Miracle-dz/UniFAR-FTUs huggingface dataset:
Microwave surface-impedance measurements of the electronic state and dissipation of magnetic vortices in superconducting LiFeAs single crystals

LiFeAs is one of the iron-based superconductors having multiple gaps with the possible sign reversal. To clarify how those novel natures affect the energy dissipation of magnetic vortices, we investigated the microwave surface impedance of LiFeAs single crystals under finite magnetic fields. The flux-flow resistivity enhanced rapidly at low magnetic fields, which is similar to the case of MgB$_{2}$. This is probably the consequence of the multiple-gap nature and the gap anisotropy. This suggest that the sign-reversal is not important for the flux-flow even for multiple-gap superconductors. As for the electronic state, the vortex core of LiFeAs turned out to be "moderately clean". Furthermore, the mean free path inside the vortex core was much shorter than that outside, and was close to the core radius. These results strongly suggest a process specific to the core boundary is important for a scattering mechanism inside the vortex core.
Modulated Inflation Models and Primordial Black Holes

For the first time, the running of the running of the spectral index $\beta_s$ has been measured by Planck. This parameter is crucial for dark matter Primordial Black Holes (PBHs) formation. We study the PBHs formation in inflation potentials with superimposed periodic oscillations. We show that the value of $\beta_s$ suggested by the recent cosmic microwave background data is easily explained in these models. As a by-product, we also show that the nonproduction of (long--lived) PBHs puts a stronger upper bound on $\beta_s$.
Current and emerging anti-angiogenic therapies in gastrointestinal and hepatobiliary cancers

Gastrointestinal tumours are a heterogeneous group of neoplasms that arise in the gastrointestinal tract and hepatobiliary system. Their incidence is rising globally and they currently represent the leading cause of cancer-related mortality worldwide. Anti-angiogenic agents have been incorporated into the treatment armamentarium of most of these malignancies and have improved survival outcomes, most notably in colorectal cancer and hepatocellular carcinoma. New treatment combinations with immunotherapies and other agents have led to unprecedented benefits and are revolutionising patient care. In this review, we detail the mechanisms of action of anti-angiogenic agents and the preclinical rationale underlying their combinations with immunotherapies. We review the clinical evidence supporting their use across all gastrointestinal tumours, with a particular emphasis on colorectal cancer and hepatocellular carcinoma. We discuss available biomarkers of response to these therapies and their utility in routine clinical practice. Finally, we summarise ongoing clinical trials in distinct settings and highlight the preclinical rationale supporting novel combinations.
MOLECULAR CLOUDS IN THE NORTH AMERICAN AND PELICAN NEBULAE: STRUCTURES

We present observations of a 4.25 deg2 area toward the North American and Pelican Nebulae in the J = 1–0 transitions of 12CO, 13CO, and C18O. Three molecules show different emission areas with their own distinct structures. These different density tracers reveal several dense clouds with a surface density of over 500 M☉ pc−2 and a mean H2 column density of 5.8, 3.4, and 11.9 × 1021 cm−2 for 12CO, 13CO, and C18O, respectively. We obtain a total mass of 5.4 × 104 M☉ (12CO), 2.0 × 104 M☉ (13CO), and 6.1 × 103 M☉ (C18O) in the complex. The distribution of excitation temperature shows two phases of gas: cold gas (∼10 K) spreads across the whole cloud; warm gas (>20 K) outlines the edge of the cloud heated by the W80 H ii region. The kinetic structure of the cloud indicates an expanding shell surrounding the ionized gas produced by the H ii region. There are six discernible regions in the cloud: the Gulf of Mexico, Caribbean Islands and Sea, and Pelican's Beak, Hat, and Neck. The areas of 13CO emission range within 2–10 pc2 with mass of (1–5) × 103 M☉ and line width of a few km s−1. The different line properties and signs of star-forming activity indicate they are in different evolutionary stages. Four filamentary structures with complicated velocity features are detected along the dark lane in LDN 935. Furthermore, a total of 611 molecular clumps within the 13CO tracing cloud are identified using the ClumpFind algorithm. The properties of the clumps suggest that most of the clumps are gravitationally bound and at an early stage of evolution with cold and dense molecular gas.
Convergence of bilateral auditory midbrain inputs on neurons in the auditory thalamus of chicken

In the avian ascending auditory pathway, the nucleus mesencephalicus lateralis pars dorsalis (MLd; the auditory midbrain center) receives inputs from virtually all lower brainstem auditory nuclei and sends outputs bilaterally to the nucleus ovoidalis (Ov; the auditory thalamic nucleus). Axons from part of the MLd terminate in a particular domain of Ov, thereby suggesting a formation of segregated pathways point‐to‐point from lower brainstem nuclei via MLd to the thalamus. However, it has not yet been demonstrated whether any spatial clustering of thalamic neurons that receive inputs from specific domains of MLd exists. Ov neurons receive input from bilateral MLds; however, the degree of laterality has not been reported yet. In this study, we injected a recombinant avian adeno‐associated virus, a transsynaptic anterograde vector into the MLd of the chick, and analyzed the distribution of labeled postsynaptic neurons on both sides of the Ov. We found that fluorescent protein‐labeled neurons on both sides of the Ov were clustered in domains corresponding to subregions of the MLd. The laterality of projections was calculated as the ratio of neurons labeled by comparing ipsilateral to contralateral projections from the MLd, and it was 1.86 on average, thereby indicating a slight ipsilateral projection dominance. Bilateral inputs from different subdomains of the MLd converged on several single Ov neurons, thereby implying a possibility of a de novo binaural processing of the auditory information in the Ov.
BAROCLINIC INSTABILITY IN STELLAR RADIATION ZONES

Surfaces of constant pressure and constant density do not coincide in differentially rotating stars. Stellar radiation zones with baroclinic stratification can be unstable. Instabilities in radiation zones are of crucial importance for angular momentum transport, mixing of chemical species, and, possibly, for magnetic field generation. This paper performs linear analysis of baroclinic instability in differentially rotating stars. Linear stability equations are formulated for differential rotation of arbitrary shape and then solved numerically for rotation nonuniform in radius. As the differential rotation increases, r- and g-modes of initially stable global oscillations transform smoothly into growing modes of baroclinic instability. The instability can therefore be interpreted as stability loss to r- and g-modes excitation. Regions of stellar parameters where r- or g-modes are preferentially excited are defined. Baroclinic instability onsets at a very small differential rotation of below 1%. The characteristic time of instability growth is about 1000 rotation periods. Growing disturbances possess kinetic helicity. Magnetic field generation by the turbulence resulting from baroclinic instability in differentially rotating radiation zones is therefore possible.
Dynamical singularity resolution in spherically symmetric black hole formation

We study numerically the effects of loop quantum gravity motivated corrections on massless scalar field collapse in Painleve-Gullstrand coordinates. Near criticality the system exhibits Choptuik scaling with a mass gap and a new scaling relationship dependant upon the quantum length scale. Classical singularities are resolved by a radiationlike phase in the quantum collapse: the black hole consists of a compact region of spacetime bounded by a single, smooth trapping horizon. The 'evaporation' is not complete but leaves behind a small expanding shell that disperses to infinity.
No temperature fluctuations in the giant H II region H 1013

While collisionally excited lines in H II regions allow one to easily probe the chemical composition of the interstellar medium in galaxies, the possible presence of important temperature fluctuations casts some doubt on the derived abundan ces. To provide new insights into this question, we have carried out a detailed study of a giant H II region, H 1013, located in the galaxy M101, for which many observational data exist and which has been claimed to harbour temperature fluctuations at a level of t 2 = 0.03− 0.06. We have first complemented the already available optical observational datasets with a mid-infrared spectrum obtained with the Spitzer Space Telescope. Combined with optical data, this spectrum provides unprecedented information on the temperature structure of this giant H II region. A preliminary analysis based on empirical temperature diagnostics suggests that temperature fluctuations should be quite weak. However , only a detailed photoionization analysis taking into acco unt the geometry of the object and observing apertures can make a correct use of all the observational data. We have performed such a study using the Cloudy 3D package based on the photoionization code Cloudy. We have been able to produce photoionization models constrained by the observed Hsurface brightness distribution and by the known properties of the ionizing stellar population than can account for most of the line ratios within their uncertainties. Since the observational constraint s are both strong and numerous, this argues against the presence of significant temperature fluctuations in H 1013. The oxygen abund ance of our best model is 12 + log O/H = 8.57, as opposed to the values of 8.73 and 8.93 advocated by Esteban et al. (2009) and Bresolin (2007), respectively, based on the significant tem perature fluctuations they derived. However, our model is not able to reproduce the intensities of the oxygen recombination lines observed by Esteban et al. (2009), as well as the very low Balmer jump temperature inferred by Bresolin (2007). We have argued that the latter might be in error, due to observational difficulties. On the other h and, the discrepancy between model and observation as regards the recombination lines cannot be attributed to observational uncertainties and requires an explanation other than te mperature fluctuations.
Mass of the black hole in the Seyfert 1.5 galaxy H 0507+164 from reverberation mapping

We present the results of our optical monitoring campaign of the X-ray source H 0507+164, a low luminosity Seyfert 1.5 galaxy at a redshift, z = 0.018. Spectroscopic observations were carried out during 22 nights in 2007, from the 21 of November to the 26 of December. Photometric observations in the R-band for 13 nights were also obtained during the same period. The continuum and broad line fluxes of the galaxy were found to vary during our monitoring period. The R-band differential light curve with respect to a companion star also shows a similar variability. Using cross correlation analysis, we estimated a time delay of τcen = 3.01 +0.42 −1.84 days (in the rest frame), (
Contextualized Measurement Scale Adaptation: A 4-Step Tutorial for Health Psychology Research

Health psychology research is inherently context specific: Different health behaviors are executed by different target groups (e.g., gender, age) in different social structures, cultures, and environments. This asks for the adaptation of research instruments to enhance specificity. For example, when using measurement scales in new contexts, translation and psychometric validation of the instruments are necessary but not sufficient if the validity of the psychological concept behind a measurement scale has not been researched. In this study, we build on existing guidelines of translation as well as psychometric validation and present four steps on how to adapt measurement scales to a new context: Step 1 asks whether the psychological concept is found in the new context. Step 2 asks whether the measurement scale and its items are understood in the new context. Step 3 asks whether a measurement scale is valid and reliable. Step 4 asks how the items of the measurement scale perform individually. Following these four steps, measurement scales are carefully translated, adapted, and validated and can therefore be transferred to very different contexts.
Anti-aging protein klotho was associated with vitamin B12 concentration in adults

Previous studies have reported that serum klotho and vitamin B12 levels are valuable aging-related markers. However, studies supporting the association between serum klotho and vitamin B12 levels are lacking. We investigated the association between serum klotho and vitamin B12 concentrations in adults in the United States. The analytic study sample was 2065 aged 40 to 79 who participated in the 2011 to 2014 National Health and Nutrition Examination Survey (NHANES). Serum klotho and vitamin B12 collected from adults who consented to the use of their samples in the future. The participants were divided into 2 groups based on estimated glomerular filtration rate (eGFR) levels (high: ≥90 mL/min/1.73 m2 or low: <90 mL/min/1.73 m2). Of the 2065 participants, the log-transformed klotho concentration was significantly correlated with log-transformed vitamin B12 in the high eGFR group, but not in the low eGFR group. After adjusting for all potential covariates, there was a significant association between klotho and vitamin B12 concentrations in the high eGFR groups (beta = 0.100, SE = 0.040). In contrast, there was no significant relationship between klotho and vitamin B12 concentrations in the low eGFR group (beta = 0.012, SE = 0.019). Serum klotho concentration was significantly associated with vitamin B12 increases in US adults with high kidney function. Vitamin B12 concentration may be an important marker of klotho concentration in older adults.
Eliashberg analysis of optical spectra reveals a strong coupling of charge carriers to spin fluctuations in doped iron-pnictideBaFe2As2superconductors

F(ω) extracted using Eliashberg’sformalism. The characteristic energy of a large peak in the spectrum around 10 meV coincide withthe resonance peak in the spin excitation spectra, giving compelling evidence that in iron-basedsuperconductors spin ﬂuctuations strongly couple to the charge carriers and mediate superconduc-tivity. In addition the spectrum is found to evolve with temperature towards a less structuredbackground at higher energies as in the spin susceptibility.
Emotional expression in human odour

Abstract Abstract Recent work has demonstrated that human body odour alters with changing emotional state and that emotionally laden odours can affect the physiology and behaviour of people exposed to them. Here we review these discoveries, which we believe add to a growing recognition that the human sense of smell and its potential role in social interactions have been underappreciated. However, we also critically evaluate the current evidence, with a particular focus on methodology and the interpretation of emotional odour studies. We argue that while the evidence convincingly indicates that humans retain a capacity for olfactory communication of emotion, the extent to which this occurs in ordinary social interaction remains an open question. Future studies should place fewer restrictions on participant selection and lifestyle and adopt more realistic experimental designs. We also need to devote more consideration to underlying mechanisms and to recognise the constraints that these may place on effective communication. Finally, we outline some promising approaches to address these issues, and raise some broader theoretical questions that such approaches may help us to answer.
The Impact of Water and Other Fluids on Pediatric Nephrolithiasis

Pediatric nephrolithiasis cases have been on the rise in the past several years, resulting in increased healthcare costs and other burdens on the juveniles with this ailment. Recent research has shown that present trends in pediatric nephrolithiasis have changed as a result of fluid intake, including water consumption, nutrition, obesity prevalence, lifestyle, and imaging procedures. A specific cause, meanwhile, is still elusive. Trends in pediatric nephrolithiasis need to be thoroughly researched. Furthermore, variables specific to pediatric nephrolithiasis that could cause greater difficulties in an affected child elevate the level of worry with cumulative prevalence. Doctors should rigorously assess patients who present with kidney stones when they have dynamics such as varied clinical presentation, high recurrence of kidney stones linked to metabolic and urinary tract problems, and the potential existence of rare genetic kidney stone illnesses. This review aims to identify adaptive risk factors and anomalies that call for specialized treatment and prescription. More specifically, the major goals of medical and surgical treatments are to eliminate kidney stone risk and stop relapse while concurrently lowering interventional barriers. A dedicated nephrolithiasis clinic run by a pediatric nephrologist, nutritionist, urologist, and clinical nurse may sometimes be beneficial for patients in serious danger. Such a clinic offers significant chances to learn more about pediatric nephrolithiasis, which has been linked to water consumption and hence fosters urgently required study in this area.
The Physical Demands of Match-Play in Academy and Senior Soccer Players from the Scottish Premiership

The present study aimed to assess the physical match performance among senior and youth soccer players from an elite Scottish Premiership club during the 2021/2022 season. Twenty-two first team (25.9 ± 4.5 years, 78.3 ± 8.2 kg, 1.82 ± 0.07 cm) and 16 youth players (16.8 ± 0.9 years, 70.1 ± 6.8 kg, 177 ± 5.8 cm) were examined. A selection of physical match performance variables were measured using a global positioning system. Linear mixed-effect regressions revealed for all examined variables no significant differences between first team and U-18 players and no significant differences between playing level by position interaction. Across both teams, Centre Backs compared to Wing Backs, showed a 295 m (p < 0.01) lower high-intensity distance, and performed on average 36 fewer very-high intensity decelerations (p = 0.03). Comparing to Wide Midfielders, Centre Backs showed lower total (1297 m, p = 0.01), high-intensity (350 m, p = 0.01), and sprint (167 m, p < 0.01) distances. Sprint distance was also lower in Centre Backs vs. Strikers (118 m, p = 0.03), and in Central Midfielders vs. both Strikers (104 m, p = 0.03) and Wide Midfielders (154 m, p = 0.01). The present findings highlight the physical match performance of elite Scottish players and provide useful information within the context of understanding how methods of physical development of youth soccer are implemented in different countries.
WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST MASS

We perform three-dimensional dust radiative transfer (RT) calculations on hydrodynamic simulations of isolated and merging disk galaxies in order to quantitatively study the dependence of observed-frame submillimeter (submm) flux density on galaxy properties. We find that submm flux density and star formation rate (SFR) are related in dramatically different ways for quiescently star-forming galaxies and starbursts. Because the stars formed in the merger-induced starburst do not dominate the bolometric luminosity and the rapid drop in dust mass and more compact geometry cause a sharp increase in dust temperature during the burst, starbursts are very inefficient at boosting submm flux density (e.g., a ≳ 16 × boost in SFR yields a ≲ 2 × boost in submm flux density). Moreover, the ratio of submm flux density to SFR differs significantly between the two modes; thus one cannot assume that the galaxies with highest submm flux density are necessarily those with the highest bolometric luminosity or SFR. These results have important consequences for the bright submillimeter-selected galaxy (SMG) population. Among them are: (1) The SMG population is heterogeneous. In addition to merger-driven starbursts, there is a subpopulation of galaxy pairs, where two disks undergoing a major merger but not yet strongly interacting are blended into one submm source because of the large (≳ 15” or ∼130 kpc at z = 2) beam of single-dish submm telescopes. (2) SMGs must be very massive (M⋆ ≳ 6 × 1010 M☉). (3) The infall phase makes the SMG duty cycle a factor of a few greater than what is expected for a merger-driven starburst. Finally, we provide fitting functions for SCUBA and AzTEC submm flux densities as a function of SFR and dust mass and bolometric luminosity and dust mass; these should be useful for calculating submm flux density in semi-analytic models and cosmological simulations when performing full RT is computationally not feasible.
Multicolor Infrared Observations of SN 2006aj. I. The Supernova Associated with XRF 060218

We report simultaneous multicolor near-infrared (NIR) observations of the supernova associated with X-ray flash 060218 during the first 16 days after the high-energy event. We find that the light curve rises and peaks relatively fast compared to other Type Ic supernovae (SNe Ic), with the characteristic broad NIR peak seen in all three bands. We find that the rise profile before the peak is largely independent of NIR wavelength, each band appearing to transition into a plateau phase around day 10-13. Since the light curve is in the plateau phase when our observations end at day 16, we can only place limits on the peak absolute magnitudes, but we estimate that SN 2006aj is one of the lowest NIR luminosity X-ray flash/gamma-ray burst (XRF/GRB) associated SNe observed to date. The broad peaks observed in the JHKs bands point to a large increase in the NIR contribution of the total flux output from days 10-16. This evolution can be seen in the broad color and spectral energy distribution diagrams constructed using UBVRIJHKs monochromatic flux measurements for the first 16 days of the event. Ultimately, a 10 day rise time would make SN 2006aj an extremely fast rise SN Ic event, faster than SN 1998bw and SN 2003dh, which combined with its underluminous nature indicates a lower amount of 56Ni ejected by the progenitor compared to other XRF/GRB-SNe. Furthermore, the lack of significant color change during the rise portion of the burst points to little or no spectral evolution over the first 10 days of activity in the NIR.
Enhancement of Perpendicular Magnetic Anisotropy and Transmission of Spin-Hall-Effect-Induced Spin Currents by a Hf Spacer Layer in W/Hf/CoFeB/MgO Layer

We report that strong perpendicular magnetic anisotropy of the ferromagnetic layer in a W/CoFeB/MgO multilayer structure can be established by inserting a Hf layer as thin as 0.25 nm between the W and CoFeB layers. The Hf spacer also allows transmission of spin currents generated by an in-plane charge current in the W layer to apply strong spin torque on the CoFeB, thereby enabling current-driven magnetic switching. The antidamping-like and field-like components of the spin torque exerted on a 1 nm CoFeB layer are of comparable magnitudes in this geometry. Both components originate from the spin Hall effect in the underlying W layer.