Miracle-dz/UniFAR-FTUs huggingface dataset:
Flat Rotation Curves Found in Merging Dusty Starbursts at z = 2.3 through Tilted-ring Modeling

The brightest 500 μm source in the XMM-LSS field, HXMM01, is a rare merger of luminous starburst galaxies at z = 2.3 with a dust-obscured star formation rate of 2000 M⊙ yr−1. Here we present high-resolution spectroscopic observations of HXMM01 with the Atacama Large Millimeter/submillimeter Array (ALMA). We detect line emission from CO J = 7 → 6, [C i] 3P2 → 3P1, and p-H2O 211 → 202 and continuum emission at 230 GHz. At a spatial resolution of 0. ″2 and a spectral resolution of 40 km s−1, the source is resolved into three distinct components, which are spatially and dynamically associated within a projected radius of 20 kpc and a radial velocity range of 2000 km s−1. For two major components, our Bayesian-based tilted-ring modeling of the ALMA spectral cubes shows almost flat rotation curves peaking at ∼500 km s−1 at galactocentric distances between 2 and 5 kpc. Each of them has a dynamical mass of ∼1011 M⊙. The combination of the dynamical masses and the archival CO J = 1 → 0 data places strong upper limits on the CO → H2 conversion factor of αCO ≲ 1.4–2.0 M⊙(K km s−1 pc2)−1. These limits are significantly below the Galactic inner disk αCO value of 4.3 M⊙(K km s−1 pc2)−1 but are consistent with those of local starbursts. Therefore, the previously estimated short gas depletion timescale of ∼200 Myr remains unchanged.
Polaronic quantum diffusion in dynamic localization regime

We investigate the quantum dynamics in a disordered electronic lattice by the time-dependent density matrix renormalization group algorithm. The on-site energy in the lattice follows the Fibonacci sequence and the electron off-diagonally couples to a sub-Ohmic phonon bath. It is found that the slope of the inverse participation ratio versus the coupling strength undergoes a sudden change that indicates a transition from static to dynamic localization, and that the generated polarons coherently diffuse via hopping-like processes, evidenced by the saturated entanglement entropy, providing a novel scenario for a transportation mechanism in strongly disordered systems. Moreover, the mean-square displacement is revealed to be insensitive to the coupling strength, implying the quantum diffusion behavior survives the energy disorder that prevails in real organic materials.
Monetary Policy Communication and Financial Markets in India

IMF Working Papers describe research in progress by the author(s) and are published to elicit comments and to encourage debate. The views expressed in IMF Working Papers are those of the author(s) and do not necessarily represent the views of the IMF, its Executive Board, or IMF management. ABSTRACT: Forward-looking monetary policy communication has become a key element of flexible inflation-targeting regimes across advanced and emerging market economies. The Reserve Bank of India’s implementation of a flexible inflation targeting framework since 2016 has been supported by a broad set of communication tools, more recently aided by policy innovations such as forward guidance on policy rates and, asset purchases, increasing the predictability of monetary policy. A review of the recent innovations of monetary policy communications during the initial waves of the pandemic suggests forward guidance likely played a key role in moderating uncertainty and supporting some asset prices. We also find that the relationship between monetary policy surprises and yields for government and corporate securities across all maturities are positive and statistically significant. The results support an important role for monetary policy communication in guiding market expectations about the monetary policy stance, including the likely path of policy interest rates. unanticipated and anticipated policy changes constructed from analysts’ surveys. The results are broadly consistent with those from Tables 3 and 4. The monetary policy surprises, unanticipated changes in the policy rate, on average, have statistically significant impact on the government security and corporate yields, and no effect on the exchange rate and stock market. In their exercise for Indonesia in Ahokpossi et al. (2020) show that the monetary policy surprises have significant impact on the money market rates but not on the bond yields, attributing this to a shallow financial market and incomplete yield curve. However, the findings here suggest that monetary policy surprises impact yields at all maturities are similar to Pescatori (2018), which examines the impact of unanticipated monetary policy changes in Chile.
Star Formation at z = 2.481 in the Lensed Galaxy SDSS J1110+6459. II. What is Missed at the Normal Resolution of the Hubble Space Telescope?

For lensed galaxy SGAS J111020.0+645950.8 at redshift z = 2.481, which is magnified by a factor of 28 ± 8, we analyze the morphology of star formation, as traced by rest-frame ultraviolet emission, in both the highly magnified source plane and simulations of how this galaxy would appear without lensing magnification. Were this galaxy not lensed, but rather drawn from a Hubble Space Telescope deep field, we would conclude that almost all its star formation arises from an exponential disk (Sérsic index of 1.0 ± 0.4) with an effective radius of measured from two-dimensional fitting to F606W using Galfit, and measured by fitting a radial profile to F606W elliptical isophotes. At the normal spatial resolution of the deep fields, there is no sign of clumpy star formation within SGAS J111020.0+645950.8. However, the enhanced spatial resolution enabled by gravitational lensing tells a very different story; much of the star formation arises in two dozen clumps with sizes of r = 30–50 pc spread across the 7 kpc length of the galaxy. The color and spatial distribution of the diffuse component suggests that still-smaller clumps are unresolved. Despite this clumpy, messy morphology, the radial profile is still well-characterized by an exponential profile. In this lensed galaxy, stars are forming in complexes with sizes well below 100 pc; such sizes are wholly unexplored by surveys of galaxy evolution at .
Mesoscopic effects in quantum phases of ultracold quantum gases in optical lattices

We present a wide array of quantum measures on numerical solutions of one-dimensional Bose- and Fermi-Hubbard Hamiltonians for finite-size systems with open boundary conditions. Finite-size effects are highly relevant to ultracold quantum gases in optical lattices, where an external trap creates smaller effective regions in the form of the celebrated 'wedding cake' structure and the local density approximation is often not applicable. Specifically, for the Bose-Hubbard Hamiltonian we calculate number, quantum depletion, local von Neumann entropy, generalized entanglement or Q measure, fidelity, and fidelity susceptibility; for the Fermi-Hubbard Hamiltonian we also calculate the pairing correlations, magnetization, charge-density correlations, and antiferromagnetic structure factor. Our numerical method is imaginary time propagation via time-evolving block decimation. As part of our study we provide a careful comparison of canonical versus grand canonical ensembles and Gutzwiller versus entangled simulations. The most striking effect of finite size occurs for bosons: we observe a strong blurring of the tips of the Mott lobes accompanied by higher depletion, and show how the location of the first Mott lobe tip approaches the thermodynamic value as a function of system size.
Theory of magnetization precession induced by a picosecond strain pulse in ferromagnetic semiconductor (Ga,Mn)As

A theoretical model of the coherent precession of magnetization excited by a picosecond acoustic pulse in a ferromagnetic semiconductor layer of (Ga,Mn)As is developed. The short strain pulse injected into the ferromagnetic layer modifies the magnetocrystalline anisotropy resulting in a tilt of the equilibrium orientation of magnetization and subsequent magnetization precession. We derive a quantitative model of this effect using the Landau-Lifshitz equation for the magnetization that is precessing in the time-dependent effective magnetic field. After developing the general formalism, we then provide a numerical analysis for a certain structure and two typical experimental geometries in which an external magnetic field is applied either along the hard or the easy magnetization axis. As a result we identify three main factors, which determine the precession amplitude: the magnetocrystalline anisotropy of the ferromagnetic layer, its thickness, and the strain pulse parameters.
Space-Efficient Storage Structure of Blockchain Transactions Supporting Secure Verification

The rapid growth of the blockchain size is a major bottleneck hindering its implementations in data-heavy applications. Current efforts improve the distributed storage ways and transactions’ storage mechanisms of blockchain, however, the blockchain distribution and integrity are destroyed. Simplified Payment Verification (SPV) is closely related to blockchain storage, but the current solutions did not explore the privacy-preserving SPV. In this paper, we propose a new storage structure for blockchain transactions, called Coloring Index (CI), to reduce the blockchain's space occupation. Specifically, we devise an index building algorithm to simply calculate the indices of transactions for the sake of information concealing. By improving the Coloring Embedder for multi-sets query, we can store the indices into the Coloring Embedder to achieve the structured storage of transactions with small space occupation. Using CI, SPV query proceeds without revealing the user's address, thereby achieving secure data sharing in applications such as the intelligent vehicles’ communications and distributed IoT. We prove CI's security against malicious full nodes when establishing possible connections between the address and the user. The experiments show that blockchain systems using our CI store one time more transactions than Merkle tree and half more than Bloom filter.
Addressing Barriers to Mental Health Wellness: Prescriptions for Marketing

The rising number of adults living with emotional and mental health challenges is a growing concern. This research examines specific barriers that may preclude individuals from achieving mental health wellness. A model (n = 382) is tested using individuals from the millennial generational cohort to outline key factors that contribute to negative behaviors and barriers that impede mental health engagement. Findings indicate that perceived stigma related to mental health conditions is negatively associated with mental health engagement and positively related to efforts to self-treat by using consumption to manage emotional distress. Trust in a mental health care provider is positively related to interest in seeking help for a mental health condition (motivation) and mental health literacy (ability). Furthermore, interest in seeking help, mental health literacy, and access to mental health services (opportunity) are also positively related to mental health engagement. The authors offer prescriptions for social marketing and public policy to help reduce obstacles to mental health wellness and to encourage the consumption of mental health services. These recommendations are put forth with the intention of heightening mental health engagement and increasing mental health care access such that consumer and societal well-being are enhanced.
Effect of Longitudinal Practice in Real and Virtual Environments on Motor Performance, Physical Activity and Enjoyment in People with Autism Spectrum Disorder: A Prospective Randomized Crossover Controlled Trial

(1) Background: People with ASD commonly present difficulty performing motor skills and a decline in physical activity (PA) level and low enjoyment of PA. We aimed to evaluate whether longitudinal practice of an activity in virtual and real environments improves motor performance and whether this improvement is transferred to a subsequent practice when changing the environment, promoting PA and providing enjoyment; (2) Methods: People with ASD, aged between 10 and 16 years, were included and distributed randomly into two opposite sequences. The participants performed a 10 session protocol, with five sessions practicing in each environment (virtual or real). Heart rate measurement was carried out and an enjoyment scale was applied; (3) Results: 22 participants concluded the protocol. Sequence A (virtual first) presented an improvement in accuracy and precision and transferred this when changing environment; they also had a greater change in heart rate reserve. The majority of participants reported “fun” and “great fun” levels for enjoyment; (4) Conclusions: The virtual reality activity presented a higher level of difficulty, with greater gains in terms of transference to the real environment. Considering PA, our task provided very light to light activity and the majority of participants enjoyed the task.
Neutron star equation of state via gravitational wave observations

Gravitational wave observations can potentially measure properties of neutron star equations of state by measuring departures from the point-particle limit of the gravitational waveform produced in the late inspiral of a neutron star binary. Numerical simulations of inspiraling neutron star binaries computed for equations of state with varying stiffness are compared. As the stars approach their final plunge and merger, the gravitational wave phase accumulates more rapidly if the neutron stars are more compact. This suggests that gravitational wave observations at frequencies around 1 kHz will be able to measure a compactness parameter and place stringent bounds on possible neutron star equations of state. Advanced laser interferometric gravitational wave observatories will be able to tune their frequency band to optimize sensitivity in the required frequency range to make sensitive measures of the late-inspiral phase of the coalescence.
Searching for the lost Unicorn: a prominent feature in the radial velocity distribution of stars in Vela from Gaia DR2 data

Stellar streams are ubiquitous in the Galactic halo and they can be used to improve our understanding of the formation and evolution of the Milky Way as a whole. The so-called Monoceros Ring might have been the result of satellite accretion. Guglielmo et al. have used N-body simulations to search for the progenitor of this structure. Their analysis shows that, if the Ring has a dwarf galaxy progenitor, it might be found in the background of one out of eight specific areas in the sky. Here, we use Gaia DR2 data to perform a systematic exploration aimed at confirming or rejecting this remarkable prediction. Focusing on the values of the radial velocity to uncover possible multimodal spreads, we identify a bimodal Gaussian distribution towards Galactic coordinates (l, b) = (271, +2) degrees in Vela, which is one of the locations of the progenitor proposed by Guglielmo et al. This prominent feature with central values 60+/-7 km/s and 97+/-10 km/s, may signal the presence of the long sought progenitor of the Monoceros Ring, but the data might also be compatible with the existence of an unrelated, previously unknown, kinematically coherent structure.
PRE-SPECTROSCOPIC FALSE-POSITIVE ELIMINATION OF KEPLER PLANET CANDIDATES

Ten days of commissioning data (Quarter 0) and 33 days of science data (Quarter 1) yield instrumental flux time series of ∼150,000 stars that were combed for transit events, termed threshold crossing events(TCE), each having a total detection statistic above 7. 1σ. TCE light curves are modeled as star+planet systems. Those returning a companion radius smaller than 2RJ are assigned a Kepler Object of Interest (KOI) number. The raw flux, pixel flux, and flux-weighted centroids of every KOI are scrutinized to assess the likelihood of being an astrophysical false positive versus the likelihood of being a planetary companion. This vetting using Kepler data is referred to as data validation (DV). Herein, we describe the DV metrics and graphics used to identify viable planet candidates amongst the KOIs. Light curve modeling tests for (1) the difference in depth of the odd- versus even-numbered transits, (2) evidence of ellipsoidal variations, and (3) evidence of a secondary eclipse event at phase = 0.5. Flux-weighted centroids are used to test for signals correlated with transit events with a magnitude and direction indicative of a background eclipsing binary. Centroid time series are complimented by analysis of images taken in-transit versus out-of-transit, the difference often revealing the pixel contributing the most to the flux change during transit. Examples are shown to illustrate each test. Candidates passing DV are submitted to ground-based observers for further false-positive elimination or confirmation/characterization.
Identification and Estimation of Quantum Linear Input-Output Systems

The system identification problem is to estimate dynamical parameters from the output data, obtained by performing measurements on the output fields. We investigate system identification for quantum linear systems. Our main objectives are to address the following general problems: (1) Which parameters can be identified by measuring the output? (2) How can we construct a system realisation from sufficient input-output data? (3) How well can we estimate the parameters governing the dynamics? We investigate these problems in two contrasting approaches; using time-dependent inputs (Sec. 3.7.1 or time-stationary (quantum noise) inputs (Sec. 3.7.2). In the time-dependent approach, the output fields are characterised by the transfer function. We show that indistinguishable minimal systems in the transfer function are related by symplectic transformations acting on the space of system modes (Ch. 6). We also present techniques enabling one to find a physical realisation of the system from the input-output data. We present realistic schemes for estimating passive quantum linear systems at the Heisenberg limit (Ch. 7) under energy resource constraint. ‘Realistic’ is our primary concern here, in the sense that there exists both experimentally feasible states and practical measurement choices that enable this heightened performance for all passive quantum linear systems. We consider both single parameter and multiple parameter estimation. In the stationary approach, the characteristic quantity is the power spectrum. We define the notion of global minimality for a given power spectrum, and characterise globally minimal systems as those with fully mixed stationary state (Sec. 6.1). The power spectrum depends on the system parameters via the transfer function. Our main result here is that under global minimality the power spectrum uniquely determines the transfer function, so the system can be identified up to a symplectic transformation (see Secs. 6.5, 6.4 6.11). We also give methods for constructing a globally minimal subsystem directly from the power spectrum (see Sec. 6.3). These results hold for pure inputs, we discuss extensions to mixed inputs and the use of additional input channels; using an appropriately chosen input in the latter case ensures that the system is always globally minimal (hence identifiable). Finally, we discuss a particular feedback control estimation problem in Chs. 8 and 9. In general, information about a parameter within a quantum linear system may be obtained at a linear rate with respect to time (in both approaches above); the so-called standard scaling. However, we see that when the system destabilises, so that its system matrix has eigenvalues very close to the imaginary axis, the quantum Fisher information is enhanced, to quadratic (Heisenberg) level. We give feedback methods enabling one to destabilise the system and give adaptive procedures for realising the Heisenberg bounds.
Social Work Students’ Self-Efficacy Toward Direct Practice Skills in Field Education Using Virtual Simulations and Scripted Role Plays

Simulations with professional actors and scripted role plays with peers are effective methods to increase direct practice skills. However, little is known about how simulations or scripted role plays conducted virtually can influence social work students' practice self-efficacy. MSW students enrolled in field seminar courses across two universities were invited to participate in an exploratory, repeated measures assessment utilizing the Counselor Activity Self-Efficacy Scales (CASES). One university (n=100) implemented the use of standardized clients, played by professional actors within field seminar; the other university (n=61) implemented scripted, peer-led role plays. Significant differences were found in pre/post scores among MSW students that participated in simulated client experiences within their field seminar. Simulations and scripted peer role plays may need to be more integrated into social work curricula when opportunities for in-person direct practice skill development are limited due to hybrid or fully remote field placements. Applied learning in social work education must be re-envisioned so programs can prepare MSW students to be effective practitioners in today’s rapidly changing environment.
The supermassive black hole and double nucleus of the core elliptical NGC 5419

We obtained adaptive-optics assisted SINFONI observations of the central regions of the giant elliptical galaxy NGC 5419 with a spatial resolution of 0.2 arcsec (approximate to 55 pc). NGC 5419 has a large depleted stellar core with a radius of 1.58 arcsec (430 pc). HST and SINFONI images show a point source located at the galaxy's photocentre, which is likely associated with the low-luminosity AGN previously detected in NGC 5419. Both the HST and SINFONI images also show a second nucleus, off-centred by 0.25 arcsec (approximate to 70 pc). Outside of the central double nucleus, we measure an almost constant velocity dispersion of sigma similar to 350 km s(-1). In the region where the double nucleus is located, the dispersion rises steeply to a peak value of similar to 420 km s(-1). In addition to the SINFONI data, we also obtained stellar kinematics at larger radii from the South African Large Telescope. While NGC 5419 shows low rotation (v < 50 km s(-1)), the central regions (inside similar to 4 r(b)) clearly rotate in the opposite direction to the galaxy's outer parts. We use orbit-based dynamical models to measure the black hole mass of NGC 5419 from the kinematical data outside of the double nuclear structure. The models imply M-BH = 7.2(-1.9)(+2.7) x 10(9) M-circle dot. The enhanced velocity dispersion in the region of the double nucleus suggests that NGC 5419 possibly hosts two supermassive black holes at its centre, separated by only approximate to 70 pc. Yet our measured M-BH is consistent with the black hole mass expected from the size of the galaxy's depleted stellar core. This suggests, that systematic uncertainties in MBH related to the secondary nucleus are small.
A Multi-Indicator Fusion-Based Approach for Fault Feature Selection and Classification of Rolling Bearings

Concerning the problems of harrowing extraction and poor classification accuracy of fault features in rolling bearing vibration signals, a fault feature selection and classification method based on multi-indicator fusion is proposed. First, the original signal is decomposed through the improved complementary ensemble local mean decomposition method into several physically meaningful product functions (PF) and single residual components; then, the three indicators of kurtosis, correlation coefficient, and Kulback–Leibler divergence are combined to extract the most suitable PF components for signal reconstruction. Ultimately, the reconstructed signal's multidomain characteristics and entropy value features are retrieved and fed into the LightGBM classifier for classification in order to achieve an intelligent diagnosis of rolling bearing problems. The statistical results demonstrate that the proposed method can efficiently identify the functional PF components and has notable benefits in extracting features from diverse experimental datasets and detecting faults.