Miracle-dz/UniFAR-FTUs huggingface dataset:
Population Genetics of the European Roma—A Review

The Roma are a group of populations with a common origin that share the Romani identity and cultural heritage. Their genetic history has been inferred through multiple studies based on uniparental and autosomal markers, and current genomic data have provided novel insights into their genetic background. This review was prompted by two factors: (i) new developments to estimate the genetic structure of the Roma at a fine-scale resolution have precisely identified the ancestral components and traced migrations that were previously documented only in historical sources, clarifying and solving debates on the origins and the diaspora of the Roma; (ii) while there has been an effort to review the health determinants of the Roma, the increasing literature on their population genetics has not been subjected to a dedicated review in the last two decades. We believe that a summary on the state of the art will benefit both the public and scholars that are approaching the subject.
ON THE STAR FORMATION PROPERTIES OF VOID GALAXIES

We measure the star formation properties of two large samples of galaxies from the SDSS in large-scale cosmic voids on timescales of 10 and 100 Myr, using Hα emission line strengths and GALEX FUV fluxes, respectively. The first sample consists of 109,818 optically selected galaxies. We find that void galaxies in this sample have higher specific star formation rates (SSFRs; star formation rates per unit stellar mass) than similar stellar mass galaxies in denser regions. The second sample is a subset of the optically selected sample containing 8070 galaxies with reliable H i detections from ALFALFA. For the full H i detected sample, SSFRs do not vary systematically with large-scale environment. However, investigating only the H i detected dwarf galaxies reveals a trend toward higher SSFRs in voids. Furthermore, we estimate the star formation rate per unit H i mass (known as the star formation efficiency; SFE) of a galaxy, as a function of environment. For the overall H i detected population, we notice no environmental dependence. Limiting the sample to dwarf galaxies still does not reveal a statistically significant difference between SFEs in voids versus walls. These results suggest that void environments, on average, provide a nurturing environment for dwarf galaxy evolution allowing for higher specific star formation rates while forming stars with similar efficiencies to those in walls.
Breast Implanted-Associated Anaplastic Large Cell Lymphoma: A Case of Advanced Disease with Flow Cytometric Findings

Breast implant-associated anaplastic large cell lymphoma (breast implant-associated ALCL) is a recently described, distinct clinicopathological entity associated with macrotextured breast implants. The diagnostic workup of a patient suspected to have breast implant-associated ALCL includes cytological assessment of effusions and tissue biopsies of any masses or enlarged lymph nodes, with morphologic and immunophenotypic evaluation and possible flow cytometric and molecular testing. We report the case of a woman found to have breast implant-associated ALCL on fine needle aspirate and core biopsy, who on surgical resection, had extensive local disease with involvement of the resection margins and lymph nodes, requiring systemic treatment. We focus on the flow cytometric findings that identified a population of large cells on the CD30/side scatter dot plot and whose immunophenotype was consistent with breast implant-associated ALCL, highlighting the value of flow cytometry as an adjunct to morphological and immunophenotypic evaluation.
MRI Detection of Carotid Intraplaque Hemorrhage and Postintervention Cognition

BACKGROUND AND PURPOSE: Cognitive improvement has been reported after carotid revascularization and attributed to treating stenosis and correcting hypoperfusion. This study investigated the effect of carotid intraplaque hemorrhage on postintervention cognition. MATERIALS AND METHODS: In this institutional review board–approved single-center study, consecutive patients scheduled for carotid surgery were recruited for preoperative carotid MR imaging (MPRAGE) and pre- and postintervention cognitive testing using the Repeatable Battery for the Assessment of Neuropsychological Status. Pre- and postintervention scores were compared using t tests and multivariable linear regression. RESULTS: Twenty-three participants were included, with endarterectomy performed in 20 (87%) and angioplasty/stent placement, in 3 (13%). Overall, statistically significant improvements occurred in the pre- versus postintervention mean Total Scale score (92.1 [SD, 15.5] versus 96.1 [SD, 15.8], P = .04), immediate memory index (89.4 [SD, 18.2] versus 97.7 [SD, 14.9], P < .001), and verbal index (96.1 [SD, 14.1] versus 103.0 [SD, 12.0], P = .002). Intraplaque hemorrhage (+) participants (n = 11) had no significant improvement in any category, and the attention index significantly decreased (99.4 [SD, 18.0] versus 93.5 [SD, 19.4], P = .045). Intraplaque hemorrhage (−) participants (n = 12) significantly improved in the Total Scale score (86.4 [SD, 11.8] versus 95.5 [SD, 12.4], P = .004), immediate memory index (82.3 [SD, 14.6] versus 96.2 [SD, 14.1], P = .002), delayed memory index (94.3 [SD, 14.9] versus 102.4 [SD, 8.0], P = .03), and verbal index (94.3 [SD, 13.2] versus 101.5 [SD, 107.4], P = .009). Postintervention minus preintervention scores for intraplaque hemorrhage (+) versus (−) groups showed statistically significant differences in the Total Scale score (−0.4 [SD, 6.8] versus 8.0 [SD, 8.5], P = .02), attention index (−5.9 [SD, 8.5] versus 4.3 [SD, 11.9], P = .03), and immediate memory index (4.2 [SD, 6.7] versus 12.2 [SD, 10.2], P = .04). CONCLUSIONS: Cognitive improvement was observed after carotid intervention, and this was attributable to intraplaque hemorrhage (−) plaque. MR imaging detection of intraplaque hemorrhage status may be an important determinant of cognitive change after intervention.
Alpha-Lipoic Acid Supplementation Restores Early Age-Related Sensory and Endothelial Dysfunction in the Skin

Many changes characterize skin aging, and the resulting dysfunctions still constitute a real challenge for our society. The aim of this study was to compare the skin aging of two rat strains, Wistar and Brown Norway (BN), considered as “poorly aging” and “healthy aging” models, respectively, and to assess the effect of alpha-lipoic acid (LPA), especially on skin microcirculation. To this purpose, various skin characteristics were studied at 6, 12, and 24 months and compared to the results of LPA treatment performed at 12 or 24 months. Skin aging occurred in both strains, but we showed an early occurrence of different age-related disorders in the Wistar strain compared to BN strain, especially regarding weight gain, glycemia dysregulation, basal skin perfusion, endothelial function, and skin resistance to low pressure. LPA treatment tended to improve skin resistance to low pressure in BN but not in Wistar despite the improvement of basal skin perfusion, endothelial function, and skin sensory sensitivity. Overall, this study confirmed the healthier aging of BN compared to Wistar strain and the positive effect of LPA on both general state and skin microcirculation.
SUZAKU OBSERVATIONS OF MODERATELY OBSCURED (COMPTON-THIN) ACTIVE GALACTIC NUCLEI SELECTED BY SWIFT/BAT HARD X-RAY SURVEY

We report the results obtained by a systematic, broadband (0.5–150 keV) X-ray spectral analysis of moderately obscured (Compton-thin, 22 ≤ log N H < 24 ) active galactic nuclei (AGNs) observed with Suzaku and Swift/Burst Alert Telescope (BAT). Our sample consists of 45 local AGNs at z < 0.1 with log L 14 − 195 keV > 42 detected in the Swift/BAT 70-month survey, whose Suzaku archival data are available as of 2015 December. All spectra are uniformly fit with a baseline model composed of an absorbed cutoff power-law component, reflected emission accompanied by a narrow fluorescent iron-Kα line from cold matter (torus), and scattered emission. The main results based on the above analysis are as follows. (1) The photon index is correlated with Eddington ratio, but not with luminosity or black hole mass. (2) The ratio of the luminosity of the iron-Kα line to the X-ray luminosity an indicator of the covering fraction of the torus, shows significant anticorrelation with luminosity. (3) The averaged reflection strength derived from stacked spectra above 14 keV is larger in less luminous ( log L 10 − 50 keV ≤ 43.3 , R = 1.04 − 0.19 + 0.17 ) or highly obscured ( log N H > 23 , R = 1.03 − 0.17 + 0.15 ) AGNs than in more luminous ( log L 10 − 50 keV > 43.3 , R = 0.46 − 0.09 + 0.08 ) or lightly obscured ( log N H ≤ 23 , R = 0.59 − 0.10 + 0.09 ) objects. (4) The ratio of the luminosity of the [ O IV ] 25.89 μm line to the X-ray luminosity is significantly smaller in AGNs with lower soft X-ray scattering fractions, suggesting that the former luminosity underestimates the intrinsic power of an AGN buried in a torus of small opening angle.
2001 QR322: a dynamically unstable Neptune Trojan?

Since early work on the stability of the first Neptunian Trojan, 2001 QR322, suggested that it was a dynamically stable, primordial body, it has been assumed that this applies to both that object and its more recently discovered brethren. However, it seems that things are no longer so clear-cut. In this work, we present the results of detailed dynamical simulations of the orbital behaviour of 2001 QR322. Using an ephemeris for the object that has significantly improved since earlier works, we follow the evolution of 19 683 test particles, placed on orbits within the observational error ellipse of 2001 QR322's orbit, for a period of 1 Gyr. We find that majority of these 'clones' of 2001 QR322 are dynamically unstable, exhibiting a near-exponential decay from both the Neptunian Trojan cloud (decay half-life of ∼550 Myr) and the Solar system (decay half-life of ∼590 Myr). The stability of the object within Neptune's Trojan cloud is found to be strongly dependent on the initial semimajor axis used, with these objects located at a≥ 30.30 au being significantly less stable than those interior to this value, as a result of their having initial libration amplitudes very close to a critical threshold dividing regular and irregular motion, located at ∼70°–75° (full extent of angular motion). This result suggests that if 2001 QR322 is a primordial Neptunian Trojan, it must be a representative of a population that was once significantly larger than that we see today and adds weight to the idea that the Neptune Trojans may represent a significant source of objects moving on unstable orbits between the giant planets (the Centaurs).
Geodesic motion around a distorted static black hole

In this paper we study geodesic motion around a distorted Schwarzschild black hole. We consider both timelike and null geodesics which are confined to the black hole's equatorial plane. Such geodesics generically exist if the distortion field has only even interior multipole moments and so the field is symmetric with respect to the equatorial plane. We specialize to the case of distortions defined by a quadrupole Weyl moment. An analysis of the effective potential for equatorial timelike geodesics shows that finite stable orbits outside the black hole are possible only for $q\in(q_{\text{min}}, q_{\text{max}}]$, where $q_{\text{min}}\approx-0.0210$ and $q_{\text{max}}\approx2.7086\times10^{-4}$, while for null equatorial geodesics a finite stable orbit outside the black hole is possible only for $q\in[q_{\text{min}},0)$. Moreover, the innermost stable circular orbits (ISCOs) are closer to the distorted black hole horizon than those of an undistorted Schwarzschild black hole for $q\in(q_{\text{min}},0)$ and a null ISCO exists for $q=q_{\text{min}}$. These results shows that an external distortion of a negative and sufficiently small quadrupole moment tends to stabilize motion of massive particles and light.
Constraining Solar Position and Velocity with a nearby Hypervelocity Star

Gravitational three-body interaction among binary stars and the supermassive black hole at the center of the Milky Way occasionally ejects a hypervelocity star (HVS) with a velocity of ∼ 1000 km s − 1 . Due to the ejection location, such an HVS initially has negligible azimuthal angular momentum L z ≃ 0 kpc km s − 1 . Even if the halo is mildly triaxial, Lz of a recently ejected nearby HVS remains negligible, since its flight time from the Galactic center is too short to accumulate noticeable torque. However, if we make a wrong assumption about the solar position and velocity, such an HVS would apparently have noticeable nonzero azimuthal angular momentum, due to the wrong reflex motion of the Sun. Conversely, with precise astrometric data for a nearby HVS, we can measure the solar position and velocity by assuming that the HVS has zero azimuthal angular momentum. Based on this idea, here we propose a method to estimate the Galactocentric distance of the Sun R0 and the Galactocentric solar azimuthal velocity V⊙ by using an HVS. We demonstrate with mock data for a nearby HVS candidate that the Gaia astrometric data, along with the currently available constraint on V⊙/R0 from the proper motion measurement of Sgr A*, can constrain R0 and V⊙ with uncertainties of ∼0.27 kpc and ∼7.8 km s−1 (or fractional uncertainties of 3%), respectively. Our method will be a promising tool to constrain (R0, V⊙), given that Gaia is expected to discover many nearby HVSs in the near future.
A NEW STATISTIC FOR ANALYZING BARYON ACOUSTIC OSCILLATIONS

We introduce a new statistic ωℓ(rs) for measuring and analyzing large-scale structure and particularly the baryon acoustic oscillations. ωℓ(rs) is a band-filtered, configuration space statistic that is easily implemented and has advantages over the traditional power spectrum and correlation function estimators. Unlike these estimators, ωℓ(rs) can localize most of the acoustic information into a single dip at the acoustic scale while avoiding sensitivity to the poorly constrained large-scale power (i.e., the integral constraint) through the use of a localized and compensated filter. It is also sensitive to anisotropic clustering through pair counting and does not require any binning of data. We measure the shift in the acoustic peak due to nonlinear effects using the monopole ω0(rs) derived from subsampled dark matter (DM) catalogs as well as from mock galaxy catalogs created via halo occupation distribution modeling. All of these are drawn from 44 realizations of 10243 particle DM simulations in a 1 h−1 Gpc box at z = 1. We compare these shifts with those obtained from the power spectrum and conclude that the results agree. We therefore expect that distance measurements obtained from ω0(rs) and P(k) will be consistent with each other. We also show that it is possible to extract the same amount of acoustic information by fitting over a finite range using either ω0(rs) or P(k) derived from equal volume surveys.
A Central Excess of Stripped-Envelope Supernovae within Disturbed Galaxies

This paper presents an analysis of core-collapse supernova distributions in isolated and interacting host galaxies, paying close attention to the selection effects involved in conducting host galaxy supernova studies. When taking into account all of the selection effects within our host galaxy sample, we draw the following conclusions. Within interacting, or ‘disturbed', systems there is a real, and statistically significant, increase in the fraction of stripped-envelope supernovae in the central regions. A discussion into what may cause this increased fraction, compared to the more common Type IIP supernovae and Type II supernovae without subclassifications, is presented. Selection effects are shown not to drive this result, and so we propose that this study provides direct evidence for a high-mass weighted initial mass function within the central regions of disturbed galaxies. Within ‘undisturbed' spiral galaxies the radial distribution of Type Ib and Type Ic supernovae is statistically very different, with the latter showing a more centrally concentrated distribution. This could be driven by metallicity gradients in these undisturbed galaxies, or radial variations in other properties (binarity or stellar rotation) driving envelope loss in progenitor stars. This result is not found in ‘disturbed' systems, where the distributions of Type Ib and Ic supernovae are consistent.
Comments on 'Phonon and magnetic structure in {\delta}-plutonium from density-functional theory' by P. S\"oderlind et al

In their recent paper [S\"oderlind, P. et al., Sci. Rep. 5, 15958 (2015)], S\"oderlind et al. discuss two subjects from a theoretical point of view: the phonon spectra and the possible magnetic structure of {\delta}-plutonium (Pu). Here, we comment on the second subject. S\"oderlind et al. compare the Pu magnetic form factor F(Q) calculated via density functional theory (DFT) with measurements of F(Q) by neutron spectroscopy [Janoschek, M. et al., Sci. Adv. 1, e1500188 (2015)]. In particular, this comparison does not consider a number of experimental facts established in the neutron spectroscopy study.
May Measurement Month 2018: an analysis of blood pressure screening results from Benin

Abstract Hypertension is the strongest cardiovascular risk factor worldwide. May Measurement Month (MMM) is an international campaign for blood pressure (BP) screening initiated by the International Society of Hypertension. This work aims to estimate the proportion and the levels of awareness, treatment, and control of hypertension in participants of the MMM survey in Benin in 2018. A cross-sectional survey focused on people aged ≥18 years was conducted in May 2018 in nine rural and urban areas in Benin. A sampling of volunteers was done. BP was measured following the MMM protocol. Hypertension was defined as a systolic BP ≥140 mm Hg and/or a diastolic BP ≥90 mm Hg (mean of the second and third readings) and/or taking antihypertensive medication. Linear regression was used to identify BP associations. A total of 2035 people were screened, including 55.9% women. The mean age was 44.2 ± 15.9 years. The percentage with hypertension was 35.4%. Of 721 participants with hypertension, 56.2% were aware of their diagnosis, 39.7% were on antihypertensive medication, and 13.6% were controlled (<140/90 mmHg). The results confirm the significant proportion of hypertension in Benin. Education programs on risk factors, early detection, and better management strategies should be developed.
Comparison of short-term results of subxiphoid and conventional video-assisted thoracoscopic surgery in diagnostic wedge resections

Background This study aimed to compare early results in patients who underwent subxiphoid wedge resection with those operated on using a multiportal approach. Methods We retrospectively evaluated 151 patients who underwent diagnostic wedge resection for suspected interstitial lung disease. Patients who underwent wedge resection via subxiphoid video-assisted thoracoscopic surgery and conventional video-assisted thoracoscopic surgery were compared. Results The study included 90 men (59.6%) and 61 women (40.4%) with a mean age of 54.8 ± 12 years. Of these, 127 patients underwent conventional video-assisted thoracoscopic surgery and 24 patients underwent subxiphoid video-assisted thoracoscopic surgery. Postoperative complications occurred in 13 patients (8.6%), with no significant difference according to surgical technique. Sex was a significant factor in the rate of complications (12.2% in men vs. 3.2% in women). There was no intraoperative mortality; the 30-day mortality rate was 4% (n = 6). Five nonsurviving patients were in the conventional video-assisted thoracoscopic surgery group and 1 was in the subxiphoid video-assisted thoracoscopic surgery group (p = 0.95). Conclusion The results of this study indicate that the subxiphoid approach reduced procedure time and length of hospital stay in the early period, while there was no significant difference between the techniques in terms of complications or mortality. Based on these findings, we conclude that surgical outcomes were as successful with the subxiphoid approach as with conventional video-assisted thoracoscopic surgery.
A Limit on Gas Accretion onto Close-in Super-Earth Cores from Disk Accretion

The core-accretion model predicts that planetary cores as massive as super-Earths undergo runaway gas accretion to become gas giants. However, the exoplanet census revealed the prevalence of super-Earths close to their host stars, which should have avoided runaway gas accretion. In fact, mass–radius relationships of transiting planets suggest that some close-in super-Earths possess H2/He atmospheres of ∼0.1%–10% by mass. Previous studies indicated that properties of a disk gas such as metallicity and the inflow/outflow cycle of a disk gas around a super-Earth can regulate accumulation of an H2/He atmosphere onto itself. In this paper, we propose a new mechanism for which radial mass accretion in a disk can limit the gas accretion onto super-Earth cores. Recent magnetohydrodynamic simulations found that magnetically driven disk winds can drive a rapid gas flow near the disk surface. Such a rapid gas flow may slip out of a planetary core and regulate gas supply to an accreting gas onto the core. We performed N-body simulations for formation of super-Earths with accretion of atmospheres in a viscous accretion disk including effects of wind-driven accretion. We found that even super-Earth cores can avoid triggering runaway gas accretion if the inflow of a disk gas toward the cores is limited by viscous accretion. Our model predicts that super-Earths having an H2/He atmosphere of ∼0.1–10 wt% form within ≲1 au of the central star, whereas gas giants are born in the outer region. This mechanism can explain the radial dependence of observed giant planets beyond the solar system.
INTERSTELLAR DETECTION OF c-C3D2

We report the first interstellar detection of c-C3D2. Doubly deuterated cyclopropenylidene, a carbene, has been detected toward the starless cores TMC-1C and L1544 using the IRAM 30 m telescope. The , 31, 3–20, 2, and 22, 1–11, 0 transitions of this species have been observed at 3 mm in both sources. The expected 1:2 intensity ratio has been found in the 30, 3–21, 2 and 31, 3–20, 2 lines, belonging to the para and ortho species, respectively. We also observed lines of the main species, c-C3H2, singly deuterated c-C3HD, and the species with one 13C off of the principal axis of the molecule, c-H13CC2H. The lines of c-C3D2 have been observed with high signal-to-noise ratio, better than 7. 5σ in TMC-1C and 9σ in L1544. The abundance of doubly deuterated cyclopropenylidene with respect to the normal species is found to be 0.4%–0.8% in TMC-1C and 1.2%–2.1% in L1544. The deuteration of this small hydrocarbon ring is analyzed with a comprehensive gas–grain model, the first including doubly deuterated species. The observed abundances of c-C3D2 can be explained solely by gas-phase processes, supporting the idea that c-C3H2 is a good indicator of gas-phase deuteration.
A survey of the Local Group of galaxies for symbiotic binary stars – I. First detection of symbiotic stars in M33

We present and discuss initial selection criteria and first results in M33 from a systematic search for extragalactic symbiotic stars. We show that the presence of diffuse interstellar gas emission can significantly contaminate the spectra of symbiotic star candidates. This important effect forces upon us a more stringent working definition of an extragalactic symbiotic star. We report the first detections and spectroscopic characterisation of 12 symbiotic binaries in M33. We found that four of our systems contain carbon-rich giants. In another two of them the giant seems to be a Zr-enhanced MS star, while the remaining six objects host M-type giants. The high number ratio of C to M giants in these binaries is consistent with the low metallicity of M33. The spatial and radial velocity distributions of these new symbiotic binaries are consistent with a wide range of progenitor star ages.