Miracle-dz/UniFAR-FTUs huggingface dataset:
Feasibility and outcomes with subclavian vein access for crescent jugular dual lumen catheter for venovenous extracorporeal membrane oxygenation in COVID-19 related acute respiratory distress syndrome

Introduction Femoral-femoral Veno-Venous ExtraCorporeal Life Support (V-V ECLS) has been associated with higher infections rates, vascular site bleeding complications, and restricted patient mobility. Jugular or bicaval dual lumen V-V ECLS conceptually overcomes some of these adverse factors, but experience has shown that jugular vein cannulation still limits mobility and has increased bleeding complications. Technique and outcomes of subclavian vein single-cannulation with Crescent jugular dual-lumen V-V ECLS is described. Method five patients with COVID-19 related acute respiratory distress syndrome (ARDS) underwent right subclavian vein V-V ECLS placement with the Crescent 32 French jugular dual-lumen V-V ECLS catheter. A standardized percutaneous technique was developed that allowed efficient insertion without need for any specialized imaging (i.e. transesophageal echocardiogram) and outcomes assessed. Results Mean age of the five patients was 41.2 years, all obese with an average basal mass index of 45.2 kg/m2 and mean days to decannulation of 24.2 days. Outcomes discovered included; improved patient mobility allowing physical rehabilitation, no vascular access site related complications requiring surgery or endovascular intervention, and none had evidence of superior vena cava syndrome. One patient had subclavian/axillary vein thrombosis with resolution after 3 months of direct-acting oral anticoagulants, and one patient had blood cultures positive at day 37, nearing decannulation. Conclusion Subclavian vein access for crescent jugular dual lumen V-V ECLS catheter appears to be safe and feasible with added benefits of decreased bleeding and increased mobility over jugular or femoral-femoral access site for long term V-V ECLS support in COVID-19 related ARDS patients.
Pure spinors and D=6 super-Yang-Mills

Pure spinor cohomology has been used to describe maximally supersymmetric theories, like D=10 super-Yang-Mills and D=11 supergravity. Supersymmetry closes on-shell in such theories, and the fields in the cohomology automatically satisfy the equations of motion. In this paper, we investigate the corresponding structure in a model with off-shell supersymmetry, N=1 super-Yang-Mills theory in D=6. Here, fields and antifields are obtained as cohomologies in different complexes with respect to the BRST operator Q. It turns out to be natural to enlarge the pure spinor space with additional bosonic variables, subject to some constraints generalising the pure spinor condition, in order to accommodate the different supermultiplets in the same generalised pure spinor wave-function. We construct another BRST operator, s, acting in the cohomology of Q, whose cohomology implies the equations of motion. We comment on the possible use of similar approaches in other models.
Accretion dynamics in the classical T Tauri star V2129 Ophiuchi

We analyze the photometric and spectroscopic variability of the classical T Tauri star V2129 Oph over several rotational cycles to test the dynamical predictions of magnetospheric accretion models. The photometric variability and the radial velocity variations in the photospheric lines can be explained by rotational modulation due to cold spots, while the radial velocity variations of the He I (5876 \AA) line and the veiling variability are due to hot spot rotational modulation. The hot and cold spots are located at high latitudes and about the same phase, but the hot spot is expected to sit at the chromospheric level, while the cold spot is at the photospheric level. Using the dipole+octupole magnetic-field configuration previously proposed in the literature for the system, we compute 3D MHD magnetospheric simulations of the star-disk system. We use the simulation's density, velocity and scaled temperature structures as input to a radiative transfer code, from which we calculate theoretical line profiles at all rotational phases. The theoretical profiles tend to be narrower than the observed ones, but the qualitative behavior and the observed rotational modulation of the H\alpha and H\beta emission lines are well reproduced by the theoretical profiles. The spectroscopic and photometric variability observed in V2129 Oph support the general predictions of complex magnetospheric accretion models with non-axisymmetric, multipolar fields.
Gaseous time projection chambers for rare event detection: results from the T-REX project. I. Double beta decay

As part of the T-REX project, a number of R&D and prototyping activities have been carried out during the last years to explore the applicability of gaseous Time Projection Chambers (TPCs) with Micromesh Gas Structures (Micromegas) in rare event searches like double beta decay, axion research and low-mass WIMP searches. In both this and its companion paper, we compile the main results of the project and give an outlook of application prospects for this detection technique. While in the companion paper we focus on axions and WIMPs, in this paper we focus on the results regarding the measurement of the double beta decay (DBD) of 136Xe in a high pressure Xe (HPXe) TPC. Micromegas of the microbulk type have been extensively studied in high pressure Xe and Xe mixtures. Particularly relevant are the results obtained in Xe + trimethylamine (TMA) mixtures, showing very promising results in terms of gain, stability of operation, and energy resolution at high pressures up to 10 bar. The addition of TMA at levels of ∼ 1% reduces electron diffusion by up to a factor of 10 with respect to pure Xe, improving the quality of the topological pattern, with a positive impact on the discrimination capability. Operation with a medium size prototype of 30 cm diameter and 38 cm of drift (holding about 1 kg of Xe at 10 bar in the fiducial volume, enough to contain high energy electron tracks in the detector volume) has allowed to test the detection concept in realistic experimental conditions. Microbulk Micromegas are able to image the DBD ionization signature with high quality while, at the same time, measuring its energy deposition with a resolution of at least a ∼ 3% FWHM @ Qββ. This value was experimentally demonstrated for high-energy extended tracks at 10 bar, and is probably improvable down to the ∼ 1% FWHM levels as extrapolated from low energy events. In addition, first results on the topological signature information (one straggling track ending in two blobs) show promising background discrimination capabilities out of reach of other experimental implementations. Moreover, microbulk Micromegas have very low levels of intrinsic radioactivity, and offer cost-effective scaling-up options. All these results demonstrate that Micromegas-read HPXe TPC remains a very competitive technique for the next generation DBD experiments.
Power law violation of the area law in quantum spin chains

Entanglement between two quantum systems is a non-classical correlation between them. Entanglement is a feature of quantum mechanics which does not appear classically, and it serves as a resource for quantum technologies. In condensed matter theory, the area law says that the amount of entanglement between a subsystem and the rest of the system is proportional to the area of the boundary of the subsystem [1]. A system that obeys an area law can be simulated more efficiently than an arbitrary quantum system, and an area law provides useful information about the low-energy physics of the system [1–3]. The area law has only been proved for one-dimensional systems with a constant-energy spectral gap [4]. However, it is widely believed that for physically reasonable quantum systems, the area law could not be violated by more than a logarithmic factor in the system’s size [5]. Here, we introduce a class of exactly solvable one dimensional models that have exponentially more entanglement than previously expected, and violate the area law by a square root factor. In addition to using recent advances in quantum information theory, we have drawn upon various branches of mathematics in our work. We hope that the tools we have developed may be useful for other problems in physics as well.
Sensory-motor training versus resistance training in the treatment of knee osteoarthritis: A randomized controlled trial

Objective To compare the effectiveness of sensory-motor training and resistance training in patients with knee osteoarthritis. Design Randomized controlled trial. Setting Istanbul University, Department of Physiotherapy and Rehabilitation. Subjects Forty-eight participants with knee osteoarthritis. Interventions Following baseline assessment, participants were randomly allocated to sensory-motor training (n = 24) and resistance training (n = 24). Both groups received training three times a week for 8 weeks. Main measures The primary outcome measure was the Western Ontario and McMaster Universities Arthritis Index (WOMAC). The secondary outcome measures were pain level, muscle strength, proprioception, range of motion, quality of life, and patient satisfaction with treatment. Patients were assessed before and after four- and eight-week interventions. Results There was no significant difference between the groups’ total WOMAC scores after four- and eight-week interventions (respectively, p = 0.415, p = 0.828). There was a significant improvement in pain level during movement and in the energy subscale SF-36 for resistance training after the four-week intervention (respectively, p = 0.012, p = 0.007). After the eight-week intervention, a significant difference was noted in favor of resistance training in the secondary outcome measure quality of life (QoL). No significant difference was found in other secondary outcomes. Conclusions At the end of the treatment, it was observed that sensory-motor training had a similar effect in the treatment of knee osteoarthritis symptoms to resistance training. These findings may suggest that sensory-motor training is an effective new method to treat patients with knee osteoarthritis.
Evolution of the early Universe in the scale invariant theory.

Analytical solutions are obtained for the early cosmological phases in the scale invariant models with curvature k=0. They complete the analytical solutions already found in the matter--dominated era by (Jesus 2018). The physical properties in the radiative era are derived from the conservation laws and compared to those of current standard models. The critical runs of the temperature T(MeV) and of the expansion rate H of the scale invariant models with low densities, Omega_m=0.04, are quite similar at the time of nucleosynthesis to those of standard models with Omega_m=0.30, leading to the same freezing number ratio of neutrons to protons.These results are consistent with the fact that the scale invariant models appear to not require the presence of dark matter.
Heat kernel based decomposition of spaces of distributions in the framework of Dirichlet spaces

Classical and nonclassical Besov and Triebel-Lizorkin spaces with complete range of indices are developed in the general setting of Dirichlet space with a doubling measure and local scale-invariant Poincare inequality. This leads to a heat kernel with small time Gaussian bounds and Holder continuity, which play a central role in this article. Frames with band limited elements of sub-exponential space localization are developed, and frame and heat kernel characterizations of Besov and Triebel-Lizorkin spaces are established. This theory, in particular, allows the development of Besov and Triebel-Lizorkin spaces and their frame and heat kernel characterization in the context of Lie groups, Riemannian manifolds, and other settings.
Investigating the Method of Da’wah and the Role of Political-Economy of Jemaah Tarbiyah in Urban Malang Society

Since the emergence of the overwhelming electoral vote for Partai Keadilan Sejahtera (Prosperous Justice Party) in the 2019 legislative election in Malang City, we discovered the impact of political-economy of Jemaah Tarbiyah on the urban society is a significant boost in electability for PKS. The subject selected is an Islamic philanthropic organisation, Ash-Shahwah Foundation (YASA) in Malang City as the sympathisers of Jemaah Tarbiyah. The supportive factors for regulating the political economy of Jemaah Tarbiyah include the method, role, and participation of YASA in Malang City. Through the method of da’wah, the figure of Jemaah Tarbiyah, Abu Haidar, stated that shalat is the key to success in life, and this has been successfully gaining hundreds of members. The role of YASA is to educate the urban society that obligatory alms become a lifestyle for their charitable politics. YASA becomes an intermediary to the connection of elite-mass or mustahiq-cadres’ relationships for gaining trust and getting massive electoral votes. The urban society participation, particularly the benefactors, can be seen from their enthusiasm in donating their wealth and demonstrating solidarity among individuals to strengthen informal religious learning courses in mosques. Findings show that the political economy of Jemaah Tarbiyah initiated the great success of gaining substantial electoral votes through philanthropic practices used as indirect support and funding for election campaigns. Notably, there is a political tendency for YASA to change its paradigm of philanthropic practice, for which the initial goal was to raise humanitarian aid and charitable funds and to shift funds toward financing a campaign.
Expansion for the product of matrices in groups

Abstract In this paper, we give strong lower bounds on the size of the sets of products of matrices in some certain groups. More precisely, we prove an analogue of a result due to Chapman and Iosevich for matrices in SL 2 ⁢ ( 𝔽 p ) {\mathrm{SL}_{2}(\mathbb{F}_{p})} with restricted entries on a small set. We also provide extensions of some recent results on expansion for cubes in Heisenberg group due to Hegyvári and Hennecart.
DRIVING DISK WINDS AND HEATING HOT CORONAE BY MRI TURBULENCE

We investigate the formation of hot coronae and vertical outflows in accretion disks by magnetorotational turbulence. We perform local three-dimensional magnetohydrodynamical (MHD) simulations with the vertical stratification by explicitly solving an energy equation with various effective ratios of specific heats, γ. Initially imposed weak vertical magnetic fields are effectively amplified by magnetorotational instability and winding caused by the differential rotation. In the isothermal case (γ = 1), the disk winds are driven mainly by the Poynting flux associated with the MHD turbulence and show quasi-periodic intermittency. In contrast, in the non-isothermal cases with γ ⩾ 1.1, the regions above 1–2 scale heights from the midplane are effectively heated to form coronae with temperature ∼50 times the initial value, which are connected to the cooler midplane region through the pressure-balanced transition regions. As a result, the disk winds are driven mainly by the gas pressure, exhibiting more time-steady nature, although the nondimensional time-averaged mass loss rates are similar to that of the isothermal case. Sound-like waves are confined in the cool midplane region in these cases, and the amplitude of the density fluctuations is larger than that of the isothermal case.
The galactic unclassified B[e] star HD 50138 - I. A possible new shell phase

Context. The observed spectral variation of HD 50138 has led different authors to classify it in a very wide range of spectral types and luminosity classes (from B5 to A0 and III to Ia) and at different evolutionary stages as either HAeBe star or classical Be. Aims. Based on new high-resolution optical spectroscopic data from 1999 and 2007 associated to a photometric analysis, the aim of this work is to provide a deep spectroscopic description and a new set of parameters for this unclassified southern B[e] star and its interstellar extinction. Methods. From our high-resolution optical spectroscopic data separated by 8 years, we perform a detailed spectral description, presenting the variations seen and discussing their possible origin. We derive the interstellar extinction to HD 50138 by taking the influences of the circumstellar matter in the form of dust and an ionized disk into account. Based on photometric data from the literature and the new Hipparcos distance, we obtain a revised set of parameters for HD 50138. Results. Because of the spectral changes, we tentatively suggest that a new shell phase could have taken place prior to our observations in 2007. We find a color excess value of E(B − V) = 0.08 mag, and from the photometric analysis, we suggest that HD 50138 is a B6-7 III-V star. A discussion of the different evolutionary scenarios is also provided.
The analysis and validation of natural frequencies and mode shapes of 3D plates in the framework of the generalized thermoelastic theory

Abstract This article considers thermal effects that induce thermoelastic damping and, which, consequently, because of the absorbed thermal energy, cause thermal stresses. The problem is stated in the framework of the generalized thermoelastic theory. The natural frequency and mode shape analyzes of 3D plates are presented under uniform and nonuniform heating. From the modeling point of view, this results in the quadratic eigenvalue problem where complex frequencies and modes are obtained. Moreover, the quality factor related to the thermoelastic damping is also calculated in terms of the imaginary and the real parts of the frequencies for both the uniform and nonuniform thermal distributions. The variation of natural frequencies with temperature is investigated and compared with the experimental results for the plates with free boundary conditions. The first two mode shapes are also examined for all clamped edges for the uniform and nonuniform cases. Complex frequencies and complex modes are observed due to the thermal effects. For the uniform case, the real part of the modes decreases and the complex part increases, while the mode’s norm remains the same as in the classical modes as temperature increases. For the nonuniform case, the mode shape analysis is performed under the assumption that the elasticity modulus, thermal expansion, and specific heat parameters are functions of temperature. The peak point of the out-of-plane displacement is shown to be shifted toward the warm zone. The obtained outcomes may help design thermal structures and allow for future extensions.
METAL-RICH PLANETARY NEBULAE IN THE OUTER REACHES OF M31

Spectroscopic data of two relatively [O iii]-luminous planetary nebulae (PNe) have been obtained with the 10.4 m Gran Telescopio Canarias. M174 and M2496 are each ∼1° from the center of M31 along opposite sides of its minor axis. The ensemble of these 2 distant PNe plus 16 similarly luminous outer-disk PNe published previously by Kwitter et al. forms a homogeneous group in luminosity, metal content, progenitor mass, age, and kinematics. The main factual findings of our work are (1) O/H (and other low-mass α elements and their ratios to O) is uniformly solar-like in all 18 PNe (〈12 + log(O/H)〉 = 8.62 ± 0.14); (2) the general sky distribution and kinematics of the ensemble much more closely resemble the rotation pattern of the classical disk of M31 than its halo or bulge; (3) the O/H gradient is surprisingly flat beyond Rg ∼ 20 kpc. The PNe are too metal-rich to be bona fide members of M31's disk or halo, and (4) the abundance patterns of the sample are distinct from those in the spiral galaxies M33, M81, and NGC 300. Using standard PN age diagnostic methods, we suggest that all of the PNe formed ∼2 Gyr ago in a starburst of metal-rich interstellar medium that followed an M31–M33 encounter about 3 Gyr ago. We review supporting evidence from stellar studies. Other more prosaic explanations, such as dwarf galaxy assimilation, are unlikely.
Planetary nebulae: the universal mass–metallicity relation for Local Group dwarf galaxies and the chemistry of NGC 205

Here we study 16 planetary nebulae (PNe) in the dwarf irregular galaxy NGC 205 by using GMOS@Gemini spectra to derive their physical and chemical parameters. The chemical patterns and evolutionary tracks for 14 of our PNe suggest that there are no type I PNe among them. These PNe have an average oxygen abundance of 12+log(O/H)=8.08$\pm$0.28, progenitor masses of 2-2.5M$_{\odot}$ and thus were born ~1.0-1.7Gyr ago. Our results are in good agreement with previous PN studies in NGC 205. The present 12+log(O/H) is combined with our previous works and with the literature to study the PN metallicity trends of the Local Group (LG) dwarf galaxies, in an effort to establish the PN luminosity- and mass-metallicity relations (LZR and MZR) for the LG dwarf irregulars (dIrrs) and dwarf spheroidals (dSphs). Previous attempts to obtain such relations failed to provide correct conclusions because were based on limited samples (Richer & McCall 1995; Gon\c{c}calves et al. 2007). As far as we are able to compare stellar with nebular metallicities, our MZR is in very good agreement with the slope of the MZR recently obtained for LG dwarf galaxies using spectroscopic stellar metallicities (Kirby et al. 2013). Actually, we found that both dIrr and dSph galaxies follow the same MZR, at variance with the differences claimed in the past. Moreover our MZR is also consistent with the global MZR of star-forming galaxies, which span a wider stellar mass range ($\sim10^6$ - $\sim10^{11}$M$\odot$).
Axions and the Strong CP Problem

Current upper bounds on the neutron electric dipole moment constrain the physically observable quantum chromodynamic (QCD) vacuum angle $|\overline{\ensuremath{\theta}}|\ensuremath{\lesssim}{10}^{\ensuremath{-}11}$. Since QCD explains a great deal of experimental data from the $100\phantom{\rule{0.3em}{0ex}}\mathrm{MeV}$ to the TeV scale, it is desirable to explain this smallness of $|\overline{\ensuremath{\theta}}|$ in the QCD framework; this is the strong $CP$ problem. There now exist two plausible solutions to this problem, one of which leads to the existence of a very light axion. The axion decay constant window, ${10}^{9}\ensuremath{\lesssim}{F}_{a}\ensuremath{\lesssim}{10}^{12}\phantom{\rule{0.3em}{0ex}}\mathrm{GeV}$ for an $O(1)$ initial misalignment angle ${\ensuremath{\theta}}_{1}$, has been obtained from astrophysical and cosmological data. For ${F}_{a}\ensuremath{\gtrsim}{10}^{12}\phantom{\rule{0.3em}{0ex}}\mathrm{GeV}$ with ${\ensuremath{\theta}}_{1}lO(1)$, axions may constitute a significant fraction of the dark matter of the universe. The supersymmetrized axion solution of the strong $CP$ problem introduces its superpartner the axino, which might have affected the evolution of the Universe significantly. The very light axion (theory, supersymmetrization, and models) using recent particle, astrophysical, and cosmological data, and present prospects for its discovery is reviewed here.