Miracle-dz/UniFAR-FTUs huggingface dataset:
A Rapid Review on matrix rhythm therapy

This brief study focuses on the effectiveness of Matrix rhythm therapy which exist as new development in the stream of physiotherapy used for the purpose of relieving pain, improves microcirculation, relaxation and increases oxygen supply of blood. A non-invasive method for gently releasing muscular tension and obtaining quick pain relief that can be used in conjunction with other forms of manual therapy or on its alone. A frequency range of 8-12 hz to stimulates the body’s natural self-healing powers storing good tissue resonance using a device by vibromassage method. The vibrating magneting field goes deep into the tissues via a reasonating head sending a phase synchronised mechanical vibration. It is used in conditions like chronic back pain, frozen shoulder, stroke, plantar fasciitis and lymphedema. In rehabilitation facilitate and compensatory education, clubs of sports, and neurological, orthopaedic, physiotherapy, and rehab centres, a new vibromassage application is being implemented.
ESG Rating and Market Valuation of the Firm: Sector Approach

The main aim of the study was to assess the impact of the ESG rating of the company on its market valuation. The research sample included stock companies of real economy sectors of financial markets of European Union Member States in years 2018-2020. The research hypothesis stated that across financial markets of European Union there are sectors in which there is a strong and positive correlation between high ESG rating of the company and its market value. The paper analysed selected measures of descriptive statistics of used variables, Pearson correlation coefficient, and constructed an Ordinary Least Squared model assessing the impact of ESG rating on the surveyed companies’ market value. Both the composites of ESG rating (ESG and ESGC) and the individual components (E, S, G and C) were analysed. Financial data and ESG ratings were extracted from Refinitiv Eikon database. Undertaken research proved ESG disclosure and rating to be the determinant of the companies market value in specific sectors, while companies controversies appeared to be the destructors of market value of companies across all sectors. Undertaken study adds new insights to the debate on the relation between companies ESG and financial performance by applying sector approach to the analysis.
Outlier-robust estimation of a sparse linear model using 𝓁1-penalized Huber's M-estimator

We study the problem of estimating a $p$-dimensional $s$-sparse vector in a linear model with Gaussian design and additive noise. In the case where the labels are contaminated by at most $o$ adversarial outliers, we prove that the $\ell_1$-penalized Huber's $M$-estimator based on $n$ samples attains the optimal rate of convergence $(s/n)^{1/2} + (o/n)$, up to a logarithmic factor. For more general design matrices, our results highlight the importance of two properties: the transfer principle and the incoherence property. These properties with suitable constants are shown to yield the optimal rates, up to log-factors, of robust estimation with adversarial contamination.
X-RAY AND NEAR-INFRARED OBSERVATIONS OF THE OBSCURED ACCRETING PULSAR IGR J18179−1621

IGR J18179−1621 is an obscured accreting X-ray pulsar discovered by INTEGRAL on 2012 February 29. We report on our 20 ks Chandra-High Energy Transmission Gratings Spectrometer observation of the source performed on 2012 March 17, on two short contemporaneous Swift observations, and on our two near-infrared (Ks, Hn, and Jn) observations performed on 2012 March 13 and 26. We determine the most accurate X-ray position of IGR J18179−1621, αJ2000 = 18h17m52. ˢ18, δJ2000 = −16°21′31. ″68 (90% uncertainty of 0.″6). A strong periodic variability at 11.82 s is clearly detected in the Chandra data, confirming the pulsating nature of the source, with the light-curve softening at the pulse peak. The quasi-simultaneous Chandra–Swift spectra of IGR J18179−1621 can be well fit by a heavily absorbed hard power law (NH = 2.2 ± 0.3 × 1023 cm−2 and photon index Γ = 0.4 ± 0.1) with an average absorbed 2–8 keV flux of 1.4 × 10−11 erg cm−2 s−1. At the Chandra-based position, a source is detected in our near-infrared (NIR) maps with Ks = 13.14 ± 0.04 mag, Hn = 16 ± 0.1 mag, and no Jn-band counterpart down to ∼18 mag. The NIR source, compatible with 2MASS J18175218−1621316, shows no variability between 2012 March 13 and 26. Searches of the UKIDSS database show similar NIR flux levels at epochs six months prior to and after a 2007 February 11 archival Chandra observation where the source's X-ray flux was at least 87 times fainter. In many ways IGR J18179−1621 is unusual: its combination of a several week long outburst (without evidence of repeated outbursts in the historical record), high absorption column (a large fraction of which is likely local to the system), and 11.82 s period does not fit neatly into existing X-ray binary categories.
HIGH-RESOLUTION IMAGES OF ORBITAL MOTION IN THE ORION TRAPEZIUM CLUSTER WITH THE LBT AO SYSTEM

The new 8.4 m LBT adaptive secondary AO system, with its novel pyramid wavefront sensor, was used to produce very high Strehl (≳ 75% at 2.16 μm) near-infrared narrowband (Brγ: 2.16 μm and [Fe ii]: 1.64 μm) images of 47 young (∼1 Myr) Orion Trapezium θ1 Ori cluster members. The inner ∼41 × 53″ of the cluster was imaged at spatial resolutions of ∼0. ″050 (at 1.64 μm). A combination of high spatial resolution and high S/N yielded relative binary positions to ∼0.5 mas accuracies. Including previous speckle data, we analyze a 15 year baseline of high-resolution observations of this cluster. We are now sensitive to relative proper motions of just ∼0.3 mas yr−1 (0.6 km s−1 at 450 pc); this is a ∼7 × improvement in orbital velocity accuracy compared to previous efforts. We now detect clear orbital motions in the θ1 Ori B2B3 system of 4.9 ± 0.3 km s−1 and 7.2 ± 0.8 km s−1 in the θ1 Ori A1A2 system (with correlations of P.A. versus time at >99% confidence). All five members of the θ1 Ori B system appear likely a gravitationally bound “mini-cluster. ” The very lowest mass member of the θ1 Ori B system (B4; mass ∼0.2 M☉) has, for the first time, a clearly detected motion (at 4.3 ± 2.0 km s−1; correlation = 99.7%) w.r. t. B1. However, B4 is most likely in a long-term unstable (non-hierarchical) orbit and may “soon” be ejected from this “mini-cluster. ” This “ejection” process could play a major role in the formation of low-mass stars and brown dwarfs.
Underlying mechanisms for normal heat transport in one-dimensional anharmonic oscillator systems with a double-well interparticle interaction

Previous studies have suggested a crossover from superdiffusive to normal heat transport in one-dimensional (1D) anharmonic oscillator systems with a double-well type interatomic interaction like V(ξ)=−ξ2/2+ξ4/4, when the system temperature is varied. In order to better understand this unusual manner of thermal transport, here we perform a direct dynamics simulation to examine how the spreading processes of the three physical quantities, i.e. the heat, the total energy and the momentum, would depend on temperature. We find three main points that are worth noting. (i) The crossover from superdiffusive to normal heat transport is well verified from a new perspective of heat spread. (ii) The spreading of the total energy is found to be very distinct from heat diffusion, especially under some temperature regimes, energy is strongly localized, while heat can be superdiffusive. So one should take care to derive a general connection between the heat conduction and energy diffusion. (iii) In a narrow range of temperatures, the spreading of momentum implies clear unusual non-ballistic behaviors; however, such unusual transport of momentum cannot be directly related to the normal transport of heat. An analysis of phonon spectra suggests that one should also take the effects of phonon softening into account. All of these results may provide insights into establishing the connection between the macroscopic heat transport and the underlying dynamics in 1D systems.
Exploring autonomous language learning behaviors through video sharing and online discussions in higher education

This current study explores how video sharing and online discussions promote learning autonomy in English language classes in a public university for the duration of the quarantine established by the Colombian government during the coronavirus pandemic. This study was conducted with 127 engineering and administration undergraduates from a public university in the department of Boyacá. This was a qualitative case study which intended to identify the extent video sharing and online discussions increase learner’s autonomy behaviors in English language learning . The instruments for data collection were student journal, student artifact, including video recordings and online discussions, interviews, and questionnaires. An open coding analysis was utilized and the results revealed that the degree of autonomous behaviors gradually could be fostered by the implementation of video sharing. Results also indicated that students are receptive to online writing discussions and showed how motivation plays a vital role in learning English and the achievement of own learning goals.
ON THE ROBUSTNESS OF z = 0–1 GALAXY SIZE MEASUREMENTS THROUGH MODEL AND NON-PARAMETRIC FITS

We present the size–stellar mass relations of nearby (z = 0.01–0.02) Sloan Digital Sky Survey galaxies, for samples selected by color, morphology, Sérsic index n, and specific star formation rate. Several commonly employed size measurement techniques are used, including single Sérsic fits, two-component Sérsic models, and a non-parametric method. Through simple simulations, we show that the non-parametric and two-component Sérsic methods provide the most robust effective radius measurements, while those based on single Sérsic profiles are often overestimates, especially for massive red/early-type galaxies. Using our robust sizes, we show for all sub-samples that the mass–size relations are shallow at low stellar masses and steepen above ∼3–4 × 1010 M☉. The mass–size relations for galaxies classified as late-type, low-n, and star-forming are consistent with each other, while blue galaxies follow a somewhat steeper relation. The mass–size relations of early-type, high-n, red, and quiescent galaxies all agree with each other but are somewhat steeper at the high-mass end than previous results. To test potential systematics at high redshift, we artificially redshifted our sample (including surface brightness dimming and degraded resolution) to z = 1 and re-fit the galaxies using single Sérsic profiles. The sizes of these galaxies before and after redshifting are consistent and we conclude that systematic effects in sizes and the size–mass relation at z ∼ 1 are negligible. Interestingly, since the poorer physical resolution at high redshift washes out bright galaxy substructures, single Sérsic fitting appears to provide more reliable and unbiased effective radius measurements at high z than for nearby, well-resolved galaxies.
TRACING RAM-PRESSURE STRIPPING WITH WARM MOLECULAR HYDROGEN EMISSION

We use the Spitzer Infrared Spectrograph to study four infalling cluster galaxies with signatures of ongoing ram-pressure stripping. H2 emission is detected in all four, and two show extraplanar H2 emission. The emission usually has a warm (T ∼ 115–160 K) and a hot (T ∼ 400–600 K) component that is approximately two orders of magnitude less massive than the warm one. The warm component column densities are typically 1019 to 1020 cm−2 with masses of 106 to 108M☉. The warm H2 is anomalously bright compared with normal star-forming galaxies and therefore may be excited by ram-pressure. In the case of CGCG 97-073, the H2 is offset from the majority of star formation along the direction of the galaxy's motion in the cluster, suggesting that it is forming in the ram-pressure wake of the galaxy. Another galaxy, NGC 4522, exhibits a warm H2 tail approximately 4 kpc in length. These results support the hypothesis that H2 within these galaxies is shock-heated from the interaction with the intracluster medium. Stripping of dust is also a common feature of the galaxies. For NGC 4522, where the distribution of dust at 8 μm is well resolved, knots and ripples demonstrate the turbulent nature of the stripping process. The Hα and 24 μm luminosities show that most of the galaxies have star-formation rates comparable to similar mass counterparts in the field. Finally, we suggest a possible evolutionary sequence primarily related to the strength of ram-pressure that a galaxy experiences to explain the varied results observed in our sample.
TWO PSEUDOBULGES IN THE “BOXY BULGE” GALAXY NGC 5746

Galaxy formation and growth under the ΛCDM paradigm is expected to proceed in a hierarchical, bottom-up fashion by which small galaxies grow into large galaxies; this mechanism leaves behind large “classical bulges” kinematically distinct from “pseudobulges” grown by internal, secular processes. We use archival data (Spitzer Space Telescope 3.6 μm wavelength, Hubble Space Telescope H-band, Two Micron All Sky Survey Ks-band, and Sloan Digital Sky Survey gri-band) to measure composite minor- and major-axis surface brightness profiles of the almost-edge-on spiral galaxy NGC 5746. These light profiles span a large range of radii and surface brightnesses to reveal an inner, high surface brightness stellar component that is distinct from the well-known boxy bulge. It is well fitted by Sérsic functions with indices n = 0.99 ± 0.08 and 1.17 ± 0.24 along the minor and major axes, respectively. Since n < 2, we conclude that this innermost component is a secularly evolved pseudobulge that is distinct from the boxy pseudobulge. This inner pseudobulge makes up 0.136 ± 0.019 of the total light of the galaxy. It is therefore considerably less luminous than the boxy structure, which is now understood to be a bar seen nearly end-on. The infrared imagery shows further evidence for secular evolution in the form of a bright inner ring of inner radius 9.1 kpc and width 1.6 kpc. NGC 5746 is therefore a giant, pure-disk SB(r)bc galaxy with no sign of a merger-built bulge. We do not understand how such galaxies form in a ΛCDM universe.
Operators with compatible ranges

A bounded operator $T$ on a finite or infinite--dimensional Hilbert space is called a disjoint range (DR) operator if $R(T)\cap R(T^*)=\{0\}$, where $T^*$ stands for the adjoint of $T$, while $R(\cdot)$ denotes the range of an operator. Such operators (matrices) were introduced and systematically studied by Baksalary and Trenkler, and later by Deng et al. In this paper we introduce a wider class of operators: we say that $T$ is a compatible range (CoR) operator if $T$ and $T^*$ coincide on $R(T)\cap R(T^*)$. We extend and improve some results about DR operators and derive some new results regarding the CoR class.
The Ratio of Helium- to Hydrogen-Atmosphere White Dwarfs: Direct Evidence for Convective Mixing

We determine the ratio of helium- to hydrogen-atmosphere white dwarf stars as a function of effective temperature from a model atmosphere analysis of the infrared photometric data from the Two Micron All Sky Survey combined with available visual magnitudes. Our study surpasses any previous analysis of this kind, both in terms of the accuracy of the Teff determinations and the size of the sample. We observe that the ratio of helium- to hydrogen-atmosphere white dwarfs increases gradually from a constant value of ~0.25 between Teff = 15,000 and 10,000 K to a value twice as large in the range 10,000 K > Teff > 8000 K, suggesting that convective mixing, which occurs when the bottom of the hydrogen convection zone reaches the underlying convective helium envelope, is responsible for this gradual transition. The comparison of our results with an approximate model used to describe the outcome of this convective mixing process implies hydrogen mass layers in the range MH/Mtot = 10−10 to 10−8 for about 15% of the DA stars that survived the DA-to-DB transition near Teff ∼ 30,000 K, the remainder having presumably more massive layers above MH/Mtot ∼ 10−6.
The metallicity of galactic winds

The abundance evolution of galaxies depends critically on the balance between the mixing of metals in their interstellar medium (ISM), the inflow of new gas and the outflow of enriched gas. We study these processes in gas columns perpendicular to a galactic disc using sub-parsec resolution simulations that track stellar ejecta with the flash code. We model a simplified ISM stirred and enriched by supernovae and their progenitors. We vary the density distribution of the gas column and integrate our results over an exponential disc to predict wind and ISM enrichment properties for disc galaxies. We find that winds from more massive galaxies are hotter and more highly enriched, in stark contrast to that which is often assumed in galaxy formation models. We use these findings in a simple model of galactic enrichment evolution, in which the metallicity of forming galaxies is the result of accretion of nearly pristine gas and outflow of enriched gas along an equilibrium sequence. We compare these predictions to the observed mass–metallicity relation, and demonstrate how the galaxy's gas fraction is a key controlling parameter. This explains the observed flattening of the mass–metallicity relation at higher stellar masses.
THE EXTREME ULTRAVIOLET DEFICIT: JET CONNECTION IN THE QUASAR 1442+101

In previous studies, it has been shown that the long-term time-averaged jet power, Q ¯ , ? > is correlated with spectral index in the extreme ultraviolet (EUV), αEUV (defined by F &ngr; ∼ &ngr; − &agr; EUV ? > computed between 700 and 1100 Å ). Larger Q ¯ ? > tends to decrease the EUV emission. This is a curious relationship because it connects a long-term average over ∼106 years with an instantaneous measurement of the EUV. The EUV appears to emit adjacent to the central supermassive black hole and the most straightforward explanation of this correlation is that the EUV-emitting region interacts in real time with the jet-launching mechanism. Alternatively stated, the Q ¯ ? > –αEUV correlation is a manifestation of a contemporaneous (real time) jet power, Q(t), correlation with αEUV. In order to explore this possibility, this paper considers the time variability of the strong radio jet of quasar 1442+101, which is not aberrated by strong Doppler enhancement. This high-redshift (z = 3.55) quasar is uniquely suited for this endeavor as the EUV is redshifted into the optical observing window allowing for convenient monitoring. More importantly, it is bright enough to be seen through the Lyman forest and its radio flux is strong enough that it has been monitored frequently. Quasi-simultaneous monitoring (five epochs spanning ∼40 years) shows that increases in Q(t) correspond to decreases in the EUV as expected.
EFFECT OF AMBIPOLAR DIFFUSION ON THE NONLINEAR EVOLUTION OF MAGNETOROTATIONAL INSTABILITY IN WEAKLY IONIZED DISKS

We study the role of ambipolar diffusion (AD) on the nonlinear evolution of the magnetorotational instability (MRI) in protoplanetary disks using the strong coupling limit, which applies in very weakly ionized gas with electron recombination time much shorter than the orbital time so that a single-fluid treatment is sufficient. The effect of AD in this limit is characterized by the dimensionless number Am, the frequency at which neutral particles collides with ions normalized to the orbital frequency. We perform three-dimensional unstratified shearing-box simulations of the MRI over a wide range of Am as well as different magnetic field strengths and geometries. The saturation level of the MRI turbulence depends on the magnetic geometry and increases with the net magnetic flux. There is an upper limit to the net flux for sustained turbulence, corresponding to the requirement that the most unstable vertical wavelength be less than the disk scale height. Correspondingly, at a given Am, there exists a maximum value of the turbulent stress αmax. For Am ≲ 1, the largest stress is associated with a field geometry that has both net vertical and toroidal flux. In this case, we confirm the results of linear analyses that show the fastest growing mode has a non-zero radial wavenumber with a growth rate exceeding that of the pure vertical field case. We find there is a very tight correlation between the turbulent stress α and the plasma 〈β〉 ≡ Pgas/Pmag ≈ 1/2α at the saturated state of the MRI turbulence regardless of field geometry, and αmax rapidly decreases with decreasing Am. In particular, we find αmax ≈ 7 × 10−3 for Am = 1 and αmax ≈ 6 × 10−4 for Am = 0.1.
A STARBURST IN THE CORE OF A GALAXY CLUSTER: THE DWARF IRREGULAR NGC 1427A IN FORNAX

Gas-rich galaxies in dense environments such as galaxy clusters and massive groups are affected by a number of possible types of interactions with the cluster environment, which make their evolution radically different than that of field galaxies. The dwarf irregular galaxy NGC 1427A, presently infalling toward the core of the Fornax galaxy cluster for the first time, offers a unique opportunity to study those processes at a level of detail not possible to achieve for galaxies at higher redshifts, when galaxy-scale interactions were more common. Using the spatial resolution of the Hubble Space Telescope/Advanced Camera for Surveys and auxiliary Very Large Telescope/FORS1 ground-based observations, we study the properties of the most recent episodes of star formation in this gas-rich galaxy, the only one of its type near the core of the Fornax cluster. We study the structural and photometric properties of young star cluster complexes in NGC 1427A, identifying 12 bright such complexes with exceptionally blue colors. The comparison of our broadband near-UV/optical photometry with simple stellar population models yields ages below ∼ 4 × 10 6 ? > years and stellar masses from a few 1000 up to ∼ 3 × 10 4 M ⊙ ? > , slightly dependent on the assumption of cluster metallicity and initial mass function. Their grouping is consistent with hierarchical and fractal star cluster formation. We use deep Hα imaging data to determine the current star formation rate in NGC 1427A and estimate the ratio, Γ, of star formation occurring in these star cluster complexes to that in the entire galaxy. We find Γ to be among the largest such values available in the literature, consistent with starburst galaxies. Thus a large fraction of the current star formation in NGC 1427A is occurring in star clusters, with the peculiar spatial arrangement of such complexes strongly hinting at the possibility that the starburst is being triggered by the passage of the galaxy through the cluster environment.
Direct photon-hadron correlation measurement and a way towards photon-triggered jets at RHIC

We report the results of γdir- and π0–hadron azimuthal correlations as a measure of the away-side jet-like correlated yields in central Au+Au and p+p collisions at sNN=200 GeV in the STAR experiment. The charged-hadron per-trigger yields at mid-rapidity with respect to high-pT γdir and π0 in central Au+Au collisions are compared with p+p collisions. Within uncertainties, the same zT(pTassoc/pTtrig) dependence of the suppression is observed for γdir- and π0- triggers. The results are compared with energy-loss model predictions. The γ − jet measurements can provide further understanding on the redistribution of in-medium energy loss. Ongoing γ − jet studies in the STAR experiment are also discussed.