Miracle-dz/UniFAR-FTUs huggingface dataset:
Stochastic gravitational wave background from magnetic deformation of newly born magnetars

Newly born magnetars are promising sources for gravitational wave (GW) detection due to their ultra-strong magnetic fields and high spin frequencies. Within the scenario of a growing tilt angle between the star's spin and magnetic axis, due to the effect of internal viscosity, we obtain improved estimates of the stochastic gravitational wave backgrounds (SGWBs) from magnetic deformation of newly born magnetars. We find that the GW background spectra contributed by the magnetars with ultra-strong toroidal magnetic fields of 10^{17} G could roughly be divided into four segments. Most notably, in contrast to the background spectra calculated by assuming constant tilt angles \chi=\pi/2, the background radiation above 1000 Hz are seriously suppressed. However, the background radiation at the frequency band \sim100-1000 Hz are moderately enhanced, depending on the strengths of the dipole magnetic fields. We suggest that if all newly born magnetars indeed have toroidal magnetic fields of 10^{17} G, the produced SGWBs should show sharp variations with the observed frequency at several tens to about 100 hertz. If these features could be observed through sophisticated detection of the SGWB using the proposed Einstein Telescope, it will provide us a direct evidence of the tilt angle evolutions and further some deep understandings about the properties of newly born magnetars.
Direct Shear Mapping: Prospects for Weak Lensing Studies of Individual Galaxy–Galaxy Lensing Systems

Abstract Using both a theoretical and an empirical approach, we have investigated the frequency of low redshift galaxy-galaxy lensing systems in which the signature of 3D weak lensing might be directly detectable. We find good agreement between these two approaches. Using data from the Galaxy and Mass Assembly redshift survey we estimate the frequency of detectable weak lensing at low redshift. We find that below a redshift of z ~ 0.6, the probability of a galaxy being weakly lensed by γ ⩾ 0.02 is ~ 0.01. We have also investigated the feasibility of measuring the scatter in the M* − Mh relation using shear statistics. We estimate that for a shear measurement error of Δγ = 0.02 (consistent with the sensitivity of the Direct Shear Mapping technique), with a sample of ~$50,000 spatially and spectrally resolved galaxies, the scatter in the M* − Mh relation could be measured. While there are currently no existing IFU surveys of this size, there are upcoming surveys that will provide this data (e.g The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX), surveys with Hector, and the Square Kilometre Array (SKA)).
Comparative study of the performance of a sliding, sliding-fuzzy type 1 and a sliding-fuzzy type 2 control of a permanent magnet synchronous machine

This paper presents a comparative study of sliding mode control, hybrid sliding type-1 fuzzy logic and hybrid sliding type-2 fuzzy logic applied on the permanent magnet synchronous machine (PMSM). We used different criteria in this comparison: qualitative, quantitative and robust during the transient and permanent operation of the system. In this article, we present a new sliding mode control strategy applied to the PMSM, this control combines sliding mode and fuzzy logic (type-1 and type-2) to find robust control. The control proposed keeping the part of the equivalent control by sliding mode and will change the part of the switching by a fuzzy controller. Simulation results with a sliding mode control, type-1 fuzzy logic controller (T1FLC) and with an interval type-2 fuzzy logic controller (IT2FLC) of a permanent magnet synchronous machine are presented. The advantage of using interval type-2 fuzzy logic controller is verified.
Phenomenological aspects of a TeV-scale alternative left-right model

We revisit the alternative left-right symmetric model, motivated by superstring-inspired $E_6$ model. We systematically analyze the constraints imposed by theoretical and experimental bounds on the parameter space of this class of models. We perform a comprehensive analysis of the Higgs sector and show that three neutral CP-even and two CP-odd Higgs bosons in addition to two charged Higgs bosons can be light, of ${\cal O}(100)$ GeV. We emphasise that our model has a potential to account for the recent Large Hadron Collider results for signal strength of Higgs decays. We also explore discovery signatures of the exotic down-type quark, which is one of the salient predictions of this model.
Total length of the genealogical tree for quadratic stationary continuous-state branching processes

We prove the existence of the total length process for the genealogical tree of a population model with random size given by a quadratic stationary continuous-state branching processes. We also give, for the one-dimensional marginal, its Laplace transform as well as the fluctuation of the corresponding convergence. This result is to be compared with the one obtained by Pfaffelhuber and Wakolbinger for constant size population associated to the Kingman coalescent. We also give a time reversal property of the number of ancestors process at all time, and give a description of the so-called lineage tree in this model.
Effects of Copper nanoparticle supplementation on growth, intestinal morphology and antioxidant status in broilers exposed to cyclic cold stress

The purpose of this research was to determine the effects of copper nanoparticles (CuNP) supplementation on growth performance, intestinalmorphology, intraepithelial lymphocytes (IELs), goblet cell (GC) count, stress hormones and oxidant/antioxidant balance of broilers exposedto cold stress. One day old broiler chickens (n=400) were allocated into five different groups and were raised under standard conditionsuntil the 21st day. The five groups were designated as thermo-neutral (TN reared in 26°C), cold stress (CS raised under 13°C±2°C for8 hours/day from d 22- d 35), CS5 (CS+ 5mg/kg diet CuNP), CS10 (CS+10mg/kg diet CuNP) and CS15 (CS+15mg/kg diet CuNP). On35th day, 16 birds per group were selected randomly for blood collection and were then humanely sacrificed for tissue sample collection.CS group had a reduced (P<0.05) body weight (BW), villus surface area (VSA), villus height to crypt depth ratio (VH: CD) but had ahigher (P<0.05) feed conversion ratio (FCR), goblet cell count, serum corticosterone and malondialdehyde (MDA) levels than the TNgroup. Inclusion of CuNP in diet linearly increased (P<0.05) BW, VH, VW, CD, VSA and GC count in jejunum and ileum. Conversely,MDA and corticosterone hormone levels and FCR, decreased linearly (P<0.05) with CuNP supplementation. In conclusion, during coldstress conditions, CuNP is a valuable feed additive in broilers with positive effects on growth performance and intestinal morphology
NONRELATIVISTIC COLLISIONLESS SHOCKS IN WEAKLY MAGNETIZED ELECTRON–ION PLASMAS: TWO-DIMENSIONAL PARTICLE-IN-CELL SIMULATION OF PERPENDICULAR SHOCK

A two-dimensional particle-in-cell simulation is performed to investigate weakly magnetized perpendicular shocks with a magnetization parameter of σ = 6 × 10−5, which is equivalent to a high Alfvén Mach number MA of ∼130. It is shown that current filaments form in the foot region of the shock due to the ion-beam–Weibel instability (or the ion filamentation instability) and that they generate a strong magnetic field there. In the downstream region, these current filaments also generate a tangled magnetic field that is typically 15 times stronger than the upstream magnetic field. The thermal energies of electrons and ions in the downstream region are not in equipartition and their temperature ratio is Te/Ti ∼ 0.3–0.4. Efficient electron acceleration was not observed in our simulation, although a fraction of the ions are accelerated slightly on reflection at the shock. The simulation results agree very well with the Rankine–Hugoniot relations. It is also shown that electrons and ions are heated in the foot region by the Buneman instability (for electrons) and the ion-acoustic instability (for both electrons and ions). However, the growth rate of the Buneman instability is significantly reduced due to the relatively high temperature of the reflected ions. For the same reason, ion–ion streaming instability does not grow in the foot region.
Systematic Search for Rings around Kepler Planet Candidates: Constraints on Ring Size and Occurrence Rate

We perform a systematic search for rings around 168 Kepler planet candidates with sufficient signal-to-noise ratios that are selected from all the short-cadence data. We fit ringed and ringless models to their lightcurves, and compare the fitting results to search for the signatures of planetary rings. First, we identify 29 tentative systems, for which the ringed models exhibit statistically significant improvement over the ringless models. The lightcurves of those systems are individually examined, but we are not able to identify any candidate that indicates evidence for rings. In turn, we find out several mechanisms of false-positives that would produce ring-like signals, and the null detection enables us to place upper limits on the size of rings. Furthermore, assuming the tidal alignment between axes of the planetary rings and orbits, we conclude that the occurrence rate of rings larger than twice the planetary radius is less than 15 percent. Even though the majority of our targets are short-period planets, our null detection provides statistical and quantitative constraints on largely uncertain theoretical models of origin, formation, and evolution of planetary rings.
Potential tuning in the S–W system. (i) Bringing Tc,2 to ambient pressure, and (ii) colliding Tc,2 with the liquid–vapor spinodal

Following Vasisht et al’s identification of the second critical point (Tc2, Pc2) for liquid silicon in the Stillinger–Weber (S–W) model for silicon, we study the variation of Tc2, Pc2 with tetrahedral repulsion parameter in an extension of the earlier ‘potential tuning’ study of this system. We use the simple isochore crossing approach to identify the location of the second critical point (before any crystallization can occur) as a function of the ‘tuning’ or ‘tetrahedrality’, parameter λ, and identify two phenomena of high interest content. The first is that the second critical point pressure Pc2, becomes less negative as λ decreases from the silicon value (meaning the drive to high tetrahedrality is decreased) and reaches zero pressure at the same value of lambda found to mark the onset of glassforming ability in an earlier study of this tunable system. The second is that, as the Tc,2 approaches the temperature of the liquid–gas spinodal, λ > 22, the behavior of the temperature of maximum density (TMD) switches from the behavior seen in most current water pair potential models (locus of TMDs has a maximum), to the behavior seen in empirical engineering multiparameter equations of state (EoS) (and also by two parameter Speedy isothermal expansion EoS) for water, according to which the locus of TMDs of HDL phase has no maximum, and the EoS for HDL has no second critical point. At λ = 23 the behavior is isomorphic with that of the mW model of water, which is now seen to conform, at least closely, to the ‘critical point free’ scenario for water.
A new adaptive elevator selection routing algorithm for 3D NoCs based on load balancing

With the development of TSV technology, the higher layer and lower layer in the vertical part in 3D NoCs are connected by TSV widely. The disadvantage of TSV is that deterministic routing algorithm cannot realize the load balancing for non-uniform flow. In order to solve the mentioned problem, an adaptive elevator selection routing algorithm (ASELB) based on load balancing for TSV is proposed for considering fully low latency transmission. According to the load flow in 3D NoCs, the data packet can choose flexibly any valid elevator to transmit in the layer with the destination node, the layer with the source node or middle layer, which guarantees the load balancing in every layer. The results of simulation show that the load in every layer (especially the load around router with TSV) can keep relative balance and avoid congestion in the certain network, and the performance of our proposing routing algorithm in the network latency is a little superior or equal to the other relative algorithms.
THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I. HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS

We present uniformly measured star formation histories (SFHs) of 40 Local Group (LG) dwarf galaxies based on color–magnitude diagram (CMD) analysis from archival Hubble Space Telescope imaging. We demonstrate that accurate SFHs can be recovered from CMDs that do not reach the oldest main sequence turn-off (MSTO), but emphasize that the oldest MSTO is critical for precisely constraining the earliest epochs of star formation. We find that: (1) the average lifetime SFHs of dwarf spheroidals (dSphs) can be approximated by an exponentially declining SFH with τ ∼ 5 Gyr; (2) lower luminosity dSphs are less likely to have extended SFHs than more luminous dSphs; (3) the average SFHs of dwarf irregulars (dIrrs), transition dwarfs, and dwarf ellipticals can be approximated by the combination of an exponentially declining SFH (τ ∼ 3–4 Gyr) for lookback ages >10–12 Gyr ago and a constant SFH thereafter; (4) the observed fraction of stellar mass formed prior to z = 2 ranges considerably (80% for galaxies with M < 105 M☉ to 30% for galaxies with M > 107 M☉) and is largely explained by environment; (5) the distinction between “ultra-faint” and “classical” dSphs is arbitrary; (6) LG dIrrs formed a significantly higher fraction of stellar mass prior to z = 2 than the Sloan Digital Sky Survey galaxies from Leitner and the SFHs from the abundance matching models of Behroozi et al. This may indicate higher than expected star formation efficiencies at early times in low mass galaxies. Finally, we provide all the SFHs in tabulated electronic format for use by the community.
Modular anomaly from holomorphic anomaly in mass deformed N = 2 superconformal field theories

We study the instanton partition functions of two well-known superconformal field theories with mass deformations. Two types of anomaly equations, namely, the modular anomaly and holomorphic anomaly, have been discovered in the literature. We provide a clean solution to the long standing puzzle about their precise relation, and obtain some universal formulas. We show that the partition function is invariant under the $SL(2,\mathbb{Z})$ duality which exchanges theories at strong coupling with those of weak coupling.
ournal of C osmology and A stroparticle hysics Precision growth index using the clustering of cosmic structures and growth data

We use the clustering properties of Luminous Red Galaxies (LRGs) and the growth rate data provided by the various galaxy surveys in order to constrain the growth index ( γ ) of the linear matter ﬂuctuations. We perform a standard χ 2 -minimization procedure between theoretical expectations and data, followed by a joint likelihood analysis and we ﬁnd a value of γ = 0 . 56 ± 0 . 05, perfectly consistent with the expectations of the ΛCDM model, and Ω m 0 = 0 . 29 ± 0 . 01, in very good agreement with the latest Planck results. Our analysis provides signiﬁcantly more stringent growth index constraints with respect to previous studies, as indicated by the fact that the corresponding uncertainty is only ∼ 0 . 09 γ . Finally, allowing γ to vary with redshift in two manners (Taylor expansion around z = 0, and Taylor expansion around the scale factor), we ﬁnd that the combined statistical analysis between our clustering and literature growth data alleviates the degeneracy and obtain more stringent constraints with respect to other recent studies.
Exact holographic mapping and emergent space-time geometry

In this paper, we propose an {\it exact holographic mapping} which is a unitary mapping from the Hilbert space of a lattice system in flat space (boundary) to that of another lattice system in one higher dimension (bulk). By defining the distance in the bulk system from two-point correlation functions, we obtain an emergent bulk space-time geometry that is determined by the boundary state and the mapping. As a specific example, we study the exact holographic mapping for $(1+1)$-dimensional lattice Dirac fermions and explore the emergent bulk geometry corresponding to different boundary states including massless and massive states at zero temperature, and the massless system at finite temperature. We also study two entangled one-dimensional chains and show that the corresponding bulk geometry consists of two asymptotic regions connected by a worm-hole. The quantum quench of the coupled chains is mapped to dynamics of the worm-hole. In the end we discuss the general procedure of applying this approach to interacting systems, and other open questions.
Optimizing Intentional Islanding Design Strategies for Enhanced Failure Resilience of Power Systems

Establishing cleaner energy generation therefore improving the sustainability of power systems is a crucial task in this century. One of the key strategies being pursued is to shift the dependence on fossil fuel to renewable technologies such as wind, solar, and nuclear. However, with the increasing number of heterogeneous components included in the power system, the complexity of the hybrid energy system becomes more significant, which makes it prone to system failures. The complex system imposes a more stringent requirement of the contingency plan to enhance the overall system resilience against potential system disruptive events. Among different strategies to ensure a resilient system, intentional islanding is commonly applied in practical applications for power systems. In this study, we address the challenges of intentional islanding design considering high penetration of renewable energy sources, and develop a hierarchical clustering-based design method for optimized intentional islanding strategies at the transmission level of a power system. To incorporate the renewable generation that relies on the inverter technology, the frequency measurements are considered to represent the transient response and further used as embedded information in the clustering algorithm. And in the case study, the stabilized post-disruption performance of the modified IEEE-9 bus test system demonstrates the capability of the proposed method for resilience enhancement.
Stability of composite vacuum Heckmann wormholes in Brans-Dicke theory

This paper discusses linearized (spherically symmetric) perturbation of static Heckmann composite thin shell wormholes in Brans-Dicke gravity. The equation of state $P= \beta^2 \sigma$ at the throat is linearized around the static solution where $\sigma$ energy density of the shell and $P$ the presume. We have shown that this thin shell wormholes is stable within the range $0\leq\beta<1$ and with all values of $\omega$ except $\omega=-2$.
The distribution and physical properties of high-redshift [O iii] emitters in a cosmological hydrodynamics simulation

Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [OIII] 88 \mu m line from galaxies at $z \sim 7 - 9$. Far-infrared lines can be used to probe the structure and kinematics of such high-redshift galaxies as well as to accurately determine their spectroscopic redshifts. We use a cosmological simulation of galaxy formation to study the physical properties of [OIII] 88 \mu m emitters. In a comoving volume of 50 $h^{-1}$ Mpc on a side, we locate 34 galaxies with stellar masses greater than $10^8\ {\rm M_\odot}$ at $z = 9$, and more than 270 such galaxies at $z = 7$. We calculate the [OIII] 88 \mu m luminosities ($L_{\rm OIII}$) by combining a physical model of HII regions with emission line calculations using the photoionization code CLOUDY. We show that the resulting $L_{\rm OIII}$, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7 - 9. Bright [OIII] emitters with $L_{\rm OIII} > 10^8 {\rm L_\odot}$ have stellar masses greater than $10^9\ {\rm M_\odot}$, star formation rates higher than $3\ {\rm M_\odot\ yr}^{-1}$, and the typical metallicity is $\sim 0.1\ {\rm Z_\odot}$. The galaxies are hosted by dark matter halos with masses greater than $10^{10.5}\ {\rm M_\odot}$. Massive galaxies show characteristic structure where the [OIII] emitting gas largely overlaps with young stars, but the emission peak is separated from the main stellar population, suggesting the stochastic and localized nature of star formation in the first galaxies. We propose to use the [OIII] 5007 \AA\ line, to be detected by James Webb Space Telescope (JWST), to study the properties of galaxies whose [OIII] 88 \mu m line emission has been already detected with ALMA.
HOW SIGNIFICANT IS RADIATION PRESSURE IN THE DYNAMICS OF THE GAS AROUND YOUNG STELLAR CLUSTERS?

The impact of radiation pressure on the dynamics of the gas in the vicinity of young stellar clusters is thoroughly discussed. The radiation over the thermal/ram pressure ratio time evolution is calculated explicitly and the crucial roles of the cluster mechanical power, the strong time evolution of the ionizing photon flux, and the bolometric luminosity of the exciting cluster are stressed. It is shown that radiation has only a narrow window of opportunity to dominate the wind-driven shell dynamics. This may occur only at early stages of the bubble evolution and if the shell expands into a dusty and/or a very dense proto-cluster medium. The impact of radiation pressure on the wind-driven shell always becomes negligible after about 3 Myr. Finally, the wind-driven model results allow one to compare the model predictions with the distribution of thermal pressure derived from X-ray observations. The shape of the thermal pressure profile then allows us to distinguish between the energy and the momentum-dominated regimes of expansion and thus conclude whether radiative losses of energy or the leakage of hot gas from the bubble interior have been significant during bubble evolution.
Bose-Einstein condensation in generalised d dimensions

The density of bosonic states are calculated for spinless free massive bosons in generalised d dimensions. The number of bosons are calculated in the lowest energy state. The Bose Einstein condensation was found in generalised dimensions (on and above d = 3) and the condensation temperature was observed to drop abruptly above three dimensions and decreases monotonically as the dimensionalities of the system increases. The rate of fall of the condensation temperature decreases as the dimensionality increases. This article is aimed to the University graduate students.
Thermally correlated states in loop quantum gravity

We study a class of loop-quantum-gravity states characterized by (ultra-local) thermal correlations that reproduce some features of the ultraviolet structure of the perturbative quantum field theory vacuum. In particular, they satisfy an analog of the Bisognano–Wichmann theorem. These states are peaked on the intrinsic geometry and admit a semiclassical interpretation. We study how the correlations extend on the spin network beyond the ultra local limit.
Stein’s method in high dimensions with applications

Let $h$ be a three times partially differentiable function on $R^n$, let $X=(X_1,\dots,X_n)$ be a collection of real-valued random variables and let $Z=(Z_1,\dots,Z_n)$ be a multivariate Gaussian vector. In this article, we develop Stein's method to give error bounds on the difference $E h(X) - E h(Z)$ in cases where the coordinates of $X$ are not necessarily independent, focusing on the high dimensional case $n\to\infty$. In order to express the dependency structure we use Stein couplings, which allows for a broad range of applications, such as classic occupancy, local dependence, Curie-Weiss model etc. We will also give applications to the Sherrington-Kirkpatrick model and last passage percolation on thin rectangles.