Miracle-dz/UniFAR-FTUs huggingface dataset:
FFECT OF WEEDING REGIME ON THE PERFORMANCE OF DIRECT-SEEDED AUS RICE

A field experiment was conducted to find out the impact of weeding regime on the performance of three Aus rice. The experimental treatment consisted of three varieties of rice viz. BRRI dhan28, Bere Ratna and Kajol Lata, and four weeding regimes viz. no weeding, one hand weeding at 35 days after sowing (DAS), two hand weedings at 20 and 35 DAS and three hand weedings at 20, 35 and 50 DAS. The experiment was laid out in a factorial randomized complete block design with three replications. Eleven weed species belonging to five families infested the experimental plots; Cyperus rotundus L. and Imperata cylindrica (L.) Baeuv. were the dominant. The effect of weeding regime on weed density (except at 20 DAS) and weed dry weight was statistically significant. The results indicated that three hand weedings at 20, 35 and 50 DAS produced the highest number of effective tillers hill-1, number of filled grains panicle-1, 1000-grain weight and grain yield. Among the varieties Bere Ratna gave the highest grain yield.
A SPECTROSCOPIC AND PHOTOMETRIC STUDY OF THE PLANETARY NEBULAE Kn 61 AND Pa 5

We present the first morpho-kinematical analysis of the planetary nebulae Kn 61 and Pa 5 and explore the nature of their central stars. Our analysis is based on high-resolution and medium-resolution spectroscopic observations, deep narrow-band imaging, and integral photometry. This material allows us to identify the morphological components and study their kinematics. The direct images and spectra indicate an absence of the characteristic [N ii] and [S ii] emission lines in both nebulae. The nebular spectrum of Kn 61 suggests a hydrogen deficient planetary nebula and the stellar spectrum of the central star reveals a hydrogen-deficient PG 1159-type star. The [O iii] position velocity diagram reveals that Kn 61 is a closed, empty, spherical shell with a thin border and a filamentary surface expanding at 67.6 km s−1 and the shell is currently not expanding isotropically. We derived a kinematic age of ∼1.6 × 104 yr for an assumed distance of 4 kpc. A photometric period of ∼5.7(±0.4) days has been detected for Kn 61, indicating the presence of a possible binary system at its core. A possible link between filamentary spherical shells and PG 1159-type stars is noted. The morphology of Pa 5 is dominated by an equatorial toroid and faint polar extensions. The equatorial region of this planetary nebula is expanding at 45.2 km s−1. The stellar spectrum corresponds to a very hot star and is dominated by a steep blue rising continuum and He ii, Balmer, and Ca ii photospheric lines.
The properties of Brightest Cluster Galaxies in the SDSS DR6 adaptive matched filter cluster catalogue

We study the properties of Brightest Cluster Galaxies (BCGs) drawn from a catalogue of more than 69000 clusters in the SDSS DR6 based on the adaptive matched filter technique (AMF, Szabo et al., 2010). Our sample consists of more than 14300 galaxies in the redshift range 0.1-0.3. We test the catalog by showing that it includes well-known BCGs which lie in the SDSS footprint. We characterize the BCGs in terms of r-band luminosities and optical colours as well as their trends with redshift. In particular, we define and study the fraction of blue BCGs, namely those that are likely to be missed by either colour-based cluster surveys and catalogues. Richer clusters tend to have brighter BCGs, however less dominant than in poorer systems. 4-9% of our BCGs are at least 0.3 mag bluer in the g-r colour than the red-sequence at their given redshift. Such a fraction decreases to 1-6% for clusters above a richness of 50, where 3% of the BCGs are 0.5 mag below the red-sequence. A preliminary morphological study suggests that the increase in the blue fraction at lower richnesses may have a non-negligible contribution from spiral galaxies. We show that a colour selection based on the g-r red-sequence or on a cut at colour u-r >2.2 can lead to missing the majority of such blue BCGs. We also extend the colour analysis to the UV range by cross-matching our catalogue with publicly available data from Galex GR4 and GR5. We show a clear correlation between offset from the optical red-sequence and the amount of UV-excess. Finally, we cross-matched our catalogue with the ACCEPT cluster sample (Cavagnolo et al., 2009), and find that blue BCGs tend to be in clusters with low entropy and short cooling times. That is, the blue light is presumably due to recent star formation associated to gas feeding by cooling flows. (abridged)
Validation and Validity: Self-Efficacy, Metacognition, and Knowledge-and-Appraisal Personality Architecture (KAPA)

This research examines and reframes the long-standing pursuit of validation in personality research, in response to a shift in the field to focus on in-ter-individual idiographic contexts and constructs by focusing on Know-ledge-and-Appraisals Personality Architecture (KAPA) as a method for per-son-centred, non-trait-based personality research. Aspects of instrument validity and validation are addressed, exploring relationships of cognition with self-variables to support the unique and informative nature of KAPA model for measuring personality architecture. First the validity of two empirical questionnaires, Self-efficacy for Performing (SEP) and the Metacognitive Thinking Questionnaire (MTQ) are demonstrated through EFA and CFA. Then the KAPA model for personality architecture, a person-based method that sits outside the traditional questionnaire approach to measuring personality, is validated by using elements of traditional validation and through exploring theoretically expected ontological relationships.
PRIMORDIAL BLACK HOLES AS DARK MATTER: ALMOST ALL OR ALMOST NOTHING

Primordial black holes (PBHs) are expected to accrete particle dark matter around them to form ultracompact minihalos (UCMHs), if the PBHs themselves do not make up most of the dark matter. We show that if most dark matter is a thermal relic, then the inner regions of UCMHs around PBHs are highly luminous sources of annihilation products. Flux constraints on gamma rays and neutrinos set strong abundance limits, improving previous limits by orders of magnitude. Assuming enough particle dark matter exists to form UCMHs, we find that ΩPBH ≲ 10−4 (for mDMc2 ≈ 100 GeV) for a vast range in PBH mass. We briefly discuss the uncertainties on our limits, including those due to the evolution of the UCMH luminosity as it annihilates.
Product differentiation and the relative importance of wine attributes: U.S. retail prices

Abstract This paper investigates the relative importance of various attributes, including varietal, brands, and geographic origin, in explaining retail wine prices for the United States market. We use a metric based on the Shapely value, from cooperative game theory, in the context of an empirical hedonic price equation estimated using a large sample of retail wine sales for home consumption over the period 2007–2019. We find that brands alone explain more than 70% of the variation in wine prices, but geographic origin and varietals retain additional explanatory power. Furthermore, information about the geographic origin appears to be a considerably more important attribute than varietals.
ALMA IMAGING AND GRAVITATIONAL LENS MODELS OF SOUTH POLE TELESCOPE—SELECTED DUSTY, STAR-FORMING GALAXIES AT HIGH REDSHIFTS

The South Pole Telescope has discovered 100 gravitationally lensed, high-redshift, dusty, star-forming galaxies (DSFGs). We present 0. ″5 resolution 870 Atacama Large Millimeter/submillimeter Array imaging of a sample of 47 DSFGs spanning , and construct gravitational lens models of these sources. Our visibility-based lens modeling incorporates several sources of residual interferometric calibration uncertainty, allowing us to properly account for noise in the observations. At least 70% of the sources are strongly lensed by foreground galaxies ( ), with a median magnification of , extending to . We compare the intrinsic size distribution of the strongly lensed sources to a similar number of unlensed DSFGs and find no significant differences in spite of a bias between the magnification and intrinsic source size. This may indicate that the true size distribution of DSFGs is relatively narrow. We use the source sizes to constrain the wavelength at which the dust optical depth is unity and find this wavelength to be correlated with the dust temperature. This correlation leads to discrepancies in dust mass estimates of a factor of two compared to estimates using a single value for this wavelength. We investigate the relationship between the [C ii] line and the far-infrared luminosity and find that the same correlation between the [C ii]/ ratio and found for low-redshift star-forming galaxies applies to high-redshift galaxies and extends at least two orders of magnitude higher in . This lends further credence to the claim that the compactness of the IR-emitting region is the controlling parameter in establishing the “[C ii] deficit. ”
TRACING THE MASS GROWTH AND STAR FORMATION RATE EVOLUTION OF MASSIVE GALAXIES FROM Z ∼ 6 TO Z ∼ 1 IN THE HUBBLE ULTRA-DEEP FIELD

We present an analysis of an H160-selected photometric catalog of galaxies in the Hubble Ultra-Deep Field, using imaging from the WFC3/IR camera on the Hubble Space Telescope in combination with archival ultraviolet, optical, and near-infrared imaging. Using these data, we measure the spectral energy distributions of ∼1500 galaxies to a limiting H160 magnitude of 27.8, from which we fit photometric redshifts and stellar population estimates for all galaxies with well-determined Spitzer IRAC fluxes, allowing for the determination of the cumulative mass function within the range 1 < z < 6. By selecting samples of galaxies at a constant cumulative number density, we are able to explore the coevolution of stellar masses and star formation rates (SFRs) for progenitor galaxies and their descendants from z ∼ 6. We find a steady increase in the SFRs of galaxies at constant number density from z ∼ 6 to z ∼ 3, accompanied by gradually declining specific star formation rates (sSFRs) during this same period. The peak epoch of star formation is also found to shift to later times for galaxies with increasing number densities, in agreement with the expectations from cosmic downsizing. The observed SFRs can fully account for the mass growth to z ∼ 2 among galaxies with cumulative number densities greater than 10−3.5 Mpc−3. For galaxies with a lower constant number density (higher mean mass), we find the observed stellar masses are ∼three times greater than that which may be accounted for by the observed star formation alone at late times, implying that growth from mergers plays an important role at z < 2. We additionally observe a decreasing sSFR, equivalent to approximately one order of magnitude, from z ∼ 6 to z ∼ 2 among galaxies with number densities less than 10−3.5 Mpc−3, along with significant evidence that at any redshift the sSFR is higher for galaxies at higher number density. The combination of these findings can qualitatively explain the previous findings of a specific star formation rate plateau at high redshift. Tracing the evolution of the fraction of quiescent galaxies for samples matched in cumulative number density over this redshift range, we find no unambiguous examples of quiescent galaxies at z > 4.
Computed Tomographic Imaging Features of COVID-19 Pneumonia Caused by the Delta (B.1.617.2) and Omicron (B.1.1.529) Variant in a German Nested Cohort Pilot Study Group

Background: The aim of this study was to evaluate CT (computed tomography) imaging differences for the Delta and the Omicron variant in COVID-19 infection. Methods: The study population was derived from a retrospective study cohort investigating chest CT imaging patterns in vaccinated and nonvaccinated COVID-19 patients. CT imaging patterns of COVID-19 infection were evaluated by qualitative and semiquantitative scoring systems, as well as imaging pattern analysis. Results: A total of 60 patients (70.00% male, 62.53 ± 17.3 years, Delta: 43 patients, Omicron: 17 patients) were included. Qualitative scoring systems showed a significant correlation with virus variants; “typical appearance” and “very high” degrees of suspicion were detected more often in patients with Delta (RSNA: p = 0.003; CO-RADS: p = 0.002; COV-RADS: p = 0.001). Semiquantitative assessment of lung changes revealed a significant association with virus variants in univariate (Delta: 6.3 ± 3.5; Omicron: 3.12 ± 3.2; p = 0.002) and multivariate analysis. The vacuolar sign was significantly associated with the Delta variant (OR: 14.74, 95% CI: [2.32; 2094.7], p = 0.017). Conclusion: The Delta variant had significantly more extensive lung involvement and showed changes classified as “typical” more often than the Omicron variant, while the Omicron variant was more likely associated with CT findings such as “absence of pulmonary changes”. A significant correlation between the Delta variant and the vacuolar sign was observed.
The CoRoT star ID 100866999: a hybrid γ Doradus-δ Scuti star in an eclipsing binary system

The presence of g- and p-modes allows testing stellar models from the core to the envelope. Moreover, binarity in an eclipsing system constrains the physical parameters of the pulsating star. CoRot ID 100866999 is a relatively large-amplitude hybrid gDor - dSct star with two clearly distinct frequency domains. The large number of detected frequencies allows a detailed study of the interaction between them. In addition, we can derive the fundamental parameters of both components from the study of the eclipsing light curve. After removing the eclipsing phases, we analyzed the data with the Period04 package up to S/N=4. The light curve was then prewhitened with these oscillation frequencies to derive the fundamental parameters of the two components. The eclipsing light curve analysis results in a (1.8+1.1)\,Mo system, both components being main sequence stars. We detect 124 frequencies related to luminosity variations of the primary. They are present in two well-separated domains: 89 frequencies in the interval [0.30;3.64]/d and 35 in the interval [14.57; 33.96]/d. There are 22 gDor frequencies separated by a constant period interval Delta P = 0.03493 d. These frequencies correspond to a series of g-modes of degree ell=1 with successive radial orders k. We identify 21 linear combinations between the first nine gDor frequencies. The dSct domain is dominated by a large-amplitude frequency F=16.9803 /d. The eight first gDor frequencies f_i are present with much lower amplitude in the delta Scuti domain as F +/- f_i. These interactions between g- and p-modes confirm the phenomenon we detected in another CoRoT star. The amplitude and the phase of the main frequency F shows a double-wave modulation along the orbital phase, giving rise to series of combination frequencies. Such combination frequencies are also detected, with lower amplitude, for the first gDor modes.
A MASSIVE MOLECULAR GAS RESERVOIR IN THE z = 2.221 TYPE-2 QUASAR HOST GALAXY SMM J0939+8315 LENSED BY THE RADIO GALAXY 3C220.3

We report the detection of CO(J = 3 → ? > 2) line emission in the strongly lensed submillimeter galaxy (SMG) SMM J0939+8315 at z = 2.221, using the Combined Array for Research in Millimeter-wave Astronomy. SMM J0939+8315 hosts a type-2 quasar, and is gravitationally lensed by the radio galaxy 3C220.3 and its companion galaxy at z = 0.685. The 104 GHz continuum emission underlying the CO line is detected toward 3C220.3 with an integrated flux density of Scont = 7.4 ± 1.4 mJy. Using the CO(J = 3 → ? > 2) line intensity of ICO(3-2) = (12.6 ± 2.0) Jy km s−1, we derive a lensing- and excitation-corrected CO line luminosity of L CO(1-0) ′ ? > = (3.4 ± 0.7) × 1010 (10.1/μL) K km s−1 pc2 for the SMG, where μL is the lensing magnification factor inferred from our lens modeling. This translates to a molecular gas mass of Mgas = (2.7 ± 0.6) × 1010 (10.1/μL) M⊙. Fitting spectral energy distribution models to the (sub)-millimeter data of this SMG yields a dust temperature of T = 63.1 − 1.3 + 1.1 ? > K, a dust mass of Mdust = (5.2 ± 2.1) × 108 (10.1/μL) M⊙, and a total infrared luminosity of LIR = (9.1 ± 1.2) ×1012 (10.1/μL) L⊙. We find that the properties of the interstellar medium of SMM J0939+8315 overlap with both SMGs and type-2 quasars. Hence, SMM J0939+8315 may be transitioning from a starbursting phase to an unobscured quasar phase as described by the “evolutionary link” model, according to which this system may represent an intermediate stage in the evolution of present-day galaxies at an earlier epoch.
The Stress of Leprosy as a Mediator of the Relationship Between Coping Resources, Coping Strategies, and Psychological Well-Being in Persons Affected by Leprosy. The Structural Equation Models Through a Correlation Study

Intoduction Psychological strength plays an important role in reducing stress due to leprosy because leprosy can cause physical, psychological, and social problems. For that reason, this study aims to investigate the relationship between coping sources, coping strategies, and psychological well-being through leprosy stress. Methods This research instrument uses a stress perception scale, coping sources, coping strategies, and psychological well-being scale to collect data from 125 participants consisting of women (33.60%) and men 66.40%. The test analysis in this study uses SmartPLS through structural equation modeling to prove the correlation. Results The results of the SEM test indicate that there is a negative relationship between coping resources and leprosy stress, with a coefficient value of (−0.380), p-value of (0.000) <0.05, and a positive relationship is obtained with psychological well-being with the coefficient value of (0.427), p-value of (0.000) <0.05. Meanwhile, the SEM test shows a negative relationship between coping strategies and stress of leprosy, with the coefficient of (−0.566), p-value of (0.000) <0.05, and a positive relationship is obtained with psychological well-being (0.355), p-value of (0.000) < 0.05. Furthermore, on psychological well-being, stress shows a negative relationship, with the coefficient of (−0.212), p-value of (0.002). Discussion Exploration of important coping sources is done to weaken the power of leprosy as a stressor and the use of effective coping strategies is needed to solve physical, psychological, and social problems for “People Affected by Leprosy”, and simultaneously these two attributes are used to achieve prosperity. psychological. better.
The primordial and evolutionary abundance variations in globular-cluster stars: a problem with two unknowns

Abundances of the proton-capture elements and their isotopes in globular-cluster stars correlate with each other in such a manner as if their variations were produced in high-temperature hydrogen burning at the same time in the past. In addition to these primordial abundance variations, the RGB stars in globular clusters, like their eld counterparts, show the evolutionary variations of the C and N abundances and 12 C/ 13 C isotopic ratio. The latter are caused by extra mixing operating in the RGB star’s radiative zone that separates the H-burning shell from the bottom of its convective envelope. We demonstrate that among the potential sources of the primordial abundance variations in globular-cluster stars proposed so far, such as the hot-bottom burning in massive AGB stars and H burning in the convective cores of supermassive and fastrotating massive MS stars, only the supermassive MS stars with M > 10 4 M can explain all the abundance correlations without any ne-tuning of free parameters. We use our assumed chemical composition for the pristine gas in M13 (NGC 6205) and its mixtures with 50% and 90% of the material partially processed in H burning in the 6 10 4 M MS model star as the initial compositions for the normal, intermediate and extreme populations of low-mass stars in this globular cluster, as suggested by its O-Na anti-correlation. We evolve these stars from the zero-age MS to the RGB tip with the thermohaline and parametric prescriptions for the RGB extra mixing. We nd that the 3 He-driven thermohaline convection cannot explain the evolutionary decline of [C/Fe] in M 13 RGB stars, which, on the other hand, is well reproduced with the universal values for the mixing depth and rate calibrated using the observed decrease of [C/Fe] with MV in the globular cluster NGC5466 that does not have the primordial abundance variations.
Superstrings in AdS2 × S2 × T6

We consider the type IIB Green–Schwarz superstring theory on AdS2 × S2 × T6 supported by homogeneous Ramond–Ramond 5-form flux and its type IIA T-duals. One motivation is to understand the solution of this theory based on integrability. This background is a limit of a 1/4 supersymmetric supergravity solution describing four intersecting D3-branes and represents a consistent embedding of AdS2 × S2 into critical superstring theory. Its AdS2 × S2 part with corresponding fermions can be described by a classically integrable PSU(1, 1|2)/SO(1, 1) × U(1) supercoset sigma model. We point out that since the RR 5-form field has non-zero components along the 6-torus directions one cannot, in general, factorize the 10D superstring theory into the supercoset part plus six bosons and six additional massless fermions. Still, we demonstrate that the full superstring model (i) is classically integrable, at least to quadratic order in fermions, and (ii) admits a consistent classical truncation to the supercoset part. Following the analogy with other integrable backgrounds and starting with the finite-gap equations of the PSU(1, 1|2)/SO(1, 1) × U(1) supercoset, we propose a set of asymptotic Bethe ansatz equations for a subset of the quantum string states.
Optimal initial perturbations in streamwise corner-flow

A focus has been put on the stability characteristics of different flow types existing on air vehicles. Flow passing over wings and different junctions on an aircraft face numerous local features, ranging from different pressure gradients, to interacting boundary layers. Primarily, stability characteristics of flow over a wing subject to negative pressure gradient is studied. The current numerical study conforms to an experimental study conducted by Saric and coworkers, in their Arizona State University wind tunnel experiments. Within that framework, a passive control mechanism has been tested to delay transition of flow from laminar to turbulence. The same control approach has been studied here, in addition to underling mechanisms playing major roles in flow transition, such as nonlinear effects and secondary instabilities.Another common three-dimensional flow feature arises as a result of streamlines passing through a junction, the so called corner-flow. For instance, this flow can be formed in the junction between the wing and fuselage on a plane. A series of direct numerical simulations using linear Navier-Stokes equations have been performed to determine the optimal initial perturbation. Optimal refers to a perturbation which can gain the maximum energy from the flow over a period of time. Power iterations between direct and adjoint Navier- Stokes equations determine the optimal initial perturbation. In other words this method seeks to determine the worst case scenario in terms of perturbation growth. Determining the optimal initial condition can help improve the design of such surfaces in addition to possible control mechanisms.