Miracle-dz/UniFAR-FTUs huggingface dataset:
THE ENVIRONMENTAL DEPENDENCE OF THE LUMINOSITY–SIZE RELATION FOR GALAXIES

We have examined the luminosity–size relationship as a function of environment for 12,150 Sloan Digital Sky Survey galaxies with precise visual classifications from the catalog of Nair & Abraham. Our analysis is subdivided into investigations of early-type galaxies and late-type galaxies. Early-type galaxies reveal a surprisingly tight luminosity–size relation. The dispersion in luminosity about the fiducial relation is only ∼0.14 dex (0.35 mag), even though the sample contains galaxies that differ by a factor of almost 100 in luminosity. The dispersion about the luminosity–size relation is comparable to the dispersion about the fundamental plane, even though the luminosity–size relation is fundamentally simpler and computed using purely photometric parameters. We attribute this to using a clean sample of elliptical galaxies and a large Petrosian size measure, implying that the fundamental plane may closely resemble a fundamental line, provided a different (and arguably better) size measurement is adopted. The key contributors to the dispersion about the luminosity–size relation are found to be color and central concentration expanding our analysis to the full range of morphological types, we show that the slope, zero point, and scatter about the luminosity–size relation are independent of environmental density. Our study thus indicates that whatever process is building galaxies is doing so in a way that preserves fundamental scaling laws even as the typical luminosity of galaxies changes with environment. However, the distribution of galaxies along the luminosity–size relation is found to be strongly dependent on galaxy environment. This variation is in the sense that, at a given morphology, larger and more luminous galaxies are rarer in sparser environments. Our analysis of late-type galaxy morphologies reveals that scatter increases toward later Hubble types. Taken together, these results place strong constraints on conventional hierarchical models in which galaxies are built up in an essentially stochastic way.
High resolution imaging of the GG Tauri system at 267 GHz

Context. Studying circumbinary disks is critical to understanding the formation mechanisms of binary stars. While optical or mid-infrared images reveal the scattered emission, millimeter observations provide direct measurements of the dust thermal emission. Aims: We study the properties of the circumbinary disk around the well-known, multiple young stellar object GG Tau with the highest possible sensitivity and spatial resolution. Methods: We mapped the continuum emission of GG Tau at 267 GHz using the IRAM Plateau de Bure interferometer equipped with upgraded receivers and LO systems. An angular resolution of 0.45'' × 0.25'' was achieved, corresponding to a linear resolution of 65 × 35 AU. Results: The GG Tau A circumbinary disk is observed as an extremely clearly defined narrow ring. The width of the ring is not resolved. Emission from the central binary is detected and clearly separated from the ring: it coincides with the GG Tau Aa position and may therefore trace a circumstellar disk around this star. The mass ratio of the circumbinary to circumprimary material is ~80. Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
Hierarchical Object Detection applied to Fish Species

Gathering information of aquatic life is often based on timeconsumingmethods utilizing video feeds. It would be beneficialto capture more information cost-effectively from video feeds.Video based object detection has an ability to achieve this.Recent research has shown promising results with the use ofYOLO for object detection of fish. As underwater conditionscan be difficult and thus fish species are hard to discriminate.This study proposes a hierarchical structure-based YOLO Fishalgorithm in both the classification and the dataset to gainvaluable information. With the use of hierarchical classificationand other techniques. YOLO Fish is a state-of-the-art objectdetector on Nordic fish species, with an mAP of 91.8%. Thealgorithm has an inference time of 26.4 ms, fast enough torun on real-time video on the high-end GPU Tesla V100.
Developing Machine Learning Techniques to Investigate the Impact of Air Quality Indices on Tadawul Exchange Index

The air quality index (AQI) can be described using different pollutant indices. Many investigators study the effect of stock prices and air quality in the field to show if there is a relationship between changing the stock market and the concentration of various pollutants. This study aims to find a relationship between Saudi Tadawul All Share Index (TASI) and multiple pollutants, including particulate matter (PM10), ozone (O3), nitrogen dioxide (NO2), sulfur dioxide (SO2), carbon monoxide (CO), and AQI. Based on tree models, the relationship is created using linear regression and two prediction models, Chi-square Automatic Interaction Detection (CHAID), and CR-Tree. In order to achieve the target of this research, the TASI dataset relates to six pollutants using time; afterward, the new dataset is divided into three parts—test, validate, and train—after eliminating the outlier data. In order to test the performance of two prediction models, R2 and various error functions are used. The linear regression model results found that PM10, NO2, CO, month, day, and year are significant, whereas O3, SO2, and AQI indices are insignificant. The test dataset showed that R2 scores are 0.995 and 0.986 for CR-Tree and CHAID, respectively, with RMSE values of 387 and 227 for CR-Tree and CHAID, respectively. The prediction models showed that the CHAID model performed better than CR-Tree because it used only three indices, namely, PM10, AQI, and O3, with year and month. The results indicated an effect between changing TASI and the three pollutants, PM10, AQI, and O3.
AGN in dusty hosts: implications for galaxy evolution

We present strong empirical evidence for a physical connection between the occurrence of a starburst (SB) and a luminous AGN phase. Drawing infrared (IR), X-ray, and optically selected samples from COSMOS, we find that the locus of type-II AGN hosts in the optical colour-magnitude (U-V/V) and colour-colour (U-V/V-J) space significantly overlaps with that of IR-luminous (LIR > 10 10 L⊙) galaxies. Based on our observations, we propose that, when simultaneously building their black hole and stellar masses, type-II AGN hosts are located in the same part of colour-colour space as dusty star-forming galaxies. In fact, our results show that IR-luminous galaxies at z 10 42 erg/s) than would be expected serendipitously, if AGN and star-formation events were unrelated. In addition, the optical and infrared properties of the AGN/SB hybrid systems tentatively suggest that the AGN phase might be coeval with a particularly active phase in a galaxy’s star-formation history. Interestingly, we also find a significant fraction of type-II AGN hosts offset from the dusty galaxy sequence in colour-colour space, possibly representing a transitional or post-starburst phase in galaxy evolution. Our findings are consistent with a scenario whereby AGN play a role in the termination of star-formation in massive galaxies.
Comoving frame models of hot star winds - I. Test of the Sobolev approximation in the case of pure line transitions

We provide hot star wind models with radiative force calculated using the solution of comoving frame (CMF) radiative transfer equation. The wind models are calculated for the first stars, O stars, and the central stars of planetary nebulae. We show that without line overlaps and with solely thermal line broadening the pure Sobolev approximation provides a reliable estimate of the radiative force even close to the wind sonic point. Consequently, models with the Sobolev line force provide good approximations to solutions obtained with non-Sobolev transfer. Taking line overlaps into account, the radiative force becomes slightly lower, leading to a decrease in the wind mass-loss rate by roughly 40%. Below the sonic point, the CMF line force is significantly lower than the Sobolev one. In the case of pure thermal broadening, this does not influence the mass-loss rate, as the wind mass-loss rate is set in the supersonic part of the wind. However, when additional line broadening is present (e.g., the turbulent one) the region of low CMF line force may extend outwards to the regions where the mass-loss rate is set. This results in a decrease in the wind mass-loss rate. This effect can at least partly explain the low wind mass-loss rates derived from some observational analyses of luminous O stars.
A CHANDRA STUDY OF THE ROSETTE STAR-FORMING COMPLEX. III. THE NGC 2237 CLUSTER AND THE REGION'S STAR FORMATION HISTORY

We present high spatial resolution Chandra X-ray images of the NGC 2237 young stellar cluster on the periphery of the Rosette Nebula. We detect 168 X-ray sources, 80% of which have stellar counterparts in USNO, Two Micron All Sky Survey, and deep FLAMINGOS images. These constitute the first census of the cluster members with 0.2 ≲ M ≲ 2 M☉. Star locations in near-infrared color–magnitude diagrams indicate a cluster age around 2 Myr with a visual extinction of 1 ≲ AV ≲ 3 at 1.4 kpc, the distance of the Rosette Nebula's main cluster NGC 2244. We derive the K-band luminosity function and the X-ray luminosity function of the cluster, which indicate a population ∼400–600 stars. The X-ray-selected sample shows a K-excess disk frequency of 13%. The young Class II counterparts are aligned in an arc ∼3 pc long suggestive of a triggered formation process induced by the O stars in NGC 2244. The diskless Class III sources are more dispersed. Several X-ray emitting stars are located inside the molecular cloud and around gaseous pillars projecting from the cloud. These stars, together with a previously unreported optical outflow originating inside the cloud, indicate that star formation is continuing at a low level and the cluster is still growing. This X-ray view of young stars on the western side of the Rosette Nebula complements our earlier studies of the central cluster NGC 2244 and the embedded clusters on the eastern side of the Nebula. The large-scale distribution of the clusters and molecular material is consistent with a scenario in which the rich central NGC 2244 cluster formed first, and its expanding H ii region triggered the formation of the now-unobscured satellite clusters Rosette Molecular Cloud (RMC) XA and NGC 2237. A large swept-up shell material around the H ii region is now in a second phase of collect-and-collapse fragmentation, leading to the recent formation of subclusters. Other clusters deeper in the molecular cloud appear unaffected by the Rosette Nebula expansion.
Prospects for Detecting Gamma-Ray Bursts at Very High Energies with the Cherenkov Telescope Array

We discuss the prospects for the detection of gamma-ray bursts (GRBs) by the Cherenkov Telescope Array (CTA), the next generation, ground-based facility of imaging atmospheric Cherenkov telescopes (IACTs) operating above a few tens of GeV. By virtue of its fast slewing capabilities, the lower energy threshold compared to current IACTs, and the much larger effective area compared to satellite instruments, CTA can measure the spectra and variability of GRBs with excellent photon statistics at multi-GeV energies, which would revolutionize our understanding of the physics of GRBs, test their validity as the origin of ultrahigh-energy cosmic rays and provide powerful probes of the extragalactic background light as well as Lorentz-invariance violation. Employing a model of the GRB population whose properties are broadly consistent with observations by the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) on-board Fermi, we simulate follow-up observations of GRBs with the Large Size Telescopes (LSTs), the component of CTA with the fastest slew speed and the best sensitivity at energies below a few hundred GeV. For our fiducial assumptions, we foresee that the LSTs can detect ∼0.1 GRBs per year during the prompt phase and ∼0.5 GRBs per year in the afterglow phase, considering only one array site and both GBM and the Space-based multi-band astronomical Variable Object Monitor (SVOM) as the alert instruments. The detection rates can be enhanced by a factor of about 5 and 6 for the prompt emission and the afterglow, respectively, assuming two array sites with the same sensitivity and that the GBM localization error can be reduced to less than 1°. The expected distribution of redshift and photon counts is presented, showing that despite the modest event rate, hundreds or more of multi-GeV photons can be anticipated from a single burst once they are detected. We also study how the detection rate depends on the intrinsic GRB properties and the delay time between the burst trigger and the follow-up observation.
Counting Dark Sub-halos with Star Stream Gaps

The Cold Dark Matter paradigm predicts vast numbers of dark matter sub-halos to be orbiting in galactic halos. The sub-halos are detectable through the gaps they create gaps in stellar streams. The gap-rate is an integral over the density of sub-halos, their mass function, velocity distribution and the dynamical age of the stream. The rate of visible gap creation is a function of the width of the stream. The available data for four streams: the NW stream of M31, the Pal~5 stream, the Orphan Stream and the Eastern Banded Structure, are compared to the LCDM predicted relation. We find a remarkably good agreement, although there remains much to be done to improve the quality of the result. The narrower streams require that there is a total population of order 10^5 sub-halos above 10^5 M_sun to create the gaps.
Morphological diversity of glandular trichomes in Urticalean Rosids

Glandular trichomes are epidermal structures that produce, store and release a variety of chemical compounds. Their high morphological diversity allows their taxonomic use at various levels. Therefore, their description and standardization of terminology become challenging. Cannabaceae is a well known family of Urticalean Rosids because of the presence of cannabinoid-secreting trichomes in Cannabis sativa . Other Urticalean Rosid families (Moraceae, Ulmaceae and Urticaceae) are neglected in this regard. Thus, the morphology and distribution of glandular trichomes were studied in Cannabaceae and Ulmaceae species and compared with published data for Moraceae and Urticaceae. Surface and anatomical analyses were performed on vegetative and floral organs. Urticalean Rosids show at least 15 types of glandular trichomes, 12 of them capitate and three filiform. In particular, Trema micrantha, a Cannabaceae species, has six different types. A trichome with biseriate stalk and pluricellular head, found in Trema micrantha and Pteroceltis tatarinowii , was not previously reported. Glandular trichomes are widely distributed in the plant body, which may be related to protection against herbivory. The greatest difficulty was the large quantity of terms and the lack of morphological details of the glandular trichomes in previous studies. A standardization of the terminology of glandular trichomes was therefore proposed.
Factors Affecting Family Welfare of Garut-Indonesia Flash Flood Survivors: A Case Study of Impact Disaster on SDGs

Disasters risk reduction and sustainable development goals (SDGs) are closely linked. The frequent disaster causing devastating impact on society and community. This study aims to analyze the driver of family welfare of survivors of the 2016 Garut flash flood. The total sample consisted of 120 families, some living in temporary sheltered evacuation sites (SF) and others having returned home (non-sheltered group/NSF). Data was obtained at the four months following the disaster. The study revealed that, compared to the respondents in the SF sites, the NSF respondents had higher income, more sources of stress, better coping strategies, and a higher level of welfare. Income, financial management, coping strategies, and economic pressure all had a positive effect on total welfare while, in the case of subjective wellbeing, greater impact came from sources of stress compared with coping strategies. Objective wellbeing, on the other hand, was only influenced by income and coping strategies.
ULTRA-SHORT-PERIOD PLANETS IN K2 SUPERPIG RESULTS FOR CAMPAIGNS 0–5

We analyzed data from Campaigns 0–5 of the K2 mission and report 19 ultra-short-period candidate planets with orbital periods of less than one day (nine of which have not been previously reported). Planet candidates range in size from 0.7 to 16 Earth radii and in orbital period from 4.2 to 23.5 hr. One candidate (EPIC 203533312, Kp = 12.5) is among the shortest-period planet candidates discovered to date ( hr), and, if confirmed as a planet, must have a density of at least to not be tidally disrupted. Five candidates have nominal radius values in the sub-Jovian desert ( and days) where theoretical models do not favor their long-term stability; the only confirmed planet in this range is thought to be disintegrating (EPIC 201637175). In addition to the planet candidates, we report on four objects that may not be planetary, including one with intermittent transits (EPIC 211152484) and three initially promising candidates that are likely false positives based on characteristics of their light curves and on radial velocity follow-up. A list of 91 suspected eclipsing binaries identified at various stages in our vetting process is also provided. Based on an assessment of our survey's completeness, we estimate an occurrence rate for ultra-short-period planets among K2 target stars that is about half that estimated from the Kepler sample, raising questions as to whether K2 systems are intrinsically different from Kepler systems, possibly as a result of their different galactic location.
AN ACCRETION DISK-OUTFLOW MODEL FOR HYSTERETIC STATE TRANSITION IN X-RAY BINARIES

We suggest a model of the advection-dominated accretion flow (ADAF) with magnetically driven outflows to explain the hysteretic state transition observed in X-ray binaries (XRBs). The transition from a thin disk to an ADAF occurs when the mass accretion rate is below a critical value. The critical mass accretion rate for the ADAF can be estimated by equating the equilibration timescale to the accretion timescale of the ADAF, which is sensitive to its radial velocity. The radial velocity of thin disks is very small, which leads to the advection of the external field in thin disks becoming very inefficient. ADAFs are present in the low/hard states of XRBs, and their radial velocity is large compared with the thin disk. The external field can be dragged inward efficiently by the ADAF, so a strong large-scale magnetic field threading the ADAF can be formed, which may accelerate a fraction of gas in the ADAF into the outflows. Such outflows may carry away a large amount of angular momentum from the ADAF, which significantly increases the radial velocity of the ADAF. This leads to a high critical mass accretion rate, below which an ADAF with magnetic outflows can survive. Our calculations show that the critical luminosity of the ADAF with magnetic outflows can be one order of magnitude higher than that for a conventional ADAF, if the ratio of gas to magnetic pressure β ∼ 4 ? > in the disk. This can naturally explain the hysteretic state transition observed in XRBs.
Ethnopharmacological study of medicinal plants from the province of Cuanza Norte (Angola)

Studies on African medicinal plants have been limited to some geographically areas, and even though more than 5400 medicinal plants are recognized and documented, other valuable medicinal plant species have not been studied. Ethnopharmacological studies are important for documenting traditional knowledge associated with the medical use of biodiversity. This study aims to document the use of medicinal plants from the Province of Cuanza Norte (Angola). The field work was conducted from December 2018 to January 2019 and the ethnobotanical data were collected using semi-structured interviews. Informants were selected in accordance with their residence and community recognition as healers. Recorded plants are listed along with their popular name, traditional use, part used, and method of preparation. A total of 131 species of medicinal plants were cited. Mukumbi (Lannea welwitschii), Santa Maria (Chenopodium ambrosioides) and Ditumbata (Boerhavia difusa) were the most cited species. Out of the total plant parts, leaves were the most frequently material used. Regarding the mode of preparation for the medicinal materials, the major form of preparation is maceration, followed by infusion and decoction. The main categories of use were infectious and parasitic diseases (e.g., Malaria); undefined pains and illness; diseases of the digestive system; and endocrine, nutritional, and metabolic diseases (e.g., Diabetes). This study revealed the importance of preserving the ethnobotanical knowledge in order to protect the biodiversity and to discover new therapeutic molecules. A comparison of the results with other studies showed that some of the traditional indications are supported by data from scientific literature.
WIMP annihilation effects on primordial star formation

We study the effects of WIMP dark matter (DM) annihilations on the thermal and chemical evolution of the gaseous clouds where the first generation of sta rs in the Universe is formed. We follow the collapse of the gas inside a typical halo virializing at very high redshift, from well before virialization until a stage where the heating from DM annihilations exceeds the gas cooling rate. The DM energy input is estimated by inserting the energy released by DM annihilations (as predicted by an adiabatic contraction of the original DM profile) in a spherically symmetric radiative transfer scheme. In addition to the heating effec ts of the energy absorbed, we include its feedback upon the chemical properties of the gas, which is critical to determine the cooling rate in the halo, and hence the fragmentation scale and Jeans mass of the first stars. We find that DM annihilation does alter the free electron and especially the H 2 fraction when the gas density is n >10 4 #/cm 3 , for our fiducial parameter values. However, even if the chan ge in the H2 abundance and the cooling efficiency of the gas is large (some times exceeding a factor 100), the effects on the temperature of the collapsing gas are far s maller (a reduction by a factor < 1.5), since the gas cooling rate depends very strongly on temperature: then, the fragmentation mass scale is reduced only slightly, hinting towards no dramatic change in the initial mass function of the first stars.