Miracle-dz/UniFAR-FTUs huggingface dataset:
A Method of Semantic Web Service Discovery Based on Bipartite Graph Matching

How to discover services for users efficiently is the key for the application of the Web service technology. The current semantic-based service discovery methods are of great inconvenience to be used and have much potential improvement for their performance. This paper proposes an information model of registered services that isn′t limited to specific service models and languages and supports semantic-annotation and interface-dependency declaration. Then, a method of service discovery based on bipartite graph matching is proposed that translates the service matchmaking to the problem of extended optimal matching for bipartite graph. It enhances the recall rate and precision as it considers the interface dependency relations within a service in matchmaking. A serial of experiments illustrate the method not only improves its efficiency much, but also has a linear complexity in time consumption to fulfill users′ requests.
EVIDENCE FOR COLD ACCRETION: PRIMITIVE GAS FLOWING ONTO A GALAXY AT z ∼ 0.274

We present UV and optical observations from the Cosmic Origins Spectrograph on the Hubble Space Telescope and Keck of a z = 0.27395 Lyman limit system (LLS) seen in absorption against the QSO PG1630+377. We detect H i absorption with log N(H i) = 17.06 ± 0.05 as well as Mg ii, C iii, Si iii, and O vi in this system. The column densities are readily explained if this is a multi-phase system, with the intermediate and low ions arising in a very low metallicity ([Mg/H] = −1.71 ± 0.06) photoionized gas. We identify via Keck spectroscopy and Large Binocular Telescope imaging a 0.3 L* star-forming galaxy projected 37 kpc from the QSO at nearly identical redshift (z = 0.27406 and Δv = −26 km s−1) with near solar metallicity ([O/H] = −0.20 ± 0.15). The presence of very low metallicity gas in the proximity of a near-solar metallicity, sub-L* galaxy strongly suggests that the LLS probes gas infalling onto the galaxy. A search of the literature reveals that such low-metallicity LLSs are not uncommon. We found that 50% (4/8) of the well-studied z ≲ 1 LLSs have metallicities similar to the present system and show sub-L* galaxies with ρ < 100 kpc in those fields where redshifts have been surveyed. We argue that the properties of these primitive LLSs and their host galaxies are consistent with those of cold mode accretion streams seen in galaxy simulations.
Relative velocity of dark matter and baryons in clusters of galaxies and measurements of their peculiar velocities

The increasing sensitivity of current experiments, which nowadays routinely measure the thermal SZ effect within galaxy clusters, provide the hope that peculiar velocities of individual clusters of galaxies will be measured rather soon using the kinematic SZ effect. Also next generation of X-ray telescopes with microcalorimeters, promise first detections of the motion of the intra cluster medium (ICM) within clusters. We used a large set of cosmological, hydrodynamical simulations, which cover very large cosmological volume, hosting a large number of rich clusters of galaxies, as well as moderate volumes where the internal structures of individual galaxy clusters can be resolved with very high resolution to investigate, how the presence of baryons and their associated physical processes like cooling and star-formation are affecting the systematic difference between mass averaged velocities of dark matter and the ICM inside a cluster. We, for the first time, quantify the peculiar motion of galaxy clusters as function of the large scale environment. We also demonstrate that especially in very massive systems, the relative velocity of the ICM compared to the cluster peculiar velocity add significant scatter onto the inferred peculiar velocity, especially when measurements are limited to the central regions of the cluster. Depending on the aperture used, this scatter varies between 50% and 20%, when going from the core (e.g. ten percent of the virial radius) to the full cluster (e.g. the virial radius).
A Brief Review of Galactic Winds

Galactic winds from star-forming galaxies play at key role in the evolution of galaxies and the inter-galactic medium. They transport metals out of galaxies, chemically-enriching the inter-galactic medium and modifying the chemical evolution of galaxies. They affect the surrounding inter-stellar and circum-galactic media, thereby inﬂuencing the growth of galaxies through gas accretion and star-formation. In this contribution we ﬁrst summarize the physical mechanisms by which the momentum and energy output from a population of massive stars and associated supernovae can drive galactic winds. We use the proto-typical example of M82 to illustrate the multiphase nature of galactic winds. We then describe how the basic properties of galactic winds are derived from the data, and summarize how the properties of galactic winds vary systematically with the properties of the galaxies that launch them. We conclude with a brief discussion of the broad implications of galactic winds.
Autler-Townes splitting in a three-dimensional transmon superconducting qubit

We have observed the Autler-Townes doublet in a superconducting Al/AlOx/Al transmon qubit that acts as an artificial atom embedded in a three-dimensional Cu microwave cavity at a temperature of 22 mK. Using pulsed microwave spectroscopy, the three lowest transmon levels are isolated, eliminating unwanted effects of higher qubit modes and cavity modes. The long coherence time (~40 us) of the transmon enables us to observe a clear Autler-Townes splitting at drive amplitudes much smaller than the transmon level anharmonicity (177 MHz). Three-level density matrix simulations with no free parameters provide excellent fits to the data. At maximum separation, the fidelity of a dark state achieved in this experiment is estimated to be 99.6-99.9%.
The Suzaku Discovery of A Hard Power-Law Component in the Spectra of Short Bursts from SGR 0501+4516

Using data with the Suzaku XIS and HXD, spectral studies of short bursts from the soft gamma repeater SGR 0501+4516 were performed. In total, 32 bursts were detected during the ~60 ks of observation conducted in the 2008 August activity. Excluding the strongest one, the remaining 31 bursts showed an average 2--40 keV fluence of 1.0(-0.5,+0.3)*10^-9 erg cm^-2. A 1--40 keV spectrum summed over them leaves significant positive residuals in the HXD-PIN band with chi^2/d.o. f. = 74/50, when fitted with a two-blackbody function. By adding a power law model, the fit became acceptable with chi^2/d.o. f. = 56/48, yielding a photon index of Gamma=1.0(-0.3,+0.4). This photon index is comparable to Gamma=1.33(-0.16,+0.23) (Enoto et al. 2010a) for the persistent emission of the same object obtained with Suzaku. The two-blackbody components showed very similar ratios, both in the temperature and the emission radii, to those comprising the persistent emission. However, the power-law to two-blackbody flux ratio was possibly higher than that of the persistent emission at 2.6 sigma level. Based on these measurements, average wide-band properties of these relatively weak bursts are compared with those of the persistent emission.
INFRARED DIAGNOSTICS FOR THE EXTENDED 12 μm SAMPLE OF SEYFERTS

We present an analysis of Spitzer IRS spectroscopy of 83 active galaxies from the extended 12 μm sample. We find rank correlations between several tracers of star formation which suggest that (1) the polycyclic aromatic hydrocarbon feature is a reliable tracer of star formation, (2) there is a significant contribution to the heating of the cool dust by stars, and (3) the H2 emission is also primarily excited by star formation. The 55–90 versus 20–30 spectral index plot is also a diagnostic of the relative contribution of starburst to active galactic nuclei (AGNs). We see there is a large change in spectral index across the sample: Δα ∼ 3 for both indices. Thus, the contribution to the IR spectrum from the AGN and starburst components can be comparable in magnitude but the relative contribution also varies widely across the sample. We find rank correlations between several AGN tracers. We find correlations of the ratios [O iii]λ5007/[O iv] 26 μm and [O iii]λ5007/[Ne v] 14 μm with the silicate strength which we adopt as an orientation indicator. This suggests that some of the [O iii]λ5007 emission in these Seyferts is subject to orientation dependent obscuration as found by Haas et al. for radio galaxies and quasars. There is no correlation of [Ne v] equivalent width with the silicate 10 μm strength, indicating that the [Ne v] emission is not strongly orientation dependent. This suggests that the obscuring material (e.g., torus) is not very optically thick at 14 μm consistent with the results of Buchanan et al. We search for correlations between AGN and starburst tracers and we conclude that the AGN and starburst tracers are not correlated. This is consistent with our conclusion that the relative strength of the AGN and starburst components varies widely across the sample. Thus, there is no simple link between AGN fueling and black hole growth and star formation in these galaxies. The density diagnostic [Ne v] 14/24 μm and [S iii] 18/33 μm line ratios are consistent with the gas being near the low density limit, i.e., ∼103 cm−3 for [Ne v] and ne∼ few hundred cm−3 for [S iii]. The distribution of silicate 10 μm and 18 μm strengths is consistent with the clumpy torus models of Sirocky et al. We find a rank correlation between the [Ne v] 14 μm line and the 6.7 μm continuum which may be due to an extended component of hot dust. The Sy 2's with a hidden broad-line region (HBLR) have a higher ratio of AGN-to-starburst contribution to the spectral energy distribution than Sy 2's without an HBLR. This may contribute to the detection of the HBLR in polarized light. The Sy 2's with an HBLR are more similar to the Sy 1's than they are to the Sy 2's without an HBLR.
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM

Based on a suite of state-of-the-art high-resolution N-body simulations, we revisit the so-called halofit model as an accurate fitting formula for the nonlinear matter power spectrum. While the halofit model has frequently been used as a standard cosmological tool to predict the nonlinear matter power spectrum in a universe dominated by cold dark matter, its precision has been limited by the low resolution of N-body simulations used to determine the fitting parameters, suggesting the necessity of an improved fitting formula at small scales for future cosmological studies. We run high-resolution N-body simulations for 16 cosmological models around the Wilkinson Microwave Anisotropy Probe best-fit cosmological parameters (one-, three-, five-, and seven-year results), including dark energy models with a constant equation of state. The simulation results are used to re-calibrate the fitting parameters of the halofit model so as to reproduce small-scale power spectra of the N-body simulations, while keeping the precision at large scales. The revised fitting formula provides an accurate prediction of the nonlinear matter power spectrum in a wide range of wavenumbers (k ⩽ 30 h Mpc−1) at redshifts 0 ⩽ z ⩽ 10, with 5% precision for k ⩽ 1 h Mpc−1 at 0 ⩽ z ⩽ 10 and 10% for 1 ⩽ k ⩽ 10 h Mpc−1 at 0 ⩽ z ⩽ 3. We discuss the impact of the improved halofit model on weak-lensing power spectra and correlation functions, and show that the improved model better reproduces ray-tracing simulation results.
Exact distribution for work and stochastic efficiency of an isothermal machine

We consider an isothermal machine composed of two Brownian particles (say particle A and B) connected by a harmonic spring. A constant load is attached to particle A, and the particle B is trapped in a harmonic confinement whose minimum is dragged with a constant velocity. We obtain the distribution for work done on particle A and particle B. The transient fluctuation theorem for these quantities is tested in the weak coupling limit for both small and large observation times. Moreover, we show that the transient fluctuation theorem for the total work done on both particles is satisfied. Furthermore, we compute the stochastic efficiency which is the ratio of the work done against the load force on particle A and the work done on particle B of this machine. The probability density function for stochastic efficiency is computed for all time. Numerical simulations are also done to verify the analytical results.
X-RAY OBSERVATIONS OF XSS J12270–4859 IN A NEW LOW STATE: A TRANSFORMATION TO A DISK-FREE ROTATION-POWERED PULSAR BINARY

We present XMM-Newton and Chandra observations of the low-mass X-ray binary XSS J12270–4859, which experienced a dramatic decline in optical/X-ray brightness at the end of 2012, indicative of the disappearance of its accretion disk. In this new state, the system exhibits previously absent orbital-phase-dependent, large-amplitude X-ray modulations with a decline in flux at superior conjunction. The X-ray emission remains predominantly non-thermal but with an order of magnitude lower mean luminosity and significantly harder spectrum relative to the previous high flux state. This phenomenology is identical to the behavior of the radio millisecond pulsar (MSP) binary PSR J1023+0038 in the absence of an accretion disk, where the X-ray emission is produced in an intra-binary shock driven by the pulsar wind. This further demonstrates that XSS J12270–4859 no longer has an accretion disk and has transformed to a full-fledged eclipsing “redback” system that hosts an active rotation-powered MSP. There is no evidence for diffuse X-ray emission associated with the binary that may arise due to outflows or a wind nebula. An extended source situated 1. ′5 from XSS J12270–4859 is unlikely to be associated, and is probably a previously uncataloged galaxy cluster.
SatCNN: satellite image dataset classification using agile convolutional neural networks

ABSTRACT With the launch of various remote-sensing satellites, more and more high-spatial resolution remote-sensing (HSR-RS) images are becoming available. Scene classification of such a huge volume of HSR-RS images is a big challenge for the efficiency of the feature learning and model training. The deep convolutional neural network (CNN), a typical deep learning model, is an efficient end-to-end deep hierarchical feature learning model that can capture the intrinsic features of input HSR-RS images. However, most published CNN architectures are borrowed from natural scene classification with thousands of training samples, and they are not designed for HSR-RS images. In this paper, we propose an agile CNN architecture, named as SatCNN, for HSR-RS image scene classification. Based on recent improvements to modern CNN architectures, we use more efficient convolutional layers with smaller kernels to build an effective CNN architecture. Experiments on SAT data sets confirmed that SatCNN can quickly and effectively learn robust features to handle the intra-class diversity even with small convolutional kernels, and the deeper convolutional layers allow spontaneous modelling of the relative spatial relationships. With the help of fast graphics processing unit acceleration, SatCNN can be trained within about 40 min, achieving overall accuracies of 99.65% and 99.54%, which is the state-of-the-art for SAT data sets.
Image Inpainting Technology Based on Image Decomposition

Aiming at the drawbacks of Total Variation(TV) model for image impainting,this paper proposes an improved inpainting model based on image decomposition.Using image decomposition technology,it extracts the structure information and texture information from the image.The improved TV model is applied to structure part of image to effectively avoid step effect in TV model on smooth region.On the process of iterative,it respectively analyzes the feature points and non-feature points to avoid the fuzziness of feature points during the inpainting.Image texture information uses improved exemplar-based inpainting technology.Matlab simulation experimental results show that the inpainting effect and the results of peak signal to noise ratio are better than that of original algorithm.
Atomic and Molecular Aspects of Astronomical Spectra

In the first section we present the atomic part where a C2+ atomic target was prepared and used to generate theoretical data to investigate recombination lines arising from electron-ion collisions in thin plasma. R-matrix method was used to describe the C2+ plus electron system. Theoretical data concerning bound and autoionizing states were generated in the intermediate-coupling approximation. The data were used to generate dielectronic recombination data for C+ which include transition lines, oscillator strengths, radiative transition probabilities, emissivities and dielectronic recombination coefficients. The data were cast in a line list containing 6187 optically-allowed transitions which include many C II lines observed in astronomical spectra. This line list was used to analyze the spectra from a number of astronomical objects, mainly planetary nebulae, and identify their electron temperature. The electron temperature investigation was also extended to include free electron energy analysis to investigate the long-standing problem of discrepancy between the results of recombination and forbidden lines analysis and its possible connection to the electron distribution. In the second section we present the results of our molecular investigation; the generation of a comprehensive, calculated line list of frequencies and transition probabilities for H2D+. The line list contains over 22 million rotational-vibrational transitions occurring between more than 33 thousand energy levels and covers frequencies up to 18500 cm-1. About 15% of these levels are fully assigned with approximate rotational and vibrational quantum numbers. A temperature-dependent partition function and cooling function are presented. Temperature-dependent synthetic spectra for the temperatures T=100, 500, 1000 and 2000 K in the frequency range 0-10000 cm-1 were also generated and presented graphically.
QUIC: A UDP-Based Secure and Reliable Transport for HTTP/2

QUIC (Quick UDP Internet Connection) is a new multiplexed and secure transport atop UDP, designed from the ground up and optimized for HTTP/2 semantics. While built with HTTP/2 as the primary application protocol, QUIC builds on decades of transport and security experience, and implements mechanisms that make it attractive as a modern general- purpose transport. QUIC provides multiplexing and flow control equivalent to HTTP/2, security equivalent to TLS, and connection semantics, reliability, and congestion control equivalent to TCP. This draft documents the early deployment of the QUIC protocol prior to standardization.
A study of faculty racial diversity in business schools: Perceptions of business deans

ABSTRACT For decades, business schools in the United States have attempted to increase faculty diversity. The goals and benefits of increasing faculty diversity include improved educational outcomes, social justice, and economic competitiveness. While Association to Advance Collegiate Schools of Business data shows that a gender gap still exists in business schools, it is not as wide as the racial gap. The authors examined whether business deans view various minority groups as underrepresented and what they think are the primary reasons for underrepresentation.
Observation of tunable band gap and anisotropic Dirac semimetal state in black phosphorus

Tuning the band gap of black phosphorus Most materials used in electronics are semiconductors. The sizable energy gap in their electronic structure makes it easy to turn the conduction of electricity on and off. Graphene naturally lacks this band gap unless it undergoes certain modifications. Kim et al. studied the electronic structure of black phosphorus—a related two-dimensional material. By sprinkling potassium atoms on top of single layers of black phosphorus, the material changed from being a semiconductor to having a gapless linear dispersion similar to that of graphene. Science, this issue p. 723 Surface doping with potassium is used to tune black phosphorus from a semiconducting to a graphene-like electronic structure. Black phosphorus consists of stacked layers of phosphorene, a two-dimensional semiconductor with promising device characteristics. We report the realization of a widely tunable band gap in few-layer black phosphorus doped with potassium using an in situ surface doping technique. Through band structure measurements and calculations, we demonstrate that a vertical electric field from dopants modulates the band gap, owing to the giant Stark effect, and tunes the material from a moderate-gap semiconductor to a band-inverted semimetal. At the critical field of this band inversion, the material becomes a Dirac semimetal with anisotropic dispersion, linear in armchair and quadratic in zigzag directions. The tunable band structure of black phosphorus may allow great flexibility in design and optimization of electronic and optoelectronic devices.
Assigning the newly reported 
Σb(6097)
 as a 
P
-wave excited state and predicting its partners

The newly observed $\Sigma_b(6097)$ provides us a good chance to further construct the high excited states of the bottom baryon family. In this work, we explain the $\Sigma_b(6097)$ to be a $1P$ state with $J^P=5/2^-$ or $3/2^-$ by giving the mass spectrum analysis and the strong decay calculation, and predict the existence of $1P$ and $2S$ partners of the $\Sigma_b(6097)$, where their masses and the corresponding decay behaviors are presented. Because of the success of describing the $\Sigma_b(6097)$ and the former observed $\Xi_b(6227)$ under the quasi-two-body treatment to the bottom baryons, we continue to predict the $\Omega_b$ partners of $\Sigma_b(6097)$ by the same method, which are the $1P$ and $2S$ states of the $bss$ baryon system. Identifying these predicted bottom baryons will be a research topic full of challenge and opportunity for future experiments especially the LHCb.
On Line Learning In Neural Networks

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Instrumentation and transformation of Java source code for automated testing with search-based testing algorithms

Search-based Software Test Data Generation is a field of research treating test input generation as a search problem. Search algorithms require that an objective function computes the quality of solution candidates. When the goal for testing is to achieve code coverage, one type of objective function uses branch distance, a heuristic describing how “close” the condition in a control flow statement is from being true. An attempt is made to define procedures to allow the calculation of branch distance for both predicates in conjunction and disjunction predicates with short-circuiting operators && and ||, by identifying and avoiding situations causing side effects and exceptions. This thesis also attempts to give examples of instrumenting and transforming control flow statements, examples which are limited or lacking in the research literature. A program implementing the defined rules for instrumentation and transformation of control flow statements was developed to validate these rules.