dataesr/scientific-paragraphs-categorization huggingface dataset:
Retrieval of dust scattering properties Dust optical properties are estimated by simulating the RDS measurements 2 throughout the sol, using radiative transfer simulations. The irradiance (E) measured by a given RDS channel is computed as: E = C × [T (μ 0 , φ 0 ) × e -τ μ 0 + 2π ∫ 0 0 ∫ -1 I (τ, μ 0 , φ 0 , μ, φ) × T (μ, φ) × R × μ × dμdφ] ( 7 ) where I is the scattered intensity simulated with a radiative transfer model, μ 0 and φ 0 are the cosine of the zenith angle and the solar azimuth angle, μ and φ are the cosine of the zenith angle and the azimuth angle of the observation, T and R are the sensor angular response and responsivity, C is a constant and τ is the total vertical opacity. Extended Data Fig. 10a  shows RDS Top5 (750 nm) signals simulated for different dust opacities and an effective radius of r eff = 1.
Acknowledgements This work has been funded by the  Spanish Ministry of Economy and Competitiveness , through the projects no. ESP2014-54256-C4-1-R  (also -2-R, -3-R and -4-R);  Ministry of Science, Innovation and Universities , projects no. ESP2016-79612-C3-1-R  (also -2-R and -3-R);  Ministry of Science and Innovation/State Agency of Research  ( 10. 13039/501100011033 ), projects no. ESP2016-80320-C2-1-R ,  RTI2018-098728-B-C31  (also -C32 and -C33),  RTI2018-099825-B-C31 ,  PID2019-109467GB-I00  and  PRE2020-092562 ;  Instituto Nacional de Técnica Aeroespacial ;  Ministry of Science and Innovation's Centre for the Development of Industrial Technology ;  Spanish State Research Agency (AEI)  Project  MDM-2017-0737   Unidad de Excelencia "María de Maeztu"-Centro de Astrobiología ; Grupos Gobierno Vasco IT1366-19; and  European Research Council   Consolidator Grant  no  818602.
Data availability All datasets of Mars 2020 are available via the Planetary Data System (PDS). Data are delivered to the PDS according to the Mars 2020 Data Management Plan available in the Mars 2020 PDS archive (https://doi. org/10. 17189/1522849). Data from the MEDA instrument referenced in this paper are available from the PDS Atmospheres node. The direct link is https://pds-atmospheres. nmsu. edu/data_and_services/ atmospheres_data/PERSEVERANCE/meda. html.
Nature has given us yet another wild card in the form of Zika virus (ZIKV). It was found in 1947, but has only recently become an important public health risk, predominantly to pregnant women and their unborn offspring. Currently, no specific therapeutic agent exists for ZIKV and treatment is mainly supportive. Natural products (NPs) can serve as a major source of potent antiviral drugs. To create this review, a comprehensive search was conducted from different databases (PubMed, ScienceDirect, Google scholar). A statistical analysis on the number of publications related to NPs and ZIKV was conducted to analyse the trend in research covering the period 1980-2020. From the data collated in this review, a number of NPs have been found to be inhibitive towards different stages of the ZIKV lifecycle in in vitro studies.
In 2022, a review article compiled using in silico data suggesting glycocin F as a natural biomolecule with high potential to be developed as a broad-spectrum antiviral agent  [14]  and a research article concluding plant extracts as a valuable source of antiviral compounds against ZIKV  [15]  had formed a foundation of support and hastened the urgent research on Zika that was required. The hallmark of this review is to scrutinise current understanding of the anti-ZIKV aspects of NPs and their underlying mechanism of actions. The current snapshot of in vitro, in vivo studies and clinical trials are also reviewed. In the last section of this review, we criticise on the way research are being conducted on ZIKV to determine whether we are going in the right direction or not by analysing the trends in PubMed publications.
The inhibitory effect was observed in various host cells including SNB-19, HEK293, and Vero E6 cell lines, indicating that the effect is not specific to particular cell lines. Cephaeline (6) exhibited similar potent activity against ZIKV replication. It is proposed that more studies should be conducted to investigate on the efficacy of both NPs in arresting vertical transmission and other ZIKV associated neurological complications in new-borns  [53]. A plant-secreted phytoalexin, resveratrol (11), was assessed for its ability to inhibit ZIKV replication. Experimental data showed that resveratrol (11) exhibited antiviral effects on ZIKV in a dose-dependent manner with > 90 % inhibition at a concentration of 80 µM. Negligible cytotoxicity effects were recorded in the host cells, Huh7 and Vero cell lines  [58].
Numerous studies have been published investigating the antimicrobial activity of antiseptic agents  [12] [13] [14] [15] [16] [17]. In vitro, 0. 05 % and 0. 1 % PVP-I were microbicidal against methicillin-sensitive S. aureus (MSSA) and MRSA within 20 s  [8, 17] , while 0. 05 % CHX required between 2 and 20-30 min to kill the various strains of MSSA and MRSA  [8, 16]. Most of the data on antimicrobial activity have been derived from in vitro studies using suspensions of microbial cells  [12] ; however, phase 2/ step 2 studies have been proposed as a progression from cell suspension tests  [18]. In one such study, the activity of a variety of antiseptics was assessed in vitro in the presence of organic material. The antiseptics were tested against microbial test suspensions pre-dried on a metal carrier; this method was suggested to be more representative of antiseptic treatment of a wound than cell suspension tests  [18].
At the time of publishing the guidelines, the only evidence available for preoperative washing with an antimicrobial soap was of moderate quality and showed that preoperative bathing with antimicrobial soap containing CHX had neither a positive nor negative impact on reducing the rate of SSIs compared with plain soap. As no other studies were available, either plain or antimicrobial soap was recommended  [2]. In a recent modeling study in France using a healthcare infection database, preoperative showering with antimicrobial soap was predicted to prevent 209 SSIs per year compared with no antimicrobial soap, leading to a potential saving of €632,210 per year based on the price of PVP-I  [59]. Preoperative nasal decolonization Nasal carriage of S. aureus at the time of surgery has been shown to increase the risk of SSIs  [60, 61].
The X-ray source sky location is derived from the position of the central peak in the focal plane. This paper presents the algorithm developed to perform the onboard localization analysis. Several processing methods were considered and compared a few years ago (Gosset 2019). A cross-correlation technique is selected to resolve the sources of X-ray photons, even with a weak intensity. This method is applied to search for multiple sources in the MXT field of view using an iterative subtraction process. For each identified source, the number of photons is evaluated using the crosscorrelation data, as well as the overall background counts. This is a new approach which was specifically designed to manage the peculiar shape of the point-spread function of the telescope. Moreover, due to space constraints, the data processing methods had to be optimized to cope with low onboard computing resources.
2009). The MXT camera is operated in two modes. In full-frame mode, the camera's front-end electronics captures an image every 200 ms and transfers it to the MXT data processing unit. The full-frame images are processed to estimate the pixel noise and derive pixel-by-pixel detection thresholds. For astrophysical observations, the camera is set to event mode. The image is integrated over 100 ms and the pixel noise component is removed by the front-end electronics  (Ceraudo et al. 2020). When the amplitude is above the detection threshold, the pixel data are transfered to the MXT data processing unit for analysis. In event mode, the first analysis step is to cluster adjacent pixels together. A photon is identified if the pixel pattern matches one of those represented in the right-hand side of Figure  1.
Point-spread Function The localization analysis presented in Section 3 takes the photon map D as an input and cross-correlates it with the image of a point source produced by the MXT optical system. This expected image, called the point-spread function, is measured and modeled on the ground and uploaded to the satellite. The point-spread function of the MXT is the result of the microporous structure  (Feldman et al. 2020 ) of its optical system. It measures the hit position probability of an incoming photon over the focal plane. It is composed of a central spot (double reflection), four cross arms (single reflection), and a diffused patch (no reflection). The MXT point-spread function has been measured and modeled by the University of Leicester team, in charge of the MXT optical system. It is modeled by the function P(y, z, E) fitted to X-ray data collected at different energies E during the MXT performance tests conducted at the Panter facility, Neuried, Germany, in 2021 November.
Localization Algorithm The localization analysis loops continuously in the MXT data processing unit. One cycle takes less than 2 s to complete. The analysis delivers the X-ray source sky location in spherical coordinates (θ, j), as well as the photon count, signal-to-noise ratio, and the localization uncertainty. This information is updated every 30 s and packaged in telemetry packets sent to the ground. The photon map D, introduced in Section 2. 1, is cross-correlated with the point-spread function presented in Section 2. 2. This method, described in Section 3. 1, was selected as it offers sensitivity to faint sources (Gosset 2019). Indeed, one can take advantage of MXT's specific point-spread function for which the cross-arm pattern can guide the search for source peak positions. The cross-correlation data are then processed to search for local maxima, as detailed in Section 3.
The MXT localization algorithm relies on many parameters, some of which were characterized and presented in this paper. All of them are configurable from the ground. During the first months of the SVOM mission, these parameters will be adjusted using real data collected in space. They will then be uploaded on board to maximize the performance of the localization algorithm. These parameters will be updated over time to follow aging effects. The SVOM satelite will be launched in 2023 and will observe gamma-ray bursts shortly after that. Moreover, SVOM will continue X-ray observations and take over when other satellites, such as Swift  (Gehrels 2004)  or Fermi  (Michelson et al. 2010) , will terminate their missions. SVOM will play an important role in multi-messenger astronomy, in particular in coincidence with gravitational wave detectors.
Context. The smallest extreme-ultraviolet (EUV) brightening events that were detected so far, called campfires, have recently been uncovered by the High Resolution EUV telescope (HRI EUV ), which is part of the Extreme Ultraviolet Imager (EUI) on board Solar Orbiter. HRI EUV has a broad bandpass centered at 17. 4 nm that is dominated by Fe ix and Fe x emission at about 1 MK. Aims. We study the thermal properties of EUI brightening events by simultaneously observing their responses at different wavelengths using spectral data from the Spectral Imaging of the Coronal Environment (SPICE) also on board Solar Orbiter and imaging data from EUI. Methods. We studied three EUI brightenings that were identified in HRI EUV data that lie within the small areas covered by the slit of the SPICE EUV spectrometer.
We obtained the line intensities of the spectral profiles by Gaussian fitting. These diagnostics were used to study the evolution of the EUI brightenings over time at the different line-formation temperatures. Results. We find that (i) the detection of these EUI brightenings is at the limit of the SPICE capabilities. They could not have been independently identified in the data without the aid of HRI EUV observations. (ii) Two of these EUI brightenings with longer lifetimes are observed up to Ne viii temperatures (0. 6 MK). (iii) All of the events are detectable in O vi (0. 3 MK), and the two longer-lived events are also detected in other transition region (TR) lines. (iv) In one case, we observe two peaks in the intensity light curve of the TR lines that are separated by 2. 7 min for C iii and 1.
The correlation between the occurrence of EUI brightenings and magnetic field activities may reveal that these EUI brightenings share similar formation and evolution mechanisms with larger brightenings or flares. Temperature is another important property to determine how small structures contribute to coronal heating. Differential emission measure (DEM) analysis helps to estimate temperatures of events  (Hannah & Kontar 2012; Cheung et al. 2015). As shown in results from a DEM analysis with data from AIA on board the SDO, the distribution of DEM-weighted temperatures in EUI brightenings and similar small EUV brightenings peaks at log[T/K] ∼ 6. 12, which is the typical coronal temperature  (Chitta et al. 2021a; Berghmans et al. 2021). Even though the DEM method is effective and widely used to diagnose the temperature information of coronal structures of different sizes, it contains uncertainty from the assumptions about the spectral response of the passbands of broadband imagers such as AIA and HRI EUV.
The DEM inversion of AIA data can be systematically biased toward 1 MK for multithermal plasma  (Guennou et al. 2012) , which may explain why 1 MK is found in EUI brightenings. Thus, spectral data are necessary to study the temperature evolution of solar events. Studies have been conducted of small solar events such as bright points, small jets, or explosive events by using lines with different formation temperatures (in the transition region (TR) and in the corona) recorded by spectrometers. For instance,  Innes et al. (1997)  reported bidirectional jets resulting from magnetic reconnection using data from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER;  Wilhelm et al. 1995)  spectrometer on board the Solar and Heliospheric Observatory (SOHO). Non-Gaussian line profiles of O vi  (103.
193 nm)  show mass flows in small structures in the TR  (Teriaca et al. 2004 ). Tian et al. (2008)  studied both cool and hot components in an EUV bright point with ten lines. All these studies enriched our understanding of the complicated TR and corona. However, the thermal properties of EUI brightenings have not been explored with spectroscopic data so far. In this study, we first investigate EUI brightenings using both imaging and spectral data. The instruments HRI EUV and SPectral Imaging of the Coronal Environment (SPICE; Spice Consortium 2020;  Fludra et al. 2021)  simultaneously observed the same region on the Sun in 2021 during the cruise phase of Solar Orbiter. This study investigates the temperature properties of EUI brightenings by combining EUV images from HRI EUV and spectra from SPICE.
Observations For the purpose of studying their temperature properties, we selected EUV brightening events that can be identified in HRI EUV data and are also covered by the slit of SPICE. In this study, we focus on three cases from two different parts of the spacecraft orbit. Information about the data sets is included in Table  1 , where all times are the starting times of the observations. The EUI data we used in this study are available in the EUI data release 5. 0 1  , and the SPICE data are included in the SPICE data release 3. 0 2. Figure  1  shows overviews of the HRI EUV field of view that is covered in these two data sets. On 23 February 2021, when Solar Orbiter had a heliocentric distance of 0. 53 AU and the angular separation between  The other data sets were obtained on 12 and 13 September 2021, when Solar Orbiter was 0.
59 AU away from the Sun and the angular separation between Earth and Solar Orbiter was about 50 •. This time, SPICE observed in sit-and-stare mode with an exposure time of 10 s, which means that the slit was kept at a fixed position on the Sun. The pixel scale of SPICE in this data set is about 470 km. Three sets of image sequences were taken by HRI EUV , but only the first and third sets have a high time cadence of 2 s. The cadence of the second sequence was set to 1 min, which is not ideal for detecting an EUI brightening, considering the short life span of the majority of these events. All HRI EUV images were taken with an exposure time of 1. 65 s and a pixel scale of 0. 492 (210 km). In this study, we used level 2 data, which are corrected for instrumental effects. The HRI EUV level 2 data are returned in units of DN (digital numbers) per second, and SPICE level 2 data are in units of W m -2 sr -1 nm -1.
Every O iv line mentioned below refers to the O iv 78. 772 nm line. In the fitting process, we used custom software based on the xcfit_block. pro routine from Solarsoft, taking the prepared data and the corresponding estimated error (see Appendix B) as inputs to obtain the parameters of the Gaussian function(s) (amplitude, line center, and position) and of the background at each point. We considered the background to be a constant along the wavelength in the window of each line. To improve the signal-to-noise ratio of the data, we binned over 4 spatial pixels along the direction of the slit. Since the width of the slit is 4 , about four times the imaging spatial scale, this binning led to square pixels in the resulting raster scans. Moreover, the spatial resolution of SPICE is estimated to be about 6 to 7 , which means that we do not lose substantial information on the target EUI brightenings because of this binning.
In the following discussion, all references to SPICE data assume the 4-pixel binning along the slit direction for an effective plate scale of 4 × 4. 392 (hereafter one SPICE-binned pixel), which is about 1540 × 1690 km for event E-1 and 1710 × 1880 km for events E-2 and E-3. From the fitting results, we obtained the radiance at every pixel after binning, as described above. A82, page 4 of 13  Unlike large-scale and long-lived structures, which can clearly be identified in HRI EUV images and spectral scanning images, EUI brightenings are difficult to distinguish in SPICE scanning data without the aid of HRI EUV data. In order to study the EUI brightening signatures in SPICE data, it is therefore first necessary to accurately align the data from the two instruments. The detailed alignment method can be found in Appendix A, where we apply a two-step approach and make use of time-series data.
By carefully aligning HRI EUV and SPICE data, we determined the positions of the EUI brightenings, as identified in HRI EUV data, in the SPICE data. An easy way of comparing the signature of EUI brightenings in HRI EUV and SPICE data is to reduce the resolution of HRI EUV to that of SPICE. However, to confirm whether the SPICE slit scanned the EUI brightening structure during the simultaneous observation time period, we used the HRI EUV data at their full resolution because this shows the evolutionary trace of EUI brightenings in time-slice images more clearly. Since data set 1 consists of rasters with three spatial steps, we are able to obtain a time-slice plot at each spatial position. In data set 2, we obtain the time-slice plot at one single spatial position, but with higher temporal resolution.
Discussion and conclusion We have analyzed three EUI brightenings that were observed simultaneously by HRI EUV and SPICE on board Solar Orbiter. These three events were observed at two widely different times, and different types of data were provided by SPICE. The first event occurred on 23 February 2021, and we used a sequence of three-step SPICE rasters with a time cadence of 20 s. This event lasted for approximately 40 s. The other two events occurred on 12 and 13 September 2021, during which SPICE observed continuously in sit-and-stare mode with a cadence of 10 s. Both events lasted for several minutes. Here we point out that the scales of all three EUI brightening events are close to that of the smallest structure SPICE can detect. Their identification therefore depends on HRI EUV high-resolution imaging.
Combining the HRI EUV imaging observations with the spectral data provided by SPICE, we find that the first event can only be observed in O vi, while the other two longer-duration EUI brightenings are detectable not only in TR lines, but also in Ne viii. In both cases, the Ne viii emission shows a single peak that coincides with the peak seen in HRI EUV. This may imply that some EUI brightenings barely reach coronal temperatures. This scenario is in one case supported by the fact that we observe two peaks in the light curve of TR lines, while the light curve A82, page 8 of 13  of Ne viii only reaches one peak in between the double peaks from the lines formed at lower temperatures. This can help us to infer the process by which the EUI brightening heats to the temperature of lower corona and then decreases.
For these reasons, we used a two-step approach that allows the direct alignment of the sit-and-stare (or high-cadence threestep rasters) SPICE data with the HRI EUV images. The first step consists of visually refining the coalignment between the context raster (reprojected over the HRI EUV data, see below) and the HRI EUV data. This was done ignoring solar rotation, as the scope is to get close enough for the next alignment step. The second alignment step makes use of the time-series data (three time series, one for each raster location for the 23 February 2021 data). In this step, we aligned HRI EUV and SPICE data by comparing time-slice images. In the time covered by the HRI EUV and SPICE high-cadence data, we fit the spectra of Ne viii, which is closest in temperature sensitivity to the HRI EUV bandpass over the average corona, with a single-Gaussian function and made a time-slice plot of the obtained line amplitude.
Acknowledgements. The authors thank the referee for helpful comments that have improved this paper. Solar Orbiter is a space mission of international collaboration between  ESA  and  NASA , operated by  ESA. The development of SPICE has been funded by  ESA  member states and  ESA. It was built and is operated by a multi-national consortium of research institutes supported by their respective funding agencies:  STFC RAL  (UKSA, hardware lead),  IAS  (CNES, operations lead),  GSFC (NASA) , MPS (DLR),  PMOD/WRC (Swiss Space Office) ,  SwRI (NASA) ,  UiO (Norwegian Space Agency). The EUI instrument.
Objective: In this open-label, multicenter, randomized, phase 3 trial, we evaluated the safety and efficacy of a novel VR therapy solution for distraction in the context of bone marrow biopsy. Methods: Bliss is a VR software with 4 imaginary interactive environments in 3 dimensions with binaural sound (head-mounted display). Efficacy regarding pain intensity was evaluated using a visual analog scale (VAS; score from 0 to 10) immediately after the biopsy. Secondary end points were anxiety and tolerance. Modified intention-to-treat analysis was performed. Results: Overall, 126 patients with previously documented untreated or suspected malignant hemopathy between September 6, 2018, and May 18, 2020, were randomly assigned in a 1:1 ratio to receive pain prevention with a mixture of nitrous oxide/oxygen (MEOPA; n=63) or VR (n=63) before and during the bone marrow biopsy.
Randomization Randomization was planned by minimization upon inclusion of patients in the study and programmed using ENNOV clinical data management software (ENNOV; Paris, France). Patients were randomly assigned 1:1 to a pain prevention program using MEOPA or VR. Treatment allocation was stratified by center, age, sex, and hemopathy. In case of intolerance in the VR arm, a change to MEOPA was permitted.