Miracle-dz/UniFAR-FTUs huggingface dataset:
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Place branding is an approach to stimulating territorial development. From the theoretical point of view, place branding in rural areas should be an inclusive and participatory process. Applications and outcomes of the process have been insufficiently investigated so far in rural areas. The oldest place brand in Slovenia, »Babica in Dedek«, is analyzed to present its socioeconomic circumstances, impacts, and challenges from the perspective of local producers. Three qualitative methods are thus applied: analysis of documents, semi-structured interviews, and a focus group. This case study has revealed factors that contribute to new marketing opportunities, product packaging, holding seminars, and advertising local products in the area. On the other hand, the empirical findings are only partly aligned with the theoretical implications: the impacts of place branding are »sectorally limited« instead of being inclusive and participative.
Nebular Spectroscopy: A Guide on H ii Regions and Planetary Nebulae

We present a tutorial on the determination of the physical conditions and chemical abundances in gaseous nebulae. We also include a brief review of recent results on the study of gaseous nebulae, their relevance for the study of stellar evolution, galactic chemical evolution, and the evolution of the universe. One of the most important problems in abundance determinations is the existence of a discrepancy between the abundances determined with collisionally excited lines and those determined by recombination lines: this is called abundance discrepancy factor (ADF) problem, and we review results related to it. Finally, we discuss the possible reasons for the large t2 values observed in gaseous nebulae.
The B3-VLA CSS sample. VIII: New optical identifications from the Sloan Digital Sky Survey. The ultraviolet-optical spectral energy distribution of the young radio sources

Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio sources (CSS/GPS) are generally considered to be mostly young radio sources. In recent years we studied at many wavelengths a sample of these objects selected from the B3-VLA catalog: the B3-VLA CSS sample. Only ~ 60 % of the sources were optically identified. We aim to increase the number of optical identifications and study the properties of the host galaxies of young radio sources. We cross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey (SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5 and 6) and near-IR data from UKIRT and 2MASS. We obtained new identifications and photometric redshifts for eight faint galaxies and for one quasar and two quasar candidates. Overall we have 27 galaxies with SDSS photometry in five bands, for which we derived the ultraviolet-optical spectral energy distribution (UV-O-SED). We extended our investigation to additional CSS/GPS selected from the literature. Most of the galaxies show an excess of ultra-violet (UV) radiation compared with the UV-O-SED of local radio-quiet ellipticals. We found a strong dependence of the UV excess on redshift and analyzed it assuming that it is generated either from the nucleus (hidden quasar) or from a young stellar population (YSP). We also compare the UV-O-SEDs of our CSS/GPS sources with those of a selection of large size (LSO) powerful radio sources from the literature. If the major process of the UV excess is caused by a YSP, our conclusion is that it is the result of the merger process that also triggered the onset of the radio source with some time delay. We do not see evidence for a major contribution from a YSP triggered by the radio sources itself.
Persistent topology of the reionisation bubble network. I: Formalism & Phenomenology

We present a new formalism for studying the topology of H II regions during the Epoch of Reionization, based on persistent homology theory. With persistent homology, it is possible to follow the evolution of topological features over time. We introduce the notion of a persistence field as a statistical summary of persistence data and we show how these fields can be used to identify different stages of reionization. We identify two new stages common to all bubble ionization scenarios. Following an initial pre-overlap and subsequent overlap stage, the topology is first dominated by neutral filaments (filament stage) and then by enclosed patches of neutral hydrogen undergoing outside-in ionization (patch stage). We study how these stages are affected by the degree of galaxy clustering. We also show how persistence fields can be used to study other properties of the ionization topology, such as the bubble size distribution and the fractal-like topology of the largest ionized region.
Collective strong coupling in a lossy optical cavity

We observe vacuum Rabi splitting in a lossy nearly confocal cavity indicating the strong coupling regime, despite a weak single-atom single-mode coupling. Strong collective interaction manifests itself in the typical N 1/2-dependence of the normal mode splitting on the number of atoms N. The TEM00-mode coupling parameters are (g, κ, γ) = 2π × (0.12, 0.8, 2.6) MHz and up to (1.33 ± 0.08) × 105 cesium atoms were loaded into the mode volume.
Determining the awareness and knowledge of officers towards ship energy efficiency measures

Improving energy efficiency practices on ships is crucial for both economic and environmental purposes. Both technical and operational applications are made to increase energy efficiency on ships. The success of energy efficiency applications on ships depends on the effective work of seafarers. Therefore, awareness and knowledge about the energy efficiency of seafarers should be enough. The aim of the study is to determine the awareness and knowledge level of seafarers on energy efficiency on ships and to evaluate energy efficiency practices in maritime transportation companies from the perception of seafarers. In the study, the survey method was used. As a result of the survey, it was found that the knowledge level of the seafarers on ship energy efficiency was low, almost half of them did not receive energy efficiency training but they were informed about the importance of the issue. At the end of the study, it was evaluated that the awareness and knowledge level of officers should be increased in order to improve energy efficiency on ships and suggestions on this issue were determined.
of the Association for Information Systems

In this essay we propose ways to improve the rigor and originality of forward looking theory in the IS field. This is accomplished by proposing a set of guidelines outlining how prospective authors should prepare their manuscripts or approach their research problems so as to enhance theory. We note in particular the potential negative effect of relying too much on reference disciplines in IS theory development and call for strategies that lead to bolder and more original theory
Optical observations of M81 galaxy group in narrow band [SII] and Hα filters: Holmberg IX

SUMMARY: We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and Hfi fllters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identifled as sources with enhanced [SII] emission relative to their Hfi emission) in this galaxy yielded no sources of this kind, besides M&H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with signiflcant Hfi emission that probably represent uncatalogued HII regions.
On the Thermodynamics of 5D Black Holes on ALF Gravitational Instantons

We investigate the thermodynamical properties of solutions to the 5D Einstein and Einstein-Maxwell-dilaton equations describing static black holes on ALF gravitational instantons. Some general expressions regarding the nut charge and potential are derived, as well as Smarr-like relations. The thermodynamics of two particular solutions representing a static black hole on Taub-Nut and Taub-Bolt instantons are examined in detail. Two different approaches for computation of the mass and the tension the Komar and counterterm method, are applied and compared. A new charged black hole on Taub-Bolt instanton is constructed and investigated.
UPDATE ON THE NATURE OF VIRGO OVERDENSITY

We use the Eighth Data Release of Sloan Digital Sky Survey catalog with its additional sky coverage of the southern Galactic hemisphere to measure the extent and to study the nature of the Virgo Overdensity (VOD). The data show that the VOD extends over no less than 2000 deg2, with its true extent likely closer to 3000 deg2. We test whether the VOD can be attributed to a tilt in the stellar halo ellipsoid with respect to the plane of the Galactic disk and find that the observed symmetry of the north–south Galactic hemisphere star counts excludes this possibility. We argue that the Virgo Overdensity, in spite of its wide area and cloud-like appearance, is still best explained by a minor merger. Its appearance and position are qualitatively similar to a near perigalacticon merger event and, assuming that the VOD and the Virgo Stellar Stream (VSS) share the same progenitor, consistent with the VSS orbit determined by Casetti-Dinescu et al.
An assessment of the evidence from ATLAS3D for a variable initial mass function

The ATLAS3D Survey has reported evidence for a non-universal stellar initial mass function (IMF) for early type galaxies (ETGs) (Cappellari et al. 2012, 2013b,a). The IMF was constrained by comparing stellar mass measurements from kinematic data with those from spectral energy distribution (SED) fitting. Here we investigate possible effects of scatter in the reported stellar mass measurements and their potential impact on the IMF determination. We find that a trend of the IMF mismatch parameter with the kinematic mass to light ratio, comparable to the trend observed by Cappellari et al. (2012), could arise if the Gaussian errors of the kinematic mass determination are typically 30%. Without additional data, it is hard to separate between the option that the IMF has a true large intrinsic variation or the option that the errors in the determination are larger than anticipated. A correlation of the IMF with other properties would help to make this distinction, but no strong correlation has been found yet. The strongest correlation is with velocity dispersion. However, it has a large scatter and the correlation depends on sample selection and distance measurements. The correlation with velocity dispersion could be partly caused by the colour-dependent calibration of the surface brightness fluctuation distances of Tonry et al. (2001). We find that the K-band luminosity limited ATLAS3D Survey is incomplete for the highest M/L galaxies below 10^10.3 M_sun. There is a significant IMF - velocity dispersion trend for galaxies with SED masses above this limit, but no trend for galaxies with kinematic masses above this limit. We also find an IMF trend with distance, but no correlation between nearest neighbour ETGs, which excludes a large environmental dependence. Our findings do not rule out the reported IMF variations, but they suggest that further study is needed.
Dietary DHA Enhanced the Textural Firmness of Common Carp (Cyprinus carpio L.) Fed Plant-Derived Diets through Restraining FoxO1 Pathways

Highlights Dietary DHA of 0.42% was beneficial to the growth of common carp fed plant-derived diets; Dietary DHA ameliorated the muscular fatty acid nutrition, and textural firmness of common carp fed plant-derived diets; Myogenic regulatory factors expression was significantly elevated, while mstna expression was decreased by dietary DHA; Dietary DHA modification to the muscular textural firmness of common carp may be attributed to the inhibition of FoxO1 pathways Abstract Omega-3 fatty acids have a positive effect on the muscle textural firmness of fish, while the intrinsic mechanism is poorly understood. To investigate the potential mechanism of textural modification caused by dietary docosahexaenoic acid ( DHA) in common carp (Cyprinus carpio L.), three plant-derived diets with varying DHA levels (0%, 0.5%, 1%, D1–D3) were prepared to feed juveniles (initial weight 15.27 ± 0.77 g) for 8 weeks, and the muscular texture, fibers density, and transcriptome were analyzed. The results showed that the growth performance, muscular DHA content, fibers density, and texture of the fish fed diets D2 and D3 were significantly ameliorated compared with the fish fed diet D1. The muscular transcriptome profiles indicated that the up-regulated genes of fish fed dietary DHA mainly in response to muscle proliferation, as well as the FoxO pathway, were significantly enriched in the D2 and D3 groups. Consistent with this, the Quantitative Real-Time PCR (qRT-PCR ) assays indicated that the expression of myogenic regulatory factors (myog, myod, mrf4, mrf5) was up-regulated in the high-DHA groups. Additionally, the expression of foxo1 (inhibitor of myofiber development) mRNA was down-regulated, while its negative regulatory pathway (MAPK and PI3K) was activated in the D2 and D3 groups. The results suggested that the DHA supplementation is beneficial to modifying the muscular textural firmness of common carp fed plant-derived diets, which could be attributed to the inhibition of FoxO1 pathways.
Auto insurance fraud detection using unsupervised learning

: Insurance fraud represents a source of significant financial loss for insurance companies, particularly auto insurance fraud. Indeed, the insured seeks to increase his indemnity by fraudulent acts or declares a false claim. Consequently, the detection of automobile insurance fraud holds an important place in the strategy of the insurance company, since it allows to reduce the costs of claims and maintain a satisfactory profit. With this in mind, insurers are always looking to have more efficient detection systems in order to overcome the limits of traditional methods. In this paper, we propose an automobile insurance fraud detection system based on Machine Learning. Two unsupervised learning algorithms will be used, namely Isolation Forest and Local Outlier Factor. According to previous studies, these two algorithms are not yet applied in auto insurance fraud detection. Both algorithms belong to the anomaly detection algorithms family which is more suitable for this type of problem. The results of this study show the possibility of developing a detection system, based on these two Machine Learning techniques, which serves to automatically detect fraud with considerable accuracy
UNDERSTANDING PHYSICAL CONDITIONS IN HIGH-REDSHIFT GALAXIES THROUGH C i FINE STRUCTURE LINES: DATA AND METHODOLOGY

We probe the physical conditions in high-redshift galaxies, specifically, the damped Lyα systems (DLAs) using neutral carbon (C i) fine structure lines and molecular hydrogen (H2). We report five new detections of C i and analyze the C i in an additional two DLAs with previously published data. We also present one new detection of H2 in a DLA. We present a new method of analysis that simultaneously constrains both the volume density and the temperature of the gas, as opposed to previous studies that a priori assumed a gas temperature. We use only the column density of C i measured in the fine structure states and the assumption of ionization equilibrium in order to constrain the physical conditions in the gas. We present a sample of 11 C i velocity components in six DLAs and compare their properties to those derived by the global C ii* technique. The resulting median values for this sample are 〈n(H i)〉 = 69 cm−3, 〈T〉 = 50 K, and 〈log(P/k)〉 = 3.86 cm−3 K, with standard deviations, σ = 134 cm−3, σT = 52 K, and σlog(P/k) = 3.68 cm−3 K. This can be compared with the integrated median values for the same DLAs: 〈n(H i)〉 = 2.8 cm−3, 〈T〉 = 139 K, and 〈log(P/k)〉 = 2.57 cm−3 K, with standard deviations σ = 3.0 cm−3, σT = 43 K, and σlog(P/k) = 0.22 cm−3 K. Interestingly, the pressures measured in these high-redshift C i clouds are similar to those found in the Milky Way. We conclude that the C i gas is tracing a higher-density, higher-pressure region, possibly indicative of post-shock gas or a photodissociation region on the edge of a molecular cloud. We speculate that these clouds may be direct probes of the precursor sites of star formation in normal galaxies at high redshift.
Probing discs around massive young stellar objects with CO first overtone emission

We present high resolution (R�50; 000) spectroastrometry over the CO 1 st overtone bandhead of a sample of seven intermediate/massive young stellar objects. These are primarily drawn from the red MSX source (RMS) survey, a systematic search for young massive stars which has returned a large, well selected sample of such objects. The mean luminosity of the sample is approximately 5� 10 4 L�, indicating the objects typically have a mass of� 15 M�. We fit the observed bandhead profiles with a model of a circums tellar disc, and find good agreement between the models and observations for all but one object. We compare the high angular precision (0: 2− 0: 8� 10 −3 arc-seconds) spectroastrometric data to the spatial distr ibution of the emitting material in the best-fitting models. N o spatial signatures of discs are detected, which is entirely consistent with the properties of the best-fitting models. Therefore, the observations suggest that the CO bandhead emission of massive young stellar objects originates in small-scale disks, in agreement with previous work. This provides further evidence that massive stars form via disc accretion, as suggested by recent simulations.
The Gender Investment Gap over the Life-Cycle

Single women hold less risky financial portfolios than single men. This paper analyzes the determinants of the “gender investment gap” based on a structural life-cycle framework. The model is able to rationalize the investment gap without introducing gender heterogeneity in preferences (e.g. in risk aversion). Rather, lower income levels and larger household sizes of single women are the main determinants for explaining the gap. Importantly, expectations about future realizations of both variables (that cannot easily be controlled for in regressions) drive most of the investment differences for young households whereas heterogeneity in observable characteristics explains the gap later in life.
Limits in late time conversion of cold dark matter into dark radiation

Structure formation creates high temperature and density regions in the Universe that allow the conversion of matter into more stable states, with a corresponding emission of relativistic matter and radiation. An example of such a mechanism is the supernova event, that releases relativistic neutrinos corresponding to 99% of the binding energy of remnant neutron star. We take this phenomena as a starting point for an assumption that similar processes could occur in the dark sector, where structure formation would generate a late time conversion of cold dark matter into a relativistic form of dark matter. We performed a phenomenological study about the limits of this conversion, where we assumed a transition profile that is a generalized version of the neutrino production in supernovae events. With this assumption, we obtained an interesting modification for the constraint over the cold dark matter density. We show that when comparing with the standard ΛCDM cosmology, there is no preference for conversion, although the best fit is within 1σ from the standard model best fit. The methodology and the results obtained qualify this conversion hypothesis, from the large scale structure point of view, as a viable and interesting model to be tested in the future with small scale data, and mitigate discrepancies between observations at this scale and the pure cold dark matter model.
THE PSEUDO-EVOLUTION OF HALO MASS

A dark matter halo is commonly defined as a spherical overdensity of matter with respect to a reference density, such as the critical density or the mean matter density of the universe. Such definitions can lead to a spurious pseudo-evolution of halo mass simply due to redshift evolution of the reference density, even if its physical density profile remains constant over time. We estimate the amount of such pseudo-evolution of mass between z = 1 and 0 for halos identified in a large N-body simulation, and show that it accounts for almost the entire mass evolution of the majority of halos with and can be a significant fraction of the apparent mass growth even for cluster-sized halos. We estimate the magnitude of the pseudo-evolution assuming that halo density profiles remain static in physical coordinates, and show that this simple model predicts the pseudo-evolution of halos identified in numerical simulations to good accuracy, albeit with significant scatter. We discuss the impact of pseudo-evolution on the evolution of the halo mass function and show that the non-evolution of the low-mass end of the halo mass function is the result of a fortuitous cancellation between pseudo-evolution and the absorption of small halos into larger hosts. We also show that the evolution of the low-mass end of the concentration–mass relation observed in simulations is almost entirely due to the pseudo-evolution of mass. Finally, we discuss the implications of our results for the interpretation of the evolution of various scaling relations between the observable properties of galaxies and galaxy clusters and their halo masses.
Assessing Possibilities & Limits for Solar Cells

proposed for Quantsol 2010 Assessing Possibilities & Limits for Solar Cells David Cahen and Lee Barnea the Weizmann Institute of Science, Rehovot 76100 ISRAEL We show how two, seemingly simple, criteria can serve to gauge • in how far significant progress is possible for different types of solar cells and • if basic bounds may limit such progress. The criteria are the ratio of • the efficiency of the best commercially available module to that of the best labor­ atory cell, BCM/BLC, and • the ratio of the open circuit voltage of this same best laboratory cell to the bandgap or effective optical absorption edge of the absorbing part of the cell, VOC/EG. BCM/BLC reflects to some extent manufacturing maturity of the cell type, shown by the significantly higher value for CdTe than for CIGS, or for the single-, compared to the multi-junction a-Si modules, with the ratios for the dye and organic systems much lower still. The ratio for the highly developed Si cells does, though, show what can be expec­ ted. Naturally, an additional ratio is that of the best laboratory cell to the ShockleyQueisser (SQ) efficiency, but that is a number, which reflects academic ability rather than industrial promise. VOC/EG expresses a limit that is to some extent related to the SQ limit, but, for example the relatively low value for dyeand organic cells may well indicate basic limitations for such cells, which I will consider as well in this lecture. The significant difference in VOC/EG between CdTe and CIGS cells may reflect the differ­ ence in grain boundary chemistry and physics of these polycrystalline thin film systems, while the low value for a-Si likely expresses (also) the importance of the a-Si tail states. The need to identify and define basic limitations, beyond that given by SQ, and to distin­ guish such limitations from lack of development effort and of maturity is becoming critic­ al for the further development of solar cells, especially for newer types, be they inorgan­ ic (classical) ones or unconventional ones. The BCM/BLC and VOC/EG criteria can play an important role in putting order in the enormous parameter space that we face in mak­ ing our choices for the future.