Miracle-dz/UniFAR-FTUs huggingface dataset:
Retrospective Analysis of Prognostic Factors in Pediatric Patients with Adrenocortical Tumor from Unique Tertiary Center with Long-Term Follow-Up

Pediatric adrenocortical tumors (PACTs) represent rare causes of malignancies. However, the south/southeast regions of Brazil are known to have a high incidence of PACTs because of the founder effect associated with a germline pathogenic variant of tumor suppressor gene TP53. We aimed to retrospectively analyze the types of variables among hormone production, radiological imaging, tumor staging, histological and genetic features that were associated with the occurrence of malignancy in 95 patients (71% females) with PACTs from a unique center. The worst prognosis was associated with those aged > 3 years (p < 0.05), high serum levels of 11-desoxicortisol (p < 0.001), tumor weight ≥ 200 g (p < 0.001), tumor size ≥ 5 cm (p < 0.05), Weiss score ≥ 5 (p < 0.05), Wieneke index ≥ 3 (p < 0.001) and Ki67 ≥ 15% (p < 0.05). Furthermore, patients with MacFarlane stage IV had an overall survival rate almost two times shorter than patients with other stages (p < 0.001). Additionally, the subtractions of BUB1B-PINK1 (<6.95) expression (p < 0.05) and IGF-IR overexpression (p = 0.0001) were associated with malignant behavior. These results helped identify patients who are likely to have an aggressive course; further multicenter prospective studies are required to confirm our results. In conclusion, PACTs with these patterns of prognostic factors could be treated using an adjuvant approach that may improve the overall survival in such patients.
Fermi-LAT kills dark matter interpretations of AMS-02 data. Or not?

A number of papers attempt to explain the positron anomaly in cosmic rays, observed by PAMELA and AMS-02, in terms of dark matter (DM) decays or annihilations. However, the recent progress in cosmic gamma-ray studies challenges these attempts. Indeed, as we show, any rational DM model explaining the positron anomaly abundantly produces final state radiation and Inverse Compton gamma rays, which inevitably leads to a contradiction with Fermi-LAT isotropic diffuse gamma-ray background measurements. Furthermore, the Fermi-LAT observation of Milky Way dwarf satellites, supposed to be rich in DM, revealed no significant signal in gamma rays. We propose a generic approach in which the major contribution to cosmic rays comes from the dark matter disc and prove that the tension between the DM origin of the positron anomaly and the cosmic gamma-ray observations can be relieved. We consider both a simple model, in which DM decay/annihilate into charged leptons, and a model-independent minimal case of particle production, and we estimate the optimal thickness of DM disk. Possible mechanisms of formation and its properties are briefly discussed.
A Flexible Phase Retrieval Framework for Flux-limited Coherent X-Ray Imaging

Coherent X-ray diffraction imaging (CXDI) experiments are intrinsically limited by shot noise, a lack of prior knowledge about the sample's support, and missing measurements due to the experimental geometry. We propose a flexible, iterative phase retrieval framework that allows for accurate modeling of Gaussian or Poissonian noise statistics, modified support updates, regularization of reconstructed signals, and handling of missing data in the observations. The proposed method is efficiently solved using alternating direction method of multipliers (ADMM) and is demonstrated to consistently outperform state-of-the-art algorithms for low-photon phase retrieval from CXDI experiments, both for simulated diffraction patterns and for experimental measurements.
Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores - II. Simulated ALMA dust emission maps

Max-Planck-Institut fu¨r Astronomie, Ko¨nigstuhl 17, 69117 Heidelberg, GermanyReceived 20 july 2012; accepted 3 october 2012ABSTRACTContext. First hydrostatic cores are predicted by theories of star formation, but their existence has never been demonstrated con-vincingly by (sub)millimeter observations. Furthermore, the multiplicity at the early phases of the star formation process is poorlyconstrained.Aims. The purpose of this paper is twofold. First, we seek to provide predictions of ALMA dust continuum emission maps from earlyClass 0 objects. Second, we show to what extent ALMA will be able to probe the fragmentation scale in these objects.Methods. Following our previous paper (Commerc¸on et al. 2012, hereafter paper I), we post-process three state-of-the-art radiation-magneto-hydrodynamic 3D adaptive mesh reﬁnement calculations to compute the emanating dust emission maps. We then producesynthetic ALMA observations of the dust thermal continuum from ﬁrst hydrostatic cores.Results. We present the ﬁrst synthetic ALMA observations of dust cont inuum emission from ﬁrst hydrostatic cores. We analyze theresults given by the diﬀerent bands and conﬁgurations and we discuss for which combi nations of the two the ﬁrst hydrostatic coreswould most likely be observed. We also show that observing dust continuum emission with ALMA will help in identifying the physi-cal processes occurring within collapsing dense cores. If the magnetic ﬁeld is playing a role, the emission pattern will show evidenceof a pseudo-disk and even of a magnetically driven outﬂow, which pure hydrodynamical calculations cannot reproduce.Conclusions. The capabilities of ALMA will enable us to make signiﬁcant pr ogress towards understanding fragmentation at the earlyClass 0 stage and discovering ﬁrst hydrostatic cores.Key words. Stars: low mass, formation - Magnetohydrodynamics (MHD), radiative transfer - Methods: numerical - Techniques:interferometric
Pulsational amplitude growth of the star KIC 3429637 (HD 178875) in the context of Am and ρ Pup stars

KIC 3429637 (HD 178875) is a δ Sct star whose light curve shows continuous pulsational amplitude growth in Kepler mission photometry. Analysis of the three largest amplitude peaks in the Fourier transform indicates different growth rates for all three. We have ruled out instrumental causes, and determine the amplitude growth to be intrinsic to the star. We calculate time-dependent convection models and compare them with the observations. We confirm earlier characterizations that KIC 3429637 is a marginal Am star through the analysis of new spectroscopic data. With the data presently available, a plausible cause of the amplitude growth is increasing pulsational driving as evolutionary changes shift the He ii driving zone deeper in this ρ Puppis star. If this model is correct, then we are watching real-time stellar evolutionary changes.
Several nonlocal sets of multipartite pure orthogonal product states

It is known that there exist sets of pure orthogonal product states which cannot be perfectly distinguished by local operations and classical communication (LOCC). Such sets are nonlocal sets which exhibit nonlocality without entanglement. These nonlocal sets can be completable or uncompletable. In this work both completable and uncompletable small nonlocal sets of multipartite orthogonal product states are constructed. Apart from nonlocality, these sets have other interesting properties. In particular, the completable sets lead to the construction of a class of complete orthogonal product bases with the property that if such a basis is given then no state can be eliminated from that basis by performing orthogonality-preserving measurements. On the other hand, an uncompletable set of the present kind contains several Shifts unextendible product bases (UPBs) that belong to qubit subspaces. Identifying these subspace UPBs, it is possible to obtain a class of high-dimensional multipartite bound entangled states. Finally, it is shown that a two-qubit maximally entangled Bell state shared between any two parties is sufficient as a resource to distinguish the states of any completable set (of the above kind) perfectly by LOCC. This constitutes an example where the amount of entanglement, sufficient to accomplish the aforesaid task, depends neither on the dimension of the individual subsystems nor on the number of parties.
An Adaptive Method to Reduce Undershoots and Overshoots in Power Switching Transistors Through a Low-Complexity Active Gate Driver

Active gate drivers lend themselves well to reducing over- and undervoltages during the commutations of hard switched power transistors, as well as to damping resonances. However, their control strategy is a major challenge, as it should account for variations of operating condition, parameter spread, and nonlinearities of the driven transistor. This article proposes an effective control method to reduce overshoots and undershoots in a power transistor driven by an active gate driver. The modulation pattern is modified on-the-fly and none a priori characterization is required. The presented method modifies the timing parameter to attain almost zero over- and undervoltages with the lowest power losses. This is achieved by combining a low-complexity active gate driver with the measurements of peak values of the drain–source voltage. The technique was experimentally assessed for a 48–12 V dc–dc converter, and resulted in better switching performance than standard solutions and open-loop control.
REIONIZATION ON LARGE SCALES. II. DETECTING PATCHY REIONIZATION THROUGH CROSS-CORRELATION OF THE COSMIC MICROWAVE BACKGROUND

We investigate the effect of patchy reionization on the cosmic microwave background (CMB) temperature. An anisotropic optical depth alters the TT power spectrum on small scales l > 2000. We make use of the correlation between the matter density and the reionization redshift fields to construct full sky maps of . Patchy reionization transfers CMB power from large scales to small scales, resulting in a non-zero cross correlation between large and small angular scales. We show that the patchy τ correlator is sensitive to small root mean square (rms) values τrms ∼ 0.003 seen in our maps. We include frequency-independent secondaries such as CMB lensing and kinetic Sunyaev–Zel'dovich (kSZ) terms, and show that patchy τ may still be detected at high significance. Reionization models that predict different values of τrms may be distinguished even for the same mean value 〈τ〉. It is more difficult to detect patchy τ in the presence of larger secondaries such as the thermal Sunyaev–Zel'dovich, radio background, and the cosmic infrared background. In this case, we show that patchy τ may be detected if these frequency-dependent secondaries are minimized to ≲ 5 μK (rms) by means of a multi-frequency analysis. We show that the patchy τ correlator provides information that is complementary to what may be obtained from the polarization and the kSZ power spectra.
Signatures of thermal hysteresis in Tamm-wave propagation

We numerically solved the boundary-value problem for Tamm waves (which may also be classified as Uller–Zenneck waves here) guided by the planar interface of a homogeneous isotropic dissipative dielectric (HIDD) material and a periodically multilayered isotropic dielectric material. The HIDD material was chosen to be VO2, which, at optical wavelengths, has a temperature-dependent refractive index with a hysteresis feature, i.e., the temperature-dependence of its refractive index varies depending upon whether the temperature is increasing or decreasing. A numerical code was implemented to extract solutions of the dispersion equation at a fixed wavelength for both p- and s-polarization states over the temperature range [50,80]°C. A multitude of Tamm waves of both linear polarization states were found, demonstrating a clear demarcation of the heating and cooling phases in terms of wavenumbers and propagation distances. Thereby, the signatures of thermal hysteresis in Tamm-wave propagation were revealed.
Extrinsic and intrinsic photoresponse in monodisperse carbon nanotube thin film transistors

Spectroscopic, time-resolved scanning photocurrent microscopy is shown to distinguish the intrinsic photoresponse of monodisperse semiconducting (99%) single-walled carbon nanotubes (SWCNTs) from the extrinsic photoresponse of the substrate. A persistent positive photocurrent induced by near-infrared excitation is attributed to the generation of free carriers by inter-band excitation in SWCNTs. For shorter excitation wavelengths, absorption by the Si substrate generates two types of photocurrent: a transient positive photoresponse, identified as a displacement current, and a persistent negative photocurrent that arises from photogating of the SWCNT thin film.
THE ACS FORNAX CLUSTER SURVEY. VIII. THE LUMINOSITY FUNCTION OF GLOBULAR CLUSTERS IN VIRGO AND FORNAX EARLY-TYPE GALAXIES AND ITS USE AS A DISTANCE INDICATOR

We use a highly homogeneous set of data from 132 early-type galaxies in the Virgo and Fornax clusters in order to study the properties of the globular cluster luminosity function (GCLF). The globular cluster system of each galaxy was studied using a maximum likelihood approach to model the intrinsic GCLF after accounting for contamination and completeness effects. The results presented here update our Virgo measurements and confirm our previous results showing a tight correlation between the dispersion of the GCLF and the absolute magnitude of the parent galaxy. Regarding the use of the GCLF as a standard candle, we have found that the relative distance modulus between the Virgo and Fornax clusters is systematically lower than the one derived by other distance estimators, and in particular, it is 0.22 mag lower than the value derived from surface brightness fluctuation measurements performed on the same data. From numerical simulations aimed at reproducing the observed dispersion of the value of the turnover magnitude in each galaxy cluster we estimate an intrinsic dispersion on this parameter of 0.21 mag and 0.15 mag for Virgo and Fornax, respectively. All in all, our study shows that the GCLF properties vary systematically with galaxy mass showing no evidence for a dichotomy between giant and dwarf early-type galaxies. These properties may be influenced by the cluster environment as suggested by cosmological simulations.
Differential Equations Driven by Π-Rough Paths

Abstract This paper revisits the concept of rough paths of inhomogeneous degree of smoothness (geometric Π-rough paths in our terminology) sketched by Lyons in 1998. Although geometric Π-rough paths can be treated as p-rough paths for a sufficiently large p, and the theory of integration of Lip γ one-forms (γ > p–1) along geometric p-rough paths applies, we prove the existence of integrals of one-forms under weaker conditions. Moreover, we consider differential equations driven by geometric Π-rough paths and give sufficient conditions for existence and uniqueness of solution.
Renyi entanglement entropies of descendant states in critical systems with boundaries: conformal field theory and spin chains

We discuss the Renyi entanglement entropies of descendant states in critical one-dimensional systems with boundaries, that map to boundary conformal field theories in the scaling limit. We unify the previous conformal-field-theory approaches to describe primary and descendant states in systems with both open and closed boundaries. We provide universal expressions for the first two descendants in the identity family. We apply our technique to critical systems belonging to different universality classes with non-trivial boundary conditions that preserve conformal invariance, and find excellent agreement with numerical results obtained for finite spin chains. We also demonstrate that entanglement entropies are a powerful tool to resolve degeneracy of higher excited states in critical lattice models.
Differentiation signatures in the Flora region

Most asteroid families are very homogeneous in physical properties. Some show greater diversity, however. The Flora family is the most intriguing of them. The Flora family is spread widely in the inner main belt, has a rich collisional history, and is one of the most taxonomically diverse regions in the main belt. As a result of its proximity to the asteroid (4) Vesta (the only currently known intact differentiated asteroid) and its family, migration between the two regions is possible. This dynamical path is one of the counter arguments to the hypothesis that there may be traces of a differentiated parent body other than Vesta in the inner main belt region. We here investigate the possibility that some of the V- and A- types (commonly interpreted as basaltoids and dunites - parts of the mantle and crust of differentiated parent bodies) in the Flora dynamical region are not dynamically connected to Vesta.
The effects of dust on the optical and infrared evolution of SN 2004et

We present an analysis of multi-epoch observations of the Type II-P supernova SN 2004et. New and archival optical spectra of SN 2004et are used to study the evolution of the Hα and [O i] 6300-A line profiles between days 259 and 646. Mid-infrared imaging with Michelle on Gemini-North and with all three instruments of the Spitzer Space Telescope was carried out between 2004 and 2010, supplemented by archival Spitzer data. We include Spitzer‘warm’ mission photometry at 3.6 and 4.5 μm obtained on days 1779, 1931 and 2151, along with ground-based and Hubble Space Telescope (HST) optical and near-infrared observations obtained between days 79 and 1803. Multiwavelength light curves are presented, as well as optical–infrared spectral energy distributions (SEDs) for multiple epochs. Starting from about day 300, the optical light curves provide evidence for an increasing amount of circumstellar extinction attributable to newly formed dust, with the additional extinction reaching 0.8–1.5 mag in the V band by day 690. The overall SEDs were fitted with multiple blackbody components, in order to investigate the luminosity evolution of the supernova, and then with Monte Carlo radiative transfer models using smooth or clumpy dust distributions, in order to estimate how much new dust condensed in the ejecta. The luminosity evolution was consistent with the decay of 56Co in the ejecta up until about day 690, after which an additional emission source is required, in agreement with the findings of Kotak et al. Clumped dust density distributions consisting of 20 per cent amorphous carbons and 80 per cent silicates by mass were able to match the observed optical and infrared SEDs, with dust masses that increased from 8 × 10−5 M⊙ on day 300 to 1.5 × 10−3 M⊙ on day 690, still significantly lower than the values needed for core-collapse supernovae to make a significant contribution to the dust enrichment of galaxies.
Programmable atom-photon quantum interface

We present the implementation of a programmable atom-photon quantum interface, employing a single trapped $^{40}\mathrm{Ca}^{+}$ ion and single photons. Depending on its mode of operation, the interface serves as a bidirectional atom-photon quantum-state converter, as a source of entangled atom-photon states, or as a quantum frequency converter of single photons. The interface lends itself particularly to interfacing ions with spontaneous parametric down-conversion--based single-photon or entangled-photon-pair sources.
Computation and visualization of accessible reciprocal space and resolution element in high-resolution X-ray diffraction mapping

An approach to visualize the accessible reciprocal space accounting the goniometer angles limitation and the resolution element in the reciprocal space is presented. The shapes of the accessible reciprocal space region for coplanar and non-coplanar geometries are given employing the additional degree of freedom provided by detector arm. The examples of the resolution elements in different points of the reciprocal space are shown. The equations obtained permit to find these regions and to calculate the experimental geometry to obtain the diffraction from any accessible reflections, which makes a further extension of previously reported methods. The introduced algorithm has been testified by experimental measurements of reciprocal space maps in coplanar and non-coplanar geometries. The examples of the resolution elements in different points of the reciprocal space are calculated to illustrate the method proposed.
Convection in a coupled fluid-porous media system

We perform linear and nonlinear stability analysis for thermal convection in a fluid overlying a saturated porous medium. We use a coupled system in which Navier-Stokes governs the free flow and Darcy's equation governs the porous-medium flow. Incorporating a dynamic pressure term in the Lions interface condition (which specifies the normal force balance across the fluid-medium interface) permits an energy bound on the typically uncooperative nonlinear advection term, enabling new nonlinear stability results. We find close agreement between the linear and nonlinear stability thresholds, indicating that the more easily obtained linear thresholds indicate global stability. Additionally, we quantify the difference between linear and nonlinear stability curves. We then compare stability thresholds produced by several common variants of the tangential interface conditions, using both numerics and asymptotics in the small Darcy number limit. Finally, we investigate the transition between porous-dominated and fluid-dominated convection. A simple theory based on critical Rayleigh numbers is put forth, and it agrees well with numerics regarding how the transition depends on the depth ratio, the Darcy number, and the thermal-diffusivity ratio.
Does the Neptunian system of satellites challenge a gravitational origin for the Pioneer anomaly

If the Pioneer anomaly (PA) was a genuine dynamical effect of gravitational origin, it should also affect the orbital motions of the Solar system's bodies moving in the space regions in which the PA manifested itself in its presently known form, i.e. as a constant and uniform acceleration approximately directed towards the Sun with a non-zero magnitude A Pio = (8.74 ± 1.33) × 10 ―10 ms ―2 after 20 au from the Sun. In this paper we preliminarily investigate its effects on the orbital motions of the Neptunian satellites Triton, Nereid and Proteus, located at about 30 au from the Sun, both analytically and numerically. Extensive observational records covering several orbital revolutions have recently been analysed for them, notably improving the knowledge of their orbits. Both analytical and numerical calculations, limited to the direct, Neptune-satellite interaction, show that the peak-to-peak amplitudes of the PA-induced radial, transverse and out-of-plane perturbations over one century are up to 300, 600 km, 8 m for Triton, 17 500, 35 000, 800 km for Nereid and 60,120 km, 30 m for Proteus. The corresponding orbital uncertainties obtained from a recent analysis of all the data available for the satellites considered are, in general, smaller by one-two orders of magnitude, although obtained without modelling a Pioneer-like extra-force. Further investigations based on a reprocessing of the satellites' real or simulated data with modified equations of motions including an additional Pioneer-type force as well are worth being implemented and may shed further light on this important issue.