Miracle-dz/UniFAR-FTUs huggingface dataset:
Phenomenology of the partially aligned 2HDM with leptonic meson decays

In this paper we present a phenomenological analysis of the Partially Aligned Two Higgs Doublet Model (PA-2HDM) by using leptonic decays of mesons and [Formula: see text]–[Formula: see text] mixing. We focus our attention in a scenario where the leading contribution to FCNC is given by the tree-level interaction with the light pseudoscalar [Formula: see text] ([Formula: see text] GeV). We show how an underlying flavor symmetry controls FCNC in the quark and lepton couplings with the pseudoscalar, without alignment between Yukawa matrices. Upper bounds on the free parameters are calculated in the context of the leptonic decays [Formula: see text] and [Formula: see text] and [Formula: see text] mixing. Also, our assumptions imply that bounds on New Physics contribution in the quark sector coming from [Formula: see text] mixing impose an upper bound on the parameters for the leptonic sector. Finally we give predictions of branching ratios for leptonic decay of mesons with FCNC and LFV.
Long noncoding RNA HOXA‐AS2 regulates the expression of SCN3A by sponging miR‐106a in breast cancer

Breast cancer is the most commonly diagnosed cancer that affects women worldwide. This study aimed to investigate the competing endogenous RNAs (ceRNAs) mechanism in breast cancer. Microarray data were downloaded from the University of California Santa Cruz (UCSC) Xena database. The limma package was used to screen the differentially expressed messenger RNAs (DEMs) and differentially expressed long noncoding RNAs (DELs). Subsequently, functional analysis was performed using DAVID tool. After constructing the protein‐protein interaction (PPI) network, we identified the major gene modules using the Cytoscape software. Univariate survival analysis in the survival package was performed. Finally, the ceRNA regulatory network was constructed to identify the critical genes. A total of 1380 DEMs and 345 DELs were identified in breast cancer samples compared with normal samples. Functional enrichment analysis showed that DEMs were mainly involved in cell division, and cell cycle. We screened four major gene modules and identified the hub nodes in these functional modules. Several DEMs (including FABP7, C4BPA, and LAMB3) and three long noncoding RNAs (lncRNAs) (LINC00092, SLC26A4.AS1, and COLCA1) exhibited significant correlation with patients' survival outcomes. In the ceRNA network, the lncRNA HOXA‐AS2 regulated the expression level of SCN3A by interacting with hsa‐miR‐106a‐5p. Thus, our study investigated the ceRNA mechanism in breast cancer. The results showed that lncRNA HOXA‐AS2 might modulate the expression of SCN3A by sponging miR‐106a in breast cancer.
The H$\mathsf{\alpha}$ Galaxy Survey - III. Constraints on supernova progenitors from spatial correlations with H$\mathsf{\alpha}$ emission

Aims. We attempt to constrain progenitors of the different types of supernovae from their spatial distributions relative to star formation regions in their host galaxies, as traced by H α + [Nii] line emission. Methods. We analyse 63 supernovae which have occurred within galaxies from our H α survey of the local Universe. Three statistical tests are used, based on pixel statistics, H α radial growth curves, and total galaxy emission-line fluxes. Results. Many type II supernovae come from regions of low or zero emission line flux, and more than would be expected if the latter accurately traces high-mass star formation. We interpret this excess as a 40% “Runaway” fraction in the progenitor stars. Supernovae of types Ib and Ic do appear to trace star formation activity, with a much higher fraction coming from the centres of bright star formation regions than is the case for the type II supernovae. Type Ia supernovae overall show a weak correlation with locations of current star formation, but there is evidence that a significant minority, up to about 40%, may be linked to the young stellar population. The radial distribution of all core-collapse supernovae (types Ib, Ic and II) closely follows that of the line emission and hence star formation in their host galaxies, apart from a central deficiency which is less marked for supernovae of types Ib and Ic than for those of type II. Core-collapse supernova rates overall are consistent with being proportional to galaxy total luminosities and star formation rates; however, within this total the type Ib and Ic supernovae show a moderate bias towards more luminous host galaxies, and type II supernovae a slight bias towards lower-luminosity hosts.
INTEGRAL Field Spectroscopy of the Extended Ionized Gas in Arp 220

Integral field optical spectroscopy with the INTEGRAL system has been used to investigate for the first time the two-dimensional kinematic and ionization properties of the extended, warm, ionized gas in Arp 220 over an area of 75. ″0 × 40. ″0 (i.e., 28 × 15 kpc). The structure of the ionized gas is divided into well-identified regions associated with the X-ray-emitting plumes and extended lobes, previously studied in detail by McDowell and collaborators. The overall ionization state of the warm gas in the plumes and lobes, as traced by the [N II]/Hα line, is consistent with high-velocity shocks expanding in a neutral ambient medium. Changes in the ionization state of the gas along the major axis of the plumes are detected, in particular in the outer regions of the northwestern plume, where the transition between the main stellar body of the galaxy and a broad, low surface brightness tidal tail is located. If the plumes are produced by a starburst-driven galactic wind, the efficiency in the conversion of mechanical to radiation energy is a factor of at least 10 smaller than in galactic winds developed in edge-on spiral galaxies with well-defined rotation and axis of outflow. The kinematic properties of the lobes, with an average velocity of +8 km s-1 (east lobe) and -79 km s-1 (west lobe), are to a first order in agreement with the predictions of the merger scenario, according to which the lobes are tidally induced gas condensations produced during the merging process. The largest velocity gradients of 50 km s-1 kpc-1 and velocity deviations of up to +280 and -320 km s-1 from the systemic velocity are associated not with the plumes but with the outer stellar envelope and broad tidal tails at distances of up to 7.5 kpc, indicating that the large-scale kinematics of the extended ionized gas in Arp 220 is most likely dominated by the tidally induced motions, and not by galactic winds associated with nuclear starbursts.
Zoom-in cosmological hydrodynamical simulation of a star-forming barred, spiral galaxy at redshift z = 2

We present gas and stellar kinematics of a high-resolution zoom-in cosmological chemodynamical simulation, which fortuitously captures the formation and evolution of a star-forming barred spiral galaxy, from redshift z ∼ 3 to z ∼ 2 at the peak of the cosmic star formation rate. The galaxy disc grows by accreting gas and substructures from the environment. The spiral pattern becomes fully organized when the gas settles from a thick (with vertical dispersion σv > 50 km s−1) to a thin (σv ∼ 25 km s−1) disc component in less than 1 Gyr. Our simulated disc galaxy also has a central X-shaped bar, the seed of which formed by the assembly of dense gas-rich clumps by z ∼ 3. The star formation activity in the galaxy mainly happens in the bulge and in several clumps along the spiral arms at all redshifts, with the clumps increasing in number and size as the simulation approaches z = 2. We find that stellar populations with decreasing age are concentrated towards lower galactic latitudes, being more supported by rotation, and having also lower velocity dispersion; furthermore, the stellar populations on the thin disc are the youngest and have the highest average metallicities. The pattern of the spiral arms rotates like a solid body with a constant angular velocity as a function of radius, which is much lower than the angular velocity of the stars and gas on the thin disc; moreover, the angular velocity of the spiral arms steadily increases as a function of time, always keeping its radial profile constant. The origin of our spiral arms is also discussed.
Photometric and spectroscopic evolution of the Type IIP supernova SN 2004et

We present optical photometry and spectroscopy of the normal type IIP supernova SN2004A, which was discovered in the galaxy NGC 6207 on 2004 January 9.84UT. Early observations indicated that the supernova was discovered at about two weeks since explosion. We estimate the distance to NGC 6207 to be 20.35 \pm 4.5 Mpc using the Standard Candle method. Using this distance, we estimate the ejected nickel mass in the explosion to be 0.032 \pm 0.02M\odo\cdot. The plateau luminosity, its duration (about 80 days) and the expansion velocity of the supernova ejecta at the middle of the plateau indicate an explosion energy of 4.7 \pm 2.7 x 10^50 ergs and an ejected envelope mass of 7.2 \pm 2.2M\odot\cdot . The ejected envelope mass implies a main sequence mass of 10 2.5\pm M\odot\cdot for the progenitor.
Backward Scattering and Coexistent State in Two-Dimensional Electron System

The results of the mean field studies on the effects of the backward scattering with large momentum transfer in a two-dimensional electron system are extended to the case with various types of the Fermi surface and coupling constants. It is found that the coexistent state of d -wave superconductivity, antiferromagnetism and π-triplet pair can be stabilized quite generally near half filling.
Thermal contact: mischief and time scales

We discuss what kind of quantum dynamics can yield thermalization. We show that any temperature measurement protocol must be sensitive to the system’s local energy scale, not just its state. Specifically, we illustrate this by showing that any temperature measurement protocol that does not resolve the system’s local Hamiltonian (such as, e.g. full state tomography) is susceptible to being fooled into measuring any value for the temperature. Since placing a system in thermal contact with a reference system at a known temperature is a way of measuring temperature, any robust notion of thermal contact must be resistant to this ‘attack’. This provides us with a necessary conditions for thermal contact between quantum systems. We then apply this condition to a scenario where one expects to find thermalization: a system repeatedly interacting with the microconstitutents of a thermal reservoir. We show such models of thermalization cannot be correct without fine-tuning.
A Westerbork survey of rich clusters of galaxies. III - Observations of the Coma Cluster at 610 MHz

An area of 1.6 deg in radius about the centre of the Cancer Cluster has been surveyed at 610 MHz with the Westerbork telescope. The minimum detectable flux in the full synthesis map obtained is 2.5 mJy (4 r.m.s. noise), which at the distance of 46 Mpc corresponds to P equals 6 x 10 to the 20th W/Hz. Two (E plus SO) galaxies and seven (S plus 1) galaxies belonging to the cluster have been detected, and these are used to construct the Radio Luminosity Function of this cluster. The results for both the ellipticals and the spirals are in agreement with those obtained for galaxies of the same type outside rich clusters. The reasonable statistics achieved in the optical interval Mx varies between -19 and no greater than -18 show that still about 50 percent of the spirals and irregulars have radio power below 6 x 10 to the 20th W/Hz. The peculiar S galaxy Zw 119-55 studied by Tifft et al. (1973) is the strongest radio source in this cluster, P equals 1.3 x 10 to the 22nd W/Hz.
of Pre-College Engineering Education Research (J-PEER) Journal of Pre-College Engineering Education Research (J-PEER) Do After-School Robotics Programs Expand the Pipeline into Do After-School Robotics Programs Expand the Pipeline into STEM Majors in College? STEM Majors in College?

Abstract One result of the growing concerns over the numbers of young people moving into science, technology, engineering and mathematics (STEM)-related careers has been the expansion of formal and informal STEM education programming for pre-college youth, from elementary school through high school. While the number of programs has grown rapidly, there is little research on their long-term impacts on participant education and career trajectories. This paper presents interim findings from a multi-year longitudinal study of three national after-school robotics programs that engage students in designing, building, and competing complex robots with the goal of inspiring long-term interest in STEM. Focusing on the subset of study participants who had enrolled in at least one year of college (approximately 480 students in 2017), this paper examines program impacts on student attitudes towards STEM and STEM careers; participation in STEM-related college courses; intention to major in STEM-related fields; and involvement in STEM-related internships and other activities. Findings include positive, statistically significant impact on multiple measures of STEM engagement in college for program participants. Abstract One result of the growing concerns over the numbers of young people moving into science, technology, engineering and mathematics (STEM)-related careers has been the expansion of formal and informal STEM education programming for pre-college youth, from elementary school through high school. While the number of programs has grown rapidly, there is little research on their long-term impacts on participant education and career trajectories. This paper presents interim findings from a multi-year longitudinal study of three national after-school robotics programs that engage students in designing, building, and competing complex robots with the goal of inspiring long-term interest in STEM. Focusing on the subset of study participants who had enrolled in at least one year of college (approximately 480 students in 2017), this paper examines program impacts on student attitudes towards STEM and STEM careers; participation in STEM-related college courses; intention to major in STEM-related fields; and involvement in STEM-related internships and other activities. Findings include positive, statistically significant impact on multiple measures of STEM engagement in college for program participants.
Chaotic correlation functions with complex fermions

We study correlation functions in the complex fermion SYK model. We focus, specifically, on the h=2 mode which explicitly breaks conformal invariance and exhibits the chaotic behaviour. We numerically explore a fermion six-point OTOC, with two and three real-time folds, respectively. While our approach is expected to yield an early-time chaotic growth, we nevertheless observe a near-maximal value. Following the program of Gross-Rosenhaus, we estimate the triple short time limit of the six point function. Unlike the conformal modes with high values of h, the h=2 mode has contact interaction dominating over the planar in the large q limit.
THE KINEMATICS OF GALACTIC SPIRAL STRUCTURE

An understanding of the states of motion of the stellar and gaseous components of spiral structure is fundamental to the problem of the origin and maintenance of spiral structure. It is important to determine the relative ordering of the parameters characterizing the several components of a spiral arm. In our own Galaxy in many cases, this can better be done in kinematic terms rather than spatially, since for the stars the results are then less sensitive to assumptions concerning the intervening absorption, while for the gas the results are less dependent on distance derivations. The data are becoming complete enough that, with appropriate analysis procedures, quantitative measures are available of the differential effects across spiral arms. Our understanding of a few of the various problems is less tentative for external galaxies than for our own. A substantial amount of the observational material can be satisfactorily interpreted in terms of the gravitational theory of density-waves. Furthermore, it is just this kinematic information which is most crucial for the observational confrontation of this theory.
Tunable bilayer two-dimensional electron gas in LaAlO3/SrTiO3 superlattices

We report magnetotransport properties of double heterointerfaces in LaAlO3/SrTiO3/LaAlO3/SrTiO3(001) (LAO/STO/LAO/STO). A strong nonlinearity in the Hall resistivity is found when the temperature is below 80 K. This effect is attributed to multichannel conduction of interfacial charges generated in double heterostructures of LAO/STO where two-dimensional electron gas (2DEG) is produced. The multichannel conduction is confirmed by back gating modulation of Hall effect. Our result suggests the possibility to achieve coupled bilayer 2DEG layers in LAO/STO superlattices.
Surface brightness correction for compact extended sources observed by the AKARI Far-Infrared Surveyor in the slow-scan mode

We present a general surface brightness correction method for compact extended sources imaged in the slow-scan pointed observation mode of the Far-Infrared Surveyor (FIS) aboard the AKARI Infrared Astronomical Satellite. Our method recovers correct surface brightness distribution maps by re-scaling archived raw FIS maps using the surface-brightness-dependent
Search for photon line-like signatures from Dark Matter annihilations with H.E.S.S.

Gamma-ray line signatures can be expected in the very-high-energy (Eγ > 100GeV) domain due to annihilation or decay of Dark Matter particles in space. Such a signal would be readily distinguishable from astrophysical gamma-ray sources that in most cases produce continuous spectra which span over several orders of magnitude in energy. Using data collected by the H.E. S.S. gamma-ray instrument, upper limits on line emission and signatures produced by internal photon bremsstrahlung are obtained in the energy range between 500 GeV and 25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. For the process χχ → γγ, limits are derived on the velocity-averaged DM annihilation cross section , based on the Einasto parametrization of the Galactic DM halo.
THE ENSEMBLE VARIABILITY PROPERTIES OF FAINT QSOS

A refined sample of 64 variable objects with stellar image structure has been identified in SA 57 to B approximately = 22.5, over a time baseline of 15 yr, sampled at 11 distinct epochs. The photometric data typically have a root-mean-square (rms) error at B = 22 of only 0.05 mag. Thirty-five quasars in this field have already been spectroscopically confirmed, 34 of which are among the sample of variables. Of the other variables, six are known spectroscopically to be stars, 10 additional objects are stars based on reliable detection of proper motion, and one is spectroscopically a narrow emission line galaxy. Of the 13 remaining variables, it is argued that they are a mixture of distant halo subdwarfs and quasars with starlike colors. We compute the ensemble average structure function and autocorrelation function from the light curves in the respective quasar rest frames, which are used to investigate the general dependences on apparent magnitude, absolute magnitude, and redshift.
Turbulent Angular Momentum Transport in Weakly-Ionized Accretion Disks

Understanding the mechanism that drives accretion has been the primary challenge in accretion disk theory. Turbulence provides a natural means of dissipation and the removal of angular momentum, but firmly establishing its presence in disks proved for many years to be difficult. The realization in the 1990s that a weak magnetic field will destabilize a disk and result in a vigorous turbulent transport of angular momentum has revolutionized the field. Much of accretion disk research now focuses on understanding the implications of this mechanism for astrophysical observations. At the same time, the success of this mechanism depends upon a sufficient ionization level in the disk for the flow to be well-coupled to the magnetic field. Many disks, such as disks around young stars and disks in binary systems that are in quiescence, are too cold to be sufficiently ionized, and so efforts to establish the presence of turbulence in these disks continues. This dissertation focuses on several possible mechanisms for the turbulent transport of angular momentum in weakly-ionized accretion disks: gravitational instability, radial convection and vortices driving compressive motions. It appears that none of these mechanisms are very robust in driving accretion. A discussion is given, based on these results, as to the most promising directions to take in the search for a turbulent transport mechanism that does not require magnetic fields. Also discussed are the implications of assuming that no turbulent transport mechanism exists for weakly-ionized disks.
Dynamical quantum phase transitions in collapse and revival oscillations of a quenched superfluid

In this work we revisit collapse and revival oscillations in superfluids suddenly quenched by strong local interactions for the case of a one-dimensional Bose-Hubbard model. As the main result we identify the inherent nonequilibrium quantum many-body character of these oscillations by revealing that they are controlled by a sequence of underlying dynamical quantum phase transitions in the real-time evolution after the quench, which manifest as temporal nonanalyticities in return probabilities or Loschmidt echos. Specifically, we find that the time scale of the collapse and revival oscillations is, firstly, set by the frequency at which dynamical quantum phase transitions appear, and is, secondly, of emergent nonequilibrium nature, since it is not only determined by the final Hamiltonian but also depends on the initial condition.