Miracle-dz/UniFAR-FTUs huggingface dataset:
NGC 7538 IRS. 1. INTERACTION OF A POLARIZED DUST SPIRAL AND A MOLECULAR OUTFLOW

We present dust polarization and CO molecular line images of NGC 7538 IRS 1. We combined data from the Submillimeter Array, the Combined Array for Research in Millimeter-wave Astronomy, and the James Clerk Maxwell Telescope to make images with ∼2. ″5 resolution at 230 and 345 GHz. The images show a remarkable spiral pattern in both the dust polarization and molecular outflow. These data dramatically illustrate the interplay between a high infall rate onto IRS 1 and a powerful outflow disrupting the dense, clumpy medium surrounding the star. The images of the dust polarization and the CO outflow presented here provide observational evidence for the exchange of energy and angular momentum between the infall and the outflow. The spiral dust pattern, which rotates through over 180° from IRS 1, may be a clumpy filament wound up by conservation of angular momentum in the infalling material. The redshifted CO emission ridge traces the dust spiral closely through the MM dust cores, several of which may contain protostars. We propose that the CO maps the boundary layer where the outflow is ablating gas from the dense gas in the spiral.
A generalization of the functional calculus of observables and notion of joint measurability to the case of non-commuting observables

For any pair of bounded observables A and B with pure point spectra, we construct an associated ‘joint observable’ which gives rise to a notion of a joint (projective) measurement of A and B, and which conforms to the intuition that one can measure non-commuting observables simultaneously, provided one is willing to give up arbitrary precision. As an application, we show how our notion of a joint observable naturally allows for a construction of a ‘functional calculus,’ so that for any pair of observables A and B as above, and any (Borel measurable) function f : R 2 → R ? > , a new ‘generalized observable’ f ( A , B ) ? > is obtained. Moreover, we show that this new functional calculus has some rather remarkable properties.
The Role of Corporate Governance in Achieving SDGs among Malaysian Companies

While the Sustainable Development Goals (SDGs) agenda is applicable to the member states of the UN, many other players are also involved, such as corporations. The primary and economic value chain activities and aims of major companies mean they will ultimately have a crucial and explicit role to play in enabling the SDGs to be attained. In Malaysia, there have been few studies on firms' engagement in reaching the SDGs. Therefore, the current study aimed to examine the roles played by corporations in enabling SDGs to be attained. A specific analysis was conducted to determine if a company’s participation in the SDGs can be influenced by first-rate corporate governance. The data was collected using content analysis of 87 corporate annual reports of public listed companies from Malaysia. The boards’ independence, size, meeting frequency, and gender diversity were the corporate governance practices examined. An annual report may include details of the company’s role in the SDGs as a proxy for the corporate’s SDG involvement. The findings shed light on the nature of business involvement in the SDGs. The SGD with the most frequent reporting was Goal 8 - Decent work and economic growth, while the SDG with the most frequent reporting was Goal 2 - Zero Hunger. These results indicate that a company’s SDG participation has a positive relationship with certain governance practices of corporations, especially the board meeting frequency. Moreover, these results may serve to emphasise to regulators and policymakers that all corporations require effectual corporate governance so that the challenges facing the world and its population every day can be addressed, leading to an improved and more sustainable future for everyone. Keywords Sustainable Development Goals (SDGs), corporate governance, Malaysia, companies, content analysis
C12 - C13 Diamond Quantum Computer with Longitudinal rf-Magnetic Field

It is shown that in the diamond $C^{12}$ structure with a linear chain of $C^{13}$ atoms which is inside a transverse static field, having a gradient along the linear chain and an rf-magnetic field in a plane with a component in the direction of the static field, one qubit rotation, the Controlled-Not (CNOT), the Controlled-Controlled-NoT (CCNOT) quantum gates, and teleportation algorithm.
A self-similar solution for thermal disc winds

This work has been partially supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC- 2013-ADG. RDA acknowledges support from STFC through an Advanced Fellowship (ST/G00711X/1), and from the Leverhulme Trust through a Philip Leverhulme Prize. Astrophysical research at the University of Leicester is supported by an STFC Consolidated Grant (ST/K001000/1). This research used the ALICE High Performance Computing Facility at the University of Leicester. Some resources on ALICE form part of the DiRAC Facility jointly funded by STFC and the Large Facilities Capital Fund of BIS. This work also used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (http://www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the UK National E-Infrastructure.
BAYESIAN TECHNIQUES FOR COMPARING TIME-DEPENDENT GRMHD SIMULATIONS TO VARIABLE EVENT HORIZON TELESCOPE OBSERVATIONS

The Event Horizon Telescope (EHT) is a millimeter-wavelength, very-long-baseline interferometry (VLBI) experiment that is capable of observing black holes with horizon-scale resolution. Early observations have revealed variable horizon-scale emission in the Galactic Center black hole, Sagittarius A* (Sgr A*). Comparing such observations to time-dependent general relativistic magnetohydrodynamic (GRMHD) simulations requires statistical tools that explicitly consider the variability in both the data and the models. We develop here a Bayesian method to compare time-resolved simulation images to variable VLBI data, in order to infer model parameters and perform model comparisons. We use mock EHT data based on GRMHD simulations to explore the robustness of this Bayesian method and contrast it to approaches that do not consider the effects of variability. We find that time-independent models lead to offset values of the inferred parameters with artificially reduced uncertainties. Moreover, neglecting the variability in the data and the models often leads to erroneous model selections. We finally apply our method to the early EHT data on Sgr A*.
Using Likelihood for Combined Data Set Analysis

The joint likelihood is a simple extension of the standard likelihood formalism that enables the estimation of common parameters across disjoint datasets. Joining the likelihood, rather than the data itself, means nuisance parameters can be dealt with independently. Application of this technique, particularly to Fermi-LAT dwarf spheroidal analyses, has already been met with great success. We present a description of the method's general implementation along with a toy Monte-Carlo study of its properties and limitations.
A new numerical scheme for constrained total variation flows and its convergence

In this paper, we propose a new numerical scheme for a spatially discrete model of constrained total variation flows, which are total variation flows whose values are constrained in a Riemannian manifold. The difficulty of this problem is that the underlying function space is not convex and it is hard to calculate the minimizer of the functional with the manifold constraint. We overcome this difficulty by "localization technique" using the exponential map and prove the finite-time error estimate in general situation. Finally, we show a few numerical results for the cases that the target manifolds are $S^2$ and $SO(3)$.
Combining spectroscopic and photometric surveys using angular cross-correlations – II. Parameter constraints from different physical effects

Future spectroscopic and photometric surveys will measure accurate positions and shapes of an increasing number of galaxies. In the previous paper of this series we studied the effects of Redshift Space Distortions (RSD), baryon acoustic oscillations (BAO) and Weak gravitational Lensing (WL) using angular cross-correlation. Here, we provide a new forecast that explores the contribution of including different observables, physical effects (galaxy bias, WL, RSD, BAO) and approximations (non-linearities, Limber approximation, covariance between probes). The radial information is included by using the cross-correlation of separate narrow redshift bins. For the auto correlation the separation of galaxy pairs is mostly transverse, while the cross-correlations also includes a radial component. We study how this information adds to our figure of merit (FoM), which includes the dark energy equation of state $w(z)$ and the growth history, parameterized by $\gamma$. We show that the Limber approximation and galaxy bias are the most critical ingredients to the modelling of correlations. Adding WL increases our FoM by 4.8, RSD by 2.1 and BAO by 1.3. We also explore how overlapping surveys perform under the different assumption and for different figures of merit. Our qualitative conclusions depend on the survey choices and scales included, but we find some clear tendencies that highlight the importance of combining different probes and can be used to guide and optimise survey strategies.
Holography of charged black holes with RF2 corrections

We investigate several holographic properties of charged black holes with RF2 corrections, which originate from Kaluza-Klein reductions of five-dimensional Gauss-Bonnet gravity. We obtain the perturbative solution and discuss its thermodynamics. The DC conductivity is calculated via the effective action approach, and the corrections to the DC conductivity are also evaluated. Moreover, we calculate the shear viscosity eta and thermal conductivity kappa(T), as well as two interesting ratios eta/s and kappa(T)mu(2)/(eta T). We find that both bounds conjectured in the literatures can be violated in the presence of the higher- order corrections RF2.
ATLAS 1.4 GHz Data Release 2 – I. Observations of the CDF-S and ELAIS-S1 fields and methods for constructing differential number counts

This is the first of two papers describing the second data release (DR2) of the Australia Telescope Large Area Survey (ATLAS) at 1.4 GHz, which comprises deep wide-field observations in total intensity, linear polarization, and circular polarization over the Chandra Deep Field-South and European Large Area Infrared Space Observatory Survey-South 1 regions. DR2 improves upon the first data release by maintaining consistent data reductions across the two regions, including polarization analysis, and including differential number counts in total intensity and linear polarization. Typical DR2 sensitivities across the mosaicked multi-pointing images are 30 uJy/beam at approximately 12"x6" resolution over a combined area of 6.4 square degrees. In this paper we present detailed descriptions of our data reduction and analysis procedures, including corrections for instrumental effects such as positional variations in image sensitivity, bandwidth smearing with a non-circular beam, and polarization leakage, and application of the BLOBCAT source extractor. We present the DR2 images and catalogues of components (discrete regions of radio emission) and sources (groups of physically associated radio components). We describe new analytic methods to account for resolution bias and Eddington bias when constructing differential number counts of radio components.
3D Equivariant Graph Implicit Functions: Appendices

We review the definition of the equivariance of the implicit function model in Section 3. In Eq. (3), we show that equivariance is satisfied if the implicit function is locally invariant to any Tg applied jointly to the observation X and the query p, for any X and p. Invariance is a special case of equivariance, where the transformation T ∗ g on the output domain is the identity function, i.e., the output is invariant regardless of the input transformation Tg . Here we clarify the use of layer equivariance in creating the equivariant implicit function model. As in Eq. (4), the graph implicit function model Fgraph is composed of the graph latent feature extractor Φgraph and the implicit decoder Ψ , where Φgraph can be further decomposed to the point encoder φ and the graph local latent aggregator ψ. We integrate the equivariant layers in φ and ψ that process the input point set X and the queries p. As shown by the literature, the composition of two equivariant functions is also an equivariant function [46]. Thus, the graph local feature extractor Φgraph that stacks sequential equivariant graph layers in φ and ψ is equivariant. Note that all the operations other than the graph convolutions involved in φ and ψ, such as the k-NN graph extration and the farthest-point-sampling for the multi-scale feature, are equivariant to the similarity transformations as well. At the end of all the equivariant graph layers in φ and ψ, we apply the invariance function Ω to obtain the locally invariant latent feature. The implicit decoder Ψ , which processes the invariant local latent feature and predicts the occupancy probability, is simply a standard ReLU-MLP as the non-equivariant implicit models. We do not include the query coordinate input p in the implicit decoder Ψ in order to satisfy translation equivariance, while the local latent feature already contains the position information. Since the local latent feature is locally invariant, the output is locally invariant as well, which satisfies Eq. (3). Thus far, we have shown how the equivariant graph layers help to build the equivariant implicit function model.
Clustering of gyrotactic microorganisms in turbulent flows

We study the spatial distribution of gyrotactic microorganisms transported by a three-dimensional turbulent flow generated by direct numerical simulations. We find that gyrotaxis combines with turbulent fluctuations to produce small scales (multi-)fractal clustering. We explain this result by showing that gyrotactic swimming cells behave like tracers in a compressible flow. The effective compressibility is derived in the limits of fluid acceleration much larger and smaller than the gravity.
Stellar Magnetic Dynamos and Activity Cycles

Abstract Using a new uniform sample of 824 solar and late-type stars with measured X-ray luminosities and rotation periods we have studied the relationship between rotation and stellar activity that is believed to be a probe of the underlying stellar dynamo. Using an unbiased subset of the sample we calculate the power law slope of the unsaturated regime of the activity – rotation relationship as LX / Lbol ∝ Roβ, where β = − 2.70 ± 0.13. This is inconsistent with the canonical β = − 2 slope to a confidence of 5σ and argues for an interface-type dynamo. We map out three regimes of coronal emission as a function of stellar mass and age, using the empirical saturation threshold and theoretical super-saturation thresholds. We find that the empirical saturation timescale is well correlated with the time at which stars transition from the rapidly rotating convective sequence to the slowly rotating interface sequence in stellar spin-down models. This may be hinting at fundamental changes in the underlying stellar dynamo or internal structure. We also present the first discovery of an X-ray unsaturated, fully convective M star, which may be hinting at an underlying rotation - activity relationship in fully convective stars hitherto not observed. Finally we present early results from a blind search for stellar X-ray cycles that can place valuable constraints on the underlying ubiquity of solar-like activity cycles.
A comparative study on nonlocal diffusion operators related to the fractional Laplacian

In this paper, we study four nonlocal diffusion operators, including the fractional Laplacian, spectral fractional Laplacian, regional fractional Laplacian, and peridynamic operator. These operators represent the infinitesimal generators of different stochastic processes, and especially their differences on a bounded domain are significant. We provide extensive numerical experiments to understand and compare their differences. We find that these four operators collapse to the classical Laplace operator as \alpha \to 2. The eigenvalues and eigenfunctions of these four operators are different, and the k-th (for k \in N) eigenvalue of the spectral fractional Laplacian is always larger than those of the fractional Laplacian and regional fractional Laplacian. For any \alpha \in (0, 2), the peridynamic operator can provide a good approximation to the fractional Laplacian, if the horizon size \delta is sufficiently large. We find that the solution of the peridynamic model converges to that of the fractional Laplacian model at a rate of O(\delta^{-\alpha}). In contrast, although the regional fractional Laplacian can be used to approximate the fractional Laplacian as \alpha \to 2, it generally provides inconsistent result from that of the fractional Laplacian if \alpha \ll 2. Moreover, some conjectures are made from our numerical results, which could contribute to the mathematics analysis on these operators.
Metadata-driven Data Migration from Object-relational Database to NoSQL Document-oriented Database

The object-relational databases (ORDB) are powerful for managing complex data, but they suffer from problems of scalability and managing large-scale data. Therefore, the importance of the migration of ORDB to NoSQL derives from the fact that the large volume of data can be handled in the best way with high scalability and availability. This paper reports our metadata-driven approach for the migration of the ORDB to document-oriented NoSQL database. Our data migration approach involves three major stages: a preprocessing stage, to extract the data and the schema's components, a processing stage, to provide the data transformation, and a post-processing stage, to store the migrated data as BSON documents. The approach maintains the benefits of Oracle ORDB in NoSQL MongoDB by supporting integrity constraint checking. To validate our approach, we developed OR2DOD (Object Relational to Document-Oriented Databases) system, and the experimental results confirm the effectiveness of our proposal.
The RMS survey: near-IR spectroscopy of massive young stellar objects

Near-infrared H- and K-band spectra are presented for 247 objects, selected from the Red MSX Source (RMS) survey as potential young stellar objects (YSOs). 195 (∼80 per cent) of the targets are YSOs, of which 131 are massive YSOs (L BOL > 5×10 3 L ⊙ , M > 8 M ⊙ ). This is the largest spectroscopic study of massive YSOs to date, providing a valuable resource for the study of massive star formation. In this paper, we present our exploratory analysis of the data. The YSOs observed have a wide range of embeddedness (2.7 < A V < 114), demonstrating that this study covers minimally obscured objects right through to very red, dusty sources. Almost all YSOs show some evidence for emission lines, though there is a wide variety of observed properties. The most commonly detected lines are Brγ, H 2 , fluorescent Fe ii, CO bandhead, [Fe ii] and He i 2-1 1 S- 1 P, in order of frequency of occurrence. In total, ∼40 per cent of the YSOs display either fluorescent Fe ii 1.6878 μm or CO bandhead emission (or both), indicative of a circumstellar disc; however, no correlation of the strength of these lines with bolometric luminosity was found. We also find that ∼60 per cent of the sources exhibit [Fe ii] or H 2 emission, indicating the presence of an outflow. Three quarters of all sources have Brγ in emission. A good correlation with bolometric luminosity was observed for both the Brγ and H 2 emission line strengths, covering 1 < L BOL < 3.5 × 10 5 L ⊙ . This suggests that the emission mechanism for these lines is the same for low-, intermediate- and high-mass YSOs, i.e. high-mass YSOs appear to resemble scaled-up versions of low-mass YSOs. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
HEALTHCARE SECTOR AND ANTI-COMPETITIVE PRACTICES IN INDIA

Health is the basic human right and an important indicator of the nations’ commitment towards the health of its citizen and hence every country strives to increase the health standard and provide basic medical facility to all. This right to health is an outcome of various legal sanctions, both internationally and of countries specific. The right to health is enshrined as a basic human right internationally. The right to health is an inclusive right, extending not only to timely and appropriate health care, but also to the underlying determinants of health as per (Report of Committee on Economic, Social and Cultural Rights). Though the Constitution of India does not expressly recognize the Right to Health as a fundamental right under Part III of the Constitution (Fundamental Rights), it is considered as an inseparable part of the Right to Life. Article 23. As a result, the child labour and human trafficking are prohibited in India. This article aims to analyse the impact of fast-changing lifestyle, habits, stress, COVID-19 pandemic and other factors on public health in India. It is more sensitized since last two years.
Visser's massive graviton bimetric theory revisited

A massive gravity theory was proposed by Visser in the late 1990s. This theory, based on a background metric b{sub {alpha}{beta}} and on an usual dynamical metric g{sub {alpha}{beta}} has the advantage of being free of ghosts as well as discontinuities present in other massive theories proposed in the past. In the present investigation, the equations of Visser's theory are revisited with particular care on the related conservation laws. It will be shown that a multiplicative factor is missing in the graviton tensor originally derived by Visser, which has no incidence on the weak field approach but becomes important in the strong field regime when, for instance, cosmological applications are considered. In this case, contrary to some previous claims found in the literature, we conclude that a nonstatic background metric is required in order to obtain a solution able to mimic the {Lambda}CDM cosmology.
ON VARIATIONS OF THE BRIGHTNESS OF TYPE Ia SUPERNOVAE WITH THE AGE OF THE HOST STELLAR POPULATION

Recent observational studies of type Ia supernovae (SNeIa) suggest correlations between the peak brightness of an event and the age of the progenitor stellar population. This trend likely follows from properties of the progenitor white dwarf (WD), such as central density, that follow from properties of the host stellar population. We present a statistically well-controlled, systematic study utilizing a suite of multi-dimensional SNeIa simulations investigating the influence of central density of the progenitor WD on the production of Fe-group material, particularly radioactive 56Ni, which powers the light curve. We find that on average, as the progenitor's central density increases, production of Fe-group material does not change but production of 56Ni decreases. We attribute this result to a higher rate of neutronization at higher density. The central density of the progenitor is determined by the mass of the WD and the cooling time prior to the onset of mass transfer from the companion, as well as the subsequent accretion heating and neutrino losses. The dependence of this density on cooling time, combined with the result of our central density study, offers an explanation for the observed age–luminosity correlation: a longer cooling time raises the central density at ignition thereby producing less 56Ni and thus a dimmer event. While our ensemble of results demonstrates a significant trend, we find considerable variation between realizations, indicating the necessity for averaging over an ensemble of simulations to demonstrate a statistically significant result.