Miracle-dz/UniFAR-FTUs huggingface dataset:
Bayesian hierarchical modelling for battery lifetime early prediction

Accurate prediction of battery health is essential for real-world system management and lab-based experiment design. However, building a life-prediction model from different cycling conditions is still a challenge. Large lifetime variability results from both cycling conditions and initial manufacturing variability, and this -- along with the limited experimental resources usually available for each cycling condition -- makes data-driven lifetime prediction challenging. Here, a hierarchical Bayesian linear model is proposed for battery life prediction, combining both individual cell features (reflecting manufacturing variability) with population-wide features (reflecting the impact of cycling conditions on the population average). The individual features were collected from the first 100 cycles of data, which is around 5-10% of lifetime. The model is able to predict end of life with a root mean square error of 3.2 days and mean absolute percentage error of 8.6%, measured through 5-fold cross-validation, overperforming the baseline (non-hierarchical) model by around 12-13%.
Coded Distributed Computing with Pre-set Assignments of Data and Output Functions

Coded distributed computing (CDC) can reduce the communication load for distributed computing systems by introducing redundant computation and creating multicasting opportunities. The optimal computation-communication tradeoff has been well studied for homogeneous systems, and some results have been obtained under heterogeneous conditions. However, the existing schemes require delicate data placement and output function assignment, which is not feasible in some practical scenarios when distributed nodes fetch data without the orchestration of a central server. In this paper, we consider the general heterogeneous distributed computing systems where the data placement and output function assignment are arbitrary but pre-set (i.e., cannot be designed by schemes). For this general heterogeneous setup, we propose two coded computing schemes, One-Shot Coded Transmission (OSCT) and Few-Shot Coded Transmission (FSCT), to reduce the communication load. These two schemes first group the nodes into clusters and divide the transmission of each cluster into multiple rounds, and then design coded transmission in each round to maximize the multicast gain. The key difference between OSCT and FSCT is that the former uses a one-shot transmission where each encoded message can be decoded independently by the intended nodes, while the latter allows each node to jointly decode multiple received symbols to achieve potentially larger multicast gains. Furthermore, with theoretical converse proofs, we derive sufficient conditions for the optimality of OSCT and FSCT, respectively. This not only recovers the existing optimality results known for homogeneous systems and 3-node systems, but also includes some cases where our schemes are optimal while other existing methods are not.
Some approaches used to overcome overestimation in Deep Reinforcement Learning algorithms

Some phenomena related to statistical noise which have been investigated by various authors under the framework of deep reinforcement learning (RL) algorithms are discussed. The following algorithms are examined: the deep Q -network (DQN), double DQN, deep deterministic policy gradient (DDPG), twin-delayed DDPG (TD3), and hill climbing algorithm. First, we consider overestimation , which is a harmful property resulting from noise. Then we deal with noise used for exploration , this is the useful noise. We discuss setting the noise parameter in the TD3 for typical PyBullet environments associated with articulate bodies such as HopperBulletEnv and Walker2DBulletEnv. In the appendix, in relation to the hill climbing algorithm, another example related to noise is considered - an example of adaptive noise.
Optimal decoy intensity for decoy quantum key distribution

In the decoy quantum key distribution, we show that a smaller decoy intensity gives a better key generation rate in the asymptotic setting when we employ only one decoy intensity and the vacuum pulse. In particular, the counting rate of single photon can be perfectly estimated in the limit that the decoy intensity is infinitesimally small. The same property holds even when the intensities cannot be perfectly identified. Further, we propose a protocol to improve the key generation rate over the existing protocol under the same decoy intensity.
Characterizing gas flow from aerosol particle injectors

A novel methodology for measuring gas flow from small orifices or nozzles into vacuum is presented. It utilizes a high-intensity femtosecond laser pulse to create a plasma within the gas plume produced by the nozzle, which is imaged by a microscope. Calibration of the imaging system allows for the extraction of absolute number densities. We show detection down to helium densities of $4\times10^{16}$~cm$^{-3}$ with a spatial resolution of a few micrometer. The technique is used to characterize the gas flow from a convergent-nozzle aerosol injector [Struct. \ Dyn. ~2, 041717 (2015)] as used in single-particle diffractive imaging experiments at free-electron laser sources. Based on the measured gas-density profile we estimate the scattering background signal under typical operating conditions of single-particle imaging experiments and estimate that fewer than 50 photons per shot can be expected on the detector.
The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

We measure the color and stellar mass dependence of clustering in spectroscopic galaxies at 0.6 < z < 0.65 using data from the Baryon Oscillation Spectroscopic Survey component of the Sloan Digital Sky Survey. We greatly increase the statistical precision of our clustering measurements by using the cross-correlation of 66,657 spectroscopic galaxies to a sample of 6.6 million fainter photometric galaxies. The clustering amplitude w(R) is measured as the ratio of the mean excess number of photometric galaxies found within a specified radius annulus around a spectroscopic galaxy to that from a random photometric galaxy distribution. We recover many of the familiar trends at high signal-to-noise ratio. We find the ratio of the clustering amplitudes of red and blue massive galaxies to be in our smallest annulus of 75–125 kpc. At our largest radii (2–4 Mpc), we find . Red galaxies therefore have denser environments than their blue counterparts at z ∼ 0.625, and this effect increases with decreasing radius. Irrespective of color, we find that w(R) does not obey a simple power-law relation with radius, showing a dip around 1 Mpc. Holding stellar mass fixed, we find a clear differentiation between clustering in red and blue galaxies, showing that clustering is not solely determined by stellar mass. Holding color fixed, we find that clustering increases with stellar mass, especially for red galaxies at small scales (more than a factor of 2 effect over 0.75 dex in stellar mass).
How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects

H and He features in photospheric spectra have seldom been used to infer quantitatively the properties of Type IIb, Ib and Ic supernovae (SNe IIb, Ib and Ic) and their progenitor stars. Most radiative transfermodels ignored non-local thermodynamic equilibrium (NLTE) effects, which are extremely strong especially in the He-dominated zones. In this paper, a comprehensive set of model atmospheres for low-mass SNe IIb/Ib/Ic is presented. Long-standing questions, such as how much He can be contained in SNe Ic, where He lines are not seen, can thus be addressed. The state of H and He is computed in full NLTE, including the effect of heating by fast electrons. The models are constructed to represent iso-energetic explosions of the same stellar core with differently massive H/He envelopes on top. The synthetic spectra suggest that 0.06-0.14 M-circle dot of He and even smaller amounts of H suffice for optical lines to be present, unless ejecta asymmetries play a major role. This strongly supports the conjecture that low-mass SNe Ic originate from binaries where progenitor mass loss can be extremely efficient.
Fluid dynamics of R-charged black holes

We construct electrically charged AdS5 black hole solutions whose charge, mass and boost-parameters vary slowly with the space-time coordinates. From the perspective of the dual theory, these are equivalent to hydrodynamic configurations with varying chemical potential, temperature and velocity fields. We compute the boundary theory transport coefficients associated with a derivative expansion of the energy momentum tensor and R-charge current up to second order. In particular, for the current we find a first order transport coefficient associated with the vorticity of the fluid.
A Tentative Gamma-Ray Line from Dark Matter Annihilation at the Fermi Large Area Telescope

The observation of a gamma-ray line in the cosmic-ray fluxes would be a smoking-gun signature for dark matter annihilation or decay in the Universe. We present an improved search for such signatures in the data of the Fermi Large Area Telescope (LAT), concentrating on energies between 20 and 300 GeV. Besides updating to 43 months of data, we use a new data-driven technique to select optimized target regions depending on the profile of the Galactic dark matter halo. In regions close to the Galactic center, we find a 4. 6σ indication for a gamma-ray line at Eγ ≈ 130 GeV. When taking into account the look-elsewhere effect the significance of the observed excess is 3. 2σ. If interpreted in terms of dark matter particles annihilating into a photon pair, the observations imply a dark matter mass of mχ = 129.8±2.4 +7−13 GeV and a partial annihilation cross-section of σvχχ → γγ = (1.27±0.32 +0.18−0.28) × 10−27cm3s−1 when using the Einasto dark matter profile. The evidence for the signal is based on about 50 photons; it will take a few years of additional data to clarify its existence.
Practical biological spread-out Bragg peak design for a carbon beam

In radiation therapy, the carbon beams has more advantages with respect to biological properties then a proton beam. The carbon beam has a high linear energy transfer (LET) to the medium and a higher relative biological effectiveness (RBE). To design the spread-out Bragg peak (SOBP) of biological dose for a carbon beam, we propose a practical method using the linear-quadratic (LQ) model and the Geant4-based Monte Carlo simulation code. Various Bragg peak profiles and LETs were calculated for each slice in the target region. To generate an appropriate biological SOBP, we applied a set of weighting factors, which are power functions in terms of energy steps, to each obtained physical dose. The designed biological SOBP showed a uniformity of 1.34%.
THE DETECTION OF THE LARGE-SCALE ALIGNMENT OF MASSIVE GALAXIES AT z ∼ 0.6

We report on the detection of the alignment between galaxies and large-scale structure at z ∼ 0.6 based on the CMASS galaxy sample from the Baryon Oscillation Spectroscopy Survey Data Release 9. We use two statistics to quantify the alignment signal: (1) the alignment two-point correlation function that probes the dependence of galaxy clustering at a given separation in redshift space on the projected angle (θp) between the orientation of galaxies and the line connecting to other galaxies, and (2) the cos (2θ)-statistic that estimates the average of cos (2θp) for all correlated pairs at a given separation s. We find a significant alignment signal out to about 70 h−1 Mpc in both statistics. Applications of the same statistics to dark matter halos of mass above 1012 h−1 M☉ in a large cosmological simulation show scale-dependent alignment signals similar to the observation, but with higher amplitudes at all scales probed. We show that this discrepancy may be partially explained by a misalignment angle between central galaxies and their host halos, though detailed modeling is needed in order to better understand the link between the orientations of galaxies and host halos. In addition, we find systematic trends of the alignment statistics with the stellar mass of the CMASS galaxies, in the sense that more massive galaxies are more strongly aligned with the large-scale structure.
OUTFLOWS, ACCRETION, AND CLUSTERED PROTOSTELLAR CORES AROUND A FORMING O STAR

We present a Submillimeter Array study in the 1.3 mm wave band of the NGC 7538 IRS 1–3 massive star-forming region. The brightest core in the millimeter continuum map, MM1, harbors the IRS 1 young O star. The core has a gas temperature of about 245 K and shows spatially unresolved emission in complex organic molecules, all typical of a hot molecular core. Toward MM1, redshifted absorption is seen in molecular lines with different energies above the ground state. This absorption probes the inward motion of the dense gas toward the central young O star, and the estimated mass accretion rate reaches 10−3 M☉ yr−1. Multiple outflows are seen in the CO and 13CO maps. The gas mass of 50 M☉ and the mass outflow rate of 2.5 × 10−3 M☉ yr−1 measured in CO line wings are dominated by the MM1 outflow, which is most likely driven by a fast wide-angle wind. Apart from MM1, we discover eight new dusty cores, MM2–9, within a projected distance of 0.35 pc from MM1. These cores show no counterpart in infrared or radio continuum emission, while seven of them appear to be forming intermediate- to high-mass stars. This manifests a deeply embedded star-forming component of the parent cloud of IRS 1–3. Apparently, we are observing a Trapezium system in formation, and the system is presumably surrounded by a cluster of lower mass stars.
CONSTRAINTS ON THE ARCHITECTURE OF THE HD 95086 PLANETARY SYSTEM WITH THE GEMINI PLANET IMAGER

We present astrometric monitoring of the young exoplanet HD 95086 b obtained with the Gemini Planet Imager between 2013 and 2016. A small but significant position angle change is detected at constant separation; the orbital motion is confirmed with literature measurements. Efficient Monte Carlo techniques place preliminary constraints on the orbital parameters of HD 95086 b. With 68% confidence, a semimajor axis of au and an inclination of are favored, with eccentricity less than 0.21. Under the assumption of a coplanar planet–disk system, the periastron of HD 95086 b is beyond 51 au with 68% confidence. Therefore, HD 95086 b cannot carve the entire gap inferred from the measured infrared excess in the SED of HD 95086. We use our sensitivity to additional planets to discuss specific scenarios presented in the literature to explain the geometry of the debris belts. We suggest that either two planets on moderately eccentric orbits or three to four planets with inhomogeneous masses and orbital properties are possible. The sensitivity to additional planetary companions within the observations presented in this study can be used to help further constrain future dynamical simulations of the planet–disk system.
Refining the Delta Debugging of Type Errors

Understanding the cause of a type error can be challenging; for over 30 years, researchers have proposed many sophisticated solutions that hardly made it into practice. Previously we presented a simple method for locating the cause of a type error in a functional program. Our method applies Zeller’s isolating delta debugging algorithm, using the compiler as a black box: Simple line-based program slicing searches for a type error location. To improve speed, we incorporated a pre-processing stage for handling parse errors. In this paper, we note that the method needs refining. We introduce a new algorithm that replaces the previous pre-processing of parse errors with on-request handling. We implemented the algorithm and evaluated it for Haskell and OCaml programs to demonstrate that it is language agnostic.
In-Place-Folding of Non-Scalar Hyper-Planes of Multi-Dimensional Arrays

Memory management plays a key role when trying to compile functional programs into efficiently executable code. In particular when using flat representations for multi-dimensional arrays, i.e., when using a single memory block for the entire data of a multi-dimensional array, in-place updates become crucial for highly competitive performance. This paper proposes a novel code generation technique for performing fold-operations on hyper-planes of multi-dimensional arrays, where the fold-operation itself operates on non-scalar sub-arrays, i.e., on vectors or higher-dimensional arrays. This technique allows for a single result array allocation over the entire folding operation without requiring the folding operation itself to be scalarised. It enables the utilisation of vector operations without any added memory allocation or copying overhead. We describe our technique in the context of SaC, sketch our implementation in the context of the compiler sac2c and provide some initial performance measurements that give an indication of the effectiveness of this new technique.
New solutions for interfacial capillary waves of permanent form

Abstract Progressive capillary waves on the interface between two homogeneous fluids confined in a channel with rigid walls parallel to the undisturbed interface are investigated. This problem is formulated as a system of integrodifferential equations that can be solved numerically via a boundary integral equation method coupled with series expansions of the unknown functions. With this highly accurate scheme and numerical continuation, we explore the global bifurcation of periodic travelling waves. It is found that there are two types of limiting profile, self-intersecting and boundary-touching, which appear either along a primary branch bifurcating from infinitesimal periodic waves or on an isolated branch existing above a certain finite amplitude. For particular sets of parameters, these two types of bifurcation curves can intersect, which can be viewed as a secondary bifurcation phenomenon occurring on the primary branch. Based on asymptotic and numerical analyses of the almost limiting waves, it is found that the boundary-touching solutions feature a circular geometry, i.e. the interface is pieced together by circular arcs of the same radius. A theoretical investigation yields the necessary conditions for the existence of these extreme waves, whereby we can predict the limiting configurations for most parameter sets. The comparisons between theoretical predictions and numerical results show good agreement.
HATS-60b–HATS-69b: 10 Transiting Planets from HATSouth

We report the discovery of 10 transiting extrasolar planets by the HATSouth survey. The planets range in mass from the super-Neptune HATS-62b, with , to the super-Jupiter HATS-66b, with , and in size from the Saturn HATS-69b, with , to the inflated Jupiter HATS-67b, with . The planets have orbital periods between days (HATS-67b) and days (HATS-61b). The hosts are dwarf stars with masses ranging from (HATS-69) to (HATS-64) and have apparent magnitudes between mag (HATS-68) and mag (HATS-66). The super-Neptune HATS-62b is the least massive planet discovered to date with a radius larger than Jupiter. Based largely on the Gaia DR2 distances and broadband photometry, we identify three systems (HATS-62, HATS-64, and HATS-65) as having possible unresolved binary star companions. We discuss in detail our methods for incorporating the Gaia DR2 observations into our modeling of the system parameters and into our blend analysis procedures.
Tip-enhanced strong coupling spectroscopy, imaging, and control of a single quantum emitter

A tunable nanotip optical cavity controls hybrid quantum states of a single emitter at room temperature. Optical cavities can enhance and control light-matter interactions. This level of control has recently been extended to the nanoscale with single emitter strong coupling even at room temperature using plasmonic nanostructures. However, emitters in static geometries, limit the ability to tune the coupling strength or to couple different emitters to the same cavity. Here, we present tip-enhanced strong coupling (TESC) with a nanocavity formed between a scanning plasmonic antenna tip and the substrate. By reversibly and dynamically addressing single quantum dots, we observe mode splitting up to 160 meV and anticrossing over a detuning range of ~100 meV, and with subnanometer precision over the deep subdiffraction-limited mode volume. Thus, TESC enables previously inaccessible control over emitter-nanocavity coupling and mode volume based on near-field microscopy. This opens pathways to induce, probe, and control single-emitter plasmon hybrid quantum states for applications from optoelectronics to quantum information science at room temperature.
Rotating Rindler-AdS Space

If the Hamiltonian of a quantum field theory is taken to be a timelike isometry, the vacuum state remains empty for all time. We search for such stationary vacua in anti-de Sitter space. By considering conjugacy classes of the Lorentz group, we find interesting one-parameter families of stationary vacua in three-dimensional anti-de Sitter space. In particular, there exists a family of rotating Rindler vacua, labeled by the rotation parameter β, which are related to the usual Rindler vacuum by nontrivial Bogolubov transformations. Rotating Rindler-AdS space possesses not only an observer-dependent event horizon but even an observer-dependent ergosphere. We also find rotating vacua in global AdS provided a certain region of spacetime is excluded.
Evaluations of the sixth phase of Coupled Model Intercomparison Project model performance on precipitation over Southeast Asia based on the moisture budget

This study evaluated the performance of the climatological precipitation over Southeast Asia using an ensemble of 48 global climate models/earth system models from the sixth phase of Coupled Model Intercomparison Project (CMIP6) suite of experiments. Multi‐source observational data sets were used to evaluate the historical simulation data of the CMIP6 ensembles towards the semi‐year mean of precipitation during November–April (NDJFMA) and May–October (MJJASO). The results indicate that the CMIP6 models were able to reproduce the large‐scale monsoonal features. Precipitation is overestimated over most eastern ocean areas in NDJFMA and over most areas in MJJASO. In terms of the ensemble bias and inter‐model uncertainty, the diagnosis of moisture budget indicates the dominant item is the dynamic convergence and the other important items have dynamic advection and evaporation. The main types of pattern bias were examined through the inter‐model empirical orthogonal function analysis, which is correlated with the global sea surface temperature and moisture flux. The climatological evaluation yielded a higher pattern correlation and a lower root‐mean square error in NDJFMA than MJJASO. Most of the models have greater standard deviations among the spatial grids than observations, especially in NDJFMA. The models with higher resolutions showed a better performance than those with lower resolutions. A model performance index is defined for the convenient comparison, the best three models are CNRM‐CM6‐1, EC‐Earth3‐Veg and NorESM2‐MM, and the worst three are INM‐CM4‐8, AWI‐ESM‐1‐1‐LR and MCM‐UA‐1‐0. This evaluation study provided useful analytics in understanding model behaviour and processes related to rainfall mechanisms which could be further examined in high‐resolution downscaling experiments in future studies.