Miracle-dz/UniFAR-FTUs huggingface dataset:
Correlation between Spatio-Temporal Evolution of Habitat Quality and Human Activity Intensity in Typical Mountain Cities: A Case Study of Guiyang City, China

The acceleration of the urbanization process brings about the expansion of urban land use, while changes in land-use transformation affect the urban habitat quality, and land-use change brings a threat to regional sustainable development. Against such a backdrop, the assessment of land use on the habitat quality and the relationship between the intensity of human activities is becoming a hot spot in terms of the current land use coordinated with habitat quality. Based on the land-use data of Guiyang in 2000, 2005, 2010, 2015 and 2020, the spatial–temporal evolution characteristics of habitat quality in the study area, combined with the spatial correlation between human activity intensity and habitat quality, were hereby analyzed using the InVEST model. The impact of human activity intensity on habitat quality was correspondingly analyzed. The results show that: (1) From 2000 to 2020, the habitat quality level in Guiyang remained stable without drastic changes, but the changes showed hierarchical distribution and were scattered, mainly reflected in the urban expansion areas of the urban–rural fringe and the key areas of industrial development, and the ecological environment quality fluctuated in a small range. (2) From 2000 to 2020, the intensity of human activities in Guiyang was mainly affected by the relatively concentrated distribution, featuring obvious and significant changes. From 2010 to 2015, the high-impact area surrounded the Guanshan Lake New Area, and the regional habitat quality presented a downward trend. In 2020, the high-impact area of the main urban area and the key industrial development zone was expected to be formed, while the low-impact area was still distributed in forest areas with complex natural conditions. (3) From 2000 to 2020, there was a significant positive correlation between human activity intensity and habitat quality in Guiyang, and such a spatial correlation was weak from 2000 to 2005. The period from 2015 to 2020 witnessed the rapid development of urban construction in Guiyang, human construction activities continue to affect the urban habitat quality. The results show that the intensity of human activities on the promoting function of land use, and the dependencies between them should be considered at the same time, and that explorations on the influence of human activities on land-use intensity and habitat quality of space link are crucial to improving the efficiency of urban land use and ecological environment protection, as well as the coordination between land use and the sustainability of urban development.
A HIGH-RESOLUTION SURVEY OF H i ABSORPTION TOWARD THE CENTRAL 200 pc OF THE GALACTIC CENTER

We present an H i absorption survey of the central 250 pc of the Galaxy. Very Large Array observations were made at 21 cm in the DnC and CnB configurations and have a resolution of ∼15″ (0.6 pc at the Galactic center (GC) distance) and a velocity resolution of ∼2.5 km s−1. This study provides H i data with high spatial resolution, comparable with the many high-resolution observations which have been made of GC sources over the past 10 years. Here we present an overview of the H i absorption toward ∼40 well-known continuum sources and a detailed comparison of the ionized, atomic, and molecular components of the interstellar medium for the Sgr B, Radio Arc, and Sgr C regions. In these well-known regions, the atomic gas appears to be closely correlated in both velocity and distribution to the ionized and molecular gas, indicating that it resides in photodissociation regions related to the H ii regions in the GC. Toward the majority of the radio continuum sources, H i absorption by the 3 kpc arm is detected, constraining these sources to lie beyond a 5 kpc distance in the Galaxy.
Time-dependent diffusion in undulating structures: Impact on axon diameter estimation

Diffusion MRI may enable non-invasive mapping of axonal microstructure. Most approaches infer axon diameters from effects of time-dependent diffusion on the diffusion-weighted MR signal by modelling axons as straight cylinders. Axons do not, however, run in straight trajectories and so far, the impact of the axonal trajectory on diameter estimation has not been systematically investigated. Here, we employ a toy-model of axons, which we refer to as undulating thin-fiber model, to analyze the impact of undulating trajectories on the diffusion-time dependence represented by the diffusion spectrum. We analyze the spectrum by its height (diffusivity at high frequencies), width (half width at half maximum), and low-frequency behavior (power law exponent). Results show that microscopic orientation dispersion of the thin-fibers is the main parameter that determines the characteristics of the diffusion spectra. Straight cylinders and undulating thin-fibers have virtually identical spectra at lower frequencies. If the straight-cylinder assumption is used to interpret data from undulating thin axons, the diameter is overestimated by an amount proportional to the undulation amplitude and the microscopic orientation dispersion. At high frequencies (short diffusion times), spectra from cylinders and undulating thin-fibers differ. The spectra from the undulating thin-fibers can also differ from that of cylinders by exhibiting power law behaviors with exponents below two. In conclusion, we argue that the non-straight nature of axonal trajectories should not be ignored when analyzing dMRI data and that careful experiments may enable separation of diffusion within straight cylinders and diffusion in undulating thin-fibers.
Predicting Fractured Carbonate Reservoirs at the Early Stage of Exploration of Oil and Gas Deposits

The paper considers a possibility of using complex information on morphological parameters of structures, unconnected porosity and reservoir pressure gradient for previously explored deposits for developing a multidimensional equation to estimate the secondary porosity on an example of reservoirs with secondary (fracturing) porosity of Upper Cretaceous deposits in the Terek-Sunzha oil and gas bearing region of Pre-Caucasus. This equation allows predicting the secondary porosity value in new anticlinal structures revealed with seismic survey at later stages of exploration in the respective oil and gas bearing region and using it as a quantitative criterion to predict existence of an entrainment trap. Keywords— fractured reservoir, oil and gas deposit, porosity, prediction, carbonate sediments, Tersek-Sunzha oil and gas bearing region
Performance evaluation of Gurez sheep in farmer’s flocks—A threatened sheep breed of Kashmir

Gurez is an indigenous breed of sheep native to the Gurez Valley of J&K, India. Despite being a unique genetic resource, this breed is largely unexplored and meagre studies have been conducted on it. Hence, a comprehensive study was conducted to study the breed in its native breeding tract. Data on growth, wool, reproduction and morphometric traits of Gurez sheep maintained under farmers' flocks in its native tract were recorded and analyzed for performance evaluation as well as the farming practices in that area with regards to the breed. Screening for parasites and brucellosis, blood biochemistry and mineral profile were also conducted. This triple purpose breed produces milk, meat as well as apparel quality wool. The average values for wool traits were 76.12, 28.31, 4.42, 5.35 and 8.18 for clean wool yield (CWY) (%), fibre diameter (FD) (Î¼), staple length (SL) (cm), crimps per cm (NCPC) and medullation (%), respectively. The coefficient of variations % of these traits ranged from low to very high indicating that the traits had low to very high variability. The least squares mean for clean wool yield (%), fiber diameter (μ), staple length (cm), crimps per cm and medullation (%) were 77.07±0.33, 29.83±0.41, 4.80±0.17, 5.04±0.28 and 9.26±0.79, respectively. The sexual dimorphism was observed in favour of males with respect to all these traits. Age had non-significant effect on these traits in the present study. Black wool samples were having higher estimates of FD, CWY (%), SL and medullation (%). NCPC was higher for white wool samples. Conservation of this unique breed and its selective breeding is highly recommended. The incidence of Eimeria (37.50%) was found to be highest in the area.
Coarse-grained model of the native cellulose I a and the transformation pathways to the I b allomorph

All-atom simulations are used to derive effective parameters for a coarse-grained description of the crystalline cellulose Ia. In this description, glucose monomers are represented by the C4 atoms and non-bonded interactions within the cellulose sheets and between the sheets by effective LennardJones interactions. The parameters are determined by two methods: the Boltzmann inversion and through monitoring of the energies associated with changes of the coarse-grained degrees of freedom. We find that the stiffness-related parameters for cellulose Ia are nearly the same as for Ib allomorph. However, the non-bonded terms are placed differently and are weaker leading to an overall lower energy, and free energy, of Ib compared to Ia. We apply the coarsegrained description to determine amorphous transition states for the room-temperature conversion process between the Ia and Ib allomorphs and to characterize the interface between the crystalline forms of the allomorphs.
A Population of Bona Fide Intermediate-mass Black Holes Identified as Low-luminosity Active Galactic Nuclei

Nearly every massive galaxy harbors a supermassive black hole (SMBH) in its nucleus. SMBH masses are millions to billions of solar mass, and they correlate with properties of spheroids of their host galaxies. While the SMBH growth channels, mergers, and gas accretion are well established, their origin remains uncertain: they could have emerged either from massive “seeds” (105–106 M⊙) formed by direct collapse of gas clouds in the early universe or from smaller (100 M⊙) BHs, end products of first stars. The latter channel would leave behind numerous intermediate-mass BHs (IMBHs, 102–105 M⊙). Although many IMBH candidates have been identified, none are accepted as definitive; thus, their very existence is still debated. Using data mining in wide-field sky surveys and applying dedicated analysis to archival and follow-up optical spectra, we identified a sample of 305 IMBH candidates having masses 3 × 10 4 M ⊙ < M BH < 2 × 10 5 M ⊙ , which reside in galaxy centers and are accreting gas that creates characteristic signatures of a type I active galactic nucleus (AGN). We confirmed the AGN nature of 10 sources (including five previously known objects that validate our method) by detecting the X-ray emission from their accretion disks, thus defining the first bona fide sample of IMBHs in galactic nuclei. All IMBH host galaxies possess small bulges and sit on the low-mass extension of the M BH – M bulge scaling relation, suggesting that they must have experienced very few if any major mergers over their lifetime. The very existence of nuclear IMBHs supports the stellar-mass seed scenario of the massive BH formation.
Anomalous temperature dependence of spin susceptibility around a nonmagnetic impurity in high-Tc cuprate superconductors

Local magnetic properties around a nonmagnetic impurity are investigated in the superconducting state of high-T c cuprates. We consider a model two-dimensional d x 2 - y 2 -wave superconductor with strong antiferromagnetic(AF) spin fluctuations and calculate the spin susceptibility around the impurity. We show that the uniform susceptibility, which is usually suppressed in spin-singlet superconductivity, increases with decreasing temperature around the impurity when the impurity scattering is in the unitarity limit. This anomalous temperature dependence is more remarkable when the impurity potential is extended spatially and the AF spin fluctuations are stronger. Our results agree with the anomalous temperature dependence of the Knight shift on Li that was recently observed in YBa 2 (Cu 1 - x Li x ) 3 O 6 + y .
Psychosocial- and disclosure-related challenges among HIV-serodiscordant couples: an interpretative phenomenological analysis study

Background: Serodiscordant refers to a couple where one has human immunodeficiency virus (HIV), and the other partner is HIV negative. HIV-serodiscordancy often results in diverse psychological and emotional challenges. Evidence demonstrates that the dynamics of living in an HIV-serodiscordant relationship are often stressful. This study explored the psychosocial- and disclosure-related challenges faced by couples in HIV-serodiscordant relationships in South Africa. Methods: An interpretative phenomenological analysis (IPA) design was followed. A total of 13 HIV-serodiscordant partners were purposively sampled. Data were collected through individual face-to-face interviews and analysed using the IPA framework. Results: The findings indicated that HIV-serodiscordant couples experienced diverse psychosocial challenges such as shock, sadness, hurt, denial and disbelief. Participants also experienced challenges such as selective disclosure and fear of further disclosure. Conclusions: The findings have implications for public health and are critical in programming and designing couple-based HIV care interventions. Couples in HIV-serodiscordant relationships would benefit more from differentiated, client-centred psychosocial support. To contribute to the HIV epidemic control and reduction of new HIV infections, specific interventions such as couples counselling, disclosure counselling, support groups, health education and safer conception risk reduction strategies need to be implemented.
THE HOST GALAXIES OF LOW-MASS BLACK HOLES

Using Hubble Space Telescope observations of 147 host galaxies of low-mass black holes (BHs), we systematically study the structures and scaling relations of these active galaxies. Our sample is selected to have central BHs with virial masses of ∼105–106 M☉. The host galaxies have total I-band magnitudes of −23.2 < MI < −18.8 mag and bulge magnitudes of −22.9 < MI < −16.1 mag. Detailed bulge–disk–bar decompositions with GALFIT show that 93% of the galaxies have extended disks, 39% have bars, and 5% have no bulges at all at the limits of our observations. Based on the Sérsic index and bulge-to-total ratio, we conclude that the majority of the galaxies with disks are likely to contain pseudobulges and very few of these low-mass BHs live in classical bulges. The fundamental plane of our sample is offset from classical bulges and ellipticals in a way that is consistent with the scaling relations of pseudobulges. The sample has smaller velocity dispersion at fixed luminosity in the Faber–Jackson plane compared with classical bulges and elliptical galaxies. The galaxies without disks are structurally more similar to spheroidals than to classical bulges according to their positions in the fundamental plane, especially the Faber–Jackson projection. Overall, we suggest that BHs with mass ≲ 106 M☉ live in galaxies that have evolved secularly over the majority of their history. A classical bulge is not a prerequisite to host a BH.
What is the apparent angle of a Kelvin ship wave pattern?

Abstract While the half-angle which encloses a Kelvin ship wave pattern is commonly accepted to be 19.47°, recent observations and calculations for sufficiently fast-moving ships suggest that the apparent wake angle decreases with ship speed. One explanation for this decrease in angle relies on the assumption that a ship cannot generate wavelengths much greater than its hull length. An alternative interpretation is that the wave pattern that is observed in practice is defined by the location of the highest peaks; for wakes created by sufficiently fast-moving objects, these highest peaks no longer lie on the outermost divergent waves, resulting in a smaller apparent angle. In this paper, we focus on the problems of free-surface flow past a single submerged point source and past a submerged source doublet. In the linear version of these problems, we measure the apparent wake angle formed by the highest peaks, and observe the following three regimes: a small Froude number pattern, in which the divergent waves are not visible; standard wave patterns for which the maximum peaks occur on the outermost divergent waves; and a third regime in which the highest peaks form a V-shape with an angle much less than the Kelvin angle. For nonlinear flows, we demonstrate that nonlinearity has the effect of increasing the apparent wake angle so that some highly nonlinear solutions have apparent wake angles that are greater than Kelvin’s angle. For large Froude numbers, the effect on apparent wake angle can be more dramatic, with the possibility of strong nonlinearity shifting the wave pattern from the third regime to the second. We expect that our nonlinear results will translate to other more complicated flow configurations, such as flow due to a steadily moving closed body such as a submarine.
Significance of Temporal Muscle Thickness in Chronic Subdural Hematoma

Background: Reduced temporal muscle thickness (TMT) was verified as an independent negative prognostic parameter for outcome in brain tumor patients. Independent thereof, chronic subdural hematoma (CSDH) is a neurosurgical condition with high recurrence rates and unreliable risk models for poor outcome. Since sarcopenia was associated with poor outcome, we investigated the possible role of TMT and the clinical course of CSDH patients. Methods: This investigation is a single-center retrospective study on patients with CSDH. We analyzed the radiological and clinical data sets of 171 patients with surgically treated CSDH at a University Hospital from 2017 to 2020. Results: Our analysis showed a significant association between low-volume TMT and increased hematoma volume (p < 0.001), poor outcome at discharge (p < 0.001), and reduced performance status at 3 months (p < 0.002). Conclusion: TMT may represent an objective prognostic parameter and assist the identification of vulnerable CSDH patients.
The HELLAS2XMM survey XIII. Multi-component analysis of the spectral energy distribution of obscured AGN

Aims. We combine near-to-mid-IR Spitzer data with shorter wavelength observations (optical to X-rays) to get insight into the properties of a sample of luminous, obscured active galactic nuclei (AGN). We aim at modelling their broad-band spectral energy distributions (SEDs) in order to estimate the main parameters related to the dusty torus that is assumed to be responsible for the reprocessed IR emission. Our final goal is to estimate the intrinsic nuclear luminosities and the Eddington ratios for our luminous, obscured AGN. Methods. The sample comprises 16 obscured high-redshift (0.9 < z < 2.1), X-ray luminous quasars (L2−10 keV ∼ 10 44 erg s −1 ) selected from the HELLAS2XMM survey in the 2–10 keV band. The optical-IR SEDs are described by a multi-component model that includes a stellar component to account for the optical and near-IR emission, an AGN component that dominates in the mid-IR (mainly emission from a dusty torus heated by nuclear radiation), and a starburst to reproduce the far-IR bump. A radiative transfer code to compute the spectrum and intensity of dust reprocessed emission was extensively tested against our multiwavelength data. While the torus parameters and the BH accretion luminosities are a direct output of the SED-fitting procedure, the BH masses were estimated indirectly by means of the local Mbulge–MBH relation. Results. The majority (∼80%) of the sources show moderate optical depth (τ9.7 μm ≤ 3), and the derived column densities NH are consistent with the X-ray inferred values (10 22 < NH < 3 × 10 23 cm −2 ) for most of the objects, confirming that the sources are moderately obscured Compton-thin AGN. Accretion luminosities in the range 5 × 10 44 < Lbol < 4 × 10 46 erg s −1 are inferred from the multiwavelength fitting procedure. We compare model luminosities with those obtained by integrating the observed SED, finding that the latter are lower by a factor of ∼2 in the median. The discrepancy can be as high as an order of magnitude for models with high optical depth (τ9.7 μm = 10). The ratio between the luminosities obtained by the fitting procedure and from the observed SED suggest that, at least for type 2 AGN, observed bolometric luminosities are likely to underestimate intrinsic ones and the effect is more severe for highly obscured sources. Bolometric corrections from the hard X-ray band are computed and have a median value of k2−10 keV ∼ 20. The obscured AGN in our sample are characterized by relatively low Eddington ratios (median λEdd ∼ 0.08). On average, they are consistent with the Eddington ratio increasing at increasing bolometric correction.
The skewed multifractal random walk with applications to option smiles

Abstract We generalize the construction of the multifractal random walk (MRW) due to Bacry et al (Bacry E, Delour J and Muzy J-F 2001 Modelling financial time series using multifractal random walks Physica A 299 84) to take into account the asymmetric character of financial returns. We show how one can include in this class of models the observed correlation between past returns and future volatilities, in such a way that the scale invariance properties of the MRW are preserved. We compute the leading behaviour of q-moments of the process, which behave as power laws of the time lag with an exponent ζ q =p−2p(p−1)λ2 for even q=2p, as in the symmetric MRW, and as ζ q =p + 1−2p 2λ2−α (q=2p + 1), where λ and α are parameters. We show that this extended model reproduces the ‘HARCH’ effect or ‘causal cascade’ reported by some authors. We illustrate the usefulness of this ‘skewed’ MRW by computing the resulting shape of the volatility smiles generated by such a process, which we compare with approximate cumulant expansion formulae for the implied volatility. A large variety of smile surfaces can be reproduced.
The structure of voids

Using high resolution N-body simulations we address the problem of emptiness of giant � 20h −1 Mpc–diameter voids found in the distribution of bright galaxies. Are the voids filled by dwarf galaxies? Do cosmological models predict too many small dark matter haloes inside the voids? Can the problems of cosmological models on small scales be addressed by studying the abundance of dwarf galaxies inside voids? We find that voids in the distribution of 10 12 h −1 M⊙ haloes (expected galactic magnitudes � M∗) are almost the same as the voids in 10 11 h −1 M⊙ haloes. Yet, much smaller haloes with masses 10 9 h −1 M⊙ and circular velocities vcirc � 20 km/s readily fill the voids: there should be almost 1000 of these haloes in a 20h −1 Mpc–diameter void. A typical void of diameter 20h −1 Mpc contains about 50 haloes with vcirc > 50 km/s. The haloes are arranged in a pattern, which looks like a miniature Universe: it has the same structural elements as the large-scale structure of the galactic distribution of the Universe. There are filaments and voids; larger haloes are at the intersections of filaments. The only difference is that all masses are four orders of magnitude smaller. There is severe (anti)bias in the distribution of haloes, which depends on halo mass and on the distance from the centre of the void. Large haloes are more antibiased and have a tendency to form close to void boundaries. The mass function of haloes in voids is different from the “normal” mass function. It is much steeper for high masses resulting in very few M33-type galaxies (vcirc � 100 km/s). We present an analytical approximation for the mass function of haloes in voids.