Miracle-dz/UniFAR-FTUs huggingface dataset:
Validation of Trauma-Informed Care Instruments: Emergency Department Environment and Transitional Secondary Environment

Background: Trauma-informed care is a paradigm of care that requires health care practitioners to understand multiple types of traumas and their effects on the trauma survivor and then incorporate that knowledge into practice. However, there are few psychometrically robust instruments to evaluate trauma-informed care, and none have been applied in the trauma patient setting. Objective: The purpose of this article is to validate two trauma-informed care instruments in the trauma patient setting. Method: Exploratory factor analysis and simultaneous pairwise marginal independence testing procedures were conducted on the “Emergency Department Environment” and the “Transitional Secondary Environment” instruments from September 2020 to November 2020. Descriptive statistics were reported for the content experts participating in the instrument validation. Result: Exploratory data analysis results for each trauma-informed care statement in the tools indicate multidimensionality of trauma-informed care core values, with statistically significant (p < .05) overlap between two or more trauma-informed care core values. After accounting for item interdependence, the associations between the trauma-informed care core values do not appear to be spurious consequences of response interdependence. Conclusion: The two instruments showed high levels of internal consistency supporting the multidimensional models posited by the trauma-informed care framework. The findings will allow for routine monitoring and early detection of gaps in health care provider behaviors in the individualized care of trauma survivors. This will enable identification of trends in trauma care delivery and inform trauma-informed care education for health care providers, ultimately enhancing the healing of trauma survivors.
A PARAMETERIZED GALAXY CATALOG SIMULATOR FOR TESTING CLUSTER FINDING, MASS ESTIMATION, AND PHOTOMETRIC REDSHIFT ESTIMATION IN OPTICAL AND NEAR-INFRARED SURVEYS

We present a galaxy catalog simulator that converts N-body simulations with halo and subhalo catalogs into mock, multiband photometric catalogs. The simulator assigns galaxy properties to each subhalo in a way that reproduces the observed cluster galaxy halo occupation distribution, the radial and mass-dependent variation in fractions of blue galaxies, the luminosity functions in the cluster and the field, and the color–magnitude relation in clusters. Moreover, the evolution of these parameters is tuned to match existing observational constraints. Parameterizing an ensemble of cluster galaxy properties enables us to create mock catalogs with variations in those properties, which in turn allows us to quantify the sensitivity of cluster finding to current observational uncertainties in these properties. Field galaxies are sampled from existing multiband photometric surveys of similar depth. We present an application of the catalog simulator to characterize the selection function and contamination of a galaxy cluster finder that utilizes the cluster red sequence together with galaxy clustering on the sky. We estimate systematic uncertainties in the selection to be at the ⩽15% level with current observational constraints on cluster galaxy populations and their evolution. We find the contamination in this cluster finder to be ∼35% to redshift z ∼ 0.6. In addition, we use the mock galaxy catalogs to test the optical mass indicator Bgc and a red-sequence redshift estimator. We measure the intrinsic scatter of the Bgc–mass relation to be approximately log normal with and we demonstrate photometric redshift accuracies for massive clusters at the ∼3% level out to z ∼ 0.7.
QoS-Aware Matchmaking for Adaptative Microservice-based Applications

Applications that make use of Internet of Things (IoT) can capture an enormous amount of raw data from sensors and actuators, which is frequently transmitted to cloud data centres for processing and analysis. However, due to varying and unpre-dictable data generation rates and network latency, this can lead to a performance bottleneck for data processing. With the emergence of Fog and Edge computing hosted microservices, data processing could be moved towards the network edge. We propose a new method for continuous deployment and adaptation of multi-tier applications along edge, fog and cloud tiers by considering resource properties and non-functional requirements (e.g. operational cost, response time and latency etc.). The proposed approach supports matchmaking of application and Cloud-To-Things infrastructure based on a subgraph pattern matching ( P-Match ) technique. Results show that the proposed approach improves resource utilisation and overall application Quality of Service. The approach can also be integrated into software engineering workbenches for the creation and deployment of cloud-native applications, enabling partitioning of an application across the multiple infrastructure tiers outlined above.
The distance to NGC1316 (Fornax A): yet another curious case ⋆

Aims. The distance of NGC 1316, the brightest galaxy in the Fornax cluster, provides an interesting test for the cosmological distance scale. First, because Fornax is the second largest cluster of galaxies within 25 Mpc after Virgo and, in contrast to Virgo, has a small line-of-sight depth; and second, because NGC 1316 is the single galaxy with the largest number of detected Type Ia supernovae (SNe Ia), giving the opportunity to test the consistency of SNe Ia distances both internally and against other distance indicators. Methods. We measure surface brightness fluctuations (SBF) in NGC 1316 from ground- and space-based imaging data. The sample provides a homogeneous set of measurements over a wide wavelength interval. The SBF magnitudes, coupled with empirical and theoretical absolute SBF calibrations, are used to estimate the distance to the galaxy. We also present the first B-band SBF measurements of NGC 1316 and use them together with the optical and near-IR SBF data to analyze the properties of field stars in the galaxy. Results. We obtain (m−M) = 31.59± 0.05(stat.)± 0.14(sys. )m ag, ord = 20.8± 0.5(stat.)± 1.5(sys.) Mpc. When placed in a consistent Cepheid distance scale, our result agrees with the distances from other indicators. On the other hand, our distance is ∼17% larger than the most recent estimate based on SNe Ia. Possible explanations for this disagreement are the uncertain level of internal extinction, and/or calibration issues. Concerning the stellar population analysis, we confirm the results from other spectro-photometric indicators: the field stars in NGC 1316 are dominated by a component with roughly solar metallicity and intermediate age. A non-negligible mismatch exists between B-band SBF models and data. We confirm that such behavior can be accounted for by an enhanced percentage of hot horizontal branch stars. Conclusions. Our study of the SBF distance to NGC 1316, and the comparison with distances from other indicators, raises some concern about the homogeneity between the calibrations of different indicators. If not properly placed in the same reference scale, significant differences can occur, with dramatic impact on the cosmological distance ladder. Our results on the stellar populations properties show that SBF data over a broad wavelength interval are an efficient means of studying the properties of unresolved systems in peculiar cases like NGC 1316.
Indoctrination, Citizenship and Political Regimes ∗

What are the origins of sincere mass support for nondemocratic regimes? Inﬂuential research on authoritarian politics commonly emphasizes the importance of repression and goods provision for generating citizen compliance. In this paper, we instead aim to draw the focus on indoctrination, and especially the use of education as a political tool. Firstly, we review and synthesize the existing, but scattered literature on indoctrination, education and mass media. Secondly, we provide a new theoretical framework, focusing on indoctrination as a political tool to shape sincere public support for autocracies. We further outline an empirical strategy on how to measure indoctrination and present ﬁrst empirical results from a pilot study in six countries, including China and Russia.
Synthesis and Characterization of CuO nanoparticles Using Morus, Citrus and Gossypium Plants Extract and Antibacterial Activities

Copper oxide (CuO) nanoparticles (NPs) were synthesized biological methods using aqueous extract of leaves of Morus, Citrus, and Gossypium. Leaves as a reducing and capping agent. The advantages of this methods are simple operation, use of cheap, natural, nontoxic and benign precursors, absence of toxic reagents and mild and environmentally friendly conditions. The green synthesized CuO NPs was characterized by X-ray diffraction (XRD) analysis demonstrated that the CuO NPs were crystalline with a mono clinic structure. The formation of NPs is monitored by recording the UV –vis optical properties exhibits in UV - region and band gap energy (Eg) greater than 3 eV. Electrical conductivity increases when temperature increases during the synthesis. Antibacterial study of the CuNPs was established using both gram positive and gram negative pathogens. Keywords :Biological methods, CuO nanoparticles, Extract, Antibacterial.
DIRECT MEASUREMENT OF THE X-RAY TIME-DELAY TRANSFER FUNCTION IN ACTIVE GALACTIC NUCLEI

The origin of the observed time lags, in nearby active galactic nuclei (AGNs), between hard and soft X-ray photons is investigated using new XMM-Newton data for the narrow-line Seyfert I galaxy Ark 564 and existing data for 1H 0707–495 and NGC 4051. These AGNs have highly variable X-ray light curves that contain frequent, high peaks of emission. The averaged light curve of the peaks is directly measured from the time series, and it is shown that (1) peaks occur at the same time, within the measurement uncertainties, at all X-ray energies, and (2) there exists a substantial tail of excess emission at hard X-ray energies, which is delayed with respect to the time of the main peak, and is particularly prominent in Ark 564. Observation (1) rules out that the observed lags are caused by Comptonization time delays and disfavors a simple model of propagating fluctuations on the accretion disk. Observation (2) is consistent with time lags caused by Compton-scattering reverberation from material a few thousand light-seconds from the primary X-ray source. The power spectral density and the frequency-dependent phase lags of the peak light curves are consistent with those of the full time series. There is evidence for non-stationarity in the Ark 564 time series in both the Fourier and peaks analyses. A sharp “negative” lag (variations at hard photon energies lead soft photon energies) observed in Ark 564 appears to be generated by the shape of the hard-band transfer function and does not arise from soft-band reflection of X-rays. These results reinforce the evidence for the existence of X-ray reverberation in type I AGN, which requires that these AGNs are significantly affected by scattering from circumnuclear material a few tens or hundreds of gravitational radii in extent.
All-electron GW methods implemented in molecular orbital space: Ionization energy and electron affinity of conjugated molecules

An efficient all-electron G$^0$W$^0$ method and a quasiparticle selfconsistent GW (QSGW) method for molecules are proposed in the molecular orbital space with the full random phase approximation. The convergence with basis set is examined. As an application, the ionization energy ($I$) and electron affinity ($A$) of a series of conjugated molecules (up to 32 atoms) are calculated and compared to experiment. The QSGW result improves the G$^0$W$^0$ result and both of them are in significantly better agreement with experimental data than those from Hartree-Fock (HF) and hybrid density functional calculations, especially for $A$. The nearly correct energy gap and suppressed self-interaction error by the HF exchange make our method a good candidate for investigating electronic and transport properties of molecular systems.
Modelling Wt and tWZ production at NLO for ATLAS analyses

The generation of single top production in the $Wt$ channel at NLO gives rise to doubly-resonant diagrams that overlap with $t \bar t$, and similarly for associated production with a $Z$ or Higgs boson. Several methods exist to remove this overlap, thus avoiding double counting and separating the two processes. In Diagram Removal 1, the amplitudes of doubly-resonant diagrams are set to zero, which also removes the interference of $Wt$ with $t \bar t$. If a measurement is performed in a region where this interference is not negligible, it would be of interest to take it into account. Another method, Diagram Subtraction, preserves the interference. However, it relies upon momentum reshuffling, which introduces uncertainties to the prediction. An alternative method, Diagram Removal 2, does not involve reshuffling and preserves the interference by subtracting the amplitude squared of the doubly-resonant diagrams from the total. The predictions of Diagram Removal 2 from MG5_aMC@NLO are compared with other predictions for $Wt$ and $tWZ$ production in the context of analyses at the ATLAS experiment. Implications of using Diagram Removal 2 are discussed, both for measurements of single top processes and when $Wt$ or $tWZ$ are treated as a background. Differential distributions are shown, investigating in what regions the predictions differ the most.
Search for gravitational lens candidates in the XMM-LSS/CFHTLS common field

Our aim was to identify gravitational lens candidates among some 5500 optical counterparts of the X-ray point-like sources in the medium-deep ~11 sq. deg. XMM-LSS survey. We have visually inspected the optical counterparts of each QSOs/AGN using CFHTLS T006 images. We have selected compact pairs and groups of sources which could be multiply imaged QSO/AGN. We have measured the colors and characterized the morphological types of the selected sources using the multiple PSF fitting technique. We found three good gravitational lens candidates: J021511.4-034306, J022234.3-031616 and J022607.0-040301 which consist of pairs of point-like sources having similar colors. On the basis of a color-color diagram and X-ray properties we could verify that all these sources are good QSO/AGN candidates rather than stars. Additional secondary gravitational lens candidates are also reported.
THE SUBSTELLAR POPULATION OF σ ORIONIS: A DEEP WIDE SURVEY

We present a deep I, Z photometric survey covering a total area of 1.12 deg2 of the σ Orionis cluster and reaching completeness magnitudes of I = 22 and Z = 21.5 mag. From I, I − Z color–magnitude diagrams we have selected 153 candidates that fit the previously known sequence of the cluster. They have magnitudes in the range I = 16–23 mag, which corresponds to a mass interval from 0.1 down to 0.008 M☉ at the most probable age of σ Orionis (2–4 Myr). Using J-band photometry, we find that 124 of the 151 candidates within the completeness of the optical survey (82%) follow the previously known infrared photometric sequence of the cluster and are probably members. We have studied the spatial distribution of the very low mass stars and brown dwarf population of the cluster and found that there are objects located at distances greater than 30 arcmin to the north and west of σ Orionis that probably belong to different populations of the Orion's Belt. For the 102 bona fide σ Orionis cluster member candidates, we find that the radial surface density can be represented by a decreasing exponential function () with a central density of σ0 = 0.23 ± 0.03 objects arcmin−2 and a characteristic radius of r0 = 9.5 ± 0.7 arcmin. From a statistical comparison with Monte Carlo simulations, we conclude that the spatial distribution of the objects located at the same distance from the center of the cluster is compatible with a Poissonian distribution and, hence, that very low mass stars and brown dwarfs are not mainly forming aggregations or sub-clustering. Using near-infrared JHK-band data from Two Micron All Sky Survey and UKIRT Deep Infrared Sky Survey and mid-infrared data from Infrared Array Camera/Spitzer, we find that about 5%–9% of the brown dwarf candidates in the σ Orionis cluster have K-band excesses and 30% ± 7% of them show mid-infrared excesses at wavelengths longer than 5.8 μm. These are probably related to the presence of disks, most of which are “transition disks. ” We have also calculated the initial mass spectrum (dN/dm) of σ Orionis from very low mass stars (∼0.10 M☉) to the deuterium-burning mass limit (0.012–0.013 M☉), i.e., complete in the entire brown dwarf regime. This mass spectrum is a rising function toward lower masses and can be represented by a power-law distribution (dN/dm ∝ m−α) with an exponent α of 0.7 ± 0.3 for an age of 3 Myr.
Modelling the Magnetic Field Configuration of Neutron Stars

The properties of the extremely strong magnetic fields of neu tron stars affect in a unique way their evolution and the associated phenomenology. Due to the lack of constraints from direct observations, our understanding of the magnetic field configur ation in neutron star interiors depends on the progress in theoret ical modelling. Here we discuss the effort in building models of magnetized neutron stars focussing on some of the recent results. In particular, we comment on the instability of purely poloidal and purely toroidal magnetic field configurations and on the e vidence in favour of the so-called twisted-torus solutions . We conclude with an outlook on the present status of the field and future directions.
Cosmic Voids in Sloan Digital Sky Survey Data Release 7

We study the distribution of cosmic voids and void galaxies using Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Using the VoidFinder algorithm as described by Hoyle & Vogeley (2002), we identify 1054 statistically significant voids in the northern galactic hemisphere with radii > 10h 1 Mpc. The filling factor of voids in the sample volume is 62%. The largest void is just over 30h 1 Mpc in effective radius. The median effective radius is 17h 1 Mpc. The voids are found to be significantly underdense, with density contrast � < 0.85 at the edges of the voids. The radial density profiles of these voids are similar to predictions of dynamically distinct underdensities in gravitational theory. We find 8,046 galaxies brighter than Mr = 20.09 within the voids, accounting for 7% of the galaxies. We compare the results of VoidFinder on SDSS DR7 to mock catalogs generated from a SPH halo model simulation as well as other �-CDM simulations and find similar void fractions and void sizes in the data and simulations. This catalog is made publicly available at http://www.physics. drexel.edu/�pan/VoidCatalog for download.
A study of the distant activity of comet C/2006 W3 (Christensen) with Herschel and ground-based radio telescopes

Comet C/2006 W3 (Christensen) was observed in November 2009 at 3.3 AU from the Sun with Herschel.The PACS instrument acquired images of the dust coma in 70-μm and 160-μm filters and spectra covering several H_2O rotational lines. Spectra in the range 450–1550 GHz were acquired with SPIRE. The comet emission continuum from 70 to 672 μm was measured, but no lines were detected. The spectral energy distribution indicates thermal emission from large particles and provides a measure of the size distribution index and dust production rate. The upper limit to the water production rate is compared to the production rates of other species (CO, CH_3OH, HCN, H_2S, OH) measured with the IRAM 30-m and Nancay telescopes. The coma is found to be strongly enriched in species more volatile than water, in comparison to comets observed closer to the Sun. The CO to H_2O production rate ratio exceeds 220%. The dust-to-gas production rate ratio is on the order of 1.
Violent intranight optical variability of the blazar S4 0954+65 during its unprecedented 2015 February outburst

In this letter we present results from intra-night monitoring in three colors (BRI) of the blazar S4 0954+65 during its recent (2015 February) unprecedented high state. We find violent variations on very short time scales, reaching magnitude change levels of 0.1–0.2 mag/h. On some occasions, changes of �0.1 mag are observed even within �10 min. During the night of 14.02. 2015 an exponential drop of �0.7 magnitudes is detected for about 5 hours. Cross-correlation between the light curves does not reveal any detectable wavelength-dependent time delays, larger than �5 min. Color changes ”bluer-when-brighter” are observed on longer time scales. Possible variability mechanisms to explain the observations are discussed and a preference to the geometrical one is given.
Two barium stars in the Galactic bulge

Barium stars conserve important information on the s-process and the third dredge-up in intermediate mass stars. Their discovery in various environments is therefore of great help to test nucleosynthesis and mixing models. Our aim is to analyse two stars with a very strong barium line detected in a large survey of red giants in the Galactic bulge. Abundance analysis was done comparing synthetic model spectra based on the COMARCS code with our medium resolution spectra. Abundances of Ba, La, Y, and Fe were determined. Beside the two main targets, the analysis was also applied to two comparison stars. We confirm that both stars are barium stars. They are the first ones of this kind identified in the Galactic bulge. Their barium excesses are among the largest values found up to now. The elemental abundances are compared with current nucleosynthesis and mixing models. Furthermore, we estimate a frequency of barium stars in the Galactic bulge of about 1%, which is identical to the value for disc stars.
Isotropic cases of static charged fluid spheres in general relativity

In this paper we study the isotropic cases of static charged fluid spheres in general relativity. For this purpose we consider two different specialization and under these we solve the Einstein-Maxwell field equations in isotropic coordinates. The analytical solutions thus we obtained are matched to the exterior Reissner-Nordstr\"om solutions which concern with the values for the metric coefficients $e^{\nu}$ and $e^{\mu}$. We derive the pressure, density, pressure-to-density ratio at the centre of the charged fluid sphere and boundary $R$ of the star. Our conclusion is that static charged fluid spheres provide a good connection to compact stars.