Miracle-dz/UniFAR-FTUs huggingface dataset:
A visual segmentation method for temporal smart card data

ABSTRACT In many cities, worldwide public transit companies use smart card system to manage fare collection. Analysis of this acquisitive information provides a comprehensive insight of user's influence in the interactive public transit network. In this regard, analysis of temporal data, describing the time of entering to the public transit network is considered as the most substantial component of the data gathered from the smart cards. Classical distance-based techniques are not always suitable to analyze this time series data. A novel projection with intuitive visual map from higher dimension into a three-dimensional clock-like space is suggested to reveal the underlying temporal pattern of public transit users. This projection retains the temporal distance between any arbitrary pair of time-stamped data with meaningful visualization. Consequently, this information is fed into a hierarchical clustering algorithm as a method of data segmentation to discover the pattern of users.
Migration of protoplanets with surfaces through discs with steep temperature gradients

We perform three-dimensional self-gravitating radiative transfer simulations of protoplanet migration in circumstellar discs to explore the impact upon migration of the radial temperature profiles in these discs. We model protoplanets with masses ranging between 10–100 M⊕, in discs with surface density profiles of Σ∝r−1/2, and temperature profiles of the form T∝r−β, where β ranges 0–2. We find that steep (β > 1) temperature profiles lead to outward migration of low-mass protoplanets in interstellar grain opacity discs, but in more optically thin discs the migration is always inwards. The trend in migration rates with changing β obtained from our models shows good agreement with those obtained using recent analytic descriptions which include consideration of the coorbital torques and their saturation. We find that switching between two models of the protoplanet, one in which accretion acts by evacuating gas and one in which gas piles up on a surface to form an atmosphere, leads to a small shift in the migration rates. If comparing these models in discs with conditions which lead to a marginally inward migration, the small shift can lead to outward migration. However, the direction and speed of migration is dominated by disc conditions rather than by the specific prescription used to model the flow near the protoplanet.
Environmental quenching and galactic conformity in the galaxy cross-correlation signal

It has long been known that environment has a large effect on star formation in galaxies. There are several known plausible mechanisms to remove the cool gas needed for star formation, such as strangulation, harassment and ram-pressure stripping. It is unclear which process is dominant, and over what range of stellar mass. In this paper, we find evidence for suppression of the cross-correlation function between massive galaxies and less massive star-forming galaxies, giving a measure of how less likely a galaxy is to be star-forming in the vicinity of a more massive galaxy. We develop a formalism for modelling environmental quenching mechanisms within the Halo Occupation Distribution formalism. We find that at $z \sim 2$ environment is not a significant factor in determining quenching of star-forming galaxies, and that galaxies are quenched with similar probabilities in group environments as they are globally. However, by $z \sim 0.5$ galaxies are much less likely to be star forming when in a group environment than when not. This increased probability of being quenched does not appear to have significant radial dependence within the halo, supportive of the quenching being caused by the halting of fresh inflows of pristine gas, as opposed to by tidal stripping. Furthermore, by separating the massive sample into passive and star-forming, we see that this effect is further enhanced when the central galaxy is passive. This effect is present only in the 1-halo term (within a halo) at high redshifts ($z>1$), but is apparent in the 2-halo term at lower redshifts ($z
Multiple input multiple output measurements and modeling in Manhattan

Narrowband MIMO measurements using 16 transmitters and 16 receivers at 2.11 GHz were carried out in Manhattan (see Ling, J. et al., IEE Electronics Letters, vol.37, no.16, p.1041-2, 2001). High capacities were found for full as well as smaller array configurations, all within 80% of the fully scattering channel capacity. Correlation model parameters are derived from the data. Spatial MIMO channel capacity statistics are found to be well represented by the separate transmitter and receiver correlation matrices, with a median relative error in capacity of 3%, in contrast with the 18% median relative error observed by assuming uncorrelated antennas. A reduced parameter model (4 parameters) has been developed to represent the channel correlation matrices statistically. These correlation matrices are used to generate H matrices with capacities that are consistent within a few percent of those measured in New York. Our spatial channel model allows simulations of H matrices for arbitrary antenna configurations. These channel matrices may be used to test receiver algorithms in system performance studies. These results may also be used for antenna array design, as the decay of mobile antenna correlation with antenna separation is reported. An important finding for the base transmitter array was that the antennas were largely uncorrelated even at antenna separations as small as two wavelengths.
A unified theory correcting Einstein-Laub electrodynamics solves dilemmas in the photon momenta and electromagnetic stress tensors

To unify and clarify the persistently debated electromagnetic stress tensors (ST) and photon momenta, we establish a theory inspired by the Einstein-Laub formalism inside an arbitrary macroscopic object immersed in any complex medium. Our generalized Einstein-Laub force and ST yield the total force experienced by any generic macroscopic object due to the internal field interacting with its atoms, charges and molecules. Appropriate scenarios are established for the conservation of a newly proposed momentum that we call non-mechanical generalized Einstein-Laub momentum, along with the kinetic and canonical momenta of photons. Our theory remains valid even in a generally heterogeneous or bounded embedding background medium without resorting to hidden momenta, and unambiguously identifies the existence domain, or validity domain, of the STs and photon momenta proposed to date. This existence domain is the region either outside a macroscopic scatterer with only exterior fields, or at its interior with only inside fields. The appropriate identification of such existence domain constitutes the basis of our unified theory. Finally, a thought experiment is proposed, which shows that the appropriate force and the photon momentum in the embedding medium can also be properly identified if the background is comparatively larger than the embedded scatterer. It also explains the fully different roles of the Abraham and Minkowski photon momenta in the embedding medium. Most importantly, our unified theory reveals that a unique formulation of the momentum conservation law is unfeasible, though a generalized expression of the ST and momentum density is achievable in terms of new concepts that we introduce, namely, the effective polarization and effective magnetization.
Matematická biologie: e-learningová učebnice [online].

Internetova ucebnice je tvořena souborem ucebnich textů klicových matematicky zaměřených předmětů ucebniho planu studijniho oboru Matematicka biologie programu Experimentalni biologie na Přirodovědecke fakultě MU.
A Prototype Modelling of Ebers for Video Transmission in Wireless Adhoc Network

Provisioning of video streaming over ad hoc wireless networks exhibits challenges associated with high packet loss rates and are delay sensitive. Excessive packet loss can cause significant degradation in quality of video perceived by users of real-time video applications. The recent studies suggest that Forward Error Correction (FEC) is a good technique for decreasing the negative impact of packet loss on video quality in error control scheme. This paper introduces an Estimation based Error Reduction Scheme(EBERS) to support video communication in ad hoc wireless networks. The EBERS considers a frame estimation parameter to support varied bandwidths and attain the delay requirements to support video communication. It is also responsible for improvising the QoS offered. The EBERS considers layered and embodies distortion limiting features owing to which reduced forward error correction is achieved, thus obtaining reduced frame errors, transmission errors and retransmission of frames. Thereby obtaining high degree of quality of service(QoS). The comparative study conducted proves the efficiency of the EBERS scheme over the existing mechanisms.
WARM DUST AROUND COOL STARS: FIELD M DWARFS WITH WISE 12 OR 22 μm EXCESS EMISSION

Using the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic catalog, we searched the WISE AllWISE catalog to investigate the occurrence of warm dust, as inferred from IR excesses, around field M dwarfs (dMs). We developed SDSS/WISE color selection criteria to identify 175 dMs (from 70,841) that show IR flux greater than the typical dM photosphere levels at 12 and/or 22 μm, including seven new stars within the Orion OB1 footprint. We characterize the dust populations inferred from each IR excess and investigate the possibility that these excesses could arise from ultracool binary companions by modeling combined spectral energy distributions. Our observed IR fluxes are greater than levels expected from ultracool companions (>3σ). We also estimate that the probability the observed IR excesses are due to chance alignments with extragalactic sources is <0.1%. Using SDSS spectra we measure surface gravity-dependent features (K, Na, and CaH 3) and find <15% of our sample indicates low surface gravities. Examining tracers of youth (Hα, UV fluxes, and Li absorption), we find <3% of our sample appear young, indicating we are observing a population of field stars ≳1 Gyr, likely harboring circumstellar material. We investigate age-dependent properties probed by this sample, studying the disk fraction as a function of Galactic height. The fraction remains small and constant to |Z| ∼ 700 pc and then drops, indicating little to no trend with age. Possible explanations for disks around field dMs include (1) collisions of planetary bodies, (2) tidal disruption of planetary bodies, or (3) failed planet formation.
THE CO-TO-H2 CONVERSION FACTOR FROM INFRARED DUST EMISSION ACROSS THE LOCAL GROUP

We estimate the conversion factor relating CO emission to H2 mass, αCO, in five Local Group galaxies that span approximately an order of magnitude in metallicity—M 31, M 33, the Large Magellanic Cloud (LMC), NGC 6822, and the Small Magellanic Cloud (SMC). We model the dust mass along the line of sight from infrared (IR) emission and then solve for the αCO that best allows a single gas-to-dust ratio (δGDR) to describe each system. This approach remains sensitive to CO-dark envelopes H2 surrounding molecular clouds. In M 31, M 33, and the LMC we find αCO ≈ 3–9 M☉ pc−2 (K km s−1)−1, consistent with the Milky Way value within the uncertainties. The two lowest metallicity galaxies in our sample, NGC 6822 and the SMC (12 + log (O/H) ≈ 8.2 and 8.0), exhibit a much higher αCO. Our best estimates are αNGC6822CO ≈ 30 M☉ pc−2 (K km s−1)−1 and αSMCCO ≈ 70 M☉ pc−2 (K km s−1)−1. These results are consistent with the conversion factor becoming a strong function of metallicity around 12 + log (O/H) ∼ 8.4–8.2. We favor an interpretation where decreased dust shielding leads to the dominance of CO-free envelopes around molecular clouds below this metallicity.
A DEEP CHANDRA X-RAY SPECTRUM OF THE ACCRETING YOUNG STAR TW HYDRAE

We present X-ray spectral analysis of the accreting young star TW Hydrae from a 489 ks observation using the Chandra High Energy Transmission Grating. The spectrum provides a rich set of diagnostics for electron temperature Te, electron density Ne, hydrogen column density NH, relative elemental abundances, and velocities, and reveals its source in three distinct regions of the stellar atmosphere: the stellar corona, the accretion shock, and a very large extended volume of warm postshock plasma. The presence of Mg xii, Si xiii, and Si xiv emission lines in the spectrum requires coronal structures at ∼10 MK. Lower temperature lines (e.g., from O viii, Ne ix, and Mg xi) formed at 2.5 MK appear more consistent with emission from an accretion shock. He-like Ne ix line ratio diagnostics indicate that Te = 2.50 ± 0.25 MK and Ne = 3.0 ± 0.2 × 1012 cm−3 in the shock. These values agree well with standard magnetic accretion models. However, the Chandra observations significantly diverge from current model predictions for the postshock plasma. This gas is expected to cool radiatively, producing O vii as it flows into an increasingly dense stellar atmosphere. Surprisingly, O vii indicates Ne = 5.7+4.4−1.2 × 1011 cm−3, 5 times lower than Ne in the accretion shock itself and ∼7 times lower than the model prediction. We estimate that the postshock region producing O vii has roughly 300 times larger volume and 30 times more emitting mass than the shock itself. Apparently, the shocked plasma heats the surrounding stellar atmosphere to soft X-ray emitting temperatures and supplies this material to nearby large magnetic structures—which may be closed magnetic loops or open magnetic field leading to mass outflow. Our model explains the soft X-ray excess found in many accreting systems as well as the failure to observe high Ne signatures in some stars. Such accretion-fed coronae may be ubiquitous in the atmospheres of accreting young stars.
Quantifying the User Experience: Practical Statistics for User Research

You're being asked to quantify usability improvements with statistics. But even with a background in statistics, you are hesitant to statistically analyze the data, as you may be unsure about which statistical tests to use and have trouble defending the use of the small test sample sizes associated with usability studies. The book is about providing a practical guide on how to use statistics to solve common quantitative problems arising in user research. It addresses common questions? you face every day? such as: Is the current product more usable than our competition? Can we be sure at least 70% of users can complete the task on the 1st attempt? How long will it take users to purchase products on the website? This book shows you which test to use, and how provide a foundation for both the statistical theory and best practices in applying them. The authors draw on decades of statistical literature from Human Factors, Industrial Engineering and Psychology, as well as their own published research to provide the best solutions. They provide both concrete solutions (excel formula, links to their own web-calculators) along with an engaging discussion about the statistical reasons for why the tests work, and how to effectively communicate the results. Provides practical guidance on solving usability testing problems with statistics for any project, including those using Six Sigma practices Show practitioners which test to use, why they work, best practices in application, along with easy-to-use excel formulas and web-calculators for analyzing data Recommends ways for practitioners to communicate results to stakeholders in plain English Table of Contents Dedication Acknowledgements About the Authors Chapter 1: Introduction and How to Use This Book Chapter 2: Quantifying User Research Chapter 3: How Precise Are Our Estimates? Confidence Intervals Chapter 4: Did We Meet or Exceed Our Goal? Chapter 5: Is There a Statistical Difference between Designs? Chapter 6: What Sample Sizes Do We Need? Part 1: Summative Studies Chapter 7: What Sample Sizes Do We Need? Part 2: Formative Studies Chapter 8: Standard Usability Questionnaires Chapter 9: Six Enduring Controversies in Measurement and Statistics Chapter 10: Wrapping Up Appendix Index
Wormholes and black universes without phantom fields in Einstein-Cartan theory

We obtain a family of regular static, spherically symmetric solutions in Einstein--Cartan theory with an electromagnetic field and a nonminimally coupled scalar field with the correct sign of kinetic energy density. At different values of its parameters, the solution, being asemptotically flat at large values of the radial coordinate, describes (i) twice asemptotically flat symmetric wormholes, (ii) asymmetric wormholes with an AdS asymptotic at the "far end", (iii) regular black holes with an extremal horizon or two simple horizons, and (iv) black universes with a de Sitter asymptotic at the "far end". As in other black universe models, it is a black hole as seen by a distant observer, but beyond its horizon there is a nonsingular expanding universe. In all these cases, both the metric and the torsion are regular in the whole space.
Galaxy formation in WMAP1 and WMAP7 cosmologies

Using the technique of Angulo & White (2010) we scale the Millennium and Millennium-II simulations of structure growth in aCDM universe from the cosmo- logical parameters with which they were carried out (based on first-year results from the Wilkinson Microwave Anisotropy Probe, WMAP1) to parameters consistent with the seven-year WMAP data (WMAP7). We implement semi-analytic galaxy formation modelling on both simulations in both cosmologies to investigate how the formation, evolution and clustering of galaxies are predicted to vary with cosmological parame- ters. The increased matter density m and decreased linear fluctuation amplitude σ8 in WMAP7 have compensating effects, so that the abundance and clustering of dark halos are predicted to be very similar to those in WMAP1 for z 6 3. As a result, local galaxy properties can be reproduced equally well in the two cosmologies by slightly altering galaxy formation parameters. The evolution of the galaxy populations is then also similar. In WMAP7, structure forms slightly later. This shifts the peak in cosmic star formation rate to lower redshift, resulting in slightly bluer galaxies at z = 0. Nev- ertheless, the model still predicts more passive low-mass galaxies than are observed. For rp 1 galaxies are predicted to be more strongly clustered for WMAP7. Differences in galaxy properties, including, clustering, in these two cosmologies are rather small out to z � 3. Given that there are still considerable residual uncertainties in galaxy formation models, it is very difficult to distinguish WMAP1 from WMAP7 through observations of galaxy properties or their evolution.
Superconductor-to-metal quantum phase transition in overdoped La 2-x Sr x CuO 4

We investigate $T_c$ and magnetic penetration depth $\lambda (T)$ near the superconductor-metal quantum phase transition in overdoped $La_{2-x}Sr_{x}CuO_{4}$ films. Both $T_c$ and superfluid density $n_s$, $\propto \lambda^{-2}$, decrease with overdoping. They obey the scaling relation $T_c \propto [\lambda^{-2}(0)]^{\alpha}$ with $\alpha \approx 1/2$. We discuss this result in the frameworks of disordered d-wave superconductors and of scaling near quantum critical points. Our result, and the linear scaling ($\alpha \approx 1$) found for the more anisotropic $Tl_2Ba_2CuO_{6+\delta}$, can both be understood in terms of quantum critical scaling, with different dimensionalities for fluctuations.
Water between Membranes

An accurate description of the structure and dynamics of interfacial water is essential for phospholipid membranes, since it determines their function and their interaction with other molecules. Here we consider water confined in stacked membranes with hydration from poor to complete, as observed in a number of biological systems. Experiments show that the dynamics of water slows down dramatically when the hydration level is reduced. All-atom molecular dynamics simulations identify three (inner, hydration and outer) regions, within a distance of approximately 1 nm from the membrane, where water molecules exhibit different degrees of slowing down in the dynamics. The slow-down is a consequence of the robustness of the hydrogen bonds between water and lipids and the long lifetime of the hydrogen bonds between water molecules near the membrane. The interaction with the interface, therefore, induces a structural change in the water that can be emphasized by calculating its intermediate range order. Surprisingly, at distances as far as ~ 2.5 nm from the interface, although the bulk-like dynamics is recovered, the intermediate range order of water is still slightly higher than that in the bulk at the same thermodynamic conditions. Therefore, the water-membrane interface has a structural effect at ambient conditions that propagates further than the often-invoked 1 nm length scale. Membrane fluctuations smear out this effect macroscopically, but an analysis performed by considering local distances and instantaneous configurations is able to reveal it, possibly contributing to our understanding of the role of water at biomembrane interfaces.
Construct Validation of the Concepts Social Presence, Emotional Presence and Connectedness

‘Social presence’ is a frequently used concept in Presence research. However, as several authors have noted, it is also a problematic concept. A literature review reveals that some of the recent discussion about the definition of ‘social presence’ deals with the distinction between ‘perceptual social presence’ (the perceptual awareness that you are not alone) and ‘connectedness’ (the emotional feeling that you are not alone, that you are in touch with someone). In an experiment we have tried to establish discriminant validation of the concepts (perceptual) social presence and connectedness and convergent validation of emotional presence and connectedness. The results support the view that perceptual awareness is a discriminant property of social presence. They partially support the similarity between connectedness and emotional presence. The experiment also explored the application of Zajonc’s theory of social facilitation as a triangulation of the notion that perceptual awareness is a prerequisite for experiencing social presence. The results give limited support for a mere presence effect.
RBFNN algorithm based on hybrid hierarchy genetic algorithm and its application

Based on the study of RBFNN (radial basis function neural network) training algorithm and genetic algorithm, a new RBFNN training algorithm-hybrid hierarchy genetic algorithm is introduced by combining hierarchy genetic algorithm and least_square method. The hybrid algorithm greatly increases the training speed while is still able to determine the structure and parameters of the RBFNN from sample data. The new training algorithm is used to identify and predict M_G chaos time series, and the simulation gives staisfied result.