Miracle-dz/UniFAR-FTUs huggingface dataset:
J/$\psi$ polarization measurements in p+p collisions at $\sqrt{s}$ = 200 and 500 GeV with the STAR experiment

In these proceedings, measurements of J/psi polarization in p+p collisions at 200 and 500 GeV via the dielectron decay channel at mid-rapidity with the STAR experiment are discussed. At 200 GeV the polarization parameter, $\lambda_{\theta}$, related to the polar anisotropy is obtained in the helicity frame as a function of transverse momentum, 2 < $p_{T}$ < 6 GeV/c, and compared to different model predictions. A new J/psi polarization measurement at 500 GeV extends the previous analysis to a wide transverse momentum range of 5 < $p_{T}$ < 16 GeV/c. Also, the polarization parameter related to the azimuthal anisotropy, $\lambda_{\phi}$, is extracted in addition to $\lambda_{\theta}$, in two reference frames: the helicity and Collins-Soper frames. This allows for the frame invariant parameter calculation vs $p_{T}$ in these two frames.
SPECTRAL MAPPING OF THE INTERMEDIATE POLAR DQ HERCULIS

We report an eclipse-mapping study of the intermediate polar DQ Her based on time-resolved optical spectroscopy (Δλ ∼ 3800–5000 Å) covering four eclipses. The spectra were sliced into 295 narrow passbands in the continuum and in the lines, and the corresponding light curves were analyzed to solve for a set of monochromatic maps of the disk brightness distribution and for the flux of an additional uneclipsed component in each band. Eclipse maps of the He ii λ4686 line indicate that an azimuthally and vertically extended bright spot at disk rim is an important source of the reprocessing of X-rays from the magnetic poles. The disk spectrum is flat with no Balmer or Helium lines in the inner regions, and shows double-peaked emission lines in the intermediate and outer disk regions, while the slope of the continuum becomes progressively redder with increasing radius. The inferred disk temperatures are in the range T ≃ 13500–5000 K and can be reasonably well described by a steady-state disk with mass accretion rate of . A comparison of the radial intensity distribution for the Balmer lines reveals a linear correlation between the slope of the distribution and the transition energy. The spectrum of the uneclipsed light is dominated by Balmer and He i lines in emission (probably from the extended nova shell) with narrow absorption cores (likely from a collimated and optically thick wind from the accretion disk). The observed narrow and redshifted Ca ii λ3934 absorption line in the total light spectra plus the inverse P-Cygni profiles of the Balmer and He ii λ4686 emission lines in spectra of the asymmetric component indicate radial inflow of gas in the innermost disk regions and are best explained in terms of magnetically controlled accretion inside the white dwarf magnetosphere. We infer projected radial inflow velocities of ∼200–500 km s−1, significantly lower than both the rotational and the free-fall velocities for the corresponding range of radii. A combined net emission He ii plus Hβ low-velocity eclipse map reveals a twisted dipole emitting pattern near disk center. This is interpreted as being the projection of accretion curtains onto the orbital plane at two specific spin phases, as a consequence of the selection in velocity provided by the spectral eclipse mapping.
Characteristics of Chronic Lymphocytic Leukemia in Sudanese Patients

Objective: Our study aimed to characterize clinical, hematological and Immunophenotyping patterns in Sudanese patients with Chronic Lymphocytic Leukemia. Methods: A cross-sectional study was conducted in Khartoum state, Sudan, during the period from April 2017 to April 2018, involved 110 CLL patients. Physical examination, Complete Blood Count and Immunophenotyping were performed for all patients to confirm the diagnosis. Clinical staging such as Rai and Binet stages were applied. The statistical analysis was performed by using SPSS version 23.0. Results: In this study, 71.8% were males and 28.2% were females. Lymphadenopathy, splenomegaly, hepatomegaly, leukocytosis, thrombocytopenia, and anemia were seen in 71%, 49%, 13%, 60.9%, 39% and 34.5% of patients respectively. However, about 90% of patients displayed an advanced Rai risk stage and 70% were at Binet stage B or C. All CLL samples expressed CD45, CD19 and CD20. All the CLL cases were negative for the T-cell marker CD3.CD5 was expressed in 80% patients; CD23 was expressed in 92.7% patients. CD22, CD79b and FMC7 were negative in 91.8%, 77.3%, and 96.4% of patients respectively. Conclusions: CLL in Sudan is a disease of the elderly and more frequently in males than females. The incidence at young patients was higher than those reported by Western studies. Most of our patients presented advanced Rai and Binet stages. CD22 may be a highly specific marker for diagnosing CLL in Sudanese patients and should be included in all diagnostic panels used to differentiate CLL from other B cell lymphoproliferative disorders in Sudan.
Characterizing uniform star formation efficiencies with marginally stable galactic discs

We examine the HI-based star formation efficiency (SFE_HI), the ratio of star formation rate to the atomic Hydrogen (HI) mass, in the context of a constant stability star-forming disk model. Our observations of HI-selected galaxies show SFE to be fairly constant (log SFE_HI = -9.65 yr-1 with a dispersion of 0.3 dex) across ~5 orders of magnitude in stellar masses. We present a model to account for this result, whose main principle is that the gas within galaxies forms a uniform stability disk and that stars form within the molecular gas in this disk. We test two versions of the model differing in the prescription that determines the molecular gas fraction, based on either the hydrostatic pressure, or the stellar surface density of the disk. For high-mass galaxies such as the Milky Way, we find that either prescription predicts SFE_HI similar to the observations. However, the hydrostatic pressure prescription is a more accurate SFE_HI predictor for low-mass galaxies. Our model is the first model that links the uniform SFE_HI observed in galaxies at low redshifts to star-forming disks with constant marginal stability. While the rotational amplitude Vmax is the primary driver of disk structure in our model, we find the specific angular momentum of the galaxy may play a role in explaining a weak correlation between SFE_HI and effective surface brightness of the disk.
RADIO TIMING AND OPTICAL PHOTOMETRY OF THE BLACK WIDOW SYSTEM PSR J1518+0204C IN THE GLOBULAR CLUSTER M5

We report on the determination of astrometric, spin, and orbital parameters for PSR J1518+0204C, a “black widow” binary millisecond pulsar in the globular cluster (GC) M5. The accurate position and orbital parameters obtained from radio timing allowed us to search for the optical companion. By using WFC3/Hubble Space Telescope images, we identified a very faint variable star (mF390W ≳ 24.8, mF606W ≳ 24.3, mF814W ≳ 23.1) located at only 0. ″25 from the pulsar's timing position. Due to its strong variability, this star is visible only in a subsample of images. However, the light curve obtained folding the available data with the orbital parameters of the pulsar shows a maximum at the pulsar inferior conjunction and a possible minimum at the pulsar superior conjunction. Furthermore, the shape of the optical modulation indicates a heating process possibly due to the pulsar wind. This is the first identification of an optical companion to a black widow pulsar in the dense stellar environment of a GC.
ASTEROSEISMIC-BASED ESTIMATION OF THE SURFACE GRAVITY FOR THE LAMOST GIANT STARS

Asteroseismology is one of the most accurate approaches to estimate the surface gravity of a star. However, most of the data from the current spectroscopic surveys do not have asteroseismic measurements, which is very expensive and time consuming. In order to improve the spectroscopic surface gravity estimates for a large amount of survey data with the help of the small subset of the data with seismic measurements, we set up a support vector regression (SVR) model for the estimation of the surface gravity supervised by 1374 Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST) giant stars with Kepler seismic surface gravity. The new approach can reduce the uncertainty of the estimates down to about 0.1 dex, which is better than the LAMOST pipeline by at least a factor of 2, for the spectra with signal-to-noise ratio higher than 20. Compared with the log g estimated from the LAMOST pipeline, the revised log g values provide a significantly improved match to the expected distribution of red clump and red giant branch stars from stellar isochrones. Moreover, even the red bump stars, which extend to only about 0.1 dex in log g, can be discriminated from the new estimated surface gravity. The method is then applied to about 350,000 LAMOST metal-rich giant stars to provide improved surface gravity estimates. In general, the uncertainty of the distance estimate based on the SVR surface gravity can be reduced to about 12% for the LAMOST data.
STELLAR AND BLACK HOLE MASS DENSITIES AS EMPIRICAL TRACERS OF CO-EVOLUTION SHOW LOCK-STEP GROWTH SINCE Z ∼ 3

At redshifts beyond , measuring the black hole (BH) galaxy relations proves to be a difficult task. The bright light of the active galactic nuclei aggravates the deconvolution of BH and galaxy properties. However, high-redshift data on these relations are vital to understand the ways in which galaxies and BHs co-evolve and the ways in which they do not. In this work we use BH and stellar mass densities (BHMDs and SMDs) to constrain the possible co-evolution of BHs with their host galaxies since . The BHMDs are calculated from quasar luminosity functions using the Soltan argument, while we use integrals over stellar mass functions or the star-formation rate density to obtain values for the SMD. We find that both quantities grow in lock-step below redshifts of with a non-evolving BHMD to SMD ratio. A fit to the data assuming a power-law relation between the BHMD and the SMD yields exponents around unity (1.0–1.5). Up to the BHMD to SMD ratio does not show a strong evolution given the larger uncertainty in the completeness of high-redshift data sets. Our results, always applying the same analysis technique, seem to be consistent across all adopted data sets.
Health Literacy and Cyberchondria Levels in Healthcare Workers and Their Relationship with Body Awareness and Physical Activity

Aim: The level of health literacy and cyberchondria of healthcare providers can affect service beneficiaries, and the influence of health literacy and cyberchondria on physical activity and body awareness remains unclear. The aim of this study was to determine the health literacy and cyberchondria levels of healthcare workers and examine their relationship with physical activity level and body awareness. Methods: This cross-sectional study was conducted between August and November 2021 on 168 healthcare professionals working at the university hospital. The Turkish Health Literacy scale (TSOY-32), Cyberchondria scale, Body Awareness Questionnaire (BAQ), and International Physical Activity Questionnaire-Short Form (IPAQ-SF) were used for outcome measurements. Results: The TSOY-32 and Cyberchondria scale total scores were 37.76±7.98 and 63.83±19.45, respectively. There were low positive and significant correlations with TSOY-32, BAQ (r=0.213, p=0.006) and IPAQ-SF (r=0.162, p=0.036), while a low negative correlation was found between cyberchondria level and BAQ (r=-0.179, p=0.022) and IPAQ-SF (r=-0.193, p=0.013). Conclusion: This study shows that, unlike predicted, health professionals did not have perfect health literacy and were found to have moderate cyberchondria. Physical activity and body awareness may affect increasing health literacy and reducing cyberchondria, which will empower individuals to make beneficial health decisions.
SHARC-II 350 μm OBSERVATIONS OF THERMAL EMISSION FROM WARM DUST IN z ⩾ 5 QUASARS

We present observations of four z ⩾ 5 SDSS quasars at 350 μm with the SHARC-II bolometer camera on the Caltech Submillimeter Observatory. These are among the deepest observations that have been made by SHARC-II at 350 μm, and three quasars are detected at ⩾3σ significance, greatly increasing the sample of 350 μm (corresponds to rest frame wavelengths of <60 μm at z ⩾ 5), detected high-redshift quasars. The derived rest frame far-infrared (FIR) emission in the three detected sources is about five to ten times stronger than that expected from the average spectral energy distribution (SED) of the local quasars given the same 1450 Å luminosity. Combining the previous submillimeter and millimeter observations at longer wavelengths, the temperatures of the FIR-emitting warm dust from the three quasar detections are estimated to be in the range of 39–52 K. Additionally, the FIR-to-radio SEDs of the three 350 μm detections are consistent with the emission from typical star-forming galaxies. The FIR luminosities are ∼1013 L☉ and the dust masses are ⩾108 M☉. These results confirm that huge amounts of warm dust can exist in the host galaxies of optically bright quasars as early as z ∼ 6. The universe is so young at these epochs (∼1 Gyr) that a rapid dust-formation mechanism is required. We estimate the size of the FIR dust-emission region to be about a few kpc, and further provide a comparison of the SEDs among different kinds of dust-emitting sources to investigate the dominant dust-heating mechanism.
A Bayesian study of the primordial power spectrum from a novel closed universe model

We constrain the shape of the primordial power spectrum using recent measurements of the cosmic microwave background (CMB) from the Wilkinson Microwave Anisotropy Probe (WMAP) 7-year data and other high-resolution CMB experiments. We also include observations of the matter power spectrum from the luminous red galaxy (LRG) subset DR7 of the Sloan Digital Sky Survey (SDSS). We consider two dierent models of the primordial power spectrum. The rst is a standard nearly scale-invariant spectrum in the form of a generalised power-law parameterised in terms of the spectral amplitude As, the spectral index ns and (possibly) the running parameter nrun. The second spectrum has a more physically motivated form derived from the Lasenby and Doran (LD) model. This model is based on the restriction of the total conformal time available in a closed Universe and the predicted primordial power spectrum depends upon just two parameters. An important feature of the LD spectrum is that it naturally incorporates an exponential fall-o on large scales, which might provide a possible explanation for the lower-than-expected power observed at low multipoles in the CMB. In addition to parameter estimation, we compare both models using Bayesian model selection. We nd there is a signicant preference for the LD model over a simple power-law spectrum.
SEDeblend: a new method for deblending spectral energy distributions in confused imaging

For high-redshift submillimetre or millimetre sources detected with single-dish telescopes, interferometric follow-up has shown that many are multiple submillimetre galaxies blended together. Confusion-limited Herschel observations of such targets are also available, and these sample the peak of their spectral energy distribution (SED) in the far-infrared. Many methods for analysing these data have been adopted, but most follow the traditional approach of extracting fluxes before model SEDs are fit, which has the potential to erase important information on degeneracies among fitting parameters and glosses over the intricacies of confusion noise. Here, we adapt the forward-modelling method that we originally developed to disentangle a high-redshift strongly lensed galaxy group, in order to tackle this general problem in a more statistically rigorous way, by combining source deblending and SED fitting into the same procedure. We call this method ‘SEDeblend’. As an application, we derive constraints on far-infrared luminosities and dust temperatures for sources within the ALMA follow-up of the LABOCA Extended Chandra Deep Field South Submillimetre Survey. We find an average dust temperature for an 870-μm-selected sample of (33.9 ± 2.4) K for the full survey. When selection effects of the sample are considered, we find no evidence that the average dust temperature evolves with redshift for sources with redshifts greater than about 1.5, when compared to those with redshifts between 0.1 and 1.5.
The Effectiveness of Group Counseling Using SIBOL Techniques in the Academic Context

This study examines the effectiveness of group counseling using the self-instruction technique empirically based on observational learning (SIBOL) to foster a steady and great attitude in life as a student. The study used quantitative methods of “within-group or individual design” using equivalent time series, pre-test, post-test1, and post-test2 with a self-efficacy scale. The study included six students of Madiun with low selfefficacy in the academic context. Data analysis was done using the T-test calculations. It was found that group counseling through SIBOL techniques improved students’ selfefficacy, as evidenced by an increase in the students’ scores from pre-test to post-test2. Keywords: Group Counseling, SIBOL, Academic Contexts 1. Introduction
Modulation instability of structured-light beams in negative-index metamaterials

One of the most fundamental properties of isotropic negative-index metamaterials (NIMs), namely opposite directionality of the Poynting vector and the wavevector, enable many novel linear and nonlinear regimes of light–matter interactions. Here, we predict distinct characteristics of azimuthal modulation instability (MI) of optical vortices with different topological charges in NIMs with Kerr-type and saturable nonlinearity. We derive an analytical expression for the spatial modulation-instability gain for the Kerr-nonlinearity case and show that a specific condition relating the diffraction and the nonlinear lengths must be fulfilled for the azimuthal MI to occur. Finally, we investigate the rotation of the necklace beams due to the transfer of orbital angular momentum of the generating vortex on the movement of solitary necklace beams. We show that the direction of rotation is opposite in positive- and negative-index materials.
The prevalence of AGN feedback in massive galaxies at z ≈ 1

We use the optical–infrared imaging in the UKIDSS Ultra Deep Survey field, in combination with the new deep radio map of Arumugam et al., to calculate the distribution of radio luminosities among galaxies as a function of stellar mass in two redshift bins across the interval 0.4 <z ≤ 1.2. This is done with the use of a new Bayesian method to classify stars and galaxies in surveys with multiband photometry, and to derive photometric redshifts and stellar masses for those galaxies. We compare the distribution to that observed locally and find agreement if we consider only objects believed to be weak-lined radio-loud galaxies. Since the local distribution is believed to be the result of an energy balance between radiative cooling of the gaseous halo and mechanical active galactic nucleus (AGN) heating, we infer that this balance was also present as long ago as z ≈ 1. This supports the existence of a direct link between the presence of a low-luminosity (‘hot-mode’) radio-loud AGN and the absence of ongoing star formation.
Pairing of weakly correlated electrons in the platinum-based centrosymmetric superconductor SrPt3P

We report a study of the normal- and superconducting-state electronic properties of the centrosymmetric compound SrPt3 Pv ia 31 P nuclear-magnetic-resonance (NMR) and magnetometry investigations. Essential features such as a sharp drop of the Knight shift at T< T c and an exponential decrease of the NMR spin-lattice relaxation ratio 1/(T1T )b elowTc are consistent with an s-wave electron pairing in SrPt3P, although a direct confirmation in the form of a Hebel-Slichter-type peak is lacking. Normal-state NMR data at T< 50 K indicate conventional features of the conduction electrons, typical of simple metals such as lithium or silver. Our data are finally compared with available NMR results for the noncentrosymmetric superconductors LaPt3Si and CePt3Si, which adopt similar crystal structures.
Effect of pollen sources on fruit set and quality of edible fig (Ficus carica L.) cv. ‘Bursa Siyahı’

The caprification practice has been used widely in fig cultivation because it affects the yield and quality of fig fruits, a phenomenon known as the ‘xenia effect’. The present study was conducted to investigate the effects of pollen sources on fruit sets and fruit quality in the ‘Bursa Siyahı’ fig cultivar in 2017 and 2018. The eleven male genotypes and five cultivars were used as pollen source. The findings obtained in the present study showed that pollen sources significantly affected fruit set, early fruiting rate, fruit size, ostiole width, skin and flesh thickness, titratable acidity (TA), pH, and soluble solids content (SSC). The fruit set ratio varied from 32.02% (‘16 03 06’) to 76.66% (‘16 08 07’), and fruit weight varied from 77.29 g (‘16 03 06’) to 106.88 g (‘16 00 01’) based on pollen sources. The ostiole diameter ranged from 3.84 mm (‘16 ZF 08’) to 7.67 mm (‘77 00 01’). The skin thickness ranged from 3.01 mm (‘Havran’) to 5.35 mm (‘16 00 01’). The principal component analysis was performed to distinguish the pollen sources for the ‘Bursa Siyahı’ cultivar. The analysis proposed that the most important factors affecting the fig quality can be reduced to five components. Fruit weight (0.958), skin thickness (0.810), flesh l* value (0.821), pH (-0.872), and SSC (0.836) value could be regarded as the characteristic indicators for PC1, PC2, PC3, PC4, and PC5, respectively. The results showed that ‘16 09 10’, ‘16 05 03’, ‘16 08 07’, and ‘16 08 12’ pollen sources are adequate pollinators for the edible ‘Bursa Siyahı’ ﬁg.
Decision Conflicts in Clinical Care during COVID-19: A Multi-Perspective Inquiry

Background: The early COVID-19-pandemic was characterized by changes in decision making, decision-relevant value systems and the related perception of decisional uncertainties and conflicts resulting in decisional burden and stress. The vulnerability of clinical care professionals to these decisional dilemmas has not been characterized yet. Methods: A cross-sectional questionnaire study (540 patients, 322 physicians and 369 nurses in 11 institutions throughout Germany) was carried out. The inclusion criterion was active involvement in clinical treatment or decision making in oncology or psychiatry during the first year of COVID-19. The questionnaires covered five decision dimensions (conflicts and uncertainty, resources, risk perception, perception of consequences for clinical processes, and the perception of consequences for patients). Data analysis was performed using ANOVA, Pearson rank correlations, and the Chi²-test, and for inferential analysis, nominal logistic regression and tree classification were conducted. Results: Professionals reported changes in clinical management (27.5%) and a higher workload (29.2%), resulting in decisional uncertainty (19.2%) and decisional conflicts (22.7%), with significant differences between professional groups (p < 0.005), including anxiety, depression, loneliness and stress in professional subgroups (p < 0.001). Nominal regression analysis targeting “Decisional Uncertainty” provided a highly significant prediction model (LQ p < 0.001) containing eight variables, and the analysis for “Decisional Conflicts” included six items. The classification rates were 64.4% and 92.7%, respectively. Tree analysis confirmed three levels of determinants. Conclusions: Decisional uncertainty and conflicts during the COVID-19 pandemic were independent of the actual pandemic load. Vulnerable professional groups for the perception of a high number of decisional dilemmas were characterized by individual perception and the psychological framework. Coping and management strategies should target vulnerability, enable the handling of the individual perception of decisional dilemmas and ensure information availability and specific support for younger professionals.