Miracle-dz/UniFAR-FTUs huggingface dataset:
Mapping the core of the Tarantula Nebula with VLT-MUSE

We introduce VLT-MUSE observations of the central 2′× 2′ (30 × 30 pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming region in the Local Group. Spectrophotometry and radial-velocity estimates of the nebular gas (superimposed on the stellar spectra) are provided for 2255 point sources extracted from the MUSE datacubes, and we present estimates of stellar radial velocities for 270 early-type stars (finding an average systemic velocity of 271 ± 41 km s−1). We present an extinction map constructed from the nebular Balmer lines, with electron densities and temperatures estimated from intensity ratios of the [S II], [N II], and [S III] lines. The interstellar medium, as traced by Hα and [N II] λ6583, provides new insights in regions where stars are probably forming. The gas kinematics are complex, but with a clear bi-modal, blue- and red-shifted distribution compared to the systemic velocity of the gas centred on R136. Interesting point-like sources are also seen in the eastern cavity, western shell, and around R136; these might be related to phenomena such as runaway stars, jets, formation of new stars, or the interaction of the gas with the population of Wolf–Rayet stars. Closer inspection of the core reveals red-shifted material surrounding the strongest X-ray sources, although we are unable to investigate the kinematics in detail as the stars are spatially unresolved in the MUSE data. Further papers in this series will discuss the detailed stellar content of NGC 2070 and its integrated stellar and nebular properties.
Supernovae from massive stars with extended tenuous envelopes

Massive stars with a core-halo structure are interesting objects for stellar physics and hydrodynamics. Using simulations for stellar evolution, radiation hydrodynamics, and radiative transfer, we study the explosion of stars with an extended and tenuous envelope (i.e., stars in which 95% of the mass is contained within 10% of the surface radius or less). We consider both H-rich supergiant and He-giant progenitors resulting from close-binary evolution and dying with a final mass of 2.8-5Msun. An extended envelope causes the supernova (SN) shock to brake and a reverse shock to form, sweeping core material into a dense shell. The shock deposited energy, which suffers little degradation from expansion, is trapped in ejecta layers of moderate optical depth, thereby enhancing the SN luminosity at early times. With the delayed 56Ni heating, we find that the resulting optical and near-IR light curves all exhibit a double-peak morphology. We show how an extended progenitor can explain the blue and featureless optical spectra of some Type IIb and Ib SNe. The dense shell formed by the reverse shock leads to line profiles with a smaller and near-constant width. This ejecta property can explain the statistically narrower profiles of Type IIb compared to Type Ib SNe, as well as the peculiar Halpha profile seen in SN1993J. At early times, our He-giant star explosion model shows a high luminosity, a blue color, and featureless spectra reminiscent of the Type Ib SN2008D, suggesting a low-mass progenitor.
Equivalence Checking of Sequential Quantum Circuits

We define a formal framework for equivalence checking of sequential quantum circuits. The model we adopt is a quantum state machine, which is a natural quantum generalization of Mealy machines. A major difficulty in checking quantum circuits (but not present in checking classical circuits) is that the state spaces of quantum circuits are continuums. This difficulty is resolved by our main theorem showing that equivalence checking of two quantum Mealy machines can be done with input sequences that are taken from some chosen basis (which are finite) and have a length quadratic in the dimensions of the state Hilbert spaces of the machines. Based on this theoretical result, we develop an (and to the best of our knowledge, the first) algorithm for checking equivalence of sequential quantum circuits with running time <inline-formula> <tex-math notation="LaTeX">$\mathcal {O}(2^{3m+5l}(2^{3m}{\,+\,}2^{3l}))$ </tex-math></inline-formula>, where <inline-formula> <tex-math notation="LaTeX">$m$ </tex-math></inline-formula> and <inline-formula> <tex-math notation="LaTeX">$l$ </tex-math></inline-formula> denote the numbers of input and internal qubits, respectively. The complexity of our algorithm is comparable with that of the known algorithms for checking classical sequential circuits in the sense that both are exponential in the number of (qu)bits. Several case studies and experiments are presented.
Magnetic field in IRC+10216 and other C-Rich Evolved Stars

During the transition from the Asymptotic Giant Branch (AGB) to Planetary Nebulae (PN), the circumstellar geometry and morphology change dramatically. Another characteristic of this transition is the high mass loss rate, that can be partially explained by radiation pressure and a combination of various factors like the stellar pulsation, the dust grain condensation and opacity in the upper atmosphere. The magnetic field can also be one of the main ingredients that shapes the stellar upper atmosphere and envelope. Our main goal is to investigate for the first time the spatial distribution of the magnetic field in the envelope of IRC+10216. More generally we intend to determine the magnetic field strength in the circumstellar envelope (CSE) of C-rich evolved stars, compare this field with previous studies for O-rich stars, and constrain the variation of the magnetic field with r the distance to the star's center. We use spectropolarimetric observations of the Stokes V parameter, collected with Xpol on the IRAM-30m radiotelescope, observing the Zeeman effect in seven hyperfine components of the CN J = 1-0 line. We use Crutcher's method to estimate the magnetic field. For C-rich evolved stars, we derive a magnetic field strength (B) between 1.6 and 14.2 mG while B is estimated to be 6 mG for the proto-PN (PPN) AFGL618, and an upper value of 8 mG is found for the PN NGC7027. These results are consistent with a decrease of B as 1/r in the environment of AGB objects, i.e., with the presence of a toroidal field. But this is not the case for PPN and PN stars. Our map of IRC+10216 suggests that the magnetic field is not homogeneously strong throughout or aligned with the envelope and that the morphology of the CN emission might have changed with time.
Resonance Oscillation of Radiative Shock Waves in Accretion Disks around Compact Objects

We extend our previous numerical simulation of accretion disks with shock waves when cooling effects are also included. We consider bremsstrahlung and other power law processes: $\Lambda \propto T^{\alpha} \rho^2$ to mimic cooling in our simulation. We employ {\it Smoothed Particle Hydrodynamics} technique as in the past. We observe that for a given angular momentum of the flow, the shock wave undergoes a steady, radial oscillation with the period is roughly equal to the cooling time. Oscillations seem to take place when the disk and cooling parameters (i.e., accretion rate, cooling process) are such that the infall time from shock is of the same order as the post-shock cooling time. The amplitude of oscillation could be up to ten percent of the distance of the shock wave from the black hole when the black hole is accreting. When the accretion is impossible due to the centrifugal barrier, the amplitude variation could be much larger. Due to the oscillation, the energy output from the disk is also seen to vary quasi-periodically. We believe that these oscillations might be responsible for the quasi periodic oscillation (QPO) behaviors seen in several black hole candidates, in neutron star systems as well as dwarf novae outbursts such as SS Cygni and VW Hyi.
PAHs as a tracer of star formation

IR emission bands at 3.3, 6.2, 7.7, 8.6 and 11.3 um are generally attributed to IR fluorescence from (mainly) FUV pumped PAHs. As such, they trace the FUV stellar flux and are a measure of star formation. We examined the IR spectral characteristics of Galactic star forming regions, normal and starburst galaxies, AGNs and ULIRGs. The goal is to analyze if PAH bands are a good qualitative and/or quantitative tracer of star formation and hence the application of PAH bands as a diagnostic in order to identify the dominant processes contributing to the IR emission from Seyfert's and ULIRGs. We develop a MIR/FIR diagnostic and compare it to known diagnostics, with these also applied to the Galactic sample. This diagnostic is based on the FIR normalized 6.2 um PAH flux and the FIR normalized 6.2 um continuum flux. The Galactic sources form a sequence spanning a range of 3 orders of magnitude, from embedded compact HII regions to exposed PDRs and the (D)ISM. The variation in the 6.2 um PAH/continuum ratio is relative small. Normal and starburst galaxies ressemble exposed PDRs. While Seyfert-2's coincide with the starburst trend, Seyfert-1's are displaced by at least a factor 10 in 6.2 um continuum flux. ULIRGs show a diverse spectral appearance (AGN hot dust continuum, starburst-like or strong dust obscuration in the nucleus). ULIRGs also seems to have more prominent FIR emission than either starburst galaxies or AGNs. We discuss the observed variation in the Galactic sample in view of the evolutionary state and the PAH/dust abundance and the use of PAHs as quantitative tracers of star formation activity. We find that PAHs may be better suited as a tracer of B stars, which dominate the Galactic stellar energy budget, than as a tracer of massive star formation (O stars).
Nanoillumination based on self-focus and field enhancement inside a subwavelength metallic structure

A subwavelength metallic structure is proposed to generate superstrong nanoillumination. Its attractive features are presented numerically with finite-difference time-domain method. By combining a subwavelength slit and a nanohole together into metallic screen, the light illuminated on the surface of the screen is firstly squeezed into the subwavelength slit with the aid of the generated surface plasmon, and then during propagation to the exit end of the slit, the light is focused on a nanohole fabricated at the bottom of the slit due to the self-imaging effect and is further enhanced by the transmission resonance when passing through the nanohole. Because of these three successive enhancement processes, the light from the nanohole could become thousand times stronger than the incident light and accordingly could have great potentials for applications in optical data storage, super-resolution imaging, lithography, photonics, and other applications that need nanoillumination.
Initial implementation of the resuscitation quality improvement program in emergency department of a teaching hospital in China

Background Cardiopulmonary resuscitation (CPR) skills may decay over time after conventional instructor-led BLS training. The Resuscitation Quality Improvement® (RQI®) program, unlike a conventional basic life support (BLS) course, is implemented through mastery learning and low-dose, high-frequency training strategies to improve CPR competence. We facilitated the RQI program to compare the performance of novices vs those with previous BLS training experience before RQI implementation and to obtain their confidence and attitude of the RQI program. Methods A single-center observational study was conducted from May 9, 2021 to June 25, 2021 in an emergency department of a tertiary hospital. The performance assessment data of both trainees with a previous training experience in conventional BLS course (BLS group) and the novice ones with no prior experience with any BLS training (Non-BLS group) was collected by RQI cart and other outcome variables were rated by online questionnaire. Outcome measurements included chest compression and ventilation in both adult-sized and infant-sized manikins. Results A total of 149 participants were enrolled. Among them, 103 participants were in BLS group and 46 participants in Non-BLS group. Post RQI training, all the trainees achieved a passing score of 75 or more, and obtained an improvement in CPR performance. The number of attempts to pass RQI for compression and ventilation practice was lower in the BLS group in both adult and infant training sessions (P < 0.05). Although the BLS group had a poor baseline, it had fewer trials and the same learning outcomes, and the BLS group had better self-confidence. Trainees were well adapted to the innovative training modality, and satisfaction among all of the participants was high. Only the respondents for non-instructor led training, the satisfaction was low in both groups (72.8% in BLS group vs 65.2% in No-BLS group, strongly agreed). Conclusion Among novices, RQI can provide excellent CPR core skills performance. But for those who had previous BLS training experience, it was able to enhance the efficiency of the skills training with less time consumption. Most trainees obtained good confidence and satisfaction with RQI program, which might be an option for the broad prevalence of BLS training in China.
The Effects of Imports and Economic Growth in Chinese Economy: A Granger Causality Approach under VAR Framework

This study inspects the association between economic growth and imports from China, based on data sourced from 2000 to 2021. For this reason, a quantitative research approach is used to determine the causality between the variables and their impact on the economy. The null hypothesis of the paper implies that the import growth rate has a significant impact on the GDP growth rate in the Peoples Republic of China. This hypothesis was rejected via the Granger causality test, as the only single directional relationship was found. However, further analysis was conducted by applying a Vector Auto-Regression (VAR) model that included leading macroeconomic variables, such as the inflation rate, the bank rate, and the exchange rate between the US dollar and Chinese yuan. The impulse responses of the model, aligned with the economic theory and the results, suggested that the import growth rate is negatively related to the GDP growth rate, while the GDP growth rate has an initial positive impact on the imports for the first three quarters, which later changes to a negative impact. This time lag suggests that while the impact between the variables is important, negative outcomes could be avoided if proper economic policy is implemented. The government of China should focus on policy implications that further promote export and substitute imported goods with domestic production.
Investigation of Curcumin-Loaded OA400 Nanoparticle’s Effect on the Expression of E6 and E7 Human Papilloma-Virus Oncogenes and P53 and Rb Factors in HeLa Cell Line

Background Curcumin, a compound derived from the root of the Curcuma longa, has been confirmed as an anticancer, chemoprotective, and gene/protein regulatory agent. Nanoformulation of curcumin has been developed to increase its targeting efficiency, solubility, controlled release, and physical and chemical stability. Objectives This study investigated the effect of new nano-type curcumin, oleic acid-derived dendrosome (OA400 nanoparticles), on the expression of E6 and E7 human papillomavirus oncogenes and P53 and Rb factors in the HeLa cell line. After preparing nano-curcumin by mixing OA400 nano-carrier and curcumin, its effect was considered on the human cervical cancer cell line (HeLa cell line RRID: CVCL_003) and normal fibroblast cells. Methods MTT assay and flow cytometry were used to evaluate cell viability and apoptosis. Furthermore, real-time RT-PCR and western blot analyses assessed RNA and protein expression of E6, E7, P53, and Rb. Statistical analyses were performed by GraphPad Prism 7 software. Results The nanoformulation of curcumin could reduce the expression of E6 and E7 oncogenes and increase P53 and Rb tumor suppressors in HeLa cancerous cells at 15 μM concentration; however, it had no significant effect on the viability of normal fibroblast cells. On the other hand, curcumin altered the expression of these genes at a 50-μM concentration. Gene and protein expression analysis indicated the up-regulation of P53 and Rb factors and the down-regulation of E6 and E7 under the influence of nano-curcumin treatment more than curcumin. Conclusions These data indicate the potential of curcumin-loaded OA400 nanoparticles to be considered as a treatment option in cervical cancer investigations.
Fortifying Brain Signals for Robust Interpretation

Brain-Media, is the discipline of decoding sophisticated human brain activity such as imagination, memories, colours, textures, patterns, etc. Existing efforts either classify brain signals or map them to an image of the same class. The second technique has only been investigated in a few papers using Electro Encephalography (EEG) datasets based on ImageNet and MNIST images. The role of Deep Neural Networks (DNN) must be researched to make them robust against malicious noise. Existing frameworks ignore the existence of such disruptive noises. The current research provides a multimodality time-series and spatial-domain hybrid framework and a unique ResilientNet Generator to classify signals robustly. In the first stage, two teachers are trained using a time series and an image dataset that shares the class. The second phase trains a ResilientNet-Generator with a new penalized-reconstruction loss-function apart from the adversarial loss. Finally, the trained ResilientNet-Generator is used as a pre-processing module for training a DNN-classifier in the third phase. It is noted that representing time-series data by the spatial domain can significantly improve accuracy compared to existing approaches. An ablation study on the resilience of trained classifiers against attacked test samples shows that DNNs can be fortified using the proposed framework.
Interdependent Infrastructure System Risk and Resilience to Natural Hazards.

Complex, interdependent systems are necessary to the delivery of goods and services critical to societal function. Here we demonstrate how interdependent systems respond to disruptions. Specifically, we change the spatial arrangement of a disruption in infrastructure and show that -- while controlling for the size -- changes in the spatial pattern of a disruption induce significant changes in the way interdependent systems fail and recover. This work demonstrates the potential to improve characterizations of hazard disruption to infrastructure by incorporating additional information about the impact of disruptions on interdependent systems.
Interacting dark energy with time varying equation of state and the 
H0
 tension

Almost in all coupled dark energy models present in the literature, the stability of the model becomes potentially sensitive to the dark energy equation of state parameter $w_x$, and a singularity arises at `$w_x = -1$'. Thus, it becomes mandatory to test the stability of the model into two separate regions, namely, the quintessence and phantom and certainly, a discontinuity appears into the parameters space of the dark energy state parameter. Such discontinuity can be removed with some choices of the coupling function. In the present work we choose one particular coupling between dark matter and dark energy which can successfully remove such instability and we allow a dynamical dark energy equation of state parameter instead of the constant one. We have considered one parameter dynamical dark energy equation of state, and the interacting scenario have been confronted with several observational data with latest origin. The results show that the present cosmological data allow an interaction in the dark sector, in agreement with some latest claims by several authors, and additionally, a phantom behaviour in the dark energy equation of state is suggested at present. Moreover, for this case the tension on $H_0$ is clearly released. As a final remark, we should mention that according to the Bayesian analysis, $\Lambda$CDM is always favored over this interacting dark energy model.
A Dynamical Model for Clustered Star Formation in the Galactic Disk

The clustered nature of star formation should produce a high degree of structure in the combined phase and chemical space in the Galactic disk. To date, observed structure of this kind has been mostly limited to bound clusters and moving groups. In this paper, we present a new dynamical model of the Galactic disk that takes into account the clustered nature of star formation. This model predicts that the combined phase and chemical space is rich in substructure and that this structure is sensitive to both the precise nature of clustered star formation and the large-scale properties of the Galaxy. The model self-consistently evolves 4 billion stars over the last 5 Gyr in a realistic potential that includes an axisymmetric component, a bar, spiral arms, and giant molecular clouds. All stars are born in clusters with an observationally motivated range of initial conditions. As direct N-body calculations for billions of stars are computationally infeasible, we have developed a method of initializing star cluster particles to mimic the effects of direct N-body effects, while the actual orbit integrations are treated as test particles within the analytic potential. We demonstrate that the combination of chemical and phase space information is much more effective at identifying truly conatal populations than either chemical or phase space alone. Furthermore, we show that comoving pairs of stars are very likely to be conatal if their velocity separation is <2 km s−1 and their metallicity separation is <0.05 dex. The results presented here bode well for harnessing the synergies between Gaia and spectroscopic surveys to reveal the assembly history of the Galactic disk.
Optimizing the signal-to-noise ratio of biphoton distribution measurements

Single-photon-sensitive cameras can now be used as massively parallel coincidence counters for entangled photon pairs. This enables measurement of biphoton joint probability distributions with orders-of-magnitude greater dimensionality and faster acquisition speeds than traditional raster scanning of point detectors; to date, however, there has been no general formula available to optimize data collection. Here we analyze the dependence of such measurements on count rate, detector noise properties, and threshold levels. We derive expressions for the biphoton joint probability distribution and its signal-to-noise ratio (SNR), valid beyond the low-count regime up to detector saturation. The analysis gives operating parameters for global optimum SNR that may be specified prior to measurement. We find excellent agreement with experimental measurements within the range of validity, and discuss discrepancies with the theoretical model for high thresholds. This work enables optimized measurement of the biphoton joint probability distribution in high-dimensional joint Hilbert spaces.
Prompt High-Energy Gamma-Ray Emission from the Synchrotron Self-Compton Process in the Reverse Shocks of Gamma-Ray Bursts

In the standard scenario of the fireball model of gamma-ray bursts (GRBs), the huge initial energy release produces a relativistic blast wave expanding into the external medium and a reverse shock moving into and heating the fireball ejecta. We calculate the high-energy gamma-ray emission due to inverse Compton scattering of the synchrotron photons from relativistic electrons in the reverse shock. Under the favorable values of the physical parameters of the GRBs and the interstellar medium, our result shows that during the prompt phase, this emission dominates over the component from the forward shock at high-energy gamma-ray bands. This mechanism can excellently account for the observations of the prompt high-energy gamma rays detected by EGRET, such as those from GRB 930131.