dataesr/scientific-paragraphs-categorization huggingface dataset:
It includes 18 longer-term ECG recordings of 18 subjects (5 men, aged 26 to 45, and 13 women, aged 20 to 50) with no significant arrhythmias. We randomly selected 5,000 (2919 normal samples and 2081 anomaly) heartbeats from each dataset to train and test the proposed framework AnoFed. Fig. 7  shows one example sample from each of the two selected databases. Table  1  presents additional information about the datasets used. It should be noted that the anomaly class contains different sub-classes of anomalies in it.
Implementation details In order to evaluate AnoFed in real time, firstly we developed a testbed using three Raspberry Pi devices (Pi 3 Model B+with 1. 4 GHz,  1 GB LPDDR2 SDRAM, and 64-bit quad-core ARMv8 CPU) as clients, as shown in Fig. 8  and a Dell workstation with 32 GB RAM and an Intel ® Core™ i-6700HQ CPU as 𝐆𝐒. For the initial (𝑟 = 0) global round, 𝐆𝐒 compiles the AE or the VAE. We used Adam as the optimizer for both the AE and the VAE. We distributed the above-mentioned datasets equally (but randomly selected) among the three edge devices. 75% of the data was used for training by each client or edge, whereas the rest was 25% for testing. Secondly, we increase the number of clients to five. In the second setting, we used a non-IID data (unbalanced and skewed) (Edges 3 and 5 with around 630 training samples each, where Edge 3 contains 60% data from the normal class and 40% data from the anomaly class.
As part of our future work, we will investigate if and how the proposed method and other similar federated learning methods proposed for healthcare applications may be vulnerable to such more advanced threats, and how they can be enhanced to be more robust. The results reported in the paper are based on two public datasets from a small population of data subjects (15 + 18 = 33). Validating the performance of our proposed method with a larger dataset covering more patients and people with normal conditions will be useful to consolidate the evidence presented in this paper. Similarly, our experiments were based on a small number of edge devices (3) and simulated local data, it will be important to re-validate the overall performance of the proposed method in a more real-world setting. Doing both will require close collaboration with healthcare organizations, which will not be trivial to achieve and will be our long-term future work.
To enhance the performance of the federated learning with a static threshold, we proposed to use kernel density estimation-based SVDD, which can provide adaptive anomaly detection without setting a hard threshold. AnoFed can address issues such as estimating the underlying data distribution automatically with each global round of federated learning for efficient and accurate anomaly detection. Additionally, we proposed an XAI module to provide some level of explainability to the results of AnoFed, by tracing back the major segments of the input that are responsible for a detected anomaly. Lastly, we tested the proposed framework by combining two benchmark datasets from PhysioNet's repository and showed that AnoFed achieved up to 98. 8% test accuracy with 10-fold cross-validation with changing distributions of data.
Temporal notion The disappearance of command packets is a particular case of bias. This means that no command is sent by the controller. This corresponds mainly to the case of failure. Thus, we propose to introduce a tolerance for the response time of the controller; therefore, we define a time boundary. However, in contrast to  [53]  and  [54]  we do not determine a fixed boundary. Here, the boundary evolves in real time to follow the evolution of the traffic, and thus the evolution of the response time of the controller (owing to an increase in the number of requests from the data plane, for example). In addition, the response times of the controller are recorded in a list Lt Response which is updated at each observation of a path setup. The length of this list is fixed to consider the observed values, which is suitable for the situation and not being polluted by another context (such as an acceleration of the requests of the switches or, an absence of a request, for example).
Experimental set up The physical topology is illustrated in Fig. 4. The network was simulated using Mininet  [55]  and the considered topology is presented in Fig. 3. The ONOS controller  [50]  is on the first machine, whereas the attacker is on another machine that uses the Kali Linux tool. The observer was implemented on the same machine as Mininet and the communication between the controller and switches was captured using the Scapy tool. Notably, the observer did not send packets to the network.
Precision and recall: A second design of experiments has been designed to analyse the performance of    our proposal according to the defined metrics. The experimental design is shown in Fig. 12. First, regarding the data plane requests (left side of Fig. 12 ) we randomized the inter-arrival of the requests: a value is determined between 3 and 15 s through a uniform law. In addition, the length of the traffic is determined by the number of bytes to transmit, and is also random. We divided the case into three possibilities: short traffic (126000 bytes to transmit, 0. 1 s is necessary for the transmission), medium traffic (1260000 bytes to transmit, 10 s is necessary for transmission), and longer traffic (12600000 bytes to transmit, 100 s is necessary for transmission). The aim was to determine the impact of an attack on different types of traffic.
Modification of the intern variables The attack considered in this section is described in section System and Threat Model. The objective of the attack is to hijack the controller and then redirect the flows in the direction of a particular host. To hijack the controller, we used a Kali Linux tools named "Metasploit" and the vulnerabilities used is the vsftp v2. 3. 4 backdoor. The results of the attack detection are shown in Fig. 16. In the figure, the decisions of the observer are represented by the following points: zero if there is no alarm and one, alternatively, whereas the time of the attack is represented by the curve: zero if there is no attack and one, alternatively. Subsequently, we developed the detection of an attack. The exchange of packets captured using Wireshark is shown in Fig.
Context. Asteroseismology is one of the few methods to derive ages of individual stars due to the high precision of their observations. Isochrone fitting is a powerful alternative method for deriving ages by studying clusters of stars. Pulsating stars in clusters should therefore allow for detailed studies of the stellar models. Aims. Our objectives are to exploit the NASA TESS data along with ESA Gaia data to search for and detect oscillations in cluster member stars. We analyse the intermediate-age open cluster NGC 2477, known to suffer from differential extinction, to explore if asteroseismology and cluster characteristics can help us understand the metallicity and extinction, as well as result in better age determinations than isochrone-fitting alone. Methods. We combined a multitude of recent observations from Gaia, high-resolution spectroscopy, and extinction maps to analyse the cluster and then search for and detect variability in the member stars using TESS full frame images (FFIs) data.
To interpret all of these data, we used stellar structure, evolution and oscillation codes. Results. We conducted an in-depth analysis of the extinction and metallicity of NGC 2477, using the most recent spectroscopic, photometric, and extinction observations for the cluster. Analysis of dust and extinction maps confirmed that the differential extinction in the direction of the cluster is not due to the background. The cluster's metallicity from high-resolution spectroscopy varies from 0. 06 to 0. 16 dex. We performed an isochrone fitting to the cluster using publically available isochrones (BASTI, MIST, and PARSEC), which provides a cluster age of between 0. 6 to 1. 1 Ga. Then using TESS FFI, we analysed the time dimension of the members of this cluster. We created optimised pixel light curves using the tessipack package which allows us to consider possible contamination by nearby stars.
General properties The cluster NGC 2477 is one of the richly populated open cluster located in Puppis' constellation (l = 253. 6 • ; b = -5. 8 • ). The distribution of stars in the cluster is shown in Fig. 1. The first comprehensive photometric study was done by  Hartwick et al. (1972). They obtained DDO 2 photometry for 26 giants stars and UBV photometry for 2000 stars. They found that the metallicity of the cluster should be 1. 5 times the metallicity of the Hyades cluster and the age to be 1. 5 ± 0. 2 Ga. The authors also pointed out strong differential reddening, later confirmed by 1 https://github. com/dinilbose/tessipack 2 David Dunlap Observatory. Rain et al. (2020)  are shown by the blue and yellow points, respectively. Hartwick & Hesser (1974). They estimated a differential reddening E(B -V) from about 0.
The derived parameters of these members are given in Table  3. A global comparison of the temperature and metallicity derived from photometric measurements  (Geisler et al. 1992) , medium-resolution spectroscopy (RAVE;  Kunder et al. 2017 ) and high-resolution spectroscopy  (Bragaglia et al. 2008; Caffau et al. 2014; Mishenina et al. 2015)  is shown in Fig. 4. The common stars N77-39, N77-42, N77-47, and N77-49 studied by A146, page 3 of 25  (a) UBV photometric data used for fitting isochrones. (b) 2MASS JHK photometric data used for fitting isochrones. -1. 0 -0. 8 -0. 6 -0. 4 -0. 2 0. 0 0. 2 0. these authors are marked as a square, triangle, circle, and diamond, respectively, in Fig. 4. As one can appreciate we see a large dispersion in the observed metallicity of NGC 2477, and the mean metallicity, considering the most recent publications, varies between -0.
Since the TESS pixel size is 21 , there can be two or more stars in an aperture. To obtain a light curve for a target we have to ensure that it is not contaminated by a nearby source. We used the Eleanor package to help extract the light curves. However, because the default aperture from Eleanor would result in some contamination in dense regions, we developed an interactive package (tessipack, Palakkatharappil & Creevey 2021) which helps to define custom apertures around the source and to then obtain the light curves from Eleanor. We acquired target pixel files (TPFs) with square target masks of 13 pixels on each side and a square background mask of 31 pixels on each side using Eleanor. We used the Gaia DR2 catalogue to search for nearby stars in the vicinity. If a star with similar or brighter magnitude falls in the aperture of a target star, the target star is disregarded since the nearby star's light contaminates the target star.
Comparison of light curves To validate the TESS FFI light curve from the tessipack package, we first compared existing light curves from the K2 mission  (Howell et al. 2014). One example of these stars is TIC 187129574, an F0 spectral type star which was observed by both TESS and the K2 mission. K2 observed the star in long cadence mode (30 min) in campaigns 111 and 112, while TESS observed the star in sector 12 in FFI mode only. We compare the K2 light curve using the pipeline aperture from the LightKurve package, with our light curve using the tessipack package and the same custom aperture. Figure A. 1 illustrates this comparison. The left panels show the apertures from K2 (top) and the same aperture but on the TESS FFI (lower). The top right panel shows the K2 light curve that is obtained from the K2 pipeline, while the lower right shows the normalised folded light curves at the dominant periodicity of both the K2 and tessipackgenerated light curves.
The same variability is contained in both light curves, thus validating our pipeline. We also compared the light curve from tessipack with other existing pipelines. In other pipelines, we cannot determine a custom aperture so we used the default apertures. tessipack packages. As can be seen, the light curves that are produced by tessipack show similar variability. As we are confident in the light curves produced by our own package, for the rest of this work we used tessipack to extract the light curves. The package also allows us to take into account the environment of the star to ensure that we know where the stellar light originates from. We analysed the full content of the cluster NGC 2477, to search for variability and oscillating stars, which we describe in the next few sections.
Identification of variability and contamination To search for variability, we analysed the light curves from Sectors 7, 8, 34, and 35 that we extracted from the TESS data, as described in the previous section. To determine the type of variable stars we performed the following steps. Firstly, we constructed a Lomb-Scargle periodogram  (Lomb 1976; Scargle 1982) , by searching up to the frequency limit (Nyquist frequency) of 277 µHz and 833 µHz for the 30-and 10-min data, respectively. Then, we produced folded light curves (phase diagrams) using the dominant frequencies to determine the oscillation type. Oscillating stars show sinusoidal phase diagrams, while other variability such as binaries show different forms of phase diagrams. Apart from extracting the optimal light curve, the environment of each member star was also inspected using the help of the tessipack package to determine contaminating sources.
MESA and GYRE We compute the evolutionary sequences and oscillations using the combination of the MESA stellar evolution code  (Paxton et al. 2011 ) and the GYRE pulsation code  (Townsend & Teitler 2013). We adopt a standard input physics 6  , the summary of adopted physics is listed in Table  A. 2. To run MESA, the following model parameters are needed: mass, initial chemical composition, and age. For the initial chemical composition, we need two of X, Y, and Z where these are the mass fractions of hydrogen, helium, and other elements, respectively, with the constraint of X + Y + Z = 1. The output of MESA is a stellar structure defined by the above parameters, and then this is used as an input to GYRE to calculate the oscillation frequencies. To determine the mass, we use the initial values obtained from our analysis in Sect.
Conclusions and remarks This work focuses on the analysis of the cluster NGC 2477. We aimed to combine the most recent observations available in the literature with those from Gaia and then to use the TESS FFI to search for and analyse the oscillating stars in the cluster. The objective was to investigate if we could use TESS observations to better constrain the ages of clusters. As TESS is an all-sky survey, this would open the possibility to better age-date clusters and to test asteroseismic models. We reviewed and analysed the most recent spectroscopic, photometric, and extinction observations for the cluster. The available literature in the data gives a wide range of metallicities, but in this work we conclude that the [M/H] of the cluster is best described by 0. 10 ± 0. 05 dex. Using 2D dust maps and the data from Gaia DR2, we have analysed the presence of dust in the direction of the cluster.
The aim of this study was to investigate the effects of this new device on tinnitus. Twelve AHL and two SSD patients aged 70. 7 ± 7. 9 years with tinnitus were fitted with bilateral hearing aids that included 3 programs: Stereophonic, BiCROS and StereoBiCROS (CROS + bilateral amplification). The short-and long-term effect of the approach on tinnitus was assessed using a tinnitus Loudness Visual Analog Scale (VAS) and the Tinnitus Handicap Inventory (THI), respectively. Both the VAS and the THI were used before and one month after the hearing aid fitting. Of the 14 patients who used their hearing aids daily (12. 6 ± 1. 6 h per day) the StereoBiCROS program was the most used program (81. 8 ± 20. 5% of the time). The average THI total score decreased from 47 (± 22) to 15 (± 16) (p = 0. 002) and the VAS-Loudness score decreased from 7 (± 1) to 2 (± 2) (p < 0.
The HAs were lent to the patients for the duration of the trial. Although the StereoBiCROS program was the default program activated when the HAs were turned Hearing thresholds and speech audiometry. Continuous and dashed lines (without symbols) represent the individual unaided auditory thresholds for the poor and best ears, respectively. Black squares and diamonds represent the averaged unaided and averaged auditory thresholds in the poor ear, respectively. Gray triangles and diamonds represent the averaged unaided and aided auditory thresholds in the best ear, respectively. on, patients were given instructions to test each of the three programs (Stereophonic, BiCROS, and StereoBiCROS) in different sound environments during the one-month trial period. They were instructed that they were free to move from one program to the other as many times as they want during the trial.
Statistical analysis Statistical analyses were performed using the XLSTAT software (Addinsoft, New York, USA). The results of the multiple measurements are shown as the means ± standard deviation. The normality of the distribution was assessed by using the Kolmogorov-Smirnov test. Because normality was never reached for any of the variables tested, non-parametric statistical tests were used. To assess differences between the utilization time between each program, we performed the Pairwise Multiple Comparisons test (also called Nemenyi's test). The repeated-samples two-sided Wilcoxon signed rank test and sign test analysis  (Hollander and Wolfe, 1973)  were used to test the putative differences between baseline and one month after HA fitting. Differences were considered as statistically significant when p < 0.
Usage of the different programs HAs were worn regularly during the 1-month trial period to reach at D + 30 the mean daily usage duration of 12. 6 ± 1. 6 h per day, ranging from 10. 0 to 14. 6 h per day. Figure  4  allows us to follow the evolution of the use of each of the programs over time, and to verify that all the programs have been tested and used by the patients during the 1-month trial period (D + 10, D + 20 and D + 30). Figure  5  shows the final distribution of the program usage at D + 30. Datalogging shows that each program has been tried out and that the StereoBiCROS program was the most used program (81. 8 ± 20. 5%), followed by the Stereophonic program (13. 5 ± 17. 6%) and the BiCROS program (4. 7 ± 6. 0%). The difference in daily usage between the StereoBiCROS and the BiCROS programs was significant (Nemenyi's test scored p < 10 -4 ) as well as the difference between the StereoBiCROS and the Stereophonic programs (Nemenyi's test scored p = 0.
Limitations of the study Some caution is required when interpreting the results of the current study, because of the relatively small number of patients. Indeed, the sample's size compromises the visibility of positive effects of the treatment and increases the possibility of false-negative results. It is well known that a lot of bias and placebo effects can occur in tinnitus studies or in treatment trials  (Duckert and Rees, 1984; Dobie, 1999). Such effects could have partly influenced our results. Indeed, although precautions were taken when informing patients of the expected results of StereoBiCROS stimulation, potential biases may have occurred. Besides, the pre-post study design cannot indicate whether it is the StereoBiCROS program which is responsible for the benefit, the other programs or all the programs.
Experiment of Study In this section, our research conducts simulations of this system on a personal computer equipped with highly computational performance, including an Intel Core i7 processor running at 3,300Hz, 8GB of RAM, and the Windows 10 operating system. These simulations take place within the MATLAB software environment and focus on the cross-docking scenario illustrated in Figure  5 , featuring several key parameters. Workstation Separation: The distance between two workstations is set at 𝒅𝒅 𝒏𝒏𝒏𝒏𝒅𝒅𝒏𝒏 = 𝟒𝟒. 𝟓𝟓 𝒎𝒎. AGV Target Velocity: The desired velocity for the AGV (Automated Guided Vehicle) is defined as 𝒗𝒗 𝑻𝑻𝑻𝑻 = 1. 2 (𝒎𝒎/𝒔𝒔 𝟐𝟐 ). AGV Acceleration Levels: The AGV's acceleration profile is categorized into four levels based on the load it carries: Heavy Carry: a = 0. 12 𝒎𝒎/𝒔𝒔 𝟐𝟐 Middle Carry: a = 0.
Background: French Guiana is the French department most affected by HIV. The situation in Western French Guiana is complicated by the transborder context and isolation of many patients. This study aims to describe the epidemiological characteristics of children born to mothers living with HIV followed in Western French Guiana. Methods: This was a retrospective and descriptive study. All children born to HIV-infected mothers between 2014 and 2018 were included. Data were collected using a survey sheet to generate an Excel database. Results: We recorded 177 newborns exposed to maternal HIV, four of whom (2. 26 %) were infected. The majority of women (87 %) were of foreign origin, and only 7 % had conventional health insurance coverage. The infection was discovered during pregnancy in 20 % of women.
Sample All children born to HIV mothers between January 1, 2014 and December 31, 2018, at the "Frank Joly" Western French Guianese Hospital and who had a complete medical file on the Cora-Doc software and/or a paper file were included. The parameters collected are summarized in Appendix 1. The evaluation criteria were: • antiretroviral therapy (ART) of mothers according to the protocol • ART treatment of babies according to the protocol • Follow-up of children up to 2 years • Number of children who followed the protocol (at least two as- sessments between Month (M) 1 and M6 + M24 assessments) • Number of children who did not follow the protocol (no follow- up after birth, less than two check-ups between M1 and M6 or no check-up at M24).
In this paper, gVirtualXray (gVXR) 3 is used. It is an open-source library written in C++ and the OpenGL Shading Language (GLSL). gVirtualXray is portable and works on a wide range of computers and operating systems (from Windows laptops to GNU/Linux Supercomputers). Wrappers to other popular languages, including Python 4 , R, Ruby, C#, Java and GNU Octave, are also available. The Analytical RT Inspection Sim- ulation Tool (aRTist)  5  developed by Bundesanstalt für Materialforschung und prüfung (BAM, Germany) also makes use of a deterministic method to simulate X-ray projections from computer-aided design (CAD) models  [10]. It provides a graphical user interface (GUI) and is dedicated to nondestructive testing (NDT) for industrial applications. CIVA by Extende 6  also uses a deterministic method to simulate X-ray or γ-ray projections.
Both aRTist and CIVA are closed-source commercial software with a license fee. The combination of deterministic modelling with GPU computing allows high-resolution X-ray projections to be simulated without scattering and without noise in a few microseconds, which opens up new perspectives and opportunities. It is possible to use gVirtualXray in real-time applications such as medical training simulators (see Figures  1a  and 1b )  [11, 12, 13]. GPUs also make it possible to embed gVirtualXray within an optimisation algorithm to register 3D hand models on 2D radiographs  [14]  or produce accurate digital twins in material science  [15]. gVirtualXray can also be used to produce a high number of realistic simulated images to train machine learning algorithms  [16, 17] , which would not have been possible a few years ago.