβ and Hα, but not other lines (perhaps because the data are too noisy). While Hβ and Hα in the models also show polarization, the structure does not match the observations. In q the model shows an enhanced polarization in the P Cygni absorption component (not seen in the observations), and the polarization absorption trough is offset from that observed.
Acknowledgements. D. C. L. acknowledges support from  NSF  grants  AST-1009571 ,  AST-1210311 , and  AST-2010001 , under which part of this research was carried out. D. J. H. thanks  NASA  for partial support through the astrophysical theory grant  80NSSC20K0524. Support for G. P. is provided by the  Ministry of Economy, Development, and Tourism's Millennium Science Initiative  through grant  IC120009 , awarded to  The Millennium Institute of Astrophysics, MAS. This work was granted access to the HPC resources of CINES under the allocation  2018 -A0050410554 ,  2019 -A0070410554  and  2020 -A0090410554  made by  GENCI, France. This research has made use of  NASA 's Astrophysics Data System Bibliographic Services. Based on observations collected at the  European Southern Observatory, Chile , under programme 089.
Production of recombinant SARS-CoV-2 antigens Hexa-His-tagged nucleocapsid expressed in E. coli. The SARS-CoV-2 nucleocapsid (GenBank YP_009724397) construct was C-terminally fused to the tobacco etch virus (TEV) protease-specific cleavage site and to a hexa-His tag by Lemay and coworkers (see ESI † for detailed protocols). Briefly, the recombinant N protein (rN) was expressed in E. coli BD792 and purified using immobilized-metal-ion chromatography (IMAC). The fractions with highest OD 280 were pooled and dialyzed against PBS pH 7. 4 and 10% glycerol in 10 K MWCO cassette. The resulting solution was sterile-filtered through a 0. 2 μm membrane, aliquoted at 0. 6 mg mL -1 in PBS pH 7. 4 and 10% glycerol and stored at -80 °C. Each step of the purification process was monitored by SDS-PAGE (Fig.
Serum (1 mL aliquots) was transferred in cryovials (Sarstedt Inc. , product 72. 694. 006) and frozen in an upright position at -20 °C until a batch was sent to the Montreal labs on dry ice. The serum samples were then stored at -80 °C until use. For ELISA assays, heat inactivated sera were diluted 1 : 50 for use, unless otherwise specified. For SPR validation assays, no heat treatment was applied to the sera, which were diluted 1 : 5 with the running buffer before analysis for the detection of IgGs. The fluidic cell with 4 independent channels was used to collect this data and the SPR instrument was placed in a laminar flow cabinet in a biosafety Level 2 (BSL2) laboratory. A panel of 20 contrived dried blood spots (DBS)  52  and matching plasma were collected from different donors at Mount Sinai Hospital (Toronto, Canada) and at the National Microbiology Laboratory (Winnipeg, Canada).