Miracle-dz/UniFAR-FTUs huggingface dataset:
Characterisation of young stellar clusters

A high number of embedded clusters is found in the Galaxy. Depending on the formation scenario, most of them can evolve to unbounded groups that are dissolved within a few tens of Myr. A systematic study of young stellar clusters showing distinct characteristics provide interesting information on the evolutionary phases during the pre-main sequence. In order to identify and to understand these phases we performed a comparative study of 21 young stellar clusters. Near-infrared data from 2MASS were used to determine the structural and fundamental parameters based on surface stellar density maps, radial density profile, and colour-magnitude diagrams. We obtained age and mass distributions by comparing pre-main sequence models with the position of cluster members in the colour-magnitude diagram. The mean age of our sample is ~ 5 Myr, where 57% of the objects is found in the 4 - 10 Myr range of age, while 43% is < 4 Myr old. Their low E(B-V) indicate that the members are not suffering high extinction Av < 1 mag), which means they are more likely young stellar groups than embedded clusters. Relations between structural and fundamental parameters were used to verify differences and similarities that could be found among the clusters. The parameters of most of the objects have the same trends or correlations. Comparisons with other young clusters show similar relations among mass, radius and density. Our sample tends to have larger radius and lower volumetric density, when compared to embedded clusters. These differences are compatible with the mean age of our sample, which we consider intermediary between the embedded and the exposed phases of the stellar clusters evolution.
Predicted Yield of Transits of Known Radial Velocity Exoplanets from the TESS Primary and Extended Missions

Radial velocity (RV) surveys have detected hundreds of exoplanets through their gravitational interactions with their host stars. Some will be transiting, but most lack sufficient follow-up observations to confidently detect (or rule out) transits. We use published stellar, orbital, and planetary parameters to estimate the transit probabilities for nearly all exoplanets that have been discovered via the RV method. From these probabilities, we predict that 25.5 − 0.7 + 0.7 of the known RV exoplanets should transit their host stars. This prediction is more than double the amount of RV exoplanets that are currently known to transit. The Transiting Exoplanet Survey Satellite (TESS) presents a valuable opportunity to explore the transiting nature of many of the known RV exoplanet systems. Based on the anticipated pointing of TESS during its two-year primary mission, we identify the known RV exoplanets that it will observe and predict that 11.7 − 0.3 + 0.3 of them will have transits detected by TESS. However, we only expect the discovery of transits for ∼3 of these exoplanets to be novel (i.e., not previously known). We predict that the TESS photometry will yield dispositive null results for the transits of ∼125 RV exoplanets. This will represent a substantial increase in the effort to refine ephemerides of known RV exoplanets. We demonstrate that these results are robust to changes in the ecliptic longitudes of future TESS observing sectors. Finally, we consider how several potential TESS extended mission scenarios affect the number of transiting RV exoplanets we expect TESS to observe.
THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: VELOCITY SHIFTS OF QUASAR EMISSION LINES

Quasar emission lines are often shifted from the systemic velocity due to various dynamical and radiative processes in the line-emitting region. The level of these velocity shifts depends both on the line species and on quasar properties. We study velocity shifts for the line peaks (not the centroids) of various narrow and broad quasar emission lines relative to systemic using a sample of 849 quasars from the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. The coadded (from 32 epochs) spectra of individual quasars have sufficient signal-to-noise ratio (S/N) to measure stellar absorption lines to provide reliable systemic velocity estimates, as well as weak narrow emission lines. The large dynamic range in quasar luminosity (∼2 dex) of the sample allowed us to explore potential luminosity dependence of the velocity shifts. We derive average line peak velocity shifts as a function of quasar luminosity for different lines, and quantify their intrinsic scatter. We further quantify how well the peak velocity can be measured as a function of continuum S/N, and demonstrate that there is no systematic bias in the velocity measurements when S/N is degraded to as low as ∼3 per SDSS pixel ( ). Based on the observed line shifts, we provide empirical guidelines on redshift estimation from [O ii] , [O iii] , [Ne v] , Mg ii, C iii], He ii , broad Hβ, C iv, and Si iv, which are calibrated to provide unbiased systemic redshifts in the mean, but with increasing intrinsic uncertainties of 46, 56, 119, 205, 233, 242, 400, 415, and 477 , in addition to the measurement uncertainties. These results demonstrate the infeasibility of measuring quasar redshifts to better than with only broad lines.
VAMYOLOX: An Accurate and Efficient Object Detection Algorithm Based on Visual Attention Mechanism for UAV Optical Sensors

Unmanned aerial vehicles (UAVs) have been widely used in various fields. As one of the key technologies in improving the autonomous sensing ability of UAV optical sensors, object detection has become a research focus in recent years. Since UAVs usually navigate at different vertical heights, the object scales and sensor field of view change violently, which brings a great difficulty to the optimization of the model. Moreover, when a UAV is flying at low level rapidly, it may cause the motion blur phenomenon on objects that are highly dense in position, leading to great challenge for distinction of these objects. To address the extremely tough problems discussed above, we propose an accurate and efficient object detection algorithm, namely, VAMYOLOX. Based on YOLOX, we first redesigned the classification and regression loss function of the model to better conduct classification and localization under complex motion blur and dense scenes. Then, we increase another prediction head to detect lots of tiny objects to ultimately improve the detection ability of the model for multiscale objects. Finally, we redesigned the neck of the network by introducing the triplet attention module (TAM) to find attention regions in scenes with dense objects and in images that cover a large area, accordingly enhancing the features extracted by the backbone network. Extensive experiments on the VisDrone dataset widely used in the research of UAV image object detection show that VAMYOLOX has achieved the state-of-the-art (SOTA) performance with good interpretability in UAV optical sensors captured scenes. On the VisDrone-DET-test-dev subset, the average precision (AP) of VAMYOLOX is 25.31%, outperforming the previous SOTA model (CornerNet) by 1.88%. On the VisDrone-DET-val subset, the AP of our method is 29.4%, achieving a highly competitive result with previous SOTA method (AMRNet). Not only that, VAMYOLOX achieves a maximum improvement of 2.72% compared to the AP of the baseline model (YOLOX). In addition, compared with other methods, our method has a significant advantage in speed and can meet the needs of different scenarios. The PyTorch code and trained models are available at https://github.com/yangyahu-1994/VAMYOLOX.
Dissipation in unsteady turbulence

Recent experiments and simulations have shown that unsteady turbulent flows, before reaching a dynamic equilibrium state, display a universal behaviour. We show that the observed universal non-equilibrium scaling can be explained using a non-equilibrium correction of Kolmogorov's energy spectrum. Given the universality of the experimental and numerical observations, the ideas presented here lay the foundation for the modeling of a wide class of unsteady turbulent flows.
WATER VAPOR DISTRIBUTION IN PROTOPLANETARY DISKS

Water vapor has been detected in protoplanetary disks. In this work, we model the distribution of water vapor in protoplanetary disks with a thermo-chemical code. For a set of parameterized disk models, we calculate the distribution of dust temperature and radiation field of the disk with a Monte Carlo method, and then solve the gas temperature distribution and chemical composition. The radiative transfer includes detailed treatment of scattering by atomic hydrogen and absorption by water of Lyα photons, since the Lyα line dominates the UV spectrum of accreting young stars. In a fiducial model, we find that warm water vapor with temperature around 300 K is mainly distributed in a small and well-confined region in the inner disk. The inner boundary of the warm water region is where the shielding of UV field due to dust and water itself become significant. The outer boundary is where the dust temperature drops below the water condensation temperature. A more luminous central star leads to a more extended distribution of warm water vapor, while dust growth and settling tends to reduce the amount of warm water vapor. Based on typical assumptions regarding the elemental oxygen abundance and the water chemistry, the column density of warm water vapor can be as high as 1022 cm−2. A small amount of hot water vapor with temperature higher than ∼300 K exists in a more extended region in the upper atmosphere of the disk. Cold water vapor with temperature lower than 100 K is distributed over the entire disk, produced by photodesorption of the water ice.
Pengaruh Insentif Pajak dan Insentif Non-pajak terhadap Manajemen Laba

Penelitian ini bertujuan untuk menguji faktor-faktor potensial yang diduga mempengaruhi tindakan manajemen laba. Adapun variabel independen dalam penelitian ini adalah insentif pajak dengan proksi (perencanaan pajak, beban pajak tangguhan, beban pajak kini dan persentase jumlah saham disetor) dan insentif non-pajak dengan proksi (leverage, capital intensity ratio, kepemilikan manajerial dan profitabilitas), sementara variabel dependentnya adalah manajemen laba. Populasi dalam penelitian ini adalah perusahaan manufaktur yang terdaftar di Bursa Efek Indonesia (BEI) pada tahun 2013-2017. Sampel penelitian ini menggunakan metode puposive sampling dan di peroleh 97 perusahaan. Metode analisis menggunkan analisis statistik deskriptif dan Generalized Method of moments. Hasil penelitian menunjukan bahwa perencanaan pajak, beban pajak tangguhan dan kepemilikan manajerial tidak berpengaruh terhadap manajemen laba, sedangkan beban pajak kini, persentase jumlah saham disetor, leverage, capital intensity ratio dan profabilitas berpengaruh positif dan signifikan terhadap manajemen laba. Dengan demikian untuk mencegah terjadinya manajemen laba, pemerintah harus memperkuat pengawasan serta memperkuat peraturan dan harus benar-benar dipatuhi oleh principal untuk mengurangi aktivitas manajemen laba yang dilakukan oleh principal agar dapat memberikan keuntungan kepada pihak tertentu.
The Origins of the Gamma-Ray Flux Variations of NGC 1275 Based on Eight Years of Fermi-LAT Observations

We present an analysis of eight years of Fermi-LAT (>0.1 GeV) γ-ray data obtained for the radio galaxy NGC 1275. The γ-ray flux from NGC 1275 is highly variable on short (∼days to weeks) timescales, and has steadily increased over this eight year timespan. By examining the changes in its flux and spectral shape in the LAT energy band over the entire data set, we found that its spectral behavior changed around 2011 February (∼MJD 55600). The γ-ray spectra at early times evolved largely at high energies, while the photon indices were unchanged at later times despite rather large flux variations. To explain these observations, we suggest that the flux changes at the early times were caused by injection of high-energy electrons into the jet while, later, the γ-ray flares were caused by a changing Doppler factor owing to variations in the jet Lorentz factor and/or changes in the angle to our line of sight. To demonstrate the viability of these scenarios, we fit the broad band spectral energy distribution data with a one-zone synchrotron self-Compton (SSC) model for flaring and quiescent intervals before and after 2011 February. To explain the γ-ray spectral behavior in the context of the SSC model, the maximum electron Lorentz factor would have changed at the early times, while a modest change in the Doppler factor adequately fits the quiescent and flaring state γ-ray spectra at the later times.
Supersymmetric Custodial Triplets

We analyze the extension of the Minimal Supersymmetric Standard Model which includes extra Y = (0,±1) supersymmetric triplets with a global SU(2)L ⊗ SU(2)R symmetry spontaneousy broken to the custodial SU(2)V by the vacuum expectation value of the neutral scalar components of doublets and triplets. The model is the supersymmetrization of the non-supersymmetric model introduced long ago by Georgi and
Variations in the Frequencies of Polymorphisms in the CYP450s Genes in Eight Major Ethnicities of Iran: A Review of the Human Data

Genetic polymorphisms in cytochrome P450 genes can cause variation in metabolism. Thus, single nucleotide variants significantly impact drug pharmacokinetics, toxicity factors, and efficacy and safety of medicines. The distribution of CYP450 alleles varies drastically across ethnicities, with significant implications for personalized medicine and the healthcare system. We combined whole-genome and exome sequencing data to provide a review of CYP450 allele polymorphisms with clinical importance. Data were collected from 800 unrelated Iranians (100 subjects from 8 major ethnicities of Iran), more than 32,000 unrelated Europeans (other than Caucasian), and four Middle Eastern countries. We analyzed the frequencies and similarities of 17 CYP450 frequent alleles related to nine important CYP450 isoenzymes and homozygous and heterozygous genotypes based on these alleles in eight major Iranian ethnics by integrating these data with population-specific linkage information and compared these datasets with mentioned populations.
Possible evolution of the circum-galactic medium around QSOs with QSO age and cosmic time revealed by Ly α haloes

We first present new Subaru narrow-band observations of the Ly α halo around the quasi-stellar object (QSO) CFHQ J232908−030158 at z = 6.42, which appears the most luminous and extended halo at z > 5 (LLy α = 9.8 × 1043 erg s−1 within 37 pkpc diameter). Then, combining these measurements with available data in the literature, we find two different evolutions of QSOs’ Ly α haloes. First is a possible short-term evolution with QSO age seen in four z > 6 QSOs. We find the anticorrelation between the Ly α halo scales with QSOs’ infrared (IR) luminosity, with J2329−0301’s halo being the brightest and largest. It indicates that ionizing photons escape more easily out to circum-galactic regions when host galaxies are less dusty. We also find a positive correlation between IR luminosity and black hole mass (MBH). Given MBH as an indicator of QSO age, we propose a hypothesis that a large Ly α halo mainly exists around QSOs in the young phase of their activity due to a small amount of dust. The second is an evolution with cosmic time seen over z ∼ 2–5. We find the increase of surface brightness towards lower redshift with a similar growth rate to that of dark matter haloes (DHs) that evolve to MDH = 1012–1013 M⊙ at z = 2. The extent of Ly α haloes is also found to increase at a rate scaling with the virial radius of growing DHs, $r_\text{vir} \propto M_\text{DH}^{1/3}(1+z)^{-1}$. These increases are consistent with a scenario that the circum-galactic medium around QSOs evolves in mass and size keeping pace with hosting DHs.
Assessing the Impact of a Shinrin-Yoku (Forest Bathing) Intervention on Physician/Healthcare Professional Burnout: A Randomized, Controlled Trial

Professional healthcare worker burnout is a crisis in the United States healthcare system. This crisis can be viewed at any level, from the national to local communities, but ultimately, must be understood at the level of the individual who is caring for patients. Thus, interventions to reduce burnout symptoms must prioritize the mental health of these individuals by alleviating some of the symptoms of depression, grief, and anxiety that accompany burnout. The practice of Shinrin-Yoku (Forest Bathing) is a specific evidence-based practice which research has shown can improve an individual’s mental health and, when performed in a group, can support a sense of social connection. We investigated the impact of a three-hour, guided Shinrin-Yoku (Forest Bathing) nature-based intervention on burnout symptoms among physicians and other healthcare workers by using a randomized, controlled trial. The Oldenburg Burnout Inventory (OLBI) and Mini-Z assessments were used to collect baseline burnout scores and participants were randomized into the intervention group, which completed the assessment again after the Shinrin-Yoku walk, or into a control group, which completed the assessments again after a day off from any clinical duties. A total of 34 participants were enrolled in the intervention group and a total of 22 participants were enrolled in the control group. Ultimately, no statistically significant differences were detected between the pre-test and post-test scores for the intervention group or between the post-test scores of the intervention group compared to the control group. However, the subjective responses collected from participants after participating in the Shinrin-Yoku walk overwhelmingly reported decreased feelings of stress and increased mental wellbeing. This raises important questions about the difference between symptoms of burnout and other aspects of mental health, as well as the limitations of a one-time nature-based intervention on levels of chronic burnout symptoms. Thus, further research on the effects of engaging healthcare providers in an ongoing practice of Shinrin-Yoku is warranted.
The Relation between Nuclear Activity and Stellar Mass in Galaxies

ABSTRACT The existence ofcorrelationsbetween nuclearpropertiesofgalaxies,such as the massoftheir central black holes, and larger scale features, like the bulge mass and luminosity,represent a fundamental constraint on galaxy evolution. Although the actual reasonsfor these relations have not yet been identiﬁed, it is widely believed that they couldstem from a connection between the processes that lead to black hole growth andstellar mass assembly. The problem of understanding how the processes of nuclearactivity and star formation can aﬀect each other became known to the literature as theStarburst-AGN connection. Despite years of investigation, the physical mechanismswhich lie at the basis of this relation are known only in part. In this work, we analyzethe problem of star formation and nuclear activity in a large sample of galaxies. Westudy the relations between the properties of the nuclear environments and of theirhost galaxies. We ﬁnd that the mass of the stellar component within the galaxies of oursample is a critical parameter, that we have to consider in an evolutionary sequence,which provides further insight in the connection between AGN and star formationprocesses.Key words: galaxies: active – galaxies: evolution – galaxies: ISM – galaxies: nuclei– galaxies: stellar content
RING-APODIZED VORTEX CORONAGRAPHS FOR OBSCURED TELESCOPES. I. TRANSMISSIVE RING APODIZERS

The vortex coronagraph (VC) is a new generation small inner working angle (IWA) coronagraph currently offered on various 8 m class ground-based telescopes. On these observing platforms, the current level of performance is not limited by the intrinsic properties of actual vortex devices, but by wavefront control residuals and incoherent background (e.g., thermal emission of the sky), or the light diffracted by the imprint of the secondary mirror and support structures on the telescope pupil. In the particular case of unfriendly apertures (mainly large central obscuration) when very high contrast is needed (e.g., direct imaging of older exoplanets with extremely large telescopes or space-based coronagraphs), a simple VC, like most coronagraphs, cannot deliver its nominal performance because of the contamination due to the diffraction from the obscured part of the pupil. Here, we propose a novel yet simple concept that circumvents this problem. We combine a vortex phase mask in the image plane of a high-contrast instrument with a single pupil-based amplitude ring apodizer, tailor-made to exploit the unique convolution properties of the VC at the Lyot-stop plane. We show that such a ring-apodized vortex coronagraph (RAVC) restores the perfect attenuation property of the VC regardless of the size of the central obscuration, and for any (even) topological charge of the vortex. More importantly, the RAVC maintains the IWA and conserves a fairly high throughput, which are signature properties of the VC.
The Balance of Thermodynamic Potentials in Solar Cells Investigated by Numerical Device Simulations

This contribution presents an extension of the classical gain/loss analysis of Brendel et al. (Appl. Phys. Lett. 93, 173503, 2008) based on the balance of free energy in a solar cell. We consider the full balance of all thermodynamic potentials by separating the excess free energy into excess chemical and electrostatic potentials. A layer by layer analysis of an exemplary silicon solar cell shows that the different functionalities of different parts of the solar cell, e.g., the neutral base and the space charge regions, are well reflected in the different pictures provided by looking at the thermodynamic potentials separately.
ON THE ASSEMBLY OF THE MILKY WAY DWARF SATELLITES AND THEIR COMMON MASS SCALE

We use a particle tagging technique to dynamically populate the N-body Via Lactea II high-resolution simulation with stars. The method is calibrated using the observed luminosity function of Milky Way (MW) satellites and the concentration of their stellar populations, and self-consistently follows the accretion and disruption of progenitor dwarfs and the buildup of the stellar halo in a cosmological “live host. ” Simple prescriptions for assigning stellar populations to collisionless particles are able to reproduce many properties of the observed MW halo and its surviving dwarf satellites, like velocity dispersions, sizes, brightness profiles, metallicities, and spatial distribution. Our model predicts the existence of approximately 1850 subhalos harboring “extremely faint” satellites (with mass-to-light ratios >5 × 103) lying beyond the Sloan Digital Sky Survey detection threshold. Of these, about 20 are “first galaxies,” i.e., satellites that formed a stellar mass above 10 M☉ before redshift 9. The 10 most luminous satellites (L > 106 L☉) in the simulation are hosted by subhalos with peak circular velocities today in the range Vmax = 10–40 km s−1 that have shed between 80% and 99% of their dark mass after being accreted at redshifts 1.7 < z < 4.6. The satellite maximum circular velocity Vmax and stellar line-of-sight velocity dispersion σlos today follow the relation Vmax = 2. 2σlos. We apply a standard mass estimation algorithm based on Jeans modeling of the line-of-sight velocity dispersion profiles to the simulated dwarf spheroidals and test the accuracy of this technique. The inner (within 300 pc) mass–luminosity relation for currently detectable satellites is nearly flat in our model, in qualitative agreement with the “common mass scale” found in MW dwarfs. We do, however, predict a weak, but significant positive correlation for these objects: M300∝L0.088 ± 0.024.