Miracle-dz/UniFAR-FTUs huggingface dataset:
Pulsational instability in B-type supergiant stars

We present results of the instability analysis of the post-main sequence massive star models against radial and nonradial pulsations. We confirm that both p- and g-modes can be excited by the -mechanism acting in the metal opacity bump. However, as opposed to the previous claims, we find that an intermediate convective zone (ICZ) related to the hydrogen burning shell is not necessary for excitation of g-modes. These modes can be reflected at a minimum of the Brunt-V¨¨¨ frequency, located at the top of the chemical composition gradient region surrounding the radiative helium core. This minimum is associated with the change of actual temperature gradient from the adiabatic value in the semiconvective zone to the radiative value above it. Thus, the existence of pulsations at this evolutionary stage does not prove the existence of the convective zone but only some reflective layer. Finally, we show that no regular patterns can be expected in oscillation spectra of blue supergiant pulsators but there is a prospect for identification of the mode degree, ‘, from multicolour photometry.
Silent Pauses and Speech Indices as Biomarkers for Primary Progressive Aphasia

Background and Objectives: Recent studies highlight the importance of investigating biomarkers for diagnosing and classifying patients with primary progressive aphasia (PPA). Even though there is ongoing research on pathophysiological indices in this field, the use of behavioral variables, and especially speech-derived factors, has drawn little attention in the relevant literature. The present study aims to investigate the possible utility of speech-derived indices, particularly silent pauses, as biomarkers for primary progressive aphasia (PPA). Materials and Methods: We recruited 22 PPA patients and 17 healthy controls, from whom we obtained speech samples based on two elicitation tasks, i.e., cookie theft picture description (CTP) and the patients’ personal narration of the disease onset and course. Results: Four main indices were derived from these speech samples: speech rate, articulation rate, pause frequency, and pause duration. In order to investigate whether these indices could be used to discriminate between the four groups of participants (healthy individuals and the three patient subgroups corresponding to the three variants of PPA), we conducted three sets of analyses: a series of ANOVAs, two principal component analyses (PCAs), and two hierarchical cluster analyses (HCAs). The ANOVAs revealed significant differences between the four subgroups for all four variables, with the CTP results being more robust. The subsequent PCAs and HCAs were in accordance with the initial statistical comparisons, revealing that the speech-derived indices for CTP provided a clearer classification and were especially useful for distinguishing the non-fluent variant from healthy participants as well as from the two other PPA taxonomic categories. Conclusions: In sum, we argue that speech-derived indices, and especially silent pauses, could be used as complementary biomarkers to efficiently discriminate between PPA and healthy speakers, as well as between the three variants of the disease.
Retinitis Pigmentosa in the Puerto Rican Population: A Geographic Distribution

Background Previous studies have reported on retinitis pigmentosa (RP) in Puerto Rico. Information on the geographic distribution of RP mutations in Puerto Rico may lead to higher rates of diagnosis and co-management. We aimed to evaluate whether there are areas with increased incidence of genes leading to RP in the Island. Materials and Methods We conducted a non-concurrent prospective study on the genotype of 241 patients with RP in Puerto Rico. We evaluated their townships to determine whether there are clusters of genes leading to RP. Genetic studies were done using the Invitae inherited retinal diseases panel analyzing 330 genes. Results A total of 100 patients were evaluated. Clusters of patients with mutations were found in certain townships. As depicted in the map, a cluster of patients with a mutation in the PDE6B gene was found in San Juan (9), those with the BBS1 gene occurred in San Juan (6) and Bayamón (4), mutations on the USH2A gene were found in Toa Baja (5), mutations in the CRB1 gene appeared in Ciales (4), and mutations in the BBS7 were found in Aibonito (2). Other mutations are scattered throughout the Island. Conclusion Clusters of mutations were identified in several townships including San Juan, Bayamón, Toa Baja, Ciales, and Aibonito. Some of these are isolated geographically. Additional mutations were identified but only the most pertinent were reported. Genetic studies are warranted in all patients with RP in Puerto Rico.
AN APPARENT PRECESSING HELICAL OUTFLOW FROM A MASSIVE EVOLVED STAR: EVIDENCE FOR BINARY INTERACTION

Massive, evolved stars play a crucial role in the metal enrichment, dust budget, and energetics of the interstellar medium; however, the details of their evolution are uncertain because of their rarity and short lifetimes before exploding as supernovae. Discrepancies between theoretical predictions from single-star evolutionary models and observations of massive stars have evoked a shifting paradigm that implicates the importance of binary interaction. We present mid- to far-infrared observations from the Stratospheric Observatory for Infrared Astronomy of a conical “helix” of warm dust (∼180 K) that appears to extend from the Wolf–Rayet star WR102c. Our interpretation of the helix is a precessing, collimated outflow that emerged from WR102c during a previous evolutionary phase as a rapidly rotating luminous blue variable. We attribute the precession of WR102c to gravitational interactions with an unseen compact binary companion whose orbital period can be constrained to 800 days < P < 1400 days from the inferred precession period, τp ∼ 1.4 × 104 yr, and limits imposed on the stellar and orbital parameters of the system. Our results concur with the range of orbital periods (P ≲ 1500 days) where spin-up via mass exchange is expected to occur for massive binary systems.
MINUTE-SCALE RAPID VARIABILITY OF THE OPTICAL POLARIZATION IN THE NARROW-LINE SEYFERT 1 GALAXY PMN J0948+0022

We report on optical photopolarimetric results of the radio-loud narrow-line Seyfert 1 (RL-NLSy1) galaxy PMN J0948+0022 on 2012 December to 2013 February triggered by flux enhancements in the near infrared and γ-ray bands. With the one-shot polarimetry of the Hiroshima One-shot Wide field Polarimeter installed on the Kanata Telescope, we detected very rapid variability in the polarized-flux (PF) light curve on MJD 56281 (2012 December 20). The rise and decay times were about 140 s and 180 s, respectively. The polarization degree (PD) reached 36% ± 3% at the peak of the short-duration pulse, while the polarization angle remained almost constant. In addition, temporal profiles of the total flux and PD showed highly variable but well correlated behavior and discrete correlation function analysis revealed that no significant time lag of more than 10 minutes was present. The high PD and minute-scale variability in PF provides clear evidence of synchrotron radiation from a very compact emission region of ∼1014 cm size with a highly ordered magnetic field. Such micro-variability of polarization is also observed in several blazar jets, but its complex relation between total flux and PD are explained by a multi-zone model in several blazars. The implied single emission region in PMN J0948+0022 might reflect a difference of jets between RL-NLSy1s and blazars.
The Type Ib SN 1999dn: one year of photometric and spectroscopic monitoring

Extensive optical and near-infrared observations of the Type Ib supernova (SNIb) 1999dn are presented, covering the first year after explosion. These new data turn this object, already considered a prototypical SNIb, into one of the best observed objects of its class. The light curve of SN 1999dn is mostly similar in shape to that of other SNeIb but with a moderately faint peak (M v = —17.2mag). From the bolometric light curve and ejecta expansion velocities, we estimate that about 0.11 M ⊙ of 56 Ni were produced during the explosion and that the total ejecta mass was 4―6 M ⊙ with a kinetic energy of at least 5 x 10 51 erg. The spectra of SN 1999dn at various epochs are similar to those of other stripped envelope SNe showing clear presence of H at early epochs. The high explosion energy and ejected mass, along with the small flux ratio [Ca II]/[I I] measured in the nebular spectrum, together with the lack of signatures of dust formation and the moderate metallicity environment is not inconsistent with a single massive progenitor (M ZAMS ≥ 23-25 M ⊙ ) for SN 1999dn.
Anomalous Longitudinal Shower Profiles and Hadronic Interactions

The bulk of air showers initiated by very high energy cosmic rays exhibits a longitudinal development in depth with a single well-defined shower maximum. However, a small fraction of showers has a profile that differs considerably from this average behaviour. In extreme cases, such anomalous longitudinal profiles can even have two distinct shower maxima. We discuss the properties of the primary interactions that lead to such profiles. Simulations are used to estimate the rate of anomalous profiles in dependence of primary energy, mass, and characteristic features of hadronic multiparticle production at very high energies.
Detection prospects of singlet fermionic dark matter

A singlet fermion which interacts only with a new singlet scalar provides a viable and minimal scenario that can explain the dark matter. The singlet fermion is the dark matter particle whereas the new scalar mixes with the Higgs boson providing a link between the dark matter sector and the standard model. In this paper, we present an updated analysis of this model focused on its detection prospects. Both the parity-conserving case and the most general case are considered. First, the full parameter space of the model is analyzed, and the regions compatible with the dark matter constraint are obtained and characterized. Then, the implications of current and future direct detection experiments are taken into account. Specifically, we determine the regions of the multidimensional parameter space that are currently excluded and those that are going to be probed by next generation experiments. Finally, indirect detection prospects are discussed and the expected signal at neutrino telescopes is calculated.
Measurement of the B0 production cross section in pp Collisions at sqrt(s) = 7 TeV

Measurements of the differential production cross sections dσ/dpT and dσ/dy B for B0 mesons produced in pp collisions at √ s = 7 TeV are presented. The dataset used was collected by the CMS experiment at the LHC and corresponds to an integrated luminosity of 40 pb−1. The production cross section is measured from B0 meson decays reconstructed in the exclusive final state J/ψ KS, with the subsequent decays J/ψ → μ+μ− and KS → π+π−. The total cross section for pT > 5 GeV and ∣∣yB∣∣ < 2.2 is measured to be 33.2± 2.5± 3.5 μb, where the first uncertainty is statistical and the second is systematic. Submitted to Physical Review Letters ∗See Appendix 1 for the list of collaboration members ar X iv :1 10 4. 28 92 v2 [ he pex ] 3 0 Ju n 20 11
Simulated gamma-ray pulse profile of the Crab pulsar with the Cherenkov Telescope Array

We present simulations of the very high energy (VHE) gamma-ray light curve of the Crab pulsar as observed by the Cherenkov Telescope Array (CTA). The CTA pulse profile of the Crab pulsar is simulated with the specific goal of determining the accuracy of the position of the interpulse. We fit the pulse shape obtained by the MAGIC telescope with a three-Gaussian template and rescale it to account for the different CTA instrumental and observational configurations. Simulations are performed for different configurations of CTA and for the ASTRI mini-array. The northern CTA configuration will provide an improvement of a factor of ~3 in accuracy with an observing time comparable to that of MAGIC (73 hours). Unless the VHE spectrum above 1 TeV behaves differently from what we presently know, unreasonably long observing times are required for a significant detection of the pulsations of the Crab pulsar with the high-energy-range sub-arrays. We also found that an independent VHE timing analysis is feasible with Large Size Telescopes (LSTs). CTA will provide a significant improvement in determining the VHE pulse shape parameters necessary to constrain theoretical models of the gamma-ray emission of the Crab pulsar. One of such parameters is the shift in phase between peaks in the pulse profile at VHE and in other energy bands that, if detected, may point to different locations of the emission regions.
New Keratoconus Risk Factors: A Cross-Sectional Case—Control Study

Purpose To evaluate risk factors associated with keratoconus in a monocentric cross-sectional case-control study. Methods This observational study occurred from June 2019 to February 2021 in a university hospital (France). The case group consisted of 195 patients with keratoconus in at least one eye who were followed up by a corneal specialist. The control group consisted of 195 patients without any evidence of keratoconus on slit-lamp examination and corneal topography, who were matched 1 : 1 to controls by age and sex. Data were collected by a self-completed paper questionnaire before the consultation, and a multivariate logistic regression was performed. Results Multivariate analysis revealed significant associations of keratoconus with family history (odds ratio [OR] = 22.2, p < 0.001), rubbing eyes (OR = 10.9, p < 0.001), allergy (any kind) (OR = 3.80, p < 0.001), smoking exposure (OR = 2.08, p=0.017), and dry eyes (OR = 1.77, p=0.045f). The worst eye was associated with the more rubbed eye (p < 0.001) and the more pressed eye during the night according to sleeping position (p < 0.041). Conclusion This study confirmed the association between keratoconus and eye rubbing, family history, and allergy. It highlighted the role of pressure on the eyes during sleep. Other less known risk factors such as dry eyes and smoking exposure should be explored in future studies.
A stellar population synthesis approach to the Oosterhoff dichotomy

We use color-magnitude diagram synthesis together with theoretical relations from non-linear pulsation models to approach the long-standing problem of the Oosterhoff dichotomy related to the distribution of the mean periods of fundamental RR Lyrae variables in globular clusters. By adopting the chemical composition determined from spectroscopic observations and a criterion to account for the hysteresis mechanism, we tuned age and mass-loss to simultaneously reproduce the morphology of both the turn-off and the Horizontal Branch of a sample of 17 globular clusters of the Milky Way and of nearby dwarf galaxies in the crucial metallicity range (-1.9<[Fe/H]<-1.4) where the Oostheroff transition is apparent. We find that the Oosterhoff dichotomy among Galactic globular clusters is naturally reproduced by models. The analysis of the relative impact of the various involved parameters indicates that the main responsibles of the dichotomy are the peculiar distribution of clusters in the age-metallicity plane and the hysteresis. In particular, there is a clear connection between the two main branches of the age-metallicity relation for Galactic globular clusters and the Oosterhoff groups. The properties of clusters' RR Lyrae belonging to other Oostheroff groups (OoInt and OoIII) are instead not well reproduced. While for OoIII clusters a larger helium abundance for a fraction of the cluster's stars can reconcile the model prediction with observations, some other parameter affecting both the Horizontal Branch morphology and the RR Lyrae periods is required to reproduce the behavior of OoInt clusters.
How to distinguish dark energy and modified gravity

The current accelerated expansion of our universe could be due to an unknown energy component (dark energy) or a modification of general relativity (modified gravity). In the literature it has been proposed that combining the probes of the cosmic expansion history and growth history can distinguish between dark energy and modified gravity. In this work, without invoking nontrivial dark energy clustering, we show that the possible interaction between dark energy and dark matter could make the interacting dark model and the modified gravity model indistinguishable. An explicit example is also given. Therefore, it is required to seek some complementary probes beyond the ones of cosmic expansion history and growth history.
Imaging investigation after urinary tract infection in childhood: narrative review of current recommendations

Background and Objective: Urinary tract infections (UTIs) are one of the most common bacterial infections in children. The imaging exams that take place after the occurrence of UTI have the main goal of detecting congenital anomalies of the kidney and urinary tract (CAKUT). The value of imaging investigation relies on guiding the management of the patient and directing measures to prevent recurrent infections and to avoid possible kidney scars. Currently, there has been a general trend to restrict the number of imaging tests performed in clinical practice as can be seen in the most important guidelines regarding the management of patients with febrile UTI. The guidelines from the American Association of Pediatrics (AAP), the National Institute for Health and Care Excellence (NICE), and the European Association of Urology (EAU)/European Society for All Pediatric Urology (ESPU) made recommendations in this regard. We believe that the critical discussion about the advantages and disadvantages of the different guidelines and protocols proposed is important for pediatricians and nephrologists and helps to define the best approach for patients. In this matter, this review aimed to provide a critical view of imaging investigation methods and guidelines after UTIs in pediatric patients. Methods: The authors performed a non-systematic search in PubMed, Cochrane, Scopus, SciELO and in renowned books from the subjects of pediatric nephrology and pediatric urology published up to August 5th, 2021, and critically selected and independently reviewed articles written mainly in English or Portuguese to produce this narrative review. Key Content and Findings: In this narrative review, shortcomings of different imaging guidelines and examinations after urinary tract infections in children are explored, while the principles and advantages of distinct imaging methods are highlighted. We find that, while an initial renal and bladder ultrasonography is of great value, more invasive exams need to be carefully selected to identify patients at risk for further complications whilst minimizing distress and other consequences to the child. Conclusions: A renal ultrasonography with good quality of images and examined by an expert is generally recommended as initial screening after UTI. Additional imaging exams depend on findings provided by renal ultrasonography. but the exam is of low
Development and validation of organizational parochialism scale

Purpose- The aim of this study is to examine the concept of organizational parochialism, which is one of the factors that determine the present and future of organizations, and to apply validity and reliability tests by developing a scale that is thought to measure this concept. Methodology- Our research was applied to 272 companies operating in the textile sector and the results were analysed in the SPSS.25 program. As a result of detailed statistical analyses, the validity and reliability tests of the developed scale were completed and it was determined that the scale statistically measures the concept of organizational parochialism. Findings- According to the results of the research, it has been seen that the concept of organizational parochialism is divided into 5 different sub-dimensions with 25 items as namely business management, financial management, competitiveness, employment management and production management. Conclusion- In today's intensely competitive environment, businesses focus on the present and they may miss the possible risks of the future. In addition to the possible risks, it is also possible for the organizations to make predictions about the future, to catch potential opportunities in a timely manner and to benefit the organization from them. It is possible to say that businesses that cannot evaluate such risks and opportunities are narrow-minded, especially in terms of management manner. In this study, a scale measuring the concept of organizational parochialism and its sub-dimensions, which was determined that have not been researched before in social sciences as a result of the literature review, was developed. In our research, it is possible to indicate that the concept has been confirmed by both the data obtained from the organizational behaviour literature and the statistical data on its measurement. Keywords: Organizational parochialism, narrow-mindedness, administrative shallowness, parochialism scale, projection determination. JEL Codes: M16, M11, M12
Matter power spectra in dynamical dark energy cosmologies

We used a suite of numerical cosmological simulations in order to investigate the effect of gas cooling and star formation on the large scale matter distribution. The simulations follow the formation of cosmic structures in five different Dark Ene rgy models: the fiducialCDM cosmology and four models where the Dark Energy density is allowed to have a non-trivial redshift evolution. Each simulation includes a variety of g as physics, ranging from radiative cooling to heating and supernovae feedback. Moreover, for each cosmology we have a control run with dark matter only, in order to allow a direct assessment of the effect of baryonic processes. We found that the power spectra of gas and stars, as well as the total matter power spectrum, are in qualitative agreement with the results of p revious works in the framework of the fiducial model, although several quantitative differ ences exist. We used the physically motivated halo model in order to investigate the backreaction of gas and stars on the dark matter distribution, finding that it is very well reproduced by simply increasing the average dark matter halo concentration by 17%, irrespective of the mass. This is in agreement with gas cooling dragging dark matter in the very center of halos, as well as adiabatic contraction steepening the relative potential wells. Moving to model universes dominated by dynamical Dark Energy, it turns out that they introduce a specific signa ture on the power spectra of the various matter components, that is qualitatively indep endent of the exact cosmology considered. This generic shape is well captured by the halo model if we blindly consider the cosmology dependences of the halo mass function, bias, and concentration. However, the details of the dark matter power spectrum can be precisely captured only at the cost of a few slight modifications to the ingredients entering in the halo model. The backreaction of baryons onto the dark matter distribution works pretty much in the same way as in the referenceCDM model, in the sense that it is very well described by an increment in the average halo concentration. Nonetheless, this increment is less pronounced than in the fiducial model (only ∼ 10%), in agreement with a series of other clues pointing toward the fact that star formation is less efficient when Dark Energy di splays a dynamical evolution.
Improved fractal geometry based texture segmentation technique

The problem of natural texture segmentation is considered. The technique is based on four texture features derived using the fractal geometry of images. These four features are fractal dimension (FD) of the original image, FD of above average (high) gray level image, FD of below (low) gray level image, and multifractal of order two. A modified box-counting approach is proposed to estimate the FD and computed features all are normalised in the same range