Miracle-dz/UniFAR-FTUs huggingface dataset:
Spatially Resolved Stellar Kinematics of the Ultra-diffuse Galaxy Dragonfly 44. I. Observations, Kinematics, and Cold Dark Matter Halo Fits

We present spatially resolved stellar kinematics of the well-studied ultra-diffuse galaxy (UDG) Dragonfly 44, as determined from 25.3 hr of observations with the Keck Cosmic Web Imager. The luminosity-weighted dispersion within the half-light radius is km s−1, lower than what we had inferred before from a DEIMOS spectrum in the Hα region. There is no evidence for rotation, with (90% confidence) along the major axis, in possible conflict with models where UDGs are the high-spin tail of the normal dwarf galaxy distribution. The spatially averaged line profile is more peaked than a Gaussian, with Gauss–Hermite coefficient h4 = 0.13 ± 0.05. The mass-to-light ratio (M/L) within the effective radius is M⊙/L⊙, similar to other UDGs and higher by a factor of six than smaller galaxies of the same luminosity. This difference between UDGs and other galaxies is, however, sensitive to the aperture that is used, and it is much reduced when the M/L ratios are measured within a fixed radius of 10 kpc. Dragonfly 44 has a rising velocity dispersion profile, from km s−1 at R = 0.2 kpc to km s−1 at R = 5.1 kpc. The profile can only be fit with a cuspy Navarro–Frenk–White profile if the orbital distribution has strong tangential anisotropy, with . An alternative explanation is that the dark matter profile has a core: a Di Cintio et al. density profile with a mass-dependent core provides a very good fit to the kinematics for a halo mass of and , i.e., isotropic orbits. This model predicts a slight positive kurtosis, in qualitative agreement with the measured h4 parameter. UDGs such as Dragonfly 44 are dark matter dominated even in their centers and can constrain the properties of dark matter in a regime where baryons usually dominate the kinematics: small spatial scales in massive halos. In a companion paper we provide constraints on the axion mass in the context of “fuzzy” dark matter models.
The supernova rate and delay time distribution in the Magellanic Clouds

We use the supernova remnants (SNRs) in the two Magellanic Clouds (MCs) as a supernova (SN) survey, ‘conducted’ over tens of kyr, from which we derive the current SN rate, and the SN delay time distribution (DTD), i.e. the SN rate versus time that would follow a hypothetical brief burst of a star formation. In a companion paper we have compiled a list of 77 SNRs in the MCs, and argued that it is a fairly complete record of the SNRs that are now in the Sedov phase of their expansions. We recover the SN DTD by comparing the numbers of SNRs observed in small individual ‘cells’ in these galaxies to the star formation histories of each cell, as calculated from resolved stellar populations by Harris & Zaritsky. We identify the visibility times of SNRs in each cell with the Sedov-phase lifetimes, which depend on the local ambient densities. The local densities are estimated from 21-cm emission, from an inverse Schmidt– Kennicutt law based on either Hα emission or the star formation rate from the resolved stellar populations, and from combinations of these tracers. This is the first SN DTD that is based on resolved stellar populations. We detect a population of ‘prompt’ Type Ia SNe (that explode within 330 Myr of star formation) at >99 per cent confidence level (CL). The best fit for the number of prompt Type Ia SNe per stellar mass formed is 2.7–11.0 × 10 −3 M −1 � , depending on the density tracer used. The 95 per cent CL range for a ‘delayed’ (from 330 Myr to a Hubble time) Type Ia component is <1.6 × 10 −13 SN yr −1 M −1 � , consistent with rate measurements in old populations. The current total (core-collapse+Ia) SN rate in the MCs is 2.5–4.6 SNe per millennium (68 per cent CL+systematics), or 1.7–3.1 SNuM [SNe (100 yr 10 10 M� ) −1 ], in agreement with the historical record and with rates measured in other dwarf irregulars. Conversely, assuming the SNRs are in free expansion, rather than in their Sedov phase, would impose on the SNRs a maximum age of 6 kyr, and would imply an MC SN rate per unit mass that is five times higher than in any type of galaxy, and a low-mass limit for core-collapse progenitors in conflict with stellar evolution theory.
The RCB star V854 Centauri is surrounded by a hot dusty shell

Aims : The hydrogen-deficient supergiants known as R Coronae Borealis (RCB) stars might be the result of a double-degenerate merger of two white dwarfs (WDs), or a final helium shell flash in a planetary nebula central star. In this context, any information on the geometry of their circumstellar environment and, in particular, the potential detection of elongated structures, is of great importance. Methods : We obtained near-IR observations of V854 Cen with the AMBER recombiner located at the Very Large Telescope Interferometer (VLTI) array with the compact array (B$\leq$35m) in 2013 and the long array (B$\leq$140m) in 2014. At each time, V854 Cen was at maximum light. The $H$- and $K$-band continua were investigated by means of spectrally dependant geometric models. These data were supplemented with mid-IR VISIR/VLT images. Results : A dusty slightly elongated over density is discovered both in the $H$- and $K$-band images. With the compact array, the central star is unresolved ($\Theta\leq2.5$\,mas), but a flattened dusty environment of $8 \times 11$ mas is discovered whose flux increases from about $\sim$20% in the $H$ band to reach about $\sim$50% at 2.3$\micron$, which indicates hot (T$\sim$1500\,K) dust in the close vicinity of the star. The major axis is oriented at a position angle (P.A.) of 126$\pm$29$\deg$. Adding the long-array configuration dataset provides tighter constraints on the star diameter ($\Theta\leq1.0$ mas), a slight increase of the overdensity to $12 \times 15$ mas and a consistent P.A. of 133$\pm$49$\deg$. The closure phases, sensitive to asymmetries, are null and compatible with a centro-symmetric, unperturbed environment excluding point sources at the level of 3% of the total flux in 2013 and 2014. The VISIR images exhibit a flattened aspect ratio at the 15-20% level at larger distances ($\sim$1$\arcsec$) with a position angle of 92$\pm$19$\deg$, marginally consistent with the interferometric observations. Conclusions : This is the first time that a moderately elongated structure has been observed around an RCB star. These observations confirm the numerous suggestions for a bipolar structure proposed for this star in the literature, which were mainly based on polarimetric and spectroscopic observations.
Optical nanoscopy via quantum control

We present a scheme for nanoscopic imaging of a quantum mechanical two-level system using an optical probe in the far-field. Existing super-resolution schemes require more than two-levels and depend on an incoherent response to the lasers. Here, quantum control of the two states proceeds via rapid adiabatic passage. We implement this scheme on an array of semiconductor self-assembled quantum dots. Each quantum dot results in a bright spot in the image with extents down to 30 nm ({\lambda}/31). Rapid adiabatic passage is established as a versatile tool in the super-resolution toolbox.
Accelerated expansion of the Universe in a higher dimensional modified gravity with Euler-Poincaré terms

A higher dimensional modified gravity theory with an action that includes dimensionally continued Euler-Poincaré forms up to second order in curvatures is considered. The variational field equations are derived. Matter in the Universe at large scales is modeled by a fluid satisfying an equation of state with dimensional dichotomy. We study solutions that describe higher dimensional steady state cosmologies with constant volume for which the three dimensional external space is expanding at an accelerated rate while the (compact) internal space is contracting. We showed that the second order Euler-Poincaré term in the constructions of higher dimensional steady state cosmologies could be crucial.
The Influence of Increased Dairy Product Consumption, as Part of a Lifestyle Modification Intervention, on Diet Quality and Eating Patterns in Female Adolescents with Overweight/Obesity

Our study examined how increased dairy consumption versus habitually low dairy consumption, against a background of healthy eating (and exercise), influenced diet quality, nutrient intake, and snacking in Canadian female adolescents (14.8 ± 2.2 years) with overweight/obesity (OW/OB). We also explored dairy consumption patterns in the group consuming dairy products. Participants were randomized into two groups: higher/recommended dairy (RDa; 4 svg/d; n = 24) or low dairy (LDa; 0–2 svg/d; n = 23). Both groups participated in a 12-week, eucaloric, lifestyle modification intervention consisting of exercise training and nutritional counseling. The intervention increased the total Canadian Healthy Eating Index score (p < 0.001) with no differences between groups. The “other food” sub-score improved more in RDa than LDa (p = 0.02), and the “saturated fat” sub-score increased more in LDa than RDa (p = 0.02). The intervention significantly increased the consumption of dairy-related nutrients more in RDa than LDa (p < 0.05). The intervention also decreased snack size in both groups (p = 0.01) and improved percentage of healthy snack energy intake more in RDa than LDa (p = 0.04). More servings of dairy products were consumed as snacks than at breakfast, lunch, or dinner (p < 0.05). Thus, our study improved diet quality, and dairy product consumption improved intakes of key related nutrients and snack consumption in adolescents with OW/OB.
Antianxiety and antidepressant effects of aqueous latex extract of Euphorbia resinifera

This study aims to examine the antianxiety and antidepressant effects of aqueous latex extract of Euphorbia resinifera in mice. Antianxiety and sedative effects were examined using the elevated plus maze test, open field test, and thiopental-induced sleeping time respectively. While the antidepressant effect was evaluated, using the forced swimming test. E. resinifera reduced the latency of sleeping and increased sleeping time significantly at 75 mg/kg. It reduced the immobility time and increased swimming significantly at all doses assessed (25, 50, and 75 mg/kg). Pretreatment with antagonists reversed these effects indicating the possible involvement of α2, 5HT2, D2, and GABAA receptors respectively. These findings confirm the traditional utilization of this plant as an antioxidant, anxiolytic, and antidepressant.
Gravitational wave background from binary systems

Basic aspects of the background of gravitational waves and its mathematical characterization are reviewed. The spectral energy density parameter {Omega}(f), commonly used as a quantifier of the background, is derived for an ensemble of many identical sources emitting at different times and locations. For such an ensemble, {Omega}(f) is generalized to account for the duration of the signals and of the observation, so that one can distinguish the resolvable and unresolvable parts of the background. The unresolvable part, often called confusion noise or stochastic background, is made by signals that cannot be either individually identified or subtracted out of the data. To account for the resolvability of the background, the overlap function is introduced. This function is a generalization of the duty cycle, which has been commonly used in the literature, in some cases leading to incorrect results. The spectra produced by binary systems (stellar binaries and massive black hole binaries) are presented over the frequencies of all existing and planned detectors. A semi-analytical formula for {Omega}(f) is derived in the case of stellar binaries (containing white dwarfs, neutron stars or stellar-mass black holes). Besides a realistic expectation of the level of background, upper and lower limits are given, tomore » account for the uncertainties in some astrophysical parameters such as binary coalescence rates. One interesting result concerns all current and planned ground-based detectors (including the Einstein Telescope). In their frequency range, the background of binaries is resolvable and only sporadically present. In other words, there is no stochastic background of binaries for ground-based detectors. « less
A HIGH-RESOLUTION STUDY OF THE ATOMIC HYDROGEN IN CO-RICH EARLY-TYPE GALAXIES

We present an analysis of new and archival Very Large Array H i observations of a sample of 11 early-type galaxies rich in CO, with detailed comparisons of CO and H i distributions and kinematics. The early-type sample consists of both lenticular and elliptical galaxies in a variety of environments. A range of morphologies and environments were selected in order to give a broader understanding of the origins, distribution, and fate of the cold gas in early-type galaxies. Six of the eleven galaxies in the sample are detected in both H i and CO. The H2 to H i mass ratios for this sample range from 0.2 to 120. The H i morphologies of the sample are consistent with that of recent H i surveys of early-type galaxies, which also find a mix of H i morphologies and masses, low H i peak surface densities, and a lack of H i in early-type galaxies that reside in high-density environments. The HI-detected galaxies have a wide range of H i masses (1.4 × 106 to 1.1 × 1010 M☉). There does not appear to be any correlation between the H i mass and morphology (E versus S0). When H i is detected, it is centrally peaked—there are no central kiloparsec-scale central H i depressions like those observed for early-type spiral galaxies at similar spatial resolutions and scales. A kinematic comparison between the H i and CO indicates that both cold gas components share the same origin. The primary goal of this and a series of future papers is to better understand the relationship between the atomic and molecular gas in early-type galaxies, and to compare the observed relationships with those of spiral galaxies where this relationship has been studied in depth.
Probing untouchable environment as a resource for quantum computing

When manipulating a quantum system S, its surrounding system, or environment, E induces unwanted effects. It is mainly due to its vastness and the lack of knowledge about the Hamiltonian HSE that governs the dynamics inside E and the interaction with S. The detail of HSE is usually extremely hard to identify, since E can hardly be measured or controlled directly. Nevertheless, here we show that it is possible to probe and control a part of, if not all, the dynamics involving E, within the timescale in which its effective dimension can be seen finite. That is, we may be able to let a noisy environment work in our favor as a part of quantum computer.
Comment on “Construction of regular black holes in general relativity”

We claim that the physical parameters of the constructed black hole solutions in general relativity (GR) coupled to nonlinear electrodynamics (NED) by Zhong-Ying Fan and Xiaobao Wang in the Paper [Phys. Rev. D 94, 124027 (2016)] are misinterpreted, despite the formalism being correct. We argue that because of these misinterpretations, the derived black hole solutions and the Lagrangian densities presented in that paper are slightly inconsistent. In this comment, we present complete black hole solutions of the given Lagrangian densities which correct the interpretation of the physical parameters of the constructed black hole solutions and lead to the correct treatment and weak field limits of the physical parameters of the constructed solutions.
Halo Concentrations and the New Baseline X-Ray Luminosity–Temperature and Mass Relations of Galaxy Clusters

The standard self-similar model of galaxy cluster formation predicts that the X-ray luminosity–temperature (LX–TX) relation of galaxy clusters should have been L X ∝ T X 2 in absence of the baryonic physics, such as radiative cooling and feedback from stars and black holes. However, this baseline relation is predicted without considering the fact that the halo concentration and the characteristic density of clusters increases as their mass decreases, which is a consequence of hierarchical structure formation of the universe. Here, we show that the actual baseline relation should be L X ∝ T X α , where α ∼ 1.7, instead of α = 2, given the mass dependence of the concentration and the fundamental plane relation of galaxy clusters. Numerical simulations show that α ∼ 1.6, which is consistent with the prediction. We also show that the baseline luminosity–mass (LX–MΔ) relation should have been L X ∝ M Δ β , where β ∼ 1.1–1.2, in contrast with the conventional prediction (β = 4/3). In addition, some of the scatter in the LX–MΔ relation can be attributed to the scatter in the concentration–mass (c–M) relation. The confirmation of the shallow slope could be proof of hierarchical clustering. As an example, we show that the new baseline relations could be checked by studying the temperature or mass dependence of gas mass fraction of clusters. Moreover, the highest-temperature clusters would follow the shallow baseline relations if the influences of cool cores and cluster mergers are properly removed.
Greenberger-Horne-Zeilinger generation protocol for $N$ superconducting transmon qubits capacitively coupled to a quantum bus

We propose a circuit quantum electrodynamics (QED) realization of a protocol to generate a Greenberger-Horne-Zeilinger (GHZ) state for $N$ superconducting transmon qubits homogeneously coupled to a superconducting transmission line resonator in the dispersive limit. We derive an effective Hamiltonian with pairwise qubit exchange interactions of the XY type, $\tilde{g}(XX+YY)$, that can be globally controlled. Starting from a separable initial state, these interactions allow to generate a multi-qubit GHZ state within a time $t_{\text{GHZ}}\sim \tilde{g}^{-1}$. We discuss how to probe the non-local nature and the genuine $N$-partite entanglement of the generated state. Finally, we investigate the stability of the proposed scheme to inhomogeneities in the physical parameters.
Ultrafast nanoscale magnetic switching via intense picosecond electron bunches

The magnetic field associated with a picosecond intense electron pulse is shown to switch locally the magnetization of extended films and nanostructures and to ignite locally spin waves excitations. Also topologically protected magnetic textures such as skyrmions can be imprinted swiftly in a sample with a residual Dzyaloshinskii-Moriya spin-orbital coupling. Characteristics of the created excitations such as the topological charge or the width of the magnon spectrum can be steered via the duration and the strength of the electron pulses. The study points to a possible way for a spatiotemporally controlled generation of magnetic and skyrmionic excitations.
Shock wave collisions in AdS5: approximate numerical solutions

We numerically study the evolution of a boost-invariant N=4 SYM medium using AdS/CFT. We consider a toy model for the collision of gravitational shock waves, finding that the energy density first increases, reaches a maximum and then starts to decrease, matching hydrodynamics for late times. For the initial conditions we consider, the hydrodynamic scale governing the late time behaviour is to very good approximation determined by the area of the black hole horizon at initial times. Our results provide a toy model for the early time evolution of the bulk system in heavy-ion collisions at RHIC and the LHC.
Fitting functions for a disk-galaxy model with different ΛCDM-halo profiles

We present an adaptation of the standard scenario of disk-galaxy formation to the concordant LCDM cosmology aimed to derive analytical expressions for the scale length and rotation speed of present-day disks that form within four different, cosmologically motivated protogalactic dark matter halo-density profiles. We invoke a standard galaxy-formation model that includes virial equilibrium of spherical dark halos, specific angular momentum conservation during gas cooling, and adiabatic halo response to the gas inflow. The mean mass-fraction and mass-to-light ratio of the central stellar disk are treated as free parameters whose values are tuned to match the zero points of the observed size-luminosity and circular speed-luminosity relations of galaxies. We supply analytical formulas for the characteristic size and rotation speed of disks built inside Einasto r^{1/6}, Hernquist, Burkert, and Navarro-Frenk-White dark matter halos. These expressions match simultaneously the observed zero points and slopes of the different correlations that can be built in the RVL space of disk galaxies from plausible values of the galaxy- and star-formation efficiencies.
Strong vorticity fluctuations and antiferromagnetic correlations in axisymmetric fluid equilibria

The macroscale structure and microscale fluctuation statistics of late-time asymptotic steady state flows in cylindrical geometries is studied using the methods of equilibrium statistical mechanics. The axisymmetric assumption permits an effective two-dimensional description in terms of the (toroidal) flow field $\sigma$ about the cylinder axis and the vorticity field $\xi$ that generates mixing within the (poloidal) planes of fixed azimuth. As for a number of other 2D fluid systems, extending the classic 2D Euler equation, the flow is constrained by an infinite number of conservation laws, beyond the usual kinetic energy and angular momentum. All must be accounted for in a consistent equilibrium description. It is shown that the most directly observable impact of the conservation laws is on $\sigma$, which displays interesting large-scale radius-dependent flow structure. However, unlike in some previous treatments, we find that the thermodynamic temperature is always positive. As a consequence, except for an infinitesimal boundary layer that maintains the correct (conserved) value of the overall poloidal circulation, the impact on $\xi$ resides in the statistics of the strongly fluctuating, fine-scale mixing, where it is sensitive to `antiferromagnetic' microscale correlations that help maintain the analogue of local charge neutrality. The poloidal flow is macroscopically featureless, displaying no large scale circulating jet- or eddy-like features (which typically emerge as negative temperature states in analogous Euler and quasigeostrophic equilibria).
Dynamic Modelling of the Brain-electrode Interface for Stereoelectroencephalography

The modelling of the brain-electrode interface has many useful applications whenever patients are implanted with intra-cranial electrodes. In general, extensive research has been performed using electrode impedance spectroscopy in cases of deep brain stimulation for patients suffering from motor disorders. The brain-electrode interface model is also useful when it comes to epileptic patients, not only for diagnosis purpose, artefact correction, but also potentially for brain tissue classification. However, for this latter application, the interface model has never been studied considering typical stereoelectroencephalography signals. In this scope, the aim of this paper is to propose a brain-electrode interface model adapted to be used considering only voltages recorded during pre-surgical investigations. Various models are discussed based on a previous study on a phantom EEG device, and compared to the expected dynamics between pairs of consecutive contacts also presented in a previous non-parametric transfer function study. From this, two new models are proposed: one based in monopolar derivation, and the other on bipolar derivation. The models are simulated, and identified for three pairs of contacts inserted in one patient. The model based on bipolar derivation had better results.