Miracle-dz/UniFAR-FTUs huggingface dataset:
The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations

We present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped-envelope Type Ib SN into a strongly interacting Type IIn SN within 1 yr. The AMI light curve clearly shows two distinct radio peaks, the second being a factor of 4 times more luminous than the first peak. This double bump morphology indicates two distinct phases of mass-loss from the progenitor star with the transition between density regimes occurring at 100–200 d. This reinforces the interpretation that SN 2014C exploded in a low-density region before encountering a dense hydrogen-rich shell of circumstellar material that was likely ejected by the progenitor prior to the explosion. The AMI flux measurements of the first light-curve bump are the only reported observations taken within ∼50 to ∼125 d post-explosion, before the blast-wave encountered the hydrogen shell. Simplistic synchrotron self-absorption and free–free absorption modelling suggest that some physical properties of SN 2014C are consistent with the properties of other Type Ibc and IIn SNe. However, our single frequency data does not allow us to distinguish between these two models, which implies that they are likely too simplistic to describe the complex environment surrounding this event. Lastly, we present the precise radio location of SN 2014C obtained with the electronic Multi-Element Remotely Linked Interferometer Network, which will be useful for future very long baseline interferometry observations of the SN.
MASSIVE STAR FORMATION IN THE LMC. I. N159 AND N160 COMPLEXES

We present images and spectral energy distributions (SEDs) of massive young stellar objects (YSOs) in three star-forming H ii regions of the Large Magellanic Cloud: N159A, N159 Papillon, and N160. We use photometry from SOFIA/FORCAST at 25.3–37.1 μm to constrain model fits to the SEDs and determine luminosities, ages, and dust content of the embedded YSOs and their local environments. By placing these sources on mid-infrared color–magnitude and color–color diagrams, we analyze their dust properties and consider their evolutionary status. Since each object in the FORCAST images has an obvious bright near-infrared counterpart in Spitzer Space Telescope images, we do not find any evidence for new, very cool, previously undiscovered Class 0 YSOs. Additionally, based on its mid-infrared colors and model parameters, N159A is younger than N160 and the Papillon. The nature of the first extragalactic protostars in N159, P1, and P2, is also discussed.
Resolved Hubble space spectroscopy of ultracool binary systems

Using the low-resolution mode of the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope (HST), we obtain spectra from 20 spatially-resolved, ultracool dwarfs, eighteen of which belong to nine very low-mass binary systems with known angular separations in the range 0$\farcs$37–0$\farcs$098. For these dwarfs, we derive their spectral types to be in the range dM7.5 to dL6 by either obtaining their PC3 index value or by comparing our STIS spectra with ground-based spectra of similar spectral resolution from Martin et al. (1999b). We have searched for H α emission in each object, but the emission is clearly detected in only two of them. We find that the distribution of H α emission in our sample is statistically different from that of single field dwarfs, suggesting an intriguing anti-correlation between chromospheric activity and binarity for M7–M9.5 dwarfs. We provide strength measuments of the main photospheric features. We derive calibrations of spectral subclasses versus $\it F814W$ and K -band absolute magnitudes for a subset of 10 dwarfs in 5 binaries that have known trigonometric parallaxes.
A refined sub-grid model for black hole accretion and AGN feedback in large cosmological simulations

In large scale cosmological hydrodynamic simulations simplified sub-grid models for gas accretion onto black holes and AGN feedback are commonly used. Such models typically depend on various free parameters, which are not well constrained. We present a new advanced model containing a more detailed description of AGN feedback, where those parameters reflect the results of recent observations. The model takes the dependency of these parameters on the black hole properties into account and describes a continuous transition between the feedback processes acting in the so-called radio-mode and quasar-mode. In addition, we implement a more detailed description of the accretion of gas onto black holes by distinguishing between hot and cold gas accretion. Our new implementations prevent black holes from gaining too much mass, particularly at low redshifts so that our simulations are now very successful in reproducing the observed present-day black hole mass function. Our new model also suppresses star formation in massive galaxies slightly more efficiently than many state-of-the-art models. Therefore, the simulations that include our new implementations produce a more realistic population of quiescent and star-forming galaxies compared to recent observations, even if some discrepancies remain. In addition, the baryon conversion efficiencies in our simulation are - except for the high mass end - consistent with observations presented in literature over the mass range resolved by our simulations. Finally, we discuss the significant impact of the feedback model on the low-luminous end of the AGN luminosity function.
Multiple Populations of Extrasolar Gas Giants

There are two planetary formation scenarios: core accretion and gravitational disk instability. Based on the fact that gaseous objects are preferentially observed around metal-rich host stars, most extrasolar gaseous objects discovered to date are thought to have been formed by core accretion. Here, we present 569 samples of gaseous planets and brown dwarfs found in 485 planetary systems that span three mass regimes with boundary values at 4 and 25 Jupiter-mass masses through performing cluster analyses of these samples regarding the host-star metallicity, after minimizing the impact of the selection effect of radial-velocity measurement on the cluster analysis. The larger mass is thought to be the upper mass limit of the objects that were formed during the planetary formation processes. In contrast, the lower mass limit appears to reflect the difference between planetary formation processes around early-type and G-type stars; disk instability plays a greater role in the planetary formation process around early-type stars than that around G-type stars. Populations with masses between 4 and 25 Jupiter masses that orbit early-type stars comprise planets formed not only via the core-accretion process but also via gravitational disk instability because the population preferentially orbits metal-poor stars or is independent of the host-star metallicity. Therefore, it is essential to have a hybrid scenario for the planetary formation of the diverse systems.
Door to Disposition Key Performance Indicator in Three Saudi Arabian Hospitals’ Emergency Departments during COVID-19 Pandemic

Objective: The COVID-19 pandemic impacted health systems and Emergency Departments (ED) services worldwide. This study attempts to assess the impact of COVID-19 on the performance of the emergency department during COVID-19 in three hospitals in Riyadh city, Saudi Arabia. Methods: Ada’a data was used for this retrospective cohort study. The hospitals included in this study were: a 300-bed maternity and children’s hospital; a 643-bed general hospital; and a 1230-bed tertiary hospital. All patients who visited the ED in the time period from September 2019 to December 2021 were included. The outcome variable was the Door to Disposition (DTD) which estimates the percentage of patients seen within 4 h from Door to Disposition. A two-way ANOVA test was used to examine the differences in the outcome variable by hospital and by the phase of COVID-19. Results: Both hospital and the phase of COVID-19 were significantly different in terms of the percentage of patients seen within four hours in the ED (DTD) (p-value < 0.05). On average, the DTD percentages dipped slightly in the early phase of COVID-19 (64.0% vs. 69.8%) and jumped sharply in the later phase (73.6%). Additionally, the average DTD score for the maternity and pediatric hospital (87.6%) was sharply higher than both general and tertiary hospitals (63.2%, and 56.5%, respectively). Conclusion: COVID-19 led to a significant drop in emergency department services performance in the early stage of the pandemic as patients spent more time at the ED. However, for the designated COVID-19 hospital, the ED performance improved as more patients spent less than 4 h at the ED in the early stages of COVID-19. This is a clear indication that careful planning and management of resources for ED services during a pandemic is effective.
Broadband Photon Spectrum and its Radial Profile of Pulsar Wind Nebulae

The observed radial profiles of the X-ray emission from pulsar wind nebulae (PWNe) have been claimed to contradict the standard 1D steady model. However, the 1D model has not been tested to simultaneously reproduce the volume-integrated spectrum and the radial profile of the surface brightness. We revisit the 1D steady model and apply it to PWNe 3C 58 and G21.5−0.9. We find that the parameters of the pulsar wind, the radius of the termination shock , and magnetization σ greatly affect both the photon spectrum and radial profile of the emission. We have shown that the parameters constrained by the entire spectrum lead to an X-ray nebula smaller than the observed nebula. We have also tested the case that reproduces only the observations in X- and gamma-rays, ignoring the radio and optical components. In this case, there are parameter sets that reproduce both the spectrum and emission profile, but the advection time to the edge of the nebula becomes much smaller than the age. Our detailed discussion clarifies that the standard 1D steady model has severe difficulty to simultaneously reproduce both the volume-integrated spectrum and the surface brightness. This implies that the model should be improved by taking into account extra physical processes such as spatial diffusion of particles. Additionally, we calculate the surface brightness profile of the radio, optical, and TeV gamma-rays. The future observations in these wavelengths are also important to probe the spatial distributions of the relativistic plasma and the magnetic field of PWNe.
Nitrogen Oxide Concentrations in Natural Waters on Early Earth

A key challenge in origins‐of‐life studies is estimating the abundances of species relevant to the chemical pathways proposed to have contributed to the emergence of life on early Earth. Dissolved nitrogen oxide anions ( NOX− ), in particular nitrate ( NO3− ) and nitrite ( NO2− ), have been invoked in diverse origins‐of‐life chemistry, from the oligomerization of RNA to the emergence of protometabolism. Recent work has calculated the supply of NOX− from the prebiotic atmosphere to the ocean and reported steady state [ NOX− ] to be high across all plausible parameter space. These findings rest on the assumption that NOX− is stable in natural waters unless processed at a hydrothermal vent. Here, we show that NOX− is unstable in the reducing environment of early Earth. Sinks due to ultraviolet photolysis and reactions with reduced iron (Fe2+) suppress [ NOX− ] by several orders of magnitude relative to past predictions. For pH = 6.5–8 and T = 0–50 °C, we find that it is most probable that [ NOX− ] <1μM in the prebiotic ocean. On the other hand, prebiotic ponds with favorable drainage characteristics may have sustained [ NOX− ] ≥1μM. As on modern Earth, most NOX− on prebiotic Earth should have been present as NO3− , due to its much greater stability. These findings inform the kind of prebiotic chemistries that would have been possible on early Earth. We discuss the implications for proposed prebiotic chemistries and highlight the need for further studies of NOX− kinetics to reduce the considerable uncertainties in predicting [ NOX− ] on early Earth.
Cosmic X-ray surveys of Active Galactic Nuclei: synergy between X-ray and infrared observations

We briefly review the synergy between X-ray and infrared observations for Active Galactic Nuclei (AGNs) detected in cosmic X-ray surveys, primarily with XMM-Newton, Chandra, and NuSTAR. We focus on two complementary aspects of this X-ray-infrared synergy (1) the identification of the most heavily obscured AGNs and (2) the connection between star formation and AGN activity. We also briefly discuss future prospects for X-ray-infrared studies over the next decade.
Transverse kinematics of the Galactic bar-bulge from VVV and Gaia

We analyse the kinematics of the Galactic bar-bulge using proper motions from the ESO public survey Vista Variables in the Via Lactea (VVV) and the second Gaia data release. Gaia has provided some of the first absolute proper motions within the bulge and the near-infrared VVV multi-epoch catalogue complements Gaia in highly extincted low-latitude regions. We discuss the relative-to-absolute calibration of the VVV proper motions using Gaia. Along lines of sight spanning $-10\lt \ell /\, \mathrm{deg}\lt 10$ and $-10\lt b/\, \mathrm{deg}\lt 5$, we probabilistically model the density and velocity distributions as a function of distance of ∼45 million stars. The transverse velocities confirm the rotation signature of the bar seen in spectroscopic surveys. The differential rotation between the double peaks of the magnitude distribution confirms the X-shaped nature of the bar-bulge. Both transverse velocity components increase smoothly along the near side of the bar towards the Galactic Centre, peak at the Galactic Centre, and decline on the far side. The anisotropy is σℓ/σb ≈ 1.1–1.3 within the bulk of the bar, reducing to 0.9–1.1 when rotational broadening is accounted for, and exhibits a clear X-shaped signature. The vertex deviation in ℓ and b is significant |ρℓb| ≲ 0.2, greater on the near side of the bar and produces a quadrupole signature across the bulge indicating approximate radial alignment. We have re-constructed the 3D kinematics from the assumption of triaxiality, finding good agreement with spectroscopic survey results. In the co-rotating frame, we find evidence of bar-supporting x1 orbits and tangential bias in the in-plane dispersion field.
Aerial-Aided Multiaccess Edge Computing: Dynamic and Joint Optimization of Task and Service Placement and Routing in Multilayer Networks

5G's feature of ubiquity in network coverage is expected to be extended to the computing domain in 6G. To accomplish ubiquity in communication and computation, integration of satellite, aerial and terrestrial networks is foreseen. In particular, the rising amount of applications such as In-Flight Entertainment and Connectivity Services (IFECS) and Software Defined Networking-enabled satellites renders network management more challenging. Moreover, the stringent Quality of Service (QoS) demands of these applications require edge computing. Network performance can be boosted by considering components of the aerial network, as potential Multi-Access Edge Computing (MEC) nodes. Thus, to cater to the QoS-critical applications, we propose an Aerial-Aided Multi-Access Edge Computing (AA-MEC) architecture that provides a framework for optimal management of computing resources and internet-based services in the sky. Furthermore, we formulate optimization problems to minimize the network latency for the two use cases of providing IFECS to aircrafts and services for offloading AI/ML tasks from satellites. Due to the dynamicity of satellite and aerial networks, we propose a re-configurable optimization. For this transforming network, we continuously identify the optimal MEC node for each application and the optimal path to the destination MEC node. In summary, our results demonstrate, that using AA-MEC improves network latency performance by 10.43% compared to the traditional approach of using only terrestrial MEC nodes, for latency-critical applications such as online gaming. Furthermore, while comparing our proposed dynamic approach with a static one, we record a minimum of 6.7% decrease in flow latency for IFECS and 56.03% decrease for computation offloading.
Growth Characteristics of Hemerocallis thunbergii Baker Seedlings depending on Cell Size in Sowing using Plug Trays

Background and objective: This study was conducted to determine the appropriate cell size, and days after sowing seeds by examining the growth of Hemerocallis thunbergii Baker (HTB) seedlings using plug trays.Methods: The growth of seedlings was examined after sowing seeds in four types of plug trays (143, 70, 18, 13 mL/cell). The sown trays were placed in a greenhouse for three repetitions per treatment. The seedling growth were measured at intervals of one month after sowing.Results: The leaf width and root length increased in proportion to the cell size, and at 90 days after sowing the highest leaf number was observed in the 143 mL/cell plug tray, followed in order by 18, 13, and 70 mL/cell plug tray. The longest leaf length was found in the 70 mL/cell plug trays, followed in order by the 70, 18, 143, and 13 mL/cell plug trays, but there was no significant difference except in 13 mL/cell plug trays. By analyzing the plant water content (PWC) of the shoots and roots, it was found that the PWC of the root system increased as the cell size increased, compared to that of the shoots, and there was a significant difference according to the cell size.Conclusion: Compared with the 143 mL cell plug tray, which had the largest cell size among the other treatment groups, the leaf number increased only for the 18 mL cell plug tray, there was no significant difference from 143 mL cell plug tray, and the leaf length was rather longer. Therefore, considering the actual production period and economic efficiency of raising the seedlings, it is considered that nursery period of 60 days or more is appropriate for HTB based on 18 mL/cell in sowing in plug trays.
BPS equations in six-dimensions and eight-dimensions

We consider the maximal supersymmetric pure Yang-Mills theories on six and eight dimensional space. We determine, in a systematic way, all the possible fractions of supersymmetry preserved by the BPS states and present the corresponding ``self-dual'' BPS equations. In six dimensions the intrinsic one has 1/4 supersymmetry, while in eight dimensions, 1/16, $2/16,\dots{},6/16. $ We apply our results to some explicit BPS configurations of finite or infinite energy on commutative or noncommutative spaces.
Pressurized steam torrefaction of wet agro-industrial residues

Pressurized Steam Torrefaction of Wet Agro-industrial Residues Paola Brachi, Francesco Miccio*, Giovanna Ruoppolo, Fernando Stanzione, Michele Miccio a Istituto di Ricerche sulla Combustione CNR, P.le V. Tecchio 80, 80125 Napoli, Italy b Istituto di Scienza e Tecnologia dei Materiali Ceramici CNR, via Granarolo 64 Faenza, Italy c Dipartimento di Ingegneria Industriale DIIN, Università di Salerno, via Giovanni Paolo II, Fisciano, Italy francesco.miccio@cnr.it
The predictability of reported drought events and impacts in the Ebro Basin using six different remote sensing data sets

The implementation of drought management plans contributes to reduce the wide range of adverse impacts caused by water shortage. A crucial element of the development of drought management plans is the selection of appropriate indicators and their associated thresholds to detect drought events and monitor their evolution. Drought indicators should be able to detect emerging drought processes that will lead to impacts with sufficient anticipation to allow measures to be undertaken effectively. However, in the selection of appropriate drought indicators the connection to the final impacts is often disregarded. This paper explores the utility of remotely sensed data sets to detect early stages of drought at the river basin scale, and how much time can be gained to inform operational land and water management practices. Six different remote sensing data sets with different spectral origin and measurement frequency are considered, complemented by a group of classical in situ hydrologic indicators. Their predictive power to detect past drought events is tested in the Ebro basin. Qualitative (binary information based on media records) and quantitative (crop yields) data of drought events and impacts spanning a period of 12 years are used as a benchmark in the analysis. Results show that early signs of drought impacts can be detected up to some 6 months before impacts are reported in newspapers, with the best correlation-anticipation relationships for the Standard Precipitation Index (SPI), the Normalized Difference Vegetation Index (NDVI) and Evapotranspiration (ET). Soil Moisture (SM) and Land Surface Temperature (LST) offer also good anticipation, but with weaker correlations, while Gross Primary Production (GPP) presents moderate positive correlations only for some of the rainfed areas. Although classical hydrological information from water levels and water flows provided better anticipation than remote sensing indicators in most of the areas, correlations were found to be weaker. The indicators show a consistent behaviour with respect to the different levels of crop yield in rainfed areas among the analysed years, with SPI, NDVI and ET providing again the stronger correlations. Overall, the results confirm remote sensing products’ ability to anticipate reported drought impacts and therefore appear as a useful source of information to support drought management decisions.
Diffuse interstellar bands in fullerene planetary nebulae: the fullerenes - diffuse interstellar bands connection

We present high-resolution (R∼15,000) VLT/UVES optical spectra of two planetary nebulae (PNe; Tc 1 and M 1-20) where C60 (and C70) fullerenes have already been found. These spectra are of hi gh-quality (S/N > 300) for PN Tc 1, which permits us to search for the expected electronic transitions of neutral C 60 and diffuse interstellar bands (DIBs). Surprisingly, we report the non-detection of the most intense optical bands of C60 in Tc 1, although this could be explained by the low C60 column density estimated from the C60 infrared bands if the C60 emission peaks far away from the central star. The strongest and most common DIBs in both fullerene PNe are normal for their reddening. Interestingly, the very broad 4428 A DIB and the weaker 6309 A DIB are found to be unusually intense in Tc 1. We also report the detection of a new broad (FWHM∼5 A) unidentified band at ∼6525 A. We propose that the 4428A DIB (probably also the 6309A DIB and the new 6525 A band) may be related to the presence of larger fullerenes (e.g., C 80, C240, C320, and C540) and buckyonions (multishell fullerenes such as C60@C240 and C60@C240@C540) in the circumstellar envelope of Tc 1.