Miracle-dz/UniFAR-FTUs huggingface dataset:
Origin and z-distribution of Galactic diffuse [C II] emission

We determine the source of the diffuse [CII] emission by studying its spatial (radial and vertical) distributions. We used the HIFI [CII] Galactic survey (GOT C+), along with HI, 12CO, and 13CO data toward 354 lines of sight, and several HIFI [CII] and [CI] position-velocity maps. We quantified the emission in each spectral line profile by evaluating the intensities in 3 km/s wide velocity bins, 'spaxels'. Using the detection of [CII] with CO or [CI], we separated the dense and diffuse gas components. We derived 2-D Galactic disk maps using the spaxel velocities for kinematic distances. We separated the warm and cold H2 gases by comparing CO emissions with and without associated [CII]. We find evidence of widespread diffuse [CII] emission with a z-scale distribution larger than that for the total [CII] or CO. and it consists of (i) diffuse molecular (CO-faint) H2 clouds and (ii) diffuse HI clouds and/or WIM. In the inner Galaxy we find a lack of [CII] detections in a majority (~62%) of HI spaxels and show that the diffuse component primarily comes from the WIM (~21%) and that the HI gas is not a major contributor to the diffuse component (~6%). The warm-H2 radial profile shows an excess in the range 4 to 7 kpc, consistent with enhanced star formation there. We derive, for the first time, the 2-D [CII] spatial distribution in the plane and the z-distributions of the individual [CII] gas component. We estimate the fractional [CII] emission tracing (i) H2 gas in dense and diffuse molecular clouds as ~48% and ~ 14%, respectively, (ii) in the HI gas ~18%, and (iii) in the WIM ~21%. Including non-detections from HI increases the [CII] in HI to ~ 27%. The z-scale distributions FWHM are [CII] sources with CO, ~130 pc, (CO-faint) diffuse H2 gas, ~200 pc, and the diffuse HI and WIM, ~330 pc. CO observations, when combined with [CII], probe the warm-H2 gas, tracing star formation.
Investigation of macrophage polarization in herniated nucleus pulposus of patients with lumbar intervertebral disc herniation

Macrophage infiltration and polarization during lumbar intervertebral disc herniation (LDH) have attracted increased attention but their role remains unclear. To explore macrophage polarization in herniated nucleus pulposus (NP) tissue of patients with LDH and investigate the association between cell frequency and different clinical characteristics or symptoms, we conducted a retrospective study by analyzing NP tissue samples from 79 patients. Clinical features and symptoms, using the visual analog scale (VAS) and Oswestry disability index (ODI), were collected. The macrophage markers CD68, CCR7, CD163, and CD206; pro‐inflammatory cytokine TNF‐α; and anti‐inflammatory factor IL‐4 were analyzed by immunohistochemistry. The frequency of polarized macrophages and positivity rate of pro‐ and anti‐inflammatory cytokines showed significant differences in some of clinical characteristics. Specifically, higher CCR7+ and TNF‐α + proportions were identified in the high‐intensity zone (HIZ) and the type of extrusion and sequestration NP tissue than in non‐HIZ and protrude NP tissue. Higher CD206+ and IL‐4+ proportion were detected in Modic changes. However, no differences in gender, age, smoking status, Pfirrmann grade, analgesic use, leg pain duration, and segments were found between groups. CD68+, CCR7+, and CD206+ cell proportions, and TNF‐α and IL‐4 showed positive associations with VAS scores preoperation. Associations between ODI and the macrophages markers were weak/insignificant. Our results indicated that macrophage polarization or macrophage‐like cells contribute to LDH pathological features. Macrophage populations displaying significant associations with VAS score reflected continuous M1/M2 transition contributing to pain during LDH. These findings may contribute to enhanced/personalized pharmacological interventions for patients with LDH considering pain heterogeneity.
Shoulder Internal Rotator Strength as Risk Factor for Shoulder Pain in Volleyball Players

Abstract The aim of this study was to identify the intrinsic factors that could increase risk of shoulder pain in adolescent volleyball players. Twenty-eight young male volleyball players (between 14 and 18 years old) participated in this study. Athletes were submitted to: isokinetic muscle strength assessment of shoulder rotator muscles, ball service speed assessment, anterior and posterior drawer test, apprehension test, groove sign and scapular dyskinesia test. Athletes were followed for 16 weeks to monitor the presence of shoulder pain. All athletes were submitted to the same training protocol. During the 16 weeks, 28.5% of the athletes (n=8) experienced shoulder pain in the dominant limb higher than 3 according to Numerical Rating Scale criteria; 71.5% of the athletes (n=20) did not experience pain, or pain equal or lower than 3. The main result of our study was that the odds of feeling pain higher than 3 was significantly higher among players who presented higher values for internal rotation peak torque (OR=1.113, CI 95%=1.006 to 1.232 and p=0.038). The odds of feeling pain increased by 11% for every N·m of the internal rotator muscles. Pre-season isokinetic rotator strength assessments can help identify adolescent volleyball players at increased risk of a shoulder injury.
A statistical fractal-diffusive avalanche model of a slowly-driven self-organized criticality system

Aims. We develop a statistical analytical model that predicts the occurrence frequency distributions and parameter correlations of avalanches in nonlinear dissipative systems in the state of a slowly-driven self-organized criticality (SOC) system. Methods. This model, called the fractal-diffusive SOC model, is based on the following four assumptions: (i) the avalanche size L grows as a diffusive random walk with time T, following L ∝ T 1/2 ; (ii) the energy dissipation rate f(t) occupies a fractal volume with dimension DS; (iii) the mean fractal dimension of avalanches in Euclidean space S = 1,2, 3i sDS ≈ (1 +S)/2; and (iv) the occurrence frequency distributions N(x) ∝ x −αx based on spatially uniform probabilities in a SOC system are given by N(L) ∝ L −S , with S being the Eudlidean dimension. We perform cellular automaton simulations in three dimensions (S = 1,2,3) to test the theoretical model. Results. The analytical model predicts the following statistical correlations: F ∝ L DS ∝ T DS /2 for the flux, P ∝ L S ∝ T S /2 for the peak energy dissipation rate, and E ∝ FT ∝ T 1+DS /2 for the total dissipated energy; the model predicts powerlaw distributions for all parameters, with the slopes αT = (1 +S)/2, αF = 1 +(S −1)/DS, αP = 2 −1/S ,a ndαE = 1 +(S −1)/(DS +2). The cellular automaton simulations reproduce the predicted fractal dimensions, occurrence frequency distributions, and correlations within a satisfactory agreement within ≈10% in all three dimensions. Conclusions. One profound prediction of this universal SOC model is that the energy distribution has a powerlaw slope in the range of αE = 1.40−1.67, and the peak energy distribution has a slope of αP = 1.67 (for any fractal dimension DS = 1, ., 3i n Euclidean space S = 3), and thus predicts that the bulk energy is always contained in the largest events, which rules out significant nanoflare heating in the case of solar flares.
Smoking and environmental tobacco smoke exposure: implications in ocular disorders

Abstract Purpose This article aims to gather and review the available knowledge on several implications of smoking and environmental tobacco smoke (ETS) exposure in ocular disorders and provides pathomechanistic insights where applicable. Materials and Methods PubMed and Scopus databases were searched for relevant studies on the association of smoking and ETS exposure with various ocular disorders. Studies with different evidence levels, e.g., in-vivo, case-control, cohort, and meta-analysis, were included. Results Smoking is an established, modifiable risk factor in several ocular diseases, including cataract, age-related macular degeneration, and Graves’ ophthalmopathy; smokers are subject to more severe disease courses and less favorable treatment outcomes. Uveitis is twice as likely in smokers; smoking may also delay its resolution. Smoking and ETS exposure are major risk factors for diseases of other organs, with associated ocular complications as well, such as diabetes mellitus. ETS exposure is also associated with ocular surface pathologies, including dry eye syndrome. In children, early-life ETS exposure and maternal smoking during pregnancy are strongly associated with refractive errors and strabismus. Currently, available data on potential risks attributable to ETS exposure regarding ocular diseases are scarce and, in some instances, controversial. Conclusion In addition to smoking, ETS exposure is also a significant public health concern with possible links to several ocular diseases. However, the level of education of at-risk populations in this regard does not match the strength of the evidence.
A systematic literature review of group-based training interventions for informal carers: impact on the behavioural and psychological symptoms of dementia (BPSD)

Abstract Objectives Caring for a relative with dementia can be extremely challenging especially when someone presents with behavioural and psychological symptoms of dementia (BPSD). The training provided to informal carers is varied and inconsistent. Group-based training programmes are often prescribed but their impact on care-recipient wellbeing and symptomology is yet to be well established. This review synthesises the literature on consensus, themes and effectiveness of informal-carer, group-based educational training programmes on BPSD symptoms. Methods Ten papers were included of which very few considered BPSD outcomes as their primary aim of investigation. Results Methodological and theoretical approaches across the empirical papers varied considerably. Generally, studies of higher quality and with some positive results on BPSD outcomes tended to incorporate teaching on structured problem-solving skills. Studies measuring for longer term changes also tended to conclude more beneficial outcomes. The length and duration of groups and the group-sizes appeared inconsequential to BPSD outcomes. Conclusion The empirical evidence is weak for carer group interventions in the management of BPSD. Practice reasons for this are discussed. Future studies designed to measure BPSD as a primary outcome would be a welcome addition to the literature.
MODELING THE REDSHIFT EVOLUTION OF THE NORMAL GALAXY X-RAY LUMINOSITY FUNCTION

Emission from X-ray binaries (XRBs) is a major component of the total X-ray luminosity of normal galaxies, so X-ray studies of high-redshift galaxies allow us to probe the formation and evolution of XRBs on very long timescales (∼10 Gyr). In this paper, we present results from large-scale population synthesis models of binary populations in galaxies from z = 0 to ∼20. We use as input into our modeling the Millennium II Cosmological Simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history (SFH) and metallicity evolution of each galaxy. We run a grid of 192 models, varying all the parameters known from previous studies to affect the evolution of XRBs. We use our models and observationally derived prescriptions for hot gas emission to create theoretical galaxy X-ray luminosity functions (XLFs) for several redshift bins. Models with low common envelope efficiencies, a 50% twins mass ratio distribution, a steeper initial mass function exponent, and high stellar wind mass-loss rates best match observational results from Tzanavaris & Georgantopoulos, though they significantly underproduce bright early-type and very bright (Lx > 1041) late-type galaxies. These discrepancies are likely caused by uncertainties in hot gas emission and SFHs, active galactic nucleus contamination, and a lack of dynamically formed low-mass XRBs. In our highest likelihood models, we find that hot gas emission dominates the emission for most bright galaxies. We also find that the evolution of the normal galaxy X-ray luminosity density out to z = 4 is driven largely by XRBs in galaxies with X-ray luminosities between 1040 and 1041 erg s−1.
Development of high-performance alkali-hybrid polarized 3 He targets for electron scattering

We present the development of high-performance polarized ³He targets for use in electron scattering experiments that utilize the technique of alkali-hybrid spin-exchange optical pumping. We include data obtained during the characterization of 24 separate target cells, each of which was constructed while preparing for one of four experiments at Jefferson Laboratory in Newport News, Virginia. The results presented here document dramatic improvement in the performance of polarized ³He targets, as well as the target properties and operating parameters that made those improvements possible. Included in our measurements were determinations of the so-called X-factors that quantify a temperature-dependent and as-yet poorly understood spin-relaxation mechanism that limits the maximum achievable ³He polarization to well under 100%. The presence of this spin-relaxation mechanism was clearly evident in our data. We also present results from a simulation of the alkali-hydrid spin-exchange optical pumping process that was developed to provide guidance in the design of these targets. Good agreement with actual performance was obtained by including details such as off-resonant optical pumping. Now benchmarked against experimental data, the simulation is useful for the design of future targets. Included in our results is a measurement of the K- ³He spin-exchange rate coefficient $$k^\mathrm{K}_\mathrm{se} = \left ( 7.46 \pm 0.62 \right )\! \times\! 10^{-20}\ \mathrm{cm^3/s}$$ over the temperature range 503 K to 563 K.
Constraints on the Alignment of Galaxies in Galaxy Clusters from $\sim$14,000 Spectroscopic Members

Torques acting on galaxies lead to physical alignments, but the resulting ellipticity correlations are difficult to predict. As they constitute a major contaminant for cosmic shear studies, it is important to constrain the intrinsic alignment signal observationally. We measured the alignments of satellite galaxies within 90 massive galaxy clusters in the redshift range 0.05<z<0.55 and quantified their impact on the cosmic shear signal. We combined a sample of 38,104 galaxies with spectroscopic redshifts with high-quality data from the Canada-France-Hawaii Telescope. We used phase-space information to select 14,576 cluster members, 14,250 of which have shape measurements and measured three different types of alignment: the radial alignment of satellite galaxies toward the brightest cluster galaxies (BCGs), the common orientations of satellite galaxies and BCGs, and the radial alignments of satellites with each other. Residual systematic effects are much smaller than the statistical uncertainties. We detect no galaxy alignment of any kind out to at least 3 r200. The signal is consistent with zero for both blue and red galaxies, bright and faint ones, and also for subsamples of clusters based on redshift, dynamical mass, and dynamical state. These conclusions are unchanged if we expand the sample with bright cluster members from the red sequence. We augment our constraints with those from the literature to estimate the importance of the intrinsic alignments of satellites compared to those of central galaxies, for which the alignments are described by the linear alignment model. Comparison of the alignment signals to the expected uncertainties of current surveys such as the Kilo-Degree Survey suggests that the linear alignment model is an adequate treatment of intrinsic alignments, but it is not clear whether this will be the case for larger surveys.
SHORT GAMMA-RAY BURSTS FROM DYNAMICALLY ASSEMBLED COMPACT BINARIES IN GLOBULAR CLUSTERS: PATHWAYS, RATES, HYDRODYNAMICS, AND COSMOLOGICAL SETTING

We present a detailed assessment of the various dynamical pathways leading to the coalescence of compact objects in globular clusters (GCs) and Short Gamma-ray Burst (SGRB) production. We consider primordial binaries, dynamically formed binaries (through tidal two-body and three-body exchange interactions), and direct impacts of compact objects (WD/NS/BH). Here, we show that if the primordial binary fraction is small, close encounters dominate the production rate of coalescing compact systems. We find that the two dominant channels are the interaction of field neutron stars (NSs) with dynamically formed binaries and two-body encounters. Under such conditions, we estimate the redshift distribution and host galaxy demographics of SGRB progenitors, and find that GCs can provide a significant contribution to the overall observed rate. Regarding the newly identified channel of close stellar encounters involving WD/NS/BH, we have carried out precise modeling of the hydrodynamical evolution, giving us a detailed description of the resulting merged system. Our calculations show that there is in principle no problem in accounting for the global energy budget of a typical SGRB. The particulars of each encounter, however, are variable in several aspects and can lead to interesting diversity. First and most importantly, the characteristics of the encounter are highly dependent on the impact parameter. This is in contrast to the merger scenario, where the masses of the compact objects dictate a typical length and luminosity scale for SGRB activity. Second, the nature of the compact star itself can produce very different outcomes. Finally, the presence of tidal tails in which material will fall back onto the central object at a later time is a robust feature of the present set of calculations. The mass involved in these structures is considerably larger than for binary mergers. It is thus possible to account generically in this scenario for a prompt episode of energy release, as well as for activity many dynamical time scales later.
Molecular depletion times and the CO-to-H2 conversion factor in metal-poor galaxies

Tracing molecular hydrogen content with carbon monoxide in low-metallicity galaxies has been exceedingly difficult. Here we present a new effort, with IRAM 30-m observations of 12CO(1-0) of a sample of 8 dwarf galaxies having oxygen abundances ranging from 12+logO/H=7.7 to 8.4. CO emission is detected in all galaxies, including the most metal-poor galaxy of our sample (0.1 Zsun); to our knowledge this is the largest number of 12CO(1-0) detections ever reported for galaxies with 12+logO/H<=8 (0.2 Zsun) outside the Local Group. We calculate stellar masses (Mstar) and star-formation rates (SFRs), and analyze our results by combining our observations with galaxy samples from the literature. Extending previous results for a correlation of the molecular gas depletion time, tau(dep), with Mstar and specific SFR (sSFR), we find a variation in tau(dep) of a factor of 200 or more (from <50 Myr to 10 Gyr) over a spread of 1000 in sSFR and Mstar. We exploit the variation of tau(dep) to constrain the CO-to-H2 mass conversion factor alpha(CO) at low metallicity, and assuming a power-law variation find alpha(CO) \propto (Z/Zsun)^1.9, similar to results based on dust continuum measurements compared with gas mass. By including HI measurements, we show that the fraction of total gas mass relative to the baryonic mass is higher in galaxies that are metal poor, of low mass, and of high sSFR. Finally, comparisons of the data with star-formation models of the molecular gas phases suggest that, at metallicities Z/Zsun<=0.2, there are some discrepancies with model predictions.
Infrared colour properties of nearby radio-luminous galaxies

By combining the data of the Two Micron All Sky Survey, the Wide-Field Infrared Survey Explorer and the AKARI satellite, we study the infrared colour properties of a sample of 2712 nearby radio-luminous galaxies (RLGs). These RLGs are divided into radio-loud (RL) active galactic nuclei (AGNs), mainly occurring at redshifts of 0.05 3.0. We also analyse the MIR colours of RL AGNs divided into low-and high-excitation radio galaxies (LERGs and HERGs, respectively). The ([3.4]-[4.6])-([4.6]-[12]) diagram clearly shows separate distributions of LERGs and HERGs and a region of overlap, which suggests that LERGs and HERGs have different MIR properties. LERGs are responsible for the double-core distribution of RL AGNs on the ([3.4]-[4.6])-([4.6]-[12]) diagram. In addition, we also suggest 90-140 mu m band spectral index a(90, 140) < -1.4 as a criterion of selecting nearby active galaxies with non-thermal emissions at far-infrared wavelengths.
Molecular gas properties of a lensed star-forming galaxy at z 3.6: a case study

We report on the galaxy MACSJ0032-arc at z(CO) = 3.6314 discovered during the Herschel Lensing snapshot Survey of massive galaxy clusters, and strongly lensed by the cluster MACSJ0032.1+1808. The successful detections of its rest-frame ultraviolet (UV), optical, far-infrared (FIR), millimeter, and radio continua, and of its CO emission enable us to characterize, for the first time at such a high redshift, the stellar, dust, and molecular gas properties of a compact star-forming galaxy with a size smaller than 2.5 kpc, a fairly low stellar mass of 4.8(-1.0)(+0.5) x 10(9) M circle dot, and a moderate IR luminosity of 4.8(-0.6)(+1.2) x 10(11) L circle dot. By combining the stretching effect of the lens with the high angular resolution imaging of the CO(10) line emission and the radio continuum at 5 GHz, we find that the bulk of the molecular gas mass and star formation seems to be spatially decoupled from the rest-frame UV emission. About 90% of the total star formation rate is undetected at rest-frame UV wavelengths because of severe obscuration by dust, but is seen through the thermal FIR dust emission and the radio synchrotron radiation. The observed CO(43) and CO(65) lines demonstrate that high-J transitions, at least up to J = 6, remain excited in this galaxy, whose CO spectral line energy distribution resembles that of high-redshift submm galaxies, even though the IR luminosity of MACSJ0032-arc is ten times lower. This high CO excitation is possibly due to the compactness of the galaxy. We find evidence that this high CO excitation has to be considered in the balance when estimating the CO-to-H-2 conversion factor. Indeed, the respective CO-to-H-2 conversion factors as derived from the correlation with metallicity and the FIR dust continuum can only be reconciled if excitation is accounted for. The inferred depletion time of the molecular gas in MACSJ0032-arc supports the decrease in the gas depletion timescale of galaxies with redshift, although to a lesser degree than predicted by galaxy evolution models. Instead, the measured molecular gas fraction as high as 6079% in MACSJ0032-arc favors the continued increase in the gas fraction of galaxies with redshift as expected, despite the plateau observed between z similar to 1.5 and z similar to 2.5.