Miracle-dz/UniFAR-FTUs huggingface dataset:
Dreams of Weaving: Creative Practice-Led Approach to Handloom Product Development in Sri Lanka Using Artisans’ Socio-Emotional Identities

Abstract Amidst the contemporary global trends of “hyper-localised” and “sustainable” fashion, the craft-based industries have been given substantial importance in recent times. Realising the competence of the Handloom weaving industry in Sri Lanka within the global fashion industry, this research proposes a new product development approach using the socio-emotional identities of the Handloom artisans. The study takes a practice-led approach following an initial data collection through qualitative research where a purposive sample of twenty-seven Handloom artisans from three provinces in Sri Lanka are interviewed and observed to identify their socio-emotional identities. The study subsequently guides the creation of an un-cut handloom textile developed by the artisans to explore the potential portrayal of the socio-emotional identities of a cross-section of Handloom weavers in Sri Lankan in the final product. This practice-led research chiefly contributes to the Handloom textile sector of Sri Lanka as it provides innovative and unforeseen avenues for new product development and contributes to the existing knowledge of craft-based research. The study affirms the need for acknowledging the Handloom artisans in Sri Lanka and adapting artisan-oriented approaches in future product development. These findings are also valuable in new product development for the Handloom weaving industry in the countries sharing the same industry attributes in the South Asian region.
Islands of shape coexistence from single-particle spectra in covariant density functional theory

Using covariant density functional theory with the DDME2 functional and labeling single-particle energy orbitals by Nilsson quantum numbers, a search for particle-hole (p-h) excitations connected to the appearance of shape coexistence is performed for Z=38 to 84. Islands of shape coexistence are found near the magic numbers Z=82 and Z=50, restricted in regions around the relevant neutron midshells N=104 and N=66 respectively, in accordance to the well accepted p-h interpretation of shape coexistence in these regions, which we call neutron-induced shape coexistence, since the neutrons act as elevators creating holes in the proton orbitals. Similar but smaller islands of shape coexistence are found near N=90 and N=60, restricted in regions around the relevant proton midshells Z=66 and Z=39 respectively, related to p-h excitations across the 3-dimensional isotropic harmonic oscillator (3D-HO) magic numbers N=112 and N=70, which correspond to the beginning of the participation of the opposite parity orbitals 1i13/2 and 1h11/2 respectively to the onset of deformation. We call this case proton-induced shape coexistence, since the protons act as elevators creating holes in the neutron orbitals, thus offering a possible microscopic mechanism for the appearance of shape coexistence in these regions. In the region around N=40, Z=40, an island is located on which both neutron p-h excitations and proton p-h excitations are present.
Impacts of Historical Atmospheric and Oceanic Warming on Heavy Snowfall in December 2020 in Japan

Strong cold air outbreaks caused heavy snowfall over the inland areas of the Sea of Japan coast of Japan in mid‐December 2020. The 48‐hr accumulated snowfall during the term broke a snowfall record at some observational stations of the Japan Meteorological Agency (JMA). We investigated the impacts of atmospheric and oceanic temperature changes due to historical global warming since the pre‐industrial period on this heavy snowfall event. Hindcast and pseudo non‐warming experiments were conducted using the nonhydrostatic model developed by the JMA. The historical climatic differences were obtained from the database for policy decision‐making for future climate change (d4PDF). Our experiments indicated that historical global warming enhanced precipitation over the whole region and enhanced heavy snowfall over the inland areas on the Sea of Japan side. In this event, the contribution of conversion from snowfall to rainfall due to warming was limited over coastal areas. The enhancement of precipitation was mainly caused by oceanic warming, which increased latent heat flux over the Sea of Japan and made the low‐level atmosphere less stable. Historical atmospheric warming suppressed precipitation due to atmospheric stabilization. Our results indicated that the heavy snowfall was caused by the cold air outbreaks under the warm sea surface temperatures in December and enhanced by historical global warming.
M31 GLOBULAR CLUSTER STRUCTURES AND THE PRESENCE OF X-RAY BINARIES

The Andromeda galaxy, M31, has several times the number of globular clusters found in the Milky Way. It contains a correspondingly larger number of low-mass X-ray binaries (LMXBs) associated with globular clusters, and as such can be used to investigate the cluster properties that lead to X-ray binary formation. The best tracer of the spatial structure of M31 globulars is the high-resolution imaging available from the Hubble Space Telescope (HST), and we have used HST data to derive structural parameters for 29 LMXB-hosting M31 globular clusters. These measurements are combined with structural parameters from the literature for a total of 41 (of 50 known) LMXB clusters and a comparison sample of 65 non-LMXB clusters. Structural parameters measured in blue bandpasses are found to be slightly different (smaller core radii and higher concentrations) than those measured in red bandpasses; this difference is enhanced in LMXB clusters and could be related to stellar population differences. Clusters with LMXBs show higher collision rates for their mass compared to clusters without LMXBs, and collision rates estimated at the core radius show larger offsets than rates estimated at the half-light radius. These results are consistent with the dynamical formation scenario for LMXBs. A logistic regression analysis finds that, as expected, the probability of a cluster hosting an LMXB increases with increasing collision rate and proximity to the galaxy center. The same analysis finds that probability of a cluster hosting an LMXB decreases with increasing cluster mass at a fixed collision rate, although we caution that this could be due to sample selection effects. Metallicity is found to be a less important predictor of LMXB probability than collision rate, mass, or distance, even though LMXB clusters have a higher metallicity on average. This may be due to the interaction of location and metallicity: a sample of M31 LMXBs with a greater range in galactocentric distance would likely contain more metal-poor clusters and make it possible to disentangle the two effects.
Componentwise compression‐expansion conditions for systems of nonlinear operator equations and applications

A Krasnoselskii type compression‐expansion fixed point theorem is adapted for the treatment of systems of semi‐linear equations. The compression‐expansion conditions are given componentwise which allows the nonlinear term of a system to have different behaviors both in components and in variables. Applications to boundary value problems for systems of second order differential equations are included.
Galaxy Populations in Massive z = 0.2–0.9 Clusters. I. Analysis of Spectroscopy

We present an analysis of stellar populations in passive galaxies in seven massive X-ray clusters at z = 0.19–0.89. Based on absorption-line strengths measured from our high signal-to-noise spectra, the data support primarily passive evolution of the galaxies. We use the scaling relations between velocity dispersions and the absorption-line strengths to determine representative mean line strengths for the clusters. From the age determinations based on the line strengths (and stellar population models), we find a formation redshift of . Based on line strength measurements from high signal-to-noise composite spectra of our data, we establish the relations between velocity dispersions, ages, metallicities [M/H], and abundance ratios [α/Fe] as a function of redshift. The [M/H]–velocity dispersion and [α/Fe]–velocity dispersion relations are steep and tight. The age–velocity dispersion relation is flat, with zero-point changes reflecting passive evolution. The scatter in all three parameters is within 0.08–0.15 dex at fixed velocity dispersions, indicating a large degree of synchronization in the evolution of the galaxies. We find an indication of cluster-to-cluster differences in metallicities and abundance ratios. However, variations in stellar populations with the cluster environment can only account for a very small fraction of the intrinsic scatter in the scaling relations. Thus, within these very massive clusters, the main driver of the properties of the stellar populations in passive galaxies appears to be the galaxy velocity dispersion.
A new proof for small cancellation conditions of 2-bridge link groups

The second author and M. Sakuma gave a complete characterization of those essential simple loops on a 2-bridge sphere of a 2-bridge link which are null- homotopic in the link complement. In this paper, we give an alternative proof to this result, by giving a simple proof for the small cancellation conditions of the upper presentations of 2-bridge link groups, which holds the key to the proof the result.
Fourth order Weyl gravity

The fourth order Weyl gravity theory of Mannheim and Kazanas is based on replacing the Einstein-Hilbert action with the square of the Weyl tensor, and on modifying the matter action of the standard model of particle physics to make it conformally invariant. This theory has been suggested as a model of both dark matter and dark energy. We argue that the conformal invariance is not a fundamental property of the theory, and instead is an artifact of the choice of variables used in its description. We deduce that in the limit of weak fields and slow motions the theory does not agree with the predictions of general relativity, and is therefore ruled out by Solar System observations.
Genetic Diversity and Population Structure of Normal Maize Germplasm Collected in South Sudan Revealed by SSR Markers

Maize is one of the leading global cereals, and in South Sudan maize cultivation occurs in nearly all of the country’s agro-ecological zones. Despite its widespread cultivation, farmers in South Sudan depend on undeveloped varieties, which results in very low yields in the field. In the current study, 27 simple sequence repeat (SSR) markers were used to investigate genetic diversity and population structures among 37 landrace maize accessions collected from farmers’ fields in South Sudan. In total, 200 alleles were revealed with an average of 7.4 alleles per locus and a range from 3.0 to 13.0 alleles per locus. The observed heterozygosity values ranged from 0.06 to 0.91 with an average of 0.35. High polymorphic information content (PIC) values were identified with a mean of 0.69, which indicates the informativeness of the chosen SSR loci. Genetic structure analysis revealed a moderate genetic differentiation among the maize populations with a fixation index of 0.16, while there was very high genetic differentiation within the groups of populations of three regions with a mean fixation index (F) of 0.37. An unweighted pair group method with an arithmetic mean (UPGMA) dendrogram clustered the 37 maize accessions into three groups with 43% genetic similarity. The clustering pattern of the maize accessions was moderately consistent with their collection area. The findings of this study will provide maize breeders with a better understanding of maize diversification as well as a reserve of genetic resources for use in the selection of advantageous and useful resources for the development of maize varieties in South Sudan.
How important is non-ideal physics in simulations of sub-Eddington accretion on to spinning black holes?

Black holes with accretion rates well below the Eddington rate are expected to be surrounded by low-density, hot, geometrically thick accretion disks. This includes the two black holes being imaged at sub-horizon resolution by the Event Horizon Telescope. In these disks, the mean free path for Coulomb interactions between charged particles is large, and the accreting matter is a nearly collisionless plasma. Despite this, numerical simulations have so far modeled these accretion flows using ideal magnetohydrodynamics. Here, we present the first global, general relativistic, 3D simulations of accretion flows onto a Kerr black hole including the non-ideal effects most likely to affect the dynamics of the disk: the anisotropy between the pressure parallel and perpendicular to the magnetic field, and the heat flux along magnetic field lines. We show that for both standard and magnetically arrested disks, the pressure anisotropy is comparable to the magnetic pressure, while the heat flux remains dynamically unimportant. Despite this large pressure anisotropy, however, the time-averaged structure of the accretion flow is strikingly similar to that found in simulations treating the plasma as an ideal fluid. We argue that these similarities are largely due to the interchangeability of the viscous and magnetic shear stresses as long as the magnetic pressure is small compared to the gas pressure, and to the sub-dominant role of pressure/viscous effects in magnetically arrested disks. We conclude by highlighting outstanding questions in modeling the dynamics of low collisionality accretion flows.
REDSHIFT EVOLUTION IN BLACK HOLE–BULGE RELATIONS: TESTING C iv-BASED BLACK HOLE MASSES

We re-examine claims for redshift evolution in black hole–bulge scaling relations based on lensed quasars. In particular, we refine the black hole (BH) mass estimates using measurements of Balmer lines from near-infrared spectroscopy obtained with Triplespec at Apache Point Observatory. In support of previous work, we find a large scatter between Balmer and UV line widths, both Mg iiλλ2796, 2803 and C ivλλ1548, 1550. There is tentative evidence that C iii]λ1909, despite being a blend of multiple transitions, may correlate well with Mg ii, although a larger sample is needed for a real calibration. Most importantly, we find no systematic changes in the estimated BH masses for the lensed sample based on Balmer lines, providing additional support to the interpretation that black holes were overly massive compared to their host galaxies at high redshift.
Can the hummingbird sign contribute to the diagnosis of idiopathic normal pressure hydrocephalus?

BACKGROUND We read with great interest the article by Atalay et al. in which they illustrate the frequent presence of hummingbird signs in their patient group with idiopathic normal pressure hydrocephalus (iNPH) [1]. The results are substantially interesting; however, we believe that some points may be further deliberated for a better understanding of this crucial study. DISCUSSION The authors declare that there are no commercial, financial, and other relationships in any way related to the subject of this article that might create any potential conflict of interest.
Sondheimer oscillation as a signature of surface Dirac fermions

Topological states of matter challenge the paradigm of symmetry breaking, characterized by gapless boundary modes and protected by the topological property of the ground state. Recently, angle-resolved photoemission spectroscopy (ARPES) has revealed that semiconductors of Bi$_{2}$Se$_{3}$ and Bi$_{2}$Te$_{3}$ belong to such a class of materials. Here, we present undisputable evidence for the existence of gapless surface Dirac fermions from transport in Bi$_{2}$Te$_{3}$. We observe Sondheimer oscillation in magnetoresistance (MR). This oscillation originates from the quantization of motion due to the confinement of electrons within the surface layer. Based on Sondheimer's transport theory, we determine the thickness of the surface state from the oscillation data. In addition, we uncover the topological nature of the surface state, fitting consistently both the non-oscillatory part of MR and the Hall resistance. The side-jump contribution turns out to dominate around 1 T in Hall resistance while the Berry-curvature effect dominates in 3 T $\sim$ 4 T.
Exact second-order structure-function relationships

Equations that follow from the Navier–Stokes equation and incompressibility but with no other approximations are ‘exact’. Exact equations relating second- and third- order structure functions are studied, as is an exact incompressibility condition on the second-order velocity structure function. Opportunities for investigations using these equations are discussed. Precisely defined averaging operations are required to obtain exact averaged equations. Ensemble, temporal and spatial averages are all considered because they produce different statistical equations and because they apply to theoretical purposes, experiment and numerical simulation of turbulence. Particularly simple exact equations are obtained for the following cases: (i) the trace of the structure functions, (ii) DNS that has periodic boundary conditions, and (iii) an average over a sphere in r-space. Case (iii) introduces the average over orientations of r into the structure-function equations. The energy dissipation rate ε appears in the exact trace equation without averaging, whereas in previous formulations ε appears after averaging and use of local isotropy. The trace mitigates the effect of anisotropy in the equations, thereby revealing that the trace of the third-order structure function is expected to be superior for quantifying asymptotic scaling laws. The orientation average has the same property.
Gravitationally lensed quasars in Gaia: I. Resolving small-separation lenses

Gaia's exceptional resolution (FWHM $\sim$ 0.1$^{\prime\prime}$) allows identification and cataloguing of the multiple images of gravitationally lensed quasars. We investigate a sample of 49 known lensed quasars in the SDSS footprint, with image separations less than 2$^{\prime\prime}$, and find that 8 are detected with multiple components in the first Gaia data release. In the case of the 41 single Gaia detections, we generally are able to distinguish these lensed quasars from single quasars when comparing Gaia flux and position measurements to those of Pan-STARRS and SDSS. This is because the multiple images of these lensed quasars are typically blended in ground-based imaging and therefore the total flux and a flux-weighted centroid are measured, which can differ significantly from the fluxes and centroids of the individual components detected by Gaia. We compare the fluxes through an empirical fit of Pan-STARRS griz photometry to the wide optical Gaia bandpass values using a sample of isolated quasars. The positional offsets are calculated from a recalibrated astrometric SDSS catalogue. Applying flux and centroid difference criteria to spectroscopically confirmed quasars, we discover 4 new sub-arcsecond-separation lensed quasar candidates which have two distinct components of similar colour in archival CFHT or HSC data. Our method based on single Gaia detections can be used to identify the $\sim$ 1400 lensed quasars with image separation above 0.5$^{\prime\prime}$, expected to have only one image bright enough to be detected by Gaia.
Scattering-Matrix Analysis of Linear Periodic Arrays of Short Electric Dipoles

Abstract : The scattering-matrix analysis of linear periodic arrays of electric dipoles given in this report was suggested by the corresponding analysis performed by Yaghjian for linear periodic arrays of electro-acoustic monopole transducers. The extension to electromagnetic antennas reported here requires the use of the more complicated vector spherical wave functions instead of scalar spherical wave functions. However, no new concepts are needed for our treatment. A general vector spherical-wave source scattering-matrix description of electromagnetic antennas is formulated, and reciprocity and power conservation are used to derive relations between the antenna reflection, receiving and scattering coefficients that constitute the scattering matrix. When the antennas are electrically small dipoles only two vector spherical wave modes, one incoming and one outgoing, are required to describe the antennas. The scattering matrix formulation is applied to analyze infinite and finite linear periodic arrays of short electric dipoles perpendicular to the array axis. For an infinite periodic linear array of short dipoles, the scattering-matrix analysis leads to a simple implicit transcendental equation for the propagation constant beta of the traveling wave in terms of the normalized separation distance kd and the phase We of the effective scattering coefficient of the array elements. Interestingly, for certain values of We and kd there can be two different values of beta. The normalized separation distance and phase of the effective scattering coefficient also prove to be the only critical variables in the N x N matrix equation for the N radiation coefficients that is derived for a finite linear array of N electric dipoles. Resonances in the curves of total power radiated versus kd for a finite array excited with one feed element demonstrate the existence of the traveling waves predicted for the corresponding infinite array.
The role of cold gas and environment on the stellar mass-metallicity relation of nearby galaxies

We investigate the relationship between stellar mass, metallicity and gas content for a magnitude- and volume-limited sample of 260 nearby late-type galaxies in different environments, from isolated galaxies to Virgo cluster members. We derive oxygen abundance estimates using new integrated, drift-scan optical spectroscopy and the base metallicity calibrations of Kewley & Ellison (2008, ApJ, 681, 1183). Combining these measurements with ultraviolet to near-infrared photometry and Hi 21 cm line observations, we examine the relations between stellar mass, metallicity, gas mass fraction and star formation rate. We find that, at fixed stellar mass, galaxies with lower gas fractions typically also possess higher oxygen abundances. We also observe a relationship between gas fraction and metal content, whereby gas-poor galaxies are typically more metal-rich, and demonstrate that the removal of gas from the outskirts of spirals may increase the observed average metallicity by ∼0.1 dex. Although some cluster galaxies are gas-deficient objects, statistically the stellar-mass metallicity relation is nearly invariant to the environment, in agreement with recent studies. These results indicate that internal evolutionary processes, rather than environmental effects, play a key role in shaping the stellar mass-metallicity relation. In addition, we present metallicity estimates based on observations of 478 nearby galaxies.
Detection of He II Reionization in the Sloan Digital Sky Survey Quasar Sample

The expansion of the universe leads to a rapid drop in the hydrogen Lyα effective optical depth of the intergalactic medium (IGM), eff ∝ (1 + z)3.8, between redshifts 4 and 3. Measurements of the temperature evolution of the IGM and of the He II opacity both suggest that He II reionizes in this redshift range. We use hydrodynamical simulations to show that the observed temperature increase associated with He II reionization leads to a relatively sudden decrease in eff around the reionization epoch of ≈10%. We find clear evidence for such a feature in the evolution of eff determined from a sample of ~1100 quasars obtained from the Sloan Digital Sky Survey. He II reionization starts at redshift ≈3.4 and lasts for Δz ≈ 0.4. The increase in the IGM temperature also explains the widths of hydrogen absorption lines as measured in high-resolution spectra.