Miracle-dz/UniFAR-FTUs huggingface dataset:
Sardinia Radio Telescope wide-band spectral-polarimetric observations of the galaxy cluster 3C 129

We present new observations of the galaxy cluster 3C 129 obtained with the Sardinia Radio Telescope in the frequency range 6000-7200 MHz, with the aim to image the large-angular-scale emission at high-frequency of the radio sources located in this cluster of galaxies. The data were acquired using the recently-commissioned ROACH2-based backend to produce full-Stokes image cubes of an area of 1 deg x 1 deg centered on the radio source 3C 129. We modeled and deconvolved the telescope beam pattern from the data. We also measured the instrumental polarization beam patterns to correct the polarization images for off-axis instrumental polarization. Total intensity images at an angular resolution of 2.9 arcmin were obtained for the tailed radio galaxy 3C 129 and for 13 more sources in the field, including 3C 129.1 at the galaxy cluster center. These data were used, in combination with literature data at lower frequencies, to derive the variation of the synchrotron spectrum of 3C 129 along the tail of the radio source. If the magnetic field is at the equipartition value, we showed that the lifetimes of radiating electrons result in a radiative age for 3C 129 of t_syn = 267 +/- 26 Myrs. Assuming a linear projected length of 488 kpc for the tail, we deduced that 3C 129 is moving supersonically with a Mach number of M=v_gal/c_s=1.47. Linearly polarized emission was clearly detected for both 3C 129 and 3C 129.1. The linear polarization measured for 3C 129 reaches levels as high as 70% in the faintest region of the source where the magnetic field is aligned with the direction of the tail.
Hollow occurrence and tree spacing in Eucalyptus tereticornis

ABSTRACT A ground-based survey of 400 Eucalyptus tereticornis trees examined the incidence of visible hollows suitable for hollow-dependent fauna. As well as the expected relationship with stem diameter, data analysis revealed a relationship between the incidence of hollows (with entrance diameter ≥10 cm) and spacing between neighbouring trees. When the distance between trees is equivalent to 0.3 times total tree height, a tree is more likely to suffer branch breakage and subsequent hollow formation. This influence of spacing, likely due to branches clashing during storms, appears to contribute a twofold difference in the incidence of hollows. This offers opportunities for the management of regrowth forests and restoration plantings, especially where one of the objectives is to encourage the formation of hollows.
The halo Boltzmann equation

Dark matter halos are the building blocks of the universe as they host galaxies and clusters. The knowledge of the clustering properties of halos is therefore essential for the understanding of the galaxy statistical properties. We derive an effective halo Boltzmann equation which can be used to describe the halo clustering statistics. In particular, we show how the halo Boltzmann equation encodes a statistically biased gravitational force which generates a bias in the peculiar velocities of virialized halos with respect to the underlying dark matter, as recently observed in N-body simulations.
The inner Galactic bar traced by the VVV survey

Aims. We use the VVV survey observations in bulge regions close to the Galactic plane to trace the bar inclination at the Galactic latitude b ∼± 1 and to investigate a distinct structure in the inner regions of the bar that was previously detected at positive latitude (b =+ 1). Methods. We use the (J −Ks) colors of the red clump stars to obtain reddening values on 6 × 6 arcmin scale, minimizing the problems arising from differential extinction. Dereddened magnitudes are then used to build the luminosity function of the bulge in regions of ∼0.4 sq deg to obtain the mean red clump magnitudes. These are used as distance indicators to trace the bar structure. Results. The luminosity function clearly shows the red clump mean magnitude variation with longitude, as expected from a large scale bar oriented towards us at positive Galactic longitude, with a dereddened magnitude varying from Ks0 = 13. 4a tl = −10 ◦ to Ks0 = 12. 4a tl =+ 10 ◦ . We detect a change in the orientation of the bar in the central regions with |l| < 4 ◦ at b = ±1 ◦ , in agreement with results obtained at positive latitudes by other authors. Our results are based on a different dataset and at different latitude, which shows that this change in the bar orientation is real. This suggests that there is an inner structure distinct to the large-scale Galactic bar, with a different orientation angle. This inner structure could be a secondary, inner bar, with a semi-major axis of ∼500 pc that is symmetric with respect to the Galactic plane.
Non-minimal derivative couplings of the composite metric

In the context of massive gravity, bi-gravity and multi-gravity non-minimal matter couplings via a specific composite effective metric were investigated recently. Even if these couplings generically reintroduce the Boulware-Deser ghost, this composite metric is unique in the sense that the ghost reemerges only beyond the decoupling limit and the matter quantum loop corrections do not detune the potential interactions. We consider non-minimal derivative couplings of the composite metric to matter fields for a specific subclass of Horndeski scalar-tensor interactions. We first explore these couplings in the mini-superspace and investigate in which scenario the ghost remains absent. We further study these non-minimal derivative couplings in the decoupling-limit of the theory and show that the equation of motion for the helicity-0 mode remains second order in derivatives. Finally, we discuss preliminary implications for cosmology.
All Static Black Holes in AdS$_3$

In this work we find the general static vacuum solution of three dimensional gravity with negative cosmological constant. Even though all solutions are locally diffeomorphic to pure $AdS_{3}$, solutions that differ globally from the latter space exist. New solutions with black holes on the $AdS_3$ boundary are found in both global and Poincare coordinates. In the Poincare coordinates such solutions are known as black funnels and black droplets. The black funnel provided by our general static metric is dual to the Hartle-Hawking state in the $1+1$ boundary theory.
TERZAN 5: AN ALTERNATIVE INTERPRETATION FOR THE SPLIT HORIZONTAL BRANCH

We consider the horizontal branch (HB) of the globular cluster Terzan 5, recently shown to be split into two parts, the fainter one (δMK ∼ 0.3 mag) having a lower metallicity than the more luminous. Both features show that it contains at least two stellar populations. The separation in magnitude has been ascribed to an age difference of ∼6 Gyr and interpreted as the result of an atypical evolutionary history for this cluster. We show that the observed HB morphology is also consistent with a model in which the bright HB is composed of second generation stars that are metal enriched and with a helium mass fraction larger (by δY ∼ 0.07) than that of first generation stars populating the fainter part of the HB. Terzan 5 would therefore be anomalous, compared to most “normal” clusters hosting multiple populations, only because its second generation is strongly contaminated by supernova ejecta; the previously proposed prolonged period of star formation, however, is not required. The iron enrichment of the bright HB can be ascribed either to contamination from Type Ia supernova ejecta of the low-iron, helium-rich, ejecta of the massive asymptotic giant branch stars of the cluster, or to its mixing with gas, accreting on the cluster from the environment, that has been subject to fast metal enrichment due to its proximity with the galactic bulge. The model proposed here requires only a small age difference of ∼100 Myr.
Entanglement spectrum of Su-Schrieffer-Heeger-Hubbard model

We investigate the entanglement spectrum of the ground state of the Su-Schrieffer-Heeger-Hubbard model. The topological phases of the model can be identified by degeneracy of the largest eigenvalues of entanglement spectrum. The study of the periodic boundary condition is enough to obtain the phase diagram of the model, without the consideration of the open boundary condition case. By analyzing the states corresponding to the degenerate entanglement spectrum and showing the related edge states in real space, physical interpretation about the relation between bulk-edge correspondence and the entanglement spectrum is presented. The method of the entanglement spectrum can be applicable in studying other topological phases of matter.
Abundance Patterns in the Interstellar Medium of the S0 Galaxy NGC 1316 (Fornax A) Revealed with Suzaku

The Suzaku X-ray satellite observed the nearby S0 galaxy NGC 1316, a merger remnant aged 3 Gyr. The total good exposure time was 48.7 ksec. The spectra were well represented by a two-temperature thermal model for the interstellar medium (ISM) plus a power-law model. The cool and hot temperatures of the thermal model were 0.48 +/- 0.03 and 0.92 +/- 0.04 keV, respectively. The excellent spectral sensitivity of Suzaku enables for the first time to measure the metal abundances of O, Ne, Mg, Si, and Fe in the ISM. The resultant abundance pattern of O, Ne, Mg, Si, and Fe is close to that of the new solar abundance determined by Lodders (2003). The measured abundance pattern is compared with those of elliptical galaxies and an S0 galaxy, observed with Suzaku. Considering the metal-enrichment from present Type Ia supernovae, the near-solar abundance pattern of the ISM in NGC~1316 indicates an enhanced {\alpha}/Fe ratio of stellar materials in the entire galaxy, like in giant elliptical galaxies.
Gender Comparisons and Associations between Lower Limb Muscle Activation Strategies and Resultant Knee Biomechanics during Single Leg Drop Landings

(1) Background: We aimed to compare gender differences in knee biomechanics and neuromuscular characteristics, and to determine the relationships between lower limb muscle pre-activations and knee biomechanics during a single leg drop landing, in order to identify riskier landing patterns to prevent injury and intervene properly. (2) Methods: Descriptive laboratory cross-sectional study on 38 healthy untrained subjects with low to moderate physical activity status. (3) Results: During the initial-contact phase of landing, females demonstrated greater peak vertical ground reaction force (GRF) normalized to body weight (49.12 ± 7.53 vs. 39.88 ± 5.69 N/kg; p < 0.001; Hedge’s g = 1.37), peak knee anterior reaction force normalized to body weight (0.23 ± 0.04 vs. 0.17 ± 0.05 N/kg; p < 0.001; Hedge’s g = 1.33), and decreased pre-activation of the semitendinosus (45.10 ± 20.05% vs. 34.03 ± 12.05%; p = 0.04; Hedge’s g = 0.67). The final regression equation was peak knee anterior reaction force = 0.024 + 0.025 (peak knee flexion moment) − 0.02 (semitendinosus-to-vastus lateralis pre-activation ratio) + 0.003 (peak vertical GRF) (R2 = 0.576, p < 0.001). (4) Conclusions: Overall, the data provided in this study support that a reduced semitendinosus-to-vastus lateralis pre-activation ratio predicted an increase in knee anterior reaction force and potentially an increase in ACL forces. Female non-athletes had gender-specific landing characteristics that may contribute to ACL injury. Future studies are warranted to consider more possible predictors of non-contact ACL injury.
Gravitational waveforms from a point particle orbiting a Schwarzschild black hole

We numerically solve the inhomogeneous Zerilli-Moncrief and Regge-Wheeler equations in the time domain. We obtain the gravitational waveforms produced by a point-particle of mass $\mu$ traveling around a Schwarzschild black hole of mass M on arbitrary bound and unbound orbits. Fluxes of energy and angular momentum at infinity and the event horizon are also calculated. Results for circular orbits, selected cases of eccentric orbits, and parabolic orbits are presented. The numerical results from the time-domain code indicate that, for all three types of orbital motion, black hole absorption contributes less than 1% of the total flux, so long as the orbital radius r_p(t) satisfies r_p(t)> 5M at all times.
Diagrams for heat kernel expansions

A diagramatic heat kernel expansion technique is presented. The method is especially well suited to the small-derivative expansion of the heat kernel, but it can also be used to reproduce the results obtained by the approach known as covariant perturbation theory. The new technique gives an expansion for the heat kernel at coincident points. It can also be used to obtain the derivative of the heat kernel, and this is useful for evaluating the expectation values of the stress-energy tensor.
Exponential Synchronization of Second-Order Fuzzy Memristor-Based Neural Networks With Mixed Time Delays via Fuzzy Adaptive Control

This article addresses the exponential synchronization problem for a class of fuzzy inertial memsirtor-based neural networks with mixed time-varying delays. First, the inertial items are described as second-order systems and transformed into first-order systems by utilizing a appropriate variable substitution. Then, the fuzzy state-feedback control strategy and fuzzy adaptive control strategy are designed to ensure the exponential synchronization under the framework of Filippov solutions. The exponential synchronization algebraic conditions are obtained by choosing a proper Lyapunov–Krasovskii functional. Finally, two numerical simulations are provided to validate the effectiveness and benefit of the proposed results.
A DETAILED FAR-ULTRAVIOLET SPECTRAL ATLAS OF MAIN-SEQUENCE B STARS

We have constructed a detailed spectral atlas covering the wavelength region 930–1225 Å for 10 sharp-lined B0–B9 stars near the main sequence. Most of the spectra we assembled are from the archives of the Far Ultraviolet Spectroscopic Explorer satellite, but for nine stars, wavelength coverage above 1188 Å was taken from high-resolution International Ultraviolet Explorer or echelle Hubble Space Telescope/Space Telescope Imaging Spectrograph spectra. To represent the tenth star at type B0.2 V, we used the Copernicus atlas of τ Sco. We made extensive line identifications in the region 949–1225 Å of all atomic features having published oscillator strengths at types B0, B2, and B8. These are provided as a supplementary data product—hence the term detailed atlas. Our list of found features totals 2288, 1612, and 2469 lines, respectively. We were able to identify 92%, 98%, and 98% of these features with known atomic transitions with varying degrees of certainty in these spectra. The remaining lines do not have published oscillator strengths. Photospheric lines account for 94%, 87%, and 91%, respectively, of all our identifications, with the remainder being due to interstellar (usually molecular H2) lines. We also discuss the numbers of lines with respect to the distributions of various ions for these three most studied spectral subtypes. A table is also given of 162 least blended lines that can be used as possible diagnostics of physical conditions in B star atmospheres.
PROBING THE PHYSICAL CONDITIONS OF ATOMIC GAS AT HIGH REDSHIFT

A new method is used to measure the physical conditions of the gas in damped Lyα systems (DLAs). Using high-resolution absorption spectra of a sample of 80 DLAs, we are able to measure the ratio of the upper and lower fine-structure levels of the ground state of C+ and Si+. These ratios are determined solely by the physical conditions of the gas. We explore the allowed physical parameter space using a Monte Carlo Markov chain method to constrain simultaneously the temperature, neutral hydrogen density, and electron density of each DLA. The results indicate that at least 5% of all DLAs have the bulk of their gas in a dense, cold phase with typical densities of ∼100 cm−3 and temperatures below 500 K. We further find that the typical pressure of DLAs in our sample is log (P/kB) = 3.4 (K cm−3), which is comparable to the pressure of the local interstellar medium (ISM), and that the components containing the bulk of the neutral gas can be quite small with absorption sizes as small as a few parsecs. We show that the majority of the systems are consistent with having densities significantly higher than expected for a purely canonical warm neutral medium, indicating that significant quantities of dense gas (i.e., nH > 0.1 cm−3) are required to match observations. Finally, we identify eight systems with positive detections of Si ii*. These systems have pressures (P/kB) in excess of 20,000 K cm−3, which suggest that these systems tag a highly turbulent ISM in young, star-forming galaxies.
Galactic rotation curves and brane-world models

In the present investigation, flat rotational curves of the galaxies are considered under the framework of brane-world models where the four-dimensional effective Einstein equation has extra terms which arise from the embedding of the 3-brane in the five-dimensional bulk. It has been shown here that these long-range bulk gravitational degrees of freedom can act as a mechanism to yield the observed galactic rotation curves without the need for dark matter. The present model has the advantage that the observed rotation curves result solely from well-established non-local effects of gravitation, such as dark radiation and dark pressure under a direct use of the condition of flat rotation curves and does not invoke any exotic matter field.
Large-scale polarized foreground component separation for Planck

ABSTRACT We use Bayesian component estimation methods to examine the prospects for large-scale polarized map and cosmological parameter estimation with simulated Planckdata assuming simpliﬁed white noise properties. The sky signal is parametrized as thesum of the CMB, synchrotron emission, and thermal dust emission. The synchrotronand dust components are modelled as power-laws, with a spatially varying spectralindex for synchrotron and a uniform index for dust. Using the Gibbs sampling tech-nique, we estimate the linear polarisation Q and U posterior amplitudes of the CMB,synchrotron and dust maps as well as the two spectral indices in ∼4 ◦ pixels. We usethe recovered CMB map and its covariance in an exact pixel likelihood algorithm toestimate the optical depth to reionization τ, the tensor-to-scalar ratio r, and to con-struct conditional likelihood slices for C EEl and C BBl . Given our foreground model,we ﬁnd σ(τ) ≈0.004 for τ = 0.1, σ(r) ≈0.03 for a model with r = 0.1, and a 95%upper limit of r < 0.02 for r = 0.0.
Rocky nests are better nesting sites than woodpecker cavities for the Eastern Rock Nuthatch Sitta Tephronota

The reproductive success of birds depends on many factors, including nest construction and placement. In the mountainous regions of southwestern Iran, broods of Eastern Rock Nuthatch Sitta tephronota were surveyed in 2016 and 2017. During the study, 11 broods in rocky cavities and 16 in abandoned Syrian woodpeckers’ Dendrocopos syriacus tree cavities were compared in terms of breeding performance (phenology, clutch size, hatching success, number of fledglings, breeding success). The Eastern Rock Nuthatch began egg-laying on March 24 and continued until April 15. The number of eggs in the clutch ranged from 3 and 7 (mean 5.6±1.19, median 6, N = 27). The two types of clutches compared usually contained 6 eggs, and the number of nestlings was statistically lower in tree cavities than in rocky nests. Hatching success was almost 30% higher in rocky nests than in tree cavities. In broods located in trees, 4 nestlings hatched most often (42%, N = 12), and in rock nests, 5 nestlings hatched (50%, N = 10). Rocky nests were also statistically greater (by over 40%) for breeding success. For all analysed broods and broods with success, roughly two extra fledglings left the rocky nests compared with tree cavities. 5 fledglings (50%, N = 10) most often left rocky nests, whereas, in general, 4 fledglings (50%, N = 10) left tree nests. Research results did not confirm that woodpecker cavities are safe nest sites for cavity dwellers.
Ammonia Sensing Properties of SnS₂/SnO₂ Nanocomposite-Based Gas Sensor by SnS₂ Annealing

Tin disulfide has been demonstrated effective for ammonia detection, while its potential application has been seriously limited by high working temperature and low sensitivity. In this article, SnS2/SnO2 nanocomposites are prepared through a two-step method. X-ray diffraction (XRD) and X-ray photoelectron spectroscopy (XPS) analysis show that the material would be transformed from SnS2 to SnS2/SnO2 composites by increasing annealing temperature. Gas testing results have shown that SnS2/SnO2 nanocomposites exhibit high sensitivity and good stability to ammonia, and the response to 100-ppm ammonia at 80 °C can reach 5.91. The sensor response was relatively stable at the target gas concentration. The high response of SnS2/SnO2 composites to ammonia at low temperatures might be due to SnS2 surface defects and heterostructure. From the perspective of atom and energy, adsorption energy has been simulated and calculated by the first principle analysis, to some extent, which proved that SnS2/SnO2 nanocomposite can improve the response to ammonia gas.
A Novel Drogue Pose Estimation Method for Autonomous Aerial Refueling Based on Monocular Vision Sensor

Drogue pose estimation is one of the key problems of autonomous aerial refueling (AAR) during the docking phase. A novel pose estimation method is proposed to remedy the failure of current methods due to the deformation of the flexible drogue. First, the key to flexible drogue pose estimation is suggested, and the concept of space-invariant features is extended. For the construction of 3L features, a preprocessing method is then proposed. Next, the problem of skeleton pose estimation is transformed into a fourth-order polynomial by constructing virtual points and presenting a point feature-based method. Subsequently, a matching method and the projection invariants of the skeleton are proposed. After that, the correspondences of reprojection points are constructed using the matched 3L features. An objective function fusing circle and line features and their derivatives are developed for optimizing the drogue pose base on the correspondences. Ultimately, the key techniques are verified in the synthetic and real data.
Controlling the non-linear intracavity dynamics of large He–Ne laser gyroscopes

A model based on Lamb's theory of gas lasers is applied to a He–Ne ring laser (RL) gyroscope to estimate and remove the laser dynamics contribution from the rotation measurements. The intensities of the counter-propagating laser beams exiting one cavity mirror are continuously observed together with a monitor of the laser population inversion. These observables, once properly calibrated with a dedicated procedure, allow us to estimate cold cavity and active medium parameters driving the main part of the non-linearities of the system. The quantitative estimation of intrinsic non-reciprocal effects due to cavity and active medium non-linear coupling plays a key role in testing fundamental symmetries of space–time with RLs. The parameter identification and noise subtraction procedure has been verified by means of a Monte Carlo study of the system, and experimentally tested on the G-PISA RL oriented with the normal to the ring plane almost parallel to the Earth's rotation axis. In this configuration the Earth's rotation rate provides the maximum Sagnac effect while the contribution of the orientation error is reduced to a minimum. After the subtraction of laser dynamics by a Kalman filter, the relative systematic errors of G-PISA reduce from 50 to 5 parts in 103 and can be attributed to the residual uncertainties on geometrical scale factor and orientation of the ring.