Miracle-dz/UniFAR-FTUs huggingface dataset:
A Note on the Extremities of Local Moran's Iis and Their Impact on Global Moran's I

By defining local Moran's Iias a ratio of quadratic forms and making use of its overall additivity to match global Moran's I, we can identify spatial objects with a strong impact on global Moran's I. First, we concentrate on the spatial properties of local Moran's Iiexpressed by the local linkage degree. Depending on whether we use the W- or C-coding of the spatial connectivity matrix, the variance of local Moran's Iifor a small local linkage degree will be either large or small. Note that spatial objects associated with a local Moran's Iiwith a large variance affect the global statistic much more than spatial objects associated with a local Moran's Iiwith a small variance. Counterintuitively, global Moran's I defined in the W-coding is most influenced by spatial objects with a small number of spatial neighbors. In contrast, spatial objects with a large number of spatial neighbors exert more impact on global Moran's I setup in the C-coding. Second, we investigate the impact of the empirical data on local Moran's Iiand show that local Moran's Iiwill only be significant for extreme absolute residuals at and around the reference location. Clusters of average regression residuals cannot be detected by local Moran's Ii. Consequently, spatial cliques of extreme residuals contribute more to significance tests on global autocorrelation.
The Nature of Bilateral Supernova Remnants

We present high-resolution radio images at 1.4 GHz of two Galactic supernova remnants (SNRs), G003.8-00.3 (formerly G003.7-00.2) and G350.0-02.0 (formerly G350.0-01.8). Although the two objects are very different in appearance, in both cases the radio emission shows a clear bilateral (or "barrel") morphology for which the axis is parallel to the Galactic plane. The majority of Galactic SNRs have now been observed at high resolution, and one can define a clear bilateral subset of the population. We consider a sample of 17 such SNRs and find a highly significant tendency for the bilateral axes of these SNRs to be aligned with the Galactic plane. We interpret this as indicating that "extrinsic" effects dominate the morphology of such remnants. Specifically, we argue that the Galactic magnetic field causes these SNRs to appear bilateral, either directly, in the form of magnetic field compression and/or quasi-perpendicular acceleration of electrons in the supernova shock, or more likely indirectly, by preprocessing the interstellar medium to produce density stratifications extended along the plane.
The Martian ionosphere in light of the Viking observations

A theoretical model has been constructed in which the ion density and the ion and electron temperature distributions are calculated by solving the coupled continuity-momentum equations and the coupled energy equations. The latest experimental results from the Viking 1 and 2 landers are used to vary some of the parameters in the model in order to obtain agreement between the theoretical and experimental results. It is found that solar EUV radiation alone is not able to maintain the observed high ion temperatures. It was also established that the energy coupling between the electron and ion gas is insufficient to account for the measured ion temperatures even in the presence of very large electron temperatures. Direct heat input to the ion gas, probably due to solar wind-ionosphere interactions, can result in ion temperature values in reasonable agreement with the observations. The ion densities calculated with the present model agree well with the Viking observations in the chemically controlled region, but at higher altitudes, dynamic transport processes need to be invoked to achieve consistency among the observed and calculated temperature and density values.
Positive solutions for a coupled system of nonlinear fractional differential equations

Using the Krasnoselskii–Zabreiko fixed point theorem, we establish two existence theorems for positive solutions of a coupled system of nonlinear fractional differential equations. Power functions and nonnegative matrices are used to characterize coupling behavior of our nonlinearities, so nonlinearities may grow differently; in fact, one may grow superlinearly, and the other may grow sublinearly. Copyright © 2014 John Wiley & Sons, Ltd.
Spectra of transitions within the second shell belonging to elements between argon and vanadium

Spectra emitted from plasmas produced through focusing the output of a 4-GW neodymium-glass laser onto plane solid targets of potassium, calcium, scandium, titanium, and vanadium were recorded with a 2-m grazing incidence spectrograph as were argon spectra emitted from a theta-pinch plasma. The analysis of the spectrograms yielded line classifications for the 2s2 2pn-2s2pn+ 1 and 2s 2pn+ 1-2pn+ 2 transition arrays. Identifications include those of beryllium i-like 2s 2p-2p2 spectra. The data is used to complete the tabulation of energy-level values for the 2s2 2pn, 2s 2pn+ 1, and 2pn+ 2 configurations of these elements.
Envelope‐Function Equation and Motion of Wave Packet in a Semiconductor Superlattice Structure

We present a new description of envelope‐function equation of the superlattice (SL). The SL wave function and corresponding effective‐mass equation are formulated in terms of a linear combination of Bloch states of the constituent material with smaller band gap. In this envelope‐function formalism, we review the fundamental concept on the motion of a wave packet in the SL structure subjected to steady and uniform electric fields F. The review confirms that the average of SL crystal momentums K = (kx, ky, q), where (kx, ky) are bulk inplane wave vectors and q SL wave vector, included in a wave packet satisfies the equation of motion 〈K〉 = 〈K〉0 + Ft/ħ; and that the velocity and acceleration theorems provide the same type of group velocity and definition of the effective mass tensor, respectively, as in the Bulk. Finally, Schlosser and Marcus's method for the band theory of metals has been used by Altarelli to include the interface‐matching condition in the variational calculation for the SL structure in the multi‐band envelope‐function approximation. We re‐examine this procedure more thoroughly and present variational equations in both general and reduced forms for SLs, which agrees in form with the proposed envelope‐function formalism. As an illustration of the application of the present work and also for a brief investigation of effects of band‐parameter difference on the subband energy structure, we calculate by the proposed variational method energies of non‐strained GaAs/Al0.32Ga0. 68As and strained In0.63Ga0. 37As/In0.73Ga0. 27As0.58P0. 42SLs with well/barrier widths of 60 Å/500 Å and 30 Å/30 Å, respectively.
An approach to remove impulse noise from a corrupted image

In this paper, we propose an efficient approach for detecting the impulse noise from corrupted images. This method is based on the principle that the feature of the digital image is usually local correlation and the feature of the impulse noise is usually located near one of the two ends of the image’s maximum and minimum gray values. After the noisy pixel has been detected by the proposed detector, a modified version of the mean filter is proposed to remove the detected impulse noise. Experimental results show that the implementation of the proposed method is simple, and it has better performance than comparison filters with regard to effective noise suppression and preservation of detail, especially when the noise ratio is very high.
Hybrid method (JM-ECS) combining the J-matrix and exterior complex scaling methods for scattering calculations

The paper proposes a hybrid method for calculating scattering processes. It combines the J-matrix method with exterior complex scaling and an absorbing boundary condition. The wave function is represented as a finite sum of oscillator eigenstates in the inner region, and it is discretized on a grid in the outer region. The method is validated for a one- and a two-dimensional model with partial wave equations and a calculation of p-shell nuclear scattering with semirealistic interactions.
RADIAL DISTRIBUTION AND TOTAL NUMBER OF GLOBULAR CLUSTERS IN M104.

Stellar images around M 104 fainter than a threshold magnitude are concentrated toward the nucleus, thus they are certainly globular clusters associated with M 104. By counting their images, the radial distribution of their projected number density is found to be similar to the luminosity profile of the spheroidal central bulge and can be represented by de Vaucouleurs' "1/4-law". The total number of globular clusters in M 104 is estimated to be (2.0+ i: o) x 10 . Key words: globular clusters- spiral galaxies- spheroidal central bulge
Development of scanning x-ray fluorescence microscope with spatial resolution of 30 nm using Kirkpatrick-Baez mirror optics

We developed a high-spatial-resolution scanning x-ray fluorescence microscope (SXFM) using Kirkpatrick-Baez mirrors. As a result of two-dimensional focusing tests at BL29XUL of SPring-8, the full width at half maximum of the focused beam was achieved to be 50×30nm2 (V×H) under the best focusing conditions. The measured beam profiles were in good agreement with simulated results. Moreover, beam size was controllable within the wide range of 30–1400nm by changing the virtual source size, although photon flux and size were in a trade-off relationship. To demonstrate SXFM performance, a fine test chart fabricated using focused ion beam system was observed to determine the best spatial resolution. The element distribution inside a logo mark of SPring-8 in the test chart, which has a minimum linewidth of approximately 50–60nm, was visualized with a spatial resolution better than 30nm using the smallest focused x-ray beam.
Near-infrared broad-line profiles in low-redshift QSOs

Near-infrared and optical spectrophotometry of six low-redshift QSOs are presented. The integrated Paα/Hα ratios cluster near the value 0.1, with one exception having a larger ratio consistent with other evidence of reddening. At least two of the Paα/Hα profile ratios decrease with observed velocity. We discuss some implications for the dynamics of the broad-line region and this ratio's usefulness as a reddening indicator. A spectrum of the He I λ10830, Paγ blend of 1226+023 is also presented
On the Reinhardt-Mahler theorem

1. Let A1, * , An be n linearly independent points in Rn, the n-dimensional Euclidean space. The set A= u= Ai+ * * * +unAn Ul, ** *, Un integers} is called a lattice, and {A1, * * *, AI is called a base of A. Let A i have co-ordinates ali, . *, ani. Then d(A) = I det(ai,) j is called the determinant of the lattice A; it is independent of the choice of a base of A. Let S be a set in Rn. A lattice A is said to be S-admissible if A has no point other than the origin 0 in the interior of S. The critical determinant A(S) of S is defined by A(S) -inf d(A), where A runs over all S-admissible lattices (A(S) = oo if S has no admissible lattice). Clearly, SC T implies A(S) ? A(T). One of the principal problems in Geometry of Numbers is to find a method for determining A(S) for a given set S. For twoand threedimensional symmetrical' convex bodies, Minkowski reduced the problem to the discussion of special classes of lattices with points on the boundary of the body. This method has been partially extended to symmetrical convex bodies in R4, but it is very difficult to apply in spaces of dimension higher than two. Reinhardt [7] and Mahler [4] independently proved that for a symmetrical convex domain K in R2, A(K) =H(K)/4, where H(K) denotes the area of a smallest symmetrical "hexagon"2 containing K. In other words, a symmetrical convex domain can be inscribed in a space-filling symmetrical convex domain with the same critical determinant. The straightforward generalization of this result to higher dimensions would be: If K is a symmetrical convex body in Rn then K is contained in a space-filling symmetrical convex body (P with A(K) =A((P) =V(6)/2n, where V(Q? ) denotes the volume of (P. The object of this note is to prove that this generalization does not hold in R,, for n _ 3.
Mid-Infrared Images of the Debris Disk around HD 141569

We have imaged the circumstellar debris disk around the A0 Ve/B9.5 Ve star HD 141569 (D = 99 pc), at λ = 12.5, 17.9, and 20.8 μm using the Keck II telescope, and confirm the general morphology from other recently published mid-infrared observations. Model fits to an assumed flat radially symmetric dust disk yield an inclination i = 53° ± 5° and a position angle of -6° ± 4° for the tilt axis and indicate the presence of a depression in optical depth by a factor of about 4 within a radial distance of 30 AU (0.″3) from the star. Such a depression is suggestive of a density depletion and is consistent with published spectral energy distributions that indicate the absence of a near-infrared excess even though a mid-infrared excess is present. Our mid-infrared results, in conjunction with previously published near-infrared scattering images, suggest that the two wavelength regimes are viewing, respectively, the inner and outer parts of a common disk structure, which is dominated by small (probably submicron) grains throughout.
A 6 second periodic X-ray source in Carina

A serendipitous source, 1E 1048.1-5937, was discovered during Einstein imaging observations of the Carina nebula. On July 13, 1979, this source had an intensity of 0.14 IPC counts/s, and the signal was 65 percent pulsed with a period of 6.44 s. An earlier observation failed to detect any source with strength greater than 1/10 the above signal. The source is therefore highly variable, perhaps transient. An Exosat observation of this source on June 20, 1985 confirmed the pulse period and refined the source position to an accuracy of 10 arcsec. On the basis of the position, the source is tentatively identified with a V = 19 optical counterpart. The X-ray spectrum is best fitted by a power law with photon index = 2.26 and a column density of 1.6 x 10 to the 22nd atoms/sq cm. The X-ray characteristics are consistent with an accretion-powered Be star binary. 8 references.
A search for X-ray counterparts to small-diameter Galactic radio sources

By comparing observations obtained with the Einstein Observatory to the Molonglo catalog of small-diameter radio sources near the Galactic plane, the number of supernova remnants contained in the radio sample has been constrained. The one known remnant among the 47 sources falling in Einstein fields was easily detected and another candidate remnant (G274.7-2.8) was discovered. The latter object has properties consistent with that of either a young shell-like or composite remnant, although an identification as a radio-loud quasar cannot be excluded. Apart from cases in which very large absorbing column densities are appropriate, upper limits to the X-ray emission from the remainder of the sample places most of the objects outside of the ranges of parameters that characterize the Galactic remnant population. 18 refs.
Underspecification in Phonetics

It is often assumed in work on the phonological underspecification of segments that while representations may at first be underspecified, they end up fully specified. Various kinds of rules are posited to ensure that in output forms all features have values for all segments. In this paper I will consider an alternative view: that underspecification may persist into phonetic representations. I begin by reviewing some of the relevant phonological phenomena and mechanisms, and some of the history of underspecification in phonetic studies. I then show how phonetic data may be taken to reflect the presence or absence of feature values in surface forms. Finally, the extent to which surface specification depends on segmental contrasts is examined. The aim of this paper is to present some phonetic phenomena that are potentially relevant to any theory of underspecification.
The Banach space $JT$ is primary.

1. In this paper we prove that the James' tree space, JT, is primary. A Banach space X is primary if whenever X = Y © Z, either Y or Z is itself isomorphic to X. Many of the classical Banach spaces are known to be primary [1], [2], [3], [4], [5], [9], [10], [13]. The space JT was constructed by R. C. James [8] as an example of a separable space not containing /, yet having non-separable dual. It has also been studied by Lindenstrauss and Stegall [11]. Every subspace of JT contains l2 [8], and JT has many subspaces isometric to the quasireflexive Banach space / [6], [7]. Here we take the norm on / to be
An illumination and affine invariant descriptor for aerial image registration

An illumination and affine invariant descriptor is proposed for registering aerial images with large illumination changes and affine transformation, low overlapping areas, monotonous backgrounds or similar features. Firstly, triangle region is detected by K-nearest neighbors (K-NN) graph of initial matched result by Scale-Invariant Feature Transform (SIFT). In order to improve the accuracy, region growth is applied to boost small and slender triangles. Then illumination and affine invariant descriptor is defined to describe triangle regions and measure their similarity. The descriptor named as IIMSA is the combination of MultiScale Autoconvolution (MSA) and multiscale retinex (MSR). The performance of the descriptor is evaluated with optical aerial images and the experimental results demonstrate that the proposed descriptor IIMSA is more distinctive than MSA and SIFT.
Remote optical detection using microcantilevers

The feasibility of microcantilever‐based optical detection is demonstrated. Microcantilevers may provide a simple means for developing single‐element and multielement infrared sensors that are smaller, more sensitive, and lower in cost than quantum well, thermoelectric, or bolometric sensors. Here we specifically report here on an evaluation of laboratory prototypes that are based on commercially available microcantilevers, such as those used in atomic force microscopy. In this work, optical transduction techniques were used to measure microcantilever response to remote sources of thermal energy. The noise equivalent power at 20 Hz for room temperature microcantilevers was found to be approximately 3.5 nW/√Hz, with a specific detectivity of 3.6×107 cm Hz1/2/W, when an uncoated microcantilever was irradiated by a low‐power diode laser operating at 786 nm. Operation is shown to be possible from dc to kHz frequencies, and the effect of cantilever shape and the role of absorptive coatings are discussed. Finally, spectral response in the midinfrared is evaluated using both coated and uncoated microcantilevers.
Turbulent boundary-layer flow over fixed aerodynamically rough two-dimensional sinusoidal waves

Results from a wind tunnel study of aerodynamically rough turbulent boundary-layer flow over a sinusoidal surface are presented. The waves had a maximum slope (ak) of 0.5 and two surface roughnesses were used. For the relatively rough surface the flow separated in the wave troughs while for the relatively smooth surface it generally remained attached. Over the relatively smooth-surfaced waves an organized secondary flow developed, consisting of vortex pairs of a scale comparable to the boundary-layer depth and aligned with the mean flow. Large-eddy simulation studies model the flows well and provide supporting evidence for the existence of this secondary flow.
Variational transition-state theory for reaction rates in dissipative systems.

Variational upper bounds are derived for the escape rate of a particle trapped in a metastable well and interacting with a dissipative medium. The theory leads to a reduced two-degrees-of-freedom Hamiltonian involving the unstable normal mode and a newly defined collective bath mode. Explicit treatment of strong nonlinearities or low-barrier systems presents no special problem
Neutral hydrogen absorption observations of the central region of NGC 5929

We present 0.15-arcsec (25-pc) resolution MERLIN observations of neutral hydrogen absorption detected towards the nuclear region of the type 2 Seyfert galaxy NGC 5929. Absorption is detected only towards the north-eastern radio component with a column density of (6.5 ± 0.6) × 1021 cm−2. Based on comparison with an HST WFPC2 continuum image, we propose that the absorption is caused by a 1.5-arcsec structure of neutral gas and dust offset 0.3 arcsec south-east of the nucleus and running NE–SW. A separate cloud of dust is apparent 1.5 arcsec to the south-west of the nucleus in the HST image. A comparison of the centroid velocity (2358 ± 5 km s−1) and full width at half-maximum (43 ± 6 km s−1) of the absorbing gas with previous [O III] observations suggests that both the neutral and ionized gas are undergoing galactic rotation towards the observer in the north-east and away from the observer in the south-west. The main structure is consistent with an inclined ring of gas and dust encircling the active galactic nucleus (AGN); alternatively it may be a bar or inner spiral arm. We do not detect neutral hydrogen absorption or dust obscuration against the radio nucleus (column density < 3.1 × 1021 cm−2) expected by a torus of neutral gas and dust in unified models of AGNs for a type 2 Seyfert galaxy.
Scientific potential of ground layer adaptive optics on large telescopes

Ground-layer Adaptive Optics offers a unique approach to enhancing the power of large telescopes to explore a wide range of astrophysical phenomena. By accessing wide fields of view with image concentrations that are significantly improved over natural seeing, ground-layer AO systems can probe stellar populations in crowded and confused regions of the Milky Way and nearby galaxies, probe the internal dynamics of large samples of galaxies in the distant universe and provide a cost effective path towards highly multiplexed observations of large samples. The improved image concentration over large fields of view offered by ground-layer AO will allow significant gains in sensitivity for multiobject spectrographs operating in the near-IR. This will lead to improved understanding of the formation of the first galaxies and stars as well as the evolution of massive galaxies when the Universe was a few billion years old. Groundlayer AO systems have the potential to eliminate poor seeing from most astronomical sites and to improve the productivity of large and extremely large telescopes.