Miracle-dz/UniFAR-FTUs huggingface dataset:
Projective bundles over toric surfaces

Let $E$ be the Whitney sum of complex line bundles over a topological space $X$. Then, the projectivization $P(E)$ of $E$ is called a \emph{projective bundle} over $X$. If $X$ is a non-singular complete toric variety, so is $P(E)$. In this paper, we show that the cohomology ring of a non-singular projective toric variety $M$ determines whether it admits a projective bundle structure over a non-singular complete toric surface. In addition, we show that two 6-dimensional projective bundles over 4-dimensional quasitoric manifolds are diffeomorphic if their cohomology rings are isomorphic as graded rings. Furthermore, we study the smooth classification of higher dimensional projective bundles over 4-dimensional quasitoric manifolds.
The Boundedness of Calderón Zygmund Operators on the Spaces Fpa,q.

Calderon-Zygmund operators are generalizations of the singular integral operators introduced by Calderon and Zygmund in the fifties [CZ]. These singular integrals are principal value convolutions of the form Tf(x) = lime®0 o|x-y|>e K(x-y) f(y) dy = p.v. K * f(x), where f belongs to some class of test functions.
The broad-band X-ray spectrum of the Seyfert 1 galaxy, MCG+8-11-11

Aims. Evidence is mounting that the main ingredients of the unification models of active galactic nuclei may behave differently from expectations, and be intimately related to fundamental physical parameters. The availability of high signal-to-noise broad-band X-ray spectra provides us with the opportunity to study in detail all the contributions from the materials invoked in these models, and infer their general properties, including whether their presence or absence is related to other quantities. Methods. We present a long (100 ks) Suzaku observation of one of the X-ray brightest AGN, MCG+8-11-11. These data are complemented with the 54-month Swift BAT spectrum, allowing us to perform a broad-band fit to the 0.6–150 keV range. Results. The fits performed in the 0.6–10 keV band provide results consistent with those of a a previous XMM-Newton observation, i.e. a lack of a soft excess, warm absorption along the line of sight, a large Compton reflection component (R � 1), and an absence of a relativistic component of the neutral iron Kα emission line. However, when the PIN and Swift BAT data are included, the reflection amount drops significantly (R � 0.2−0.3), and a relativistic iron line is required, the latter being confirmed by a phenomenological analysis in a restricted energy band (3–10 keV). When a self-consistent model is applied to the whole broad-band data, the observed reflection component appears to be entirely associated with the relativistic component of the iron Kα line. Conclusions. The implied scenario, though strongly model-dependent, requires that all the reprocessing spectral components from Compton-thick material be associated with the accretion disc, and no evidence of a classical pc-scale torus is found. The narrow core of the neutral iron Kα line is therefore produced in Compton-thin material, such as the BLR, similarly to what is found in another Seyfert galaxy, NGC 7213, but with the notable difference that MCG+8-11-11 presents spectral signatures from an accretion disc. The very low accretion rate of NGC 7213 could explain the lack of relativistic signatures in its spectrum, but the absence of the torus in both sources is more difficult to explain, since their luminosities are comparable, and their accretion rates are completely different.
AN EMPIRICAL METHOD FOR IMPROVING THE QUALITY OF RXTE PCA SPECTRA

We fitted all of the several hundred RXTE PCA spectra of the Crab individually to a simple power-law model; the total number of counts in the composite spectrum is >109. We then used the spectrum of residuals to derive a calibration tool, called pcacorr, that we apply to large samples of spectra for GX 339–4, H1743–322, and XTE J1550–564. Application of the tool improved the quality of all the fits, and the improvement is dramatic for spectra with ≳ 107 counts. The Crab residual spectrum is somewhat different for each of the five Proportional Counter Array (PCA) detectors, but it was relatively stable over the course of the mission. We recommend that pcacorr be routinely applied to spectra with ≳ 106 counts and that one include a systematic error of 0.1%, rather than the 0.5–1% value that has customarily been used. We expect that application of the tool will result in an increase in sensitivity of the PCA to faint spectral features by up to an order of magnitude.
THE STAR CLUSTER MASS–GALACTOCENTRIC RADIUS RELATION: IMPLICATIONS FOR CLUSTER FORMATION

Whether or not the initial star cluster mass function is established through a universal, galactocentric-distance-independent stochastic process, on the scales of individual galaxies, remains an unsolved problem. This debate has recently gained new impetus through the publication of a study that concluded that the maximum cluster mass in a given population is not solely determined by size-of-sample effects. Here, we revisit the evidence in favor and against stochastic cluster formation by examining the young ( ≲ ? > a few × 10 8 ? > year old) star cluster mass–galactocentric radius relation in M33, M51, M83, and the Large Magellanic Cloud. To eliminate size-of-sample effects, we first adopt radial bin sizes containing constant numbers of clusters, which we use to quantify the radial distribution of the first- to fifth-ranked most massive clusters using ordinary least-squares fitting. We supplement this analysis with an application of quantile regression, a binless approach to rank-based regression taking an absolute-value-distance penalty. Both methods yield, within the 1 &sgr; ? > to 3 &sgr; ? > uncertainties, near-zero slopes in the diagnostic plane, largely irrespective of the maximum age or minimum mass imposed on our sample selection, or of the radial bin size adopted. We conclude that, at least in our four well-studied sample galaxies, star cluster formation does not necessarily require an environment-dependent cluster formation scenario, which thus supports the notion of stochastic star cluster formation as the dominant star cluster-formation process within a given galaxy.
Search for $2\beta$ decay of $^{106}$Cd with an enriched $^{106}$CdWO$_4$ crystal scintillator in coincidence with four HPGe detectors

A radiopure cadmium tungstate crystal scintillator, enriched in Cd106 to 66%, with mass of 216 g (Cd106WO4), was used to search for double-β decay processes in Cd106 in coincidence with four ultra-low-background high-purity germanium detectors in a single cryostat. Improved limits on the double-β processes in Cd106 have been set on the level of 1020−1021 yr after 13 085 h of data taking. In particular, the half-life limit on the two-neutrino electron capture with positron emission, T2νɛβ+1/2≥1.1×1021 yr, has reached the region of theoretical predictions. With this half-life limit the effective nuclear matrix element for the 2νɛβ+ decay is bounded as M2νɛβ+eff≤1.1. The resonant neutrinoless double-electron captures to the 2718-, 2741-, and 2748-keV excited states of Pd106 are restricted at the level of T1/2≥(8.5×1020−1.4×1021) yr.
A lattice Boltzmann model for multiphase fluid flows

A lattice Boltzmann equation method for simulating multiphase immiscible fluid flows with variation of density and viscosity, based on the model proposed by Gunstensen et al. for two‐component immiscible fluids [Phys. Rev. A 43, 4320 (1991)] is developed. The numerical measurements of surface tension and viscosity agree well with theoretical predictions. Several basic numerical tests, including spinodal decomposition, two‐phase fluid flows in two‐dimensional channels, and two‐phase viscous fingering, are shown in agreement of experiments and analytical solutions.
Nuclear star clusters in 228 spiral galaxies in the HST/WFPC2 archive: catalogue and comparison to other stellar systems

We present a catalogue of photometric and structural properties of 228 nuclear star clusters (NSCs) in nearby late-type disk galaxies. These new measurements are derived from a homogeneous analysis of all suitable WFPC2 images in the $HST$ archive. The luminosity and size of each NSC is derived from an iterative PSF-fitting technique, which adapts the fitting area to the effective radius ($r_{\rm eff}$) of the NSC, and uses a WFPC2-specific PSF model tailored to the position of each NSC on the detector. The luminosities of NSCs are $\leq\! 10^8L_{\rm V,\odot}$, and their integrated optical colours suggest a wide spread in age. We confirm that most NSCs have sizes similar to Globular Clusters (GCs), but find that the largest and brightest NSCs occupy the regime between Ultra Compact Dwarf (UCD) and the nuclei of early-type galaxies in the size-luminosity plane. The overlap in size, mass, and colour between the different incarnations of compact stellar systems provides a support for the notion that at least some UCDs and the most massive Galactic GCs, may be remnant nuclei of disrupted disk galaxies. We find tentative evidence for the NSCs' $r_{\rm eff}$ to be smaller when measured in bluer filters, and discuss possible implications of this result. We also highlight a few examples of complex nuclear morphologies, including double nuclei, extended stellar structures, and nuclear $F606W$ excess from either recent (circum-)nuclear star formation and/or a weak AGN. Such examples may serve as case studies for ongoing NSC evolution via the two main suggested mechanisms, namely cluster merging and $in\ situ$ star formation.
COMPARING NARROW- AND BROAD-LINE AGNs IN A NEW DIAGNOSTIC DIAGRAM FOR EMISSION-LINE GALAXIES BASED ON WISE DATA

Using a new color–color diagnostic diagram in the mid-infrared (MIR) built from WISE data, the MIRDD, we compare narrow-emission-line galaxies (NELGs) that exhibit different activity types (star-forming galaxies (SFGs) and active galactic nuclei (AGNs), i.e., LINERs, Seyfert 2 galaxies (Sy2s), and Transition-type Objects (TOs)), as determined using one standard diagnostic diagram in the optical (BPT–VO), with broad-line AGNs (QSOs and Sy1s) and BL Lac objects at low redshift ( z ≤ 0.25 ? > ). We show that the BL Lac objects occupy the same region as the LINERs in the MIRDD, whereas the QSOs and Sy1s occupy an intermediate region between the LINERs and the Sy2s. In the MIRDD these galaxies trace a sequence that can be reproduced by a power law, F &ngr; = &ngr; &agr; ? > , where the spectral index, α, varies from 0 to −2, which is similar to what is observed in the optical/ultraviolet part of the spectra of AGNs with different luminosities. For the NELGs with different activity types, we perform a stellar-population synthesis analysis, confirming that their specific positions in the MIRD depend on their star formation histories (SFH) and demonstrating that the W 2 − W 3 ? > color is tightly correlated with the level of star formation in their host galaxies. In good agreement with the SFH analysis, a comparison of their MIR colors with the colors yielded by spectral energy distributions (SEDs) of galaxies with different activity types shows that the SED of the LINERs is similar to the SEDs of the QSOs and Sy1s, consistent with AGN galaxies with mild star formation, whereas the SEDs of the Sy2s and TOs are consistent with AGN galaxies with strong star formation components. For the BL Lac objects, we show that their blue MIR colors can only be fitted with an SED that has no star formation component, consistent with AGNs in elliptical-type galaxies. From their similarities in MIR colors and SEDs, we infer that, in the nearby universe, the level of star formation activity most probably increases in the host galaxies of emission-line galaxies with different activity types along the sequence BL Lac → ? > LINER → ? > QSO/Sy1 → ? > Sy2 → ? > TO → ? > SFG.
A KENNICUTT–SCHMIDT LAW FOR INTERVENING ABSORPTION LINE SYSTEMS

We argue that most strong intervening metal absorption line systems, where the rest equivalent width of the Mg ii λ2796 line is >0.5 Å, are interstellar material in, and outflowing from, star-forming disks. We show that a version of the Kennicutt–Schmidt law is readily obtained if the Mg ii equivalent widths are interpreted as kinematic broadening from absorbing gas in outflowing winds originating from star-forming galaxies. Taking a phenomenological approach and using a set of observational constraints available for star-forming galaxies, we are able to account for the density distribution of strong Mg ii absorbers over cosmic time. The association of intervening material with star-forming disks naturally explains the metallicity and dust content of strong Mg ii systems, as well as their high H i column densities, and does not require the advection of metals from compact star-forming regions into the galaxy halos to account for the observations. We find that galaxies with a broad range of luminosities can give rise to absorption of a given rest equivalent width and discuss possible observational strategies to better quantify true galaxy–absorber associations and further test our model. We show that the redshift evolution in the density of absorbers closely tracks the star formation history of the universe and that strong intervening systems can be used to directly probe the physics of both bright and faint galaxies over a broad redshift range. In particular, in its simplest form, our model suggests that many of the statistical properties of star-forming galaxies and their associated outflows have not evolved significantly since z ∼ 2. By identifying strong intervening systems with galaxy disks and quantifying a version of the Kennicutt–Schmidt law that applies to them, a new probe of the interstellar medium is found which provides complementary information to that obtained through emission studies of galaxies. Implications of our results for galaxy feedback and enrichment of the intergalactic medium are discussed.
Determination of Physical Properties of Pads for Maximizing Cooling in Evaporative Cooled Store

Evaporatively cooled storage structure, nowadays, is increasingly being used for on-farm storage of fruits and vegetables. Various design and concepts for constructing this structure are being applied. A structure using pad as cooling medium was designed and constructed for storage of fruits and vegetables. Physical properties of commonly used cooling pads, such as safeda, partal and root pads were studied and rate of water evaporation from their surfaces at different environmental conditions were evaluated for this structure in this investigation. The average bulk density of safeda, partal and root pads varied from 38–46 kg/m3, 35–40 kg/m3 and 111–313 kg/m3 respectively; and decreased with the increase in their thickness. The average true densities of partai, safeda and root pads were found to be 1000, 750 and 590 kg/m3, respectively and among the three cooling pads, partal had maximum porosity and root pad the minimum. The surface evaporation of water from the cooling pads increased with increase in ambient temperature and decrease in the relative humidity irrespective of pad materials and thickness. The highest surface evaporation of 14.87g of water per minute was found to be from the partal cooling pad of 7 mm thickness.
Increasing stability and accuracy of the lattice Boltzmann scheme: recursivity and regularization

In the present paper a lattice Boltzmann scheme is presented which exhibits an increased stability and accuracy with respect to standard singleor multi-relaxa-tion-time (MRT) approaches. The scheme is based on a single-relaxation-time model where a special regularization procedure is applied. This regularization is based on the fact that, for a-thermal ows, there exists a recursive way to express the velocity distribution function at any order (in the Hermite series sense) in terms of the density, velocity, and stress tensor. A linear stability analysis is conducted which shows enhanced dispersion/dissipation relations with respect to existing models. The model is then validated on two (one 2D and one 3D) moderately high Reynolds number simulations (Re 1000) at moderate Mach numbers (Ma 0:5). In both cases the results are compared with an MRT model and an enhanced accuracy and stability is shown by the present model.
Factors Influencing Solar Energy Technology Adoption by Households in Western Province Sri Lanka

The acceptance and slow growth of solar energy in Sri Lanka is a major barrier. The aim of this study was to identify the factors which are more considerable when adopting solar energy technology. Technology Acceptance Model (TAM), Diffusion Of Innovation (DOI), Theory of Planned Behavior (TPB) and Transaction Cost Economics theory (TCE) are the theories that are used to develop the research foundation. Basically five key factors have been identified: namely Relative Advantage, Perceived Behavioural Control, Perceived Ease of Use, Awareness of the Technology and Perceived Cost. A self-administrated questionnaire was conducted to collect data from a sample of 384 respondent households. Structural Equation Modeling (SEM) was used to test the hypothesis. The result of the study indicates that all the key factors have a positive impact with adoption of solar energy technology. Creating better awareness of the benefits of solar energy usage and increase awareness among people towards their responsibility to use green energy sources can encourage the rate of usage amount in domestic consumers. Providing financial support, obtaining continuous feedback and providing free technical advisory schemes are also good practical implications. From a managerial viewpoint these findings can be used for strategic planning to determine effective marketing activities to change customer’s intention to ensure sustainable business growth. Important policy making decision and investment decisions can be taken by these estimates. In consumer’s perspective the study enhances knowledge on solar energy as a power source of green energy for small scale households in urban areas. Though geographical unfairness act as the main limitation, since the high density of population, income level and urbanization of observed area, the result can be generalized to the urbanized households.
The influence of river discharge on gravel bar hyporheic microbial community structure and putative metabolic functions

Microbial communities in the hyporheic zone (HZ) are important in self-purification as the riverbed is metabolically active and responsible for the retention, storage and mineralisation of organic matter transported to the surface water. However, studies exploring HZ microbial community responses to disturbances (e.g. floods) remain scarce. Here, we characterised the microbial community structure among the three (downwelling, upwelling and intermediate) HZ points within and among gravel bars at high and low discharge levels in a dam-regulated river using 16S rRNA metabarcoding. We observed significant dissimilarity in the microbial community at low discharge exhibiting local adaptation due to gravel bar spatial environmental heterogeneity. Moreover, the homogenisation effect resulted in similar microbial community structures among the three points within the gravel bars at high discharge. Microbial communities across adjacent gravel bars were dissimilar, potentially attributing to different bar morphologies. Our study highlights the role of spatial environmental heterogeneity in the biological processes that govern microbial community structure at three hyporheic points in gravel bars at two discharge levels. Our results are essential to understand the HZ microbial communities’ response to the river discharge levels.
Independent Innexin Radiation Shaped Signaling in Ctenophores

Innexins facilitate cell-cell communication by forming gap junctions or non-junctional hemichannels, which play important roles in metabolic, chemical, ionic, and electrical coupling. The lack of knowledge regarding the evolution and role of these channels in ctenophores (comb jellies), the likely sister group to the rest of animals, represents a substantial gap in our understanding of the evolution of intercellular communication in animals. Here we identify and phylogenetically characterize the complete set of innexins of four ctenophores: Mnemiopsis leidyi, Hormiphora californensis, Pleurobrachia bachei, and Beroe ovata. Our phylogenetic analyses suggest that ctenophore innexins diversified independently from those of other animals and were established early in the emergence of ctenophores. We identified a four-innexin genomic cluster, which was present in the last common ancestor of these four species and has been largely maintained in these lineages. Evidence from correlated spatial and temporal gene expression of the M. leidyi innexin cluster suggest that this cluster has been maintained due to constraints related to gene regulation. We describe basic electrophysiological properties of putative ctenophore hemichannels from muscle cells using intracellular recording techniques, showing substantial overlap with the properties of bilaterian innexin channels. Together, our results suggest that the last common ancestor of animals had gap junctional channels also capable of forming functional innexin hemichannels, and that innexin genes have independently evolved in major lineages throughout Metazoa.
Studying metal-protein interactions using fluorescent protein indicators

Metals are widespread environmental toxins that disrupt normal cellular processes through their interactions with proteins and other macromolecules. In this study, we developed the metalsensitive fluorescent protein mseGFP as a ratiometric reporter capable of binding heavy metals. We found that mseGFP bound mercury and lead tightly but had substantially lower sensitivity to other metals. By comparison, the redox sensor roGFP2 functioned as a ratiometric indicator for transition metals, with the highest sensitivity for copper, followed by nickel and cobalt. mseGFP and roGFP2 could also report metal binding through fluorescence quenching, and we used this effect to measure high affinity interactions for both proteins with copper and iron. Crystal structure analysis of mseGFP complexed with phenylarsine oxide revealed an unexpected mode of heavy metal interaction, with mseGFP binding PAO with 2:2 stoichiometry. Glutathione strongly inhibited most metal interactions with the fluorescent protein reporters, but increased the affinity of arsenic and cadmium for mseGFP. When expressed in HEK293T cells, mseGFP reported uptake of mercury and phenylarsine oxide from surrounding media. Glutathione depletion enhanced binding of phenylarsine oxide to mseGFP in cells, validating the importance of glutathione in modulating metal-protein interactions.