Miracle-dz/UniFAR-FTUs huggingface dataset:
iPTF16abc and the population of Type Ia supernovae: comparing the photospheric, transitional, and nebular phases

Key information about the progenitor system and the explosion mechanism of Type Ia supernovae (SNe Ia) can be obtained from early observations, within a few days from explosion. iPTF16abc was discovered as a young SN Ia with excellent early time data. Here, we present photometry and spectroscopy of the SN in the nebular phase. A comparison of the early time data with a sample of SNe Ia shows distinct features, differing from normal SNe Ia at early phases but similar to normal SNe Ia at a few weeks after maximum light (i.e. the transitional phase) and well into the nebular phase. The transparency time-scales (t_0) for this sample of SNe Ia range between ∼25 and 41 d indicating a diversity in the ejecta masses. t_0 also weakly correlates with the peak bolometric luminosity, consistent with the interpretation that SNe with higher ejecta masses would produce more ^(56)Ni . Comparing the t_0 and the maximum luminosity, L_(max) distribution of a sample of SNe Ia to predictions from a wide range of explosion models we find an indication that the sub-Chandrasekhar mass models span the range of observed values. However, the bright end of the distribution can be better explained by Chandrasekhar mass delayed detonation models, hinting at multiple progenitor channels to explain the observed bolometric properties of SNe Ia. iPTF16abc appears to be consistent with the predictions from the M_(ch) models.
User Musical Taste Prediction Technique Using Music Metadata and Features

The digital music market has been growing significantly in the past years. In music streaming services, music recommendation plays a key role, but Korean users’ recognition about their music service is not high because the service’s recommendation accuracy is not good. Therefore, this paper suggests technique to predict the user’s musical taste. This technique proceeds through a four-step process; data collection, data pre-processing, feature extraction, and machine learning. Collection of data was taken from TOP 100 chart in ‘Melon’, the number one music service provider in Korea from December 2013 to March 2015. Then, collected MP3 file format is converted into WAV file format. In the stage of feature extraction, we classify the genre from the music’s metadata and extract factors that can be taken using STFT’s ZCR, Spectral Rolloff, Spectral Flux. In the stage of machine learning, we produce a prediction model in a variety of classification techniques. To measure the performance of the created prediction model, 456 data were used for training dataset and 130 data were used for validation dataset. Since the results of experiment show an average of 78% of accuracy, the proposed technique seems to be effective.
The signature of dark energy perturbations in galaxy cluster surveys

Models of dynamical dark energy unavoidably possess fluctuations in the energy density and pressure of that new component. In this paper we estimate the impact of dark energy fluctuations on the number of galaxy clusters in the Universe using a generalization of the spherical collapse model and the Press-Schechter formalism. The observations we consider are several hypothetical Sunyaev-Zel'dovich and weak lensing (shear maps) cluster surveys, with limiting masses similar to ongoing (SPT, DES) as well as future (LSST, Euclid) surveys. Our statistical analysis is performed in a 7-dimensional cosmological parameter space using the Fisher matrix method. We find that, in some scenarios, the impact of these fluctuations is large enough that their effect could already be detected by existing instruments such as the South Pole Telescope, when priors from other standard cosmological probes are included. We also show how dark energy fluctuations can be a nuisance for constraining cosmological parameters with cluster counts, and point to a degeneracy between the parameter that describes dark energy pressure on small scales (the effective sound speed) and the parameters describing its equation of state.
Non-Covalent Complexes between DNA-Binding Drugs and Double-Stranded Oligodeoxynucleotides: A Study by ESI Ion-Trap Mass Spectrometry

We developed an assay that utilizes electrospray ionization mass spectrometry (ESI-MS) to determine rapidly the noncovalent binding of drugs with oligodeoxynucleotides and to assess their relative affinities and stoichiometries. The method uses a set of self-complementary oligodeoxynucleotides that differ in length (6-mer to 12-mer), motif (GC-rich or AT-rich), and sequence, and these were annealed to form duplexes. To the oligodeoxynucleotides are bound a group of drugs (distamycin, Hoechst 33258, Hoechst 33342, berenil and actinomycin D abbreviated as D1, D2, D3, D4, and D5, respectively) that are classic minor-groove binders and intercalators. A second group (porphyrin H2TMpyP-4, metalloporphyrin CuTMpyP-4, FeTMpyP-4 and MnTMpyP-4 and [Ru(II)12S4dppz]Cl2 abbreviated as D6, D7, D8, D9, and D10) binds via mixed modes (i.e., groove binders and intercalators). The results confirm the binding stoichiometry and show preferred binding of minor-groove binders (distamycin, Hoechst 33258, Hoechst 33342, and bere.
Melilite-type borates Bi2ZnB2O7 and CaBiGaB2O7

The bismuth borates Bi2ZnB2O7 and CaBiGaB2O7 have been synthesized by solid-state reactions at temperatures in the 650−825 °C range at 1 atm pressure. These compounds are the only synthetic diborate members of the melilite family, A2XZ2O7, in which layers of A cations alternate with XZ2O7 tetrahedral layers. Except for CdBiGaB2O7, the synthesis of other substituted bismuth borate melilites has been unsuccessful. The crystal structures of Bi2ZnB2O7 and CaBiGaB2O7 have been determined by powder X-ray diffraction and refined by the Rietveld method using powder neutron diffraction data. CaBiGaB2O7 adopts the regular tetragonal melilite structure (P421m space group, Z = 2) containing B2O7 tetrahedral dimers. The refinement of split eight-coordinated sites for the Ca2+ and Bi3+ interlayer cations suggests the presence of additional disorder. Bi2ZnB2O7 adopts a unique orthorhombic melilite superstructure (Pba2 space group, Z = 4) containing both tetrahedral B2O7 and triangular B2O5 dimers. The Bi3+ cations occu.
L2 Learners’ Enhanced Pragmatic Comprehension of Implicatures via Computer-Mediated Communication and Social Media Networks

Second or foreign language (L2) learners‘ development of interlanguage pragmatic (ILP) competence to understand and properly interpret utterances under certain social and cultural circumstances plays a pivotal role in the achievement of communicative competence. The current study was designed to explore the effects of synchronous computer-mediated communication (SCMC) and asynchronous computer-mediated communication (ACMC) course modules delivered through social media networks (SMN) on the development of the Iranian L2 learners‘ comprehension of implicatures. The participants of the study were 90 English-as-a-foreign-language (EFL) undergraduate students attending three intact classes. The classes were randomly assigned to one control and two experimental (SCMC and ACMC) groups. An open-ended implicature comprehension test was used to assess students‘ ILP development in this pretest-posttest comparison-group study. The control group received the traditional teacher-fronted instruction, and the S/ACMC groups received instruction via synchronous and asynchronous modules of SMNs for 4 months, respectively. Students‘ attitudes towards the CMC-based courses were also sought. Split-plot ANOVA results indicated that both experimental groups developed significant ILP ability to comprehend and interpret L2 implicatures after the instruction; however, by comparison, the ACMC group improved more considerably. It is concluded that, first, comprehending L2 implicatures is not impervious to computer-mediated instruction and, second, different CMC affordances may result in differential ILP developmental effects in teaching L2 pragmatics. The findings can help L2 teachers decide how to use CMC affordances and SMN modules to raise L2 learners‘ pragmatic awareness.
Traffic conditions detection based on digital image and support vector machine

To avoid the drawbacks of the physical detection which damaged to the road seriously,affected by weather conditions and has complexity of the algorithm,a traffic conditions detection method using support vector machine to classify the different degrees of traffic conditions image is studied,using pyramid histogram of edge orientation gradients as the descriptive characteristics of the image.The experiments show that the studied methods could improve the average classification accuracy of the adverse weather conditions,and in all kinds of weather conditions,four categories of traffic conditions image's average classification accuracy is more than 92%,able to detect different degrees of traffic conditions.
Measurement of Process Conditions Present in Pilot Scale Iron Ore Sintering

An improved experimental technique has been developed to measure, concurrently, the oxygen partial pressures and temperatures within a pilot scale iron ore sinter pot as a function of time. The measurements and thermodynamic calculations have demonstrated that the oxygen partial pressure at peak bed temperature and during cooling can be oxidising or reducing relative to hematite. Examples of typical microstructures and phase assemblages observed in product sinters are presented. Potential mechanisms of hematite and magnetite formation at sub-liquidus and sub-solidus conditions are demonstrated. The relative impacts of changes to coke rate and draft pressure drop on the process conditions and proportions of the phases formed in the sinter have been measured. Increasing coke rate was shown to result in a faster sinter heating rates, higher peak bed temperatures and times at peak temperature. Higher draft pressures across the sinter bed resulted in faster sinter heating rates and shorter times at peak temperature.
25th Anniversary Article: Understanding the Lithiation of Silicon and Other Alloying Anodes for Lithium‐Ion Batteries

Alloying anodes such as silicon are promising electrode materials for next‐generation high energy density lithium‐ion batteries because of their ability to reversibly incorporate a high concentration of Li atoms. However, alloying anodes usually exhibit a short cycle life due to the extreme volumetric and structural changes that occur during lithium insertion/extraction; these transformations cause mechanical fracture and exacerbate side reactions. To solve these problems, there has recently been significant attention devoted to creating silicon nanostructures that can accommodate the lithiation‐induced strain and thus exhibit high Coulombic efficiency and long cycle life. In parallel, many experiments and simulations have been conducted in an effort to understand the details of volumetric expansion, fracture, mechanical stress evolution, and structural changes in silicon nanostructures. The fundamental materials knowledge gained from these studies has provided guidance for designing optimized Si electrode structures and has also shed light on the factors that control large‐volume change solid‐state reactions. In this paper, we review various fundamental studies that have been conducted to understand structural and volumetric changes, stress evolution, mechanical properties, and fracture behavior of nanostructured Si anodes for lithium‐ion batteries and compare the reaction process of Si to other novel anode materials.
Integrating QCA and HLM for Multilevel Research on Organizational Configurations

Mixed methods systematically combine multiple research approaches—either in basic parallel, sequential, or conversion designs or in more complex multilevel or integrated designs. Multilevel mixed designs are among the most valuable and dynamic. Yet current multilevel designs, which are rare in the mixed methods literature, do not strongly integrate qualitative and quantitative approaches for use in one study. This lack of integration is particularly problematic for research in the organization sciences because of the variety of multilevel concepts that researchers study. In this article, we develop a multilevel mixed methods technique that integrates qualitative comparative analysis (QCA) with hierarchical linear modeling (HLM). This technique is among the first of the multilevel ones to integrate qualitative and quantitative methods in a single research design. Using Miles and Snow’s typology of generic strategies as an example of organizational configurations, we both illustrate how researchers may apply this technique and provide recommendations for its application and potential extensions. Our technique offers new opportunities for bridging macro and micro inquiries by developing strong inferences for testing, refining, and extending multilevel theories of organizational configurations.
GAS OUTFLOWS IN SEYFERT GALAXIES: EFFECTS OF STAR FORMATION VERSUS AGN FEEDBACK

Large-scale, weakly collimated outflows are very common in galaxies with large infrared luminosities. In complex systems in particular, where intense star formation (SF) coexists with an active galactic nucleus (AGN), it is not clear yet from observations whether the SF, the AGN, or both are driving these outflows. Accreting supermassive black holes are expected to influence their host galaxies through kinetic and radiative feedback processes, but in a Seyfert galaxy, where the energy emitted in the nuclear region is comparable to that of the body of the galaxy, it is possible that stellar activity is also playing a key role in these processes. In order to achieve a better understanding of the mechanisms driving the gas evolution especially at the nuclear regions of these galaxies, we have performed high-resolution three-dimensional hydrodynamical simulations with radiative cooling considering the feedback from both SF regions, including supernova (Type I and II) explosions and an AGN jet emerging from the central region of the active spiral galaxy. We computed the gas mass lost by the system, separating the role of each of these injection energy sources on the galaxy evolution, and found that at scales within 1 kpc an outflow can be generally established considering intense nuclear SF only. The jet alone is unable to drive a massive gas outflow, although it can sporadically drag and accelerate clumps of the underlying outflow to very high velocities.
QUENCHING OF CARBON MONOXIDE AND METHANE IN THE ATMOSPHERES OF COOL BROWN DWARFS AND HOT JUPITERS

We explore quench kinetics in the atmospheres of substellar objects using updated timescale arguments, as suggested by a thermochemical kinetics and diffusion model that transitions from the thermochemical-equilibrium regime in the deep atmosphere to a quench-chemical regime at higher altitudes. More specifically, we examine CO quench chemistry on the T dwarf Gliese 229B and CH4 quench chemistry on the hot-Jupiter HD 189733b. We describe a method for correctly calculating reverse rate coefficients for chemical reactions, discuss the predominant pathways for interconversion as indicated by the model, and demonstrate that a simple timescale approach can be used to accurately describe the behavior of quenched species when updated reaction kinetics and mixing-length-scale assumptions are used. Proper treatment of quench kinetics has important implications for estimates of molecular abundances and/or vertical mixing rates in the atmospheres of substellar objects. Our model results indicate significantly higher Kzz values than previously estimated near the CO quench level on Gliese 229B, whereas current-model–data comparisons using CH4 permit a wide range of Kzz values on HD 189733b. We also use updated reaction kinetics to revise previous estimates of the Jovian water abundance, based upon the observed abundance and chemical behavior of carbon monoxide. The CO chemical/observational constraint, along with Galileo entry probe data, suggests a water abundance of approximately 0.51–2.6 × solar (for a solar value of H2O/H2 = 9.61 × 10−4) in Jupiter's troposphere, assuming vertical mixing from the deep atmosphere is the only source of tropospheric CO.
Multi-wavelength observations of the young binary system Haro 6-10: The case of misaligned discs

Context. We present a multi-wavelength, high-resolution observational survey of the young binary system Haro 6-10 (GV Tau, IRAS 04263+2426), which harbours one of the few known infrared companions. Aims. The primary goal of this project is to determine the physical and geometrical properties of the circumstellar and circumbinary material in the Haro 6-10 system. Methods. High-resolution optical (HST/WFPC2) and near-infrared (VLT/NACO) images in different bands were analysed to investigate the large-scale structures of the material around the binary. Mid-infrared interferometry (VLTI/MIDI) and spectroscopy (TIMMI2 at the 3.6 m ESO telescope) were carried out to determine the structure and optical depth of the circumstellar material around the individual components. Results. The multi-wavelength observations suggest that both components of the binary system Haro 6-10 are embedded in a common envelope. The measured extinction indicates a dust composition of the envelope similar to that of the interstellar medium. Each component of the system has a circumstellar disc-like structure typical of young stars. The discs are highly misaligned: the northern component is seen almost edge-on and the southern component is an almost face-on disc. Conclusions. The two main formation scenarios of binary systems with misaligned discs are the gravitational capture of a passing object in a dense environment and the fragmentation of the collapsing molecular cloud. Given the low-density environment of the Taurus-Aurigae star-forming region, the first scenario is unlikely for Haro 6-10. The binary system most probably formed via fragmentation of two different parts of the collapsing molecular cloud combined with other dynamical processes related to the cloud and/or the protostars. This can also be the explanation for other binary systems with an infrared companion.
Eclipse timing variation analysis of OGLE-IV eclipsing binaries towards the Galactic Bulge – I. Hierarchical triple system candidates

We report a study of the eclipse timing variation (ETV) of short period ($P_1\le 6^d$) eclipsing binaries (EB) monitored during the photometric survey OGLE-IV. From the 425\,193 EBs we selected approximately 80\,000 binaries that we found suitable for further examination. Among them we identified 992 potential hierarchical triple (or multiple ) system candidates exhibiting light-travel-time effect (LTTE). Besides, we obtained the orbital parameters of these systems and carried out statistical analyses on the properties of these candidates. We found that (i) there is a significant lack of triple systems where the outer period is less than 500 days; (ii) the distribution of the outer eccentricities has a maximum around $e_2\approx0.3$; (iii) the outer mass ratio calculated from an estimated minimum mass of the third component is lower than $q_2\sim 0.5$ for the majority of the sample. We also present some systems that deserve special attention. (i) There are four candidates that show double periodic ETV, which we explain by the presence of a fourth companion. (ii) For two systems the perturbations of the third component are also found to be significant therefore we give a combined dynamical and LTTE ETV solution. (iii) For one system the third component is found to be probably in the substellar mass domain.
Herschel-PACS measurements of nitrogen enrichment in nebulae around Wolf-Rayet stars

For three nebulae that have early-WN Wolf-Rayet exciting stars, NGC 6888, WR 8 and Abell 48, we have obtained Herschel-PACS line scans of the [N III] 57 um and [O III] 88 micron lines, along with the 122 and 205 micron lines of [N II]. From the former two lines we have derived N$^{2+}$/O$^{2+}$ abundance ratios, equal to the overall N/O ratio under a wide range of nebular conditions. We find that all of the nebulae observed possess significant nitrogen enrichment, with derived N/O ratios greater than solar. The two nebulae with massive Wolf-Rayet exciting stars, NGC 6888 and WR8 are found to have N/O ratios that are enhanced by factors of 7 - 10 relative to the solar N/O ratio, consistent with an origin as material ejected just before the onset of the Wolf-Rayet phase. The other nebula, Abell 48, has recently been reclassified as a member of the rare class of three planetary nebulae that have early-WN central stars and are not of Peimbert Type I. We derive a nebular N/O ratio for it that is a factor of 4 enhanced relative to solar and slightly above the range of N/O values that have been measured for the other three members of its [WN] planetary nebula class.
OFFSETS BETWEEN THE X-RAY AND THE SUNYAEV–ZEL'DOVICH-EFFECT PEAKS IN MERGING GALAXY CLUSTERS AND THEIR COSMOLOGICAL IMPLICATIONS

Observations reveal that the peaks of the X-ray map and the Sunyaev–Zel'dovich (SZ) effect map of some galaxy clusters are offset from each other. In this paper, we perform a set of hydrodynamical simulations of mergers of two galaxy clusters to investigate the spatial offset between the maxima of the X-ray and the SZ surface brightness of the merging clusters. We find that significantly large SZ–X-ray offsets (>100 kpc) can be produced during the major mergers of galaxy clusters (with mass > 1 × 1014 M☉). The significantly large offsets are mainly caused by a “jump effect” that occurrs between the primary and secondary pericentric passages of the two merging clusters, during which the X-ray peak may jump to the densest gas region located near the center of the small cluster, but the SZ peak remains near the center of the large one. Our simulations show that merging systems with higher masses and larger initial relative velocities may result in larger offset sizes and longer offset time durations; and only nearly head-on mergers are likely to produce significantly large offsets. We further investigate the statistical distribution of the SZ–X-ray offset sizes and find that (1) the number distribution of the offset sizes is bimodal with one peak located at low offsets ∼0 and the other at large offsets ∼350–450 h−1 kpc, but the objects with intermediate offsets are scarce; and (2) the probabilities of the clusters in the mass range higher than 2 × 1014 h−1 M☉ that have offsets larger than 20, 50, 200, 300, and 500 h−1 kpc are 34.0%, 11.1%, 8.0%, 6.5%, and 2.0%, respectively, at z = 0.7. The probability is sensitive to the underlying pairwise velocity distribution and the merger rate of clusters. We suggest that the SZ–X-ray offsets provide a probe to the cosmic velocity fields on the cluster scale and the cluster merger rate, and future observations on the SZ–X-ray offsets for a large number of clusters may put strong constraints on them. Our simulation results suggest that the SZ–X-ray offset in the Bullet Cluster, together with the mass ratio of the two merging clusters, requires a relative velocity larger than 3000 km s−1 at an initial separation 5 Mpc. The cosmic velocity distribution at the high-velocity end is expected to be crucial in determining whether there exists an incompatibility between the existence of the Bullet Cluster and the prediction of a ΛCDM model.