Miracle-dz/UniFAR-FTUs huggingface dataset:
A Computer Vision System for Street Sweeper Robot

With the spread of Covid-19, more people wear personal protective equipment such as gloves and masks. However, they are littering them all over streets, parking lots and parks. This impacts the environment and damages especially the marine ecosystem. Thus, this waste should not be discarded in the environment. Moreover, it should not be recycled with other plastic materials. Actually, they have to be separated from regular trash collection. Furthermore, littering gloves and masks yields more workload for street cleaners and presents potential harm for them. In this paper, we design a computer vision system for a street sweeper robot that picks up the masks and gloves and disposes them safely in garbage containers. This system relies on Deep Learning techniques for object recognition. In particular, three Deep Learning models will be investigated. They are: You Only Look Once (YOLO) model, Faster Region based Convolutional Neural Network (Faster R-CNN) and DeepLab v3+. The experiment results showed that YOLO is the most suitable approach to design the proposed system. Thus, the performance of the proposed system is 0.94 as F1 measure, 0.79 as IoU, 0.94 as mAP, and 0.41 s as Time to process one image. © 2022,International Journal of Advanced Computer Science and Applications. All Rights Reserved.
Impossibility of Spin Polarized States for Neutron Star/Proto-Neutron Star Matter in β-Equilibrium Condition

It is shown explicitly that a ferromagnetic transition of neutron star (NS)/proto-neutron star (PNS) matter in the β-equilibrium condition with σ-ω-ρ exchange type of mean field approximation can actually occur if and only if the neutrinos remain trapped within the system, and perhaps it is also necessary for the neutrinos/anti-neutrinos to carry some finite nonzero mass. It is further shown that the electrons also play a significant role in this transition process. It is therefore, very much unlikely that such a transition of spin polarization can really take place in old neutron stars of very low temperature, whereas, the possibility of spontaneous ferromagnetic transition cannot be ruled out in a newly born PNS.
The Magnetohydrodynamic Kelvin-Helmholtz Instability: A Three-dimensional Study of Nonlinear Evolution

We investigate through high-resolution three-dimensional simulations the nonlinear evolution of compressible magnetohydrodynamic flows subject to the Kelvin-Helmholtz instability. As in our earlier work, we have considered periodic sections of flows that contain a thin, transonic shear layer but are otherwise uniform. The initially uniform magnetic field is parallel to the shear plane but oblique to the flow itself. We confirm in three-dimensional flows the conclusion from our two-dimensional work that even apparently weak magnetic fields embedded in Kelvin-Helmholtz unstable plasma flows can be fundamentally important to nonlinear evolution of the instability. In fact, that statement is strengthened in three dimensions by this work because it shows how field-line bundles can be stretched and twisted in three dimensions as the quasi-two-dimensional Cat's Eye vortex forms out of the hydrodynamical motions. In our simulations twisting of the field may increase the maximum field strength by more than a factor of 2 over the two-dimensional effect. If, by these developments, the Alfvén Mach number of flows around the Cat's Eye drops to unity or less, our simulations suggest that magnetic stresses will eventually destroy the Cat's Eye and cause the plasma flow to self-organize into a relatively smooth and apparently stable flow that retains memory of the original shear. For our flow configurations, the regime in three dimensions for such reorganization is 4 ≲ MAx ≲ 50, expressed in terms of the Alfvén Mach number of the original velocity transition and the initial Alfvén speed projected to the flow plan. When the initial field is stronger than this, the flow either is linearly stable (if MAx ≲ 2) or becomes stabilized by enhanced magnetic tension as a result of the corrugated field along the shear layer before the Cat's Eye forms (if MAx ≳ 2). For weaker fields the instability remains essentially hydrodynamic in early stages, and the Cat's Eye is destroyed by the hydrodynamic secondary instabilities of a three-dimensional nature. Then, the flows evolve into chaotic structures that approach decaying isotropic turbulence. In this stage, there is considerable enhancement to the magnetic energy due to stretching, twisting, and turbulent amplification, which is retained long afterward. The magnetic energy eventually catches up to the kinetic energy, and the nature of flows becomes magnetohydrodynamic. Decay of the magnetohydrodynamic turbulence is enhanced by dissipation accompanying magnetic reconnection. Hence, in three dimensions as in two dimensions, very weak fields do not modify substantially the character of the flow evolution but do increase global dissipation rates.
Deep Hubble Space Telescope Imaging of Sextans A. I. The Spatially Resolved Recent Star Formation History

We have measured stellar photometry from deep Cycle 7 Hubble Space Telescope/WFPC2 imaging of the dwarf irregular galaxy Sextans A. The imaging was taken in three filters: F555W (V; eight orbits), F814W (I; 16 orbits), and F656N (Hα; one orbit). Combining these data with Cycle 5 WFPC2 observations provides nearly complete coverage of the optically visible portion of the galaxy. The Cycle 7 observations are nearly 2 mag more sensitive than the Cycle 5 observations, which provides unambiguous separation of the faint blue helium-burning stars (BHeB stars) from contaminant populations. The depth of the photometry allows us to compare recent star formation histories recovered from both the main-sequence stars and the BHeB stars for the last 300 Myr. The excellent agreement between these independent star formation rate (SFR) calculations is a resounding confirmation for the legitimacy of using the BHeB stars to calculate the recent SFR. Using the BHeB stars we have calculated the global star formation history over the past 700 Myr. The history calculated from the Cycle 7 data is remarkably identical to that calculated from the Cycle 5 data, implying that both halves of the galaxy formed stars in concert. We have also calculated the spatially resolved star formation history, combining the fields from the Cycle 5 and Cycle 7 data. The star-forming regions are found in three major zones of the galaxy. One of these zones is extremely young, consisting of only a single star-forming region that is less than 20 Myr old. Two of these zones are associated with high column density neutral gas, while the third, and oldest, is not. Our interpretation of this pattern of star formation is that it is an orderly stochastic process. Star formation begins on the edge of a gas structure and progressively eats away at the cloud, breaking it up and inducing further star formation. A more quantitative analysis of the star formation process must await a larger sample of galaxies with spatially resolved star formation histories to allow correlation studies with the physical properties of the galaxy.
A Layered Aggregate Engine for Analytics Workloads

This paper introduces LMFAO (Layered Multiple Functional Aggregate Optimization), an in-memory optimization and execution engine for batches of aggregates over the input database. The primary motivation for this work stems from the observation that for a variety of analytics over databases, their data-intensive tasks can be decomposed into group-by aggregates over the join of the input database relations. We exemplify the versatility and competitiveness of LMFAO for a handful of widely used analytics: learning ridge linear regression, classification trees, regression trees, and the structure of Bayesian networks using Chow-Liu trees; and data cubes used for exploration in data warehousing. LMFAO consists of several layers of logical and code optimizations that systematically exploit sharing of computation, parallelism, and code specialization. We conducted two types of performance benchmarks. In experiments with four datasets, LMFAO outperforms by several orders of magnitude on one hand, a commercial database system and MonetDB for computing batches of aggregates, and on the other hand, TensorFlow, Scikit, R, and AC/DC for learning a variety of models over databases.
In Vitro Evaluation of the Broad-Spectrum Antimicrobial Potential of Lactic Acid Bacteria Isolated from Milk Whey and Nunu for Veterinary Applications

Background Information One of the characteristic of bacteria zoonoses diseases is their tendency to re-emerge, as such they said to be responsible for a very high proportion of morbidity and mortality. Many documented zoonotic diseases and reported to be resistant to some conventional antibiotics. Similarly challenging is the fact that most of the antibiotics currently being used against these diseases are reported not to be completely metabolized and are often released in unmetabolized forms which when they find their ways into the food chain becomes health issue. Metabolites from some Lactic Acid Bacteria are being harnessed as a bio-active compounds for the novel unconventional control of these diseases which this research seeks to make contribution. Abstract Zoonoses incidences continue to play significant roles in both human and veterinary medicine and their eradication especially in the developing country like Nigeria, is difficult. Zoonotic food-borne infections caused by Gram-positive and Gram-negative bacteria are re-emerging. Several findings indicated that the cell-free supernatant derived from some Lactic Acid Bacteria have some antibacterial effects when applied directly or added to food during packaging. The aim of this study was to investigate the in vitro antagonistic effect of cell-free supernatant derived from some LAB species isolated from whey and Nunu (obtained from a locally fermented milk product) against some zoonotic bacteria pathogens (Escherichia coli, Salmonella sp. and Staphylococcus aureus. Streptococcus sp. and Salmonella sp. Four (4) LAB isolates were isolated, identified using basic morphological and biochemical characterization and screened on the basis of functional and technological characterization. The Cell-free supernatant from these strains, Lactobacillus casei LB01, Lactobacillus sp. LB02, Lactobacillus acidophilus LB03 and Lactobacillus plantarum LB04 were prepared by centrifugation at 10,000 rpm for 5 minutes and used against the indicator organisms at 107 CFU/ml using agar well diffusion method. The cell-free supernatant inhibited the growth of both Gram- positive and Gram-negative bacteria strains of veterinary origins. Our findings suggest that the LAB strains have the potential for antibiotic alternatives for the control of several zoonotic diseases. This holds a great advantage in the current efforts to tackling and reducing the prevalence and spread of zoonotic diseases which are re-emerging in Nigeria
Derivation of the Disorder Induced Interaction and the Phase Diagram of Cuprate Superconductors

We show that an electronic phase transition described by the Cahn-Hilliard equation has important applications to cuprate superconductors. The simulations of the local charge density and free energy reveal two main features: i) The segregation process creates tiny isolated regions with potential wells where the holes can be bound in single-particle levels. ii) The clustering process also gives rise to an effective two-body pairing interactions and superconducting amplitudes $\Delta_{sc}(\vec r)$ at low temperatures. The resulting system resembles a granular superconductor with the resistivity transition driven by Josephson coupling among these nanoscale grains. This approach reproduces the well known critical temperature transition $T_c(p)$ as function of the doping level $p$. The derived $p \times T$ phase diagram reproduces the main features measured by several experiments. Furthermore, the local density of states with spatial dependent gaps $\Delta(\vec r)$ is due to the intragrain single-particle bound states that remain above $T_c$, which characterizes the pseudogap phase and reproduces many measurements.
Non-fiducial cosmological test from geometrical and dynamical distortions around voids

We present a new cosmological test using the distribution of galaxies around cosmic voids without assuming a fiducial cosmology. The test is based on a physical model for the void-galaxy cross-correlation function projected along and perpendicular to the line of sight. We treat correlations in terms of void-centric angular distances and redshift differences between void-galaxy pairs, hence it is not necessary to assume a fiducial cosmology. This model reproduces the coupled dynamical (Kaiser effect, RSD) and geometrical (Alcock-Paczynski effect, GD) distortions that affect the correlation measurements. It also takes into account the scale mixing due to the projection ranges in both directions. The model is general, so it can be applied to an arbitrary cylindrical binning scheme, not only in the case of the projected correlations. It primarily depends on two cosmological parameters: $\Omega_m$, the matter fraction of the Universe today (sensitive to GD), and $\beta$, the ratio between the growth rate factor of density perturbations and the tracer bias (sensitive to RSD). In the context of the new generation of galaxy spectroscopic surveys, we calibrated the test using the Millennium XXL simulation for different redshifts. The method successfully recovers the cosmological parameters. We studied the effect of measuring with different projection ranges, finding robust results up to wide ranges. The resulting data covariance matrices are relatively small, which reduces the noise in the Gaussian likelihood analysis and will allow the usage of a smaller number of mock catalogues. The performance evaluated in this work indicates that the developed method is a promising test to be applied on real data.
Early growth of typical high-redshift black holes seeded by direct collapse

Understanding the growth of high redshift massive black holes (MBHs) is a problem of great astrophysical interest. The most luminous quasars at $z>6$ are frequently observed but they represent only the tip of the iceberg as the majority of the low luminosity AGN population remains undetected. In the present study, we perform a radiation hydrodynamics cosmological simulation to study the growth of "normal" black holes in the high redshift universe. In our simulation we model the formation of Pop III and Pop II stars along with their chemical, mechanical and radiative feedback. We consider both UV and X-ray emission from an accreting BH to simulate its radiative feedback. The selected halo has a mass of $\rm 3 \times 10^{10}~M_{\odot}$ at $z=7.5$ and we turn on radiative feedback from a MBH seed of $\rm 10^5~M_{\odot}$ along with in-situ star formation at $z=12$ when the halo mass reaches well above the atomic cooling limit. We find that the MBH accretes only about 2200 $\rm M_{\odot}$ during 320 Myr and the average mass accretion onto the MBH is a few times $\rm 10^{-6}~M_{\odot}/yr$. Our results suggest that the stunted growth of MBH is a consequence of supernovae in tandem with MBH feedback which drive large outflows and evacuate the gas from MBH vicinity. This may explain why a population of low luminosity AGN has not been detected so-far at $z>6$; the large contrast between the star formation rate and the MBH accretion rate may make then hard to detect even in upcoming deep surveys.
Correlation of Language Assessment Batteries of Toddlers With Developmental Language Delay

Objective To analyze the correlation between standardized language assessment batteries of toddlers and developmental language delays. Methods A total of 319 children with suspected language developmental delays were enrolled in this study retrospectively. They underwent the Receptive and Expressive Vocabulary Test (REVT) for vocabulary development assessment and at least one of two language assessment batteries: The Sequenced Language Scale for Infants (SELSI) or the Preschool Receptive-Expressive Language Scale (PRES) for language development assessment. The correlation of the results for receptive and expressive language between the scales were analyzed. Results The participants were divided into two groups: SELSI and REVT (n=45) and PRES and REVT (n=273). When the children’s results were classified into groups (average, mild delay, and delay), receptive and expressive scores were significantly correlated with each other in both SELSI-REVT and PRES-REVT groups. In addition, the correlation of mean developmental age between tests are analyzed. In the SELSI-REVT group, there was weak correlation of mean developmental age between tests for receptive and expressive language. In the PRES-REVT group, there was a strong positive correlation of mean developmental age for receptive and expressive language in children aged >36 months. Attention deficits during the test was found to be the statistically significant factor affecting the differences between the tests. The odds ratios for receptive and expressive language were 2.60 (95% confidence interval,1.15–5.84) and 1.94 (95% confidence interval, 1.15–3.27), respectively. Conclusion This study examined the correlations and influencing factors between language development evaluation tools for toddlers. An integrated interpretation of comprehensive language and vocabulary evaluation tools may be possible in children older than 3 years of language developmental age.
Authigenic Formation of Clay Minerals in the Abyssal North Pacific

Present estimates of the biogeochemical cycles of calcium, strontium, and potassium in the ocean reveal large imbalances between known input and output fluxes. Using pore fluid, incubation, and solid sediment data from North Pacific multi‐corer cores we show that, contrary to the common paradigm, the top centimeters of abyssal sediments can be an active site of authigenic precipitation of clay minerals. In this region, clay authigenesis is the dominant sink for potassium and strontium and consumes nearly all calcium released from benthic dissolution of calcium carbonates. These observations support the idea that clay authigenesis occurring over broad regions of the world ocean may be a major buffer for ocean chemistry on the time scale of the ocean overturning circulation, and key to the long‐term stability of Earth's climate.
Opportunities for Astrophysical Science from the Inner and Outer Solar System

Astrophysical measurements away from the 1 AU orbit of Earth can enable several astrophysical science cases that are challenging or impossible to perform from Earthbound platforms, including: building a detailed understanding of the extragalactic background light throughout the electromagnetic spectrum; measurements of the properties of dust and ice in the inner and outer solar system; determinations of the mass of planets and stellar remnants far from luminous stars using gravitational microlensing; and stable time-domain astronomy. Though potentially transformative for astrophysics, opportunities to fly instrumentation capable of these measurements are rare, and a mission to the distant solar system that includes instrumentation expressly designed to perform astrophysical science, or even one primarily for a different purpose but capable of precise astronomical investigation, has not yet been flown. In this White Paper, we describe the science motivations for this kind of measurement, and advocate for future flight opportunities that permit intersectional collaboration and cooperation to make these science investigations a reality.
Fly-in-fly-out work: A review of the impact of an extreme form of work-related travel on mental health

Large distances between work and home require many workers to stay away from home for work over extended periods. An extreme case of such work is fly-in-fly-out (FIFO) work. FIFO work requires workers to stay, over a fixed number of days or weeks, in remote employer-arranged accommodation. Given the disruptive nature of this work arrangement, it is important to develop an understanding of its implications for worker mental health. Based on a systematic review, we identify mostly negative mental health implications of FIFO work and propose an integrative model that brings together FIFO work's key features: the simultaneous fracturing and blending of personal and work lives. The model can guide future research. For example, we suggest that researchers investigate how FIFO workers and other work-related travelers experience fracturing and blending, and how they manage the frequent fluctuation between these two extremes. Plain language summary Fly-in-fly-out work represents a specific and extreme case of work-related travel in which workers are housed by employers and have fixed schedules that prescribe blocks of time at work followed by blocks of time at home, alongside other rules. This paper provides an overview of the literature regarding the mental health implications of FIFO work. Moreover, an integrative model of FIFO work is proposed that brings together its key defining attributes: the simultaneous fracturing and blending of personal and work lives, which FIFO workers, and by extension other work-related travellers, experience. The model identifies the key attributes of this type of work arrangement that shape fracturing namely the commute (i.e., duration, mode, distance) and rosters (i.e., length and ratio of time on and off) and blending experiences, namely accommodation (i.e., type and quality), extent to which autonomy is limited (i.e., via choice in food, activities, scheduling) and social isolation. While developed for an extreme, highly standardized, and specific case of work-related travel, the model may also be useful in research focused on work related travel more broadly,
Exploring the dimming event of RW Aurigae A through multi-epoch VLT/X-shooter spectroscopy

Context. RW Aur A is a classical T Tauri star that has suddenly undergone three major dimming events since 2010. The reason for these dimming events is still not clear. Aims. We aim to understand the dimming properties, examine accretion variability, and derive the physical properties of the inner disc traced by the CO ro-vibrational emission at near-infrared wavelengths (2.3 μm). Methods. We compared two epochs of X-shooter observations, during and after the dimming. We modelled the rarely detected CO bandhead emission in both epochs to examine whether the inner disc properties had changed. The spectral energy distribution was used to derive the extinction properties of the dimmed spectrum and compare the infrared excess between the two epochs. Lines tracing accretion were used to derive the mass accretion rate in both states. Results. The CO originates from a region with physical properties of T = 3000 K, NCO = 1 × 1021 cm−2 and vk sin i = 113 km s−1. The extinction properties of the dimming layer were derived with the effective optical depth ranging from τeff ~2.5−1.5 from the UV to the near-IR. The inferred mass accretion rate Ṁacc is ~1.5 × 10−8 M⊙ yr−1 and ~2 × 10−8 M⊙ yr−1 after and during the dimming respectively. By fitting the spectral energy distribution, additional emission is observed in the infrared during the dimming event from dust grains with temperatures of 500–700 K. Conclusions. The physical conditions traced by the CO are similar for both epochs, indicating that the inner gaseous disc properties do not change during the dimming events. The extinction curve is flatter than that of the interstellar medium, and large grains of a few hundred microns are thus required. When we correct for the observed extinction, the mass accretion rate is constant in the two epochs, suggesting that the accretion is stable and therefore does not cause the dimming. The additional hot emission in the near-IR is located at about 0.5 au from the star and is not consistent with an occulting body located in the outer regions of the disc. The dimming events could be due to a dust-laden wind, a severe puffing-up of the inner rim, or a perturbation caused by the recent star-disc encounter.