Miracle-dz/UniFAR-FTUs huggingface dataset:
Re‐evaluation of neohesperidine dihydrochalcone (E 959) as a food additive

Abstract The present opinion deals with the re‐evaluation of neohesperidine dihydrochalcone (E 959) when used as a food additive. It is obtained by catalytic hydrogenation of a flavanone – neohesperidine – which is naturally occurring and thus isolated by alcohol extraction in bitter oranges (Citrus aurantium). Based on in vivo data in rat, neohesperidine dihydrochalcone is likely to be absorbed, also in humans, and to become systemically available. It does not raise a concern regarding genotoxicity. The toxicity data set consisted of studies on subchronic and prenatal developmental toxicity. No human studies were available. The data set was considered sufficient to derive a new acceptable daily intake (ADI). Based on the weight of evidence (WoE) analysis, the Panel considered unlikely that neohesperidine dihydrochalcone would lead to adverse effects on health in animals in the dose ranges tested. The Panel also considered that a carcinogenicity study was not warranted and that the lack of human data did not affect the overall confidence in the body of evidence. The Panel derived an ADI of 20 mg/kg bodyweight (bw) per day based on a no observed adverse effect level (NOAEL) of 4,000 mg/kg bw per day from a 13‐week study in rat, applying the standard default factors of 100 for inter‐ and intraspecies differences and of 2 for extrapolation from subchronic to chronic exposure. For the refined brand‐loyal exposure assessment scenario, considered to be the most appropriate for the risk assessment, the exposure estimates at the mean ranged from < 0.01 to 0.09 mg/kg bw per day and at the 95th percentile (P95) from 0.01 to 0.24 mg/kg bw per day. Considering the derived ADI of 20 mg/kg bw per day, the exposure estimates were below the reference value in all age groups. Therefore, the Panel concluded that dietary exposure to the food additive neohesperidine dihydrochalcone (E 959) at the reported uses and use levels would not raise a safety concern.
The Rest-Frame Extreme-Ultraviolet Spectral Properties of Quasi-stellar Objects

We use a sample of 332 Hubble Space Telescope spectra of 184 quasi-stellar objects (QSOs) with z > 0.33 to study the typical ultraviolet spectral properties of QSOs, with emphasis on the ionizing continuum. Our sample is nearly twice as large as that from previous work by W. Zheng and colleagues and provides much better spectral coverage in the extreme-ultraviolet (EUV). The overall composite continuum can be described by a power law with index αEUV = -1.76 ± 0.12 (fν ∝ να) between 500 and 1200 Å. The corresponding results for subsamples of radio-quiet and radio-loud QSOs are αEUV = -1.57 ± 0.17 and αEUV = -1.96 ± 0.12, respectively. We also derive αEUV for as many individual objects in our sample as possible, totaling 39 radio-quiet and 40 radio-loud QSOs. The typical individually measured values of αEUV are in good agreement with the composites. We find no evidence for evolution of αEUV with redshift for either radio-loud or radio-quiet QSOs. However, we do find marginal evidence for a trend toward harder EUV spectra with increasing luminosity for radio-loud objects. An extrapolation of our radio-quiet QSO spectrum is consistent with existing X-ray data, suggesting that the ionizing continuum may be represented by a single power law. The resulting spectrum is roughly in agreement with models of the intergalactic medium photoionized by the integrated radiation from QSOs.
Supervised Contrastive Learning For Musical Onset Detection

This paper applies supervised contrastive learning to musical onset detection to alleviate the issue of noisy annotated data for onset datasets. The results are compared against a state-of-the-art, convolutional, cross-entropy model. Both models were trained on two datasets. The first dataset comprised of a manually annotated selection of music. This data was then augmented with inaccurate labelling to produce the second data set. When trained on the original data the supervised contrastive model produced an F1 score of 0.878. This was close to the cross-entropy model score of 0.888. This showed that supervised contrastive loss is applicable to onset detection but does not outperform cross-entropy models in an ideal training case. When trained on the augmented set the contrastive model consistently outperformed the cross-entropy model across increasing percentage inaccuracies, with a difference in F1 score of 0.1 for the most inaccurate data. This demonstrates the robustness of supervised contrastive learning with inaccurate data for onset detection, suggesting that supervised contrastive loss could provide a new onset detection architecture which is invariant to noise in the data or inaccuracies in labelling.
Improvement of Rice Agronomic Traits by Editing Type-B Response Regulators

Type-B response regulator proteins in rice contain a conserved receiver domain, followed by a GARP DNA binding domain and a longer C-terminus. Some type-B response regulators such as RR21, RR22 and RR23 are involved in the development of rice leaf, root, flower and trichome. In this study, to evaluate the application potential of type-B response regulators in rice genetic improvement, thirteen type-B response regulator genes in rice were respectively knocked out by using CRISPR/Cas9 genome editing technology. Two guide RNAs (gRNAs) were simultaneously expressed on a knockout vector to mutate one gene. T0 transformed plants were used to screen the plants with deletion of large DNA fragments through PCR with specific primers. The mutants of CRISPR/Cas9 gene editing were detected by Cas9 specific primer in the T1 generation, and homozygous mutants without Cas9 were screened, whose target regions were confirmed by sequencing. Mutant materials of 12 OsRRs were obtained, except for RR24. Preliminary phenotypic observation revealed variations of various important traits in different mutant materials, including plant height, tiller number, tillering angle, heading date, panicle length and yield. The osrr30 mutant in the T2 generation was then further examined. As a result, the heading date of the osrr30 mutant was delayed by about 18 d, while the yield was increased by about 30%, and the chalkiness was significantly reduced compared with those of the wild-type under field high temperature stress. These results indicated that osrr30 has great application value in rice breeding. Our findings suggest that it is feasible to perform genetic improvement of rice by editing the type-B response regulators.
Kinetics and Mechanism of Metal Nanoparticle Growth via Optical Extinction Spectroscopy and Computational Modeling: The Curious Case of Colloidal Gold.

An overarching computational framework unifying several optical theories to describe the temporal evolution of gold nanoparticles (GNPs) during a seeded growth process is presented. To achieve this, we used the inexpensive and widely available optical extinction spectroscopy, to obtain quantitative kinetic data. In situ spectra collected over a wide set of experimental conditions were regressed using the physical model, calculating light extinction by ensembles of GNPs during the growth process. This model provides temporal information on the size, shape, and concentration of the particles, and any electromagnetic interactions between them. Consequently, we were able to describe the mechanism of GNP growth and divide the process into distinct genesis periods. We provide explanations for several longstanding mysteries, e.g., the phenomena responsible for the purple-greyish hue during the early stages of GNP growth, the complex interactions between nucleation, growth and aggregation events, and a clear distinction between agglomeration and electromagnetic interactions. The presented theoretical formalism has been developed in a generic fashion so that it can readily be adapted to other nanoparticulate formation scenarios such as the genesis of various metal nanoparticles.
Imaging of Dissipative Structures in the Near Field of a Turbulent Non-premixed Jet Flame

Abstract Two-dimensional laser Rayleigh measurements of thermal gradient structures are performed in a turbulent non-premixed jet flame. The measurements focus on the near field (10 nozzle diameters downstream of the jet exit) where traditional scaling laws from the self-similar far field of non-reacting jets are not necessarily applicable. The optical performance of the high-resolution imaging system is characterized. The square of the temperature gradient field is analyzed by calculating the power spectral density (PSD) and by directly measuring the thicknesses of the layer-like structures. Fully resolved spectra extending over three orders of magnitude in PSD are obtained using a new noise cancellation technique. Some spatial filtering (smoothing) is necessary to reliably measure the layer-normal structure widths in the images. The probability density function (PDF) of the layer widths is found to be approximately log-normal. The PDFs of the 20-percent-full-width layer thicknesses have peak values at 216 and 368 μm for r/d = 0 and r/d = 1, respectively. The peak of the layer-thickness probability density function (PDF) occurs at a length scale where the PSD is at approximately 0.5 percent of its maximum in both the low-temperature centerline region and the region near the maximum mean temperature.
Modal Tracking Based on Group Theory

Issues in modal tracking in the presence of crossings and crossing avoidances between eigenvalue traces are solved via the theory of point groups. The von Neumann–Wigner theorem is used as a key factor in predictively determining mode behavior over arbitrary frequency ranges. The implementation and capabilities of the proposed procedure are demonstrated using characteristic mode decomposition as a motivating example. The procedure is, nevertheless, general and can be applied to an arbitrarily parametrized eigenvalue problem. A treatment of modal degeneracies is included and several examples are presented to illustrate modal tracking improvements and the immediate consequences of improper modal tracking. An approach leveraging a symmetry-adapted basis to accelerate computation is also discussed. A relationship between geometrical and physical symmetries is demonstrated on a practical example.
Laboratory Evaluation and Field Feasibility of Micro-Encapsulated Insecticide Effect on Rhodnius prolixus and Triatoma dimidiata Mortality in Rural Households in Boyacá, Colombia

Simple Summary Vector control strategies need to adapt due to the increase in insecticide resistance among several vector species. Insecticide spraying requires great economic and logistical efforts due to repeated application every six months. This study evaluated the feasibility of micro-encapsulated insecticide on mortality on Rhodnius prolixus and Triatoma dimidiata and its effect on household colonization after one year application in a rural community in Colombia. Findings suggest the ability of this paint to prevent colonization and demonstrated positive population perception. Complementary use of insecticide spraying and micro-encapsulated paints suggest this could be a more efficient public health approach that could reduce costs and logistical efforts. Abstract Chagas disease is a neglected vector-borne zoonosis caused by the parasite Trypanosoma cruzi that is primarily transmitted by insects of the subfamily Triatominae. Although control efforts targeting domestic infestations of Rhodnius prolixus have been largely successful, with several regions in Boyacá department certified free of T. cruzi transmission by intradomicile R. prolixus, novel native species are emerging, increasing the risk of disease. Triatoma dimidiata is the second most important species in Colombia, and conventional control methods seem to be less effective. In this study we evaluated the efficacy and usefulness of micro-encapsulated insecticide paints in laboratory conditions and its applicability in rural communities to avoid triatomine domiciliation. Laboratory conditions measured mortality at 6 months and 12 months, with an average mortality between 93–100% for T. dimidiata and 100% for R. prolixus. Evaluation of triatomine infestation in rural households was measured after one year, with an overall perception of effectiveness in reducing household domiciliation. Although triatomines were still spotted inside and around the homes, our findings demonstrate the ability of micro-encapsulated insecticide to prevent colonization inside the households when comparing infestation rates from previous years. Current control measures suggest insecticide spraying every six months, which implies great economic cost and logistical effort. Complementary triatomine control measures with insecticide spraying and micro-encapsulated insecticide paint would make public health efforts more efficient and reduce the frequency of treatment.
Adsroption of Bismarck Brown R Dyes Using Mesoporous Silica MCM-48

Bismarck Brown R (BBR) dye has been adsorption using mesoporous silica (MCM-48). We synthesized the adsorbent using Ludox HS-40 as a silica source and surfactants of Cetyl Trimethylammonium Bromide (CTAB) and Triton X-100. The characterization of MCM-48 was performed using Fourier transform infrared (FTIR), X-ray diffraction (XRD), and scanning electron microscopy (SEM). Various contact times were used to study the adsorption kinetics, and concentrations were used to study the adsorption isotherm. The optimum contact time of Bismarck Brown R dye was one hundred twenty minutes, and the adsorption followed a pseudo-second-order model. Based on the equation Langmuir and Freundlich adsorption isotherms, the adsorption capacity values of each are 158.7301 mg g -1 and 4.3601 mg g -1 . Our results showed that the material can be used as a new dye adsorbent.
Algebraic approach to solve tt dilepton equations

The set of nonlinear equations describing the standard model kinematics of the top quark antiquark production system in the dilepton decay channel has at most a fourfold ambiguity due to two not fully reconstructed neutrinos. Its most precise solution is of major importance for measurements of top quark properties like the top quark mass and $t\overline{t}$ spin correlations. Simple algebraic operations allow one to transform the nonlinear equations into a system of two polynomial equations with two unknowns. These two polynomials of multidegree eight can in turn be analytically reduced to one polynomial with one unknown by means of resultants. The obtained univariate polynomial is of degree 16. The number of its real solutions is determined analytically by means of Sturm's theorem, which is as well used to isolate each real solution into a unique pairwise disjoint interval. The solutions are polished by seeking the sign change of the polynomial in a given interval through binary bracketing.
AGN feedback in galaxy group 3C 88: cavities, shock, and jet reorientation

We present results from the deep Chandra observation (105 ksec), together with new Giant Metrewave Radio Telescope and Very Large Array data of the AGN outburst in the radio-loud galaxy group 3C 88. The system shows a prominent X-ray cavity on the eastern side with a diameter of $\sim$50 kpc at $\sim28$ kpc from the nucleus. The total enthalpy of the cavity is $3.8\times10^{58}$ erg and the average power required to inflate the X-ray bubble is $\sim2.0\times10^{43}$ erg s^-1. From surface brightness profiles we detect a shock with a Mach number of $M=1.4\pm0.2$, consistent with the value obtained from temperature jump. The shock energy is estimated to be $1.9\times10^{59}$ erg. The size and total enthalpy of the cavity in 3C 88 are the largest known in galaxy groups, as well as the shock energy. The eastern X-ray cavity is not aligned with the radio jet axis. This factor, combined with the radio morphology, strongly suggests jet reorientation in the last tens of million years. The bright rim and arm features surrounding the cavity show metallicity enhancement, suggesting they originated as high metallicity gas from the group center, lifted by the rising X-ray bubbles. Our Chandra study of 3C 88 also reveals that galaxy groups with powerful radio AGN can have high cavity power, although deep X-ray observations are typically required to confirm the cavities in galaxy groups.
The structure and spectrum of the accretion shock in the atmospheres of young stars

The structure and spectrum of the accretion shock have been self-consistently simulated for a wide range of parameters typical for Classical T Tauri Stars (CTTS). Radiative cooling of the shocked gas was calculated, taking into account the self-absorption and non-equilibrium (time-dependent) effects in the level populations. These effects modify the standard cooling curve for an optically thin plasma in coronal equilibrium, however the shape of high-temperature ($T>3\times10^5$ K) part of the curve remains unchanged. The applied methods allow us to smoothly describe the transition from the cooling flow to the hydrostatic stellar atmosphere. Thanks to this approach, it has been found that the narrow component of HeII lines is formed predominantly in the irradiated stationary atmosphere (hotspot), i.e. at velocities of the settling gas $<2$ km s$^{-1}$. The structure of the pre-shock region is calculated simultaneously with the heated atmosphere. The simulation shows that the pre-shock gas produces a noticeable emission component in HeII lines and practically does not manifest itself in HeI lines ($\lambda\lambda$ 5876, 10830 {\AA}). The UV spectrum of the hotspot is distorted by the pre-shock gas, namely numerous red-shifted emission and absorption lines overlap each other forming a pseudo-continuum. The spectrum of the accretion region at high pre-shock densities $\sim10^{14}$ cm$^{-3}$ is fully formed in the in-falling gas and can be qualitatively described as a spectrum of a star with an effective temperature derived from the Stefan-Boltzmann law via the full energy flux.
A distant OB association around RAFGL 5475

Context. Observations of the galactic disk at mid-infrared and longer wavelengths reveal a wealth of structures indicating the existence of complexes of recent massive star formation. However, little or nothing is known about the stellar component of those complexes. Aims. We have carried out observations aiming at the identification of early-type stars in the direction of the bright infrared source RAFGL 5475, around which several interstellar medium structures usually associated with the presence of massive stars have been identified. Our observations have the potential of revealing the suspected but thus far unknown stellar component of the region around RAFGL 5475. Methods. We have carried out near-infrared imaging observations (JHKs bands) designed to reveal the presence of early-type stars based on their positions in color–color and color–magnitude diagrams centered on the location of RAFGL 5475. We took into account the possibility that candidates found might belong to a foreground population physically related either to M 16 or M 17, two giant HII regions lying midway between the Sun and RAFGL 5475. Results. The near-infrared color–color diagram shows clear evidence for the presence of a moderately obscured population of early-type stars in the region imaged. By studying the distribution of extinction in their direction and basic characteristics of the interstellar medium we show that these new early-type stars are most likely associated with RAFGL 5475. Conclusions. By investigating the possible existence of massive early-type stars in the direction of RAFGL 5475 we have discovered the existence of a new OB association. A very preliminary assessment of its contents suggests the presence of several O-type stars, some of them likely to be associated with structures in the interstellar medium. The new association is located at 4 kpc from the Sun in the Scutum-Centaurus arm.
Broadband High-Energy Observations of the Superluminal Jet Source GRO J1655–40 during an Outburst

The X-ray/radio transient superluminal jet source GRO J1655-40 was recently suggested to contain a black hole from optical observations. Because it is a relatively close-by system (d ~ 3.2 kpc), it can likely provide us with rich information about the physics operating in both Galactic and extragalactic jet sources. We present the first simultaneous broadband high-energy observations of GRO J1655-40 during the 1995 July-August outburst by three instruments: ASCA, WATCH/Granat, and BATSE/CGRO, in the energy band from 1 keV to 2 MeV. Our observations strengthen the interpretation that GRO J1655-40 contains a black hole. We detected a two-component energy spectrum, commonly seen from other Galactic black hole binaries, but never detected from a neutron star system. Combining our results with the mass limits derived from optical radial velocity and orbital period measurements, we further constrain the mass of the central object to be between 3.3 and 5.8 M☉, above the well-established mass upper limit of 3.2 M☉ for a neutron star (the optical mass function for GRO J1655-40 is 3.16 ± 0.2 M☉). This system is therefore the first Galactic superluminal jet source for which there is strong evidence that the system contains a stellar mass black hole. The inclination angle of the binary system is constrained to be between 76° and 87°, consistent with estimates obtained from optical light curves and radio jet kinematics.
Dusty Superwind from a Galaxy with a Compact Obscured Nucleus: Optical Spectroscopic Study of NGC 4418

We report our optical spectroscopic study of the nucleus and its surrounding region of a nearby luminous infrared galaxy NGC 4418. This galaxy has been known to host a compact obscured nucleus, showing distinct characteristics such as a very compact (∼20 pc) submillimeter and mid-infrared core and dusty circumnuclear region with massive molecular gas concentration. We detected dusty superwind outflow at ≳1 kpc scale along the disk semiminor axis in both shock-heated emission lines and enhanced interstellar Na D absorption. This superwind shows basic characteristics similar to those of the prototypical superwind in the starburst galaxy M82, such as a kiloparsec-scale extended structure of gas and dust along the disk minor axis, outflowing components (multiphase gas and dust), physical conditions of the ionized gas, and monotonically blueshifting radial velocity field with increasing distance from the nucleus on the front side of the superwind. We also detected a moderately extinct starburst population in the Sloan Digital Sky Survey nuclear spectrum with a burst age of ≃10 Myr and stellar mass of ≃1 × 107 M☉. It is powerful enough to drive the superwind within the dynamical age of the superwind (≃10 Myr). On the basis of comparison between this starburst–superwind scenario and the observations in terms of the burst age, stellar mass, infrared luminosity, and obscuration in the optical bands, we argue that this superwind-driving starburst is separate from the submillimeter core even if the core is a very young star cluster. Therefore, this galaxy hosts both the enshrouded compact core and the superwind-driving circumnuclear starburst.
Corporate Innovation Programs: A Way to Organize Creative Time in Companies

It is widely regarded that employees are an important source of creativity. Hence, many companies offer specific programs to foster creative outputs. For this, employees are granted time to work on creative ideas, beyond Research and Development departments, called corporate innovation programs. How does one organize this time? Our research indicates that schedule autonomy is very important and that it has a high impact on creative results. Innovation programs can be implemented by a spontaneous time model with free time allocation, or by a predetermined version with fixed timeslots. We discuss the advantages of both models, as well as the implications of how to implement this in a company context.