Miracle-dz/UniFAR-FTUs huggingface dataset:
Prevalence of Multidrug Resistance in Pseudomonas Aeruginosa in Healthcare Facilities

Pseudomonas aeruginosa is on the list of Gram-negative pathogens that are increasingly being counted as significant causes of nosocomial infections leading to significantly raised levels of morbidity and mortality. Life-threatening infections become more debilitating for those having a compromised immunity. The importance of Pseudomonas aeruginosa as a disease-causing microbe is enhanced through its increasing resistance to antibiotic drugs, the virulence factors plus its strength to adapt to wider environmental conditions. Pseudomonas aeruginosa possesses multiple acquired and intrinsic mechanisms providing resistance, often with augmented rates of resistance to multiple antimicrobial drugs. In the last decade, the global dissemination of the presumed ‘hazardous clones’ of multiple drug-resistant and extensively drug-resistant Pseudomonas aeruginosa have emerged as a serious threat to communal healthcare requiring extensive study and should be managed with determination and urgency. From the list of infections that are due to Gram-negative bacteria, Pseudomonas aeruginosa counts as a leading microbe causative for health-care-related infections in hospitalized individuals. In accordance with the guidelines by WHO, certain measures adopted in healthcare settings can help prevent transmission of multidrug-resistant Pseudomonas aeruginosa including hand hygiene (using alcohol-based solutions), contact precautions, cleanliness of the environment, isolation of patient (cohort or single room), plus surveillance. Keywords: Antibiotic resistance, Nosocomial, Infections, Resistance mechanisms, Pseudomonas aeruginosa
Spin Glass a Bridge Between Quantum Computation and Statistical Mechanics

We show two fascinating topics lying between quantum information processing and statistical mechanics. First, we introduce an elaborated technique, the surface code, to prepare the particular quantum state with robustness against decoherence. Second, we show another interesting technique to employ quantum nature, quantum annealing. Through both of the topics, we would shed light on the birth of the interdisciplinary field between quantum mechanics and statistical mechanics.
Cosmic Ray Spectrum in Supernova Remnant Shocks

We performed kinetic simulations of diffusive shock acceleration in Type Ia supernova remnants (SNRs) expanding into a uniform interstellar medium (ISM). The preshock gas temperature is the primary parameter that governs the cosmic ray (CR) acceleration, while magnetic field strength and CR injection rate are secondary parameters. SNRs in the hot ISM, with an injection fraction smaller than 10^{-4}, are inefficient accelerators with less than 10 % energy getting converted to CRs. The shock structure is almost test-particle like and the ensuing CR spectrum can be steeper than E^{-2}. Although the particles can be accelerated to the knee energy of 10^{15.5}Z eV with amplified magnetic fields in the precursor, Alfv'enic drift of scattering centers softens the source spectrum as steep as E^{-2.1} and reduces the CR acceleration efficiency.
What kind of energy is the mass

In 1905, Einstein discovered the famous equation: E=mc^2, which means that the rest mass of a particle is some kind of energy. This energy is generally referred to as "rest energy", since the particle is believed to be at rest. This paper proposes a new interpretation to the term mc^2. Observing the similarity between the term mc^2 and the kinetic energy term mv^2/2, we propose to interpret mc^2 as being one term of kinetic energy. In other words we propose that, in the called "rest frame", the massive particles are not really at rest, but they are doing a special kind of motion at the light speed c. In this interpretation the "mass" is not an intrinsic property of the particle. The "mass" is simply the kinetic energy associated with this special kind of motion. The more important consequence of this hypothesis is that the term mc^2, present in the relativistic Hamiltonian, must be rewritten as: mc^2 => p_0 c, where p_0 = mc is the modulus of the instantaneous linear moment \vec{p}_0 associated with the special motion. We analyse a physical scenario in which this special motion is a Microscopic Orbital Circular Motion (MOCM). The characteristic length scale of the MOCM is of the order of the Compton wavelength of the particle.
ON THE INCONSISTENCY BETWEEN COSMIC STELLAR MASS DENSITY AND STAR FORMATION RATE UP TO z ∼ 8

In this paper, we test the discrepancy between the stellar mass density (SMD) and instantaneous star formation rate in the redshift range 0 < z < 8 using a large observational data sample. We first compile the measurements of SMDs up to z ∼ 8. Comparing the observed SMDs with the time-integral of instantaneous star formation history (SFH), we find that the observed SMDs are lower than that implied from the SFH at z < 4. We also use the Markov chain Monte Carlo (MCMC) method to derive the best-fitting SFH from the observed SMD data. At 0.5 < z < 6, the observed star formation rate densities are larger than the best-fitting one, especially at z ∼ 2 where they are larger by a factor of about two. However, at lower (z < 0.5) and higher redshifts (z > 6), the derived SFH is consistent with the observations. This is the first time that the discrepancy between the observed SMD and instantaneous star formation rate has been tested up to very high redshift z ≈ 8 using the MCMC method and a varying recycling factor. Several possible reasons for this discrepancy are discussed, such as underestimation of SMD, initial mass function, and evolution of cosmic metallicity.
Constraining High-Energy Cosmic Neutrino Sources: Implications and Prospects

We consider limits on the local (z=0) density (n0) of extragalactic neutrino sources set by the nondetection of steady high-energy neutrino sources producing ≳50 TeV muon multiplets in the present IceCube data, taking into account the redshift evolution, luminosity function, and neutrino spectrum of the sources. We show that the lower limit depends moderately on source spectra and strongly on redshift evolution. We find n0≳10-8–10-7 Mpc-3 for standard candle sources evolving rapidly, ns∝(1+z)3, and n0≳10-6–10-5 Mpc-3 for nonevolving sources. The corresponding upper limits on their neutrino luminosity are Lνμeff≲1042–1043 erg s-1 and Lνμeff≲1041–1042 erg s-1, respectively. Applying these results to a wide range of classes of potential sources, we show that powerful “blazar” jets associated with active galactic nuclei are unlikely to be the dominant sources. For almost all other steady candidate source classes (including starbursts, radio galaxies, and galaxy clusters and groups), an order of magnitude increase in the detector sensitivity at ∼0.1–1 PeV will enable a detection (as point sources) of the few brightest objects. Such an increase, which may be provided by next-generation detectors like IceCube-Gen2 and an upgraded KM3NET, can improve the limit on n0 by more than 2 orders of magnitude. Future gamma-ray observations (by Fermi, the High-Altitude Water Cherenkov Observatory, and the Cherenkov Telescope Array) will play a key role in confirming the association of the neutrinos with their sources.
Single-gap s-wave superconductivity in Cu$_x$TiSe$_2$

The in-plane thermal conductivity $\kappa$ of the layered superconductor Cu$_x$TiSe$_2$ was measured down to temperatures as low as $T_c$/40, at $x$ = 0.06 near where the CDW order vanishes. The absence of a residual linear term at $ T \to 0$ is strong evidence for conventional s-wave superconductivity in this system. This is further supported by the slow magnetic field dependence, also consistent with a single gap, of uniform magnitude across the Fermi surface. Comparison with the closely related material NbSe$_2$, where the superconducting gap is three times larger on the Nb 4$d$ band than on the Se 4$p$ band, suggests that in Cu$_{0.06}$TiSe$_2$ the Se 4$p$ band is below the Fermi level and the Ti 3$d$ band is alone responsible for the superconductivity.
EMOTIONAL FINANCE: AN EMPIRICAL STUDY ON PSYCHOLOGY OF INVESTORS IN AHMEDABAD

PURPOSE – The author aims to examine the psychology of investors and relationship between different Behavioral biases. Author also examines the impact of emotions influence the behaviour of investors. Author has also mentioned the principal concerns associated to investors. DESIGN – This study investigates the influence the influence of behavioral biases and emotions on investors. It also studied the relationship between biases through correlation. ORIGINALITY/VALUE – Prior studies focus merely on the aspect of emotions finance. Our study provides comprehensive outlook on both behavioral finance and emotional finance.
A Novel Differentially-Fed Dual-Polarized Shared Aperture Antenna Array

This communication proposes a novel dual-polarized shared-aperture antenna array with wide bandwidth (BW) by carefully designing and tightly arranging the elements. The single element comprises four L-probes and four parasitic patches, differentially fed by microstrip lines for each polarization, with a profile of around <inline-formula> <tex-math notation="LaTeX">$0.073\lambda _{\mathbf {0}}$ </tex-math></inline-formula> (<inline-formula> <tex-math notation="LaTeX">$\lambda _{\mathbf {0}}$ </tex-math></inline-formula> is one free-space wavelength at the center frequency). Simulated results show that the impedance BW (<inline-formula> <tex-math notation="LaTeX">$\vert \,\,{S} _{\mathbf {11}}\,\,\vert < -10$ </tex-math></inline-formula> dB) is 35% for both orthogonal polarizations, with a low cross-polarization level and a peak gain up to 9.7 dBi. The shared-aperture property is investigated using two <inline-formula> <tex-math notation="LaTeX">$1\times $ </tex-math></inline-formula> 2 arrays. Subsequently, two <inline-formula> <tex-math notation="LaTeX">$4\times $ </tex-math></inline-formula> 4 dual-polarized arrays with ideal differential feeds are employed to illustrate how the proposed shared-aperture approach can improve the aperture efficiency. Finally, a dual-polarized <inline-formula> <tex-math notation="LaTeX">$4\times $ </tex-math></inline-formula> 4 array prototype with microstrip line feeding networks arranged in different layers is designed, fabricated, and experimentally verified. It presents an overlapped BW of 25.4% from 23 to 29.7 GHz for the two orthogonal polarizations, a peak gain of 19.8 dBi, and an isolation larger than 18 dB. Most of all, the <inline-formula> <tex-math notation="LaTeX">$4\times $ </tex-math></inline-formula> 4 array occupies only a size of <inline-formula> <tex-math notation="LaTeX">$3.32\lambda _{\mathbf {0}} \times 3.28\lambda _{\mathbf {0}} \times 0.087\lambda _{\mathbf {0}}$ </tex-math></inline-formula>.
On graph bipartization

The author discusses an undirected, connected graph G(V,E) without multiple edges and self loops. The minimum node (edge) deletion bipartite subgraph problem for G(V,E) is considered. Constant time computable upper and lower bounds are presented on the number of nodes (edges) deleted. The bounds are useful when very little is known about G(V,E). Heuristic solutions for each of these problems are introduced. The time complexity of both heuristics is O( mod V mod /sup 2/). <<ETX>>
A Prospective Randomized Comparative Study Between Midvastus and Standard Medial Parapatellar Approaches for Total Knee Replacement Regarding the Peri-Operative Factors

Introduction The aim of this study was to determine whether the midvastus (MV) approach in patients who underwent total knee replacement (TKR) results in differences regarding peri-operative parameters, such as surgical time, blood loss, transfusion need and complications, when compared with medial parapatellar approach (MP). Methods This was a prospective randomized comparative study of patients who received primary TKR. The first group consisted of patients where the MP approach was used and the second those where the MV approach was utilized. Patient’s age, body mass index (BMI), stage of osteoarthritis (OA), prosthesis design, duration of surgery, blood loss in the drainage, hemoglobin (Hb), and intra-operative complications were recorded. Results From December 2019 to June 2020 a total of 107 (22 males, 85 females) and 38 (seven males, 31 females) patients were operated on with the MP and MV approaches, respectively. The two groups did not differ in terms of age, BMI, gender and stage of OA, however, pre-operative haemoglobin (Hb) was higher in the MP group [mean 13,5 (1.3) versus 13.1 (0.73)]. There was no significant difference in Hb decline pre- and post-operatively and in drain volume between groups. The mean Hb drop was similar for the MP [-2.2 (1.08)] and MV [-2.52 (1.06)] groups, and even though the transfusion rates were lower for the MP group, it did not reach significance. The duration of surgery was significantly longer in the MV group, with a mean time of 95.6 (12.94) minutes versus 89.4 (14.28) in the MP group. Overall complications did not differ significantly among the two surgical approaches. Multivariate logistic regression demonstrated that pre-operative Hb [OR 2.6 95% CI (1.43, 4.75)] and approach [OR 4.15 95% CI (1.15, 14.98)] were significantly correlated with the need for transfusion when gender, BMI, redon drainage, prosthesis size and duration of surgery were considered together. Conclusion In our experience, total knee replacement performed with either the midvastus or medial parapatellar approach does not result in any advantage with regards to the intra-operative complications, drain blood volume or difference in Hb drop post-operative. However, the midvastus approach presents a longer operation time, with the risk of higher transfusion rates for the patients.
Free‐Body Diagrams: Necessary or Sufficient?

The Rutgers PAER group is working to help students develop various scientific abilities. One of the abilities is to create, understand and learn to use for qualitative reasoning and problem solving different representations of physical processes such as pictorial representations, motion diagrams, free‐body diagrams, and energy bar charts. Physics education literature indicates that using multiple representations is beneficial for student understanding of physics ideas and for problem solving. We developed a special approach to construct and utilize free‐body diagrams for representing physical phenomena and for problem solving. We will examine whether students draw free‐body diagrams in solving problems when they know they will not receive credit for it; the consistency of their use in different conceptual areas; and if students who use free‐body diagrams while solving problems in different areas of physics are more successful then those who do not.
The transition from quasar radio-loud to radio-quiet state in the framework of the black hole scalability hypothesis

Aims. There are several lines of evidence that active galactic nuclei (AGN) can be regarded as scaled-up X-ray binaries (XRB). The timescales of the evolutionary phenomena in these two classes are proportional to the black hole (BH) masses. Consequently, unlike in the case of XRBs, the evolution of AGNs is too slow to be followed directly. What could be done, however, is to assign particular types of active galaxies to different evolutionary stages observable in XRBs. We studied such an assignment for three quasars with clear signatures of a recent transition from the radio-loud to the radio-quiet state. Methods. The quasars we investigated have large-scale radio lobes that are clearly asymmetric – one lobe is of Fanaroff-Riley II type, while the other one is a diffuse relic devoid of a hotspot. We suggest that the prime cause of the asymmetry of these radio sources is that the nuclei of their host galaxies currently produce no jets. To prove that, we observed them with milliarcsecond resolution to check if they are similar to those in radio-quiet quasars. Results. The observations carried out with the EVN revealed that the nuclei of the quasars under investigation are not of a core-jet type that is characteristic for radio-loud, lobe-dominated quasars. It follows that the lobes are no longer fuelled and that the apparent asymmetry results from the orientation, which causes a time lag of the order of 10 6 years between their images: the lobe perceived as a relic is nearer than the lobe with a hotspot and so it is observed in a later stage of the decay. Conclusions. The three AGNs under investigation were radio-loud earlier, but now they have switched to the radio-quiet state. In the framework of the XRB/AGN unification, the above means that they have left the very high state and have moved now to the high/soft state. If this scenario is correct it poses a challenge to the so-called spin paradigm. While a radio-loud AGN must have a spinning BH in its centre, the BH of a radio-quiet AGN does not necessarily have low spin; AGNs with high-spin BHs, like those we deal with here, may become radio-quiet.
HYPOGLYCEMIC ACTIVITY OF ORIGANUM VULGARE L. AQUEOUS EXTRACT IN HYPERGLYCEMIA INDUCED BY IMMOBILIZATION STRESS IN RABBITS

Currently diabetes mellitus (DM) is a worldwide problem linked to hyperglycemia and has affected people both in developing and developed countries. DM is divided into Type 1 (T1DM) and Type 2 (T2DM). Moreover, the T2DM is the most prevalence form that encompasses a reduce responsiveness to insulin-sensitive cells or defects in insulin secretion. Exposure to chronic immobilization stress contributes to the development of hyperglycemia and hyperlipidemia that can lead to cardiovascular complications. Herbs with hypoglycemic properties, especially Origanum vulgare L. , would be useful in hyperglycemia treatment. Oral administration of aqueous extract showed significant effect on hyperglycemia and improving glucose tolerance. In addition, extract of O. vulgare reduced total cholesterol, low-density lipoprotein cholesterol levels, and vice versa increased high-density lipoprotein cholesterol levels, and also decreased liver enzymes levels (alanine aminotransferase and aspartate aminotransferase) compared with untreated group and might be recommended as herbal remedy in the treatment of stress-induced hyperglycemia. The present study was undertaken to evaluate antihyperglycemic activities of O. vulgare leaf extract and some biochemical parameters in hyperglycemia induced by immobilization stress in rabbits.
Tomographic weak-lensing shear spectra from large N-body and hydrodynamical simulations

Context. Forthcoming experiments will enable us to determine tomographic shear spectra at a high precision level. Most predictions about them have until now been based on algorithms yielding the expected linear and non-linear spectrum of density fluctuations. Even when simulations have been used, so-called Halofit predictions on fairly large scales have been needed. Aims. We wish to go beyond this limitation. Methods. We perform N-body and hydrodynamical simulations within a sufficiently large cosmological volume to allow a direct connection between simulations and linear spectra. While covering large length-scales, the simulation resolution is good enough to allow us to explore the high-� harmonics of the cosmic shear (up to � ∼ 50 000), well into the domain where baryon physics becomes important. We then compare shear spectra in the absence and in presence of various kinds of baryon physics, such as radiative cooling, star formation, and supernova feedback in the form of galactic winds. Results. We distinguish several typical properties of matter fluctuation spectra in the different simulations and test their impact on shear spectra. Conclusions. We compare our outputs with those obtainable using approximate expressions for non-linear spectra, and identify substantial discrepancies even between our results and those of purely N-body results. Our simulations and the treatment of their outputs however enable us, for the first time, to obtain shear results that are fully independent of any approximate expression, also in the high-� range, where we need to incorporate a non-linear power spectrum of density perturbations and the effects of baryon physics. This will allow us to fully exploit the cosmological information contained in future high-sensitivity cosmic shear surveys, exploring the physics of cosmic shears via weak lensing measurements.
Formation dynamics and distribution function of cities population

From the data analysis we defined distribution function against the population on the level of various structure units, namely regions, federal districts and the country on the whole. We have studied peculiarities of the distribution function deformation due to the structure units’ enlargement. Using the master equation in the continuous approximation, we obtain the Fokker-Plank equation for the distribution function with symmetric transition rates. In addition, we offer a model where transitions only between neighbour states are possible. Moreover in this case it is proposed the in and out transition probability rate for any states are different We define condition for the formal equivalence of both models to the problem that is described by the stochastic differential equation with additive and multiplicative white noises. We have analyzed the corresponding Fokker-Plank equation in the Ito and Stratonovich calculus, and obtained a solution of the Tsallis distribution type. We demonstrate a comparison of theoretical results with those of the data analysis on the level a cumulative distributions. We have used the maximum likelihood method for fitting. The obtained results allow us to attribute the specific value of the Tsallis distribution nonextensivity parameter to the empiric curves.
Stability of binary on highly eccentric orbit

It is known, that possibility to capture on a satellite orbit is decreased with primary orbital eccentricity increasing. It means, that satellites of planet on eccentric orbit are less stable. We study problem by analytical and numeric methods. A difference between case of infinitesimal mass satellite and true binary system is shown. The dependence of orbital energy on external eccentricity is derived for binary system. In result of our studying, we can conclude, that extrasolar planets may have significantly smaller satellites, than planets in our solar system. Moreover, dependence on eccentricity makes restriction on giant planets migration in our Solar System. The application to a flight dynamics and mission design is discussed.
Exploring Neutrino Interactions with MicroBooNE

Recently, MiniBooNE observed an electromagnetic excess at low energy. What is the nature of this excess? What about the nature of the low-energy excess at LSND 20 years ago? The MicroBooNE detector will see neutrinos from the same Booster beam at Fermilab as used by MiniBooNE. MicroBooNE's design will enable us to discriminate photons from electrons elucidating the MiniBooNE and LSND low-energy electromagnetic excesses. MicroBooNE is a 170 ton liquid argon time projection chamber (LArTPC) capable of imaging neutrino interactions with the detail of a bubble chamber, but with electronic data acquisition and processing. In addition to shining light on the low-energy excesses and measuring low-energy neutrino cross sections, MicroBooNE is leading the way for a more extensive short-baseline neutrino physics program at Fermilab and it also serves as a R&D project towards a long-baseline multi-kiloton scale LArTPC detector.