Miracle-dz/UniFAR-FTUs huggingface dataset:
Formation of Cyanoformaldehyde in the interstellar space

Cyanoformaldehyde (HCOCN) molecule has recently been suspected towards the Sagittarius B2(N) by the Green Bank telescope, though a confirmation of this observation has not yet been made. In and around a star forming region, this molecule could be formed by the exothermic reaction between two abundant interstellar species, H2CO and CN. Till date, the reaction rate coefficient for the formation ofthis molecule is unknown. Educated guesses were used to explain the abundance of this molecule by chemical modeling. In this paper, we carried out quantum chemical calculations to find out empirical rate coefficients for the formation of HCOCN and different chemical properties during the formation of HCOCN molecules. Though HCOCN is stable against unimolecular decomposition, this gas phase molecule could be destroyed by many other means, like: ion-molecular reactions or by the effect of cosmic rays. Ionmolecular reaction rates are computed by using the capture theories. We have also included the obtained rate coefficients into our large gas-grain chemical network to study the chemical evolution of these species in various interstellar conditions. Formation of one of the isotopologue(DCOCN) of HCOCN is also studied. Our study predicts the possibility of finding HCOCN and DCOCN in the ice phase with a reasonably high abundance. In order to detect HCOCN or DCOCN in various interstellar environments, it is necessary to know the spectroscopic properties of these molecules. To this effect, we carried out quantum chemical calculations to find out different spectral parameters of HCOCN for the transition in electronic, infrared and rotational modes. We clearly show how the isotopic substitution (DCOCN) plays a part in the vibrational progressions of HCOCN.
Comparison between numerical-relativity and post-Newtonian waveforms from spinning binaries: The orbital hang-up case

We compare results from numerical simulations of spinning binaries in the ‘‘orbital hang-up’’ case, where the binary completes at least nine orbits before merger, with post-Newtonian results using the approximants Taylor T1, T4, and Et. We find that, over the ten cycles before the gravitational-wave frequency reaches M! ¼ 0:1, the accumulated phase disagreement between numerical relativity (NR) and 2.5 post-Newtonian (PN) results is less than three radians, and is less than 2.5 radians when using 3.5PN results. The amplitude disagreement between NR and restricted PN results increases with the black holes’ spin, from about 6% in the equal-mass case to 12% when the black holes’ spins are Si=M 2 ¼ 0:85. Finally, our results suggest that the merger waveform will play an important role in estimating the spin from such inspiral waveforms.
COHERENT PIONS FROM NEUTRINO SCATTERING OFF NUCLEI

We describe a model for pion production off nucleons and coherent pions from nuclei induced by neutrinos in the 1 GeV energy regime. Besides the dominant Delta pole contribution, it takes into account the effect of background terms required by chiral symmetry. Moreover, the model uses a reduced nucleon-to-Delta resonance axial coupling, which leads to coherent pion production cross sections around a factor two smaller than most of the previous theoretical estimates. Nuclear effects like medium corrections on the Delta propagator and final pion distortion are included.
A two-step optimised BERT-based natural language processing algorithm

Sentiment analysis involving the identification of sentiment polarities from textual data is a very popular area of research. Many research works that have explored and extracted sentiments from textual data such as financial news have been able to do so by employing BERT-based NLP algorithms in applications with high computational needs, and also by manually labelling sample data with help from financial experts. We propose an approach which makes possible the development of quality NLP models without the need for high computing power, or inputs from financial experts in labelling focused dataset for NLP model development. Our approach introduces a two-step optimised BERT-based NLP model for extracting sentiments from financial news. Our work shows that with little effort that involves manually labelling a small but relevant and focused sample data of financial news, one could achieve a high performing and accurate multi-class NLP model on financial news.
COOL YOUNG STARS IN THE NORTHERN HEMISPHERE: β PICTORIS AND AB DORADUS MOVING GROUP CANDIDATES

As part of our continuing effort to identify new, low-mass members of nearby, young moving groups (NYMGs), we present a list of young, low-mass candidates in the northern hemisphere. We used our proven proper-motion selection procedure and ROSAT X-ray and GALEX-UV activity indicators to identify 204 young stars as candidate members of the β Pictoris and AB Doradus NYMGs. Definitive membership assignment of a given candidate will require a measurement of its radial velocity and distance. We present a simple system of indices to characterize the young candidates and help prioritize follow-up observations. New group members identified in this candidate list will be high priority targets for (1) exoplanet direct imaging searches, (2) the study of post-T-Tauri astrophysics, (3) understanding recent local star formation, and (4) the study of local galactic kinematics. Information available now allows us to identify eight likely new members in the list. Two of these, a late-K and an early-M dwarf, we find to be likely members of the β Pic group. The other six stars are likely members of the AB Dor moving group. These include an M dwarf triple system, and three very cool objects that may be young brown dwarfs, making them the lowest-mass, isolated objects proposed in the AB Dor moving group to date.
The Factors of Millennials’ Continuance Intention to Use Digital Wallets in Indonesia

The growth of digital wallets increases the convenience of consumers in making transactions. The convenience that consumers feel in using digital wallets further increases their consumption. Companies influence the age group, such as millennials, with high potential in using digital wallets. The research emphasized the consumer behavior of millennials in using digital wallets. The study aimed to examine the variables that affected digital wallet users in terms of perceived usefulness, perceived risk, customer attitude, customer satisfaction, and continuance intention to use. The questionnaire was distributed using the G-form using the determination of respondents by purposive sampling. The number of respondents was 276. The measurement of reliability and validity used loadings values, Cronbach’s alpha, Composite Reliability (CR), Average Variance Extracted (AVE), and discriminant validity. In measuring the fit model, the Standardized Root Mean Square Residual (SRMR) value was used. Then, the research used Partial Least Square-Structural Equation Model (PLS-SEM) to test the hypothesis. The results show that perceived usefulness affects customer attitudes toward using digital wallets. Meanwhile, perceived risk has no effect on customer attitudes. Customer attitude impacts customer satisfaction and continuance intention to use digital wallet users directly and indirectly. Moreover, millennials strengthen the influence of customer attitude on continuance intention to use. The effect is negative, meaning that if the age of the millennials increases, it will cause a decreased attitude change towards continuance intention to use digital wallets.
Influence of Demographic Factors on Retirement Planning and Socio-Economic Status of Civil Servants in Uganda: Reflections from Pensioners from Busoga Sub-Region

This study provides a Ugandan perspective on the influence of demographic factors on retirement planning and the socio-economic status of civil servants. The study collected data from 236 pensioners using a questionnaire survey. The demographic factors included gender, marital status, age, income, and educational level. Using multiple regression, the study concludes that there is a low predictive influence of demographic factors on retirement planning and socio-economic status. Only educational level and monthly income have significant influences on retirement planning and the socioeconomic status of the retirees. This study offers a solid ground for increasing civil servants’ salaries in Uganda. Also, the government may consider identifying resources for the professional development needs of civil servants.
LONG-TIMESCALE BEHAVIOR OF THE BLAZHKO EFFECT FROM RECTIFIED KEPLER DATA

In order to benefit from the four year unprecedented precision of the Kepler data, we extracted light curves from the pixel photometric data of the Kepler space telescope for 15 Blazhko RR Lyrae stars. To collect all the flux from a given target as accurately as possible, we defined tailor-made apertures for each star and quarter. In some cases, the aperture finding process yielded sub-optimal results, because some flux have been lost even if the aperture contains all available pixels around the star. This fact stresses the importance of those methods that rely on the whole light curve instead of focusing on the extrema (O − C diagrams and other amplitude independent methods). We carried out detailed Fourier analysis of the light curves and the amplitude independent O − C diagram. We found 12 (80%) multiperiodically modulated stars in our sample. This ratio is much higher than previously found. Resonant coupling between radial modes, a recent theory for explaining the Blazhko effect, allows single, multiperiodic, or even chaotic modulations. Among the stars with two modulations, we found three stars (V355 Lyr, V366 Lyr, and V450 Lyr) where one of the periods dominates in amplitude modulation, but the other period has a larger frequency modulation amplitude. The ratio between the primary and secondary modulation periods is almost always very close to the ratios of small integer numbers. It may indicate the effect of undiscovered resonances. Furthermore, we detected the excitation of the second radial overtone mode f2 for three stars where this feature was formerly unknown. Our data set comprises the longest continuous, most precise observations of Blazhko RR Lyrae stars ever published. These data are made publicly available and will be unrivaled for years to come.
Optimizing weak lensing mass estimates for cluster profile uncertainty

Weak lensing measurements of cluster masses are necessary for calibrating mass-observable relations (MORs) to investigate the growth of structure and the properties of dark energy. However, the measured cluster shear signal varies at fixed massM200m due to inherent ellipticity of background galaxies, intervening structures along the line of sight and variations in the cluster structure due to scatter in concentrations, asphericity and substructure. We use N-body simulated haloes to derive and evaluate a weak lensing circular aperture mass measurement Map that minimizes the mass estimate variance � (Map − M200m) 2 � in the presence of all these forms of variability. Depending on halo mass and observational conditions, the resulting mass estimator improves on Map filters optimized for circular NFW-profile clusters in the presence of uncorrelated large-scale structure (LSS) about as much as the latter improve on an estimator that only minimizes the influence of shape noise. Optimizing for uncorrelated LSS while ignoring the variation of internal cluster structure puts too much weight on the profile near the cores of haloes, and under some circumstances can even be worse than not accounting for LSS at all. We briefly discuss the impact of variability in cluster structure and correlated structures on the design and performance of weak lensing surveys intended to calibrate cluster MORs.
Optical excitations in electron microscopy

This review discusses how low-energy, valence excitations created by swift electrons can render information on the optical response of structured materials with unmatched spatial resolution. Electron microscopes are capable of focusing electron beams on sub-nanometer spots and probing the target response either by analyzing electron energy losses or by detecting emitted radiation. Theoretical frameworks suited to calculate the probability of energy loss and light emission (cathodoluminescence) are revisited and compared with experimental results. More precisely, a quantum-mechanical description of the interaction between the electrons and the sample is discussed, followed by a powerful classical dielectric approach that can be in practice applied to more complex systems. We assess the conditions under which classical and quantum-mechanical formulations are equivalent. The excitation of collective modes such as plasmons is studied in bulk materials, planar surfaces, and nanoparticles. Light emission induced by the electrons is shown to constitute an excellent probe of plasmons, combining sub-nanometer resolution in the position of the electron beam with nanometer resolution in the emitted wavelength. Both electron energy-loss and cathodoluminescence spectroscopies performed in a scanning mode of operation yield snap shots of plasmon modes in nanostructures with fine spatial detail as compared to other existing imaging techniques, thus providing an ideal tool for nanophotonics studies.
THE ALIGNMENT OF THE POLARIZATION OF HERBIG Ae/Be STARS WITH THE INTERSTELLAR MAGNETIC FIELD

We present a study of the correlation between the direction of the symmetry axis of the circumstellar material around intermediate mass young stellar objects and that of the interstellar magnetic field. We use CCD polarimetric data on 100 Herbig Ae/Be stars. A large number of them show intrinsic polarization, which indicates that their circumstellar envelopes are not spherical. The interstellar magnetic field direction is estimated from the polarization of field stars. There is an alignment between the position angle of the Herbig Ae/Be star polarization and that of the field stars for the most polarized objects. This may be an evidence that the ambient interstellar magnetic field plays a role in shaping the circumstellar material around young stars of intermediate mass and/or in defining their angular momentum axis.
Theoretical support for the {pi}(1300) and the recently claimed f{sub 0}(1790) as molecular resonances

A study of three-pseudoscalar {pi}KK and {pi}{pi}{eta} coupled system is made by solving the Faddeev equations within an approach based on unitary chiral dynamics. A resonance with total isospin one and spin-parity J{sup {pi}=}0{sup -} is found with mass {approx}1400 MeV when the KK system gets reorganized as the f{sub 0}(980). This resonance is identified with the {pi}(1300) listed by the Particle Data Group. Further, the two-body amplitude which describes the interaction between a {pi} and the f{sub 0}(980) is extracted from the study of the {pi}KK and {pi}{pi}{eta} system and is then employed to study the f{sub 0}(980){pi}{pi} system. As a result, a scalar resonance is found near 1790 MeV which drives the two f{sub 0}(980){pi} systems to resonate as the {pi}(1300) while the invariant mass of the two pions falls in the mass region of the scalar {sigma}(600). These findings support the existence of a new f{sub 0} resonance near 1790 MeV, as found by the BES and Crystal Barrel collaborations. Our results show that this f{sub 0}(1790) is definitely distinct to f{sub 0}(1710), the latter of which seems to possess a glueball structure dominantly.
Origin of the antihierarchical growth of black holes

Observational studies have revealed a “downsizing” trend in black hole (BH) growth: the number densities of luminous AGN peak at higher redshifts than those of faint AGN. This would seem to imply that massive black holes formed before low mass black holes, in apparent contradiction to hierarchical clustering scenarios. We investigate whether this observed “downsizing” in BH growth is reproduced in a semianalytic model for the formation and evolution of galaxies and black holes, set within the hierarchical paradigm for structure formation (Somerville et al. 2008; S08). In this model, black holes evolve from light seeds (� 100M⊙) and their growth is mergerdriven. The original S08 model (baseline model) reproduces the number density of AGN at intermediate redshifts and luminosities, but underproduces luminous AGN at very high redshift (z > 3) and overproduces them at low redshift (z < 1). In addition, the baseline model underproduces low-luminosity AGN at low redshift (z < 1). In order to solve these problems, we consider several modifications to the physical processes in the model: (1) a ‘heavy’ black hole seeding scenario (2) a sub-Eddington accretion rate ceiling that depends on the cold gas fraction, and (3) an additional black hole accretion mode due to disk instabilities. With these three modifications, the models can explain the observed downsizing, successfully reproduce the bolometric AGN luminosity function and simultaneously reproduce galaxy and black hole properties in the local Universe. We also perform a comparison with the observed soft and hard X-ray luminosity functions of AGN, including an empirical correction for torus-level obscuration, and reach similar conclusions. Our best-fit model suggests a scenario in which disk instabilities are the main driver for moderately luminous Seyfert galaxies at low redshift, while major mergers are the main trigger for luminous AGN.
Ammonia observations in the LBV nebula G79.29+0.46 - Discovery of a cold ring and some warm spots

The surroundings of Luminous Blue Variable (LBV) stars are excellent laboratories to study the effects of their high UV radiation, powerful winds, and strong ejection events onto the surrounding gas and dust. The LBV G79.29+0.46 powered two concentric infrared rings which may interact with the infrared dark cloud (IRDC) G79.3+0.3. The Effelsberg 100m telescope was used to observe the NH_3 (1,1), (2,2) emission surrounding G79.29+0.46 and the IRDC. In addition, we observed particular positions in the (3,3) transition toward the strongest region of the IRDC. We report here the first coherent shell-like structure of dense NH_3 gas associated with an evolved massive star. The shell, two or three orders of magnitude more tenuous than the IRDC, is well traced in both ammonia lines, and surrounds the ionized nebula. The NH_3 emission in the IRDC is characterized by a low and uniform rotational temperature (T_rot ~ 10 K) and moderately high opacities in the (1,1) line. The rest of the observed field is spotted by warm or hot zones (T_rot > 30 K) and characterized by optically thin emission of the (1,1) line. The NH_3 abundances are about 10^{-8} in the IRDC, and 10^{-10}-10^{-9} elsewhere. The warm temperatures and low abundances of NH_3 in the shell suggest that the gas is being heated and photo-dissociated by the intense UV field of the LBV star. An outstanding region is found to the south-west (SW) of the LBV star within the IRDC. The NH_3 (3,3) emission at the centre of the SW region reveals two velocity components tracing gas at temperatures > 30K. The northern edge of the SW region agrees with the border of the ring nebula and a region of continuum enhancement; here, the opacity of the (1,1) line and the NH_3 abundance do not decrease as expected in a typical clump of an isolated cold dark cloud. This strongly suggests some kind of interaction between the ring nebula and the IRDC.
Cryogenic resonant microwave cavity searches for hidden sector photons

The hidden sector photon is a weakly interacting hypothetical particle with sub-eV mass that kinetically mixes with the photon. We describe a microwave frequency light shining through a wall experiment where a cryogenic resonant microwave cavity is used to try and detect photons that have passed through an impenetrable barrier, a process only possible via mixing with hidden sector photons. For a hidden sector photon mass of 53 $\mu$eV we limit the hidden photon kinetic mixing parameter $\chi < 1.7\times10^{-7}$, which is an order of magnitude lower than previous bounds derived from cavity experiments in the same mass range. In addition, we use the cryogenic detector cavity to place new limits on the kinetic mixing parameter for hidden sector photons as a form of cold dark matter.
Heating and enriching the intracluster medium

We present numerical simulations of galaxy clusters with stochastic heating from active galactic nuclei (AGN) that are able to reproduce the observed entropy and temperature profiles of non-cool-core (NCC) clusters. Our study uses N-body hydrodynamical simulations to investigate how star formation, metal production, black hole accretion and the associated feedback from supernovae and AGN heat and enrich diffuse gas in galaxy clusters. We assess how different implementations of these processes affect the thermal and chemical properties of the intracluster medium (ICM), using high-quality X-ray observations of local clusters to constrain our models. For the purposes of this study we have resimulated a sample of 25 massive galaxy clusters extracted from the Millennium Simulation. Sub-grid physics is handled using a semi-analytic model of galaxy formation, thus guaranteeing that the source of feedback in our simulations is a population of galaxies with realistic properties. We find that supernova feedback has no effect on the entropy and metallicity structure of the ICM, regardless of the method used to inject energy and metals into the diffuse gas. By including AGN feedback, we are able to explain the observed entropy and metallicity profiles of clusters, as well as the X-ray luminosity–temperature scaling relation for NCC systems. A stochastic model of AGN energy injection motivated by anisotropic jet heating – presented for the first time here – is crucial for this success. With the addition of metal-dependent radiative cooling, our model is also able to produce CC clusters, without overcooling of gas in dense, central regions.
Few remarks on the Higgs boson decays in gauge-Higgs unification

In the scenario of gauge-Higgs unification, the origin of the Higgs boson is the higher-dimensional gauge boson. Very characteristic predictions are made of the Higgs boson interactions in this scenario, reflecting its origin. In particular, a remarkable claim has been made: the contribution of nonzero Kaluza-Klein modes to the Higgs decay $H\ensuremath{\rightarrow}Z\ensuremath{\gamma}$ exactly vanishes in the minimal SU(3) electroweak unified model, at least at the one-loop level. In this brief paper, in order to see whether this prediction is a general feature of the scenario or the consequence of the specific choice of the model, matter content, or the order of perturbative expansion, we perform an operator analysis. We demonstrate that no relevant operator exists, respecting the gauge symmetry SU(3) in the bulk. We also comment on the possibly important contribution to the photonic decay $H\ensuremath{\rightarrow}\ensuremath{\gamma}\ensuremath{\gamma}$ due to the nonzero Kaluza-Klein modes of light quarks.
The effects of a magnetic field on planetary migration in laminar and turbulent discs

We investigate the migration of low-mass planets ($5 M_{\oplus}$ and $20 M_{\oplus}$) in accretion discs threaded with a magnetic field using 2D MHD code in polar coordinates. We observed that, in the case of a strong azimuthal magnetic field where the plasma parameter is $\beta\sim 1-2$, density waves at the magnetic resonances exert a positive torque on the planet and may slow down or reverse its migration. However, when the magnetic field is weaker (i.e., the plasma parameter $\beta$ is relatively large), then non-axisymmetric density waves excited by the planet lead to growth of the radial component of the field and, subsequently, to development of the magneto-rotational instability, such that the disc becomes turbulent. Migration in a turbulent disc is stochastic, and the migration direction may change as such. To understand migration in a turbulent disc, both the interaction between a planet and individual turbulent cells, as well as the interaction between a planet and ordered density waves, have been investigated.