Miracle-dz/UniFAR-FTUs huggingface dataset:
Pressure dependence of upper critical fields in FeSe single crystals

We investigate the pressure dependence of the upper critical fields (μ0Hc2) for FeSe single crystals with pressure up to 2.57 GPa. The superconducting (SC) properties show a disparate behavior across a critical pressure where the pressure-induced antiferromagnetic phase coexists with superconductivity. The magnetoresistance for H//ab and H//c is very different: for H//c, magnetic field induces and enhances a hump in the resistivity close to the Tc for pressures higher than 1.2 GPa, while it is absent for H//ab. Since the measured μ0Hc2 for FeSe samples is smaller than the orbital limited upper critical field ( H orb c 2 ) ? > estimated by the Werthamer, Helfand and Hohenberg model, the Maki parameter (α) related to Pauli spin-paramagnetic effects is additionally considered to describe the temperature dependence of μ0Hc2(T). Interestingly, the α value is hardly affected by pressure for H//ab, while it strongly increases with pressure for H//c. The pressure evolution of the μ0Hc2(0) for the FeSe single crystals is found to be almost similar to that of Tc(P), suggesting that the pressure-induced magnetic order adversely affects the upper critical fields as well as the SC transition temperature.
High-resolution Hubble Space Telescope Imaging Survey of Local Star-forming Galaxies. I. Spatially Resolved Obscured Star Formation with Hα and Paschen-β Recombination Lines

We present a sample of 24 local star-forming galaxies observed with broadband and narrowband photometry from the Hubble Space Telescope (HST) that are part of the Great Observatories All-sky Luminous Infrared Galaxies Survey of local luminous and ultraluminous infrared galaxies. With narrowband filters around the emission lines Hα (and [N ii]) and Paβ, we obtain robust estimates of the dust attenuation affecting the gas in each galaxy, probing higher attenuation than can be traced by the optical Balmer decrement Hα/Hβ alone by a factor of >1 mag. We also infer the dust attenuation toward the stars via a spatially resolved spectral energy distribution fitting procedure that uses all available HST imaging filters. We use various indicators to obtain the star formation rate (SFR) per spatial bin and find that Paβ traces star-forming regions where the Hα and the optical stellar continuum are heavily obscured. The dust-corrected Paβ SFR recovers the 24 μm inferred SFR with a ratio of −0.14 ± 0.32 dex and the SFR inferred from the 8 to 1000 μm infrared luminosity at −0.04 ± 0.23 dex. Both in a spatially resolved and integrated sense, rest-frame near-infrared recombination lines can paint a more comprehensive picture of star formation across cosmic time, particularly with upcoming JWST observations of Paschen-series line emission in galaxies as early as the epoch of reionization.
SARCS strong-lensing galaxy groups - II. Mass-concentration relation and strong-lensing bias

Our work is based on the stacked weak-lensing analysis of a sample of 80 strong-lensing galaxy groups. Our main results are the following: (i) the lensing signal does not allow us to firmly reject a simple singular isothermal sphere mass distribution compared to the expected NFW mass profile; (ii) we obtain an average concentration $c_{200}=8. 6_{-1.3}^{+2.1}$ that is much higher than the expected value from numerical simulations for the corresponding average mass $M_{200}=0. 73_{-0.10}^{+0.11}\times10^{14}\mathrm{M_{\odot}}$; (iii) the combination of our results with those at larger mass scales gives a mass-concentration relation $c(M)$ over nearly two decades in mass, with a slope in disagreement with predictions from numerical simulations using unbiased populations of dark matter haloes; (iv) our combined $c(M)$ relation matches results from simulations using only haloes with a large strong-lensing cross section, i.e. elongated with a major axis close to the line of sight; (v) for the simplest case of prolate haloes, we estimate with a toy model a lower limit on the minor:major axis ratio $a/c=0.5$ for the average SARCS galaxy group. Our analysis based on galaxy groups confirmed the results obtained at larger mass scales: strong lenses present apparently too large concentrations, which can be explained by triaxial haloes preferentially oriented with the line of sight. Because more massive systems already have large lensing cross sections, they do not require a large elongation along the line of sight, contrary to less massive galaxy groups. Therefore, it is natural to observe larger lensing (projected) concentrations for such systems, resulting in an overall mass-concentration relation steeper than that of non-lensing haloes.
A Strong Transfer Baseline for RGB-D Fusion in Vision Transformers

—The Vision Transformer (ViT) architecture has recently established its place in the computer vision literature, with multiple architectures for recognition of image data or other visual modalities. However, training ViTs for RGB-D object recognition remains an understudied topic, viewed in recent literature only through the lens of multi-task pretraining in multiple modalities. Such approaches are often computationally intensive and have not yet been applied for challenging object-level classiﬁcation tasks. In this work, we propose a simple yet strong recipe for transferring pretrained ViTs in RGB-D domains for single-view 3D object recognition, focusing on fusing RGB and depth representations encoded jointly by the ViT. Compared to previous works in multimodal Transformers, the key challenge here is to use the atested ﬂexibility of ViTs to capture cross-modal interactions at the downstream and not the pretraining stage. We explore which depth representation is better in terms of resulting accuracy and compare two methods for injecting RGB-D fusion within the ViT architecture (i.e., early vs. late fusion). Our results in the Washington RGB- D Objects dataset demonstrates that in such RGB → RGB-D scenarios, late fusion techniques work better than most popularly employed early fusion. With our transfer baseline, adapted ViTs score up to 95.1% top-1 accuracy in Washington, achieving new state-of-the-art results in this benchmark. We additionally evaluate our approach with an open-ended lifelong learning protocol, where we show that our adapted RGB-D encoder leads to features that outperform unimodal encoders, even without explicit ﬁne-tuning. We further integrate our method with a robot framework and demonstrate how it can serve as a perception utility in an interactive robot learning scenario, both in simulation and with a real robot.
Multi-Task Option Learning and Discovery for Stochastic Path Planning

This paper addresses the problem of reliably and efﬁciently solving broad classes of long-horizon stochastic path planning problems. Starting with a vanilla RL formulation with a stochastic dynamics simulator and an occupancy matrix of the environment, our approach computes useful options with policies as well as high-level paths that compose the discovered options. Our main contributions are ( 1 ) data-driven methods for creating abstract states that serve as end points for helpful options, ( 2 ) methods for computing option policies using auto-generated option guides in the form of dense pseudo-reward functions, and ( 3 ) an overarching algorithm for composing the computed options. We show that this approach yields strong guarantees of executability and solvability: under fairly general conditions, the computed option guides lead to composable option policies and consequently ensure downward reﬁnability. Empirical evaluation on a range of robots, environments, and tasks shows that this approach effectively transfers knowledge across related tasks and that it outperforms existing approaches by a signiﬁcant margin.
Polaritonic coherent perfect absorption based on self-hybridization of a quasi-bound state in the continuum and exciton.

Enhancement of light-matter interactions is of great importance for many nanophotonic devices, and one way to achieve it is to feed energy perfectly to the strongly coupled system. Here, we propose gap-perturbed dimerized gratings based on bulk WS2 for flexible control of the strong coupling or self-hybridization of a quasi-bound state in the continuum (quasi-BIC) and exciton. The simulation results show that when a gap perturbation is introduced into the system resulting in the Brillouin zone folding, BIC transforms into quasi-BIC whose quality factor (Q-factor) is related to the value of gap perturbation. The strong coupling results in the anti-crossover behavior of the absorption spectra, and thus a Rabi splitting energy of 0.235 eV is obtained. With the assistance of temporal coupled-mode theory, the conditions for the strong critical coupling are obtained, and finally successful achievement of polaritonic coherent perfect absorption in the proposed system. This work could provide ideas for enhancing light-matter interactions and strong theoretical support for all-optical tuning and modulation.
A multi-wavelength study of the young star V1118 Orionis in outburst

Context. The accretion history of low-mass young stars is not smooth but shows spikes of accretion that can last from months and years to decades and centuries. Aims. Observations of young stars in outbursts can help us understand the temporal evolution of accreting stars and the interplay between the accretion disk and the stellar magnetosphere. Methods. The young late-type star V1118 Orionis was in outburst from 2005 to 2006. We followed the outburst with optical and near-infrared photometry. The X-ray emission was further probed with observations taken with XMM-Newton and Chandra during and after the outburst. In addition, we obtained mid-infrared photometry and spectroscopy withSpitzer at the peak of the outburst and in the post-outburst phase. Results. The spectral energy distribution of V1118 Ori varied significantly over the course of the outburst. The optical flux showed the largest variations, most likely caused by enhanced emission by a hot spot. The hot spot dominated the optical and near-infrared emission at the peak of the outburst, while the disk emission dominated in the mid-infrared. The emission silicate feature in V1118 Ori is flat and does not vary in shape, but was slightly brighter at the peak of the outburst compared to the post-outburst spectrum. The X-ray flux correlated with the optical and infrared fluxes, indicating that accretion a! ected the magnetically active corona and the stellar magnetosphere. The thermal structure of the corona was variable with some indication of a cooling of the coronal temperature in the early phase of the outburst with a gradual return to normal values. Color‐color diagrams in the optical and infrared showed variations during the outburst, with no obvious signature of reddening caused by circumstellar matter. Using Monte-Carlo realizations of star+disk+hotspot models to fit the spectral energy distributions in “quiescence” and at the peak of the outburst, we determined that the mass accretion rate varied from about 2.5" 10 # 7 M$ yr # 1 to 1.0" 10 # 6 M$ yr # 1 ; in addition, the fractional area of the hotspot increased significantly. Conclusions. The multi-wavelength study of the V1118 Ori outburst helped us to understand the variations in spectral energy distributions and demonstrated the interplay between the disk and the stellar magnetosphere in a young, strongly accreting star.
Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST

We investigate the potential of using a sample of very high-redshift (2 ≲ z ≲ 6) (VHZ) Type Ia supernovae (SNe Ia) attainable by JWST on constraining cosmological parameters. At such high redshifts, the age of the universe is young enough that the VHZ SN Ia sample comprises the very first SNe Ia of the universe, with progenitors among the very first generation of low-mass stars that the universe has made. We show that the VHZ SNe Ia can be used to disentangle systematic effects due to the luminosity distance evolution with redshifts intrinsic to SN Ia standardization. Assuming that the systematic evolution can be described by a linear or logarithmic formula, we found that the coefficients of this dependence can be determined accurately and decoupled from cosmological models. Systematic evolution as large as 0.15 mag and 0.45 mag out to z = 5 can be robustly separated from popular cosmological models for linear and logarithmic evolution, respectively. The VHZ SNe Ia will lay the foundation for quantifying the systematic redshift evolution of SN Ia luminosity distance scales. When combined with SN Ia surveys at comparatively lower redshifts, the VHZ SNe Ia allow for the precise measurement of the history of the expansion of the universe from z ∼ 0 to the epoch approaching reionization.
Robust Person Identification: A WiFi Vision-based Approach

Person re-identification (Re-ID) has become increasingly im-portant as it supports a wide range of security applications. Traditional person Re-ID mainly relies on optical camera-based systems, which incur several limitations due to the changes in the appearance of people, occlusions, and human poses. In this work, we propose a WiFi vision-based system, 3D-ID, for person Re-ID in 3D space. Our system leverages the advances of WiFi and deep learning to help WiFi devices “see”, identify, and recognize people. In particular, we leverage multiple antennas on next-generation WiFi devices and 2D AoA estimation of the signal reflections to enable WiFi to visualize a person in the physical environment. We then leverage deep learning to digitize the visualization of the person into 3D body representation and extract both the static body shape and dynamic walking patterns for person Re-ID. Our evaluation results under various indoor environments show that the 3D-ID system achieves an overall rank-1 accuracy of 85 . 3%. Results also show that our system is resistant to various attacks. The proposed 3D-ID is thus very promising as it could augment or complement camera-based systems.
Radiation protection and shielding materials for crewed missions on the surface of Mars

A potential crewed mission to Mars would require us to solve a number of problems, including how to protect astronauts against the devastating effects of energetic charged particles from Solar and Galactic sources. The radiation environment on Mars is of particular interest, since maintaining optimal absorbed doses by astronauts is crucial to their survival. Here, we give an overview of the conditions on Mars, as determined by theoretical models and in-situ measurements, and present the main proposed strategies to mitigate radiation exposure while on Mars. Specifically, we focus on the passive shielding technique. Several widely used materials, along with some innovative ones and combinations of those, are studied for their behavior against Solar Energetic Particle Events and Galactic Cosmic Rays in the Martian environment. For that purpose, we implement the GEANT4 package, a Monte-Carlo numerical model developed by CERN, which is specifically applied to simulate interactions of radiation with matter. A description of our model will be given, followed by outputs of the numerical model. We conclude that hydrogen-rich materials act as better attenuators, as expected, but other materials can be helpful against cosmic rays too.
A Combinatorial Perspective on the Optimization of Shallow ReLU Networks

The NP-hard problem of optimizing a shallow ReLU network can be characterized as a combinatorial search over each training example's activation pattern followed by a constrained convex problem given a fixed set of activation patterns. We explore the implications of this combinatorial aspect of ReLU optimization in this work. We show that it can be naturally modeled via a geometric and combinatoric object known as a zonotope with its vertex set isomorphic to the set of feasible activation patterns. This assists in analysis and provides a foundation for further research. We demonstrate its usefulness when we explore the sensitivity of the optimal loss to perturbations of the training data. Later we discuss methods of zonotope vertex selection and its relevance to optimization. Overparameterization assists in training by making a randomly chosen vertex more likely to contain a good solution. We then introduce a novel polynomial-time vertex selection procedure that provably picks a vertex containing the global optimum using only double the minimum number of parameters required to fit the data. We further introduce a local greedy search heuristic over zonotope vertices and demonstrate that it outperforms gradient descent on underparameterized problems.
Radio emission of the Moon before and after the Lunar Prospector impact

The direct impact of the American spacecraft Lunar Prospector into the Moon on July 31, 1999 was accompanied by seismic effects comparable to a big moonquake. Such an impact can be accompanied by radio seismic radiation of the lunar surface layers. For registration of the lunar radio seismic radiation after the Lunar Prospector impact radio observations of the Moon on two 64-m radio telescopes at 13, 21, and 90 cm were conducted on July 30 - August 2, 1999. Changes of the radio temperature of the south polar regions after the impact were detected. The Lunar Prospector impact may have been the cause of these changes. Recommendations about the registration of the lunar radio seismic radiation during the Leonid meteor showers are given.
Co-axial metrics on the sphere and algebraic numbers

In this paper, we study properties of the set of tuples (t_1,.t_n) such that a conical metric of constant curvature 1 with conic singularities at t_1,. ,t_n with prescribed angles exists on the Riemann sphere and the monodromy group of its developing map is isomorphic to a subgroup of the unit circle.
Adult survivors of a first primary invasive cancer had increased risk for cardiovascular disease

SOURCE CITATION Florido R, Daya NR, Ndumele CE, et al. Cardiovascular disease risk among cancer survivors: the Atherosclerosis Risk In Communities (ARIC) study. J Am Coll Cardiol. 2022;80:22-32. 35772913.
THE DEEP LOOK AT THE HARD X-RAY SKY: THE SWIFT–INTEGRAL X-RAY (SIX) SURVEY

The supermassive black holes at the center of active galactic nuclei (AGNs) are surrounded by obscuring matter that can block nuclear radiation. Depending on the amount of blocked radiation, the flux from the AGN can be too faint to be detected by currently flying hard X-ray (above 15 keV) missions. At these energies only ∼1% of the intensity of the cosmic X-ray background (CXB) can be resolved into point-like sources that are AGNs. In this work, we address the question of undetected sources contributing to the CXB with a very sensitive and new hard X-ray survey: the Swift–INTEGRAL X-ray survey, which is obtained with the new approach of combining the Swift/BAT and INTEGRAL/IBIS X-ray observations. We merge the observations of both missions, which enhances the exposure time and reduces systematic uncertainties. As a result, we obtain a new survey over a wide sky area of 6200 deg2 that is more sensitive than the surveys of Swift/BAT or INTEGRAL/IBIS alone. Our sample comprises 113 sources: 86 AGNs (Seyfert-like and blazars), 5 galaxies, 2 clusters of galaxies, 3 Galactic sources, 3 previously detected unidentified X-ray sources, and 14 unidentified sources. The scientific outcome from the study of the sample has been properly addressed to study the evolution of AGNs at redshift below 0.4. We do not find any evolution using the 1/Vmax method. Our sample of faint sources is a suitable target for the new generation hard X-ray telescopes with focusing techniques.
Wait a second! Assessing the impact of different desktop push notification types on software developers

Push notifications, which are at the core of most modern productivity and social tools, come in different shapes and sizes - all competing for one’s attention while creating the illusion of multitasking. At best, a notification may intervene in support of a primary task (e.g., a note about the correct use of a library), and at worst a notification may result in a complete context switch (e.g., answering an urgent and unrelated email). This paper presents a controlled single blind study conducted with 65 software professionals with the aim to further understand how different types of notifications may affect people during an immersive task. Insights are drawn from various angles, including mouse pointer logs, session recordings, temporal measures (e.g., time on task and time to resume task) as well as subjective workload assessments. Results indicate that participants who received either actionable or informational interventions managed to resume their tasks more efficiently than those who received actionable or informational intrusions. Actionable intrusions had a significant impact on overall task duration and levels of perceived effort while informational intrusions, which were largely ignored, had the largest impact on the participant’s ability to resume the task efficiently, which also resulted in high levels of frustration. The time to decide whether to engage with a notification was also a factor that contributed to the overall task duration, and this was particularly noticed when an actionable intervention was presented, resulting in a significant impact on mental demand and perceived performance.
The role of disc self-gravity in circumbinary planet systems – I. Disc structure and evolution

Supported by QMUL Research-IT and funded by EPSRC grant EP/K000128/1; and the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure.
Skyrme pseudo-potential-based EDF parametrization for spuriousity-free MR EDF calculations

First exploratory steps toward a pseudo-potential-based Skyrme energy density functional for spuriousity-free multi-reference calculations are presented. A qualitatively acceptable fit can be accomplished by adding simple three- and four-body contact terms to the standard central plus spin–orbit two-body terms. To achieve quantitative predictive power, higher-order terms, e.g. velocity-dependent three-body terms, will be required.
Numerical investigation of activation energy of radiative magnetohydrodynamic Williamson nanofluid flow

The activation energy (AE) of mixed convective, radiative magnetohydrodynamic Williamson nanofluid flow across an exponentially stretched sheet was investigated numerically. To convert the governing nonlinear partial differential equations into coupled ordinary differential equations, suitable similarity variables were introduced. The “Runge Kutta method” with the procedure of shooting was used to solve the resulting system of nonlinear ordinary differential equations with boundary conditions. The effects of various factors on profiles of nanoparticle volume fraction, temperature, and velocity were explored, and the results were presented graphically. The acquired results show that they are in great agreement with those found in the open literature. It is found that concentration profile is an increasing function of AE E whereas it decreases for chemical reaction rate constant σ* ${\sigma }^{* }$ and temperature difference δ $\delta $ . It is also evident from the table that the local Sherwood number rises as the chemical reaction rate constant and temperature differences arise, and falls as the AE is enhanced.