Miracle-dz/UniFAR-FTUs huggingface dataset:
Group sparse RLS algorithms

Group sparsity is one of the important signal priors for regularization of inverse problems. Sparsity with group structure is encountered in numerous applications. However, despite the abundance of sparsity‐based adaptive algorithms, attempts at group sparse adaptive methods are very scarce. In this paper, we introduce novel recursive least squares (RLS) adaptive algorithms regularized via penalty functions, which promote group sparsity. We present a new analytic approximation for ℓp,0 norm to utilize it as a group sparse regularizer. Simulation results confirm the improved performance of the new group sparse algorithms over regular and sparse RLS algorithms when group sparse structure is present. Copyright © 2013 John Wiley & Sons, Ltd.
Disentangling theorem and monogamy for entanglement negativity

Entanglement negativity is a measure of mixed-state entanglement increasingly used to investigate and characterize emerging quantum many-body phenomena, including quantum criticality and topological order. We present two results for the entanglement negativity: a disentangling theorem, which allows the use of this entanglement measure as a means to detect whether a wave function of three subsystems $A,\phantom{\rule{0.28em}{0ex}}B$, and $C$ factorizes into a product state for parts $A{B}_{1}$ and ${B}_{2}C$; and a monogamy relation conjecture based on entanglement negativity, which states that if $A$ is very entangled with $B$, then $A$ cannot be simultaneously very entangled also with $C$.
First results from the Herschel Gould Belt Survey in Taurus

The whole of the Taurus region (a total area of 52 deg2) has been observed by the Herschel Spectral and Photometric Imaging Receiver (SPIRE) and Photodetector Array Camera and Spectrometer (PACS) instruments at wavelengths of 70, 160, 250, 350 and 500 μm as part of the Herschel Gould Belt Survey. In this paper we present the first results from the part of the Taurus region that includes the Barnard 18 and L1536 clouds. A new source-finding routine, the Cardiff Source-finding AlgoRithm (csar), is introduced, which is loosely based on clumpfind, but that also generates a structure tree, or dendrogram, which can be used to interpret hierarchical clump structure in a complex region. Sources were extracted from the data using the hierarchical version of csar and plotted on a mass–size diagram. We found a hierarchy of objects with sizes in the range 0.024–2.7 pc. Previous studies showed that gravitationally bound prestellar cores and unbound starless clumps appeared in different places on the mass–size diagram. However, it was unclear whether this was due to a lack of instrumental dynamic range or whether they were actually two distinct populations. The excellent sensitivity of Herschel shows that our sources fill the gap in the mass–size plane between starless and pre-stellar cores, and gives the first clear supporting observational evidence for the theory that unbound clumps and (gravitationally bound) prestellar cores are all part of the same population, and hence presumably part of the same evolutionary sequence.
Realized BEKK-CAW Models

Abstract Estimating time-varying conditional covariance matrices of financial returns play important role in portfolio analysis, risk management, and financial econometrics research. The availability of high-frequency financial data can provide an additional data source for dynamic covariance modeling. In this paper, we propose to use the information of asset return vector and realized covariance measures simultaneously to develop a new conditional covariance matrix model. We derive the stationary condition of the new model. We use the normal and Wishart distributions to construct the quasi-log-likelihood function. We also consider the variance targeting (VT) method, which plugs in the weighted average of the sample covariance matrix of returns and the sample mean of realized covariance measure for the unconditional covariance matrix, in order to maximize the quasi-log-likelihood function. We show the consistency and asymptotic normality of the quasi-maximum likelihood (QML) and VT estimators. We investigate the finite sample property of these estimators via Monte Carlo experiments. The empirical example for the bivariate data of the Nikkei 225 index and its futures indicates that the first-step VT estimation could have non-negligible effects on the standard errors of the second-step VT estimates.
The survival of dynamical fossils in dwarf spheroidal galaxies in conventional and modified dynamics

The survival of unbound density substructure against orbital mixing imposes strong constraints on the slope of the underlying gravitational potential and provides a new test on modified gravities. Here we investigate whether the interpretation that the stellar clump in Ursa Minor (UMi) dwarf spheroidal galaxy is a ‘dynamical fossil’ is consistent with MOdified Newtonian Dynamics (MOND). For UMi mass models inferred by fitting the velocity dispersion profile, the stellar clump around the second peak of UMi is erased very rapidly, within 1.25 Gyr (6.5 orbits), even with the inclusion of self-gravity. We find that the clump can hardly survive for more than 2 Gyr even under more generous conditions. Alternative scenarios which could lead to a kinematically cold clump are discussed but, so far, none of them was found to be fully satisfactory. Our conclusion is that the cold clump in UMi poses a challenge for both Lambda cold dark matter (ΛCDM) and MOND.
EVIDENCE FOR PRE-EXISTING DUST IN THE BRIGHT TYPE IIn SN 2010jl

SN 2010jl was an extremely bright, Type IIn supernova (SN) which showed a significant infrared (IR) excess no later than 90 days after explosion. We have obtained Spitzer 3.6 and 4.5 μm and JHK observations of SN 2010jl ∼90 days post-explosion. Little to no reddening in the host galaxy indicated that the circumstellar material lost from the progenitor must lie in a torus inclined out of the plane of the sky. The likely cause of the high mid-IR flux is the reprocessing of the initial flash of the SN by pre-existing circumstellar dust. Using a three-dimensional Monte Carlo radiative-transfer code, we have estimated that between 0.03 and 0.35 M☉ of dust exists in a circumstellar torus around the SN located 6 × 1017 cm away from the SN and inclined between 60° and 80° to the plane of the sky. On day 90, we are only seeing the illumination of approximately 5% of this torus, and expect to see an elevated IR flux from this material up until day ∼ 450. It is likely this dust was created in a luminous blue variable (LBV) like mass-loss event of more than 3 M☉, which is large but consistent with other LBV progenitors such as η Carinae.
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS

We present new theoretical stellar yields and surface abundances for three grids of metal-rich asymptotic giant branch (AGB) models. Post-processing nucleosynthesis results are presented for stellar models with initial masses between 1 M☉ and 7.5 M☉ for Z = 0.007, and 1 M☉ and 8 M☉ for Z = 0.014 (solar) and Z = 0.03. We include stellar surface abundances as a function of thermal pulse on the AGB for elements from C to Bi and for a selection of isotopic ratios for elements up to Fe and Ni (e.g., / ), which can be obtained from observations of molecules in stars and from the laboratory analysis of meteoritic stardust grains. Ratios of elemental abundances of He/H, C/O, and N/O are also included, which are useful for direct comparison to observations of AGB stars and their progeny, including planetary nebulae. The integrated elemental stellar yields are presented for each model in the grid for hydrogen, helium, and all stable elements from C to Bi. Yields of Li are also included for intermediate-mass models with hot bottom burning. We present the first slow neutron-capture (s-process) yields for super solar metallicity AGB stars with Z = 0.03, and the first complete s-process yields for models more massive than 6 M☉ at all three metallicities.
FIRST LONG-TERM OPTICAL SPECTRAL MONITORING OF A BINARY BLACK HOLE CANDIDATE E1821+643. I. VARIABILITY OF SPECTRAL LINES AND CONTINUUM

We report the results of the first long-term (1990–2014) optical spectrophotometric monitoring of a binary black hole candidate QSO E1821+643, a low-redshift, high-luminosity, radio-quiet quasar. In the monitored period, the continua and Hγ fluxes changed about two times, while the Hβ flux changed about 1.4 times. We found periodical variations in the photometric flux with periods of 1200, 1850, and 4000 days, and 4500-day periodicity in the spectroscopic variations. However, the periodicity of 4000–4500 days covers only one cycle of variation and should be confirmed with a longer monitoring campaign. There is an indication of the period around 1300 days in the spectroscopic light curves, buts with small significance level, while the 1850-day period could not be clearly identified in the spectroscopic light curves. The line profiles have not significantly changed, showing an important red asymmetry and broad line peak redshifted around +1000 km s−1. However, Hβ shows a broader mean profile and has a larger time lag (τ ∼ 120 days) than Hγ (τ ∼ 60 days). We estimate that the mass of the black hole is ∼2.6 × 109 M⊙. The obtained results are discussed in the frame of the binary black hole hypothesis. To explain the periodicity in the flux variability and high redshift of the broad lines, we discuss a scenario where dense, gas-rich, cloudy-like structures are orbiting around a recoiling black hole.
Constructive and intuitionistic integration theory and functional analysis

There are ample reasons to develop mathematics constructively, for instance because one is interested in the foundations of mathematics or in programming on a highly abstract level. But is it possible to do advanced mathematics constructively? Bishop and his followers showed that large parts of abstract analysis and algebra can be developed constructively. But nevertheless the discussion about the applicability of constructive mathematics to mathematical physics started again. This discussion gave rise to a number of precise mathematical problems. Some of these problems have already been solved, others will be answered in this thesis. These problems all belong to functional analysis, part of which is developed constructively in this thesis. To be more precise, the thesis contains a constructive substitute for the ergodic theorem, a constructive Peter-Weyl theorem for representations of compact groups, approximation theorems for almost periodic functions and a spectral theorem for unbounded normal operators on Hilbert spaces. Moreover, parts of the theory of algebras of operators are developed constructively: two representation theorems are proved, one for finite dimensional and one for Abelian von Neumann algebras. A simple proof is given that the spectral measure is independent of the choice of the basis of the underlying Hilbert space. Finally, a representation theorem for normal functionals is proved. As a tool which is interesting in its own right parts of integration theory are redeveloped, using a metric related to convergence in measure. It is proved that many measures are regular, that is, integrable sets can be approximated by compact sets. This result is used to extend some important intuitionistic theorems. Finally, a representation theorem for Chan's measurable spaces is given, making it possible to understand these spaces intuitionistically.
Assimilation of Tropical Cyclone Track and Wind Radius Data with an Ensemble Kalman Filter

AbstractImproving tropical cyclone (TC) forecasts is one of the most important issues in meteorology, but TC intensity forecasting is a challenging task. Because the lack of observations near TCs usually results in degraded accuracy of the initial fields, utilizing TC advisory data in data assimilation typically has started with an ensemble Kalman filter (EnKF). In this study, TC minimum sea level pressure (MSLP) and position information were directly assimilated using the EnKF, and the impacts of these observations were investigated by comparing different assimilation strategies. Another experiment with TC wind radius data was carried out to examine the influence of TC shape parameters. Sensitivity experiments indicated that the direct assimilation of TC MSLP and position data yielded results that were superior to those based on conventional assimilation of TC MSLP as a standard surface pressure observation. Assimilation of TC radius data modified the outer circulation of TCs closer to observations. The .
RiscyROP: Automated Return-Oriented Programming Attacks on RISC-V and ARM64

Return-oriented programming (ROP) is a powerful run-time exploitation technique to attack vulnerable software. Modern RISC architectures like RISC-V and ARM64 pose new challenges for ROP execution due to the lack of a stack-based return instruction and strict instruction alignment. Further, the large number of caller-saved argument registers significantly reduces the gadget space available to the attacker. Consequently, existing ROP gadget tools for other processor architectures cannot be applied to these RISC architectures. Previous work on RISC-V provides only manual construction of ROP attacks against specially crafted programs, and no analysis of ROP attacks has been conducted for ARM64 yet. In this paper, we address these challenges and present RiscyROP, the first automated ROP gadget finding and chaining toolkit for RISC-V and ARM64. RiscyROP analyzes available gadgets utilizing symbolic execution, and automatically generates complex multi-stage chains to conduct arbitrary function calls. Our approach enables the first investigation of the gadget space on RISC-V and ARM64 real-world binaries. RiscyROP successfully builds ROP chains that enable an attacker to execute arbitrary function calls for the nginx web server as well as any binary that contains the libc library.
MONTE CARLO SIMULATIONS OF NONLINEAR PARTICLE ACCELERATION IN PARALLEL TRANS-RELATIVISTIC SHOCKS

We present results from a Monte Carlo simulation of a parallel collisionless shock undergoing particle acceleration. Our simulation, which contains parameterized scattering and a particular thermal leakage injection model, calculates the feedback between accelerated particles ahead of the shock, which influence the shock precursor and “smooth” the shock, and thermal particle injection. We show that there is a transition between nonrelativistic shocks, where the acceleration efficiency can be extremely high and the nonlinear compression ratio can be substantially greater than the Rankine–Hugoniot value, and fully relativistic shocks, where diffusive shock acceleration is less efficient and the compression ratio remains at the Rankine–Hugoniot value. This transition occurs in the trans-relativistic regime and, for the particular parameters we use, occurs around a shock Lorentz factor γ0 = 1.5. We also find that nonlinear shock smoothing dramatically reduces the acceleration efficiency presumed to occur with large-angle scattering in ultra-relativistic shocks. Our ability to seamlessly treat the transition from ultra-relativistic to trans-relativistic to nonrelativistic shocks may be important for evolving relativistic systems, such as gamma-ray bursts and Type Ibc supernovae. We expect a substantial evolution of shock accelerated spectra during this transition from soft early on to much harder when the blast-wave shock becomes nonrelativistic.
Attrition of Workers with Minoritized Identities on AI Teams

The effects of AI systems are far-reaching and affect diverse communities all over the world. The demographics of AI teams, however, do not reflect this diversity. Instead, these teams, particularly at big tech companies, are dominated by Western, White, and male workers. Strategies for preventing harms done by AI must also include making these teams more representative of the diverse communities that these technologies affect. The pipeline of students from K-12 and university level contributes to this - those with minoritized identities are underrepresented or excluded from pursuing computer science careers. However there has been relatively little attention given to how the culture at tech companies, let alone AI teams, contribute to attrition of minoritized people in the workplace. The current study uses semi-structured interviews with minoritized workers on AI teams, managers of AI teams, and leaders working on diversity, equity, and inclusion (DEI) in the tech field (N = 43), to investigate the reasons why these workers leave these AI teams. The themes from these interviews describe how the culture and climate of these teams may contribute to attrition of minoritized workers, and strategies for making these teams more inclusive and representative of the diverse communities affected by technologies developed by these AI teams. Specifically, the current study found that AI teams in which minoritized workers thrive tend to foster a strong sense of interdisciplinary collaboration, support professional career development, and are run by diverse leaders who understand the importance of undoing the traditional White, Eurocentric, and male workplace norms. These go beyond the “quick fixes” that are prevalent in DEI practices.
ISPAD Clinical Practice Consensus Guidelines 2022: Diabetes in adolescence

Division of Population Medicine, School of Medicine, Cardiff University, Cardiff, UK Royal Children's Hospital, Melbourne, Australia Murdoch Children's Research Institute, Melbourne, Australia Department of Paediatrics, University of Melbourne, Melbourne, Australia Department of Endocrinology & Diabetes, Queensland Children's Hospital, South Brisbane, Australia Department of Anglophone Studies, Universität Duisburg Essen, Essen, Germany Institute of Psychiatry, Psychology and Neuroscience, Bart's Health and East London Foundation Trust, London, UK Division of Endocrinology, Boston Children's Hospital, Boston, Massachusetts, USA Department of Medicine (Endocrinology), Albert Einstein College of Medicine, Montefiore Medical Center, Bronx, New York, USA Instituto de Investigaciones Materno Infantil, Facultad de Medicina, University of Chile, Santiago, Chile
Novel Results on the Large-Signal Dynamic Admittance of $p-n$-Junctions

Recent theoretical results obtained by Barybin and Santos have suggested that the dynamic admittance of the $p-n$-junction is proportional to the modified Bessel function of the first kind which depend on an amplitude of ac signal. This result extends the conventional theory usually encountered in known papers and textbooks. In this letter, some experimental results are presented to confirm our theoretical prediction. The measurements were performed with a lock-in amplifier, using a low noise operational amplifier. Two types of the $p-n$-diodes were employed to check our theory: 1N914B diode, typically used for high-frequency applications, and 1N4007 diode, typically used in power supplies. Experimental results are consistent with the theoretical ones if a fitting parameter allowing for generation--recombination processes in the depletion layer is taken into account.
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe

Broadband photometry of galaxies measures an unresolved mix of complex stellar populations, gas, and dust. Interpreting these data is a challenge for models: many studies have shown that properties derived from modeling galaxy photometry are uncertain by a factor of two or more, and yet answering key questions in the field now requires higher accuracy than this. Here, we present a new model framework specifically designed for these complexities. Our model, Prospector-α, includes dust attenuation and re-radiation, a flexible attenuation curve, nebular emission, stellar metallicity, and a six-component nonparametric star formation history. The flexibility and range of the parameter space, coupled with Monte Carlo Markov chain sampling within the Prospector inference framework, is designed to provide unbiased parameters and realistic error bars. We assess the accuracy of the model with aperture-matched optical spectroscopy, which was excluded from the fits. We compare spectral features predicted solely from fits to the broadband photometry to the observed spectral features. Our model predicts Hα luminosities with a scatter of ∼0.18 dex and an offset of ∼0.1 dex across a wide range of morphological types and stellar masses. This agreement is remarkable, as the Hα luminosity is dependent on accurate star formation rates, dust attenuation, and stellar metallicities. The model also accurately predicts dust-sensitive Balmer decrements, spectroscopic stellar metallicities, polycyclic aromatic hydrocarbon mass fractions, and the age- and metallicity-sensitive features Dn4000 and Hδ. Although the model passes all these tests, we caution that we have not yet assessed its performance at higher redshift or the accuracy of recovered stellar masses.
MEASUREMENT OF THE HALO BIAS FROM STACKED SHEAR PROFILES OF GALAXY CLUSTERS

We present observational evidence of the two-halo term in the stacked shear profile of a sample of ∼1200 optically selected galaxy clusters based on imaging data and the public shear catalog from the CFHTLenS. We find that the halo bias, a measure of the correlated distribution of matter around galaxy clusters, has amplitude and correlation with galaxy cluster mass in very good agreement with the predictions based on the LCDM standard cosmological model. The mass–concentration relation is flat but higher than theoretical predictions. We also confirm the close scaling relation between the optical richness of galaxy clusters and their mass.
EXPLORING THE INTERSTELLAR MEDIA OF OPTICALLY COMPACT DWARF GALAXIES

We present new Very Large Array H i spectral line, archival Sloan Digital Sky Survey, and archival Spitzer Space Telescope imaging of eight star-forming blue compact dwarf galaxies that were selected to be optically compact (optical radii <1 kpc). These systems have faint blue absolute magnitudes (MB ≳ −17), ongoing star formation (based on emission-line selection by the Hα or [O iii] lines), and are nearby (mean velocity = 3315 km s−1 ≃ 45 Mpc). One galaxy in the sample, ADBS 113845+2008, is found to have an H i halo that extends 58 r-band scale lengths from its stellar body. In contrast, the rest of the sample galaxies have H i radii to optical-scale-length ratios ranging from 9.3 to 26. The size of the H i disk in the “giant disk” dwarf galaxy ADBS 113845+2008 appears to be unusual as compared with similarly compact stellar populations.
Finite Size Scaling and Numerical Simulation of Statistical Systems

The theory of Finite Size Scaling describes a build-up of the bulk properties when a small system is increased in size. This description is particularly important in strongly correlated systems where critical fluctuations develop with increasing system size, including phase transition points, polymer conformations. Since numerical computer simulations are always done with finite samples, they rely on the Finite Size Scaling theory for data extrapolation and analysis. With the advent of large scale computing in recent years, the use of the size-scaling methods has become increasingly important.