Miracle-dz/UniFAR-FTUs huggingface dataset:
Mechanisms of Axon Growth and Regeneration: Moving between Development and Disease

Axons differ in their growth potential: whereas during development, axons rapidly grow to their targets, in the adult mammalian, CNS axons have lost their ability to grow and therefore fail to regenerate. Recent progress has enabled a better understanding of how developmental mechanisms direct axon regeneration. Focusing on neuronal polarization, where one neurite is singled out to become the axon, has uncovered the mechanisms initiating axon growth and growth restraint. This has helped to define the processes that need to be reactivated to induce axon regeneration: microtubule stabilization and actin dynamics. The molecular machinery underlying axon growth and axon regeneration is remarkably similar and includes the Rho-GTPases Cdc42, Rac-1, and RhoA, as well as the actin regulators cofilin and Myosin II. Importantly, neuron-intrinsic growth inhibitors in the adult nervous system, including the voltage-gated calcium channel subunit α2δ2 and the presynaptic active zone protein Munc13, restrain dynamics while the components driving axon growth remain largely present. The identified molecules suggest that synaptic transmission and axon growth may be processes that exclude each other. As a result, axon regeneration may be hampered by synaptic transmission and, thus, by the maturation of the CNS. This research has led to several translational avenues to induce axon regeneration and functional recovery after spinal cord injury and stroke; these include the drugs epothilones, gabapentinoids, and baclofen. Thus, the investigation of axon growth and regeneration side by side has been instrumental to coax the regenerative potential of the CNS.
Quantum ultracold atomtronics

It is known that a semiclassical analysis is not always adequate for atomtronics devices, but that a fully quantum analysis is often necessary to make reliable predictions. While small numbers of atoms at a small number of sites are tractable using the density matrix, a fully quantum analysis is often not straightforward as the system becomes larger. We show that the fully quantum positive-P representation is then a viable calculational tool. We postulate an atomtronic phase gate consisting of four wells in a Bose-Hubbard configuration, for which the semiclassical dynamics are controllable using the phase of the atomic mode in one of the wells. We show that the quantum predictions of the positive-P representation for the performance of this device have little relation to those found semiclassically, and that the performance depends markedly on the actual quantum states of the initially occupied modes. We find that initial coherent states lead to closest to classical dynamics, but that initial Fock states give results that are quite different. A fully quantum analysis also opens the door for deeply quantum atomtronics, in which properties such as entanglement and Einstein-Podolsky-Rosen steering become valuable technical attributes of a device.
Scanamorphos: A Map-making Software for Herschel and Similar Scanning Bolometer Arrays

Scanamorphos is public software available to postprocess scan observations performed with the Herschel photometer arrays. This postprocessing mainly consists in subtracting the total low-frequency noise (both its thermal and nonthermal components), masking high-frequency artefacts such as cosmic ray hits, and projecting the data onto a map. Although it was developed for Herschel, it is also applicable with minimal adjustment to scan observations made with some other imaging arrays subjected to low-frequency noise, provided they entail sufficient redundancy; it was successfully applied to P-Artémis, an instrument operating on the APEX telescope. Contrary to matrix-inversion softwares and high-pass filters, Scanamorphos does not assume any particular noise model, and does not apply any Fourier-space filtering to the data, but is an empirical tool using purely the redundancy built in the observations—taking advantage of the fact that each portion of the sky is sampled at multiple times by multiple bolometers. It is an interactive software in the sense that the user is allowed to optionally visualize and control results at each intermediate step, but the processing is fully automated. This paper describes the principles and algorithm of Scanamorphos and presents several examples of application.
Revealing a new region of gamma-ray emission in the vicinity of HESS J1825–137

HESS J1825–137 is a bright very high-energy gamma-ray source that has been firmly established as a pulsar wind nebula (PWN), and one of the most extended gamma-ray objects within this category. The progenitor supernova remnant (SNR) for this PWN has not been firmly established. We carried out an analysis of gamma-ray observations in the region of HESS J1825–137 with the Fermi–LAT that reveals emission in the direction away from the Galactic plane. The region lies beyond the PWN and reaches a distance from the pulsar compatible with the supposed location of the SNR shock front. The spectrum of the gamma-rays is hard with a photon index of ∼1.9 in the 10–250 GeV range. Several scenarios for the origin of the emission are discussed, including the SNR as a source of high-energy particles and the ‘leakage’ of leptons from the PWN.
High order dark wavefront sensing simulations

Dark wavefront sensing takes shape following quantum mechanics concepts in which one is able to “see” an object in one path of a two-arm interferometer using an as low as desired amount of light actually “hitting” the occulting object. A theoretical way to achieve such a goal, but in the realm of wavefront sensing, is represented by a combination of two unequal beams interferometer sharing the same incoming light, and whose difference in path length is continuously adjusted in order to show different signals for different signs of the incoming perturbation. Furthermore, in order to obtain this in white light, the path difference should be properly adjusted vs the wavelength used. While we incidentally describe how this could be achieved in a true optomechanical setup, we focus our attention to the simulation of a hypothetical “perfect” dark wavefront sensor of this kind in which white light compensation is accomplished in a perfect manner and the gain is selectable in a numerical fashion. Although this would represent a sort of idealized dark wavefront sensor that would probably be hard to match in the real glass and metal, it would also give a firm indication of the maximum achievable gain or, in other words, of the prize for achieving such device. Details of how the simulation code works and first numerical results are outlined along with the perspective for an in-depth analysis of the performances and its extension to more realistic situations, including various sources of additional noise.
Gravitational-Wave Detection using Multivariate Analysis

Searches for gravitational-wave bursts (transient signals, typically of unknown waveform) require identification of weak signals in background detector noise. The sensitivity of such searches is often critically limited by non-Gaussian noise fluctuations which are difficult to distinguish from real signals, posing a key problem for transient gravitational-wave astronomy. Current noise rejection tests are based on the analysis of a relatively small number of measured properties of the candidate signal, typically correlations between detectors. Multivariate analysis (MVA) techniques probe the full space of measured properties of events in an attempt to maximise the power to accurately classify events as signal or background. This is done by taking samples of known background events and (simulated) signal events to train the MVA classifier, which can then be applied to classify events of unknown type. We apply the boosted decision tree (BDT) MVA technique to the problem of detecting gravitational-wave bursts associated with gamma-ray bursts. We find that BDTs are able to increase the sensitive distance reach of the search by as much as 50%, corresponding to a factor of ~3 increase in sensitive volume. This improvement is robust against trigger sky position, large sky localisation error, poor data quality, and the simulated signal waveforms that are used. Critically, we find that the BDT analysis is able to detect signals that have different morphologies to those used in the classifier training and that this improvement extends to false alarm probabilities beyond the 3{\sigma} significance level. These findings indicate that MVA techniques may be used for the robust detection of gravitational-wave bursts with a priori unknown waveform.
Andreev reflection from noncentrosymmetric superconductors and Majorana bound-state generation in half-metallic ferromagnets

We study Andreev reflection at an interface between a half metal and a superconductor with spin-orbit interaction. While the absence of minority carriers in the half metal makes singlet Andreev reflection impossible, the spin-orbit interaction gives rise to triplet Andreev reflection (i.e., the reflection of a majority electron into a majority hole or vice versa). As an application of our calculation, we consider a thin half-metal film or wire laterally attached to a superconducting contact. If the half metal is disorder free, an excitation gap is opened that is proportional to the spin-orbit interaction strength in the superconductor. For electrons with energy below this gap a lateral half-metal--superconductor contact becomes a perfect triplet Andreev reflector. We show that the system supports localized Majorana end states in this limit.
THE CURIOUS MORPHOLOGY AND ORIENTATION OF ORION PROPLYD HST-10

HST-10 is one of the largest proplyds in the Orion Nebula and is located approximately 1′ SE of the Trapezium. Unlike other proplyds in Orion, however, the long-axis of HST-10 does not align with θ1 C, but is instead aligned with the rotational axis of the HST-10 disk. This cannot be easily explained using current photoevaporation models. In this Letter, we present high spatial resolution near-infrared images of the Orion proplyd HST-10 using Keck/NIRC2 with the Laser Guide Star Adaptive Optics system, along with multi-epoch analysis of HH objects near HST-10 using Hubble Space Telescope (HST) WFPC2 and Advanced Camera for Surveys cameras. Our narrowband near-IR images resolve the proplyd ionization front (IF) and circumstellar disk down to 23 AU at the distance to Orion in Br γ, He i, H2, and polycyclic aromatic hydrocarbon (PAH) emission. Br γ and He i emission primarily trace the IF (with the disk showing prominently in silhouette), while the H2 and PAH emission trace the surface of the disk itself. PAH emission also traces small dust grains within the proplyd envelope which is asymmetric and does not coincide with the IF. The curious morphology of the PAH emission may be due to UV heating by both θ1 COri and θ2 AOri. Multi-epoch HST images of the HST-10 field show proper motion of three knots associated with HH 517, clearly indicating that HST-10 has a jet. We postulate that the orientation of HST-10 is determined by the combined ram pressure of this jet and the FUV-powered photo-ablation flow from the disk surface.
DISCOVERY OF A SUPER-Li-RICH TURNOFF STAR IN THE METAL-POOR GLOBULAR CLUSTER NGC 6397

We report on the discovery of a super-Li-rich turnoff (TO) star in the old (12 Gyr), metal-poor ([Fe/H] = −2.1 dex) globular cluster (GC) NGC 6397, based on high-resolution MIKE/Magellan spectra. This star shows an unusually high lithium abundance of A(Li)NLTE = 4.03 ± 0.06 ± 0.14 dex (or, 4.21, accounting for possible contamination from a binary companion) that lies above the canonical Li-plateau by a factor of 100. This is the highest Li enhancement found in a Galactic GC dwarf star to date. We discuss several enhancement mechanisms, but none can unambiguously explain such a high overabundance. The spectrum of the star shows a possible indication of binarity, but its line strengths and chemical element abundance ratios are fully compatible with other TO stars in this GC, seemingly ruling out mass transfer from an asymptotic giant branch companion as origin of the high A(Li). A possible cause is an interaction with a red giant that has undergone cool bottom processing.
Energy-Dispersive X-Ray Spectrum Simulation with NIST DTSA-II: Comparing Simulated and Measured Electron-Excited Spectra

Abstract Electron-excited X-ray microanalysis with energy-dispersive spectrometry (EDS) proceeds through the application of the software that extracts characteristic X-ray intensities and performs corrections for the physics of electron and X-ray interactions with matter to achieve quantitative elemental analysis. NIST DTSA-II is an open-access, fully documented, and freely available comprehensive software platform for EDS quantification, measurement optimization, and spectrum simulation. Spectrum simulation with DTSA-II enables the prediction of the EDS spectrum from any target composition for a specified electron dose and for the solid angle and window parameters of the EDS spectrometer. Comparing the absolute intensities for measured and simulated spectra reveals correspondence within ±25% relative to K-shell and L-shell characteristic X-ray peaks in the range of 1–11 keV. The predicted M-shell intensity exceeds the measured value by a factor of 1.4–2.2 in the range 1–3 keV. The X-ray continuum (bremsstrahlung) generally agrees within ±10% over the range of 1–10 keV. Simulated EDS spectra are useful for developing an analytical strategy for challenging problems such as estimating trace detection levels.
Domain-specific model differencing for graphical domain-specific languages

The evolution of models as a result of collaborative effort must be tracked and maintained. The usage of text-based version control systems is ubiquitous, however, it does not assist domain users in comprehending the semantics of model differences. To overcome these concerns, we propose ---called DSMCompare---, a complete solution. It considers both the abstract and concrete syntax of a domain-specific language (DSL) to express model differences and facilitates the definition of domain-specific semantics for specific difference patterns. The method extends the DSL automatically to allow for the description of modifications and adapts its graphical concrete syntax to visualize the differences. It moreover enables the creation of semantic differencing rules for identifying recurrent domain-specific difference patterns. Because these rules may conflict with one another, we provide algorithms for resolving conflicts and scheduling rules. We report on evaluations based on synthetic models and version histories of models provided by third parties to illustrate the applicability and effectiveness of our approach. We also outline an extension of DSMCompare to three-way differencing.
The path towards the automatic provision of blended modeling environments

Blended modeling aims to enhance the development of complex software-intensive systems by seamless integration of textual and graphical modeling. Manual provision of the synchronization transformations between notations is considered to be a tedious and error-prone task. Moreover, as synchronized languages and/or notations evolve, transformations become redundant as the implicit mappings they represent are no longer accurate. This research proposes a language- and notation-agnostic solution for the automatic generation of synchronization transformations between arbitrary domain-specific modeling languages. We contribute with i) a mapping modeling language defined appositely for the definition of explicit mapping rules in a mapping model and ii) higher-order transformations for the automatic generation of synchronization transformations driven by mapping models. The approach is successfully validated against two use cases.
Dynamic adaptation for distributed systems in model-driven engineering

Modern-day software systems operate within complex, uncertain, and highly dynamic environments. Managing such systems is a significant challenge; developing self-managing autonomic systems is one way to reduce development and maintenance efforts. In the context of distributed systems, achieving this autonomy through dynamic adaptation is particularly challenging due to the volatile host environment. Model-Driven Engineering (MDE) is a software development paradigm that advocates the use of models as the primary artifacts rather than source code. MDE promises higher-quality software at a lower cost through abstractions, automation, and analyses. The goal of our work is to leverage MDE to facilitate the development and maintenance of distributed applications with dynamic adaptation capabilities. We assume that the structure and behavior of the application has been modeled using the Component-and-Connector (C&C) paradigm and the 'Monitor-Analyze-Plan-Execute with shared Knowledge' (MAPE-K) reference architecture. In the initial work, we have developed a model-level monitoring infrastructure, and adapted existing code generation and deployment support to generate a distributed system from the C&C models and deploy it automatically on a suitable platform. In future work, we plan to investigate how the monitoring and adaptation capabilities of cloud-native containerization and orchestration platforms (i.e., Docker and Kubernetes) can be leveraged for dynamic adaptation, and how this system-level adaptation can be combined effectively with any model-level monitoring, planning, and adaptation capabilities.
Quasars in the Galactic Anti-Center Area from LAMOST DR3

We present a sample of quasars discovered in an area near the Galactic Anti-Center covering 150°≤l≤210° and ∣b∣≤30°, based on LAMOST Data Release 3 (DR3). This sample contains 151 spectroscopically confirmed quasars. Among them 80 are newly discovered with LAMOST. All these quasars are very bright, with i magnitudes peaking around 17.5 mag. All the new quasars were discovered serendipitously from objects that were originally targeted with LAMOST as stars having bluer colors, except for a few candidates targeted as variable, young stellar objects. This bright quasar sample at low Galactic latitudes will help fill the gap in the spatial distribution of known quasars near the Galactic disk that are used to construct an astrometric reference frame for the purpose of accurate proper motion measurements that can be applied to, for example, Gaia. They are also excellent tracers to probe the kinematics and chemistry of the interstellar medium in the Milky Way disk and halo via absorption line spectroscopy.
Semi-supervised pre-processing for learning-based traceability framework on real-world software projects

The traceability of software artifacts has been recognized as an important factor to support various activities in software development processes. However, traceability can be difficult and time-consuming to create and maintain manually, thereby automated approaches have gained much attention. Unfortunately, existing automated approaches for traceability suffer from practical issues. This paper aims to gain an understanding of the potential challenges for the underperforming of the state-of-the-art, ML-based trace link classifiers applied in real-world projects. By investigating different industrial datasets, we found that two critical (and classic) challenges, i.e. data imbalance and sparse problems, lie in real-world projects’ traceability automation. To overcome these challenges, we developed a framework called SPLINT to incorporate hybrid textual similarity measures and semi-supervised learning strategies as enhancements to the learning-based traceability approaches. We carried out experiments with six open-source platforms and ten industry datasets. The results confirm that SPLINT is able to operate at higher performance on two communities’ datasets. Specifically, the industrial datasets, which significantly suffer from data imbalance and sparsity problems, show an increase in F2-score over 14% and AUC over 8% on average. The adjusted class-balancing and self-training policies used in SPLINT (CBST-Adjust) also work effectively for the selection of pseudo-labels on minor classes from unlabeled trace sets, demonstrating SPLINT’s practicability.
Understanding automated code review process and developer experience in industry

Code Review Automation can reduce human efforts during code review by automatically providing valuable information to reviewers. Nevertheless, it is a challenge to automate the process for large-scale companies, such as Samsung Electronics, due to their complexity: various development environments, frequent review requests, huge size of software, and diverse process among the teams. In this work, we show how we automated the code review process for those intricate environments, and share some lessons learned during two years of operation. Our unified code review automation system, Code Review Bot, is designed to process review requests holistically regardless of such environments, and checks various quality-assurance items such as potential defects in the code, coding style, test coverage, and open source license violations. Some key findings include: 1) about 60% of issues found by Code Review Bot were reviewed and fixed in advance of product releases, 2) more than 70% of developers gave positive feedback about the system, 3) developers rapidly and actively responded to reviews, and 4) the automation did not much affect the amount or the frequency of human code reviews compared to the internal policy to encourage code review activities. Our findings provide practical evidence that automating code review helps assure software quality.
Erratum: Multiplicity of disc-bearing stars in Upper Scorpius and Upper Centaurus-Lupus

We present observations of disc-bearing stars in Upper Scorpius (US) and Upper Centaurus-Lupus (UCL) with moderate resolution spectroscopy in order to determine the influence of multiplicity on disc persistence after ${\sim }5\hbox{--}20\, \mathrm{Myr}$. Discs were identified using infrared (IR) excess from the Wide-field Infrared Survey Explorer (WISE) survey. Our survey consists of 55 US members and 28 UCL members, using spatial and kinematic information to assign a probability of membership. Spectra are gathered from the ANU 2.3 m telescope using the Wide Field Spectrograph (WiFeS) to detect radial velocity variations that indicate the presence of a companion. We identify two double-lined spectroscopic binaries, both of which have strong IR excess. We find the binary fraction of disc-bearing stars in US and UCL for periods up to 20 yr to be $0.06^{+0.07}_{-0.02}$ and $0.13^{+0.06}_{-0.03}$, respectively. Based on the multiplicity of field stars, we obtain an expected binary fraction of ${\sim }0.12^{+0.02}_{-0.01}$. The determined binary fractions for disc-bearing stars do not vary significantly from the field, suggesting that overall lifetime of discs may not differ between single and binary star systems.