cssi/SciSciGPT-SciSciNet huggingface dataset:
Contrastive Explanations In Neural Networks

Visual explanations are logical arguments based on visual features that justify the predictions made by neural networks. Current modes of visual explanations answer questions of the form ‘Why P.7’. These Why questions operate under broad contexts thereby providing answers that are irrelevant in some cases. We propose to constrain these Why questions based on some context Q so that our explanations answer contrastive questions of the form ‘Why P, rather than Q.7’. In this paper, we formalize the structure of contrastive visual explanations for neural networks. We define contrast based on neural networks and propose a methodology to extract defined contrasts. We then use the extracted contrasts as a plug-in on top of existing ‘Why P?’ techniques, specifically Grad-CAM. We demonstrate their value in analyzing both networks and data in applications of largescale recognition, fine-grained recognition, subsurface seismic analysis, and image quality assessment.
The Hopf monoid of orbit polytopes

Many families of combinatorial objects have a Hopf monoid structure. Aguiar and Ardila introduced the Hopf monoid of generalized permutahedra and showed that it contains various other notable combinatorial families as Hopf submonoids, including graphs, posets, and matroids. We introduce the Hopf monoid of orbit polytopes, which is generated by the generalized permutahedra that are invariant under the action of the symmetric group. We show that modulo normal equivalence, these polytopes are in bijection with integer compositions. We interpret the Hopf structure through this lens, and we show that applying the first Fock functor to this Hopf monoid gives a Hopf algebra of compositions. We describe the character group of the Hopf monoid of orbit polytopes in terms of noncommutative symmetric functions, and we give a combinatorial interpretation of the basic character and its polynomial invariant.
Sofosbuvir terminated RNA is more resistant to SARS-CoV-2 proofreader than RNA terminated by Remdesivir

SARS-CoV-2 is responsible for COVID-19, resulting in the largest pandemic in over a hundred years. After examining the molecular structures and activities of hepatitis C viral inhibitors and comparing hepatitis C virus and coronavirus replication, we previously postulated that the FDA-approved hepatitis C drug EPCLUSA (Sofosbuvir/Velpatasvir) might inhibit SARS-CoV-2. We subsequently demonstrated that Sofosbuvir triphosphate is incorporated by the relatively low fidelity SARS-CoV and SARS-CoV-2 RNA-dependent RNA polymerases (RdRps), serving as an immediate polymerase reaction terminator, but not by a host-like high fidelity DNA polymerase. Other investigators have since demonstrated the ability of Sofosbuvir to inhibit SARS-CoV-2 replication in lung and brain cells; additionally, COVID-19 clinical trials with EPCLUSA and with Sofosbuvir plus Daclatasvir have been initiated in several countries. SARS-CoV-2 has an exonuclease-based proofreader to maintain the viral genome integrity. Any effective antiviral targeting the SARS-CoV-2 RdRp must display a certain level of resistance to this proofreading activity. We report here that Sofosbuvir terminated RNA resists removal by the exonuclease to a substantially higher extent than RNA terminated by Remdesivir, another drug being used as a COVID-19 therapeutic. These results offer a molecular basis supporting the current use of Sofosbuvir in combination with other drugs in COVID-19 clinical trials.
Discovery of X-Ray Emission from G328.4+0.2, a Crab-like Supernova Remnant

G328.4+0.2 is a moderately small (5' × 5') Galactic radio supernova remnant (SNR) at a distance of at least 17 kpc that has been long suggested to be Crab-like. Here we report on the detection with ASCA of the X-ray emission from the SNR. The X-ray source is faint with an observed flux of (6.0 ± 0.8) × 10-13 ergs s-1 cm-2 over the 2-10 keV band. The emission is heavily cut off at low energies and no flux is detected below 2 keV. Spectral analysis confirms that the column density to the source is indeed large, NH ~ 1023 atoms cm-2, and consistent with the total column density of hydrogen through the Galaxy at this position. Good fits to the spectrum can be obtained for either thermal plasma or nonthermal power-law models, although the lack of detected line emission as well as other evidence argues against the former interpretation. The power-law index we find, αP = 2.9, is consistent with other Crab-like SNRs. In the radio band, G328.4+0.2 is nearly as luminous as the Crab Nebula, yet in the X-ray band, it is some 70 times fainter. Nevertheless, its inferred soft X-ray band luminosity is greater than all but the brightest pulsar-powered synchrotron nebulae and implies that G328.4+0.2 contains a rapidly spinning, as yet undetected, pulsar that is losing energy at a rate of ~1038 ergs s-1.
Aspherical manifolds that cannot be triangulated

By a result of Manolescu there are topological closed n-manifolds that cannot be triangulated for each n 5. We show here that for n 6 we can choose such manifolds to be aspherical. AMS classication numbers
Addendum to: Commensurations of the Johnson kernel

Let K.S/ be the subgroup of the extended mapping class group, Mod.S/, generated by Dehn twists about separating curves. In our earlier paper, we showed that Comm.K.S//a Aut.K.S//a Mod.S/ when S is a closed, connected, orientable surface of genus g 4. By modifying our original proof, we show that the same result holds for g 3, thus confirming Farb’s conjecture in all cases (the statement is not true for g 2). 20F36 The purpose of this note is to extend the results of our paper “Commensurations of the Johnson kernel” to the lone remaining case. We briefly review the notation and basic ideas before explaining the improvement. We refer the reader to our earlier paper for further details [1]. Let SDSg denote a closed, connected, orientable surface of genus g , and let Mod.S/ denote the extended mapping class group (orientation reversing elements are allowed). The Torelli group I.S/ is the subgroup of Mod.S/ consisting of elements that act trivially on H1.S;Z/, and the Johnson kernel K.S/ is the subgroup of I.S/ generated by Dehn twists about separating curves. The abstract commensurator of a group A , denoted Comm.A/, is the group of isomorphisms of finite index subgroups ofA (under composition), with two such isomorphisms equivalent if they agree on a finite index subgroup of A . The product of W G! H with W G 0 ! H 0 is a map defined on 1 .H\G 0 /.
Cochains and homotopy type

Finite type nilpotent spaces are weakly equivalent if and only if their singular cochains are quasi-isomorphic as E∞ algebras. The cochain functor from the homotopy category of finite type nilpotent spaces to the homotopy category of E∞ algebras is faithful but not full.
DNA confined in a two-dimensional strip geometry

Semiflexible polymers characterized by the contour length L and persistent length confined in a spatial region D have been described as a series of “spherical blobs” and “deflecting lines” by de Gennes and Odjik for and , respectively. Recently new intermediate regimes (extended de Gennes and Gauss-de Gennes) have been investigated by Tree et al. (Phys. Rev. Lett., 110 (2013) 208103). In this letter we derive scaling relations to characterize these transitions in terms of universal scaled fluctuations in d-dimension as a function of , and D, and show that the Gauss-de Gennes regime is absent and the extended de Gennes regime is vanishingly small for polymers confined in a 2D strip. We validate our claim by an extensive Brownian dynamics (BD) simulation which also reveals that the prefactor A used to describe the chain extension in the Odjik limit is independent of the physical dimension d and is the same as previously found by Yang et al. (Phys. Rev. E, 76 (2007) 011804). Our studies are relevant for optical maps of DNA stretched inside a nanostrip.
Sprintz: Time Series Compression for the Internet of Things

Thanks to the rapid proliferation of connected devices, sensor-generated time series constitute a large and growing portion of the world's data. Often, this data is collected from distributed, resource-constrained devices and centralized at one or more servers. A key challenge in this setup is reducing the size of the transmitted data without sacrificing its quality. Lower quality reduces the data's utility, but smaller size enables both reduced network and storage costs at the servers and reduced power consumption in sensing devices. A natural solution is to compress the data at the sensing devices. Unfortunately, existing compression algorithms either violate the memory and latency constraints common for these devices or, as we show experimentally, perform poorly on sensor-generated time series. We introduce a time series compression algorithm that achieves state-of-the-art compression ratios while requiring less than 1KB of memory and adding virtually no latency. This method is suitable not only for low-power devices collecting data, but also for servers storing and querying data; in the latter context, it can decompress at over 3GB/s in a single thread, even faster than many algorithms with much lower compression ratios. A key component of our method is a high-speed forecasting algorithm that can be trained online and significantly outperforms alternatives such as delta coding. Extensive experiments on datasets from many domains show that these results hold not only for sensor data but also across a wide array of other time series.
Resolving the Unresolved Cosmic X-Ray Background in the Chandra Deep Fields

We present a measurement of the surface brightness of the cosmic X-ray background (CXB) in the Chandra Deep Fields, after excluding all detected X-ray, optical, and infrared sources. The work is motivated by a recent X-ray stacking analysis by Worsley and collaborators, which showed that galaxies detected by HST but not by Chandra may account for most of the unresolved CXB at E > 1 keV. We find that after excluding HST and Spitzer IRAC sources, some CXB still remains, but it is marginally significant: (3.4 ± 1.4) × 10-13 ergs cm-2 s-1 deg-2 in the 1-2 keV band and (4 ± 9) × 10-13 ergs cm-2 s-1 deg-2 in the 2-5 keV band, or 7% ± 3% and 4% ± 9% of the total CXB, respectively. Of the 1-2 keV signal resolved by the HST sources, 34% ± 2% comes from objects with optical colors typical of "normal" galaxies (which make up 25% of the HST sources), while the remaining flux comes from objects with colors of starburst and irregular galaxies. In the 0.65-1 keV band (just above the bright Galactic O VII line), the remaining diffuse intensity is (1.0 ± 0.2) × 10-12 ergs cm-2 s-1 deg-2. This flux includes emission from the Galaxy as well as from the hypothetical warm-hot intergalactic medium (WHIM), and provides a conservative upper limit on the WHIM signal that comes interestingly close to theoretical predictions.
When Will we Know a Muon Collider is Feasible? Status and Directions of Muon Accelerator R&D

Over the last decade there has been significant progress in developing the concepts and technologies needed to produce, capture, accelerate and collide high intensity beams of muons. At present, a high-luminosity multi-TeV muon collider presents a viable option for the next generation of lepton-lepton collider, which is believed to be needed to fully explore high energy physics in the era following the LHC discoveries. This paper briefly reviews the status of the accelerator R&D, addresses the question of the feasibility of a Muon Collider, what needs to be done to prove it and presents projected timeline of the project.
Quantifying fermionic decoherence in many-body systems

Practical measures of electronic decoherence, called distilled purities, that are applicable to many-body systems are introduced. While usual measures of electronic decoherence such as the purity employ the full N-particle density matrix which is generally unavailable, the distilled purities are based on the r-body reduced density matrices (r-RDMs) which are more accessible quantities. The r-body distilled purities are derivative quantities of the previously introduced r-body reduced purities [I. Franco and H. Appel, J. Chem. Phys. 139, 094109 (2013)] that measure the non-idempotency of the r-RDMs. Specifically, the distilled purities exploit the structure of the reduced purities to extract coherences between Slater determinants with integer occupations defined by a given single-particle basis that compose an electronic state. In this way, the distilled purities offer a practical platform to quantify coherences in a given basis that can be used to analyze the quantum dynamics of many-electron systems. Exact expressions for the one-body and two-body distilled purities are presented and the utility of the approach is exemplified via an analysis of the dynamics of oligo-acetylene as described by the Su-Schrieffer-Heeger Hamiltonian. Last, the advantages and limitations of the purity, reduced purity, and distilled purity as measures of electronic coherence are discussed.
Endpoint bounds for quasiradial Fourier multipliers

We consider quasiradial Fourier multipliers, i.e., multipliers of the form \(m(a(\xi ))\) for a class of distance functions a. We give a necessary and sufficient condition for the multiplier transformations to be bounded on \(L^p\) for a certain range of p. In addition, when m is compactly supported in \((0,\infty )\), we give a similar result for associated maximal operators.
Interdisciplinary Collaboration through Designing 3D Simulation Case Studies

Interdisciplinary collaboration is essential for the advance of research. As domain subjects become more and more specialized, researchers need to cross disciplines for insights from peers in other areas to have a broader and deeper understand of a topic at micro- and macro-levels. We developed a 3D virtual learning environment that served as a platform for faculty to plan curriculum, share educational beliefs, and conduct cross-discipline research for effective learning. Based upon the scripts designed by faculty from five disciplines, virtual doctors, nurses, or patients interact in a 3D virtual hospital. The teaching vignettes were then converted to video clips, allowing users to view, pause, replay, or comment on the videos individually or in groups. Unlike many existing platforms, we anticipated a value-added by adding a social networking capacity to this virtual environment. The focus of this paper is on the cost-efficiency and system design of the virtual learning environment.
The Tail of PSR J0002+6216 and the Supernova Remnant CTB 1

We have carried out VLA imaging and a Fermi timing analysis of the 115 ms gamma-ray and radio pulsar PSR J0002+6216. We found that the pulsar lies at the apex of a narrowly collimated cometary-like 7 arcmin tail of non-thermal radio emission which we identify as a bow-shock pulsar wind nebula. The tail of the nebula points back toward the geometric center of the supernova remnant CTB 1 (G116.9+0.2) 28 arcmin away, at a position angle $\theta_\mu=113^\circ$. We measure a proper motion with 2.9$\sigma$ significance from a Fermi timing analysis giving $\mu$=115$\pm$33 mas yr$^{-1}$ and $\theta_\mu=121^\circ\pm{13}^\circ$, corresponding to a large transverse pulsar velocity of 1100 km s$^{-1}$ at a distance of 2 kpc. This proper motion is of the right magnitude and direction to support the claim that PSR J0002+6216 was born from the same supernova that produced CTB 1. We explore the implications for pulsar birth periods, asymmetric supernova explosions, and mechanisms for pulsar natal kick velocities.
Traversable wormholes from surgically modified Schwarzschild spacetimes

In this paper I present a new class of traversalle wormholes. This is done by surgically grafting two Schwarzschild spacetimes together in such a way that no event horizon is to form. This surgery concentrates a non-zero stress-energy on the boundary layer between the two asymptotically flat regions. We investigate this stress-energy in detail using the “junction condition” formalism. A feature of the present analysis is that this class of traversible wormholers is sufficiently simple for a (partial) dynamical stability analysis to be carried out. The stability analysis places constraints on the equation of the state o the exotic matter that comprises the throat of the wormhole.
Charged lepton flavor violation: An experimenter’s guide

Abstract Charged lepton flavor violation (CLFV) is a clear signal of new physics; it directly addresses the physics of flavor and of generations. The search for CLFV has continued from the early 1940s, when the muon was identified as a separate particle, until today. Certainly in the LHC era the motivations for continued searches are clear and have been covered in many reviews. This review is focused on the experimental history with a view toward how these searches might progress. We examine the status of searches for charged lepton flavor violation in the muon, tau, and other channels, and then examine the prospects for new efforts over the next decade. Finally, we examine what paths might be taken after the conclusion of upcoming experiments and what facilities might be required.
What triggers star formation in galaxies

Processes that promote the formation of dense cold clouds in the interstellar media of galaxies are reviewed. Those that involve background stellar mass include two-fluid instabilities, spiral density wave shocking, and bar accretion. Young stellar pressures trigger gas accumulation on the periphery of cleared cavities, which often take the form of rings by the time new stars form. Stellar pressures also trigger star formation in bright-rim structures, directly squeezing the pre-existing clumps in nearby clouds and clearing out the lower density gas between them. Observations of these processes are common. How they fit into the empirical star formation laws, which relate the star formation rate primarily to the gas density, is unclear. Most likely, star formation follows directly from the formation of cold dense gas, whatever the origin of that gas. If the average pressure from the weight of the gas layer is large enough to produce a high molecular fraction in the ambient medium, then star formation should follow from a variety of processes that combine and lose their distinctive origins. Pressurized triggering might have more influence on the star formation rate in regions with low average molecular fraction. This implies, for example, that the arm/interarm ratio of star formation efficiency should be higher in the outer regions of galaxies than in the main disks.
Energy Cascades and Flux Locality in Physical Scales of the 3D Navier-Stokes Equations

Rigorous estimates for the total – (kinetic) energy plus pressure – flux in \({\mathbb{R}^3}\) are obtained from the three dimensional Navier-Stokes equations. The bounds are used to establish a condition – involving Taylor length scale and the size of the domain – sufficient for existence of the inertial range and the energy cascade in decaying turbulence (zero driving force, non-increasing global energy). Several manifestations of the locality of the flux under this condition are obtained. All the scales involved are actual physical scales in \({\mathbb{R}^3}\) and no regularity or homogeneity/scaling assumptions are made.
Recursion Relations in $p$-adic Mellin Space

In this work, we formulate a set of rules for writing down p -adic Mellin amplitudes at tree-level. The rules lead to closed-form expressions for Mellin amplitudes for arbitrary scalar bulk diagrams. The prescription is recursive in nature, with two different physical interpretations: one as a recursion on the number of internal lines in the diagram, and the other as reminiscent of on-shell BCFW recursion for flat-space amplitudes, especially when viewed in auxiliary momentum space. The prescriptions are proven in full generality, and their close connection with Feynman rules for real Mellin amplitudes is explained. We also show that the integrands in the Mellin–Barnes representation of both real and p -adic Mellin amplitudes, the so-called pre-amplitudes, can be constructed according to virtually identical rules, and that these pre-amplitudes themselves may be re-expressed as products of particular Mellin amplitudes with complexified conformal dimensions.
A Search for Aperiodic Millisecond Variability in Cygnus X-1

We have conducted a search for aperiodic millisecond variability in the integrated 1-25 keV X-ray region of Cyg X-1. We have examined HEAO A-1 archival data and Rossi X-Ray Timing Explorer (RXTE) guest observer data for evidence of excess power above the Poisson noise floor using the relative integral power analysis and the Fourier transform method. Our results are in disagreement with the results of Meekins and coworkers. We attribute the discrepancy to an instrumental effect for which Meekins and coworkers did not apply a correction. With the correction we see no evidence for excess power above 25 Hz in the HEAO A-1 data. Our analysis of RXTE data is in agreement with previously published results of different data sets and shows no indication of excess power above 30 Hz.
Dark matter in dwarf spheroidal galaxies and indirect detection: a review.

Indirect dark matter searches targeting dwarf spheroidal galaxies (dSphs) have matured rapidly during the past decade. This has been because of the substantial increase in kinematic data sets from the dSphs, the new dSphs that have been discovered, and the operation of the Fermi-LAT and many ground-based gamma-ray experiments. Here we review the analysis methods that have been used to determine the dSph dark matter distributions, in particular the ‘J-factors’, comparing and contrasting them, and detailing the underlying systematics that still affect the analysis. We discuss prospects for improving measurements of dark matter distributions, and how these interplay with future indirect dark matter searches.
Correlated Electron Materials and Field Effect Transistors for Logic: A Review

Correlated electron systems are among the centerpieces of modern condensed matter sciences, where many interesting physical phenomena, such as metal-insulator transition and high-T c superconductivity appear. Recent efforts have been focused on electrostatic doping of such materials to probe the underlying physics without introducing disorder as well as to build field-effect transistors that may complement conventional semiconductor metal-oxide-semiconductor field effect transistor (MOSFET) technology. This review focuses on metal-insulator transition mechanisms in correlated electron materials and three-terminal field effect devices utilizing such correlated oxides as the channel layer. We first describe how electron-disorder interaction, electron-phonon interaction, and/or electron correlation in solids could modify the electronic properties of materials and lead to metal-insulator transitions. Then we analyze experimental efforts toward utilizing these transitions in field effect transistors and their ...
Singular Spectrum for Radial Trees

We prove several results showing that absolutely continuous spectrum for the Laplacian on radial trees is a rare event. In particular, we show that metric trees with unbounded edges have purely singular spectrum and that, generically (in the sense of Baire), radial trees have purely singular continuous spectrum.
Gas Accretion and Galactic Chemical Evolution: Theory and Observations

This chapter reviews how galactic inflows influence galaxy metallicity. The goal is to discuss predictions from theoretical models, but particular emphasis is placed on the insights that result from using models to interpret observations. Even as the classical “G-dwarf problem” endures in the latest round of observational confirmation, a rich and tantalizing new phenomenology of relationships between M∗, Z, SFR, and gas fraction is emerging both in observations and in theoretical models. A consensus interpretation is emerging in which star-forming galaxies do most of their growing in a quiescent way that balances gas inflows and gas processing, and metal dilution with enrichment. Models that explicitly invoke this idea via equilibrium conditions can be used to infer inflow rates from observations, while models that do not assume equilibrium growth tend to recover it self-consistently. Mergers are an overall subdominant mechanism for delivering fresh gas to galaxies, but they trigger radial flows of previously accreted gas that flatten radial gas-phase metallicity gradients and temporarily suppress central metallicities. Radial gradients are generically expected to be steep at early times and then flattened by mergers and enriched inflows of recycled gas at late times. However, further theoretical work is required in order to understand how to interpret observations. Likewise, more observational work is needed in order to understand how metallicity gradients evolve to high redshifts.
Collision probabilities of migrating small bodies and dust particles with planets

Probabilities of collisions of migrating small bodies and dust particles produced by these bodies with planets were studied. Various Jupiter-family comets, Halley-type comets, long- period comets, trans-Neptunian objects, and asteroids were considered. The total probability of collisions of any considered body or particle with all planets did not exceed 0.2. The amount of water delivered from outside of Jupiter's orbit to the Earth during the formation of the giant planets could exceed the amount of water in Earth's oceans. The ratio of the mass of water delivered to a planet by Jupiter-family comets or Halley-type comets to the mass of the planet can be greater for Mars, Venus, and Mercury, than that for Earth. 1. Model of migration of small bodies and dust particles In the present paper we discuss the probabilities of collisions of migrating small bodies and dust particles produced by these bodies with planets. Ipatov & Mather (2003, 2004a- b, 2006, 2007), Ipatov et al. (2004), and several other authors cited in the above papers studied the probabilities with Earth, Venus, and Mars. In our above papers (which can be found on astro-ph and http://faculty.cua.edu/ipatov/list-publications.htm), the prob- abilities of the collisions were calculated based on the time variations of orbits of bodies and particles during their dynamical lifetimes (until all bodies or particles reached 2000 AU from the Sun or collided with the Sun). Using the same time variations, below we consider also the probabilities of collisions with the giant planets and Mercury. The orbital evolution of >30,000 bodies with initial orbits close to those of Jupiter- family comets (JFCs), Halley-type comets, long-period comets, trans-Neptunian objects, and asteroids in the resonances 3/1 and 5/2 with Jupiter, and also of >20,000 dust particles produced by these small bodies was integrated during their dynamical lifetimes. We considered the gravitational influence of planets, but omitted the influence of Mercury (exclusive for Comet 2P/Encke). In about a half of calculations of migration of bodies, we used the method by Bulirsh-Stoer (1966) (BULSTO code), and in other runs we used a symplectic method (RMVS3 code). The integration package of Levison & Duncan (1994) was used. For dust particles, only the BULSTO code was used, and the gravitational influence of all planets, the Poynting-Robertson drag, radiation pressure, and solar wind drag were taken into account. The ratiobetween the radiation pressure force and the gravitational force varied from 60.0004 to 0.4. For silicates, such values ofcorrespond to particle diameters d between >1000 and 1 microns; d is proportional to 1/�. In our calculations, planets were considered as material points, so literal collisions did not occur. However, using the algorithm suggested by Ipatov (1988) with the correction that takes into account a different velocity at different parts of the orbit (Ipatov & Mather
Yang-Mills theory, 2 + 1 and 3 + 1 dimensions ∗

I review the analysis of (2+1)-dimensional Yang-Mills (YM2+1) theory via the use of gauge-invariant matrix variables. The vacuum wavefunction, string tension, the propagator mass for gluons, its relation to the magnetic mass for YM3+1 at nonzero temperature and the extension of our analysis to the Yang-Mills-Chern-Simons theory are discussed. A possible extension to 3 + 1 dimensions is also briefly considered.
Estimates for radial solutions of the homogeneous Landau equation with Coulomb potential

Motivated by the question of existence of global solutions, we obtain pointwise upper bounds for radially symmetric and monotone solutions to the homogeneous Landau equation with Coulomb potential. The estimates say that blow up in the $L^\infty$-norm at a finite time $T$ can occur only if the $L^{3/2}$-norm of the solution concentrates for times close to $T$. The bounds are obtained using the comparison principle for the Landau equation and for the associated mass function. This method provides long-time existence results for the isotropic version of the Landau equation with Coulomb potential, recently introduced by Krieger and Strain.
Small permutation classes

We establish a phase transition for permutation classes (downsets of permutations under the permutation containment order): there is an algebraic number $\kappa$, approximately 2.20557, for which there are only countably many permutation classes of growth rate (Stanley-Wilf limit) less than $\kappa$ but uncountably many permutation classes of growth rate $\kappa$, answering a question of Klazar. We go on to completely characterize the possible sub-$\kappa$ growth rates of permutation classes, answering a question of Kaiser and Klazar. Central to our proofs are the concepts of generalized grid classes (introduced herein), partial well-order, and atomicity (also known as the joint embedding property).
NEURAL BELIEF REASONER

The embodiment of the invention relates to a neural belief reasoner. Embodiments of the present disclosure relate to a generation model for unsupervised learning, and more particularly, to a generation model specifying a belief function. Technologies for a neural belief reasoner model generative models that specifies belief functions are described. Aspects include receiving, by a device operatively coupled to a processor, a request for a belief function, and processing, by the device, the request for the belief function in the generative model based on trained probability parameters and a minimization function to determine a generalized belief function defined by fuzzy sets. Data corresponding to the generalized belief function is output, e.g., as a belief value and plausibility value.
Physics with reactor neutrinos

Neutrinos produced by nuclear reactors have played a major role in advancing our knowledge of the properties of neutrinos. The first direct detection of the neutrino, confirming its existence, was performed using reactor neutrinos. More recent experiments utilizing reactor neutrinos have also found clear evidence for neutrino oscillation, providing unique input for the determination of neutrino mass and mixing. Ongoing and future reactor neutrino experiments will explore other important issues, including the neutrino mass hierarchy and the search for sterile neutrinos and other new physics beyond the standard model. In this article, we review the recent progress in physics using reactor neutrinos and the opportunities they offer for future discoveries.
Dual-tip-enhanced ultrafast CARS nanoscopy

Coherent anti-Stokes Raman scattering (CARS) and, in particular, femtosecond adaptive spectroscopic techniques (FAST CARS) have been successfully used for molecular spectroscopy and microscopic imaging. Recent progress in ultrafast nano-optics provides flexibility in generation and control of optical near fields, and holds promise to extend CARS techniques to the nanoscale. In this theoretical study, we demonstrate ultrafast subwavelentgh control of coherent Raman spectra of molecules in the vicinity of a plasmonic nanostructure excited by ultrashort laser pulses. The simulated nanostructure design provides localized excitation sources for CARS by focusing incident laser pulses into subwavelength hot spots via two self-similar nanolens antennas connected by a waveguide. Hot-spot-selective dual-tip-enhanced CARS (2TECARS) nanospectra of DNA nucleobases are obtained by simulating optimized pump, Stokes and probe near fields using tips, laser polarization- and pulse-shaping. This technique may be used to explore ultrafast energy and electron transfer dynamics in real space with nanometre resolution.
Bayesian Ages for Early-type Stars from Isochrones Including Rotation, and a Possible Old Age for the Hyades

We combine recently computed models of stellar evolution using a new treatment of rotation with a Bayesian statistical framework to constrain the ages and other properties of early-type stars. We find good agreement for early-type stars and clusters with known young ages, including ? Pictoris, the Pleiades, and the Ursa Majoris moving group. However, we derive a substantially older age for the Hyades open cluster (750 ? 100 Myr compared to 625 ? 50 Myr). This older age results from both the increase in main-sequence lifetime with stellar rotation and from the fact that rotating models near the main-sequence turnoff are more luminous, overlapping with slightly more massive (and shorter-lived) nonrotating ones. Our method uses a large grid of nonrotating models to interpolate between a much sparser rotating grid, and also includes a detailed calculation of synthetic magnitudes as a function of orientation. We provide a web interface at http://www.bayesianstellarparameters.info, where the results of our analysis may be downloaded for individual early-type () Hipparcos stars. The web interface accepts user-supplied parameters for a Gaussian metallicity prior and returns posterior probability distributions on mass, age, and orientation.
Optimal Period of Workload Redistribution for Dynamic Bulk Synchronous Computations in Heterogeneous Computing Systems

In dynamic bulk synchronous computations, processors may change their workloads from phase to phase. Such workload change will possibly increase the duration of a phase and the overall parallel execution time. Therefore, it is necessary to redistribute workload at runtime to reduce the parallel time. However, such workload redistribution at runtime can be expensive and the overhead of frequent runtime workload redistribution may exceed the benefit of workload redistribution and balancing. The problem of finding the optimal period of runtime workload redistribution for dynamic bulk synchronous computations is motivated by the combined consideration of parallel execution time and system overhead for workload redistribution and balancing. We develop an analytical method to solve the problem in heterogeneous computing systems. We also demonstrate numerical data of the analytical method and simulation results that verify the analytical data.
Continuity of discrete homomorphisms of diffeomorphism groups

In [7], Filipckewicz proved the following result: Given two C manifolds M and N , the groups Diffc.M / and Diffc.N / are isomorphic (as discrete groups) if and only if the manifolds M and N are C diffeomorphic. Moreover, if such an isomorphism exists it is given by conjugation with a fixed element of Diff.M /. Filipckewicz’s theorem implies in particular that two different smooth exotic 7–spheres have different diffeomorphism groups.
Off the Beaten Path: Gaia Reveals GD-1 Stars outside of the Main Stream

Tidally disrupted globular clusters are transformed into thin, dynamically cold streams of stars that are extremely valuable tracers of the large- and small-scale distribution of mass in the Galaxy. Using data from the Gaia second data release combined with Pan-STARRS photometry, we present a sample of highly probable members of the longest cold stream in the Milky Way, GD-1. The resulting map of GD-1: (1) extends the apparent length of the stream by 20°, (2) reveals plausible locations for the progenitor, (3) detects high-contrast gaps along the stream, and (4) indicates the existence of stream members perturbed off the main stream track. These discoveries are only possible because of the exquisite astrometry from Gaia, which permits a clean separation of the stream from Milky Way stars. The additional length and a proper treatment of the progenitor will aid in dynamical modeling of GD-1 for mapping the large-scale dark matter distribution. The complex morphology of the stream points to a turbulent history; detailed phase-space properties of the perturbed stream members could potentially constrain dark matter substructure in the Milky Way.
A Machine-Learning Approach for Earthquake Magnitude Estimation

In this study we develop a single-station deep-learning approach for fast and reliable estimation of earthquake magnitude directly from raw waveforms. We design a regressor composed of convolutional and recurrent neural networks that is not sensitive to the data normalization, hence waveform amplitude information can be utilized during the training. Our network can predict earthquake magnitudes with an average error close to zero and standard deviation of ~0.2 based on single-station waveforms without instrument response correction. We test the network for both local and duration magnitude scales and show a station-based learning can be an effective approach for improving the performance. The proposed approach has a variety of potential applications from routine earthquake monitoring to early warning systems.
Colorless states in perturbative QCD: Charmonium and rapidity gaps

Abstract We point out that an unorthodox way to describe the production of rapidity gaps in deep inelastic scattering, recently proposed by Buchmuller and Hebecker, suggests a description of the production of heavy quark bound states which is in agreement with data. The approach questions the conventional treatment of the color quantum number in perturbative QCD.
AN ALTERNATIVE APPROACH TO MEASURING REVERBERATION LAGS IN ACTIVE GALACTIC NUCLEI

Motivated by recent progress in the statistical modeling of quasar variability, we develop a new approach to measuring emission-line reverberation lags to estimate the size of broad-line regions (BLRs) in active galactic nuclei. Assuming that all emission-line light curves are scaled, smoothed, and displaced versions of the continuum, this alternative approach fits the light curves directly using a damped random walk model and aligns them to recover the time lag and its statistical confidence limits. We introduce the mathematical formalism of this approach and demonstrate its ability to cope with some of the problems for traditional methods, such as irregular sampling, correlated errors, and seasonal gaps. We redetermine the lags for 87 emission lines in 31 quasars and reassess the BLR size-luminosity relationship using 60 Hβ lags. We confirm the general results from the traditional cross-correlation methods, with a few exceptions. Our method, however, also supports a broad range of extensions. In particular, it can simultaneously fit multiple lines and continuum light curves which improves the lag estimate for the lines and provides estimates of the error correlations between them. Determining these correlations is of particular importance for interpreting emission-line velocity-delay maps. We can also include parameters for luminosity-dependent lags or line responses. We use this to detect the scaling of the BLR size with continuum luminosity in NGC 5548.
Implementation of epidemic routing with IP convergence layer in ns-3

We present the Epidemic routing protocol implementation in ns-3. It is a full-featured DTN protocol in that it supports the message abstraction and store-and-haul behavior. We compare the performance of our Epidemic routing ns-3 implementation with the existing implementation of Epidemic in the ONE simulator, and discuss the differences.
The Coma-Leo I distance ratio and the Hubble constant

Abstract The diameter-velocity dispersion relation in B, V, and K for three early-type galaxies in the Leo I (M96) group is derived from published photometry and kinematic data. The relations in all three colors have slopes which agree well with those for the Coma cluster. The RMS scatter of the Leo I galaxies in each color is extremely small, consistent with the group's compactness. These relations yield estimates of the Coma-Leo I distance ratio of 9.01 ± 0.51, 8.77 ± 0.43, and 8.82 ± 0.31, respectively, with a weighted mean of 8.84 ± 0.23. The general agreement among the three colors indicates that the early-type galaxies in Leo I and Coma have similar stellar populations. The Coma-Leo I distance ratio coupled with estimates of the absolute distance to the Leo I group allows the Hubble constant to be determined, free of the uncertainties which arise when working with the Virgo cluster. Several high quality distance estimates are available from a variety of techniques: Cepheids in M96 (Tanvir, N.R., et al., 1995, Natur, 377, 27) and M95 (Graham, J.A., et al., 1997, ApJ, 477, 535), surface brightness fluctuations (Tonry, J.L., et al., 1997, ApJ, 475, 399), planetary nebulae luminosity functions (Ciardullo, R., et al., 1993, ApJ, 419, 479), and the luminosity of the red giant branch tip (Sakai, S., Freedman, W.L., & Madore, B.F., 1996, in: Formation of the Galactic Halo, Inside and Out, eds. H. Morrison & A. Sarajedini, PASP Conf. Series Vol. 92). Adopting a cosmic recession velocity of the Coma cluster in the microwave background frame of 7200 ± 300 km s−1, these distance estimates lead to values of the Hubble constant ranging from 70 to 81 km s−1 Mpc−1, with an unweighted mean of 75 ± 6 km s−1 Mpc−1.
Reinforcement-driven spread of innovations and fads

We investigate how social reinforcement drives the spread of permanent innovations and transient fads. We account for social reinforcement by endowing each individual with M + 1 possible awareness states 0, 1, 2,..., M, with state M corresponding to adopting an innovation. An individual with awareness k 1. When individuals can abandon the innovation at rate λ, the population fraction that remains clueless about the fad undergoes a phase transition at a critical rate λc; this transition is second order for M = 1 and first order for M > 1, with macroscopic fluctuations accompanying the latter. The time for the fad to disappear has an intriguing non-monotonic dependence on λ.
Increase of SERS Signal upon Heating or Exposure to a High-Intensity Laser Field: Benzenethiol on an AgFON Substrate

The surface-enhanced Raman scattering (SERS) signal from an AgFON plasmonic substrate, recoated with benzenethiol, was observed to increase by about 100% upon heating for 3.5 min at 100 °C and 1.5 min at 125 °C. The signal intensity was found to increase further by about 80% upon a 10 s exposure to a high-intensity (3.2 kW/cm2) 785 nm CW laser, corresponding to 40 mW in a 40 ± 5 μm diameter spot. The observed increase in the SERS signal may be understood by considering the presence of benzenethiol molecules in an intermediate or “precursor” state in addition to conventionally ordered molecules forming a self-assembled monolayer. The increase in the SERS signal arises from the conversion of the molecules in the precursor state to the chemisorbed state due to thermal and photothermal effects.
Endoscopic character identities for depth-zero supercuspidal $L$-packets

One of the conjectural properties of a Langlands correspondence is its compatibility with endoscopic induction. DeBacker and Reeder have recently constructed a partial local Langlands correspondence for p-adic groups, focusing on L-packets consisting of depth-zero supercuspidal representations. In this paper we prove the conjectural endoscopic transfer for these L-packets.
Correlation functions and cumulants in elliptic flow analysis

Abstract We consider various methods of flow analysis in heavy ion collisions and compare experimental data on corresponding observables to the predictions of our saturation model proposed earlier [Nucl. Phys. A 708 (2002) 413]. We demonstrate that, due to the nature of the standard flow analysis, azimuthal distribution of particles with respect to reaction plane determined from the second order harmonics should always be proportional to cos2(φ−ΨR) independent of the physical origin of particle correlations (flow or non-flow). The amplitude of this distribution is always physical and proportional to v2. Two-particle correlations analysis is, therefore, a more reliable way of extracting the shape of physical azimuthal anisotropy. We demonstrate that two-particle correlation functions generated in our minijet model of particle production [Nucl. Phys. A 708 (2002) 413] are in good agreement with the data reported by PHENIX. We discuss the role of non-flow correlations in the cumulant flow analysis and demonstrate using a simple example that if the flow is weak, higher order cumulants analysis does not significantly reduce the contribution of non-flow correlations to elliptic flow observable v2 in RHIC data.
Achievable Rate of Private Function Retrieval from MDS Coded Databases

We study the problem of private function retrieval (PFR) in a distributed storage system. In PFR the user wishes to retrieve a linear combination of $M$ messages stored in non-colluding (N, K) MDS coded databases while revealing no information about the coefficients of the intended linear combination to any of the individual databases. We present an achievable scheme for MDS coded PFR with a rate that matches the capacity for coded private information retrieval derived recently, $R= (1+R_{c}+R_{c}^{2}+\cdots +R_{c}^{M-1})^{-1}=\frac{1-R_{c}}{1-R_{c}^{M}}$ , where $R_{c}=\frac{K}{N}$ is the rate of the MDS code.
THE IMPACT OF THE CONVECTIVE BLUESHIFT EFFECT ON SPECTROSCOPIC PLANETARY TRANSITS

We present here a small anomalous radial velocity (RV) signal expected to be present in RV curves measured during planetary transits. This signal is induced by the convective blueshift (CB) effect-a net blueshift emanating from the stellar surface, resulting from a larger contribution of rising hot and bright gas relative to the colder and darker sinking gas. Since the CB radial component varies across the stellar surface, the light blocked by the planet during a transit will have a varying RV component, resulting in a small shift of the measured RVs. The CB-induced anomalous RV curve is different than, and independent of, the well-known Rossiter-McLaughlin (RM) effect, where the latter is used for determining the sky-projected angle between the host star rotation axis and the planet's orbital angular momentum axis. The observed RV curve is the sum of the CB and RM signals, and they are both superposed on the orbital Keplerian curve. If not accounted for, the presence of the CB RV signal in the spectroscopic transit RV curve may bias the estimate of the spin-orbit angle. In addition, future very high precision RVs will allow the use of transiting planets to study the CB of their host stars.
Cutting sequences on square-tiled surfaces

We characterize cutting sequences of infinite geodesics on square-tiled surfaces by considering interval exchanges on specially chosen intervals on the surface. These interval exchanges can be thought of as skew products over a rotation, and we convert cutting sequences to symbolic trajectories of these interval exchanges to show that special types of combinatorial lifts of Sturmian sequences completely describe all cutting sequences on a square-tiled surface. Our results extend the list of families of surfaces where cutting sequences are understood to a dense subset of the moduli space of all translation surfaces.