Miracle-dz/UniFAR-FTUs huggingface dataset:
Retrieval method for the bianisotropic polarizability tensor of Willis acoustic scatterers

Acoustic materials displaying coupling between pressure and momentum are known as Willis materials. The simplest Willis materials are comprised of sub-wavelength scatterers that couple monopoles to dipoles and {\it vice versa}, with the interaction defined by a polarizability tensor. We propose a method for retrieving the polarizability tensor for sub-wavelength Willis acoustic scatterers using a finite set of scattering amplitudes. We relate the polarizability tensor to standard T-matrix and S-matrix scattering formalisms. This leads to an explicit method for retrieving the components of the polarizability tensor in terms of a small set of scattered pressure data in the near- or far-field. Numerical examples demonstrate the retrieval method for one and two dimensional configurations.
High-Resolution Optical Fiber Salinity Sensor With Self-Referenced Parallel Fabry–Perot Fiber Microcavity

A high-resolution salinity sensor based on a self-referenced parallel Fabry–Perot fiber microcavity is proposed. The sensor is fabricated by inserting a short piece of exposed-core microstructure fiber (ECF) between multimode fiber (MMF) and single-mode fiber (SMF). Due to the unique exposed-core fiber structure and the specially designed SMF-MMF-ECF-SMF structure, two prominent parallel Fabry–Perot interferometers (FPIs) are constructed. Besides, a self-referenced differential phase-demodulation technology is proposed to eliminate the wavelength uncertainty of the spectra measurement devices. Enhanced demodulation system stability and accuracy are achieved by analyzing the phase shift responses of the reflection spectrum. A high salinity-phase sensitivity of 17.36 deg/ ‰ in the range from 0 ‰ to 35 ‰ is obtained, and the corresponding refractive index (RI) sensitivity is <inline-formula> <tex-math notation="LaTeX">${1.04} \times {10} ^{{5}}$ </tex-math></inline-formula> deg/RIU. The salinity resolution and RI resolution are as low as 0.0058 ‰ and <inline-formula> <tex-math notation="LaTeX">${9.6} \times {10} ^{-{7}}$ </tex-math></inline-formula> RIU, respectively, which gives a great potential for harsh environmental monitoring and label-free biochemical analysis.
Very high-gain and low-excess noise near-infrared single-photon avalanche detector: an NIR solid state photomultiplier

A new family of photodetectors with a Discrete Amplification (DA) mechanism allows the realization of very high gain and low excess noise factor in the visible and near infrared spectral regions and offers an alternative to conventional photomultiplier tubes and Geiger mode avalanche photodetectors. These photodetectors can operate in linear detection mode with gain-bandwidth product in excess of 4X1014 and in photon counting mode with count rates up to 108 counts/sec. Potential benefits of this technology over conventional avalanche photodetectors include ultra low excess noise factor, very high gain, and lower reset time (<< 1 μs). In the photon counting mode, the devices can be operated in the non-gated mode under a constant dc bias. Because of its unique characteristics of self-quenching and self-recovery, no external quenching circuit is needed. We present the discrete amplification design approach used for the development of a solid state photomultiplier in the near infrared wavelength region. The demonstrated device performance far exceeds any available solid state photodetectors in the near infrared wavelength range. The measured devices have the following performance characteristics: gain > 2X105, excess noise factor < 1.05, rise time < 350ps, fall time < 500ps, dark current < 2X106 cps, operating voltage < 60V. These devices are ideal for researchers in the field of deep space optical communication, spectroscopy, industrial and scientific instrumentation, Ladar/Lidar, quantum cryptography, night vision and other military, defence and aerospace applications.
Lack of High-Quality, Frequent Feedback Contributes to Low Success Rates for Community College Students

Most students who enter a community college never finish. In fact, “fewer than four of every ten complete any type of degree or certificate within six years” (Bailey et al., 2015). One reason for low success rates is the lack of high-quality, frequent feedback provided to students. Feedback has been shown to improve student learning and success. The purpose of this systematic literature review was to understand the root causes for the lack of productive, consistent feedback. To this end, traditional peer-reviewed research, public scholarship sources, and faculty perspectives were included in this literature review. One cause identified was the lack of comprehensive faculty training in pedagogy in general and in how to provide high-quality feedback specifically. Another reason was lack of time. Faculty who teach in community colleges typically have heavy teaching loads, along with service and other responsibilities that make it difficult to provide regular, high-quality feedback to students. Finally, many students have a negative perception of feedback and therefore, often ignore it. When students do not use feedback, faculty can determine that providing feedback is not a good use of their time. There is ample evidence in the literature that supporting faculty to provide high-quality feedback is effective for promoting students’ academic success.
Charm hadronisation measurements with the ALICE experiment

Charm quarks are produced in hard scatterings at the early stages of the hadronic collisions due to the heavy mass of the quark. The production cross section of charm can be described by pQCD calculations based on the factorisation approach. This description traditionally assumes universal fragmentation functions of charm into hadrons among different collision systems. The ALICE experiment measured charmed-baryon production in pp collisions for different baryon species, observing a significant enhancement of the charm baryon-to-meson yield ratios, for pT < 10–12 GeV/c, with respect to measurements performed at e+e− and ep colliders. Measurements of charmed baryon production in pp collisions also provide a fundamental reference for heavy-ion collisions, in which an enhancement of the baryon-to-meson ratio could be due to an additional hadronisation mechanism via coalescence of charm quarks with lighter quarks in a deconfined medium. This contribution discusses the latest measurements of charm production performed by the ALICE Collaboration in pp collisions at the LHC via D mesons, Λc+, Σc0,+,++, Ξc0,+, and Ωc0 baryons at midrapidity at √s = 5.02 and 13 TeV. The most recent measurements of the Λc+/D0 ratio in Pb–Pb collisions at √sNN = 5.02 are also presented, together with the first measurement of the charm fragmentation fraction into hadrons in pp and p–Pb collisions at the same energy.
Mapping Jet-ISM Interactions in X-ray Binaries with ALMA: A GRS 1915$+$105 Case Study

We present Atacama Large Millimetre/Sub-Millimetre Array (ALMA) observations of IRAS 19132+1035, a candidate jet-ISM interaction zone near the black hole X-ray binary (BHXB) GRS 1915+105. With these ALMA observations (combining data from the 12 m array and the Atacama Compact Array), we map the molecular line emission across the IRAS 19132+1035 region. We detect emission from the $^{12}$CO [$J=2-1$], $^{13}$CO [$\nu=0$, $J=2-1$], C$^{18}$O [$J=2-1$], ${\rm H}_{2}{\rm CO}$ [$J=3_{0,3}-2_{0,2}$], ${\rm H}_{2}{\rm CO}$ [$J=3_{2,2}-2_{2,1}$], ${\rm H}_{2}{\rm CO}$ [$J=3_{2,1}-2_{2,0}$], SiO [$\nu=0$, $J=5-4$], CH$_3$OH [$J=4_{2,2}-3_{1,2}$], and CS [$\nu=0$, $J=5-4$] transitions. Given the morphological, spectral, and kinematic properties of this molecular emission, we present several lines of evidence that support the presence of a jet-ISM interaction at this site, including a jet-blown cavity in the molecular gas. This compelling new evidence identifies this site as a jet-ISM interaction zone, making GRS 1915$+$105 the third Galactic BHXB with at least one conclusive jet-ISM interaction zone. However, we find that this interaction occurs on much smaller scales than was postulated by previous work, where the BHXB jet does not appear to be dominantly powering the entire IRAS 19132+1035 region. Using estimates of the ISM conditions in the region, we utilize the detected cavity as a calorimeter to estimate the time-averaged power carried in the GRS 1915+105 jets of $(8.4^{+7.7}_{-8.1})\times10^{32}\,{\rm erg\,s}^{-1}$. Overall, our analysis demonstrates that molecular lines are excellent diagnostic tools to identify and probe jet-ISM interaction zones near Galactic BHXBs.
Adaptively heterogeneous transfer learning for hyperspectral image classification

ABSTRACT Convolutional Neural Network (CNN) has been proved excellent for hyperspectral image(HSI) classification on the basis of large training set. However, the lack of available samples degrades the performance of CNNs in practical HSI classification. Although transfer learning is a typical strategy to address the issue of limited training samples, such methods tend to reload source model’s feature extractors directly ignoring their generalization. Furthermore, most existing adaptive transfer learning algorithms pay attention to spectral features of HSI while the obvious difference between RGB image and HSI’s spatial features is overlooked. In this paper, the proposed method can solve the mentioned problems to some extent. Firstly, the proposed adaptive heterogeneous transfer (AHT) can measure their transferability and find appropriate solution to transfer knowledge. It computes feature extractors’ transferability based on feature maps and influences the learning process of target model through backpropagation, therefore, target model is prone to receive knowledge from feature extractors with high generalization. Secondly, the proposed method lays emphasis on HSI’s spatial features. It adopts the methodology of spatial attention and calculates the regularization loss based on spatial features. Experiments were conducted on two widely used HSI datasets. The results demonstrate the method’s effectiveness when few samples are available.
Relevance of CYP2D6 Gene Variants in Population Genetic Differentiation

A significant portion of the variability in complex features, such as drug response, is likely caused by human genetic diversity. One of the highly polymorphic pharmacogenes is CYP2D6, encoding an enzyme involved in the metabolism of about 25% of commonly prescribed drugs. In a directed search of the 1000 Genomes Phase III variation data, 86 single nucleotide polymorphisms (SNPs) in the CYP2D6 gene were extracted from the genotypes of 2504 individuals from 26 populations, and then used to reconstruct haplotypes. Analyses were performed using Haploview, Phase, and Arlequin softwares. Haplotype and nucleotide diversity were high in all populations, but highest in populations of African ancestry. Pairwise FST showed significant results for eleven SNPs, six of which were characteristic of African populations, while four SNPs were most common in East Asian populations. A principal component analysis of CYP2D6 haplotypes showed that African populations form one cluster, Asian populations form another cluster with East and South Asian populations separated, while European populations form the third cluster. Linkage disequilibrium showed that all African populations have three or more haplotype blocks within the CYP2D6 gene, while other world populations have one, except for Chinese Dai and Punjabi in Pakistan populations, which have two.
Gas Sloshing in Abell 2204: Constraining the Properties of the Magnetized Intracluster Medium

The rich galaxy cluster Abell 2204 exhibits edges in its X-ray surface brightness at ∼65 and west and east of its center, respectively. The presence of these edges, which were interpreted as sloshing cold fronts, implies that the intracluster medium (ICM) was recently disturbed. We analyze the properties of the ICM using multiple Chandra observations of Abell 2204. We find a density ratio of and a temperature ratio of (projected, or 1.87 ± 0.56 deprojected) across the western edge, and correspondingly and (projected, or 1.25 ± 0.26 deprojected) across the eastern edge. These values are typical of cold fronts in galaxy clusters. This, together with the spiral pattern observed in the cluster core, supports the sloshing scenario for Abell 2204. No Kelvin–Helmholtz eddies are observed along the cold front surfaces, indicating that they are effectively suppressed by some physical mechanism. We argue that the suppression is likely facilitated by the magnetic fields amplified in the sloshing motion and deduce from the measured gas properties that the magnetic field strength should be greater than 24 ± 6 μG and 32 ± 8 μG along the west and east cold fronts, respectively.
Short-coherence length superconductivity in the Attractive Hubbard Model in three dimensions

We study the normal state and the superconducting transition in the Attractive Hubbard Model in three dimensions, using self-consistent diagrammatics. Our results for the self-consistent T -matrix approximation are consistent with 3D- XY power-law critical scaling and ﬁnite-size scaling. This is in contrast to the exponential 2D- XY scaling the method was able to capture in our previous 2D calculation. We ﬁnd the 3D transition temperature at quarter-ﬁlling and U = − 4 t to be T c = 0 . 207 t . The 3D critical regime is much narrower than in 2D and the ratio of the mean-ﬁeld transition to T c is about 5 times smaller than in 2D. We also ﬁnd that, for the parameters we consider, the pseudogap regime in 3D (as in 2D) coincides with the critical scaling regime.
A MISSION TO EXPLORE THE PIONEER ANOMALY

AbstractThe Pioneer 10 and 11 spacecraft yielded the mostprecise navigation in deep space to date. These spacecrafthad exceptional acceleration sensitivity. However, analysisof their radio-metric tracking data has consistently indi-cated that at heliocentric distances of ∼20–70 astronomi-cal units, the orbit determinations indicated the presenceof asmall, anomalous,Dopplerfrequency drift. The drift isa blue-shift, uniformly changing with a rate of ∼ (5.99 ±0.01) × 10 −9 Hz/s, which can be interpreted as a con-stant sunward acceleration of each particular spacecraftof a P = (8.74±1.33)×10 −10 m/s 2 (Anderson et al. 1998;Turyshev et al. 1999; Anderson et al. 2002a). The natureof this anomaly remains unexplained. This signal has be-come known as the Pioneer anomaly.The inability to explain the anomalous behavior ofthe Pioneers with conventional physics has contributedto growing discussion about its origin. There is now anincreasing number of proposals that attempt to explainthe anomaly outside conventional physics. This progressemphasizes the need for a new experiment to explore thedetected signal. Furthermore, the recent extensive eﬀortsled to the conclusion that only a dedicated experimentcould ultimately determine the nature of the found signal.We discuss the Pioneer anomaly and present the nextsteps towards an understanding of its origin. We speciﬁ-cally focus on the development of a mission to explore thePioneer Anomaly in a dedicated experiment conducted indeep space. This joint European-US mission is motivatedby the desire to better understand the laws of fundamen-tal physics as they aﬀect dynamics in the solar system.The mission could lead to a major discovery in the 21stcentury and, with readily available technologies, it couldbe ﬂown well within the Cosmic Vision time frame.Key words: Fundamental physics, Pioneer anomaly, solarsystem dynamics, deep space navigation, gravitation1. BackgroundThe exploration of the solar system’s frontiers - the regionbetween 25-250 astronomical units (AU) from the Sun -is a most ambitious and exciting technological challenge.The scientiﬁc goals for possible deep-space missions arewell-recognized and include studies of the gas and dustdistributions, exploration of the heliopause and the spacebeyond, measurements of the magnetic ﬁelds and particleﬂuxes, studies of the Oort Cloud and Kuiper Belt Objects,encounters with distant bodies, and investigation of thedynamical background of the solar system by studying
Infrared CO emission from young stars : high-resolution spectroscopy

We have detected the high-density, high-temperature, neutral material within 10-200 R ○. of five young stars through high-resolution (20-40 km s −1 ) spectroscopy of the first overtone bands of CO at 2.3 μm. We find a remarkable diversity in the band head profiles toward these sources, ranging from distinctly double-peaked (DG Tau), through broad bumps with emission extending up to 200 km s −1 from the stellar velocity (WL 16, NGC 2024 IRS 2, and S106 IRS 4), to narrow lines having a FWHM velocity of ∼50 km s −1 (SVS 13)
A parallel high-throughput approach to liquid crystal screening

A technique has been developed for the high-throughput (HT) parallel screening of liquid crystal (LC) phase transitions, using optical anisotropic effects observed only in the LC state to allow the determination of melting and clearing points. A camera was used to monitor optical changes observed in arrays of LC samples upon heating, when illuminated with plane polarized light and viewed through a second polarizer aligned perpendicular to the plane of polarized light. Data was processed using Image Pro Plus, extracting values for the melting point and clearing point of each sample in the array. When compared with literature and conventional differential scanning calorimetry the new technique was found to be in excellent agreement, establishing the technique as a viable HT alternative. The method was used to analyze a 75 formulation library prepared using liquid handling for HT clearing point determination, showing the scope and power of the technique in the analysis of larger libraries.
Link between brightest cluster galaxy properties and large scale extensions of 38 DAFT/FADA and CLASH clusters in the redshift range 0.2 < z < 0.9

Context. In the context of large-scale structure formation, clusters of galaxies are located at the nodes of the cosmic web, and continue to accrete galaxies and groups along filaments. In some cases, they show a very large extension and a preferential direction. Brightest cluster galaxies (BCGs) are believed to grow through the accretion of many small galaxies, and their structural properties are therefore expected to vary with redshift. In some cases BCGs show an orientation comparable to that of the cluster to which they belong. Aims. We analyse the morphological properties of 38 BCGs from the DAFT/FADA and CLASH surveys, and compare the position angles of their major axes to the direction of the cluster elongation at large scale (several Mpc). Methods. The morphological properties of the BCGs were studied by applying the GALFIT software to HST images and fitting the light distribution with one or two Sérsic laws, or with a Nuker plus a Sérsic law. The cluster elongations at very large scale were estimated by computing density maps of red sequence galaxies. Results. The morphological analysis of the 38 BCGs shows that in 11 cases a single Sérsic law is sufficient to account for the surface brightness, while for all the other clusters two Sérsic laws are necessary. In five cases, a Nuker plus a Sérsic law give a better fit. For the outer Sérsic component, the effective radius increases with decreasing redshift, and the effective surface brightness decreases with effective radius, following the Kormendy law. An agreement between the major axis of the BCG and the cluster elongation at large scale within ±30 deg is found for 12 clusters out of the 21 for which the PAs of the BCG and of the large-scale structure can be defined. Conclusions. The variation with redshift of the effective radius of the outer Sérsic component agrees with the growing of BCGs by accretion of smaller galaxies from z = 0.9 to 0.2, and it would be interesting to investigate this variation at higher redshift. The directions of the elongations of BCGs and of their host clusters and large scale structures surrounding them agree for 12 objects out of 21, implying that a larger sample is necessary to reach more definite conclusions.
Subleading Poles in the Numerical Unitarity Method at Two Loops

We describe the unitarity approach for the numerical computation of two-loop integral coefficients of scattering amplitudes. It is well known that the leading propagator singularities of an amplitude's integrand are related to products of tree amplitudes. At two loops, Feynman diagrams with doubled propagators appear naturally, which lead to subleading pole contributions. In general, it is not known how these contributions can be directly expressed in terms of a product of on-shell tree amplitudes. We present a universal algorithm to extract these subleading pole terms by releasing some of the on-shell conditions. We demonstrate the new approach by numerically computing two-loop four-gluon integral coefficients.
Colimits of algebras revisited

It has “been open for some time whether, given an algebraic theory (triple, monad) Π in a cocomplete category K, also the category KΠ of Π-algebras must be cocomplete. We solve this in the negative by exhibiting a free algebraic theory Π in the category Gra of graphs such that GraΠ is not cocomplete. Further, we improve somewhat the well-known colimit theorem of Barr and Linton by showing that the base category need not be complete.
Pre-Matching Circuit for High-Frequency Ultrasound Transducers

High-frequency ultrasound transducers offer higher spatial resolution than low-frequency ultrasound transducers; however, their maximum sensitivity are lower. Matching circuits are commonly utilized to increase the amplitude of high-frequency ultrasound transducers because the size of the piezoelectric material decreases as the operating frequency of the transducer increases. Thus, it lowers the limit of the applied voltage to the piezoelectric materials. Additionally, the electrical impedances of ultrasound transducers generally differ at the resonant-, center-, and anti-resonant-frequencies. The currently developed most-matching circuits provide electrical matching at the center frequency ranges for ultrasound transmitters and transducers. In addition, matching circuits with transmitters are more difficult to use to control the echo signal quality of the transducers because it is harder to control the bandwidth and gain of an ultrasound transmitter working in high-voltage operation. Therefore, we provide a novel pre-matching circuit method to improve the amplitude and bandwidth of high-frequency ultrasound transducers at the resonant-, center-, and anti-resonant-frequency ranges, with an ultrasound receiver and transducer. To verify the pre-matching circuit, pulse-echo response tests were conducted on the ultrasound transducers. The results show that the designed pre-matching circuits provide higher amplitude (5.63- and 2.02-times) and wider bandwidth (175.55% and 62.01%) for the high-frequency ultrasound transducer compared to the original circuit without a pre-matching circuit, and the parallel capacitor with a series-inductor circuit, respectively; therefore, the proposed pre-matching circuit is an appropriate solution for improving the amplitudes and bandwidths of high-frequency ultrasound transducers over wide frequency ranges.