Miracle-dz/UniFAR-FTUs huggingface dataset:
Using meaningful places as an indicator for sense of place in the management of social-ecological systems

Sense of place is increasingly advocated to support the management of social-ecological systems. Given the concept’s complexity, we suggest that an indicator for sense of place is needed to facilitate its application in practical planning. We propose such an indicator called “meaningful places,” defined as geographic locations to which (i) immediately perceived as well as socially constructed meanings are ascribed and (ii) evaluative attachments are tied. We applied the indicator in two independent case studies, Lübeck and Lahn, both of which aimed to integrate sense of place in an actual planning process. The case studies differed in the spatial scale of the meaningful places, the indicator’s operationalization, and the specific assessment methods. In the Lübeck case, semi-structured interviews and a simple mapping method were used to analyze participants’ “home-regions. ” The results revealed diverse but overlapping locations characterized as aesthetic, different from others, close to nature, and quiet (place meanings). In the Lahn case, a public participation GIS (public participation geographic information system [PPGIS]) survey was conducted and yielded insights into the spatial distribution of meaningful places. The results reflect a wide range of place meanings linked to, for example, activities, aesthetic qualities, or well-being. Furthermore, participants expressed different intensities of place attachments. Although the indicator is still in an exploratory stage, it allows for reflection on potential benefits for planning practitioners. The resulting data can be combined with spatial information usually used in planning processes, e.g., about the state of the underlying physical environment and/or foreseeable drivers of change. This offers new opportunities for managers regarding the determination of priorities to conserve meaningful places, the anticipation of conflicts, and the utilization of the communicative power of meaningful places. We argue that the benefits for planning justify a new direction of research devoted to the development and further advancement of the indicator.
Star Formation in the Cometary Tails Associated with Cluster Galaxies

We investigate the star-formation in cometary tails of galaxies in clusters. In particular, we focus on the evolution of molecular clouds in the tails that generate the stars. Assuming that the gas tails had been derived from the galaxies through ram-pressure stripping, we found that the gas must have been stripped mostly not in the form of molecular clouds, but in the form of H I gas or molecular gas that is not in clouds. Moreover, the molecular clouds are condensed in the tails, even away from the host galaxies. We also found that magnetic fields may be required to suppress the Kelvin–Helmholtz (KH) instability on the surface of molecular clouds, because otherwise the KH instability may destroy the molecular clouds before stars are formed in them.
Warm Dark Matter Galaxies with Central Supermassive Black Holes

We generalize the Thomas–Fermi approach to galaxy structure to include central supermassive black holes and find, self-consistently and non-linearly, the gravitational potential of the galaxy plus the central black hole (BH) system. This approach naturally incorporates the quantum pressure of the fermionic warm dark matter (WDM) particles and shows its full power and clearness in the presence of supermassive black holes. We find the main galaxy and central black hole magnitudes as the halo radius rh, halo mass Mh, black hole mass MBH, velocity dispersion σ, and phase space density, with their realistic astrophysical values, masses and sizes over a wide galaxy range. The supermassive black hole masses arise naturally in this framework. Our extensive numerical calculations and detailed analytic resolution of the Thomas–Fermi equations show that in the presence of the central BH, both DM regimes—classical (Boltzmann dilute) and quantum (compact)—do necessarily co-exist generically in any galaxy, from the smaller and compact galaxies to the largest ones. The ratio R(r) of the particle wavelength to the average interparticle distance shows consistently that the transition, R≃1, from the quantum to the classical region occurs precisely at the same point rA where the chemical potential vanishes. A novel halo structure with three regions shows up: in the vicinity of the BH, WDM is always quantum in a small compact core of radius rA and nearly constant density; in the region rAri, the WDM gravity potential dominates, and the known halo galaxy shows up with its astrophysical size. DM is a dilute classical gas in this region. As an illustration, three representative families of galaxy plus central BH solutions are found and analyzed: small, medium and large galaxies with realistic supermassive BH masses of 105M⊙, 107M⊙ and 109M⊙, respectively. In the presence of the central BH, we find a minimum galaxy size and mass Mhmin≃107M⊙, larger (2.2233×103 times) than the one without BH, and reached at a minimal non-zero temperature Tmin. The supermassive BH heats up the DM and prevents it from becoming an exactly degenerate gas at zero temperature. Colder galaxies are smaller, and warmer galaxies are larger. Galaxies with a central black hole have large masses Mh>107M⊙>Mhmin; compact or ultracompact dwarf galaxies in the range Math input error cannot harbor central BHs. We find novel scaling relations MBH=DMh38 and rh=CMBH43, and show that the DM galaxy scaling relations Mh=bΣ0rh2 and Mh=aσh4/Σ0 hold too in the presence of the central BH, Σ0 being the constant surface density scale over a wide galaxy range. The galaxy equation of state is derived: pressure P(r) takes huge values in the BH vicinity region and then sharply decreases entering the classical region, following consistently a self-gravitating perfect gas P(r)=σ2ρ(r) behavior.
Halo histories versus galaxy properties at z = 0-III. The properties of star-forming galaxies

Author(s): Tinker, JL; Hahn, CH; Mao, YY; Wetzel, AR | Abstract: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We measure how the properties of star-forming central galaxies correlate with large-scale environment, d, measured on 10 h-1 Mpc scales. We use galaxy group catalogues to isolate a robust sample of central galaxies with high purity and completeness. The galaxy properties we investigate are star formation rate (SFR), exponential disc scale length Rexp, and Sersic index of the galaxy light profile, nS. We find that, at all stellar masses, there is an inverse correlation between SFR and δ, meaning that above-average star-forming centrals live in underdense regions. For nS and Rexp, there is no correlation with δ at M* ≲ 1010.5 M⊙, but at higher masses there are positive correlations; a weak correlation with Rexp and a strong correlation with nS. These data are evidence of assembly bias within the star-forming population. The results for SFR are consistent with a model in which SFR correlates with present-day halo accretion rate, Mh. In thismodel, galaxies are assigned to haloes using the abundance-matching ansatz, which maps galaxy stellar mass onto halo mass. At fixed halo mass, SFR is then assigned to galaxies using the same approach, but Mh is used to map onto SFR. The best-fitting model requires some scatter in the Mh-SFR relation. The Rexp and nS measurements are consistent with a model in which both of these quantities are correlated with the spin parameter of the halo, λ. Halo spin does not correlate with δ at low halo masses, but for higher mass haloes, high-spin haloes live in higher density environments at fixed Mh. Put together with the earlier instalments of this series, these data demonstrate that quenching processes have limited correlation with halo formation history, but the growth of active galaxies, as well as other detailed galaxies properties, are influenced by the details of halo assembly.
Snake instability of dark solitons in fermionic superfluids

(Dated: October 10, 2013)We present numerical calculations of the snake instability in a Fermi superﬂuid within theBogoliubov-de Gennes theory of the BEC to BCS crossover using the random phase approxima-tion complemented by time-dependent simulations. We examine the snaking behaviour across thecrossover and quantify the timescale and lengthscale of the instability. While the dynamic showsextensive snaking before eventually producing vortices and sound on the BEC side of the crossover,the snaking dynamics is preempted by decay into sound due to pair breaking in the deep BCSregime. At the unitarity limit, hydrodynamic arguments allow us to link the rate of snaking to theexperimentally observable ratio of inertial to physical mass of the soliton. In this limit we witness anunresolved discrepancy between our numerical estimates for the critical wavenumber of suppressionof the snake instability and recent experimental observations with an ultra-cold Fermi gas.
A New Single-Phase Flying Inductor-Based Common Grounded Converter for Dual-Purpose Application

This article presents a new common grounded flying inductor-based converter as power electronics interface suitable for application in both dc or single-phase ac grids using the same terminals. This topology enables direct connection of the negative terminal of the input dc power supply to the negative polarity of the converter output. Therefore, the leakage current is eliminated completely. The voltage boosting feature in single-stage and operation in a wide range of input dc power supply is the other benefit of the proposed solution. Since electrolytic capacitors are not used in the structure, the life of the converter is increased. The operation modes of the converter are explained in detail. Also, the design considerations for passive elements are discussed. To verify the accuracy of the performance of the proposed topology, a laboratory prototype (3.6 kW/6 kW) was built. Also, the related experimental results are presented.
BEYOND THE BRIM OF THE HAT: KINEMATICS OF GLOBULAR CLUSTERS OUT TO LARGE RADII IN THE SOMBRERO GALAXY

We have obtained radial velocity measurements for 51 new globular clusters around the Sombrero galaxy. These measurements were obtained using spectroscopic observations from the AAOmega spectrograph on the Anglo-Australian Telescope and the Hydra spectrograph at WIYN. Combining our own past measurements and velocity measurements obtained from the literature, we have constructed a large database of radial velocities that contains a total of 360 confirmed globular clusters. Previous studies' analyses of the kinematics and mass profile of the Sombrero globular cluster system have been constrained to the inner ∼9′ (∼24 kpc or ∼5Re), but our new measurements have increased the radial coverage of the data, allowing us to determine the kinematic properties of M104 out to ∼15′ (∼41 kpc or ∼9Re). We use our set of radial velocities to study the GC system kinematics and to determine the mass profile and V-band mass-to-light profile of the galaxy. We find that M/LV increases from 4.5 at the center to a value of 20.9 at 41 kpc (∼9Re or 15′), which implies that the dark matter halo extends to the edge of our available data set. We compare our mass profile at 20 kpc (∼4Re or ∼7.′4) to the mass computed from X-ray data and find good agreement. We also use our data to look for rotation in the globular cluster system as a whole, as well as in the red and blue subpopulations. We find no evidence for significant rotation in any of these samples.
Integrating Light Curve and Atmospheric Modeling of Transiting Exoplanets

Spectral retrieval techniques are currently our best tool to interpret the observed exoplanet atmospheric data. Said techniques retrieve the optimal atmospheric components and parameters by identifying the best fit to an observed transmission/emission spectrum. Over the past decade, our understanding of remote worlds in our galaxy has flourished thanks to the use of increasingly sophisticated spectral retrieval techniques and the collective effort of the community working on exoplanet atmospheric models. A new generation of instruments in space and from the ground is expected to deliver higher quality data in the next decade; it is therefore paramount to upgrade current models and improve their reliability, their completeness, and the numerical speed with which they can be run. In this paper, we address the issue of reliability of the results provided by retrieval models in the presence of systematics of unknown origin. More specifically, we demonstrate that if we fit directly individual light curves at different wavelengths (L-retrieval), instead of fitting transit or eclipse depths, as it is currently done (S-retrieval), the said methodology is more sensitive against astrophysical and instrumental noise. This new approach is tested, in particular, when discrepant simulated observations from Hubble Space Telescope/Wide Field Camera 3 and Spitzer/IRAC are combined. We find that while S-retrievals converge to an incorrect solution without any warning, L-retrievals are able to flag potential discrepancies between the data sets.
Overcoming Barriers to Engagement with Educational Video Games for Self-Directed Learning: A Mixed-Methods Case Study

Research has established increased engagement and positive behavioral, attitudinal, and learning outcomes from educational games. Although engagement begets these benefits, there is a lack of research on how students engage with educational games, especially when self-directed. Additionally, research on the effects of engagement on performance is conflicting. This study aimed to identify barriers to students' self-directed engagement with two anatomy educational games, methods to overcome identified barriers, and the impact of engagement on learning performance. Employing the within-case and cross-case approach and triangulation of data, four educational-game specific barriers emerged (from most common to least common): 1) negative perceptions of educational games, 2) incompatible audience, 3) incompatible difficulty, and 4) price. Path analysis found that engagement may have insignificant, positive effects on performance. These findings indicate that students' self-directed engagement with educational games is impeded by unique barriers and engagement may not be vital for performance. Suggestions for game design and marketing emerged to help developers, teachers, and researchers overcome identified barriers.
Almost gone: SN 2008S and NGC 300 2008OT-1 are fainter than their progenitors

We present late-time Hubble and Spitzer Space Telescope imaging of SN 2008S and NGC 300 2008OT-1, the prototypes of a common class of stellar transients whose true nature is debated. Both objects are still fading and are now >15 times fainter than the progenitors in the mid-IR and are undetected in the optical and near-IR. Data from the Large Binocular Telescope and Magellan show that neither source has been variable in the optical since fading in 2010. We present models of surviving sources obscured by dusty shells or winds and find that extreme dust models are needed for surviving stars to be successfully hidden by dust. Explaining these transients as supernovae explosions, such as the electron capture supernovae believed to be associated with extreme AGB stars, seems an equally viable solution. Though SN 2008S is not detected in Chandra X-Ray Observatory data taken in 2012, the flux limits allow the fading IR source to be powered solely by the shock interaction of ejecta with the circumstellar medium if the shock velocity at the time of the observation was >20% slower than estimated from emission line widths while the transient was still optically bright. Continued SST monitoring and 10-20 micron observations with JWST can resolve any remaining ambiguities.
GASP. II. A MUSE View of Extreme Ram-Pressure Stripping along the Line of Sight: Kinematics of the Jellyfish Galaxy JO201

This paper presents a spatially resolved kinematic study of the jellyfish galaxy JO201, one of the most spectacular cases of ram-pressure stripping (RPS) in the GAs Stripping Phenomena in galaxies with MUSE (GASP) survey. By studying the environment of JO201, we find that it is moving through the dense intracluster medium of Abell 85 at supersonic speeds along our line of sight, and that it is likely accompanied by a small group of galaxies. Given the density of the intracluster medium and the galaxy’s mass, projected position, and velocity within the cluster, we estimate that JO201 must so far have lost ∼50% of its gas during infall via RPS. The MUSE data indeed reveal a smooth stellar disk accompanied by large projected tails of ionized ( ) gas, composed of kinematically cold (velocity dispersion <40 km s−1) star-forming knots and very warm (>100 km s−1) diffuse emission, that extend out to at least from the galaxy center. The ionized -emitting gas in the disk rotates with the stars out to ∼6 kpc; but, in the disk outskirts, it becomes increasingly redshifted with respect to the (undisturbed) stellar disk. The observed disturbances are consistent with the presence of gas trailing behind the stellar component resulting from intense face-on RPS along the line of sight. Our kinematic analysis is consistent with the estimated fraction of lost gas and reveals that stripping of the disk happens outside-in, causing shock heating and gas compression in the stripped tails.
Common continuum polarization properties: a possible link between proto-planetary nebulae and Type Ia Supernova progenitors

The lines of sight to highly reddened SNe Ia show peculiar continuum polarization curves, growing towards blue wavelengths and peaking at λmax≲0. 4μm , like no other sightline to any normal Galactic star. We examined continuum polarization measurements of a sample of asymptotic giant branch (AGB) and post-AGB stars from the literature, finding that some proto-planetary nebulae (PPNe) have polarization curves similar to those observed along SN Ia sightlines. These polarization curves are produced by scattering on circumstellar dust. We discuss the similarity and the possibility that at least some SNe Ia might explode during the post-AGB phase of their binary companion. Furthermore, we speculate that the peculiar SN Ia polarization curves might provide observational support to the core-degenerate progenitor model.
Recurrent CME-like Eruptions in Emerging Flux Regions. I. On the Mechanism of Eruptions

We report on three-dimensional (3D) magnetohydrodynamic (MHD) simulations of recurrent eruptions in emerging flux regions. We find that reconnection of sheared field lines, along the polarity inversion line of an emerging bipolar region, leads to the formation of a new magnetic structure, which adopts the shape of a magnetic flux rope (FR) during its rising motion. Initially, the FR undergoes a slow-rise phase and, eventually, it experiences a fast-rise phase and ejective eruption toward the outer solar atmosphere. In total, four eruptions occur during the evolution of the system. For the first eruption, our analysis indicates that the torus instability initiates the eruption and that tether-cutting reconnection of the field lines, which envelop the FR, triggers the rapid acceleration of the eruptive field. For the following eruptions, we conjecture that it is the interplay between tether-cutting reconnection and torus instability that causes the onset of the various phases. We show the 3D shape of the erupting fields, focusing more on how magnetic field lines reconnect during the eruptions. We find that when the envelope field lines reconnect mainly with themselves, hot and dense plasma is transferred closer to the core of the erupting FR. The same area appears to be cooler and less dense when the envelope field lines reconnect with neighboring sheared field lines. The plasma density and temperature distribution, together with the rising speeds, energies, and size of the erupting fields, indicate that they may account for small-scale (mini) coronal mass ejections.
Relational Network for Skeleton-Based Action Recognition

With the fast development of effective and low-cost human skeleton capture systems, skeleton-based action recognition has attracted much attention recently. Most existing methods use Convolutional Neural Network (CNN) and Recurrent Neural Network (RNN) to extract spatio-temporal information embedded in the skeleton sequences for action recognition. However, these approaches are limited in the ability of relational modeling in a single skeleton, due to the loss of important structural information when converting the raw skeleton data to adapt to the input format of CNN or RNN. In this paper, we propose an Attentional Recurrent Relational Network-LSTM (ARRN-LSTM) to simultaneously model spatial configurations and temporal dynamics in skeletons for action recognition. We introduce the Recurrent Relational Network to learn the spatial features in a single skeleton, followed by a multi-layer LSTM to learn the temporal features in the skeleton sequences. Between the two modules, we design an adaptive attentional module to focus attention on the most discriminative parts in the single skeleton. To exploit the complementarity from different geometries in the skeleton for sufficient relational modeling, we design a two-stream architecture to learn the structural features among joints and lines simultaneously. Extensive experiments are conducted on several popular skeleton datasets and the results show that the proposed approach achieves better results than most mainstream methods.
Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

Globular clusters (GCs) are some of the most visible tracers of the merging and accretion histories of galaxy halos. Metal-poor GCs, in particular, are thought to arrive in massive galaxies largely through dry, minor merging events, but it is rare to see a direct connection between GCs and visible stellar streams. NGC 474 is a post-merger early-type galaxy with dramatic fine structures made of concentric shells and radial streams that have been more clearly revealed by deep imaging. We present a study of GCs in NGC 474 to better establish the relationship between merger-induced fine structure and the GC system. We find that many GCs are superimposed on visible streams and shells, and about 35% of GCs outside are located in regions of fine structure. The spatial correlation between GCs and fine structure is significant at the 99.9% level, which shows that this correlation is not coincidental. The colors of GCs on fine structures are mostly blue, and we also find an intermediate-color population that is dominant in the central region and that will likely passively evolve to have colors consistent with a traditional metal-rich GC population. The association of the blue GCs with fine structures is direct confirmation that many metal-poor GCs are accreted onto massive galaxy halos through merging events and that the progenitors of these mergers are sub- galaxies.
MODL: A Modular Ontology Design Library

Pattern-based, modular ontologies have several beneficial properties that lend themselves to FAIR data practices, especially as it pertains to Interoperability and Reusability. However, developing such ontologies has a high upfront cost, e.g. reusing a pattern is predicated upon being aware of its existence in the first place. Thus, to help overcome these barriers, we have developed MODL: a modular ontology design library. MODL is a curated collection of well-documented ontology design patterns, drawn from a wide variety of interdisciplinary use-cases. In this paper we present MODL as a resource, discuss its use, and provide some examples of its contents.