Miracle-dz/UniFAR-FTUs huggingface dataset:
The VIMOS Public Extragalactic Redshift Survey (VIPERS): Downsizing of the blue cloud and the influence of galaxy size on mass quenching over the last eight billion years

We use the full VIPERS redshift survey in combination with SDSS-DR7 to explore the relationships between star-formation history (using d4000), stellar mass and galaxy structure, and how these relationships have evolved since z~1. We trace the extents and evolutions of both the blue cloud and red sequence, by fitting double Gaussians to the d4000 distribution of galaxies in narrow stellar mass bins, for four redshift intervals over 0 10^11 M_sun, d4000<1.55) drops sharply by a factor five between z~0.8 and z~0.5. These galaxies are becoming quiescent at a rate that largely matches the increase in the numbers of massive passive galaxies seen over this period. We examine the size-mass relation of blue cloud galaxies, finding that its high-mass boundary runs along lines of constant M*/r_e or equivalently inferred velocity dispersion. Larger galaxies can continue to form stars to higher stellar masses than smaller galaxies. As blue cloud galaxies approach this high-mass limit, they start to be quenched, their d4000 values increasing to push them towards the green valley. In parallel, their structures change, showing higher Sersic indices and central stellar mass densities. For these galaxies, bulge growth is necessary for them to reach the high-mass limit of the blue cloud and be quenched by internal mechanisms. The blue cloud galaxies that are being quenched at z~0.8 lie along the same size-mass relation as present day quiescent galaxies, and seem the likely progenitors of today's S0s.
Determinants of regular use of hearing aids among older adults in Tehran (Iran)

ABSTRACT The present study aimed to examine the determinants of the regular use of hearing aids among older adults.The data for this cross-sectional study was obtained from a study titled ‘Development and evaluation of a Structural Equation Model for Identifying Factors Associated with the Actual Use of Hearing Aids among Older Adults with Hearing Loss in Tehran. ’ Briefly, 300 hearing users aged 60 and older residing in Tehran were selected using stratified random sampling and administered the study’s self-assessment instruments. SPSS (v. 24) software was used to analyze data using descriptive statistics, independent t-test, chi-square, and binary logistic regression analysis.The mean age of the participants was 71.38 (SD=8). Of the study population, 50.7% were female, and 49.3% were male. In addition, 63.3% of the participants used hearing aids regularly. The multiple logistic regression model controlling the simultaneous effect of the variables indicated that the regular use of hearing aids was influenced by a variety of factors, including education level, hearing aid satisfaction, self-reported hearing impairment, perceived social support, extroversion personality trait, and emotional stability (P≤.05). The main findings of the present study can aid hearing healthcare providers in designing effective interventions and strategies and promoting the regular use of hearing aids among older adults by improving their understanding of the associated factors.
Electron Capture Supernovae of Super-AGB Stars: Dependence on Central Density and Flame Physics

Stars of $\sim$ 8 - 10 $M_{\odot}$ on the main-sequence form strongly electron-degenerate O+Ne+Mg core and become super-AGB stars. If such an O+Ne+Mg core grows to 1.38 $M_\odot$, electron captures $^{20}$Ne$(e,\nu_e)^{20}$F$(e,\nu_e)^{20}$O take place and ignite a Ne-O deflagration at the center. In this paper, we perform two-dimensional hydrodynamics simulations of the propagation of the Ne-O flame to see whether such a flame induces a collapse of the O+Ne+Mg core due to electron capture behind the flame or trigger a thermonuclear explosion. We present a series of models to explore how the outcome depends on model parameters for the central density in the range from $10^{9.80}$ to $10^{10.20}$ g cm$^{-3}$, flame structure of both centered and off-centered ignition kernels, special and general relativistic effects, turbulent flame speed formula and the treatments of laminar burning phase. We find that the O+Ne+Mg core obtained from the stellar evolution calculation has a high tendency to collapse into a neutron star. We obtain the conditions which divide the electron-capture collapse or thermonuclear explosion. We discuss the nucleosynthesis constraints and the possible observational signals of this class of supernovae.
High cadence spectropolarimetry of moving magnetic features observed around a pore

Context. Moving magnetic features (MMFs) are small-size magnetic elements that are seen to stream out from sunspots, generally during their decay phase. Several observational results presented in the literature suggest them to be closely related to magnetic filaments that extend from the penumbra of the parent spot. Nevertheless, few observations of MMFs streaming out from spots without penumbra have been reported. The literature still lacks analyses of the physical properties of these features. Aims. We investigate physical properties of monopolar MMFs observed around a small pore that had developed penumbra in the days preceding our observations and compare our results with those reported in the literature for features observed around sunspots. Methods. We analyzed NOAA 11005 during its decay phase with data acquired at the Dunn Solar Telescope in the Fe i 617. 3n m and the Ca ii 854.2 nm spectral lines with IBIS, and in the G-band. The field of view showed monopolar MMFs of both polarities streaming out from the leading negative polarity pore of the observed active region. Combining different analyses of the data, we investigated the temporal evolution of the relevant physical quantities associated with the MMFs as well as the photospheric and chromospheric signatures of these features. Results. We show that the characteristics of the investigated MMFs agree with those reported in the literature for MMFs that stream out from spots with penumbrae. Moreover, observations of at least two of the observed features suggest them to be manifestations of emerging magnetic arches.
Néel-XXZ state overlaps: odd particle numbers and Lieb–Liniger scaling limit

We specialize a recently-proposed determinant formula (Brockmann, De Nardis, Wouters and Caux 2014 J. Phys. A: Math. Theor. 47 145003) for the overlap of the zero-momentum Néel state with Bethe states of the spin-1/2 XXZ chain to the case of an odd number of downturned spins, showing that it is still of ‘Gaudin-like’ form, similar to the case of an even number of down spins. We generalize this result to the overlap of q-raised Néel states with parity-invariant Bethe states lying in a nonzero magnetization sector. The generalized determinant expression can then be used to derive the corresponding determinants and their prefactors in the scaling limit to the Lieb–Liniger (LL) Bose gas. The odd number of down spins directly translates to an odd number of bosons. We furthermore give a proof that the Néel state has no overlap with non-parity-invariant Bethe states. This is based on a determinant expression for overlaps with general Bethe states that was obtained in the context of the XXZ chain with open boundary conditions (Pozsgay 2013 arXiv:1309.4593, Kozlowski and Pozsgay 2012 J. Stat. Mech. P05021, Tsuchiya 1998 J. Math. Phys. 39 5946). The statement that overlaps with non-parity-invariant Bethe states vanish is still valid in the scaling limit to LL which means that the Bose–Einstein condensate state (De Nardis, Wouters, Brockmann and Caux 2014 Phys. Rev. A 89 033601) has zero overlap with non-parity-invariant LL Bethe states.
COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies – III. Comparison with semi-analytic models of galaxy formation

We compare the semi-analytic models of galaxy formation of Fu et al. which track the evolution of the radial profiles of atomic and molecular gas in galaxies, with gas fraction scaling relations derived from a stellar mass-limited sample of 299 galaxies from the CO Legacy Database for GASS. These galaxies have measurements of the CO(1-0) line from the IRAM 30-m telescope and the HI line from Arecibo, as well as measurements of star formation rates, stellar masses, galaxy sizes and concentration parameters from GALEX+SDSS photometry. The models provide a good description of how condensed baryons in star-forming galaxies are partitioned into atomic and molecular gas and stars as a function of galaxy stellar mass and stellar surface density. The models do not reproduce the observed tight relation between stellar surface mass density and bulge-to-disc ratio in these galaxies. The current implementation of 'radio-mode feedback' in the models produces trends that disagree strongly with the data. In the models, gas cooling shuts down in nearly all galaxies in dark matter haloes above a mass of similar to 10(12) M-circle dot. As a result, stellar mass is the observable that best predicts whether a galaxy has little or no neutral gas, that is, whether a galaxy has been quenched. In contrast, our data show that quenching is largely independent of stellar mass. Instead, there are clear thresholds in bulge-to-disc ratio and in stellar surface density that demarcate the location of quenched galaxies in our chosen parameter space. We speculate that the disagreement between the models and the observations may be resolved if radial transport of gas from the outer disc is included as an additional bulge formation mechanism in the models. In addition, we propose that processes associated with bulge formation play a key role in depleting the neutral gas in galaxies and that gas accretion is suppressed in a significant fraction of galaxies following the formation of the bulge, even in dark matter haloes of low mass.
USING Hα MORPHOLOGY AND SURFACE BRIGHTNESS FLUCTUATIONS TO AGE-DATE STAR CLUSTERS IN M83

We use new WFC3 observations of the nearby grand-design spiral galaxy M83 to develop two independent methods for estimating the ages of young star clusters. The first method uses the physical extent and morphology of Hα emission to estimate the ages of clusters younger than τ ≈ 10 Myr. It is based on the simple premise that the gas in very young (τ< a few Myr) clusters is largely coincident with the cluster stars, is in a small, ring-like structure surrounding the stars in slightly older clusters since massive star winds and supernovae have had time to push out the natal gas (e.g., τ ≈ 5 Myr), and is in a larger ring-like bubble for still older clusters (i.e., ≈5–10 Myr). If no Hα is associated with a cluster it is generally older than ≈10 Myr. The second method is based on an observed relation between pixel-to-pixel flux variations within clusters and their ages. This method relies on the fact that the brightest individual stars in a cluster are most prominent at ages around 10 Myr, and fall below the detection limit (i.e., MV < −3.5) for ages older than about 100 Myr. Older clusters therefore have a smoother appearance and smaller pixel-to-pixel variations. The youngest clusters also have lower flux variations, hence the relationship is double valued. This degeneracy in age can be broken using other age indicators such as Hα morphology. These two methods are the basis for a new morphological classification system which can be used to estimate the ages of star clusters based on their appearance. We compare previous age estimates of clusters in M83 determined from fitting UBVIHα measurements using predictions from stellar evolutionary models with our new morphological categories and find good agreement, at the ≈95% level. The scatter within categories is ≈0.1 dex in log τ for young clusters (<10 Myr) and ≈0.5 dex for older (>10 Myr) clusters. A by-product of this study is the identification of 22 “single-star” H ii regions in M83, with central stars having ages ≈4 Myr.
Protostar Mass due to Infall and Dispersal

The mass of a protostar is calculated from the infall and dispersal of an isothermal sphere in a uniform background. For high contrast between peak and background densities and for short dispersal time td, the accretion is “self-limiting”; gas beyond the core is dispersed before it accretes, and the protostar mass approaches a time-independent value of low mass. For lower density contrast and longer dispersal time, the accretion “runs away”; gas accretes from beyond the core, and the protostar mass approaches massive star values. The final protostar mass is approximately the initial gas mass whose free-fall time equals td. This mass matches the peak of the IMF for gas temperature 10 K, peak and background densities 106 and 103 cm−3, respectively, and td comparable to the core free-fall time tcore. The accretion luminosity exceeds 1 L☉ for 0.1 Myr, as in the “Class 0” phase. For td/tcore = 0.4–0.8 and temperature 7-50 K, self-limiting protostar masses are 0.08-5 M☉. These protostar and core masses have ratio 0.4 ± 0.2, as expected if the core mass distribution and the initial mass function have the same shape.
On the migration-induced formation of the 9:7 mean motion resonance

We study formation of 9:7 mean motion resonance (MMR) as a result of convergent migration of two planets embedded in a disc. Depending on the migration parameters, initial orbits and planets' masses the system may pass through the resonance or enter it (permanently or temporarily). We illustrate that a stable equilibrium of the averaged system (a periodic orbit of the N-body model) is surrounded by the region of permanent resonance capture. The size of this region depends on the migration parameters as well as the planets mass ratio. A system located inside this region tends towards the equilibrium (the capture is permanent). On the other hand, the system located outside the region evolves away from the equilibrium and leaves the resonance. We verify recent results of Delisle et al. and Xu & Lai where they show that for $m_1 \lesssim m_2$ the equilibrium is unstable when the migration is added, so the capture cannot be permanent. We show that for particular migration parameters the situation may be reversed, i.e., the equilibria are unstable for $m_1 \gtrsim m_2$. We illustrate that 9:7~MMR consists of two modes separated with a separatrix. The inner one is centred at the equilibrium and the outer one has no equilibrium in its centre. A system located outside the region of stable capture evolves from the inner into the outer mode. The evolution occurs along families of periodic orbits of the averaged system, that play a crucial role in the dynamics of the system after the resonance capture.
Stochastic resonance for exploration geophysics

Stochastic resonance (SR) is a phenomenon in which signal to noise (SN) ratio gets improved by noise addition rather than removal as envisaged classically. SR was first claimed in climatology a few decades ago and then in other disciplines as well. The same as it is observed in natural systems, SR is used also for allowable SN enhancements at will. Here I report a proof of principle that SR can be useful in exploration geophysics. For this I perform high frequency GaussVanicek variance spectral analyses (GVSA) of model traces characterized by varying levels of complexity, completeness and pollution. This demonstration justifies all further research on SR in applied geophysics, as energy demands and depletion of reachable supplies potentially make SR vital in a near future.
Four-pion production in τ decays and e+ e-annihilation : An update

An improved description of four-pion production in electron-positron annihilation and in $\ensuremath{\tau}$-lepton decays is presented. The model amplitude is fitted to recent data from BABAR which cover a wide energy range and which were obtained exploiting the radiative return. Predicting $\ensuremath{\tau}$-decay distributions from ${e}^{+}{e}^{\ensuremath{-}}$ data and comparing these predictions with ALEPH and CLEO results, the validity of isospin symmetry is confirmed within the present experimental errors. A good description of two- and three-pion subdistributions is obtained. Special emphasis is put on the predictions for $\ensuremath{\omega}\ensuremath{\pi}(\ensuremath{\rightarrow}{\ensuremath{\pi}}^{+}{\ensuremath{\pi}}^{\ensuremath{-}}{\ensuremath{\pi}}^{0})$ in ${e}^{+}{e}^{\ensuremath{-}}$ annihilation and in $\ensuremath{\tau}$ decay. The model amplitude is implemented in the Monte Carlo generator PHOKHARA.
flavio: a Python package for flavour and precision phenomenology in the Standard Model and beyond

flavio is an open source tool for phenomenological analyses in flavour physics and other precision observables in the Standard Model and beyond. It consists of a library to compute predictions for a plethora of observables in quark and lepton flavour physics and electroweak precision tests, a database of experimental measurements of these observables, a statistics package that allows to construct Bayesian and frequentist likelihoods, and of convenient plotting and visualization routines. New physics effects are parameterised as Wilson coefficients of dimension-six operators in the weak effective theory below the electroweak scale or the Standard Model EFT above it. At present, observables implemented include numerous rare $B$ decays (including angular observables of exclusive decays, lepton flavour and lepton universality violating $B$ decays), meson-antimeson mixing observables in the $B_{d,s}$, $K$, and $D$ systems, tree-level semi-leptonic $B$, $K$, and $D$ decays (including possible lepton universality violation), rare $K$ decays, lepton flavour violating $\tau$ and $\mu$ decays, $Z$ pole electroweak precision observables, the neutron electric dipole moment, and anomalous magnetic moments of leptons. Not only central values but also theory uncertainties of all observables can be computed. Input parameters and their uncertainties can be easily modified by the user. Written in Python, the code does not require compilation and can be run in an interactive session. This document gives an overview of the features as of version 1.0 but does not represent a manual. The full documentation of the code can be found in its web site.
The ALMA early science view of FUor/EXor objects - IV. Misaligned outflows in the complex star-forming environment of V1647 Ori and McNeil's Nebula

Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) Fondo Nacional de Desarrollo Cientifico y Tecnologico (FONDECYT) 3150550 1171246 Millennium Science Initiative (Chilean Ministry of Economy) Nucleus RC 130007 National Aeronautics and Space Administration GO6-17013A Joint Committee of ESO/Government of Chile Science and Technology Foundation of Portugal (FCT) IF/00194/2015 Spanish Ministerio de Economia y Competitividad AYA2014-55840-P University of Oklahoma Homer L. Dodge endowed chair Netherlands Organisation for Scientific Research (NWO). 639.041. 439
Two Orders of Magnitude Variation in the Star Formation Efficiency across the Premerger Galaxy NGC 2276

We present the first spatially resolved (∼0.5 kpc) measurements of the molecular gas depletion time τdepl across the disk of the interacting spiral galaxy NGC 2276, a system with an asymmetric morphology in various star formation rate (SFR) tracers. To estimate τdepl, we use new NOEMA observations of the 12CO(1–0) emission tracing the bulk molecular gas reservoir in NGC 2276, and extinction-corrected Hα measurements obtained with the PMAS/PPaK integral field unit for robust estimates of the SFR. We find a systematic decrease in τdepl of 1–1.5 dex across the disk of NGC 2276, with a further, abrupt drop in τdepl of ∼1 dex along the galaxy’s western edge. The global τdepl in NGC 2776 is , consistent with literature measurements for the nearby galaxy population. Such a large range in τdepl on subkiloparsec scales has never previously been observed within an individual isolated or premerger system. When using a metallicity-dependent molecular gas conversion factor the variation decreases by 0.5 dex. We attribute the variation in τdepl to the influence of galactic-scale tidal forces and ram pressure on NGC 2276's molecular interstellar medium. Our observations add to the growing body of numerical and observational evidence that galaxy–galaxy interactions significantly modify the molecular gas properties and star-forming activity within galactic disks throughout the interaction, and not just during the final merger phase.
Frequency Of CD34 Expression In Acute Lymphoblastic Leukaemia And Its Correlation With Clinicopathological Characteristics: A Single Centre Experience From Pakistan.

Background This study was carried out to determine the frequency of CD34 positivity in acute lymphoblastic leukaemia (B-ALL) in our population and to report its association with the clinicopathological profile at the time of diagnosis. Methods The cross-sectional study was conducted at National Institute of Blood Diseases and Bone Marrow Transplantation, Karachi, Pakistan, from March 2020 till December 2020.Newly diagnosed patients were selected, from both genders and all age groups. Relevant history and findings of physical examination were recorded. Immunohistochemistry was done on trephine biopsy and molecular studies were carried on bone marrow aspirates or peripheral blood samples. Results Out of 105 patients enrolled, 67 (63.8%) were males, with a male to female ratio (M: F) 1.8:1. Of the total patients, 62 (59.04%) were above 15 years of age. CD34 was expressed in 73 (69.5%) cases. Lymphadenopathy, splenomegaly, and hepatomegaly were separately noted in context to CD 34 expression in 22 (66.6%), 24 (64.8%), and 14 (58.3%) patients, respectively. CNS disease was seen in a total of 3(2.75%) subjects, in which 2 (66.6%) of the patients had CD34 expression. Total 81 patients in our study fall into the high-risk group out of which CD 34 expression was seen in 58(71.6%) subjects. Cytogenetic analysis, BCR-ABL p190, and MLL gene rearrangement were investigated in all participants. Cytogenetic analysis revealed an abnormality in 20 (19%) cases out of which 13 (17.8%) cases were from CD34 positive group. Conclusion Our study reported CD34 expression in more than two-thirds of cases. High-risk disease was significantly associated with CD34 expression.
Thermofield dynamics extension of the open string field theory

We study the application of the rules of thermofield dynamics (TFD) to the covariant formulation of open-string field theory. We extend the states space and fields according to the duplication rules of TFD and construct the corresponding classical action. The result is interpreted as a theory whose fields would encode the statistical information of open strings. The physical spectrum of the free theory is studied through the cohomology of the extended Becchi, Rouet, Stora and Tyutin (BRST) charge, and, as a result, we get new fields in the spectrum emerging by virtue of the quantum entanglement, and, noticeably, it presents degrees of freedom that could be identified as those of closed strings. We also show, however, that their appearing in the action is directly related to the choice of the inner product in the extended algebra, so that different sectors of fields could be eliminated from the theory by choosing that product conveniently. Finally, we study the extension of the three-vertex interaction and provide a simple prescription for it of which the results at tree level agree with those of the conventional theory.