Miracle-dz/UniFAR-FTUs huggingface dataset:
Constructing a Digital Twin of the Birdcage Coil in an MR Scanner by Map Matching: For Radio Frequency Heating Evaluation of Implantable Medical Devices

Radio frequency (RF)-induced heating associated with medical implants is a critical concern when performing a magnetic resonance imaging (MRI) scan. The purpose of this study is to construct a “digital twin” of RF coil integrated in an MRI scanner by <inline-formula> <tex-math notation="LaTeX">$B_{1}^{+}$ </tex-math></inline-formula> map matching, reproducing the physical electromagnetic (EM) field, allowing it to be a qualified test environment for heating evaluations. <inline-formula> <tex-math notation="LaTeX">$B_{1}^{+}$ </tex-math></inline-formula> map inside an American Society for Testing Material (ASTM) phantom with various positions was used to characterize the physical EM field. A loaded tuned two-port birdcage body coil model was established to generate the numerical EM field and optimized to minimize the difference between the measured and simulated fields, which was quantified by “mean symmetric mean absolute percentage error” (mSMAPE). The amplitude of the simulated field was normalized to MR sequence labeling. Finally, the average specific absorption rate (SAR) inside the ASTM phantom was measured in a calorimetry experiment and compared to simulation one heated by the pre-established coil. A heating experiment was performed on an insulated cable to further validate the established test environment. The impact of excitation parameters and the port location was investigated. mSMAPE of the optimized field was less than 10%. The difference between the simulated and measured average SAR was 8.5%. <inline-formula> <tex-math notation="LaTeX">$R^{2}$ </tex-math></inline-formula> for the linear regression of the temperature rise and predicted power deposition using the optimized field was 0.993. The digital twin was successfully constructed and verified a sufficiently accurate description of the physical field. The established construction method of the digital twin provides a handy choice for building RF test environment and may create more possibilities for the development of this area.
Irradiation effect on leaf sclerophylly, gas exchange and stomata in sweet orange (Citrus sinensis)

The study was carried out in mutated population of sweet orange [Citrus sinensis (L.) Osbeck] cv. Mosambi developed from varying dose of gamma rays (10-35 Gy) to determine its effect on leaf sclerophylly, photosynthesis and leaf anatomical characters at the Division of Fruits and Horticultural Technology, ICAR-Indian Agricultural Research Institute, New Delhi during 2017 and 2018. As compared to wild type leaf area, fresh and dry mass was stimulated by 19.53, 18.42 and 20.37% in mutant GS-3 developed from 10 Gy, while in the mutants GS-33 and GS-35 developed from 35 Gy >50% inhibitory effects were noticed. Leaves were however, 82.06% more succulent in the mutant developed from 30 Gy. Mutated population showed dose dependent effect with regard to SLA, SLW and DFT. A significant decline in the photosynthetic rate and stomatal conductance was noticed at 35 Gy in GS-32, whereas mutant GS-34 developed from the same irradiation dose had the minimum transpiration rate. Stomata length and width in the mutants GS-17 and GS-15 as compared to wild type registered an increase of 25.50% and 15.96%. A general reduction in stomata number was observed in the mutated populations. Our result indicated alteration in traits of the mutated population which are of significance and can be used as a selection criterion for improvement of sweet orange.
Supervised Classification of Motor-Rehabilitation Body Movements with RGB Cameras and Pose Tracking Data

The technological evolution allowed the use of a single camera for precise and effective body tracking, reducing the cost and increasing the accessibility of applications in places where depth cameras and wearable sensors are not available. This paper describes and implements a supervised machine learning process consisting of a mobile application used as a motion capture device which also transforms the data into an input for a machine learning model that classifies upper and lower limbs movements (24 types of human movements). The user performs movements in front of the camera, and the trained model classifies them. We designed the system to work in a motor-rehabilitation context to assist the professional while the patient does physical exercises. The implementation can summarize the movements made during the rehabilitation sessions by counting the repetitions and classifying them when done completely or reached a specific range of motion.
PROBING THE TERMINATOR REGION ATMOSPHERE OF THE HOT-JUPITER XO-1b WITH TRANSMISSION SPECTROSCOPY

We report here the first infrared spectrum of the hot-Jupiter XO-1b. The observations were obtained with the NICMOS instrument on board the Hubble Space Telescope during a primary eclipse of the XO-1 system. Near photon-noise-limited spectroscopy between 1.2 and 1.8 μm allows us to determine the main composition of this hot-Jupiter's planetary atmosphere with good precision. This is the third hot-Jupiter's atmosphere for which spectroscopic data are available in the near-IR. The spectrum shows the presence of water vapor (H2O), methane (CH4), and carbon dioxide (CO2), and suggests the possible presence of carbon monoxide (CO). We show that the published IRAC secondary transit emission photometric data are compatible with the atmospheric composition at the terminator determined from the NICMOS spectrum, with a range of possible mixing ratios and thermal profiles; additional emission spectroscopy data are needed to reduce the degeneracy of the possible solutions. Finally, we note the similarity between the 1.2–1.8 μm transmission spectra of XO-1b and HD 209458b, suggesting that in addition to having similar stellar/orbital and planetary parameters the two systems may also have a similar exoplanetary atmospheric composition.
Fabrication and Manipulation of Non-Spherical Particles in Microfluidic Channels: A Review

Non-spherical shape is a general appearance feature for bioparticles. Therefore, a mechanical mechanism study of non-spherical particle migration in a microfluidic chip is essential for more precise isolation of target particles. With the manipulation of non-spherical particles, refined disease detection or medical intervention for human beings will be achievable in the future. In this review, fabrication and manipulation of non-spherical particles are discussed. Firstly, various fabrication methods for non-spherical microparticle are introduced. Then, the active and passive manipulation techniques for non-spherical particles are briefly reviewed, including straight inertial microchannels, secondary flow inertial microchannels and deterministic lateral displacement microchannels with extremely high resolution. Finally, applications of viscoelastic flow are presented which obviously increase the precision of non-spherical particle separation. Although various techniques have been employed to improve the performance of non-spherical particle manipulation, the universal mechanism behind this has not been fully discussed. The aim of this review is to provide a reference for non-spherical particle manipulation study researchers in every detail and inspire thoughts for non-spherical particle focused device design.
Global well posedness for a two-fluid model

We study a two fluid system which models the motion of a charged fluid with Rayleigh friction, and in the presence of an electro-magnetic field satisfying Maxwell's equations. We study the well-posdness of the system in both space dimensions two and three. Regardless of the size of the initial data, we first prove the global well-posedness of the Cauchy problem when the space dimension is two. However, in space dimension three, we construct global weak-solutions \`a la Leray, and we prove the local well-posedness of Kato-type solutions. These solutions turn out to be global when the initial data are sufficiently small. Our results extend Giga-Yoshida (1984) ones to the space dimension two, and improve them in terms of requiring less regularity on the velocity fields.
Detection of faint broad emission lines in type 2 AGN – I. Near-infrared observations and spectral fitting

This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge funding from PRIN/MIUR and PRIN/INAF. MB acknowledges support from the FP7 Career Integration Grant “eEASy” (CIG 321913).
Asymptotic expansions and in-equalities for hypergeometric functions

Ramanujan's work on the asymptotic behaviour of the hypergeometric function has been recently refined to the zero-balanced Gaussian hypergeometric function F ( a , b ; a + b ; x ) as x →1.We extend these results for F ( a , b ; c ; x ) when a , b , c >0 and c a + b .
Star-formation history and X-ray binary populations: the case of the Large Magellanic Cloud

In the present work we investigate the link between high-mass X-ray binaries (HMXBs) and star formation in the Large Magellanic Cloud (LMC), our nearest star-forming galaxy. Using optical photometric data, we identify the most likely counterpart of 44 X-ray sources. Among the 40 HMXBs classified in this work, we find 33 Be/X-ray binaries, and 4 supergiant XRBs. Using this census and the published spatially resolved star-formation history map of the LMC, we find that the HMXBs (and as expected the X-ray pulsars) are present in regions with starformation bursts ∼6–25 Myr ago, in contrast to the Small Magellanic Cloud (SMC), for which this population peaks at later ages (∼25–60 Myr ago). We also estimate the HMXB production rate to be equal to 1 system per ∼ 43.5 × 10−3 M yr−1 or 1 system per ∼143 M of stars formed during the associated star-formation episode. Therefore, the formation efficiency of HMXBs in the LMC is ∼17 times lower than that in the SMC. We attribute this difference primarily in the different ages and metallicity of the HMXB populations in the two galaxies. We also set limits on the kicks imparted on the neutron star during the supernova explosion. We find that the time elapsed since the supernova kick is ∼3 times shorter in the LMC than the SMC. This in combination with the average offsets of the HMXBs from their nearest star clusters results in ∼4 times faster transverse velocities for HMXBs in the LMC than in the SMC.
Virial sequences for thick discs and haloes: flattening and global anisotropy

Stellar haloes and thick discs are tracer populations and make only a modest contribution to the overall gravity field. Here, we exploit the virial theorem to provide formulae for the ratio of the globally averaged equatorial to vertical velocity dispersion of a tracer population in spherical and flattened dark matter haloes. This gives virial sequences of possible physical models in the plane of global anisotropy and flattening. The tracer may have any density distribution, although there are particularly simple results for power laws and exponentials. We prove the Flattening Theorem: for a spheroidally stratified tracer density with axis ratio q in equilibrium in a dark density potential with axis ratio g, the ratio of globally averaged equatorial to vertical velocity dispersion depends only on the combination q/g. As the stellar halo density and velocity dispersion of the Milky Way are accessible to observations, this provides a new method for measuring the flattening of the dark matter distribution in our Galaxy. If the kinematics of the local halo subdwarfs are representative, then the Milky Way’s dark halo model is oblate with a flattening in the potential of g≈ 0.85, corresponding to dark matter density contours with flattening ≈0.7. The fractional pressure excess for power-law populations is roughly proportional to both the ellipticity and the fall-off exponent. Given the same pressure excess, if the density profile of one stellar population declines more quickly than that of another, then it must be rounder. This implies that the dual halo structure claimed by Carollo et al. for the Galaxy – a flatter inner halo and a rounder outer halo – is inconsistent with the virial theorem. For the thick disc, we provide formulae for the virial sequences of double-exponential discs in logarithmic and Navarro–Frenk–White (NFW) haloes. There are good matches to the observational data on the flattening and anisotropy of the thick disc if the thin disc is exponential with a short scalelength ≈2.6 kpc and local surface density of 56 ± 6 M⊙ pc−2, together with a logarithmic dark halo. Thin discs with long scalelengths ≈3.5 kpc are disfavoured. Likewise, NFW potentials do not seem to produce virial sequences matching the thick disc kinematics.
Health beliefs and health anxiety as predictors of COVID-19 health behavior: Data from Serbia

The end of 2019 and the beginning of 2020 were marked by the appearance of the virus SARS-CoV-2, which led to a health crisis around the world. Health preventive behavior was highlighted as, at that time, the only form of prevention of the spread of the disease. Factors that will lead people to adhere to the recommended forms of behavior have become the subject of research in various scientific disciplines. The Model of Health Belief is one of the dominant frameworks for studying health behaviors, and thus behaviors related to COVID-19. Health anxiety and beliefs about illness and preventive behavior are the starting point for considering the level at which individuals adhere to the recommended measures. The main goal of this research was to examine a model in which health anxiety and health beliefs are predictors of preventive health behavior in relation to COVID-19. The sample consisted of 420 respondents, 66.3% of whom were women. They completed an online questionnaire comprising the following instruments: Short Health Anxiety Inventory, COVID-19 Health Belief Scale, and COVID-19 Health Behavior Scale with two subscales-Protection in Social Contacts and Hygiene. After controlling for effects of gender and presence of chronic disease, perceived benefit of preventive behavior and the observed barrier can predict protection in social contacts. Hygiene can be predicted by the perceived benefit of preventive behavior and the perceived barrier. Health anxiety has not been shown to be a significant predictor of health behavior. The paper discusses the theoretical and practical implications of the obtained results. The obtained results partially support the Model of Health Beliefs. In order to increase the degree to which individuals adhere to health behaviors, the benefits of preventive behaviors should be emphasized while the barriers should be reduced.
Versatile fluoride substrates for Fe-based superconducting thin films

We demonstrate the growth of Co-doped BaFe2As2 (Ba-122) thin films on CaF2 (001), SrF2 (001), and BaF2 (001) single crystal substrates using pulsed laser deposition. All films are grown epitaxially despite of a large misfit of −10.6% for BaF2 substrate. For all films, a reaction layer is formed at the interface confirmed by X-ray diffraction and for the films grown on CaF2 and BaF2 additionally by transmission electron microscopy. The superconducting transition temperature of the film on CaF2 is around 27 K, whereas the corresponding values of the films on SrF2 and BaF2 are around 22 K and 21 K, respectively. The Ba-122 on CaF2 shows almost identical crystalline quality and superconducting properties as films on Fe-buffered MgO.
Nonlinear collisionless damping of Weibel turbulence in relativistic blast waves

The Weibel/filamentation instability is known to play a key role in the physics of weakly magnetized collisionless shock waves. From the point of view of high energy astrophysics, this instability also plays a crucial role because its development in the shock precursor populates the downstream with a small-scale magneto-static turbulence which shapes the acceleration and radiative processes of suprathermal particles. The present work discusses the physics of the dissipation of this Weibel-generated turbulence downstream of relativistic collisionless shock waves. It calculates explicitly the first-order nonlinear terms associated to the diffusive nature of the particle trajectories. These corrections are found to systematically increase the damping rate, assuming that the scattering length remains larger than the coherence length of the magnetic fluctuations. The relevance of such corrections is discussed in a broader astrophysical perspective, in particular regarding the physics of the external relativistic shock wave of a gamma-ray burst.
STRUCTURAL EVOLUTION OF EARLY-TYPE GALAXIES TO z = 2.5 IN CANDELS

Projected axis ratio measurements of 880 early-type galaxies at redshifts 1 < z < 2.5 selected from CANDELS are used to reconstruct and model their intrinsic shapes. The sample is selected on the basis of multiple rest-frame colors to reflect low star-formation activity. We demonstrate that these galaxies as an ensemble are dust-poor and transparent and therefore likely have smooth light profiles, similar to visually classified early-type galaxies. Similar to their present-day counterparts, the z > 1 early-type galaxies show a variety of intrinsic shapes; even at a fixed mass, the projected axis ratio distributions cannot be explained by the random projection of a set of galaxies with very similar intrinsic shapes. However, a two-population model for the intrinsic shapes, consisting of a triaxial, fairly round population, combined with a flat (c/a ∼ 0.3) oblate population, adequately describes the projected axis ratio distributions of both present-day and z > 1 early-type galaxies. We find that the proportion of oblate versus triaxial galaxies depends both on the galaxies' stellar mass, and—at a given mass—on redshift. For present-day and z < 1 early-type galaxies the oblate fraction strongly depends on galaxy mass. At z > 1, this trend is much weaker over the mass range explored here (1010 < M*/M☉ < 1011), because the oblate fraction among massive (M* ∼ 1011 M☉) was much higher in the past: 0.59 ± 0.10 at z > 1, compared to 0.20 ± 0.02 at z ∼ 0.1. When combined with previous findings that the number density and sizes of early-type galaxies substantially increase over the same redshift range, this can be explained by the gradual emergence of merger-produced elliptical galaxies, at the expense of the destruction of pre-existing disks that were common among their high-redshift progenitors. In contrast, the oblate fraction among low-mass early-type galaxies (log (M*/M☉) < 10.5) increased toward the present, from z = 0 to 0.38 ± 0.11 at z > 1 to 0.72 ± 0.06 at z = 0. We speculate that this lower incidence of disks at early cosmic times can be attributed to two factors: low-mass, star-forming progenitors at z > 1 were not settled into stable disks to the same degree as at later cosmic times, and the stripping of gas from star-forming disk galaxies in dense environments is an increasingly important process at lower redshifts.
Curvature constraints from large scale structure

We modified the CLASS code in order to include relativistic galaxy number counts in spatially curved geometries; we present the formalism and study the effect of relativistic corrections on spatial curvature. The new version of the code is now publicly available. Using a Fisher matrix analysis, we investigate how measurements of the spatial curvature parameter ΩK with future galaxy surveys are affected by relativistic effects, which influence observations of the large scale galaxy distribution. These effects include contributions from cosmic magnification, Doppler terms and terms involving the gravitational potential. As an application, we consider angle and redshift dependent power spectra, which are especially well suited for model independent cosmological constraints. We compute our results for a representative deep, wide and spectroscopic survey, and our results show the impact of relativistic corrections on spatial curvature parameter estimation. We show that constraints on the curvature parameter may be strongly biased if, in particular, cosmic magnification is not included in the analysis. Other relativistic effects turn out to be subdominant in the studied configuration. We analyze how the shift in the estimated best-fit value for the curvature and other cosmological parameters depends on the magnification bias parameter, and find that significant biases are to be expected if this term is not properly considered in the analysis.
Updated templates for the interpretation of LHC results on supersymmetry in the context of mSUGRA

In this short note, we describe the preparation of updated templates for the interpretation of SUSY results from the LHC in the context of mSUGRA. The standard (m0;m1=2) plane is shown for xed > 0 and mt = 173.2 GeV. Two scenarios are considered: (1) A0 = 0 GeV and tan( ) = 10 and (2) A0 = 500 GeV and tan( ) = 40. In each case, the universal scalar mass parameter m0 varies in the range m02 [40; 3000] GeV, while the universal gaugino mass parameter m1=2 varies in the range m1=2 2 [100; 1000] GeV. We delineate notable regions in parameter space, including the region with a charged LSP (stau), the LEP2 reach, and the cosmologically preferred region with 100% neutralino dark matter. The templates also show mass contours for a few key particles (gluino, squark and Higgs boson). The mass spectrum is calculated with the SoftSusy-3.2.4 package, while the neutralino relic density is obtained with MicrOMEGAs version 2.4.
The large $\mathcal{N}=4$ superconformal $\mathcal{W}_\infty$ algebra

The most general large ${\cal N}=4$ superconformal ${\cal W}_{\infty}$ algebra, containing in addition to the superconformal algebra one supermultiplet for each integer spin, is analysed in detail. It is found that the ${\cal W}_{\infty}$ algebra is uniquely determined by the levels of the two $\mathfrak{su}(2)$ algebras, a conclusion that holds both for the linear and the non-linear case. We also perform various cross-checks of our analysis, and exhibit two different types of truncations in some detail.