Miracle-dz/UniFAR-FTUs huggingface dataset:
Towards a unified framework for approximate quantum error correction

Recent work on approximate quantum error correction (QEC) has opened up the possibility of constructing subspace codes that protect information with high fidelity in scenarios where perfect error correction is impossible. Motivated by this, we investigate the problem of approximate subsystem codes. Subsystem codes extend the standard formalism of subspace QEC to codes in which only a subsystem within a subspace of states is used to store information in a noise-resilient fashion. Here, we demonstrate easily checkable sufficient conditions for the existence of approximate subsystem codes. Furthermore, for certain classes of subsystem codes and noise processes, we prove the efficacy of the transpose channel as a simple-to-construct recovery map that works nearly as well as the optimal recovery channel. This work generalizes our earlier approach [H.K. Ng and P. Mandayam, Phys. Rev. A 81 062342 (2010)] of using the transpose channel for approximate correction of subspace codes to the case of subsystem codes, and brings us closer to a unifying framework for approximate QEC.
Association of Parental Screen Addiction with Young Children’s Screen Addiction: A Chain-Mediating Model

Preschool children are immersed in screen media, yet little study has been conducted on screen addiction among them. This study aimed to investigate the relationship between parental screen addiction and young children’s screen addiction and to verify factors that mediate this relationship. A total of 477 parents of kindergarteners (3–6 years old) were recruited via six kindergartens in Henan province, China. They completed the Problematic Media Use Measure Short Form of Children, the Self-Rating Anxiety Scale, the Child–Parent Relationship Scale, and the Parental Screen Addiction Scale. The results showed that the relationships between each pair of parental screen addiction, parental anxiety, and children’s screen addiction were significantly positive, but the parent–child relationship was negatively correlated with the other variables. Parental screen addiction can directly and indirectly affect children’s screen addiction through parental anxiety and the parent–child relationship. The findings contribute to the development of family protection mechanisms against screen addiction in children.
Accelerate the Mobilization of African and International Scientific Expertise to Boost Interdisciplinary Research for the Success of the Sahelian Great Green Wall by 2030

The Sahelian Great Green Wall (SGGW) is an influential project to combat desertification and promote sustainable land management on a large scale, involving 11 countries in the Sahel region of Africa. The UNCCD’s 2020 progress report showed a mixed picture concerning the meeting of the initial targets. At the One Planet Summit in 2021, announcements were made to consolidate the implementation of the SGGW, most notably with the creation of the Great Green Wall Accelerator. In this context, our paper sets out to review the scientific work conducted with regard to the SGGW. We have thus carried out a bibliometric analysis of the literature on SGGW. Although the initiative involves 11 countries and covers a large spectrum of scientific disciplines, our results show the predominance of ecological studies in the SGGW literature and a concentration of studies in certain geographies of interest, such as northern Senegal. Moreover, based on a secondary analysis of publications on land restoration and sustainable ecosystem management in Sahelian countries, we show that the literature relevant to SGGW topics is richer and fills in the information gaps we have identified at thematic and geographical levels. By showing that SGGW studies are overly focused on certain topics and geographical areas, our paper argues for a better interdisciplinary mobilization of researchers working on GGW-related topics. The scientific and operational success of the project depends on stronger networking between the different research teams and themes, both in Africa and internationally.
Analytical approach to excitonic properties of MoS2

We present an analytical investigation of the optical absorption spectrum of monolayer molybdenumdisulfide. Based on the density matrix formalism, our approach gives insights into the microscopic origin of excitonic transitions, their relative oscillator strength, and binding energy. We show analytical expressions for the carrier-light coupling element, which contains the optical selection rules and well describes the valleyselective polarization in MoS2. In agreement with experimental results, we find the formation of strongly bound electron-hole pairs due to the efficient Coulomb interaction. The absorption spectrum of MoS2 on a silicon substrate features two pronounced peaks at 1.91 eV and 2.05 eV corresponding to the A and B exciton, which are characterized by binding energies of 420 meV and 440 meV, respectively. Our calculations reveal their relative oscillator strength and predict the appearance of further low-intensity excitonic transitions at higher energies. The presented approach is applicable to other transition metal dichalcogenides and can be extended to investigations of trion and biexcitonic effects.
Time evolution of superradiant instabilities for charged black holes in a cavity

Departamento de Fisica da Universidade de Aveiro and I3N, Campus de Santiago,3810-183 Aveiro, Portugal(Received 8 January 2014; published 6 March 2014)Frequency domain studies have recently demonstrated that charged scalar fields exhibit fast growingsuperradiant instabilities when interacting with charged black holes in a cavity. Here, we present a timedomain analysis of the long time evolution of test charged scalar field configurations on the Reissner-Nordstrombackground,withorwithoutamirrorlikeboundarycondition.InitialdataaretakentobeeitheraGaussian wave packet or a regularized (near the horizon) quasibound state. Then, Fourier transforming thedata obtained in the evolution confirms the results obtained in the frequency domain analysis, in particularfor the fast growing modes. We show that spherically symmetric (l ¼ 0) modes have even faster growthratesthanthel ¼ 1modesfora“small”fieldcharge.Thus,ourstudyconfirmsthatthissetupisparticularlypromising for considering the nonlinear development of the superradiant instability, since the fast growthmakes the signal overcome the numerical error that dominates for small growth rates, and the analysis maybe completely done in spherical symmetry.
Clump mass function at an early stage of molecular cloud evolution – II. Galactic cloud complexes

The statistical approach for derivation of the clump mass function (ClMF) developed by Donkov, Veltchev & Klessen is put to observational test through comparison with mass distributions of clumps from molecular emission and dust continuum maps of Galactic cloud complexes, obtained by various authors. The results indicate gravitational boundedness of the dominant clump population, with or without taking into account the contribution of their thermal and magnetic energy. The ClMF can be presented by combination of two power-law functions separated by a characteristic mass from about ten to hundreds solar masses. The slope of the intermediate-mass ClMF is shallow and nearly constant (-0.25 \gtrsim \Gamma_{IM} \gtrsim -0.55) while the high-mass part is fitted by models that imply gravitationally unstable clumps and exhibit slopes in a broader range (-0.9 \gtrsim \Gamma_{IM} \gtrsim -1.6), centered at the value of the stellar initial mass function (\Gamma_{HM} \gtreqless -1.3).
The mid-infrared polarization of the Herbig Ae star WL 16: An interstellar origin?

We present high-resolution (0".4) mid-infrared (mid-IR) polarimetric images and spectra of WL 16, a Herbig Ae star at a distance of 125 pc. WL 16 is surrounded by a protoplanetary disk of $\sim$ 900 AU in diameter, making it one of the most extended Herbig Ae/Be disks as seen in the mid-IR. The star is behind, or embedded in, the $\rho$ Ophiuchus molecular cloud, and obscured by 28 magnitudes of extinction at optical wavelengths by the foreground cloud. Mid-IR polarization of WL 16, mainly arises from aligned elongated dust grains present along the line of sight, suggesting a uniform morphology of polarization vectors with an orientation of 33\degr (East from North) and a polarization fraction of $\sim$ 2.0\%. This orientation is consistent with previous polarimetric surveys in the optical and near-IR bands to probe large-scale magnetic fields in the Ophiuchus star formation region, indicating that the observed mid-IR polarization toward WL 16 is produced by the dichroic absorption of magnetically aligned foreground dust grains by a uniform magnetic field. Using polarizations of WL 16 and Elias 29, a nearby polarization standard star, we constrain the polarization efficiency, \textit{$p_{10.3}/A_{10.3}$}, for the dust grains in the $\rho$ Ophiuchus molecular cloud to be $\sim$ 1.0\% mag$^{-1}$. WL 16 has polycyclic aromatic hydrocarbon (PAH) emission features detected at 8.6, 11.2, 12.0, and 12.7 $\mu$m by our spectroscopic data, and we find an anti-correlation between the PAH surface brightness and the PAH ionization fraction between the NW and SW sides of the disk.
The bifurcated age–metallicity relation of Milky Way globular clusters and its implications for the accretion history of the galaxy

We use recently derived ages for 61 Milky Way (MW) globular clusters (GCs) to show that their age-metallicity relation (AMR) can be divided into two distinct, parallel sequences at [Fe/H] $\ga -1.8$. Approximately one-third of the clusters form an offset sequence that spans the full range in age ($\sim 10.5$--13 Gyr), but is more metal rich at a given age by $\sim 0.6$ dex in [Fe/H]. All but one of the clusters in the offset sequence show orbital properties that are consistent with membership in the MW disk. They are not simply the most metal-rich GCs, which have long been known to have disk-like kinematics, but they are the most metal-rich clusters at all ages. The slope of the mass-metallicity relation (MMR) for galaxies implies that the offset in metallicity of the two branches of the AMR corresponds to a mass decrement of 2 dex, suggesting host galaxy masses of $M_{*} \sim 10^{7-8} \msol$ for GCs that belong to the more metal-poor AMR. We suggest that the metal-rich branch of the AMR consists of clusters that formed in-situ in the disk, while the metal-poor GCs were formed in relatively low-mass (dwarf) galaxies and later accreted by the MW. The observed AMR of MW disk stars, and of the LMC, SMC and WLM dwarf galaxies are shown to be consistent with this interpretation, and the relative distribution of implied progenitor masses for the halo GC clusters is in excellent agreement with the MW subhalo mass function predicted by simulations. A notable implication of the bifurcated AMR, is that the identical mean ages and spread in ages, for the metal rich and metal poor GCs are difficult to reconcile with an in-situ formation for the latter population.
GALAXY INTERACTIONS IN COMPACT GROUPS. I. THE GALACTIC WINDS OF HCG16

Using the WiFeS integral field spectrograph, we have undertaken a series of observations of star-forming galaxies in compact groups. In this first paper dedicated to the project, we present the analysis of the spiral galaxy NGC 838, a member of the Hickson Compact Group 16, and of its galactic wind. Our observations reveal that the wind forms an asymmetric, bipolar, rotating structure, powered by a nuclear starburst. Emission line ratio diagnostics indicate that photoionization is the dominant excitation mechanism at the base of the wind. Mixing from slow shocks (up to 20%) increases further out along the outflow axis. The asymmetry of the wind is most likely caused by one of the two lobes of the wind bubble bursting out of its H i envelope, as indicated by line ratios and radial velocity maps. The characteristics of this galactic wind suggest that it is caught early (a few Myr) in the wind evolution sequence. The wind is also quite different from the galactic wind in the partner galaxy NGC 839 which contains a symmetric, shock-excited wind. Assuming that both galaxies have similar interaction histories, the two different winds must be a consequence of the intrinsic properties of NGC 838 and NGC 839 and their starbursts.
SLOW SHOCKS AND CONDUCTION FRONTS FROM PETSCHEK RECONNECTION OF SKEWED MAGNETIC FIELDS: TWO-FLUID EFFECTS

In models of fast magnetic reconnection, flux transfer occurs within a small portion of a current sheet triggering stored magnetic energy to be thermalized by shocks. When the initial current sheet separates magnetic fields which are not perfectly anti-parallel, i.e., they are skewed, magnetic energy is first converted to bulk kinetic energy and then thermalized in slow magnetosonic shocks. We show that the latter resemble parallel shocks or hydrodynamic shocks for all skew angles except those very near the anti-parallel limit. As for parallel shocks, the structures of reconnection-driven slow shocks are best studied using two-fluid equations in which ions and electrons have independent temperature. Time-dependent solutions of these equations can be used to predict and understand the shocks from reconnection of skewed magnetic fields. The results differ from those found using a single-fluid model such as magnetohydrodynamics. In the two-fluid model, electrons are heated indirectly and thus carry a heat flux always well below the free-streaming limit. The viscous stress of the ions is, however, typically near the fluid-treatable limit. We find that for a wide range of skew angles and small plasma β an electron conduction front extends ahead of the slow shock but remains within the outflow jet. In such cases, conduction will play a more limited role in driving chromospheric evaporation than has been predicted based on single-fluid, anti-parallel models.
X-RAY PROPERTIES OF NARROW-LINE SEYFERT 1 GALAXIES WITH VERY SMALL BROADLINE WIDTHS

Narrow-line Seyfert 1 galaxies (NLS1s) with very small broadline widths (say, FWHM(Hβ) ≲1200 km s−1) represent the extreme type of Seyfert 1 galaxies that have small black hole masses (MBH) and/or high Eddington ratios (L/LEdd). Here, we study the X-ray properties of a homogeneously and optically selected sample of 13 such objects, termed as very narrow line Seyfert 1 galaxies, using archival XMM-Newton data. It is found that the Fe Kα emission line is at most weak in these objects. A soft X-ray excess is ubiquitous, with the thermal temperatures falling within a strict range of 0.1–0.2 keV. Our result highlights the puzzling independence of the thermal temperature by extending the relations to even smaller FWHM(Hβ), i.e., smaller MBH (∼106 M☉) and/or higher L/LEdd. The excess emission can be modeled by a range of viable models, though the disk reflection and Comptonization models generally give somewhat better fits over the smeared absorption and the p-free models. At the Eddington ratios around unity and above, the X-ray spectral slopes in the 2–10 keV band are systematically flatter than the predictions of the relationship with L/LEdd suggested previously. Short timescale (1–2 hr) X-ray variability is common, which, together with the variability amplitude computed for some of the objects, is supportive of the scenario that NLS1s are indeed active galactic nuclei with relatively small MBH.
Docking and Molecular Dynamics-Based Identification of Interaction between Various Beta-Amyloid Isoforms and RAGE Receptor

Beta-amyloid peptide (Aβ) is a ligand associated with RAGE (Advanced glycosylation end product-specific receptor). Aβ is translocated in complexes with RAGE from the blood to brain across the blood–brain barrier (BBB) by transcytosis. Aβ and its isoforms are important factors in the Alzheimer’s disease (AD) pathogenesis. However, interaction with RAGE was previously studied for Aβ but not for its isoforms. The present study has been directed at identifying the key interaction interfaces between RAGE and Aβ isoforms (Aβ40, Aβ42, phosphorylated and isomerized isoforms pS8-Aβ42, isoD7-Aβ42). Two interfaces have been identified by docking: they are represented by an extended area at the junction of RAGE domains V and C1 and a smaller area linking C1 and C2 domains. Molecular dynamics (MD) simulations have shown that all Aβ isoforms form stable and tightly bound complexes. This indicates that all Aβ isoforms potentially can be transported through the cell as part of a complex with RAGE. Modeling of RAGE interaction interfaces with Aβ indicates which chemical compounds can potentially be capable of blocking this interaction, and impair the associated pathogenic cascades. The ability of three RAGE inhibitors (RAP, FPS-ZM1 and RP-1) to disrupt the RAGE:Aβ interaction has been probed by docking and subsequently the complexes’ stability verified by MD. The RP-1 and Aβ interaction areas coincide and therefore this inhibitor is very promising for the RAGE:Aβ interaction inhibition.
Spatially evolving vortex-gas turbulent free shear layers: Part 1. Effect of velocity ratio, and upstream and downstream conditions on spread-rate

The relevance of the vortex-gas model to the large scale dynamics of temporally evolving turbulent free shear layers in an inviscid incompressible fluid has recently been established by extensive numerical simulations (Suryanarayanan et al, Phys. Rev. E 89, 013009, 2014). Here, the effects of the velocity ratio across a spatially evolving 2D free shear layer are investigated by vortex-gas simulations, using a computational model based on Basu et al (1992, 1995), but with a crucial improvement that ensures conservation of global circulation. These are carried out for a range of values of the velocity ratio parameter $\lambda= (U_1-U_2)/(U_1+U_2)$, where $U_1$ and $U_2$ ($< U_1$) are respective velocities across the layer. The simulations show that the conditions imposed at the beginning of the free shear layer and at the exit to the domain can affect the flow evolution in their respective neighborhoods, the latter being particularly strong as $\lambda \rightarrow 1$. In between the two neighborhoods is a regime of universal self-preserving growth rate given by a universal function of $\lambda$ The computed growth rates are located within the scatter of experimental data on plane mixing layers, and in close agreement with recent high Reynolds number experiments and 3D LES studies, past the mixing transition, and support the view that free shear layer growth can be largely explained by the 2D vortex dynamics of the quasi-two-dimensional large scale structures.
Love and Respect of Manual Work in Liberalized Tanzania: A Study of Primary and Secondary Schools in Mbeya and Rukwa

This paper analysed the status of love and respect for manual work among primary and secondary school students in liberalized Tanzania. It looked at how work-oriented education in public and private primary and secondary schools is practiced in the context of liberalization and how such work-oriented skills enhance agricultural inclination among recipients. Qualitative research approach and phenomenological research designs were deemed relevant. A total of 104 participants were purposively and systematic-randomly sampled including head teachers, Education for Self-Reliance (ESR) teachers, ESR prefects, teachers (not ESR) and pupils (not ESR prefects). Data was collected using in -depth interview, FGDs, direct observations and documentary review. To achieve trustworthiness, the researcher employed a number of measures such as combination of data sources such as interviews, observations, and relevant documents. The study revealed that sweeping, watering flowers and gardens and slashing were major types of manual work that students did. Most of students felt badly, less motivated and did not cherish to do the manual works. The paper concludes that the manual works done in schools did not enhance agricultural inclination and the modality on how they were provided as punishments counteracted good intentions of their use. To link education with work, production and to enhance students’ inclination in agriculture, the paper argues for revitalization of ESR at all levels of education. Furthermore, manual work should not be provided as punishment but rather as part and parcel of students’ learning.
Orbital parameters, chemical composition, and magnetic field of the Ap binary HD 98088 ⋆

ABSTRACT HD 98088 is a synchronised, double-lined spectroscopic binary system with a mag-netic Ap primary component and an Am secondary component. We study this raresystem using high-resolution MuSiCoS spectropolarimetric data, to gain insight intothe eﬀect of binarity on the origin of stellar magnetism and the formation of chemicalpeculiarities in A-type stars. Using a new collection of 29 high-resolution Stokes VQUspectra we re-derive the orbital and stellar physical parameters and conduct the ﬁrstdisentangling of spectroscopic observations of the system to conduct spectral analysisof the individual stellar components. From this analysis we determine the projectedrotational velocities of the stars and conduct a detailed chemical abundance analysis ofeach component using both the Synth3and Zeemanspectrum synthesis codes. Thesurface abundances of the primary component are typical of a cool Ap star, while thoseof the secondary component are typical of an Am star. We present the ﬁrst magneticanalysis of both components using modern data. Using Least-Squares Deconvolution,we extract the longitudinal magnetic ﬁeld strength of the primary component, which isobserved to vary between +1170 and -920 G with a period consistent with the orbitalperiod. There is no ﬁeld detected in the secondary component. The magnetic ﬁeld inthe primary is predominantly dipolar, with the positive pole oriented approximatelytowards the secondary.Key words: stars: magnetic ﬁelds, stars: abundances, stars: chemically peculiar,(stars:) binaries: spectroscopic, stars: individual: HD 98088
Deriving Information on Play and Playfulness of 3–5-Year-Olds from Short Written Descriptions: Analyzing the Frequency of Usage of Indicators of Playfulness and Their Associations with Maternal Playfulness

Playfulness is an individual differences variable that enables people to (re-)frame almost any situation into an entertaining, amusing, intellectually stimulating and/or personally interesting situation by interacting playfully with others, by resolving tension, by liking complexity over simplicity and/or by having a preference for unusual topics, persons and/or activities. We asked 208 German-speaking mothers of 3–5-year-olds to describe their child in 5–10 sentences. Using a list of criteria for playfulness (e.g., actively initiating humor, playful exchange with others or widespread interests), we found that mothers used, on average, two playful characteristics to describe their child (17% did not report any). Greater usage of playful descriptors in the written texts was positively related mainly to greater other-directed and intellectual playfulness of the mothers. The findings are encouraging and suggest that the list of playful criteria in descriptions of children could be used in the study of inter-individual differences in playfulness in young children.