Miracle-dz/UniFAR-FTUs huggingface dataset:
Quantum interference in the spin-polarized heavy fermion compound CeB6: Evidence for topological deformation of the Fermi surface in strong magnetic fields

We report susceptibility experiments in magnetic fields up to 60thinspthinspT and show conclusively that the de Haas{endash}van Alphen oscillations originate from a single spin Fermi surface. New observed frequencies present in magnetic breakdown and quantum interference oscillations indicate that the Fermi-surface topology changes as a function of the applied field while maintaining a constant volume. These results are not expected from the Anderson lattice model. {copyright} {ital 1998} {ital The American Physical Society}
Multiplexed holographic aperture masking with liquid-crystal geometric phase masks

Sparse Aperture Masking (SAM) allows for high-contrast imaging at small inner working angles, however the performance is limited by the small throughput and the number of baselines. We present the concept and first lab results of Holographic Aperture Masking (HAM) with extreme liquid-crystal geometric phase patterns. We multiplex subapertures using holographic techniques to combine the same subaperture in multiple non-redundant PSFs in combination with a non-interferometric reference spot. This way arbitrary subaperture combinations and PSF configurations can be realized, giving HAM more uv-coverage, better throughput and improved calibration as compared to SAM, at the cost of detector space.
Measurements of magnetic fields over the pulsation cycle in six roAp stars with FORS 1 at the VLT

Received xx/Accepted yy Abstract. With FORS1 at the VLT we have tried for the first time to measure the magnetic field variation over the pulsation cycle in six roAp stars to begin the study of how the magnetic field and pulsation interact. For the star HD101065, which has one of the highest photometric pulsation amplitudes of any roAp star, we found a signal at the known photometric pulsation frequency at the 3� level in one data set; however this could not be confirmed by later observations. A preliminary simple calculation of the expected magnetic variations over the pulsation cycle suggests that they are of the same order as our current noise levels, leading us to expect that further observations with increased S/N have a good chance of achieving an unequivocal detection.
MC3D-simulating polarization maps and more

MC3D is a three-dimensional, self-consistent continuum radiative transfer code. It can be used to determine the spatial temperature distribution in arbitrary dust/electron configurations, such as around young stellar objects or active galactic nuclei. Based on this temperature distribution, MC3D allows calculation of polarization maps, images, and spectral energy distributions. We present the numerical techniques applied in this code, describe its capabilities, and show instructive examples of previous applications.
In-medium viscous coefficients of a hot hadronic gas mixture

We estimate the shear and the bulk viscous coefficients for a hot hadronic gas mixture constituting of pions and nucleons. The viscosities are evaluated in the relativistic kinetic theory approach by solving the transport equation in the relaxation time approximation for binary collisions ($\pi\pi$,$\pi N$ and $NN$). Instead of vacuum cross-sections usually used in the literature we employ in-medium scattering amplitudes in the estimation of the relaxation times. The modified cross-sections for $\pi\pi$ and $\pi N$ scattering are obtained using one-loop modified thermal propagators for $\rho$, $\sigma$ and $\Delta$ in the scattering amplitudes which are calculated using effective interactions. The resulting suppression of the cross sections at finite temperature and baryon density is observed to significantly affect the $T$ and $\mu_N$ dependence of the viscosities of the system.
3D modeling of electric fields in the LUX detector

This work details the development of a three-dimensional (3D) electric field model for the LUX detector. The detector took data to search for weakly interacting massive particles (WIMPs) during two periods. After the first period completed, a time-varying non-uniform negative charge developed in the polytetrafluoroethylene (PTFE) panels that define the radial boundary of the detector's active volume. This caused electric field variations in the detector in time, depth and azimuth, generating an electrostatic radially-inward force on electrons on their way upward to the liquid surface. To map this behavior, 3D electric field maps of the detector's active volume were generated on a monthly basis. This was done by fitting a model built in COMSOL Multiphysics to the uniformly distributed calibration data that were collected on a regular basis. The modeled average PTFE charge density increased over the course of the exposure from -3.6 to −5.5 μC/m2. From our studies, we deduce that the electric field magnitude varied locally while the mean value of the field of ∼200 V/cm remained constant throughout the exposure. As a result of this work the varying electric fields and their impact on event reconstruction and discrimination were successfully modeled.
Gauge-invariant Variables and Entanglement Entropy

The entanglement entropy (EE) of gauge theories in three spacetime dimensions is analyzed using manifestly gauge-invariant variables defined directly in the continuum. Specifically, we focus on the Maxwell, Maxwell-Chern-Simons (MCS), and nonabelian Yang-Mills theories. Special attention is paid to the analysis of edge modes and their contribution to EE. The contact term is derived without invoking the replica method and its physical origin is traced to the phase space volume measure for the edge modes. The topological contribution to the EE for the MCS case is calculated. For all the abelian cases, the EE presented in this paper agrees with known results in the literature. The EE for the nonabelian theory is computed in a gauge-invariant gaussian approximation, which incoprorates the dynamically generated mass gap. A formulation of the contact term for the nonabelian case is also presented.
The Soft Gamma-Ray Spectral Variability of Cygnus X-1

We have used observations of Cyg X-1 from the Compton Gamma Ray Observatory and BeppoSAX to study the variation in the MeV γ-ray emission between the hard and soft spectral states, using spectra that cover the energy range from 20 keV up to 10 MeV. These data provide evidence for significant spectral variability at energies above 1 MeV. In particular, whereas the hard X-ray flux decreases during the soft state, the flux at energies above 1 MeV increases, resulting in a significantly harder γ-ray spectrum at energies above 1 MeV. This behavior is consistent with the general picture of galactic black hole candidates having two distinct spectral forms at soft γ-ray energies. These data extend this picture, for the first time, to energies above 1 MeV. We have used two different hybrid thermal/nonthermal Comptonization models to fit broadband spectral data obtained in both the hard and soft spectral states. These fits provide a quantitative estimate of the electron distribution and allow us to probe the physical changes that take place during transitions between the low and high X-ray states. We find that there is a significant increase (by a factor of ~4) in the bolometric luminosity as the source moves from the hard state to the soft state. Furthermore, the presence of a nonthermal tail in the Comptonizing electron distribution provides significant constraints on the magnetic field in the source region.
A REVIEW ON PRIVACY POLICY DESIGN FOR USER’S UPLOADED IMAGES ON CONTENT SHARING SITES

: With the rising volume of pictures clients share through friendly destinations, keeping up with security has turned into a significant issue, as exhibited by a new influx of advertised occurrences where clients accidentally shared individual data. Considering these occurrences, the need of instruments to assist clients with controlling admittance to their common substance is evident. Toward tending to this need, we propose an Adaptive Privacy Policy Prediction (A3P) framework to assist clients with forming security settings for their pictures. We look at the job of social setting, picture content, and metadata as potential signs of clients' protection inclinations. We propose a two-level system which as indicated by the client's accessible history on the site, decides the best accessible security strategy for the client's pictures being transferred. Our answer depends on a picture order system for picture classifications which might be related with comparable arrangements, and on an approach expectation calculation to consequently create a strategy for each recently transferred picture, likewise as per clients' social highlights. Over the long run, the produced strategies will follow the advancement of clients' protection mentality. We give the aftereffects of our broad assessment north of 5,000 strategies, which exhibit the adequacy of our framework, with expectation exactnesses more than 90%.
Superconductivity and crystalline electric field effects in the filled skutterudite series Pr ( Os 1 − x Ru x ) 4 Sb 12

X-ray powder-diffraction, magnetic-susceptibility Χ (T), and electrical resistivity ρ(T) measurements were made on single crystals of the filled skutterudite series Pr(Os 1 - x Ru x ) 4 Sb 1 2 . One end of the series (x=0) isa heavy fermion superconductor with a superconducting critical temperature T c =1.85 K, while the other end (x= I ) is a conventional superconductor with T c 1 K. The lattice constant a decreases approximately linearly with increasing Ru concentration x. As Ru (Os) is substituted for Os (Ru), T c decreases nearly linearly with substituent concentration and exhibits a minimum with a value of T c = 0.75 K at x=0.6, suggesting that the two types of superconductivity compete with one another. Crystalline electric field effects in Χ d c (T) and ρ(T) due to the splitting of the Pr 3 + ninefold degenerate Hund's rule J=4 multiplet are observed throughout the series, with the splitting between the ground state and the first excited state increasing monotonically as x increases. The fits to the Χ d c (T) and ρ(T) data are consistent with a Γ 3 doublet ground state for all values of x, although reasonable fits can be obtained for a Γ 1 ground state for x values near the end member compounds (x = 0 or x = 1).
Polaritonic hybrid-epsilon-near-zero modes: engineering strong optoelectronic coupling and dispersion in doped cadmium oxide bilayers.

Polaritonic materials that support epsilon-near-zero (ENZ) modes offer the opportunity to design light-matter interactions at the nanoscale through phenomena like resonant perfect absorption and extreme sub-wavelength light concentration. To date, the utility of ENZ modes is limited in propagating polaritonic systems by a relatively flat spectral dispersion, which gives ENZ modes small group velocities and short propagation lengths. Here we overcome this constraint by coupling ENZ modes to surface plasmon polariton (SPP) modes in doped cadmium oxide ENZ-on-SPP bilayers. What results is a strongly coupled hybrid mode, characterized by strong anti-crossing and a large spectral splitting on the order of 1/3 of the mode frequency. The resonant frequencies, dispersion, and coupling of these polaritonic-hybrid-epsilon-near-zero (PH-ENZ) modes are controlled by tailoring the modal oscillator strength and the ENZ-SPP spectral overlap, which can potentially be utilized for actively tunable strong coupling at the nanoscale. PH-ENZ modes ultimately leverage the most desirable characteristics of both ENZ and SPP modes through simultaneous strong interior field confinement and mode propagation.
HIDEEP – an extragalactic blind survey for very low column‐density neutral hydrogen

We have earned out an extremely long integration time (9000 s beam - 1 ) 21-cm blind survey of 60 deg 2 in Centaurus using the Parkes multibeam system. We find that the noise continues to fall as √t o b s throughout, enabling us to reach an HI column-density limit of 4.2 x 10 1 8 cm - 2 for galaxies with a velocity width of 200 km s - 1 in the central 32 deg 2 region, making this the deepest survey to date in terms of column density sensitivity. The H i data are complemented by very deep optical observations from digital stacking of multi-exposure UK Schmidt Telescope R-band films, which reach an isophotal level of 26.5 R mag arcsec - 2 (≃27.5 B mag arcsec - 2 ). 173 Hi sources have been found, 96 of which have been uniquely identified with optical counterparts in the overlap area. There is not a single source without an optical counterpart. Although we have not measured the column densities directly, we have inferred them from the optical sizes of their counterparts. All appear to have a column density of N H 1 = 10 2 0 . 6 5 ′ 0 . 3 8 . This is at least an order of magnitude above our sensitivity limit, with a scatter only marginally larger than the errors on N H 1 . This needs explaining. If confirmed it means that H 1 surveys will only find low surface brightness (LSB) galaxies with high M H 1 /L B . Gas-rich LSB galaxies with lower HI mass to light ratios do not exist. The paucity of low column-density galaxies also implies that no significant population will be missed by the all-sky H 1 surveys being carried out at Parkes and Jodrell Bank.
The hard X-ray view of the low-luminosity blazar in the radio galaxy NGC6251

We present results from a BeppoSAX (July 2001) observation of the FR I radio galaxy NGC 6251, together with a re-analysis of archival ASCA (October 1994) and Chandra (September 2000) data. The weak detection above 10 keV and the lack of iron ﬂuorescent K α emission lines in the BeppoSAX spectrum rule out that the bulk of the X-ray emission is due to an obscured Seyfert nucleus. The study of the multiwavelength spectral energy distribution suggests instead that X-rays probably originate as inverse-Compton of synchrotron seed photons in a relativistic jet, indicating that NGC 6251 hosts a low radio luminosity ( L 5 GHz ∼ 10 40 erg s − 1 ) blazar. The BeppoSAX spectrum is ﬂatter than in the earlier ASCA observation. This might be due to the emergence of a diﬀerent spectral component during phases of lower X-ray ﬂux. In this context, we discuss some possible explanations for the intense and mildly-ionized ﬂuorescent iron line measured by ASCA.
Correlation between Magnetic Properties and Depinning Field in Field-Driven Domain Wall Dynamics in GdFeCo Ferrimagnets

The influence of temperature on the magnetic-field-driven domain wall (DW) motion is investigated in GdFeCo ferrimagnets with perpendicular magnetic anisotropy (PMA). We find that the depinning field strongly depends on temperature. Moreover, it is also found that the saturation magnetization exhibits a similar dependence on temperature to that of depinning field. From the creep-scaling criticality, a simple relation between the depinning field and the properties of PMA is clearly identified theoretically as well as experimentally. Our findings open a way for a better understanding how the magnetic properties influence on the depinning field in magnetic system and would be valuably extended to depinning studies in other system.
Dipole of the luminosity distance as a test for dark energy models

The dependence of Hubble parameter on redshift can be determined directly from the dipole of luminosity distance to Supernovae Ia. We investigate the possibility of using the data on dipole of the luminosity distance obtained from the Supernovae Ia compilations SDSS, Union2.1, JLA and Pantheon to distinguish the dark energy models.
Dependence of nonlinear refractive index of ZnSe on Be and Mg content

The values of the nonlinear refractive index n2 and the two-photon absorption coefficient β of ternary and quaternary ZnSe-based mixed crystals were extracted from the standard backward degenerate four wave mixing (DFWM) and nonlinear transmission measurements at 532 nm, respectively. Studied crystals were grown by the modified high-pressure Bridgman method. We found that the value of the nonlinear refractive index n2 for Zn0.79Be0. 21Se is higher than that for Zn0.80Mg0. 20Se. However, the opposite behaviour was found in the case of two-photon absorption coefficient β for these compounds. We also found that the values of the nonlinear refractive index n2 and the two-photon absorption coefficient β for Zn0.83Be0. 04Mg0.13Se are about five times lower and three times higher than that for Zn0.80Mg0. 13Se, respectively. In the case of ternary ZnSe-based crystals we noticed that the value of the nonlinear refractive index n2 decreases with increasing Mg or Be content. However, the value of the two-photon absorption coefficient β increases with increasing Mg or Be content.
Group-theoretical classification of multipole order: Emergent responses and candidate materials

The multipole moment is an established concept of electrons in solids. Entanglement of spin, orbital, and sublattice degrees of freedom is described by the multipole moment, and spontaneous multipole order is a ubiquitous phenomenon in strongly correlated electron systems. In this paper, we present group-theoretical classification theory of multipole order in solids. Intriguing duality between the real space and momentum space properties is revealed for odd-parity multipole order which spontaneously breaks inversion symmetry. Electromagnetic responses in odd-parity multipole states are clarified on the basis of the classification theory. A direct relation between the multipole moment and the magnetoelectric effect, Edelstein effect, magnetopiezoelectric effect, and dichromatic electron transport is demonstrated. More than 110 odd-parity magnetic multipole materials are identified by the group-theoretical analysis. Combining the list of materials with the classification tables of multipole order, we predict emergent responses of the candidate materials.
ET Probes, Nodes, and Landbases: A Proposed Galactic Communications Architecture and Implied Search Strategies.

Land-based beacons, information laden probes sent into our solar system, and more distal communication nodes have each been proposed as the most likely means by which we might be contacted by ET. Each method, considered in isolation from ET's point of view, has limitations and flaws. An overarching galactic communication architecture that tethers together probes, nodes, and land bases is proposed to be a better overall solution. From this more efficient construct flows several conclusions: (a) Earth has been thoroughly surveilled, (b) Earth will be contacted in due course, (c) SETI beyond half the distance that Earth's EM has reached (~35-50 LY) is futile, and (d) the very quiescence of the galaxy paradoxically implies that that Drake's N = many, and that there is a system of galactic governance. Search strategies are proposed to detect the described probe-node-land base communications pathway.
Anchoring Magnetic Fields in Turbulent Molecular Clouds. II. From 0.1 to 0.01 pc

We compared the magnetic field directions inferred from polarimetry data obtained from 100 pc scale inter-cloud media (ICM) and from subparsec scale molecular cloud cores. The highly correlated result led us to conclude that cloud turbulence must be sub-Alfvénic. Here we extend the study with 0.01 pc cores observed by interferometers. The inferred field directions at this scale significantly deviate from that of the surrounding ICM. An obvious question to ask is whether this high-resolution result contradicts the sub-Alfvénic picture concluded earlier. We performed MHD simulations of a slightly super-critical (magnetic criticality = 2) clouds with Alfvénic Mach number MA = 0.63 (MA ≡ σV/VA , where σV and VA are, respectively, local 3D velocity dispersion and Alfvén velocity; means the average within the entire simulated volume; e.g., Burkhart et al. ), which can reproduce the Paper I results, and observed the development toward smaller scales. Interestingly, all subregions hosting cores with nH2 > 105/cc (the typical density observed by interferometers) possess MA = 2–3. Not too surprisingly, these slightly super-Alfvénic cores result in B-field orientation offsets comparable to the interferometer observations. The result suggests that gravity can concentrate (and maybe also contribute to, which requires further study to confirm) turbulent energy and create slightly super-Alfvénic cores out of sub-Alfvénic clouds. The results of our simulations also agree with the observed velocity-scale, mass-scale, and field-density relations.
A New Gravitational Lens Candidate with Large Image Separation in the SDSS DR5 Data

The discovery of a gravitational lens candidate is reported. The quasars SDSS J111611.73+411821.5 and SDSS J111610.68+411814.4 are recognized as two images of the same object, being strongly lensed by the closer galaxy SDSS J111611.03+411820.9. The source is located at a redshift of z~3, while the redshift of the lens galaxy is z~0.25. The separation of the images is large,~13 arcsec. Commonly used models of the mass distribution for the lens galaxy with values of the parameters in the expected range describe the positions and fluxes of the images.
On the numerical solution of a variable-coefficient Burgers equation arising in granular segregation

We study a variable-coefficient Burgers equation arising in the modelling of segregation of dry bidisperse granular mixtures. The equation is subject to nonlinear boundary conditions for the particle flux. We construct a strongly implicit Crank--Nicolson type of numerical scheme for the latter equation. The scheme is benchmarked against a standard exact solution of kink type, showing second-order of accuracy and good discrete conservation properties. Two segregation problems considered in the literature are then solved and discussed. The first is the case of a linear kinetic stress profile, which renders the governing equation of constant-coefficient type, while the second is the case of a variable kinetic stress profile based on an expression fit to particle dynamics simulation data.
A Unique Small-Scale Gravitational Arc in A1201

We present a snapshot Hubble Space Telescope (HST) image of the galaxy cluster A1201 (z = 0.169), revealing a tangential arc 2'' from the brightest cluster galaxy (BCG). Keck Echelle Spectrograph and Imager (ESI) spectroscopy confirms that the arc is gravitational in nature and that the source galaxy lies at z = 0.451. We construct a model of the gravitational potential of the cluster that faithfully reproduces the observed arc morphology. Despite the relaxed appearance of the cluster in the HST frame, the best-fit ellipticity of the total matter distribution is ϵtotal ≥ 0.5, in contrast to the light distribution of the BCG (ϵBCG = 0.23 ± 0.03) on 2'' scales. Further deep optical observations and pointed X-ray spectro-imaging observations with Chandra are required to determine whether this elongation is due to a single elongated dark matter halo or a more complex distribution of matter in the cluster core. We compare the arc with a sample drawn from the published literature and confirm that it is unique among tangential systems in the small physical scales that it probes (~6 kpc). In anticipation of a more thorough investigation of this cluster across a broad range of physical scales, we use our fiducial lens model to estimate the projected mass and mass-to-light ratio of the cluster within a radius of 6 kpc, obtaining M = (5.9) × 1011 M☉, M/LV = 9.4 (M/L)☉. Overall our results confirm the importance of HST snapshot surveys for identifying rare lensing constraints on cluster mass distributions. In combination with follow-up optical and X-ray observations, the arc in A1201 should help to increase our understanding of the physics of cluster cores.