Miracle-dz/UniFAR-FTUs huggingface dataset:
PANIC: a 3D dislocation dynamics model for climb and glide in epitaxial films and heterostructures

This paper presents PANIC, a 3D discrete mesoscale dislocation dynamics model which includes a fully quantitative treatment of both dislocation climb and dislocation glide, including climb driven by both osmotic and mechanical stresses and climb enabled by both bulk and pipe diffusion, including full elastic anisotropy for materials with hexagonal symmetry. Efficient calculations can be performed for epitaxial thin films, multilayers and device structures with free surfaces, including those with irregular geometries (e.g. islands). The model also includes the capability to simulate dislocation dynamics during the growth of the thin films or heterostructures. The model has been validated against experiment for thin films of GaN, AlN and AlGaN but is widely applicable to other material systems, both hexagonal and cubic.
ANISOTROPIC ACTIVE GALACTIC NUCLEUS OUTFLOWS AND ENRICHMENT OF THE INTERGALACTIC MEDIUM. II. METALLICITY

We investigate the large-scale influence of outflows from active galactic nuclei (AGNs) in enriching the intergalactic medium (IGM) with metals in a cosmological context. We combine cosmological simulations of large-scale structure formation with a detailed model of metal enrichment, in which outflows expand anisotropically along the direction of least resistance, distributing metals into the IGM. The metals carried by the outflows are generated by two separate stellar populations: stars located near the central AGN, and stars located in the greater galaxy. Using this algorithm, we performed a series of five simulations of the propagation of AGN-driven outflows in a cosmological volume of size (128 h−1 Mpc)3 in a ΛCDM universe, and analyze the resulting metal enrichment of the IGM. We found that the metallicity induced in the IGM is greatly dominated by AGNs having bolometric luminosity L>109L☉, sources with 108 < L/L☉ < 109 having a negligible contribution. Our simulations produced an average IGM metallicity of [O/H] = −5 at z = 5.5, which then rises gradually, and remains relatively flat at a value [O/H] = −2.8 between z = 2 and z = 0. The ejection of metals from AGN host galaxies by AGN-driven outflows is found to enrich the IGM to >10%–20% of the observed values, the number dependent on redshift. The enriched IGM volume fractions are small at z>3, then rise rapidly to the following values at z = 0: 6%–10% of the volume enriched to [O/H]> − 2.5, 14%–24% volume to [O/H]> − 3, and 34%–45% volume to [O/H]> − 4. At z ⩾ 2, there is a gradient of the induced enrichment, the metallicity decreasing with increasing IGM density, enriching the underdense IGM to higher metallicities, a trend more prominent with increasing anisotropy of the outflows. This can explain observations of the metal-enriched low-density IGM at z ∼ 3–4.
A DETAILED STUDY OF THE ACCRETION DISK SURROUNDING THE HIGH-MASS PROTOSTAR NGC 7538 S

We present deep high-angular resolution observations of the high-mass protostar NGC 7538 S, which is in the center of a cold dense cloud core with a radius of 0.5 pc and a mass of ∼2000 M☉. These observations show that NGC 7538 S is embedded in a compact elliptical core with a mass of 85–115 M☉. The star is surrounded by a rotating accretion disk, which powers a very young, hot molecular outflow approximately perpendicular to the rotating accretion disk. The accretion rate is very high, ∼(1.4–2.8) × 10−3 M☉ yr−1. Evidence for rotation of the disk surrounding the star is seen in all largely optically thin molecular tracers, H13CN J = 1 → 0, HN13C J = 1 → 0, H13CO+ J = 1 → 0, and DCN J = 3 → 2. Many molecules appear to be affected by the hot molecular outflow, including DCN and H13CO+. The emission from CH3CN, which has often been used to trace disk rotation in young high-mass stars, is dominated by the outflow, especially at higher K levels. Our new high angular resolution observations show that the rotationally supported part of the disk is smaller than we previously estimated. The enclosed mass of the inner, rotationally supported part of the disk (D ∼ 5″, i.e., 14,000 AU) is ∼14–24 M☉.
Near-Optimal Derandomization of Medium-Width Branching Programs

We give a deterministic white-box algorithm to estimate the expectation of a read-once branching program of length n and width w in space Õ(logn+√logn·logw). In particular, we obtain an almost optimal space Õ(logn) derandomization of programs up to width w=2√logn. Previously, the best known space complexity for this problem was O(min{logn· logw,log3/2n+√logn· logw}) via the classic algorithms of Savitch (JCSS 1970) and Saks and Zhou (JCSS 1999), which only achieve space Õ(logn) for w=polylog(n). We prove this result by showing that a variant of the Saks-Zhou algorithm developed by Cohen, Doron, and Sberlo (ECCC 2022) still works without executing one of the steps in the algorithm, the so-called random shift step. This allows us to extend their algorithm from computing the nth power of a w× w stochastic matrix to multiplying n distinct w× w stochastic matrices with no degradation in space consumption. In the regime where w≥ n, we also show that our approach can achieve parameters matching those of the original Saks-Zhou algorithm (with no loglog factors). Finally, we show that for w≤ 2√logn, an algorithm even simpler than our algorithm and that of Saks and Zhou achieves space O(log3/2 n).
Experience Rating as an Automatic Stabilizer

Unemployment-insurance taxes are experience rated, penalizing firms that dismiss workers. We examine whether experience rating serves as an automatic stabilizer in the labor market. Taking advantage of the variation in layoff penalties across states, we utilize detailed data on state tax schedules and assess whether firms are less responsive to labor-demand shocks when facing higher layoff penalties. Our findings show that average layoff penalties from UI reduce firm adjustments to negative shocks by 11%. This indicates that experience rating contributes to labor market stabilization. For example, during the Great Recession, experience rating preserved nearly a million jobs.
Exchange rate regimes and economic performance: Does CFA zone membership beneﬁt their economies?

: This paper aims to evaluate the importance and impact of CFA zone membership by distinguishing between the effects of being in monetary union from those which arose from anchoring the CFA franc. Using de jure and de facto regime classification schemes and a sample of 35 SSA countries over the 1985-2009 period, our results show that the CFA zone membership has been beneficial in terms of inflation, while it has not resulted in a significant effect on growth. Finally, we evidence that greater fiscal discipline can be associated with peg regimes in SSA, but not necessarily with monetary union. JEL
Institutional Characteristics and Its Effect on Public Health Service Delivery under Decentralization in Local Government Authorities in Tanzania

: This article examines the effects of institutional characteristics on public health service delivery under decentralisation in rural Tanzania. It adopted a cross sectional design to examine institutional characteristics and its effects on health service delivery at Pangani and Urambo Local Government Authorities (LGAs). Both qualitative and quantitative approaches were employed; primary data were collected by using interviews, questionnaires, FGDs and observation. The study established that, the instructional characteristics impaired significantly the decentralisation initiatives for improved health service delivery in the rural areas in Tanzania. Institutional characteristics, legal frame work, systems and administrative structures were the main hindrance in the implementation of decentralisation for improved health services and its delivery. The institutional effects resulted to poor health service delivery infrastructures in terms of equipments availability, drugs and medicines, health workers, distance, delayed service, time management, lack of accountability and transparency. The study recommends a review of the existing framework, administrative systems, structures and processes and human resource capacity building.
Using nmagic to probe the dark matter halo and orbital structure of the X-ray bright, massive elliptical galaxy, NGC 4649

We create dynamical models of the massive elliptical galaxy, NGC 4649, using the N-body made-to-measure code, NMAGIC, and kinematic constraints from long-slit and planetary nebula (PN) data. We explore a range of potentials based on previous determinations from X-ray observations and a dynamical model fitting globular cluster (GC) velocities and a stellar density profile. The X-ray mass distributions are similar in the central region but have varying outer slopes, while the GC mass profile is higher in the central region and on the upper end of the range further out. Our models cannot differentiate between the potentials in the central region, and therefore if non-thermal pressures or multi-phase components are present in the hot gas, they must be smaller than previously inferred. In the halo, we find that the PN velocities are sensitive tracers of the mass, preferring a less massive halo than that derived from the GC mass profile, but similar to one of the mass distributions derived from X-rays. Our results show that the GCs may form a dynamically distinct system, and that the properties of the hot gas derived from X-rays in the outer halo have considerable uncertainties that need to be better understood. Estimating the mass in stars using photometric information and a stellar population mass-to-light ratio, we infer a dark matter mass fraction in NGC 4649 of \tilde0.39 at 1R_e (10.5 kpc) and \tilde0.78 at 4R_e. We find that the stellar orbits are isotropic to mildly radial in the central \tilde6 kpc depending on the potential assumed. Further out, the orbital structure becomes slightly more radial along R and more isotropic along z, regardless of the potential assumed. In the equatorial plane, azimuthal velocity dispersions dominate over meridional velocity dispersions, implying that meridional velocity anisotropy is the mechanism for flattening the stellar system.
Thermal SZ fluctuations in the ICM: probing turbulence and thermodynamics in Coma cluster with Planck

We report the detection of thermal Sunyaev-Zeldovich effect (SZ) fluctuations in the intracluster medium (ICM) of Coma cluster observed with ${\it Planck}$. The SZ data links the maximum observable X-ray scale to the large Mpc scale, extending our knowledge of the power spectrum of ICM fluctuations. Deprojecting the 2-d SZ perturbations into 3-d pressure fluctuations, we find an amplitude spectrum which peaks at $\delta P/P = 33\pm 12\%$ and $74\pm19\%$ in the $15'$ and $40'$ radius region, respectively. We perform tests to ensure fluctuations are intrinsic to the cluster and not due to noise contamination. By using high-resolution hydrodynamical models, we improve the ICM turbulence constraints in Coma, finding 3-d Mach number ${\rm Ma_{3d}}= 0.8\pm0.3$ (15' region), increasing to supersonic values at larger radii (40'), and an injection scale $L_{\rm inj}\approx 500$ kpc. Such properties are consistent with driving due to mergers, in particular tied to internal galaxy groups. The large pressure fluctuations show that Coma is in adiabatic mode (mediated by sound waves), rather than isobaric mode (mediated by buoyancy waves). As predicted by turbulence models, the distribution of SZ fluctuations is log-normal with mild non-Gaussianities (heavy tails). The substantial non-thermal pressure support implies hydrostatic mass bias $b_M=-15\%$ to $-45\%$ from the core to the outskirt region, respectively. While total SZ power probes the thermal energy content, the SZ fluctuations constrain the non-thermal deviations important for precision cosmology. The proposed, novel approach can be exploited by multifrequency observations using ground based interferometers and future space CMB missions.
Superconformal generalization of the chaotic inflation model

A model of chaotic inflation based on the theory of a scalar field with potential λ4 perfectly matches the observational data if one adds to it a tiny non-minimal coupling to gravity with ξ0. 002. We describe embedding of this model into the superconformal theory with spontaneous breaking of superconformal symmetry, and into supergravity. A model with small ξ is technically natural: setting the small parameter ξ to zero leads to a point of enhanced symmetry in the underlying superconformal theory.
Considerations on Visitor Satisfaction as Part of an Integral Evaluation Methodology

This research article presents the application of a model of museum visitors’ satisfaction which was developed through visitor studies in four museums in Argentina. The model aimed to identify what influence the visitors’ own characteristics, as well as their perception of the experience the museum offers them, had on their overall satisfaction. Data was collected in two stages: one before the visit and another one immediately after. This process permitted the identification of certain common pat terns to all the case studies in relation to visitors’ satisfaction, a necessary condition to better understand their needs and behavior, in order to generate memorable experiences.
Renormalized vacuum polarization and stress tensor on the horizon of a Schwarzschild black hole threaded by a cosmic string

We calculate the renormalized vacuum polarization and stress tensor for a massless, arbitrarily coupled scalar field in the Hartle–Hawking vacuum state on the horizon of a Schwarzschild black hole threaded by an infinite straight cosmic string. This calculation relies on a generalized Heine identity for non-integer Legendre functions which we derive without using specific properties of the Legendre functions themselves.
Plate Tectonic Consequences of Competing Models for the Origin and History of the Banda Sea Subducted Oceanic Lithosphere

The Banda Arc, situated west of Irian Jaya and in the easternmost extension of the Sunda subduction zone system, reveals a characteristic bowl-shaped geometry in seismic tomographic images. This indicates that the oceanic lithosphere still remains attached to the surrounding continental margins of northern Australia and the Bird's Head microcontinent. Major controversies exist between authors proposing an allochthonous or autochthonous origin of the Bird's Head block. Either scenario has important implications for plate kinematic models aiming to reconstruct the tectonic evolution of the region and the late Jurassic seaoor spreading geometry of this now subducted Argo-Tanimbar-Seram (ATS) ocean basin. Wider implications affect the tectonic conguration of the Tethyan-Pacic realm, the distribution of plate boundaries as well as the shape and size of continental blocks which have been rifted off the northeastern Gondwana margin during the Late Jurassic and are now accreted to the SE Asia margin. We apply structural geology restoration techniques to unfold the subducted oceanic lithosphere of the Banda Slab. Our slab unfolding results help to discriminate between the different hypotheses concerning the origin and kinematic history of the Bird's Head tectonic block. According to our preferred model, the block is required to rotate 20-35 degrees clockwise relative to its present-day position and that the initial geometry of the ATS ocean basin was more or less rectangular shaped. We evaluate currently accepted plate kinematic scenarios for the Jurassic and younger seaoor spreading history north of Australia in conjunction with our restored ocean basin geometry and conclude that the Bird's Head block is autochthonous to western Irian Jaya, with its western margin being a continental transform margin during the rifting and opening of the ATS ocean.
Reconstruction of Ultrasound RF Echoes Modelled as Stable Random Variables. IEEE Transactions on Computational Imaging, 1(2), 86-95.

This paper introduces a new technique for reconstruction of biomedical ultrasound images from simulated compressive measurements, based on modeling data with stable distributions. The proposed algorithm exploits two types of prior information: On the one hand, our proposed approach is based on the observation that ultrasound RF echoes are best characterized statistically by alpha-stable distributions. On the other hand, through knowledge of the acquisition process, the support of the RF echoes in the Fourier domain can be easily inferred. Together, these two facts form the basis of an ℓ p minimization approach that employs the iteratively reweighted least squares (IRLS) algorithm, but in which the parameter p is judiciously chosen, by relating it to the characteristic exponent of the underlying alpha-stable distributed data. We demonstrate, through Monte Carlo simulations, that the optimal value of the parameter p is just below that of the characteristic exponent, α , which we estimate from the data. Our reconstruction results show that the proposed algorithm outperforms previously proposed reconstruction techniques, both visually and in terms of two objective evaluation measures. ultrasound imaging, high resolution imaging, Doppler signal processing, Detection and estimation with application to Multidimensional biomedical and image including parametric modeling, spectral analysis and application to ﬂow estimation, Sparse representation, Inverse problems.
THE JET-DRIVEN OUTFLOW IN THE RADIO GALAXY SDSS J1517+3353: IMPLICATIONS FOR DOUBLE-PEAKED NARROW-LINE ACTIVE GALACTIC NUCLEUS

We report on the study of an intriguing active galaxy that was selected as a potential multiple supermassive black hole merger in the early-type host SDSS J151709.20+335324.7 (z = 0.135) from a complete search for double-peaked [O iii] lines from the SDSS spectroscopic quasi-stellar object (QSO) database. Ground-based SDSS imaging reveals two blue structures on either side of the photometric center of the host galaxy, separated from each other by about 5.7 kpc. From a combination of SDSS fiber and Keck/HIRES long-slit spectroscopy, it is demonstrated that, in addition to these two features, a third distinct structure surrounds the nucleus of the host galaxy. All three structures exhibit highly ionized line emission with line ratios characteristic of Seyfert II active galactic nuclei. The analysis of spatially resolved emission-line profiles from the HIRES spectrum reveal three distinct kinematic subcomponents, one at rest and the other two moving at −350 km s−1 and 500 km s−1 with respect to the systemic velocity of the host galaxy. A comparison of imaging and spectral data confirm a strong association between the kinematic components and the spatial knots, which implies a highly disturbed and complex active region in this object. A comparative analysis of the broadband positions, colors, kinematics, and spectral properties of the knots in this system lead to two plausible explanations: (1) a multiple active galactic nucleus (AGN) produced due to a massive dry merger, or (2) a very powerful radio jet-driven outflow. Subsequent VLA radio imaging reveals a clear jet aligned with the emission-line gas, confirming the latter explanation. We use the broadband radio measurements to examine the impact of the jet on the interstellar medium of the host galaxy, and find that the energy in the radio lobes can heat a significant fraction of the gas to the virial temperature. Finally, we discuss tests that may help future surveys distinguish between jet-driven kinematics and true black-hole binaries. J1517+3353 is a remarkable laboratory for AGN feedback and warrants deeper follow-up study. In the Appendix, we present high-resolution radio imaging of a second AGN with double-peaked [O iii] lines, SDSS J112939.78+605742.6, which shows a sub-arcsecond radio jet. If the double-peaked nature of the narrow lines in radio-loud AGNs are generally due to radio jet interactions, we suggest that extended radio structure should be expected in most of such systems.
PROBING THE STRUCTURE OF THE OUTFLOW IN THE TIDAL DISRUPTION FLARE Sw J1644+57 WITH LONG-TERM RADIO EMISSION

The recently discovered high-energy transient Sw J1644+57 is thought to arise from the tidal disruption of a passing star by a dormant massive black hole. The long-term, bright radio emission of Sw J1644+57 is believed to result from the synchrotron emission of the blast wave produced by an outflow expanding into the surrounding medium. Using the detailed multi-epoch radio spectral data, we are able to determine the total number of radiating electrons in the outflow at different times, and further the evolution of the cross section of the outflow with time. We find that the outflow gradually transits from a conical jet to a cylindrical one at later times. The transition may be due to collimation of the outflow by the pressure of the shocked jet cocoon that forms while the outflow is propagating in the ambient medium. Since cylindrical jets usually exist in active galactic nuclei (AGNs) and extragalactic jets, this may provide independent evidence that Sw J1644+57 signals the onset of an AGN.
THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. XI. THE SPATIALLY RESOLVED RECENT STAR FORMATION HISTORY OF M31

We measure the recent star formation history (SFH) across M31 using optical images taken with the Hubble Space Telescope as part of the Panchromatic Hubble Andromeda Treasury (PHAT). We fit the color–magnitude diagrams in ∼9000 regions that are ∼100 pc × 100 pc in projected size, covering a 0.5 square degree area (∼380 kpc2, deprojected) in the NE quadrant of M31. We show that the SFHs vary significantly on these small spatial scales but that there are also coherent galaxy-wide fluctuations in the SFH back to ∼500 Myr, most notably in M31's 10 kpc star-forming ring. We find that the 10 kpc ring is at least 400 Myr old, showing ongoing star formation (SF) over the past ∼500 Myr. This indicates the presence of molecular gas in the ring over at least 2 dynamical times at this radius. We also find that the ring’s position is constant throughout this time, and is stationary at the level of 1 km s−1, although there is evidence for broadening of the ring due to the diffusion of stars into the disk. Based on existing models of M31's ring features, the lack of evolution in the ring’s position makes a purely collisional ring origin highly unlikely. Besides the well-known 10 kpc ring, we observe two other ring-like features. There is an outer ring structure at 15 kpc with concentrated SF starting ∼80 Myr ago. The inner ring structure at 5 kpc has a much lower star formation rate (SFR) and therefore lower contrast against the underlying stellar disk. It was most clearly defined ∼200 Myr ago, but is much more diffuse today. We find that the global SFR has been fairly constant over the last ∼500 Myr, though it does show a small increase at 50 Myr that is 1.3 times the average SFR over the past 100 Myr. During the last ∼500 Myr, ∼60% of all SF has occurred in the 10 kpc ring. Finally, we find that in the past 100 Myr, the average SFR over the PHAT survey area is 0.28 ± 0.03 M ⊙ ? > yr − 1 ? > with an average deprojected intensity of 7.3 × 10 − 4 ? > M ⊙ ? > yr − 1 kpc − 2 ? > , which yields a total SFR of ∼0.7 M ⊙ ? > yr − 1 ? > when extrapolated to the entire area of M31's disk. This SFR is consistent with measurements from broadband estimates.