dataesr/scientific-paragraphs-categorization huggingface dataset:
All units of distance are given in R S. Northern solstice occurred on 24 May 2017 during our study interval (Day 114 of 2017 or Day 4,862 doy2004), such that the latitude of the Sun is nearly fixed at its maximum value ~26. 5°throughout the interval considered here (taken to be constant in the plot). Fits to data in prior studies have provided varying estimates of the hinging distance of 16 and 29 R S in  Arridge et al. (2008)  and ~27 ± 6 R S in  Carbary et al. (2015). Here we take illustrative r H values of 20 R S , shown by the southernmost black dashed line in Figure  2b , and 30 R S shown by the northernmost black dashed line, with the region between being shaded dark gray. The lighter-gray-shaded regions extend 2. 5 R S north and south of the darker-shaded region, giving an initial indication of the region where Cassini may be expected to encounter the tail plasma/current sheet.
Due to the northward displacement of apoapsis, combined with the southward seasonal displacement of the plasma/current sheet, in all cases the spacecraft is expected to be located closer to the center of the plasma sheet on its southern outbound passes than on its northern inbound passes, crossing through the sheet center outbound ~2 R S southward of the planetary equatorial plane at a radial distance from Saturn of ~17 R S. Of course, this picture of the current sheet and its location should be considered only as a rough guide, given the PPO-related north-south oscillations and thickening and thinning effect discussed in section 1 (Figure  1 ). Overall, we thus examine data from 43. 5 Cassini Revs over an interval of ~9. 5 months. As will be discussed in section 2. 3, during this interval the northern PPO period was near fixed at ~10.
(2009) , they are typically dominated by protons in the energy ranges specified above  (Kotova et al. , 2015). We also use channels E0-E4 which detect electrons with energies of 110-365 keV (E0), 220-485 keV (E1), 340-1,350 keV (E2), 600-4,950 keV (E3), and 790-4,750 keV (E4). The typical time resolution of these data is ~5. 3 s, though this can increase or decrease during some specific intervals. The fluxes in these channels in general correspond to the high-energy tail of the thermal distribution (observations of which are not available due to prior malfunction of the Cassini low-energy plasma instrument), showing significant increases on entering the plasma sheet from near background levels in the open tail lobes. Dynamical events are thus detected, while the relative flux observed from Rev to Rev also gives an overall indication of the magnetospheric state in terms of its hot plasma population.
UVIS The Ultraviolet Imaging Spectrograph (UVIS) data set employed here uses the far ultraviolet (FUV) channel of the instrument consisting of 64 spatial × 1,024 spectral pixels, providing observing in the range 110-190 nm. The detector slews over portions of Saturn with the rotation of the spacecraft, providing a two-dimensional pseudo-image of the area covered. Depending on the distance of Cassini from Saturn's poles, multiple sweeps are occasionally necessary to complete a fully mapped image of Saturn's aurora. Mapping of the information from each pixel is achieved using Cassini SPICE pointing information from the NAIF Planetary Data System by projecting the data onto an ellipsoid 1,100 km above Saturn's 1 bar level, the altitude at which auroral emissions peak in intensity  (Gérard et al.
10. 1029/2020JA027907 Journal of Geophysical Research: Space Physics and above, a near order of magnitude increase, to be indicative of significant solar wind-driven compressions of the magnetosphere, resulting in the subsolar magnetopause being displaced inward to ~16 R S or less. This indicative value is plotted as a horizontal dotted line in Figure  4d. The model data then generally indicate the presence of two significant compressions per solar rotation in the early interval sourced from Stereo-A, and generally one compression region per solar rotation in the later interval sourced from OMNI. These findings are in accord with solar coronal field measurements from the Wilcox Solar Observatory (http://wso. stanford. edu/synsourcel. html). Early in the interval the effective tilt of the solar magnetic dipole was sufficient to result in two clear equatorial crossings of the heliospheric current sheet per solar rotation, consistent with two fast solar wind streams and two CIR-related compressions with a ~13 day periodicity.
Figures  5f-5k  show UVIS and HST auroral images projected into the northern (NH) and southern (SH) hemispheres, together with Rev number and start and stop times. Start times are also indicated in the time series panels by the vertical black dashed lines, with correspondingly labeled ticks shown at the top of the panels. White dotted circles and radial lines show 10°steps of latitude and 30°intervals of longitude (2 hr LT), respectively. All images are oriented with midnight (00/24 hr LT) at the top and dawn (06 hr LT) to the left. Brightness is given by the logarithmic color scale on the right saturating at 100 kR, with regions for which no data are available being shaded gray. The mapped Cassini magnetic footprint is shown by the yellow circle. 10. 1029/2020JA027907 reconnection, moving toward antiphase conditions favorable for modulated reconnection at the end.
Intensities in kilo-Rayleighs (kR) are indicated by the color scale to the right of the projections, saturating white at 100 kR. The same scale is used for all the images displayed in this paper, again allowing ready cross-comparison between intervals. The footprint of the Cassini spacecraft, mapped along model field lines into the ionosphere is shown as a yellow circle. The model employed consists of the  Dougherty et al. (2018)  internal planetary field model plus the  Bunce et al. (2007)  ring current model for a subsolar magnetopause at 22 R S. Figure  6  shows selected data on an expanded time base which we refer to below in discussion of the compression event, where the right hand panels (Figures  6h-6n ) show data from the northern inbound pass of Rev 280 during the compression event, while the left hand panels (Figures  6a-6g ) show data from the equivalent portion of quiet Rev 279.
The intervals shown in each case are such that at the end of each plotting interval Cassini is located 5 R S from Saturn's center, with data from the preceding 3. 5 days being shown. These intervals thus contain the inbound apoapsides at the start of these Revs, indicated by the black tick marks at the top of the plots. Though PPO phases are not shown in the figure, blue and red vertical dotted lines show the times for local PPO phases Ψ N = 0°and Ψ S = 180°, respectively, as in Figure  5. These again thus indicate the times at which the local plasma/current sheet is expected to be thin due to the effects of the northern and southern PPO systems, respectively. Figures  6a  and 6h  show RPWS spectrograms using the same range and background powers as in Figure  5a. Figures  6b-6d  and 6i-6k show the three residual spherical polar components of the magnetic field as in Figure  5b , plotted using a common vertical scale of 12 nT, though with the ranges adjusted to accommodate the data.
Revs 290-293: Compression Events L1 and L2 Our third example returns to the proximal orbit interval to examine data from Revs 290-293, the final four Revs of the Cassini mission consisting of three and a half orbits before the end of mission in Saturn's atmosphere during the periapsis pass of Rev 293. The data from these Revs span a ~22. 6 day interval from 20. 9 hr UT on Day 235 to 10. 6 hr UT on Day 258 of 2017, as indicated by the arrow marked "3" in Figure  4f. The model solar wind/IMF data from both Stereo-A (blue) and OMNI (red) sources lie within their regimes of approximate validity during the later part of this interval, as shown in Figure  4 , but exhibit little correspondence during the rather disturbed conditions then prevailing. The GCR fluxes, however, show minimum values during Rev 290 indicative of rarefaction conditions on this Rev (agreeing with the model data sourced from OMNI), followed by a rapid uninterrupted rise to peak values during the first half of Rev 292, and then a Forbush decrease continuing to the end of mission.
The Cassini footprint is located just poleward of the emission close to midnight, consistent with the quiet northern lobe conditions observed at this time in the time series panels. The second image displayed, in Figure  9j ), is contemporaneous with the intensification of the SKR emission and onset of the LFE, and is the first image in the UVIS sequence to show storm-related features, with a brightening of the auroras throughout the dawn sector to peak intensities of ~140 kR. The Cassini footprint at noon lies just to the west of the brightened region and is again just poleward of the auroral region, consistent with the tail lobe location indicated in the in situ data at this time    10n ). Three hours later, contemporaneous with the onset of the hot plasma injection event at Cassini, Figure  9k  shows the image with the brightest emissions peaking at ~600 kR, together with broadening of the region of bright dawn emissions and expansion into the premidnight sector.
, 2018). Events F1 and F1* are also of somewhat different nature, with event F1 occurring near a peak in GCR flux with following rather weak Forbush decrease onset, similar to many other events, while subsequent event F1* relates to a further sharp increase in the rate of decline of the GCR flux occurring ~5 days later. The relationship between the nature of the responses, whether major or minor, with the PPO beat phase is also evident in Figure  12f , with the major events mainly occurring within the intervals when the beat phase lies between 90°and 270°via 180°in the center of the panel, and the minor events occurring when the event lies outside that range, within the top and bottom segments of the panel. Our examination of the Cassini data reveals not only the solar-modulated semirecurrent intervals of high activity related to magnetospheric compressions, however, but also the similarly semirecurrent intervals of magnetospheric quiet related to extended intervals of solar wind rarefaction.
Summary We have examined Cassini remote sensing and in situ data from the set of F ring and proximal orbits at the end of mission, augmented by HST auroral observations and model solar wind data, to investigate the state of Saturn's magnetosphere and its relation to concurrent heliospheric conditions. The nature of the study and its principal findings are summarized as follows. a. The Cassini F ring and proximal orbits explored the nightside tail to distances of ~21 R S in the postmidnight to midnight sector, passing inbound from apoapsis through the northern outer plasma sheet/tail lobe region, and outbound through the southern and central plasma sheet region, via a variably close periapsis on the dayside. The very close similarity of both the sequence of twenty F ring orbits and the subsequent sequence of 22 and a half proximal orbits, is such that the Rev-to-Rev variations in observed parameters may be attributed dominantly to variations in the physical conditions prevailing, rather than to differences in orbit geometry.
The spacecraft orbital period also corresponded quite closely to one quarter of the effective solar rotation period at Saturn of ~26 days, such that four-Rev sequences of repetitive heliospheric conditions represent a first approximation, with ~11. 5 such sequences being observed over the ~10 month interval of study. Heliospheric conditions inferred from model solar wind/IMF and Cassini GCR flux data evolved from the occurrence of two CIRs per solar rotation during the earlier F ring orbits to one CIR per rotation during the later F ring and proximal orbits (with one exception), this reflecting the late declining phase of the solar cycle. An ICME-related shock is also anticipated to have impacted on the final Rev, based on concurrent Cassini SEP flux data. b. Overall results demonstrate a very clear correspondence between in situ magnetospheric magnetic field and energetic particle data, together with remote sensing observations of SKR, auroral hiss, and auroral UV emissions, with the inferred simultaneous heliospheric conditions.
Individual compression-related disturbance intervals last on average for ~2. 7 days (typically ~2-3. 5 days), thus corresponding to approximately six Saturn planetary/PPO rotation periods, as well as to ~40% of a Cassini orbital period and ~10% of a solar rotation. Compression events are centered close to the times predicted from a combination principally of model solar wind/IMF and GCR flux considerations, with the center time minus the predicted time having a mean and SD of 0. 2 ± 1. 6 days, such that the onsets occur on average ~-1. 2 ± 1. 6 days before our predicted times. This difference is not considered significant, given the typical ~± 1. 5 day uncertainties in the model SW/IMF data, and the ~2 day smoothing of the GCR flux data. The detailed response in the in situ data depends, of course, on the orbit segment on which the compression event occurs.
Figures 5a to 5e show field and plasma parameters in a time series format plotted over the interval of Revs 278-281. Figure5ashows a RPWS spectrogram (section 2. 2. 3) between frequencies of 1 Hz and 2 MHz, with powers given in dB above background for each frequency band, as indicated by the color scale on the right of the panel, saturating at 40 dB. The background values were determined from the powers in each band over the full ~9. 5 month interval examined in this paper, given by the minimum 10% of values in each channel, thus providing consistency across all the RPWS spectrograms shown in the paper. The principal emissions observed are SKR at frequencies above a few kHz, and auroral hiss at frequencies below a few 100 Hz. Figure5bshows 1 min averaged residual magnetic field data in spherical KGS coordinates, from which theDougherty et al.
Acknowledgments Work at Leicester was supported by  STFC  Consolidated Grant  ST/N000749/ 1. T. J. B. was supported by  STFC   Quota Studentship   ST/N504117/1 , and E. J. B. by a  Royal Society Wolfson Research Merit Award. L. L. was supported by  CNES  and  PNP/PNST programs of CNRS/INSU. M. K. D. and G. J. H. were supported by  UKRI/STFC  Grant  ST/N000692/1.
Data Availability Statements The UV observations were obtained from the ESA/NASA Hubble Space Telescope GO program 14811. The original data can be retrieved from the MAST archive at https://archive. stsci. edu/access-mast-data, and the processed data from the APIS service (http://apis. obspm. fr). The Cassini/RPWS and MAG original data are accessible through the PDS archive (https://pds. nasa. gov/). Calibrated data from the Cassini mission are available from the NASA Planetary Data System at the Jet Propulsion Laboratory (https://pds. jpl. nasa. gov/). 10. 1029/2020JA027907.
Image analysis and quantification For all staining, four to seven spinal cord sections from each of six Hri +/+ and six Hri -/- mice were scored. The H&E and LFB stains of brain and spinal cord sections were screened for evidence of inflammation or demyelination, respectively, using a light microscope (Axioscope, Zeiss) connected to a digital camera (AxioCam MRc, Zeiss) and the Zen pro 2. 0 imaging software (Zeiss). Since no signs of inflammation or demyelination were observed, no further quantification analysis was performed. The Iba-1 immunostaining of brain and spinal cord sections was screened for evidence of microglial/macrophages clusters, as previously described (51), using a light microscope (Axioscope, Zeiss) connected to a digital camera (AxioCam MRc, Zeiss) and the Zen pro 2. 0 imaging software (Zeiss).
Since microglial/macrophages clusters were observed in the spinal cord but not in the brain, no further quantification analysis of Iba-1 immunostaining in the brain was performed. The Thioflavin S stain of brain and spinal cord sections was screened for evidence of Thioflavin S-bound protein aggregates, using the EGFP filter (wavelength, 488 nm) in a microscope (Axio Imager Z1, Zeiss) connected to a digital camera (AxioCam 506 mono, Zeiss) and the Zen pro 2. 0 imaging software (Zeiss). Since Thioflavin S-bound protein aggregates were observed in the spinal cord but not in the brain, no further quantification analysis of Thioflavin S immunostaining in the brain was performed. Quantitative analysis of the Iba-1 immunostaining and the Thioflavin S staining of spinal cord sections was performed on 4x and 20x magnification, using ImageJ 1.
15s (National Institute of Health, USA) imaging software. Images were calibrated in ImageJ. The white or grey matter areas of the spinal cord were measured at 4x magnification using the ImageJ freehand selections tool. The number of microglial/macrophages clusters and the number of Thioflavin S-bound protein aggregates was counted at 20x magnification over the entire white matter or grey matter areas of the spinal cord. Staining is expressed as number of microglial/macrophages clusters or the number of Thioflavin S-bound protein aggregates per mm 2 of white matter or grey matter areas.
Statistics For all experiments statistic was performed using GraphPad Prism software 8. 0 (GraphPad Software Inc, San Diego, CA, U. S. A. ). Results of the experiments in cell lines were analyzed by Student t-test or one-way ANOVA. For quantifications of thioflavin aggregates and microglial clusters, statistic was performed by multiple t-test analysis and results were considered significant when P<0. 05. Statistical significance in figure panels have been denoted as "*", "**", and "***" for P < 0. 05, P < 0. 01, and P < 0. 001, respectively.
a solution to this important visualization challenge by allowing researchers to view volumetric objects in an entirely intuitive fashion. With this motivation, we present DIVA, a user-friendly software tool that automatically creates detailed three-dimensional reconstructions of raw experimental image stacks that are integrated in virtual reality. In DIVA's immersive virtual environment, users can view, manipulate and perform volumetric measurements on their microscopy images as they would to real physical objects. In contrast to similar solutions, our software provides high-quality volume rendering with native TIFF file com-✩ Maxime Dahan died on the 28 th of July, 2018. * Mohamed El Beheiry and Jean-Baptiste Masson Email address: mohamed. el-beheiry@curie. fr and jean-baptiste. masson@pasteur.
VR is a promising vehicle through which experimentally acquired images can be better understood. It allows instantaneous understanding of complicated 3D morphologies and, notably, through controller-aided interaction it allows entirely natural selection of voxels in 3D space. In our view, image visualisation in VR should be readily available to all research laboratories (as software such as ImageJ and Icy are  [12, 13] ) and it must provide tools adapted for processing the enormous diversity of microscopy images. With this motivation, we introduce DIVA, a complete software application that allows easy integration and navigation inside any 3D.
Implementation The software architecture on which DIVA is based, entitled Lean Mapper, consists in arranging distinct subsystems to interact with each other via a toplevel supervisor. Specifically, a data subsystem, which holds loaded imaging data is decoupled from a user-facing interface subsystem. A unique data identifier is used as a reference by the supervisor to trigger events. For example, when the user adjusts a slider to increase the ambient lighting in the interface subsystem, the corresponding event is emitted to the data subsystem which alters the rendered value in real-time. Among the advantages of this data-oriented approach includes low-latency user interactions with data and fluid navigation, Examples of uses of DIVA for optical and electron microscopy images are shown in Figure  1  and corresponding videos in the supplementary material.
interacting or observing. This has the result of maintaining a high frame rate even on modest computer configurations. Accordingly, DIVA runs comfortably on mid-range laptop computers. Numerous microscopy modalities generate multi-channel or multi-colour image types. Accordingly, DIVA supports visualisation of up to four different channels, whose colour and absorption (transfer function) characteristics can be individually customized. Figure  1 (c) shows an example of a multi-colour confocal image rendered in DIVA's VR context. Additionally, time-series images can be moved where dynamic cellular processes can be observed from every angle using VR. The software has integrated sample images for the user to test upon downloading.
After electrophoresis, films were immersed in PBS for neutralization, followed by fixation in 100% EtOH for 1. 5h and drying. Films were glued onto a glass slide and rehydrated in TE buffer with DNA stain SYBRâ Gold for 20 minutes. Image analysis were performed with CometScore 2. 0 free software. For each cell, the extent of DNA damage was calculated as percentage of pixels in the comet tail by dividing the measurement of the intensity of all tail pixels by the total intensity of all pixels in head and tail of comets, as previously described  (Perdry et al. , 2018). For each animal, the median of minimum 150 cells was determined.
ACKNOWLEDGMENTS We are grateful to  Drs. Lisa Del Bell Belluz  and  Boris Mihaljevic  for technical assistance with the infection of ATM mice and the RT 2 profiler PCR array, respectively. We acknowledge the  Biochemical Imaging Center Umea ˚(BICU)  at  Umea  ˚University and the  National Microscopy Infrastructure (NMI)  ( VR-RFI 2016-00968 ) for providing assistance with microscopy. This investigation was supported by grants from the  Swedish Cancer Society  ( CAN 2017/315  and  20 0699 PjF ), the  Swedish Research Council  ( 2018-02521 ), the  Kempestiftelserna  ( JCK-1826 ), the  Cancer Research Foundation in Northern Sweden  ( AMP20-993  and  AMP 17-884 ), and  Umea ˚University  (to T. F. ) and the  German Academic Scholarship Foundation and Erasmus+  (to D. B. ).
Méthodes Une étude monocentrique prospective a été réalisée dans un service de néonatalogie afin de recueillir l'ensemble des prescriptions. Une liste exhaustive des médicaments contenant des parabènes commercialisés en France a été répertoriée à partir de la base de données Thériaque. Cette liste a été croisée avec les prescriptions recueillies afin d'établir un profil d'exposition aux parabènes. Pour chaque médicament prescrit contenant des parabènes, un dosage par HPLC-UV a été réalisée afin de déterminer la dose journalière de parabènes moyenne reçue par les nouveau-nés hospitalisés.
Matériel et méthode : L'identification des médicaments comportant des parabènes dans leur formulation a été réalisée à partir de la base de données Thériaque®, par utilisation de la recherche de spécialités avec excipients. Quatre parabènes ont été recherchés sous leur forme parent ou sous leur forme de sel sodique (Tableau 1). La méthode de dosage a été validée selon les recommandations du chapitre « Validation de méthode analytique » du guide GERPAC/SFPC  (25). La méthode était linéaire sur la gamme d'étalonnage utilisée (r² ≥ 0,997) et la limite de quantification était de 0,13 µg/mL. Les coefficients de variation de la précision étaient inférieurs à 12% et les taux de recouvrement de la justesse étaient compris entre 92 et 113%. Les quantités journalières moyennes et cumulées de parabènes administrées ont été calculées en tenant compte des concentrations obtenues pour chaque spécialité et des doses prescrites.