Miracle-dz/UniFAR-FTUs huggingface dataset:
Holographic model with a NS-NS field

We consider a holographic model constructed through using the D4/D8-$\overline{\rm D8}$ brane configuration with a background field. We study some properties of the effective field theory in this intersecting brane construction, and calculate the effects of this NS-NS background field on some underlying dynamics. We also discuss some other general brane configurations.
HIGH VELOCITY COMPACT CLOUDS IN THE SAGITTARIUS C REGION

We report the detection of extremely broad emission toward two molecular clumps in the Galactic central molecular zone. We have mapped the Sagittarius C complex (−0.°61 < l < −0.°27, −0.°29 < b < 0.°04) in the HCN J = 4–3, 13CO J = 3–2, and H13CN J = 1–0 lines with the ASTE 10 m and NRO 45 m telescopes, detecting bright emission with 80–120 km s−1 velocity width (in full-width at zero intensity) toward CO−0.30−0.07 and CO−0.40−0.22, which are high velocity compact clouds (HVCCs) identified with our previous CO J = 3–2 survey. Our data reveal an interesting internal structure of CO−0.30−0.07 comprising a pair of high velocity lobes. The spatial-velocity structure of CO−0.40−0.22 can be also understood as a multiple velocity component, or a velocity gradient across the cloud. They are both located on the rims of two molecular shells of about 10 pc in radius. Kinetic energies of CO−0.30−0.07 and CO−0.40−0.22 are (0.8–2) × 1049 erg and (1–4) × 1049 erg, respectively. We propose several interpretations of their broad emission: collision between clouds associated with the shells, bipolar outflow, expansion driven by supernovae (SNe), and rotation around a dark massive object. These scenarios cannot be discriminated because of the insufficient angular resolution of our data, though the absence of a visible energy source associated with the HVCCs seems to favor the cloud–cloud collision scenario. Kinetic energies of the two molecular shells are 1 × 1051 erg and 0.7 × 1051 erg, which can be furnished by multiple SN or hypernova explosions in 2 × 105 yr. These shells are candidates of molecular superbubbles created after past active star formation.
Vision-Based Semantic Segmentation in Scene Understanding for Autonomous Driving: Recent Achievements, Challenges, and Outlooks

Scene understanding plays a crucial role in autonomous driving by utilizing sensory data for contextual information extraction and decision making. Beyond modeling advances, the enabler for vehicles to become aware of their surroundings is the availability of visual sensory data, which expand the vehicular perception and realizes vehicular contextual awareness in real-world environments. Research directions for scene understanding pursued by related studies include person/vehicle detection and segmentation, their transition analysis, lane change, and turns detection, among many others. Unfortunately, these tasks seem insufficient to completely develop fully-autonomous vehicles i.e., achieving level-5 autonomy, travelling just like human-controlled cars. This latter statement is among the conclusions drawn from this review paper: scene understanding for autonomous driving cars using vision sensors still requires significant improvements. With this motivation, this survey defines, analyzes, and reviews the current achievements of the scene understanding research area that mostly rely on computationally complex deep learning models. Furthermore, it covers the generic scene understanding pipeline, investigates the performance reported by the state-of-the-art, informs about the time complexity analysis of avant garde modeling choices, and highlights major triumphs and noted limitations encountered by current research efforts. The survey also includes a comprehensive discussion on the available datasets, and the challenges that, even if lately confronted by researchers, still remain open to date. Finally, our work outlines future research directions to welcome researchers and practitioners to this exciting domain.
The need for accurate redshifts in supernova cosmology

Recent papers have shown that a small systematic redshift shift (Δ z∼ 10−5) in measurements of type Ia supernovae can cause a significant bias (∼1%) in the recovery of cosmological parameters. Such a redshift shift could be caused, for example, by a gravitational redshift due to the density of our local environment. The sensitivity of supernova data to redshift shifts means supernovae make excellent probes of inhomogeneities. We therefore invert the analysis, and try to diagnose the nature of our local gravitational environment by fitting for Δ z as an extra free parameter alongside the usual cosmological parameters. Using the Joint Light-curve SN Ia dataset we find the best fit includes a systematic redshift shift of Δ z = (2.6+2.7−2.8) × 10−4. This is a larger shift than would be expected due to gravitational redshifts in a standard Λ-Cold Dark Matter universe (though still consistent with zero), and would correspond to a monopole Doppler shift of about 100 km s−1 moving away from the Milky-Way. However, since most supernova measurements are made to a redshift precision of no better than 10−3, it is possible that a systematic error smaller than the statistical error remains in the data and is responsible for the shift; or that it is an insignificant statistical fluctuation. We find that when Δ z is included as a free parameter while fitting to the JLA SN Ia data, the constraints on the matter density shifts to Ωm = 0.313+0.042−0.040, bringing it into better agreement with the CMB cosmological parameter constraints from Planck. A positive Δ z∼ 2.6×10−4 would also cause us to overestimate the supernova measurement of Hubble's constant by Δ H0 ∼ 1 kms−1Mpc−1. However this overestimation should diminish as one increases the low-redshift cutoff, and this is not seen in the most recent data.
THE ALFALFA “ALMOST DARKS” CAMPAIGN: PILOT VLA HI OBSERVATIONS OF FIVE HIGH MASS-TO-LIGHT RATIO SYSTEMS

We present new Very Large Array (VLA) H i spectral line imaging of five sources discovered by the ALFALFA extragalactic survey. These targets are drawn from a larger sample of systems that were not uniquely identified with optical counterparts during ALFALFA processing, and as such have unusually high H i mass to light ratios. The candidate “Almost Dark” objects fall into four broad categories: (1) objects with nearby H i neighbors that are likely of tidal origin; (2) objects that appear to be part of a system of multiple H i sources, but which may not be tidal in origin; (3) objects isolated from nearby ALFALFA H i detections, but located near a gas-poor early type galaxy; (4) apparently isolated sources, with no object of coincident redshift within ∼400 kpc. Roughly 75% of the 200 objects without identified counterparts in the α. 40 database (Haynes et al. ) fall into category 1 (likely tidal), and were not considered for synthesis follow-up observations. The pilot sample presented here (AGC193953, AGC208602, AGC208399, AGC226178, and AGC233638) contains the first five sources observed as part of a larger effort to characterize H i sources with no readily identifiable optical counterpart at single dish resolution (3.′5). These objects span a range of H i mass [7.41 < log(MHi ) < 9.51] and H i mass to B-band luminosity ratios (3 < MHi /LB < 9). We compare the H i total intensity and velocity fields to optical imaging drawn from the Sloan Digital Sky Survey and to ultraviolet imaging drawn from archival GALEX observations. Four of the sources with uncertain or no optical counterpart in the ALFALFA data are identified with low surface brightness optical counterparts in Sloan Digital Sky Survey imaging when compared with VLA H i intensity maps, and appear to be galaxies with clear signs of ordered rotation in the H i velocity fields. Three of these are detected in far-ultraviolet GALEX images, a likely indication of star formation within the last few hundred Myrs. One source (AGC208602) is likely tidal in nature, associated with the NGC 3370 group. Consistent with previous efforts, we find no “dark galaxies” in this limited sample. However, the present observations do reveal complex sources with suppressed star formation, highlighting both the observational difficulties and the necessity of synthesis follow-up observations to understand these extreme objects.
MID-INFRARED GALAXY LUMINOSITY FUNCTIONS FROM THE AGN AND GALAXY EVOLUTION SURVEY

We present galaxy luminosity functions at 3.6, 4.5, 5.8, and 8.0 μm measured by combining photometry from the IRAC Shallow Survey with redshifts from the AGN and Galaxy Evolution Survey (AGES) of the NOAO Deep Wide-Field Survey Boötes field. The well defined IRAC samples contain 3800–5800 galaxies for the 3.6–8.0 μm bands with spectroscopic redshifts and z < 0.6. We obtained relatively complete luminosity functions in the local redshift bin of z < 0.2 for all four IRAC channels that are well fitted by Schechter functions. After analyzing the samples for the whole redshift range, we found significant evolution in the luminosity functions for all four IRAC channels that can be fitted as an evolution in M* with redshift, ΔM* = Qz. While we measured Q = 1.2 ± 0.4 and 1.1 ± 0.4 in the 3.6 and 4.5 μm bands consistent with the predictions from a passively evolving population, we obtained Q = 1.8 ± 1.1 in the 8.0 μm band consistent with other evolving star formation rate estimates. We compared our luminosity functions with the predictions of semianalytical galaxy formation and found the best agreement at 3.6 and 4.5 μm, rough agreement at 8.0 μm, and a large mismatch at 5.8 μm. These models also predicted a comparable Q-value to our luminosity functions at 8.0 μm, but predicted smaller values at 3.6 and 4.5 μm. We also measured the luminosity functions separately for early- and late-type galaxies. While the luminosity functions of late-type galaxies resemble those for the total population, the luminosity functions of early-type galaxies in the 3.6 and 4.5 μm bands indicate deviations from the passive evolution model, especially from the measured flat luminosity density evolution. Combining our estimates with other measurements in the literature, we found 53 ± 18% of the present stellar mass of early-type galaxies was assembled at z = 0.7.
X-ray emission from hot accretion flows

Abstract Radiatively inefficient, hot accretion flows are widely considered as a relevant accretion mode in low-luminosity AGNs. We study spectral formation in such flows using a refined model with a fully general relativistic description of both the radiative (leptonic and hadronic) and hydrodynamic processes, as well as with an exact treatment of global Comptonization. We find that the X-ray spectral index–Eddington ratio anticorrelation as well as the cut-off energy measured in the best-studied objects favor accretion flows with rather strong magnetic field and with a weak direct heating of electrons. Furthermore, they require a much stronger source of seed photons than considered in previous studies. The nonthermal synchrotron radiation of relativistic electrons seems to be the most likely process capable of providing a sufficient flux of seed photons. Hadronic processes, which should occur due to basic properties of hot flows, provide an attractive explanation for the origin of such electrons.
Association between Periodontitis and Inflammatory Bowel Disease- Review of Current Literature on the Biologic Plausibility

Periodontitis, a chronic inflammatory disease of the supporting tissues of teeth, is etiologically associated with a subset of pathogenic organisms that thrive in the anoxic niche provided by the diseased periodontal pockets. These anaerobic gram-negative organisms resident in plaque biofilm and causing an overwhelming chronic inflammatory response in periodontal tissues have also been associated with other systemic chronic inflammatory diseases like cardiovascular, renal, and adverse pregnancy outcomes as per literature being published for the past twenty years or more. This paper aims to provide an overview on the biological plausibility of a strong association between systemic seeding of pathogenic oral bacteria and chronic bowel diseases like Inflammatory Bowel Diseases by reviewing recent literature from open-source journals on the same topic. Knowledge of the association between oral bacteria and gut inflammatory diseases will help in broadening the preventive and therapeutic options available currently by suggesting measures to suppress the systemic hyper-immune response.
Effect of fabric structure on the performance of screen-printed ultra-high frequency radio frequency identification tag antenna for wireless radio frequency energy harvesting

Textile materials are the ideal substrate of the antenna of eco-friendly wireless radio frequency (RF) energy harvesting technology for sustainable battery-free operation of wearable electronic devices, while few of the work published have been focused on the effect of textile properties on the energy harvesting performance. This work will clarify the effect of typical fabric surface structures on the energy harvesting performance of Radio Frequency Identification (RFID) antenna. The antennas were screen-printed onto three different weave structures, and performance for the different fabric-based antennas were studied. The results showed that the antenna printed on plain fabric, which has the smallest porosity and lower surface roughness, was able to achieve a maximum transmission distance of 110 cm and output voltage of 3.003 mV at 69 cm. Consequently, in order to improve the energy harvesting performance of antenna, the smooth and compact fabric surface is more beneficial to highly efficient energy harvesting.
Stripe formation instability in crossing traffic flows

At the intersection of two unidirectional traffic flows a stripe formation instability is known to occur. In this paper we consider coupled time evolution equations for the densities of the two flows in their intersection area. We show analytically how the instability arises from the randomness of the traffic entering the area. The Green function of the linearized equations is shown to form a Gaussian wave packet whose oscillations correspond to the stripes. Explicit formulas are obtained for various characteristic quantities in terms of the traffic density and comparison is made with the much simpler calculation on a torus and with numerical solution of the evolution equations.
4He adsorbed outside a single carbon nanotube

The phase diagrams of 4He adsorbed on the external surfaces of single armchair carbon nanotubes with radii in the range 3.42–10.85 A are calculated using the diffusion Monte Carlo method. For nanotubes narrower than a (10,10) one, the ground state is an incommensurate solid similar to the one found for H2 on the same substrates. For wider nanotubes, the phase with the minimum energy per particle is a liquid layer. Curved √3×√3 registered solids similar to the ones found on graphene and graphite were unstable for all the tubes considered.
Survival of patients with stage IIIC and IIID melanomas with nodal metastases in the light of new therapies

Introduction Within stage III melanoma prognosis and outcomes significantly vary. Advances in systemic therapy improved prognosis in metastatic melanoma. Adjuvant therapy in stage III significantly lowered relapses, although the effect on survival is less evident. Analysis of treatment results in stage IIIC and IIID before introduction of the modern adjuvant therapy, but after introduction of the effective systemic therapy in metastatic relapse, is needed. Aim To analyse the clinical outcomes in patients with stage IIIC and IIID melanoma before the introduction of the novel adjuvant therapy. Material and methods Consecutive stage IIIC and IIID melanoma patients treated in 2015–2018 in 4 reference centres in Poland were enrolled in the analysis of RFS and OS (in-transit metastases excluded). Median follow-up was 26.6 months (1.7–67.2). Results There were 224 stage IIIC and 49 stage IIID patients. Recurrence was observed in 170 (62.2%); 102 (45.5%) deaths in stage IIIC and 28 (57.1%) in stage IIID were reported. RFS and OS were better in stage IIIC compared to stage IIID. RFS and OS in the IIIC group were 19.7 and 36.2 months, respectively, and in IIID – 8.9 and 27.8 months, respectively. Conclusions The survival of patients with high-risk melanomas has improved in recent years, however, it is still unsatisfactory. The major changes in melanoma management related to the introduction of the adjuvant therapy require further careful observation.
Silicon quantum electronics

This review describes recent groundbreaking results in Si, Si/SiGe, and dopant-based quantum dots, and it highlights the remarkable advances in Si-based quantum physics that have occurred in the past few years. This progress has been possible thanks to materials development of Si quantum devices, and the physical understanding of quantum effects in silicon. Recent critical steps include the isolation of single electrons, the observation of spin blockade, and single-shot readout of individual electron spins in both dopants and gated quantum dots in Si. Each of these results has come with physics that was not anticipated from previous work in other material systems. These advances underline the significant progress toward the realization of spin quantum bits in a material with a long spin coherence time, crucial for quantum computation and spintronics.
Effect of fibre stacking orientation on the mechanical and thermal properties of laminated kenaf fibre/epoxy composites

ABSTRACT Natural fibre-reinforced composites have been developed by researchers and industries as a solution to reduce the use of synthetic fibres. Kenaf fibre is one of the most abundant natural fibres in Indonesia. This study aimed to obtain the mechanical and thermal properties of kenaf fibre-reinforced epoxy laminated composites fabricated using a vacuum-assisted resin infusion method. The alkaline-treated fibres were arranged in the orientations 0°/0°/0°/0° and 0°/90°/0°/90°. Density measurements, mechanical tests, and thermogravimetric analysis were carried out on the epoxy and the composites. The results of the mechanical testing showed that the tensile, flexural, and compression strengths of the kenaf fibre-reinforced epoxy composites with a 0°/0°/0°/0° fibre orientation were higher than those of the composites with a 0°/90°/0°/90° fibre orientation, with values of (96.61 ± 10.18) MPa, (131.01 ± 6.60) MPa, and (71.96 ± 5.50) MPa, respectively. Scanning electron microscope observations showed that the composites had good fibre-matrix adhesion. The thermal stability of the epoxy was enhanced from 557 °C to 571 °C by incorporating kenaf fibre with 0°/0°/0°/0° orientation. With reference to the Indonesian National Standard 01-4449–2006, the two composites could be classified as T2 45 High Density Fibreboard.
DNS of heat transfer in a transitional channel flow accompanied by a turbulent puff-like structure

Direct numerical simulations of turbulent heat transfer in fully-developed channel flows have been performed in a range of friction Reynolds number between 60 and 180, based on the friction velocity and the channel half width $\delta$, with emphasis on a puff-like structure, large-scale spatial intermittency. For the Reynolds numbers lower than 80 with a large computational domain of 51.2 x 2 x 22.5, the turbulent puff was observed and its significant influences on the momentum and heat transports were found. The spatial structure of the equilibrium puff, or the localized turbulence, was examined with taking account of two different thermal boundary conditions: the uniform heat-flux heating and the constant temperature difference between the walls. It was revealed that there existed a localized strong turbulent region in the form of an oblique band, along which a spanwise secondary flow was induced. In consequence, at the present lowest Reynolds number as low as 60, the flow remained turbulent and the larger Nusselt numbers than those without puff was obtained by the presence of puff.
An analytic solution for the minimal bathtub toy model: challenges in the star formation history of high-z galaxies

We study the minimal ``bathtub" toy model as an analytic tool for capturing key processes of galaxy evolution and identifying robust successes and challenges in reproducing observations at high redshift. The source and sink terms of the continuity equations for gas and stars are expressed in simple terms from first principles. The assumed dependence of star-formation rate (SFR) on gas mass self-regulates the system into a unique asymptotic behavior, which is approximated by an analytic quasi-steady-state solution (QSS). We address the validity of the QSS at different epochs independent of earlier conditions. At high z, where the accretion is assumed to consist of gas only, the specific SFR is robustly predicted to be sSFR = [(1+z)/3]^{5/2} Gyr^{-1}, slightly higher than the cosmological specific accretion rate, in agreement with observations at z=3-8. The gas fraction is expected to decline slowly, and the observations constrain the SFR efficiency per dynamical time to epsilon=0.02. The stellar-to-virial mass ratio f_sv is predicted to be constant in time, and the observed value requires an outflow mass-lading factor of eta=1-3, depending on the penetration efficiency of gas into the galaxy. However, at z=2, where stars are also accreted through mergers, the simplest model has an apparent difficulty in matching observations. The model that maximizes the sSFR, with the outflows fully recycled, falls short by a factor 3 in sSFR, and overestimates f_sv. With strong outflows, the model can reproduce the observed f_sv but at the expense of underestimating the sSFR by an order of magnitude. We discuss potential remedies including a bias due to the exclusion of quenched galaxies.
Radiative, two-temperature simulations of low luminosity black hole accretion flows in general relativity

We present a numerical method which evolves a two-temperature, magnetized, radiative, accretion flow around a black hole, within the framework of general relativistic radiation magnetohydrodynamics. As implemented in the code KORAL, the gas consists of two sub-components -- ions and electrons -- which share the same dynamics but experience independent, relativistically consistent, thermodynamical evolution. The electrons and ions are heated independently according to a standard prescription from the literature for magnetohydrodynamical turbulent dissipation. Energy exchange between the particle species via Coulomb collisions is included. In addition, electrons gain and lose energy and momentum by absorbing and emitting synchrotron and bremsstrahlung radiation, and through Compton scattering. All evolution equations are handled within a fully covariant framework in the relativistic fixed-metric spacetime of the black hole. Numerical results are presented for five models of low luminosity black hole accretion. In the case of a model with a mass accretion rate $\dot{M}\sim10^{-8} \dot M_{\rm Edd}$, we find that radiation has a negligible effect on either the dynamics or the thermodynamics of the accreting gas. In contrast, a model with a larger $\dot{M}\sim 4\times 10^{-4} \dot M_{\rm Edd}$ behaves very differently. The accreting gas is much cooler and the flow is geometrically less thick, though it is not quite a thin accretion disk.