Miracle-dz/UniFAR-FTUs huggingface dataset:
Maternal pre-pregnancy anemia and childhood anemia in Indonesia: a risk assessment using a population-based prospective longitudinal study

OBJECTIVES Anemia in children under 5 years of age is often overlooked despite its detrimental effects. The public health approach to anemia prevention includes the maternal pre-pregnancy phase. This study investigated the association between pre-pregnancy anemia and the risk of anemia in children under 5 years of age. METHODS This cohort study included non-pregnant women from the 2007 Indonesian Family Life Survey (IFLS) and their children under 5 in the 2014 IFLS. The anemia status of mothers and children was determined based on hemoglobin (Hb) levels using Hemocue. Mantel-Haenszel adjusted relative risks (aRRs), including risk stratification by covariates, were used for the final risk assessment. RESULTS In total, 637 children in the 2014 IFLS were included. The risk of having a child with anemia was 1.71-fold higher in women with pre-pregnancy anemia than in women without pre-pregnancy anemia (aRR, 1.71; 95% confidence interval [CI], 1.03 to 2.85). After risk stratification based on potential confounding variables, maternal pre-pregnancy anemia remained an independent risk factor for anemia in children who still breastfed at the time of data collection (relative risk [RR], 2.11; 95% CI, 1.16 to 3.86), in children who were given water earlier than 6 months of age (RR, 2.08; 95% CI, 1.20 to 3.61), in children of mothers with a normal or underweight pre-pregnancy body mass index (RR, 1.94; 95% CI, 1.20 to 3.14), and in children of mothers without current anemia (RR, 2.20; 95% CI, 1.21 to 3.99). CONCLUSIONS Pre-pregnancy anemia increased the risk of childhood anemia. A public health approach emphasizing pre-conception maternal health would enable better maternal and child morbidity risk prevention.
Towards One-shot Learning via Attention (invited paper)

Though the deep neural networks enabled us to create systems that would be incredible ten years ago, still most of them learn gradually and offline. We introduce an approach to how to overcome this limitation. We have implemented it by the well-known attention mechanism that transforms one latent space into another using a list of key-value pairs defining the correspondence between points in the two spaces. We can express any point in the first space as a mixture of keys and map it to a point in the second space that is an analogical mixture of values. While encoders and decoders of these spaces we train only gradually, the keys and values of the transformation we can collect online so that we constantly improve the mapping quality, achieving the perfect mapping of the current situation immediately. We demonstrate our approach to one-shot learning on the simplified imitation game in the human-robot interaction, where we map the representations of the robot’s body and the examinator’s body seen by the robot.
DHIGLS: DRAO H i INTERMEDIATE GALACTIC LATITUDE SURVEY

Observations of Galactic H i gas for seven targeted regions at intermediate Galactic latitude are presented at angular resolution using data from the DRAO Synthesis Telescope (ST) and the Green Bank Telescope (GBT). The DHIGLS data are the most extensive arcminute-resolution measurements of the diffuse atomic interstellar medium beyond those in the Galactic plane. The acquisition, reduction, calibration, and mosaicking of the DRAO ST data and the cross calibration and incorporation of the short-spacing information from the GBT are described. The high quality of the resulting DHIGLS products enables a variety of new studies in directions of low Galactic column density. We analyze the angular power spectra of maps of the integrated H i emission (column density) from the data cubes for several distinct velocity ranges. In fitting power-spectrum models based on a power law, but including the effects of the synthesized beam and noise at high spatial frequencies, we find exponents ranging from −2.5 to −3.0. Power spectra of maps of the centroid velocity for these components give similar results. These exponents are interpreted as being representative of the three-dimensional density and velocity fields of the atomic gas, respectively. We find evidence for dramatic changes in the H i structures in channel maps over even small changes in velocity. This narrow line emission has counterparts in absorption spectra against bright background radio sources, quantifying that the gas is cold and dense and can be identified as the cold neutral medium phase. Fully reduced DHIGLS H i data cubes and other data products are available at www.cita. utoronto.ca/DHIGLS.
METAL-MASS-TO-LIGHT RATIOS OF THE PERSEUS CLUSTER OUT TO THE VIRIAL RADIUS

We analyzed XMM-Newton data of the Perseus cluster out to ∼1 Mpc, or approximately half the virial radius. Using the flux ratios of Lyα lines of H-like Si and S to Kα line of He-like Fe, the abundance ratios of Si/Fe and S/Fe of the intracluster medium (ICM) were derived using the APEC plasma code v2.0. 1. The temperature dependence of the line ratio limits the systematic uncertainty in the derived abundance ratio. The Si/Fe and S/Fe in the ICM of the Perseus cluster show no radial gradient. The emission-weighted averages of the Si/Fe and S/Fe ratios outside the cool core are 0.91 ± 0.08 and 0.93 ± 0.10, respectively, in solar units according to the solar abundance table of Lodders. These ratios indicate that most Fe was synthesized by supernovae Ia. We collected K-band luminosities of galaxies and calculated the ratio of Fe and Si mass in the ICM to K-band luminosity, iron-mass-to-light ratio (IMLR), and silicon-mass-to-light ratio (SMLR). Within ∼1 Mpc, the cumulative IMLR and SMLR increase with radius. Using Suzaku data for the northwest and east directions, we also calculated the IMLR out to ∼1.8 Mpc, or about the virial radius. We constrained the SMLR out to this radius and discussed the slope of the initial mass function of stars in the cluster. Using the cumulative IMLR profile, we discuss the past supernova Ia rate.
STELLAR ARCHEOLOGY IN THE GALACTIC HALO WITH ULTRA-FAINT DWARFS. VII. HERCULES

We present the first time-series study of the ultra-faint dwarf galaxy Hercules. Using a variety of telescope/instrument facilities we secured about 50 V and 80 B epochs. These data allowed us to detect and characterize 10 pulsating variable stars in Hercules. Our final sample includes six fundamental-mode (ab-type) and three first-overtone (c-type) RR Lyrae stars, and one Anomalous Cepheid. The average period of the ab-type RR Lyrae stars, 〈Pab〉 = 0.68 days (σ = 0.03 days), places Hercules in the Oosterhoff II group, as found for almost the totality of the ultra-faint dwarf galaxies investigated so far for variability. The RR Lyrae stars were used to obtain independent estimates of the metallicity, reddening, and distance to Hercules, for which we find [Fe/H] = −2.30 ± 0.15 dex, E(B − V) = 0.09 ± 0.02 mag, and (m − M)0 = 20.6 ± 0.1 mag, in good agreement with the literature values. We have obtained a V, B − V color–magnitude diagram (CMD) of Hercules that reaches V ∼ 25 mag and extends beyond the galaxy's half-light radius over a total area of 40′ × 36′. The CMD and the RR Lyrae stars indicate the presence of a population as old and metal-poor as (at least) the Galactic globular cluster M68.
ACCELERATION, MAGNETIC FLUCTUATIONS, AND CROSS-FIELD TRANSPORT OF ENERGETIC ELECTRONS IN A SOLAR FLARE LOOP

Plasma turbulence is thought to be associated with various physical processes involved in solar flares, including magnetic reconnection, particle acceleration, and transport. Using RHESSI observations and the X-ray visibility analysis, we determine the spatial and spectral distributions of energetic electrons for a flare (GOES M3.7 class, 2002 April 14, 23:55 UT), which was previously found to be consistent with a reconnection scenario. It is demonstrated that because of the high density plasma in the loop, electrons have to be continuously accelerated about the loop apex of length ∼2 × 109 cm and width ∼7 × 108 cm. Energy-dependent transport of tens of keV electrons is observed to occur both along and across the guiding magnetic field of the loop. We show that the cross-field transport is consistent with the presence of magnetic turbulence in the loop, where electrons are accelerated, and estimate the magnitude of the field line diffusion coefficient for different phases of the flare. The energy density of magnetic fluctuations is calculated for given magnetic field correlation lengths and is larger than the energy density of the non-thermal electrons. The level of magnetic fluctuations peaks when the largest number of electrons is accelerated and is below detectability or absent at the decay phase. These hard X-ray observations provide the first observational evidence that magnetic turbulence governs the evolution of energetic electrons in a dense flaring loop and is suggestive of their turbulent acceleration.
The star cluster-field star connection in nearby spiral galaxies. I. Data analysis techniques and application to NGC 4395

Context. It is generally assumed that a large fraction of stars are initially born in clusters. However, a large fraction of these disrupt on short timescales and the stars end up belonging to the field. Understanding this process is of paramount importance if we wish to constrain the star formation histories of external galaxies using star clusters. Aims. We attempt to understand the relation between field stars and star clusters by simultaneously studying both in a number of nearby galaxies. Methods. As a pilot study, we present results for the late-type spiral NGC 4395 using HST/ACS and HST/WFPC2 images. Different detection criteria were used to distinguish point sources (star candidates) and extended objects (star cluster candidates). Using a synthetic CMD method, we estimated the star formation history. Using simple stellar population model fitting, we calculated the mass and age of the cluster candidates. Results. The field star formation rate appears to have been roughly constant, or to have possibly increased by up to about a factor of two, for ages younger than ∼300 Myr within the fields covered by our data. Our data do not allow us to constrain the star formation histories at older ages. We identify a small number of clusters in both fields. Neither massive (>10 5 M� ) clusters nor clusters with ages ≥1 Gyr were found in the galaxy and we found few clusters older than 100 Myr. Conclusions. Based on our direct comparison of field stars and clusters in NGC 4395, we estimate the ratio of star formation rate in clusters that survive for 10 7 to 10 8 years to the total star formation to be Γ ∼ 0.03. We suggest that this relatively low Γ value is caused by the low star formation rate of NGC 4395.
Counting statistics in multistable systems

Using a microscopic model for stochastic transport through a single quantum dot that is modified by the Coulomb interaction of environmental (weakly coupled) quantum dots, we derive generic properties of the full counting statistics for multistable Markovian transport systems. We study the temporal crossover from multimodal to broad unimodal distributions depending on the initial mixture, the long-term asymptotics and the divergence of the cumulants in the limit of a large number of transport branches. Our findings demonstrate that the counting statistics of a single resonant level may be used to probe background charge configurations.
Universal rules for visible-light absorption in hybrid perovskite materials

A variety of organic-inorganic hybrid perovskites (APbX3) consisting of mixed center cations [A = CH3NH3+, HC(NH2)2+, and Cs+] with different PbX3− cages (X = I, Br, and Cl) have been developed to realize high-efficiency solar cells. Nevertheless, clear understanding of the effects of A and X on the optical transition has been lacking. Here, we present universal rules that allow the unified interpretation of the optical absorption in various hybrid perovskites. In particular, we find that the influence of the A-site cation on the light absorption is rather significant and the absorption coefficient (α) reduces to half when CH3NH3+ is replaced with HC(NH2)2+ in the APbI3 system. Our density functional theory calculations reproduce all of the fine absorption features observed in HC(NH2)2PbI3 and CH3NH3PbBr3, allowing the unique assignment of the interband transitions in the Brillouin zone. In contrast to general understanding that the A-site cation involves weakly in the optical process, our theoretical cal.
VIOLENT INTRANIGHT OPTICAL VARIABILITY OF A RADIO-LOUD NARROW-LINE SEYFERT 1 GALAXY: SDSS J094857.3+002225

SDSS J094857.3+002225 is a very radio-loud narrow-line Seyfert 1 (NLS1) galaxy. Here, we report our discovery of the intranight optical variability (INOV) of this galaxy through the optical monitoring in the B and R bands that covered seven nights in 2009. Violent rapid variability in the optical bands was identified in this RL-NLS1 for the first time, and the amplitudes of the INOV reaches 0.5 mag in both the B and R bands on the timescale of several hours. The detection of the INOV provides a piece of strong evidence supporting the fact that the object carries a relativistic jet with a small viewing angle, which confirms the conclusion drawn from the previous multi-wavelength studies.
A new, precise measurement of the primordial abundance of deuterium

The metal-poor (Z � 1/100 Z� ) damped Lyman α system (DLA) at redshift zabs = 3.049 84 in the zem � 3.030 QSO SDSS J1419+0829 has near-ideal properties for an accurate deter- mination of the primordial abundance of deuterium (D/H)p. We have analysed a high-quality spectrum of this object with software specifically designed to deduce the best-fitting value of D/H and to assess comprehensively the random and systematic errors affecting this determi- nation. We find (D/H)DLA = (2.535 ± 0.05) × 10 −5 , which in turn impliesb,0h 2 = 0.0223 ± 0.0009, in very good agreement withb,0h 2 (CMB) = 0.0222 ± 0.0004 deduced from the angular power spectrum of the cosmic microwave background (CMB). If the value in this DLA is indeed the true (D/H)p produced by big bang nucleosynthesis (BBN), there may be no need to invoke non-standard physics nor early astration of D to bring togetherb,0 h 2 (BBN) andb,0 h 2 (CMB). The scatter between most of the reported values of (D/H)p in the literature may be due largely to unaccounted systematic errors and biases. Further progress in this area will require a homogeneous set of data comparable to those reported here and analysed in a self-consistent manner. Such an endeavour, while observationally demanding, has the potential of improving our understanding of BBN physics, including the relevant nuclear reactions, and the subsequent processing of light nuclides through stars.
Horizon quantum mechanics for spheroidal sources

We start investigating the extension of the horizon quantum mechanics to the case of non-spherical sources. We first study the location of trapping surfaces in space-times resulting from an axial deformation of static isotropic systems, and show that the Misner-Sharp mass evaluated on the corresponding undeformed spherically symmetric space provides the correct gravitational radius to locate the horizon. We finally propose a way to determine the deformation parameter in the quantum theory.
Harmonically trapped atoms with spin–orbit coupling

We study harmonically trapped one-dimensional atoms subjected to an equal combination of Rashba and Dresselhaus spin–orbit coupling induced by Raman transition. We first examine the wave function and the degeneracy of the single-particle ground state, followed by a study of two weakly interacting bosons or fermions. For the two-particle ground state, we focus on the effects of the interaction on the degeneracy, the spin density profiles, and the density–density correlation functions. Finally we show how these studies help us to understand the many-body properties of the system.
Phosphorylation on PstP controls cell wall metabolism and antibiotic tolerance in 1 Mycobacterium smegmatis 2

12 13 The mycobacterial cell wall is a dynamic structure that protects Mycobacterium 14 tuberculosis and its relatives from environmental stresses. Modulation of cell wall 15 metabolism under stress is thought to be responsible for decreased cell wall permeability 16 and increased tolerance to antibiotics. The signaling pathways that control cell wall 17 metabolism under stress, however, are poorly understood. Here, we examine the 18 signaling capacity of a cell wall master regulator, the Serine Threonine Phosphatase 19 PstP, in the model organism Mycobacterium smegmatis. We studied how interference 20 with a regulatory phosphorylation site on PstP affects growth, cell wall metabolism and 21 antibiotic tolerance. We find that a phospho-mimetic mutation, pstP T171E, slows 22 growth, misregulates both mycolic acid and peptidoglycan metabolism in different 23 conditions, and interferes with antibiotic tolerance. These data suggest that 24 phosphorylation on PstP controls its substrate specificity and is important in the 25 transition between growth and stasis. 26
A family of accelerated inexact augmented Lagrangian methods with applications to image restoration

In this paper, we focus on a class of convex optimization problems subject to equality or inequality constraints and have developed an Accelerated Inexact Augmented Lagrangian Method (AI-ALM). Di(cid:11)erent relative error criteria are designed to solve the subproblem of AI-ALM inexactly, and the popular used relaxation step is exploited to accelerate the convergence. By a uni(cid:12)ed variational analysis, we establish the global convergence of AI-ALM and its sublinear convergence rate in terms of the primal iterative residual, the objective function value gap and constraint violation, respectively. Numerical experiments on testing the image restoration problem with di(cid:11)erent types of images indicate that AI-ALM is e(cid:11)ective and promising. In appendix, we also extend AI-ALM to solve a general multi-block problem and brie(cid:13)y discuss convergence of the extended method.
Fluctuation-dominated phase ordering at a mixed order transition

Mixed order transitions are those which show a discontinuity of the order parameter as well as a divergent correlation length at the transition (critical) point. We show that the behavior of the order parameter correlation function along the transition line of mixed order transitions can change from normal critical behavior with power law decay, to fluctuation-dominated phase ordering as a parameter is varied. The defining features of fluctuation-dominated order are anomalous fluctuations which remain large in the thermodynamic limit, and correlation functions which approach a finite value through a cusp singularity as the separation scaled by the system size approaches zero. We demonstrate that fluctuation-dominated order sets in along a portion of the transition line of an Ising model with truncated long-range interactions which was earlier shown to exhibit mixed order transitions. We also argue that this connection may hold more generally.
CLASH: DISCOVERY OF A BRIGHT z ≃ 6.2 DWARF GALAXY QUADRUPLY LENSED BY MACS J0329.6-0211

We report the discovery of a zphot = 6.18+0.05− 0.07 (95% confidence level) dwarf galaxy, lensed into four images by the galaxy cluster MACS J0329.6-0211 (zl = 0.45). The galaxy is observed as a high-redshift dropout in HST/ACS/WFC3 CLASH and Spitzer/IRAC imaging. Its redshift is securely determined due to a clear detection of the Lyman break in the 18-band photometry, making this galaxy one of the highest-redshift multiply lensed objects known to date with an observed magnitude of F125W =24.00 ± 0.04 AB mag for its most magnified image. We also present the first strong-lensing analysis of this cluster uncovering 15 additional multiply imaged candidates of five lower-redshift sources spanning the range zs ≃ 2–4. The mass model independently supports the high photometric redshift and reveals magnifications of 11.6+8.9− 4.1, 17.6+6.2− 3.9, 3.9+3.0− 1.7, and 3.7+1.3− 0.2, respectively, for the four images of the high-redshift galaxy. By delensing the most magnified image we construct an image of the source with a physical resolution of ∼200 pc when the universe was ∼0.9 Gyr old, where the z ≃ 6.2 galaxy occupies a source-plane area of approximately 2.2 kpc2. Modeling the observed spectral energy distribution using population synthesis models, we find a demagnified stellar mass of , subsolar metallicity (Z/Z☉ ∼ 0.5), low dust content (AV ∼ 0.1 mag), a demagnified star formation rate (SFR) of yr−1, and a specific SFR of ∼3.4 Gyr−1, all consistent with the properties of local dwarf galaxies.
Effect of Arm Pivot Joints on Stiffness Discrimination in Haptic Environments

We investigated the effect of arm pivot joints that are typically used during haptic exploration by evaluating four joints of the human arm (metacarpophalangeal joint of the index finger, wrist, elbow, and shoulder joints). Using a virtual stiffness discrimination task, a four-session psychophysical experiment was conducted with 38 participants (25 male and 13 female); each session was conducted with one of the four joints as the pivot joint during haptic exploration. The participants were asked to judge the stiffness of the top surface of two computer-generated cylinders by determining the stiffer one while using their dominant hand’s index finger. A two-alternative forced-choice procedure was employed by assigning one cylinder a constant stiffness value of 1.0 N/mm (standard side) and the remaining cylinder a variable stiffness value (comparison side). Using a custom-made stylus for the Geomagic TouchTM (3D Systems, Inc., Rock Hill, SC, USA) haptic interface, the participants were able to feel the stiffness of these virtual surfaces only with their index fingers. It was observed that the average Weber fraction monotonically decreased as the pivot joint shifted toward the torso (i.e., a shift from the metacarpophalangeal joint to the shoulder joint); this decrease was not statistically significant, which suggests that the selection of the pivot joint was not a determining factor for the sensitivity to discriminate stiffness. In general, the palpation speed and force exerted by the participants on the standard side during the haptic exploration showed a tendency to increase when the pivot joint shifted toward the torso; the difference in average palpation speed and force across the pivot joints was not statistically significant.
Magnetoresistance of vertical Co-graphene-NiFe junctions controlled by charge transfer and proximity-induced spin splitting in graphene

Graphene is hailed as an ideal material for spintronics due to weak intrinsic spin–orbit interaction that facilitates lateral spin transport and tunability of its electronic properties, including a possibility to induce magnetism in graphene. Another promising application of graphene is related to its use as a spacer separating ferromagnetic metals (FMs) in vertical magnetoresistive devices, the most prominent class of spintronic devices widely used as magnetic sensors. In particular, few-layer graphene was predicted to act as a perfect spin filter. Here we show that the role of graphene in such devices (at least in the absence of epitaxial alignment between graphene and the FMs) is different and determined by proximity-induced spin splitting and charge transfer with adjacent ferromagnetic metals, making graphene a weak FM electrode rather than a spin filter. To this end, we report observations of magnetoresistance (MR) in vertical Co-graphene-NiFe junctions with 1–4 graphene layers separating the ferromagnets, and demonstrate that the dependence of the MR sign on the number of layers and its inversion at relatively small bias voltages is consistent with spin transport between weakly doped and differently spin-polarized layers of graphene. The proposed interpretation is supported by the observation of an MR sign reversal in biased Co-graphene-hBN-NiFe devices and by comprehensive structural characterization. Our results suggest a new architecture for vertical devices with electrically controlled MR.