Miracle-dz/UniFAR-FTUs huggingface dataset:
Cloud-radiative impact on the dynamics and predictability of an idealized extratropical cyclone

Abstract. Extratropical cyclones drive midlatitude weather, including extreme events, and determine midlatitude climate. Their dynamics and predictability are strongly shaped by cloud diabatic processes. While the cloud impact due to latent heating is much studied, little is known about the impact of cloud radiative heating (CRH) on the dynamics and predictability of extratropical cyclones. Here, we address this question by means of baroclinic life cycle simulations performed at a convection-permitting resolution of 2.5 km with the ICON model. The simulations use a newly implemented channel setup with periodic boundary conditions in the zonal direction. Moreover, the simulations apply a new modeling technique for which only CRH interacts with the cyclone, which circumvents changes in the mean state due to clear-sky radiative cooling that has complicated the interpretation of previous work. We find that CRH increases the kinetic energy of the cyclone system. The impact is most prominent at upper levels. To understand the CRH impact on the upper-tropospheric circulation, we diagnose the evolution of differences in potential vorticity between a simulation with and without CRH, and we quantify through which processes these differences grow over the course of the cyclone's life cycle. According to this diagnostic, CRH affects the cyclone mostly via the intensification of latent heating from cloud microphysical processes. Near the tropopause, direct diabatic modification of potential vorticity by intensified latent heat release precedes further changes in the tropopause by the upper-tropospheric divergent flow, which represents an indirect impact of latent heat release. Subsequently, differences in the tropopause structure amplify with the rotational flow during the highly nonlinear stage of the baroclinic wave. Our results show that although CRH is comparably small in magnitude, it can affect extratropical cyclones by changing cloud microphysical heating and subsequently the large-scale flow. The CRH impact follows a previously identified mechanism of multi-stage upscale error growth. At the same time, simulations in which CRH is disabled after certain days show that the CRH impact operates throughout the entire intensification phase of the cyclone. This means that CRH does not merely provide an arbitrary initial perturbation to the cyclone, from which differences grow in a generic way. Instead, our results suggest that uncertainties associated with the representation of CRH in numerical models have a more systematic impact and may more fundamentally influence model predictions of extratropical cyclones.
Measurement of the Reaction pp→ppπ+π-π0 with CELSIUS/WASA at 1.36 GeV

A versatile detector setup prepared by the CELSIUS/WASA collaboration for exclusive studies of rare processes produced in proton and deuteron collisions with hydrogen and deuterium pellet targets is presented. For the near-threshold production of light mesons, π0 and η, the scattered beam and target particles are measured in the forward detector, while the products of the decaying mesons are registered in a central detector covering close-to-4π sr.The central detector is composed of a mini-drift chamber consisting of 1738 straw tubes for tracking of the charged particles and a plastic scintillator barrel consisting of 146 scintillation counters providing fast signals of the passing particles. These two detector parts are placed inside of a superconducting solenoid providing an axial magnetic field.Outside of the solenoid is placed an electromagnetic calorimeter consisting of 1012 CsI crystals. The construction, calibration and performance of the plastic scintillator barrel is presented in detail. Its main purpose is the discrimination of charged and neutral particles on the trigger level. It is also used for the identification of charged particles by ΔE-p (ΔE-E) technique in the off-line analysis.The mini-drift chamber is a detector for determination of particles momenta and reaction vertex. It is built with minimum structural material and designed to withstand high particle fluxes at a luminosity 1032cm-2s-1. The design of the mini-drift chamber, a description of the calibration procedure, its performance and integration in the data analysis are presented.The overall performance of the WASA detector is demonstrated by the analysis of the pp→ppπ+π-π0 reaction at 1.36 GeV incident proton energy. The total cross section for the non-resonant part of the reaction is estimated for the first time in this energy region to be 4.6 ±1.2 -0.9 +0.7 μb. The pp→ppη part of the total reaction cross section is estimated to be 4.8 μb which is consistent with the existing experimental information.
[Fe IV] Emission in Ionized Nebulae

This paper presents an analysis of [Fe IV] emission based on new identifications and previous measurements of [Fe IV] lines in 30 Doradus, IC 4846, M42, SMC N88A, and SBS 0335-052. The Fe abundances obtained by adding the abundances of the relevant Fe ions (mainly Fe++ and Fe3+) are found to be lower, by factors in the range 2.6-5.9, than the Fe abundances implied by [Fe III] emission and an ionization correction factor derived from ionization models. The most likely explanation of this discrepancy is that either the collision strengths for [Fe IV] or the Fe ionization fractions predicted by models are unreliable. The available data allow one neither to distinguish between these two possibilities nor to exclude another possible explanation: that the discrepancy implies the presence of a gradient in the Fe abundance within the ionized gas. Further measurements of [Fe IV] lines and checks on the Fe3+ atomic data and ionization models are needed to reach a definitive conclusion. The discrepancy introduces an uncertainty in the determination of Fe abundances in ionized nebulae. This uncertainty has implications for our understanding of both the evolution of dust in ionized nebulae and the chemical history of low-metallicity galaxies.
Optical light curve of GRB 121011A: a textbook for the onset of GRB afterglow in a mixture of ISM and wind-type medium

We report the optical observations of GRB 121011A by the 0.8m TNT facility at Xinglong observatory, China. The light curve of the optical afterglow shows a smooth and featureless bump during the epoch of ∼130 s and ∼5000 s with a rising index of 1.57 ± 0.28 before the break time of 539 ± 44 s, and a decaying index of about 1.29 ± 0.07 up to the end of our observations. Moreover, the X-ray light curve decays in a single power-law with a slope of about 1.51 ± 0.03 observed by XRT onboard Swift from 100 s to about 10 000 s after the burst trigger. The featureless optical light curve could be understood as an onset process under the external-shock model. The typical frequency has been below or near the optical one before the deceleration time, and the cooling frequency is located between the optical and X-ray wavelengths. The external medium density has a transition from a mixed stage of ISM and wind-type medium before the peak time to the ISM at the later phase. The joint-analysis of X-ray and optical light curves shows that the emissions from both frequencies are consistent with the prediction of the standard afterglow model without any energy injections, indicating that the central engine has stopped its activity and does not restart anymore after the prompt phase.
Psychometric analysis and Validity of Readiness for Interprofessional Learning Scale in undergraduate Chilean nurses

: Introduction : Interprofessional education offers health students an opportunity to learn, practice, and improve communication and collaboration skills through learning experiences with other professions. It is important to determine their willingness to actively engage with other students in their learning process, which is assessed through the Readiness for Interprofessional Learning scale, one of the most widely used internationally. The objective was to adapt and validate the Readiness for Interprofessional Learning Scale to Spanish among nursing students. Method: The study design was cross-sectional quantitative, with a sample of 330 nursing students of different years. Cronbach's Alpha and exploratory and confirmatory factor analysis were performed. Results: The original scale had 23 items, only 16 met the validity and reliability criteria. The 16 items are distributed in the dimensions: Teamwork and collaboration (T: 10 items), Patient Centered Work (EP: 4 items) and Professional identity (PI: 2 items). Cronbach's alpha index for the full scale was 0.8259 (CyTE α=0.81; PC α= 0.77 and PI α=0.61). Conclusion: the RIPL scale validated in this study has adequate reliability and validity for the dimensions Teamwork and collaboration and Patient Centered Work . Elaboration of new items are required for Professional Identity
The relationship between cancer progression and social environment in Drosophila

The ecological benefits of sociality in gregarious species are widely acknowledged. However, only 35 limited data is available on how the social environment influences non-communicable disease outcomes. 36 For instance, despite extensive research over the past decades, the role of the social environment on 37 cancer progression remains unclear and controversial. This is mainly because epidemiological studies 38 suffer from the complexity of inter-correlated factors and it is still unknown whether distinct social 39 group composition can also differentially affect tumor growth. Here, we exposed adult Drosophila with 40 colorectal-like tumors to different social environments. We show that both cancerous flies bred in 41 complete isolation, or in a group with non-cancerous individuals, exhibit increased tumor progression 42 compared to those bred with other cancerous conspecifics. Based on video-tracking and social 43 interaction analyses, we propose that this dramatic effect may be a consequence of perceived social 44 isolation due to differential social interaction rates. We found that flies can discriminate between 45 individuals at different stages of tumor growth; control flies actively avoid flies with cancer but only at 46 the later stages of tumor development, whereas cancerous flies display strong social interactions with 47 cancerous flies in the early stages of tumor growth. Our study demonstrates the reciprocal links between 48 cancer and social interactions, as well as highlighting how sociality impacts health and fitness in animals 49 and its potential implications for disease ecology and ecosystem dynamics.
Future supernovae data and quintessence models

The possibility of unambiguously determining the equation of state of the cosmic dark energy with existing and future supernovae data is investigated. We consider four evolution laws for this equation of state corresponding to four quintessential models, i.e. (i) a cosmological constant, (ii) a general barotropic fluid, (iii) a perfect fluid with a linear equation of state and (iv) a more physical model based on a pseudo-Nambu-Goldstone boson field. We explicitly show the degeneracies present not only within each model but also between the different models: they are caused by the multi-integral relation between the equation of state of dark energy and the luminosity distance. Present supernova observations are analysed using a standard Χ 2 method and the minimal Χ 2 values obtained for each model are compared. We confirm the difficulty in discriminating between these models using present type Ia supernovae data only. By means of simulations, we then show that future SNAP observations will not remove all the degeneracies. For example, wrong estimations of Ω m with a good value of Χ 2 m i n could be found if the right cosmological model is not used to fit the data. Finally, we give some probabilities for obtaining unambiguous results, free from degeneracies. In particular, the probability of confusing a cosmological constant with a true barotropic fluid with an equation of state different from -1 is shown to be 95 per cent at a 2σ level.
NbN single-photon detectors with saturated dependence of quantum efficiency

The possibility of creating NbN superconducting single-photon detectors with saturated dependence of quantum efficiency (QE) versus normalized bias current was investigated. It was shown that the saturation increases for the detectors based on finer films with a lower value of Rs300/Rs20. The decreasing of Rs300/Rs20 was related to the increasing influence of quantum corrections to conductivity of superconductors and, in turn, to the decrease of the electron diffusion coefficient. The best samples have a constant value of system QE 94% at Ib/Ic ∼ 0.8 and wavelength 1310 nm.
Noncommutativity in Effective Loop Quantum Cosmology

We construct a noncommutative extension of the Loop Quantum Cosmology effective scheme for the flat FLRW model with a free scalar field via a theta deformation. Firstly, a deformation is implemented in the configuration sector, among the holonomy variable and the matter degree of freedom. We show that this type of noncommutativity retains, to some degree, key features of the Loop Quantum Cosmology paradigm for a free field. Secondly, a deformation is implemented in the momentum sector, among the momentum associated with the holonomy variable and the momentum associated with the matter field. We show that in this latter case the scalar field energy density is the same as the one in standard Loop Quantum Cosmology.
Observational constraints on the specific accretion-rate distribution of X-ray-selected AGNs

This paper estimates the specific accretion-rate distribution of AGN using a sample of 4821 X-ray sources from both deep and shallow surveys. The specific accretion-rate distribution is defined as the probability of a galaxy with a given stellar mass and redshift hosting an active nucleus with a certain specific accretion rate. We find that the probability of a galaxy hosting an AGN increases with decreasing specific accretion rate. There is evidence that this trend reverses at low specific accretion rates, $\lambda<10^{-4}-10^{-3}$ (in Eddington units). There is also a break close to the Eddington limit, above which the probability of an accretion event decreases steeply. The specific accretion-rate distribution evolves such that the fraction of AGN among galaxies drops toward lower redshifts. This decrease in the AGN duty cycle is responsible for the strong evolution of the accretion density of the Universe from redshift $z\approx1-1.5$ to the present day. Our analysis also suggests that this evolution is accompanied by a decoupling of accretion events onto black holes from the formation of stars in galaxies. There is also evidence that at earlier times the relative probability of high vs low specific accretion-rate events among galaxies increases. We argue that this differential redshift evolution of the AGN duty cycle with respect to $\lambda$ produces the AGN downsizing trend, whereby luminous sources peak at earlier epochs compared to less luminous ones. Finally, we also find a stellar-mass dependence of the specific accretion-rate distribution, with more massive galaxies avoiding high specific accretion-rate events.
Excessive Hyaluronan Production Promotes Acquisition of Cancer Stem Cell Signatures through the Coordinated Regulation of Twist and the Transforming Growth Factor (cid:2) (TGF- (cid:2) )-Snail Signaling Axis

Background: Hyaluronan overproduction is implicated in breast cancer progression. Results: Hyaluronan overproduction expands cancer stem-like cells through the up-regulation of Snail and Twist expression. Conclusion: Hyaluronan overproduction allows plastic cancer cells to revert to stem cell states via Twist and the transforming growth factor (cid:2) -Snail signaling axis. Significance: These findings will help to understand the unique hyaluronan-dependent mechanisms that govern cancer cell plasticity and cancer stem cell expansion.
High-redshift major mergers weakly enhance star formation

Galaxy mergers are believed to trigger strong starbursts. This is well assessed by observations in the local Universe. However, the efficiency of this mechanism has poorly been tested so far for high-redshift, actively star-forming, galaxies. We present a suite of pc-resolution hydrodynamical numerical simulations to compare the star formation process along a merging sequence of high- and low-redshift galaxies, by varying the gas mass fraction between the two models. We show that, for the same orbit, high-redshift gas-rich mergers are less efficient than low-redshift ones at producing starbursts; the star formation rate excess induced by the merger and its duration are both around 10 times lower than in the low gas fraction case. The mechanisms that account for the star formation triggering at low redshift – the increased compressive turbulence, gas fragmentation, and central gas inflows – are only mildly, if not at all, enhanced for high gas fraction galaxy encounters. Furthermore, we show that the strong stellar feedback from the initially high star formation rate in high-redshift galaxies does not prevent an increase of the star formation during the merger. Our results are consistent with the observed increase of the number of major mergers with increasing redshift being faster than the respective increase in the number of starburst galaxies.
PREDICTABLE EFFECTS OF VISUAL SALIENCE IN EXPERIMENTAL DECISIONS AND GAMES

Bottom-up stimulus-driven visual salience is largely automatic, effortless, and independent of a person’s “top-down” perceptual goals; it depends only on features of a visual stimulus. Algorithms have been carefully trained to predict stimulusdriven salience values for each pixel in any image. The economic question we address is whether these salience values help explain economic decisions. Our first experimental analysis shows that when people pick between sets of fruits that have artificially induced value, predicted salience (which is uncorrelated with value by design) leads to mistakes. Our second analysis uses evidence from games in which choices are locations in images. When players are trying to cooperatively match locations, predicted salience is highly correlated with the success of matching (r = .57). In competitive hider-seeker location games, players choose salient locations more often than predicted by the unique Nash equilibrium. This tendency creates a disequilibrium “seeker’s advantage” (seekers win more often than predicted in equilibrium). The result can be explained by level-k models in which predicted stimulus-driven salience influences level-0 choices and thereby influences overall perceptions, beliefs, and choices of higher-level players. The third analysis shows that there is an effect of visual salience in matrix games, but it is small and statistically weak. Applications to behavioral IO, price and tax salience, nudges and design, and visually influenced beliefs are suggested. JEL Codes: D91, C91, C72.
SPATIALLY RESOLVED Hα MAPS AND SIZES OF 57 STRONGLY STAR-FORMING GALAXIES AT z ∼ 1 FROM 3D-HST: EVIDENCE FOR RAPID INSIDE-OUT ASSEMBLY OF DISK GALAXIES

We investigate the buildup of galaxies at z ∼ 1 using maps of Hα and stellar continuum emission for a sample of 57 galaxies with rest-frame Hα equivalent widths >100 Å in the 3D-HST grism survey. We find that the Hα emission broadly follows the rest-frame R-band light but that it is typically somewhat more extended and clumpy. We quantify the spatial distribution with the half-light radius. The median Hα effective radius re(Hα) is 4.2 ± 0.1 kpc but the sizes span a large range, from compact objects with re(Hα) ∼ 1.0 kpc to extended disks with re(Hα) ∼ 15 kpc. Comparing Hα sizes to continuum sizes, we find =1.3 ± 0.1 for the full sample. That is, star formation, as traced by Hα, typically occurs out to larger radii than the rest-frame R-band stellar continuum; galaxies are growing their radii and building up from the inside out. This effect appears to be somewhat more pronounced for the largest galaxies. Using the measured Hα sizes, we derive star formation rate surface densities, ΣSFR. We find that ΣSFR ranges from ∼0.05 M☉ yr−1 kpc−2 for the largest galaxies to ∼5 M☉ yr−1 kpc−2 for the smallest galaxies, implying a large range in physical conditions in rapidly star-forming z ∼ 1 galaxies. Finally, we infer that all galaxies in the sample have very high gas mass fractions and stellar mass doubling times <500 Myr. Although other explanations are also possible, a straightforward interpretation is that we are simultaneously witnessing the rapid formation of compact bulges and large disks at z ∼ 1.
Primordial black holes as dark matter: converting constraints from monochromatic to extended mass distributions

The model in which Primordial Black Holes (PBHs) constitute a non-negligible fraction of the dark matter has (re)gained popularity after the first detections of binary black hole mergers. Most of the observational constraints to date have been derived assuming a single mass for all the PBHs, although some more recent works tried to generalize constraints to the case of extended mass functions. Here we derive a general methodology to obtain constraints for any PBH Extended Mass Distribution (EMD) and any observables in the desired mass range. Starting from those obtained for a monochromatic distribution, we convert them into constraints for EMDs by using an equivalent, effective mass Meq that depends on the specific observable. We highlight how limits of validity of the PBH modelling affect the EMD parameter space. Finally, we present converted constraints on the total abundance of PBH from microlensing, stellar distribution in ultra-faint dwarf galaxies and CMB accretion for Lognormal and Power Law mass distributions, finding that EMD constraints are generally stronger than monochromatic ones.
A Residual Source of Energetic Neutral Atoms Across the Sky Obtained by the Neutral Particle Detector on board Venus Express

We have surveyed the sky for residual energetic neutral atom (ENA) signals in the energy range of 0.2–3.0 keV. Approximately three years of data obtained by the Neutral Particle Detector (NPD) on board Venus Express (VEX) from May 2006 through August 2009 have been analyzed. After applying strict viewing criteria to minimize all known signals and subtracting the UV background from the Milky Way, we find a residual energy spectral shape with a ledge/bump at around 0.5 keV and a break in the spectral slope at about 1.0 keV. When the ENA spectrum is divided by the energy dependent charge exchange cross section its slope above 1 keV has a spectral power‐law index of 1.5, which is consistent with that measured in‐situ in the inner heliosheath (HS) by the Low‐Energy Charged Particle (LECP) instrument (>40 keV) on board Voyager‐1 (V1). The ledge/bump at about 0.5 keV appears consistent with twice the plasma flow velocity obtained by the V1 measurements in the inner HS.
Quantum Interference Effects in Electronic Transport through Nanotube Contacts

Quantum interference has dramatic effects on electronic transport through nanotube contacts. In optimal configuration the intertube conductance can approach that of a perfect nanotube (4e 2 /h). The maximum conductance increases rapidly with the contact length up to 10 nm, beyond which it exhibits long-wavelength oscillations. This is attributed to the resonant interference phenomena in the contact region. For two concentric nanotubes symmetry breaking can reduce the maximum intertube conductance from 4e 2 /h to 2e 2 /h. The phenomena discussed here can serve as a foundation for building nanotube electronic circuits and high-speed nanoscale electromechanical devices.