Miracle-dz/UniFAR-FTUs huggingface dataset:
X-ray-Underluminous Active Galactic Nuclei Relative to Broad Emission Lines in Ultraluminous Infrared Galaxies

We present X-ray spectra of four ultraluminous infrared galaxies (ULIRGs) with detectable broad near-infrared emission lines produced by active galactic nuclei (AGNs): Mrk 463, PKS 1345+12, IRAS 05189-2524, and IRAS 07598+6508. With the exception of IRAS 07598+6508, high-quality X-ray spectra obtained with XMM or Chandra show modest (30–340 eV) equivalent widths of the 6.4 keV Fe Kα emission line and clear signatures for absorption at a level of 4–33 × 1022 cm-2 for the main power-law components from the AGNs. These spectral properties are typical of Compton-thin AGNs, and so we estimate absorption-corrected 2–10 keV X-ray luminosities for the AGNs, LX(2–10 keV) using the Compton-thin assumption. We compare the LX(2–10 keV) values with broad optical/near-infrared emission-line luminosities and confirm a previous finding by Imanishi &Ueno that the LX(2–10 keV) to broad emission-line luminosity ratios in ULIRGs are systematically lower than those of moderately infrared-luminous type 1 AGNs. A comparison of independent energy diagnostic methods suggests that the AGNs are underluminous in the 2–10 keV band with respect to their overall spectral energy distributions, as opposed to the broad emission lines being overluminous. This X-ray underluminosity should be taken into account when using 2–10 keV X-ray data to investigate the energetic contribution from AGNs to the large infrared luminosities of ULIRGs.
QUANTUM DECOHERENCE IN DISORDERED MESOSCOPIC SYSTEMS

We point out that the low temperature saturation of the electron phase decoherence time in a disordered conductor can be explained within the existing theory of weak localization provided the effect of quantum (high frequency) fluctuations is taken into account. Making use of the fluctuation-dissipation theorem we evaluate the quantum decoherence time, the crossover temperature below which thermal effects become unimportant, and the weak localization correction $\ensuremath{\delta}\ensuremath{\sigma}$ at $T\phantom{\rule{0ex}{0ex}}=\phantom{\rule{0ex}{0ex}}0$. For 1D systems the latter is found to be $\ensuremath{\delta}\ensuremath{\sigma}/\ensuremath{\sigma}\ensuremath{\propto}1/\sqrt{N}$, where $N$ is the number of conducting channels.
Comparative analysis of turbulent effects on thermal plasma characteristics inside the plasma torches with rod- and well-type cathodes

The thermal plasma characteristics inside the two non-transferred plasma torches with rod-type cathode (RTC) and well-type cathode (WTC) are analysed in conjunction with turbulent effects on them in the atmospheric-pressure conditions. A control volume method and a modified semi-implicit pressure linked equations revised algorithm are used for solving the governing equations, i.e. conservation equations of mass, momentum, and energy together with a current continuity equation for arc discharge. A cold flow analysis is introduced to find the cathode spot position in the WTC torch, and both the laminar and turbulent models are employed to gain a physical insight into the turbulent effects on the thermal plasma characteristics produced inside the two torches. The numerical analysis for an RTC torch shows that slightly different values of plasma temperature and velocity between the laminar and turbulent calculations occur and the radial temperature profiles are constricted at the axis with increasing the gas flow rate, and that the large turbulent viscosities appear mostly near the anode wall. These calculated results indicate that the turbulent effects on the thermal plasma characteristics are very weak in the whole discharge region inside the RTC torch. On the other hand, the calculated results of the two numerical simulations for a WTC torch present that the significantly different values of plasma characteristics between the two models appear in the whole torch region and the plasma temperatures decrease with increasing the gas flow rate because the relatively strong turbulent effects are prevailing in the entire interior region of the WTC torch. From the comparisons of plasma net powers calculated and measured in this work, the turbulent modelling turns out to provide the more accurately calculated results close to the measured ones compared with the laminar one, especially for the torch with WTC. This is because the turbulent effects are considerably strong in the WTC torch and subsequently govern the thermal plasma characteristics inside it.
Tornado Formation from Downdraft Interaction In the FACE Mesonetwork

Abstract A tornado observed on 15 June 1973 in the FACE surface mesonetwork was studied on the mesoscale and cloud scale. Downdrafts from two preexisting cumulonimbi, initially 80 km apart, met along a north-south line in the center of the mesonet 30 min before tornado formation. Fed by the convergence of flow from the outflows of the predecessor cumulonimbi, a line of deep cumuli formed and developed rapidly. A tornado was observed as it dropped from this cumulus line. When the tornado dissipated 10 min later, heavy precipitation was reaching the surface and new outflow began to spread from the now vigorous cumulonimbus that had spawned the tornado. The life cycle of the tornado and a period of 90 rain surrounding its occurrence studied in detail from observed surface winds, radar reflectivity and surface rain gage data. The evolution of the parent cloud and tornado in a tropical thermodynamic environment with local forcing, weak shear and winds, and a potentially unstable sounding contrasts with the con.
Phase transitions of a GUP-corrected Schwarzschild black hole within isothermal cavities

We investigate the impact of the generalized uncertainty principle to all orders in the Planck length on thermodynamics parameters and on the stability of the Schwarzschild black hole within isothermal cavities. Using the Euclidean action formalism, the thermodynamics properties of the black hole are derived with important corrections compared to the standard case. In particular, we find that the black hole remnant is unstable and may decay to a stable large black hole via a phase transition of first order.
Scene-based wavefront correction with spatial light modulators

Spatial light modulators (SLM) are used in different microscopy setups. Examples are optical tweezers, programmable phase contrast imaging, confocal imaging, and aberration correction. We report on a method that measures and corrects specimen-induced aberrations in wide-field microscopy without additional optical components (e.g. Shack-Hartmann sensors) by taking advantage of the SLM that is already used in the setup. Different local gratings are written into the SLM which is positioned in a plane conjugate to the pupil of the imaging system. Multiple images are recorded and based on the shift of subimages we deduce the wavefront. We demonstrate first experimental results of this method for a system using a high resolution LCoS modulator.
A Simulation of the Intracluster Medium With Feedback from Cluster Galaxies

We detail method and report first results from a three-dimensional hydrodynamical and N-body simulation of the formation and evolution of a Coma-sized cluster of galaxies, with the intent of studying the history of the hot, X-ray emitting intracluster medium. Cluster gas, galaxies, and dark matter are included in the model. The galaxies and dark matter fell gravitational forces; the cluster gas also undergoes hydrodynamical effects such as shock heating and PdV work. For the first time in three dimensions, we include modeling of ejection of processed gas from the simulated galaxies by winds, including heating and heavy element enrichment. For comparison, we employ a `pure infall' simulation using the same initial conditions but with no galaxies or winds. We employ an extreme ejection history for galactic feedback in order to define the boundary of likely models. As expected, feedback raises the entropy of the intracluster gas, preventing it from collapsing to densities as high as those attained in the infall model. The effect is more pronounced in subclusters formed at high redshift. The cluster with feedback is always less X-ray luminous, but experiences more rapid luminosity evolution, than the pure infall cluster. Even employing an extreme ejection model, the final gas temperature is only approximately 15% larger than in the infall model. The radial temperature profile is very nearly isothermal within 1.5 Mpc. The cluster galaxies in the feedback model have a velocity dispersion approximately 15% lower than the dark matter. This results in the true ratio of specific energies in galaxies to gas being less than one, beta(sub spec) approximately 0.7. The infall model predicts beta(sub spec) approximately 1.2. Large excursions in these values occur over time, following the complex dynamical history of the cluster. The morphology of the X-ray emission is little affected by feedback. The emission profiles of both clusters are well described by the standard beta-model with beta(sub fit) approximately equal to 0.7 - 0.9. X-ray mass estimates based on the assumptions of hydrostatic equilibrium and the applicability of the beta-model are quite accurate in both cases. A strong, radial iron abundance gradient is present, which develops as a consequence of the steepening of the galaxy density profile over time. Spectroscopic observations using nonimaging detectors with wide (approximately 45 min) fields of view dramatically smear the gradient. Observations with arcminute resolution, made available with the ASCA satellite, would readily resolve the gradient.
The X-ray luminosity function of galaxies in the Coma cluster

The XMM-Newton survey of the Coma cluster of galaxies covers an area of 1.86 square degrees with a mosaic of 16 pointings and has a total useful integration time of 400 ks. Detected X-ray sources with extent less than 10 �� were correlated with cataloged galaxies in the Coma cluster region. The redshift information, which is abundant in this region of the sky, allowed us to separate cluster members from background and foreground galaxies. For the background sources, we recover a typical LogN − LogS in the flux range 10 −15 −10 −13 ergs s −1 cm −2 in the 0.5−2.0 keV band. The X-ray emission from the cluster galaxies exhibits X-ray colors typical of thermal emission. The luminosities of Coma galaxies lie in the 10 39 −10 41 ergs s −1 interval in the 0.5−2.0 keV band. The luminosity function of Coma galaxies reveals that their X-ray activity is suppressed with respect to the field by a factor of 5.6, indicating a lower level of X-ray emission for a given stellar mass.
Gravity and Nongravity Modes in the VIRMOS-DESCART Weak-Lensing Survey

We analyze the weak-lensing data of the VIRMOS imaging survey using projections (called E- and B-modes) of the two independent observable correlation functions. The E-mode contains all the lensing signal, while noise and systematics contribute equally to the E-and B-modes provided that intrinsic alignment is negligible. The mode separation allows a measurement of the signal with smaller error bars and a separate channel to test for systematic errors. We apply various transformations, including a spherical harmonic space power spectrum C and C, which provides a direct measurement of the projected dark matter distribution for 500 < l < 104.
Metric redefinitions in Einstein-Aether theory

'Einstein-Aether' theory, in which gravity couples to a dynamical, timelike, unit-norm vector field, provides a means for studying Lorentz violation in a generally covariant setting. Demonstrated here is the effect of a redefinition of the metric and 'aether' fields in terms of the original fields and two free parameters. The net effect is a change of the coupling constants appearing in the action. Using such a redefinition, one of the coupling constants can be set to zero, simplifying studies of solutions of the theory.
Atomistic simulations of dislocation mobility in Al, Ni and Al/Mg alloys

Dislocation velocities and mobilities are studied using molecular dynamics simulations for edge and screw dislocations in pure aluminium and nickel, and edge dislocations in Al–2.5%Mg and Al–5.0%Mg random substitutional alloys using EAM potentials. In the pure materials, the velocities of all dislocations are close to linear with the ratio of (applied stress)/(temperature) at low velocities consistent with phonon drag models, and quantitative agreement with the experiment is obtained for the mobility in Al. At higher velocities, different behaviour is observed. The edge dislocation velocity remains dependent solely on (applied stress)/(temperature) up to approximately 1.0 MPa K−1, and approaches a plateau velocity that is lower than the smallest ‘forbidden’ speed predicted by continuum models. In contrast, above a velocity around half of the smallest continuum wave speed, the screw dislocation damping has a contribution dependent solely on stress with a functional form close to that predicted by a radiation damping model of Eshelby. At the highest applied stresses, there are several regimes of nearly constant (transonic) velocity separated by velocity gaps in the vicinity of forbidden velocities; various modes of dislocation disintegration and destabilization were also encountered in this regime. In the alloy systems, there is a temperature- and concentration-dependent pinning regime where the velocity drops sharply below the pure metal velocity. Above the pinning regime but at moderate stresses, the velocity is again linear in (applied stress)/(temperature) but with a lower mobility than in the pure metal.
Electronic structure, elastic properties, surface energies, and work functions of NiGe and PtGe within the framework of density-functional theory for various surface terminations

We present a comprehensive theoretical study of the electronic structure, elastic properties, surface energies, and work functions of $\mathrm{NiGe}$ and $\mathrm{PtGe}$ within the framework of density functional theory (DFT). Our calculated lattice constants are within 1\char21{}2% of recently reported experimental values. Calculated work functions for the (001) surfaces of $\mathrm{NiGe}$ and $\mathrm{PtGe}$ are 4.57 and $4.83\phantom{\rule{0.3em}{0ex}}\mathrm{eV}$, respectively, suggesting that both metals and their alloys can be used as self-aligned contacts to $p$-type germanium. We identify the growth conditions necessary to stabilize this orientation. We report on an unusual surface reconstruction of the $\mathrm{NiGe}(101)\text{\char21{}}\mathrm{Ge}$-terminated surface.
Viscoelastic flow in a periodically constricted tube: The combined effect of inertia, shear thinning, and elasticity

The flow of a shear‐thinning viscoelastic fluid (Separan AP‐30) through a periodically constricted tube (PCT) is simulated using a mixed pseudospectral finite difference numerical method and a variety of constitutive equations. The results obtained with viscoelastic models show, at best, a small increase in the flow resistance beyond the value computed for a purely viscous inelastic fluid. The largest increase was observed with the modified Phan‐Thien–Tanner model. This model, in addition to fitting the standard viscometric data (viscosity and first normal stress difference), predicts a nonzero second normal stress difference and allows for dynamic behavior characterized by nonaffine deformation and stress overshoot in start‐up of shear flow. All the calculated values, although they show the correct tendency, are well below the experimentally measured values of Deiber and Schowalter (1981).
A Wide Field Planetary Camera 2 Study of the Resolved Stellar Population of the Pegasus Dwarf Irregular Galaxy (DDO 216)

The stellar population of the Pegasus dwarf irregular galaxy is investigated in images taken in the F439W (B), F555W (V), and F814W (I) bands with the Wide Field Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. With WFPC2 the Pegasus dwarf is highly resolved into individual stars to limiting magnitudes of about 25.5 in B and V and 25 in I. These and ground-based data are combined to produce color-magnitude diagrams that show the complex nature of the stellar population in this small galaxy. A young (<0.5 Gyr) main-sequence stellar component is present and clustered in two centrally located clumps, while older stars form a more extended disk or halo. The colors of the main sequence require a relatively large extinction of AV = 0.47 mag. The mean color of the well-populated red giant branch (RGB) is relatively blue, consistent with a moderate-metallicity young, or older metal-poor, stellar population. The RGB also has significant width in color, implying a range of stellar ages and/or metallicities. A small number of extended asymptotic giant branch stars are found beyond the RGB tip. Near the faint limits of our data is a populous red clump superposed on the RGB. Efforts to fit self-consistent stellar population models based on the Geneva stellar evolutionary tracks yield a revised distance of 760 kpc. Quantitative fits to the stellar population are explored as a means of constraining the star formation history. The numbers of main-sequence and core helium burning blue-loop stars require that the star formation rate was higher in the recent past, by a factor of 3–4 about 1 Gyr ago. Unique results cannot be obtained for the star formation history over longer time baselines without better information on stellar metallicities and deeper photometry. The youngest model consistent with the data contains stars with constant metallicity of Z = 0.001 that mainly formed 2–4 Gyr ago. If stellar metallicity declines with increasing stellar age, then older ages are allowed of up to ≈8 Gyr. However, even at its peak of star-forming activity, the intermediate-age–dominated model for the Pegasus dwarf most likely remained relatively dim, with MV ≈ -14.
PHASE TRANSITIONS IN A FOREST-FIRE MODEL

We investigate a forest-fire model with the density of empty sites as a control parameter. The model exhibits three phases, separated by one first-order phase transition and one ``mixed'' phase transition which shows critical behavior on only one side and hysteresis. The critical behavior is found to be that of the self-organized critical forest-fire model [B. Drossel and F. Schwabl, Phys. Rev. Lett. 69, 1629 (1992)], whereas in the adjacent phase one finds the spiral waves of the Bak, Chen, and Tang forest-fire model [P. Bak, K. Chen, and C. Tang, Phys. Lett. A 147, 297 (1990)]. In the third phase one observes clustering of trees with the fire burning at the edges of the clusters. The relation between the density distribution in the spiral state and the percolation threshold is explained and the implications for stationary states with spiral waves in arbitrary excitable systems are discussed. Furthermore, we comment on the possibility of mapping self-organized critical systems onto ``ordinary'' critical systems.
Integrable Matrix Product States from boundary integrability

We consider integrable Matrix Product States (MPS) in integrable spin chains and show that they correspond to “operator valued” solutions of the so-called twisted Boundary Yang-Baxter (or reflection) equation. We argue that the integrability condition is equivalent to a new linear intertwiner relation, which we call the “square root relation”, because it involves half of the steps of the reflection equation. It is then shown that the square root relation leads to the full Boundary Yang-Baxter equations. We provide explicit solutions in a number of cases characterized by special symmetries. These correspond to the “symmetric pairs” (SU(N),SO(N)) and (SO(N),SO(D)\otimes⊗SO(N-D)), where in each pair the first and second elements are the symmetry groups of the spin chain and the integrable state, respectively. These solutions can be considered as explicit representations of the corresponding twisted Yangians, that are new in a number of cases. Examples include certain concrete MPS relevant for the computation of one-point functions in defect AdS/CFT.
Landau transport equations in a slave-boson mean-field theory of the t − J model

In this paper we generalize slave-boson mean-field theory for $t\ensuremath{-}J$ model to the time-dependent regime, and derive transport equations for $t\ensuremath{-}J$ model, both in the normal and superconducting states. By eliminating the boson and constraint fields exactly at zero temperature in the linear-response regime we obtain a set of transport equations for physical electrons which have the same form as Landau transport equations for normal Fermi liquid and Fermi-liquid superconductor, respectively, with all Landau parameters explicitly given. Our theory can be viewed as a refined version of U(1) Gauge theory where all lattice effects are retained and strong correlation effects are reflected as strong Fermi-liquid interactions in the transport equation. Some experimental consequences are discussed.
Magnetic properties of the itinerant metamagnetic system Co ( S 1 − x Se x ) 2 under high magnetic fields and high pressure

The magnetization of the $\mathrm{Co}({\mathrm{S}}_{1\ensuremath{-}x}{\mathrm{Se}}_{x}{)}_{2}$ system with $0l~xl~0.2$ has been measured under high magnetic fields and high pressure. Ferromagnetic ${\mathrm{CoS}}_{2}$ exhibits a second-order transition at ${T}_{c}=122\mathrm{K}. $ Substitution of 10% Se for S in ${\mathrm{CoS}}_{2}$ reduces the Curie temperature to ${T}_{c}=27\mathrm{K}$ and the transition to first order. $\mathrm{Co}({\mathrm{S}}_{1\ensuremath{-}x}{\mathrm{Se}}_{x}{)}_{2}$ with $0.12l~x$ becomes an exchange-enhanced Pauli paramagnet. The itinerant metamagnetic transition has been observed in the paramagnet. ${\mathrm{C}\mathrm{o}(\mathrm{S}}_{0.9}{\mathrm{Se}}_{0.1}{)}_{2}$ also shows a transition just above ${T}_{c}. $ Using the experimental data, the magnetic phase diagram of $\mathrm{Co}({\mathrm{S}}_{1\ensuremath{-}x}{\mathrm{Se}}_{x}{)}_{2}$ is determined. With increasing pressure, the Curie temperature of ${\mathrm{CoS}}_{2}$ decreases and the ferromagnetic transition changes to first order at $P\ensuremath{\approx}0.4\mathrm{GPa}. $ In the pressure regime of the first-order transition $Pg0.4\mathrm{GPa},$ the metamagnetic transition is observed just above ${T}_{c}. $ In ${\mathrm{C}\mathrm{o}(\mathrm{S}}_{0.9}{\mathrm{Se}}_{0.1}{)}_{2},$ the ferromagnetism disappears at 0.25 GPa and paramagnetism appears. The observed magnetic properties and the magnetic phase diagram of $\mathrm{Co}({\mathrm{S}}_{1\ensuremath{-}x}{\mathrm{Se}}_{x}{)}_{2}$ can be qualitatively described with a theory of the itinerant electron metamagnetism at finite temperatures.