Miracle-dz/UniFAR-FTUs huggingface dataset:
Probing a massive radio galaxy with gravitational lensing

The gravitational lens system CLASS B2108+213 has two lensed images separated by 4.56 arcsec. Such a wide image separation suggests that the lens is either a massive galaxy or composed of a group of galaxies. To investigate the structure of the lensing potential we have carried out new high-resolution imaging of the two lensed images at 1.7 GHz with the Very Long Baseline Array (VLBA) and at 5 GHz with global Very Long Baseline Interferometry (VLBI). Compact and extended emission is detected from the two lensed images, which provides additional constraints to the lensing mass model. We find that the data are consistent with either a single lensing galaxy or a two galaxy lens model that takes account of a nearby companion to the main lensing galaxy within the Einstein radius of the system. However, for an ensemble of global power-law mass models, those with density profiles steeper than isothermal are a better fit. The best-fitting profile for a single spherical mass model has a slope of gamma = 2.45(-0.18)(+0.19). The system also has a third radio component which is coincident with the main lensing galaxy. This component is detected at milliarcsecond scales for the first time by the 1.7-GHz VLBA and 5-GHz global VLBI imaging. However, the third radio component is found not to be consistent with a core lensed image because the radio spectrum differs from the two lensed images, and its flux density is too high when compared to what is expected from simple mass models with a variable power-law density profile and/or a reasonable core radius. Furthermore, 1.4 GHz imaging of the system with the Multi-Element Radio Link Interferometric Network (MERLIN) finds extended lobe emission on either side of the main lensing galaxy. Therefore, the radio emission from the third radio component is almost certainly from an active galactic nucleus (AGN) within the main lensing galaxy, which is classified as a Fanaroff-Riley I (FR I) type radio source.
Spectral and Timing Studies of Cyg X-1 in the Low/Hard State with Suzaku

AbstractFrom 2005 to 2009, 25 observations of Cyg X-1 were performed with Suzaku, achiev-ing a total exposure of 446 ks. In all observations, the source was found in the low/hardstate, while the 1.5–12.0 keV count rate of the All-Sky Monitor onboard RXTE varied bya factor of ∼ 3. In each observation, the 10–60 keV HXD-PIN spectrum and the 60–400keV HXD-GSO spectrum were ﬁtted successfully by a thermal Comptonization model plusreﬂection by a thick neutral material. As the soft X-ray intensity increased, the Comptony-parameter was found to decrease from 1.0 to 0.6, while the solid angle of reﬂection toincrease by ∼ 30%. Also conducted was timing analysis over a frequency range of 10 −3 –10 Hz. As the source became brighter in soft X-rays, the characteristic frequency of hardX-ray variation increased from 0.03 to 0.3 Hz, while the fractional hard X-ray variationintegrated over 10 −3 –10 −2 Hz decreased by a factor of ∼ 5. The signals in the 60–200keV band were generally found to vary on shorter time scales than those in the 10–60 keVband. These spectral and timing results can be consistently interpreted by presuming thatincreases in the mass accretion rate cause the Comptonizing hot corona to shrink, while theoptically-thick disk to intrude deeper therein.Key words: black hole physics — accretion — stars: individual (Cygnus X -1)—X-ray:binaries1
MHD simulation of the inner‐heliospheric magnetic field

Maps of the radial magnetic field at a heliocentric distance of 10 solar radii are used as boundary conditions in the MHD code CRONOS to simulate a three‐dimensional inner‐heliospheric solar wind emanating from the rotating Sun out to 1 AU. The input data for the magnetic field are the result of solar surface flux transport modeling using observational data of sunspot groups coupled with a current‐sheet source surface model. Among several advancements, this allows for higher angular resolution than that of comparable observational data from synoptic magnetograms. The required initial conditions for the other MHD quantities are obtained following an empirical approach using an inverse relation between flux tube expansion and radial solar wind speed. The computations are performed for representative solar minimum and maximum conditions, and the corresponding state of the solar wind up to the Earth's orbit is obtained. After a successful comparison of the latter with observational data, they can be used to drive outer‐heliospheric models.
HD 106906: A Case Study for External Perturbations of a Debris Disk

Models of debris disk morphology are often focused on the effects of a planet orbiting interior to or within the disk. Nonetheless, an exterior planetary-mass perturber can also excite eccentricities in a debris disk, via Laplace–Lagrange secular perturbations in the coplanar case or Kozai–Lidov perturbations for mutually inclined companions and disks. HD 106906 is an ideal example of such a a system, as it harbors a confirmed exterior companion at a projected separation of 650 au outside a resolved, asymmetric disk. We use collisional and dynamical simulations to investigate the interactions between the disk and the companion, and to use the disk’s observed morphology to place constraints on the companion’s orbit. We conclude that the disk’s observed morphology is consistent with perturbations from the observed exterior companion. Generalizing this result, we suggest that exterior perturbers, as well as interior planets, should be considered when investigating the cause of observed asymmetries in a debris disk.
Suppression of galactic outflows by cosmological infall and circumgalactic medium

We investigate the relative importance of two galactic outflow suppression mechanisms : a) Cosmological infall of the intergalactic gas onto the galaxy, and b) the existence of a hot circumgalactic medium (CGM). Considering only radial motion, the infall reduces the speed of outflowing gas and even halts the outflow, depending on the mass and redshift of the galaxy. For star forming galaxies there exists an upper mass limit beyond which outflows are suppressed by the gravitational field of the galaxy. We find that infall can reduce this upper mass limit approximately by a factor of two (independent of the redshift). Massive galaxies ($\gtrsim 10^{12} M_{\odot}$) host large reservoir of hot, diffuse CGM around the central part of the galaxy. The CGM acts as a barrier between the infalling and outflowing gas and provides an additional source of outflow suppression. We find that at low redshifts ($z\lesssim3.5$), the CGM is more effective than the infall in suppressing the outflows. Together, these two processes give a mass range in which galaxies are unable to have effective outflows. We also discuss the impact of outflow suppression on the enrichment history of the galaxy and its environment.
Probing Satellite Quenching With Galaxy Clustering

Satellites within simulated massive clusters are significantly spatially correlated with each other, even when those satellites are not gravitationally bound to each other. This correlation is produced by satellites that entered their hosts relatively recently, and is undetectable for satellites that have resided in their hosts for multiple dynamical timescales. Therefore, a measurement of clustering statistics of cluster satellites may be used to determine the typical accretion redshifts of those satellites into their observed hosts. We argue that such measurements may be used to determine the fraction of satellite galaxies that were quenched by their current hosts, thereby discriminating among models for quenching of star formation in satellite galaxies.
Finite Lattice and Phenomenological Approximations for the Anomaly in the Density of a Water-like Lattice Gas Model

We propose a model for a two dimensional, associative water-like lattice gas with one single variable representing both long and short-range interactions. The corresponding hamiltonian was solved exactly, by state enumeration in a finite lattice, so to obtain an analytic expression for the partition function. The lattice dimensions were chosen based on geometric characteristics of the stable phases found in previous works using Monte Carlo simulations. An expression for the particle density in the finite lattice was then obtained, and coexistence curves with a region of anomaly in the density presented in a phase diagram. In the end, a phenomenological theory for the system density is proposed and compared to the previous results.
Walking Behavior of Older Adults in Temuco, Chile: The Contribution of the Built Environment and Socio-Demographic Factors

The amount of walking for daily transport has decreased significantly over the last decades in Temuco, Chile. Moreover, the percentage of older adults (aged over 65) who did not meet the recommendations of at least 150 min of physical activity per week has increased during this time. In this regard, the present study examines the contribution of socio-demographic and built environment factors on the walking behavior of older adults in Temuco, Chile, with a view to improving their level of physical activity. A cross-sectional study was conducted among 463 older adults aged 60 years and over. Travel Diary Data taken from “Encuesta Origin Destino” (EOD) 2013, Geographic information systems (GIS), audits (PEDS with certain revisions) and finally, multiple regression analysis, were used to examine the objectives. Associations were found between the walking behavior of older adults and several socio-demographic factors, as well as several built environment factors including destination (the number of parks and the land use mix), functionality (street connectivity, length of street sections and off-street parking lots) and aesthetics (views of nature, building height, and articulation in building design). These findings should be considered by urban/transport policymakers to improve the walking behavior of older adults in this city.
WASP 0639-32: a new F-type subgiant/K-type main-sequence detached eclipsing binary from the WASP project

Aims. Our aim is to measure the masses and radii of the stars in a newly-discovered detached eclipsing binary system to a high precision (≈1%), enabling the system to be used for the calibration of free parameters in stellar evolutionary models. Methods. Photometry from the Wide Angle Search for Planets (WASP) project was used to identify 1SWASP J063930.33-322404.8 (TYC 7091-888-1, WASP 0369-32 hereafter) as a detached eclipsing binary system with total eclipses and an orbital period of P = 11.66 days. Lightcurve parameters for WASP 0639-32 are obtained using the EBOP lightcurve model, with standard errors evaluated using a prayer-bead algorithm. Radial velocities were measured from 11 high-resolution spectra using a broadening function approach, and an orbit was fitted using SBOP. Observed spectra were disentangled and an equivalent width fitting method was used to obtain effective temperatures and metallicities for both stars. A Bayesian framework is used to explore a grid of stellar evolution models, where both helium abundance and mixing length are free to vary, and use observed parameters (mass, density, temperature, and metallicity) for each star to obtain the age and constrain the helium abundance of the system. Results. The masses and radii are found to be M1 = 1.1544 ± 0.0043 M⊙, R1 = 1.833 ± 0.023 R⊙, and M2 = 0.7833 ± 0.0028 M⊙, R2 = 0.7286 ± 0.0081 R⊙ for the primary and secondary, respectively. The effective temperatures were found to be T1 = 6330 ± 50 K and T2 = 5400 ± 80 K for the primary and secondary star, respectively. The system has an age of 4.2−0.1+0.8 Gyr, and a helium abundance in the range 0.251–0.271. Conclusions. WASP 0639-32 is a rare example of a well-characterised detached eclipsing binary system containing a star near the main-sequence turn-off point. This makes it possible to measure a precise age for the stars in this binary system and to estimate their helium abundance. Further work is needed to explore how this helium abundance estimate depends on other free parameters in the stellar models.
Beta-decay study of $T_z=-2$ proton-rich nucleus $^{20}$Mg

The $\beta$ decay of the drip-line nucleus $^{20}$Mg gives important information on resonances in $^{20}$Na, which are relevant for the astrophysical $rp$-process. A detailed $\beta$ decay spectroscopic study of $^{20}$Mg was performed by a continuous-implantation method. A detection system was specially developed for charged-particle decay studies, giving improved spectroscopic information including the half-life of $^{20}$Mg, the excitation energies, the branching ratios, and the log $ft$ values for the states in $^{20}$Na populated in the $\beta$ decay of $^{20}$Mg. A new proton branch was observed and the corresponding excited state in $^{20}$Na was proposed. The large isospin asymmetry for the mirror decays of $^{20}$Mg and $^{20}$O was reproduced, as well. However, no conclusive conclusion can be draw about the astrophysically interesting 2645~keV resonance in $^{20}$Na due to the limited statistics.
Testing Feedback-regulated Star Formation in Gas-rich, Turbulent Disk Galaxies

In this paper we compare the molecular gas depletion times and midplane hydrostatic pressure in turbulent, star-forming disk galaxies to internal properties of these galaxies. For this analysis we use 17 galaxies from the DYNAMO sample of nearby (z ∼ 0.1) turbulent disks. We find a strong correlation, such that galaxies with lower molecular gas depletion time (tdep) have higher gas velocity dispersion (σ). Within the scatter of our data, our observations are consistent with the prediction that made in theories of feedback-regulated star formation. We also show a strong, single power-law correlation between midplane pressure (P) and star formation rate surface density (ΣSFR), which extends for 6 orders of magnitude in pressure. Disk galaxies with lower pressure are found to be roughly in agreement with theoretical predictions. However, in galaxies with high pressure we find P/ΣSFR values that are significantly larger than theoretical predictions. Our observations could be explained with any of the following: (1) the correlation of ΣSFR−P is significantly sublinear; (2) the momentum injected from star formation feedback (p*/m*) is not a single, universal value; or (3) alternate sources of pressure support are important in gas-rich disk galaxies. Finally, using published survey results, we find that our results are consistent with the cosmic evolution of tdep(z) and σ(z). Our interpretation of these results is that the cosmic evolution of tdep may be regulated not just by the supply of gas but also by the internal regulation of star formation via feedback.
Linking the Supermassive Black Hole Growth with the Megamaser Emission

High-resolution observations of the central few 100 pc of the galactic nuclear environments remain prohibitive for large statistical samples, which are crucial for tracing the links between central black hole formation, galaxy formation and AGN activity over cosmic time. With this contribution, we present novel ways of connecting the physics of black hole accretion with its immediate environs via a new quantitative evaluation of the degree to which the strength and spatial configuration of the water maser emission is associated with the nuclear nebular galactic activity. We discuss possible evolutionary/causal connections between these two types of emission, together with criteria that could dramatically enhance our search for mega-maser systems in nearby galactic centers. These are timely results given the interest in combining high-resolution observations with extremely large optical telescopes and large arrays that start to conquer the sub-millimeter window.
Influence of Palliative Care Qualifications on the Job Stress Factors of General Practitioners in Palliative Care: A Survey Study

Due to demographic change, the number of patients in palliative care (PC) is increasing. General Practitioners (GPs) are important PC providers who often have known their patients for a long time. PC can be demanding for GPs. However, there are few studies on the job stress factors of GPs performing PC and the potential influence of their PC training. To get more insights, a postal survey was performed with GPs in North Rhine, Germany. The questionnaire was based on a literature search, qualitative pre-studies, and the Hospital Consultants’ Job Stress & Satisfaction Questionnaire (HCJSSQ). Participants state that a high level of responsibility, conflicting demands, and bureaucracy are the most important stressors they experienced in PC. The influence of PC qualification level on their perceived job stress factors is low. Only advanced but not specialist qualification shows a correlation with renumeration-related stress. Gender and work experience are more dominant influences. In our study, female GPs and physicians with more work experience tend to be more stressed. In conclusion, organisational barriers, such as administration, should be reduced and renumeration should be increased to facilitate the daily work of GPs.
uvbyβ photometry of early type open cluster and field stars

Context. The β Cephei stars and slowly pulsating B (SPB) stars are massive main sequence variables. The strength of their pulsational driving strongly depends on the opacity of iron-group elements. As many of those stars naturally occur in young open clusters, whose metallicities can be determined in several fundamental ways, it is logical to study the incidence of pulsation in several young open clusters. Aims. To provide the foundation for such an investigation, Stromgren-Crawford uvbyβ photometry of open cluster target stars was carried out to determine effective temperatures, luminosities, and therefore cluster memberships. Methods. In the course of three observing runs, uvbyβ photometry for 168 target stars was acquired and transformed into the standard system by measurements of 117 standard stars. The list of target stars also included some known cluster and field β Cephei stars, as well as β Cephei and SPB candidates that are targets of the asteroseismic part of the Kepler satellite mission. Results. The uvbyβ photometric results are presented. The data are shown to be on the standard system, and the properties of the target stars are discussed: 140 of these are indeed OB stars, a total of 101 targets lie within the β Cephei and/or SPB star instability strips, and each investigated cluster contains such potential pulsators. Conclusions. These measurements will be taken advantage of in a number of subsequent publications.
On the Possible Trajectories of Particles with Spin. III. Particles in the Stationary Homogeneous Electric Field

The behavior of spinning particles in the stationary homogeneous magnetic field is considered and all types of trajectories for massive and massless particles are found. It is shown that spin of particles in a magnetic field is always arranged parallel or antiparallel to the field. Helicity $e$ plays a role of electric charge. The oscillation frequency of massless particle in a magnetic field increases.
Mapping 2‐D Bedload Rates Throughout a Sand‐Bed River Reach From High‐Resolution Acoustical Surveys of Migrating Bedforms

This paper introduces a method for determining spatially‐distributed, 2‐D bedload rates using repeat, high‐resolution surveys of the bed topography. As opposed to existing methods, bedform parameters and bedload rates are computed from bed elevation profiles interpolated along the local bedform velocities. The bedform velocity fields are computed applying Large‐Scale Particle Image Velocimetry, initially developed for surface velocity measurements, to pairs of successive Digital Elevation Models (DEMs). The bathymetry data are interpolated along the direction of each bedform velocity and the mean height of the closest bedform is computed. The dune shape factor is also evaluated along each bedform direction of travel. The local bedload fluxes can be computed by multiplying the bedform velocity by its mean height averaged over the successive two DEMs, and they can be time‐averaged over a series of DEM pairs. This method is applied to a high‐resolution acoustical survey of an approximately 300 m long by 40 m wide reach of the Colorado River in Grand Canyon upstream from Diamond Creek, USA. The repeat period was about 6–10 min and bed elevation was interpolated every 0.25 m. The obtained results provide insight to the spatial and temporal variability of bedload rates, bedform parameters and bedload fluxes through cross‐sections. The method can be applied to other repeated acoustical surveys of river reaches provided that the space and time resolutions are high enough to capture the local movement of bedforms.
Amplitudes for the analysis of the decay J / ψ → K + K − π 0

We construct an analytical model for two channel, two-body scattering amplitudes, and then apply it in the description of the three-body $J/\psi \to K^+K^-\pi^0$ decay. In the construction of the partial wave amplitudes, we combine the low energy resonance region with the Regge asymptotic behavior determined from direct two-body production. We find that resonance production in the $K\pi$ channel in $J/\psi$ decays seems to differ from that observed in direct $K\pi$ production, while the mass distribution in the $K\bar K$ channel may be compatible.
Incidence of Nephrotoxicity among People Living with Human Immunodeficiency Virus on Tenofovir Treatment in a Tertiary Hospital in the Philippines

Objective: We aimed to determine the incidence and risk factors of nephrotoxicity among Filipino human immunodeficiency virus (HIV) patients on tenofovir disoproxil fumarate (TDF). Methods: Retrospective cohort study; we reviewed medical records of HIV adults on TDF in the University of the Philippines-Philippine General Hospital (UP-PGH) clinic from January 2004 - December 2016. Nephrotoxicity was defined as at least a 20% decline in estimated glomerular filtration rate (eGFR). Relevant demographic and laboratory data were collected. Statistical analysis was performed to compare characteristics between groups. Kaplan-Meier method was used to determine incidence rate over time, and incidence density rates of nephrotoxicity were calculated. Results: 654 patients were included, with mean age of 29 years (18-69) and male-female ratio of 72:1. Nephrotoxicity incidence was 51.38% with a density rate of 11.05 per 10,000 person days. Kaplan Meier analysis showed probability of nephrotoxicity of 50% at 20.4 months. Cox regression modeling of covariates revealed low CD4 as a significant covariate for predicting a subsequent 20% eGFR decline. Conclusion: TDF may contribute to a decline in GFR over time. Half of patients taking TDF developed mild nephrotoxicity by 20.5 months. Clinicians must consider the potential risk of nephrotoxicity with prolonged use especially among young patients with low CD4 counts.