Miracle-dz/UniFAR-FTUs huggingface dataset:
Aharonov-Bohm-Like Oscillations in Quantum Hall Corrals

Experimental study of quantum Hall corrals reveals Aharonov-Bohm-Like (ABL) oscillations. Unlike the Aharonov-Bohm effect which has a period of one flux quantum, $\Phi_{0}$, the ABL oscillations possess a flux period of $\Phi_{0}/f$, where $f$ is the integer number of fully filled Landau levels in the constrictions. Detection of the ABL oscillations is limited to the low magnetic field side of the $\nu_{c}$ = 1, 2, 4, 6. integer quantum Hall plateaus. These oscillations can be understood within the Coulomb blockade model of quantum Hall interferometers as forward tunneling and backscattering, respectively, through the center island of the corral from the bulk and the edge states. The evidence for quantum interference is weak and circumstantial.
LHC Phenomenology of SO(10) Models with Yukawa Unification

In this paper we study an SO(10) SUSY GUT with Yukawa unification for the third generation. We perform a global χ2 analysis given to obtain the GUT boundary conditions consistent with 11 low energy observables, including the top, bottom and tau masses. We assume a universal mass, m16, for squarks and sleptons and a universal gaugino mass, M1/2. We then analyze the phenomenological consequences for the LHC for 15 benchmark models with fixed m16 = 20 TeV and with varying values of the gluino mass. The goal of the present work is to (i) evaluate the lower bound on the gluino mass in our model coming from the most recent published data of CMS and (ii) to compare this bound with similar bounds obtained by CMS using simplified models. The bottom line is that the bounds coming from the same sign di-lepton analysis are comparable for our model and the simplified model studied assuming B(g̃ → t t̄ χ̃1) = 100%. However the bounds coming from the purely hadronic analyses for our model are 10 20% lower than obtained for the simplified models. This is due to the fact that for our models the branching ratio for the decay g̃ → g χ̃1,2 is significant. Thus there are significantly fewer b-jets. We find a lower bound on the gluino mass in our models with Mg̃ & 1000 GeV. Finally, there is a theoretical upper bound on the gluino mass which increases with the value of m16. For m16 ≤ 30 TeV, the gluino mass satisfies Mg̃ ≤ 2.8 TeV at 90% CL. Thus, unless we further increase the amount of fine-tuning, we expect gluinos to be discovered at LHC 14. ar X iv :1 30 7. 77 23 v2 [ he pph ] 6 S ep 2 01 3
Rényi Entropies of Multidimensional Oscillator and Hydrogenic Systems with Applications to Highly Excited Rydberg States

The various facets of the internal disorder of quantum systems can be described by means of the Rényi entropies of their single-particle probability density according to modern density functional theory and quantum information techniques. In this work, we first show the lower and upper bounds for the Rényi entropies of general and central-potential quantum systems, as well as the associated entropic uncertainty relations. Then, the Rényi entropies of multidimensional oscillator and hydrogenic-like systems are reviewed and explicitly determined for all bound stationary position and momentum states from first principles (i.e., in terms of the potential strength, the space dimensionality and the states’s hyperquantum numbers). This is possible because the associated wavefunctions can be expressed by means of hypergeometric orthogonal polynomials. Emphasis is placed on the most extreme, non-trivial cases corresponding to the highly excited Rydberg states, where the Rényi entropies can be amazingly obtained in a simple, compact, and transparent form. Powerful asymptotic approaches of approximation theory have been used when the polynomial’s degree or the weight-function parameter(s) of the Hermite, Laguerre, and Gegenbauer polynomials have large values. At present, these special states are being shown of increasing potential interest in quantum information and the associated quantum technologies, such as e.g., quantum key distribution, quantum computation, and quantum metrology.
Predicting Maximal Aerobic Capacity based on Self-Reported Physical Activity Levels among Adolescents

Growing evidence has indicated a positive association between physical activity and cardiorespiratory fitness (i.e., maximal aerobic capacity or VO2 max). Limited evidence, however, is available among adolescents. This research aimed to predict VO2 max based on the physical activity level and estimate the discriminant capacity of the physical activity levels on the VO2 max status among adolescents. This research was a cross-sectional study in 141 adolescents (age 19±1 year old, 83% male). The VO2 max was assessed using the 1-mile run test. Physical activity was measured using the International Physical activity Questionnaire-Long Form. Multiple linear regression was conducted to predict the VO2 max using physical activity level data (in metabolic equivalent of tasks (Mets/week), sex, and body mass index (BMI). The discriminant capacity of the total and domain-specific physical activity in discriminating high and low VO2 max was estimated with the area under the curve (AUC). The Youden Index determined cut-off points, sensitivity, and specificity. Multiple regression analysis revealed a significant predicting equation of VO2 based on total physical activities, BMI, and sex. The equation explained a significant proportion of VO2 max variances. The total and domain-specific physical activity significantly discriminated low and high VO2 max status, while the highest AUC was based on total physical activity, followed by other physical activity domains. A cut-off of total physical activity levels for predicting the VO2 max was successfully generated, with high sensitivity and specificity. Adequate evidence, thus, supports the prediction of VO2 max based on self-reported physical activity levels among adolescents.
Models of cuspy triaxial stellar systems – IV. Rotating systems

Fil: Carpintero, Daniel Diego. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Centro Cientifico Tecnologico Conicet - La Plata. Instituto de Astrofisica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronomicas y Geofisicas. Instituto de Astrofisica la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronomicas y Geofisicas; Argentina
Hypertensive disorders during pregnancy and elevated blood pressure in the offspring

Background: Hypertensive disorders during pregnancy (HDP), including gestational hypertension, preeclampsia (PE), and chronic hypertension, affect approximately 10% of pregnancies worldwide. PE was associated with elevated blood pressure (BP) in the offspring confirmed by previous literature. No previous systematic review has investigated the associations between the subtypes of HDP and BP in offspring. Therefore, from the published literature, the present systematic review and meta-analysis aims to reach to a clear consensus on this topic. Methods: The Cochrane Handbook for Systematic Reviews of Interventions was used to structure our methodological approach, and the Preferred Reporting Items for Systematic Reviews and Meta Analyses Protocols guidelines to this protocol. We will include cohort, case-control, and cross-sectional studies, in which HDP or its subtypes were reported and BP in the offspring was the outcome of interest. A systematic search of PubMed, Embase, the Cochrane library, and Web of Science will be conducted according to a specific search strategy. The titles and abstracts of all literature will be reviewed independently by 2 authors. A standardized data collection form will be used for data extraction. The overall pooled estimates will be calculated by meta-analysis in Revman 5.3 based on an inverse variance method. According to the heterogeneity by the I2, a random-effect model or a fixed-effect model will be chosen to pool data. Risk of bias and quality of the studies will be assessed by a suitable bias classification tool. Results: This study will provide high-quality evidence of the effects in offspring BP, which were influenced by different subtypes of HDP. Conclusion: This systematic review will infer a conclusion on the associations between different subtypes of HDP and BP in offspring. Ethics and dissemination: Due to the data come from the published study, the present systematic review and meta-analysis does not require ethics approval. Findings will be published in a peer-reviewed journal. Registration: Supporting data can be found at the International Prospective Register of Systematic Reviews (PROSPERO) website, with registration number CRD 42018110872.
Extending semi-numeric reionization models to the first stars and galaxies

Semi-numeric methods have made it possible to efficiently model the epoch of reionisation (EoR). While most implementations involve a reduction to a simple three-parameter model, we introduce a new mass-dependent ionising efficiency parameter that folds in physical parameters that are constrained by the latest numerical simulations. This new parameterization enables the effective modeling of a broad range of host halo masses containing ionising sources, extending from the smallest Population III host halos with $M \sim 10^6 M_\odot$, which are often ignored, to the rarest cosmic peaks with $M \sim 10^{12} M_\odot$ during EoR. We compare the resulting ionising histories with a typical three-parameter model and also compare with the latest constraints from the Planck mission. Our model results in a optical depth due to Thomson scattering, $\tau_{\mathrm{e}}$ = 0.057, that is consistent with Planck. The largest difference in our model is shown in the resulting bubble size distributions which peak at lower characteristic sizes and are broadened. We also consider the uncertainties of the various physical parameters and comparing the resulting ionising histories broadly disfavors a small contribution from galaxies. As the smallest haloes cease a meaningful contribution to the ionising photon budget after $z = 10$, implying they play a role in determining the start of EoR and little else.
ELLIPTICAL GALAXY MASSES OUT TO FIVE EFFECTIVE RADII: THE REALM OF DARK MATTER

We estimate the masses of elliptical galaxies out to five effective radii using planetary nebulae and globular clusters as tracers. A sample of 15 elliptical galaxies with a broad variation in mass is compiled from the literature. A distribution function-maximum likelihood analysis is used to estimate the overall potential slope, normalization, and velocity anisotropy of the tracers. We assume power-law profiles for the potential and tracer density and a constant velocity anisotropy. The derived potential power-law indices lie in between the isothermal and Keplerian regime and vary with mass: there is tentative evidence that the less massive galaxies have steeper potential profiles than the more massive galaxies. We use stellar mass-to-light ratios appropriate for either a Chabrier/KTG (Kroupa, Tout & Gilmore) or Salpeter initial mass function to disentangle the stellar and dark matter components. The fraction of dark matter within five effective radii increases with mass, in agreement with several other studies. We employ simple models to show that a combination of star formation efficiency and baryon extent are able to account for this trend. These models are in good agreement with both our measurements out to five effective radii and recent Sloan Lens ACS Survey measurements within one effective radii when a universal Chabrier/KTG initial mass function is adopted.
THE ENVIRONMENT OF MASSIVE QUIESCENT COMPACT GALAXIES AT 0.1 < z < 0.4 IN THE COSMOS FIELD

We use Hectospec mounted on the 6.5 m MMT to carry out a redshift survey of red ( r − i > 0.2 ? > , g − r > 0.8 ? > , r < 21.3 ? > ) galaxies in the Cosmological Evolution Survey (COSMOS) field to measure the environments of massive compact quiescent galaxies at intermediate redshift. The > 90 % ? > complete magnitude limited survey includes redshifts for 1766 red galaxies with r < 20.8 ? > covering the central square degree of the field; 65% of the redshifts in this sample are new. We select a complete magnitude limited quiescent sample based on the rest-frame UVJ colors. When the density distribution is sampled on a scale of 2 Mpc, massive compact galaxies inhabit systematically denser regions than the parent quiescent galaxy population. Noncompact quiescent galaxies with the same stellar masses as their compact counterparts populate a similar distribution of environments. Thus the massive nature of quiescent compacts accounts for the environment dependence and appears fundamental to their history.
EVOLUTION OF GALAXY GROUPS IN THE ILLUSTRIS SIMULATION

We present the first study of the evolution of galaxy groups in the Illustris simulation. We focus on dynamically relaxed and unrelaxed galaxy groups representing dynamically evolved and evolving galaxy systems, respectively. The evolutionary state of a group is probed from its luminosity gap and separation between the brightest group galaxy and the center of mass of the group members. We find that the Illustris simulation overproduces galaxy systems with a large luminosity gap, known as fossil systems, in comparison to observations and the probed semi-analytical predictions. However, this simulation is just as successful as the probed semi-analytic model in recovering the correlation between luminosity gap and offset of the luminosity centroid. We find evolutionary tracks based on luminosity gap that indicate that a group with a large luminosity gap is rooted in one with a small luminosity gap, regardless of the position of the brightest group galaxy within the halo. This simulation helps to explore, for the first time, the black hole mass and its accretion rate in galaxy groups. For a given stellar mass of the brightest group galaxies, the black hole mass is larger in dynamically relaxed groups with a lower rate of mass accretion. We find this to be consistent with the latest observational studies of radio activity in the brightest group galaxies in fossil groups. We also find that the intragalactic medium in dynamically evolved groups is hotter for a given halo mass than that in evolving groups, again consistent with earlier observational studies.
MASS DISTRIBUTIONS OF STARS AND CORES IN YOUNG GROUPS AND CLUSTERS

We investigate the relation of the stellar initial mass function and the dense core mass function (CMF), using stellar masses and positions in 14 well-studied young groups. Initial column density maps are computed by replacing each star with a model initial core having the same star formation efficiency (SFE). For each group the SFE, core model, and observational resolution are varied to produce a realistic range of initial maps. A clump-finding algorithm parses each initial map into derived cores, derived core masses, and a derived CMF. The main result is that projected blending of initial cores causes derived cores to be too few and too massive. The number of derived cores is fewer than the number of initial cores by a mean factor of 1.4 in sparse groups and 5 in crowded groups. The mass at the peak of the derived CMF exceeds the mass at the peak of the initial CMF by a mean factor of 1.0 in sparse groups and 12.1 in crowded groups. These results imply that in crowded young groups and clusters, the mass distribution of observed cores may not reliably predict the mass distribution of protostars that will form in those cores.
Complete integrability of Nonlocal Nonlinear Schr\"odinger equation

Based on the completeness relation for the squared solutions of the Lax operator $L$ we show that a subset of nonlocal equations from the hierarchy of nonlocal nonlinear Schrodinger equations (NLS) is a completely integrable system. The spectral properties of the Lax operator indicate that there are two types of soliton solutions. The relevant action-angle variables are parametrized by the scattering data of the Lax operator. The notion of the symplectic basis, which directly maps the variations of the potential of $L$ to the variations of the action-angle variables has been generalized to the nonlocal case. We also show that the inverse scattering method can be viewed as a generalized Fourier transform. Using the trace identities and the symplectic basis we construct the hierarchy Hamiltonian structures for the nonlocal NLS equations.
Exact renormalization group flow in an expanding Universe and screening of the cosmological constant

We obtain the exact renormalization group (RG) flow equation for a self interacting real scalar field in an expanding cosmological background. The beta functional for the potential in the local potential approximation is determined in terms of the mode functions defining the vacuum of the theory. For a scalar in an inflating universe, which is released in the Bunch-Davies vacuum, the flow equation is analyzed in detail using the optimized cutoff function for the quartically truncated potential. In that case, the constant term in the potential, which can in fact be viewed as the cosmological constant, decreases as the IR cutoff is removed, supporting the existence of a quantum mechanical screening mechanism. On the other hand, the running of the quartic coupling constant at IR is altered by the expansion, which seems to affect the quantum triviality of the theory.
Constraints on the exponential $f(R)$ model from latest Hubble parameter measurements

We investigate the viable exponential $f(R)$ gravity in the metric formalism with $f(R)=-\beta R_s (1-e^{-R/R_s})$. The latest sample of the Hubble parameter measurements with 23 data points is used to place bounds on this $f(R)$ model. A joint analysis is also performed with the luminosity distances of Type Ia supernovae and baryon acoustic oscillations in the clustering of galaxies, and the shift parameters from the cosmic microwave background measurements, which leads to $0.240 1.47$ at 1$\sigma$ confidence level. The evolutions of the deceleration parameter $q(z)$ and the effective equations of state $\omega_{de}^{eff}(z)$ and $\omega_{tot}^{eff}(z)$ are displayed. By taking the best-fit parameters as prior values, we work out the transition redshift (deceleration/acceleration) $z_T$ to be about 0.77. It turns out that the recent observations are still unable to distinguish the background dynamics in the $\Lambda$CDM and exponential $f(R)$ models.
CAN WE SEE NAKED SINGULARITIES

We study singularities which can form in a spherically symmetric gravitational collapse of a general matter field obeying weak energy condition. We show that null naked singularities that form in such a collapse can never be observed. No energy can come out of these singularities; thus they will have no physical consequences outside. As this happens for any null singularity, we do not need to assume specific form of matter and establish role of initial data. Hence our result is very general.
eLISA eccentricity measurements as tracers of binary black hole formation

Up to hundreds of black hole binaries individually resolvable by eLISA will coalesce in the Advanced LIGO and Virgo band within 10 yr, allowing for multiband gravitational wave observations. Binaries formed via dynamical interactions in dense star clusters are expected to have eccentricities ${e}_{0}\ensuremath{\sim}{10}^{\ensuremath{-}3}\ensuremath{-}{10}^{\ensuremath{-}1}$ at the frequencies ${f}_{0}={10}^{\ensuremath{-}2}\text{ }\text{ }\mathrm{Hz}$ where eLISA is most sensitive, while binaries formed in the field should have negligible eccentricity in both frequency bands. We estimate that eLISA should always be able to detect a nonzero ${e}_{0}$ whenever ${e}_{0}\ensuremath{\gtrsim}{10}^{\ensuremath{-}2}$; if ${e}_{0}\ensuremath{\sim}{10}^{\ensuremath{-}3}$, eLISA should detect nonzero eccentricity for a fraction $\ensuremath{\sim}90%$ ($\ensuremath{\sim}25%$) of binaries when the observation time is ${T}_{\mathrm{obs}}=5$ (2) yr, respectively. Therefore eLISA observations of black hole binaries have the potential to distinguish between field and cluster formation scenarios.
Pollen analysis of honey from Laghouat region (Algeria)

Abstract A microscopic analysis of 41 samples of honey obtained from several locations in the Laghouat region revealed the presence of 98 pollen types belonging to 48 families. Asteraceae, Fabaceae and Nitrariaceae were present in all the samples. Brassicaceae, Rhamnaceae and Apiaceae were identified in more than 80% of the samples. The families with highest diversity of pollen types were Fabaceae and Asteraceae with 13 and 11 types, respectively, Apiaceae and Boraginaceae with five types each. Twenty-seven honey samples (65.85%) were found to be monofloral and the remaining 14 polyfloral. The pollen types from Ziziphus lotus, Peganum harmala, Echium sp. , Tamarix sp. , Lotus, Eucalyptus sp. , Eruca vesicaria and Thapsia garganica appeared as the predominant pollen. Eighteen pollen types were classified as very frequent, present in more than 50% of the samples. The number of pollen types identified per sample ranged between 14 and 40 (mean of 24.41). For the quantitative analysis, the pollen content of the studied honey samples ranged from medium (class II, 48.78% of the samples) to high (class III, 53.65% of the samples), where the pollen density ranged from 26 607 to 660 992 in 10 g of honey, with an average of 160 880 grains per 10 g.
Learners’ Perceptions and Attitudes towards the Use of Mind-mapping Technique in Enhancing their Understanding of Short Stories

Learners’ proficiency in ESL includes their ability in comprehending a reading text. Short stories are often found difficult due to linguistic and cultural elements found in the texts. Despite this, Part 2 Diploma students in Universiti Teknologi MARA Perak are required to read a selection of short stories as part of their English class syllabus. In this study, a mind mapping technique is used to assist learners to understand the short stories well. This technique is chosen as its concept involves the process of associating ideas and information through relationship ties. 60 students from 2 English classes were introduced to this mind-mapping technique which they had to apply when discussing the plot of the story and the traits of the main character to ascertain their understanding of the short story. Although the students managed to complete the task well, it was not known whether the mind-mapping technique had helped them in enhancing their understanding of the short stories. Therefore, this paper aims to find out their perceptions and attitudes towards the use of mind-maps in comprehending short stories through a survey questionnaire using 5-Likert scale. The data from the survey underwent a statistical analysis using SPSS before discussing the findings. The findings revealed that the respondents of this study had a positive attitude towards the use of mind-map and perceived it as a useful tool in helping them to understand short stories. Thus, the mind-mapping technique should continue to be used in reading class to help learners to enhance their comprehension of short stories.