Miracle-dz/UniFAR-FTUs huggingface dataset:
Scaling behaviour of the critical current in clean epitaxial Ba(Fe1-xCox)2As2 thin films

The angular-dependent critical current density, Jc(theta), and the upper critical field, Hc2(theta), of epitaxial Ba(Fe1-xCox)2As2 thin films have been investigated. No Jc(theta) peaks for H || c were observed regardless of temperatures and magnetic fields. In contrast, Jc(theta) showed a broad maximum at theta=90 degree, which arises from intrinsic pinning. All data except at theta=90 degree can be scaled by the Blatter plot. Hc2(theta) near Tc follows the anisotropic Ginzburg-Landau expression. The mass anisotropy increased from 1.5 to 2 with increasing temperature, which is an evidence for multi-band superconductivity.
Massive black hole factories: Supermassive and quasi-star formation in primordial halos

Context. Supermassive stars and quasi-stars (massive stars with a central black hole) are both considered as potential progenitors for the formation of supermassive black holes. They are expected to form from rapidly accreting protostars in massive primordial halos. Aims. We explore how long rapidly accreting protostars remain on the Hayashi track, implying large protostellar radii and weak accretion luminosity feedback. We assess the potential role of energy production in the nuclear core, and determine what regulates the evolution of such protostars into quasi-stars or supermassive stars. Methods. We followed the contraction of characteristic mass shells in rapidly accreting protostars, and inferred the timescales for them to reach nuclear densities. We compared the characteristic timescales for nuclear burning with those for which the extended protostellar envelope can be maintained. Results. We find that the extended envelope can be maintained up to protostellar masses of 3.6 × 10 8 u m 3 M� ,w here u m denotes the accretion rate in solar masses per year. We expect the nuclear core to exhaust its hydrogen content in 7 × 10 6 yr. If accretion rates u m � 0.14 can still be maintained at this point, a black hole may form within the accreting envelope, leading to a quasi-star. Alternatively, the accreting object will gravitationally contract to become a main-sequence supermassive star. ·
Exuberant Innovation: The Human Genome Project

We present a detailed synthesis of the development of the Human Genome Project (HGP) from 1986 to 2003 in order to test the “social bubble” hypothesis that strong social interactions between enthusiastic supporters of the HGP weaved a network of reinforcing feedbacks that led to a widespread endorsement and extraordinary commitment by those involved in the project, beyond what would be rationalized by a standard cost-benefit analysis in the presence of extraordinary uncertainties and risks. The vigorous competition and race between the initially public project and several private initiatives is argued to support the social bubble hypothesis. We also present quantitative analyses of the concomitant financial bubble concentrated on the biotech sector. Confirmation of this hypothesis is offered by the present consensus that it will take decades to exploit the fruits of the HGP, via a slow and arduous process aiming at disentangling the extraordinary complexity of the human complex body. The HGP has ushered other initiatives, based on the recognition that there is much that genomics cannot do, and that “the future belongs to proteomics”. We present evidence that the competition between the public and private sector actually played in favor of the former, since its financial burden as well as its horizon was significantly reduced (for a long time against its will) by the active role of the later. This suggests that governments can take advantage of the social bubble mechanism to catalyze long-term investments by the private sector, which would not otherwise be supported.
MAGNETOHYDROSTATIC EQUILIBRIUM STRUCTURE AND MASS OF FILAMENTARY ISOTHERMAL CLOUD THREADED BY LATERAL MAGNETIC FIELD

Herschel observations have recently revealed that interstellar molecular clouds consist of many filaments. Polarization observations in optical and infrared wavelengths indicate that the magnetic field often runs perpendicular to the filament. In this article, we study the magnetohydrostatic configuration of isothermal gas in which the thermal pressure and the Lorentz force are balanced against the self-gravity, and the magnetic field is globally perpendicular to the axis of the filament. The model is controlled by three parameters: center-to-surface density ratio (ρc/ρs), plasma β of surrounding interstellar gas (β0), and the radius of the hypothetical parent cloud normalized by the scale-height (), although there remains freedom in how the mass is distributed against the magnetic flux (mass loading). In the case where is small enough, the magnetic field plays a role in confining the gas. However, the magnetic field generally has the effect of supporting the cloud. There is a maximum line-mass (mass per unit length) above which the cloud is not supported against gravity. Compared with the maximum line-mass of a nonmagnetized cloud (, where cs and G represent, respectively, the isothermal sound speed and the gravitational constant), that of the magnetized filament is larger than the nonmagnetized one. The maximum line-mass is numerically obtained as , where Φcl represents one half of the magnetic flux threading the filament per unit length. The maximum mass of the filamentary cloud is shown to be significantly affected by the magnetic field when the magnetic flux per unit length exceeds Φcl ≳ 3 pc μG (cs/190 m s−1)2.
“Ferrocrinology”—Iron Is an Important Factor Involved in Gluco- and Lipocrinology

“Ferrocrinology” is the term used to describe the study of iron effects on the functioning of adipose tissue, which together with muscle tissue makes the largest endocrine organ in the human body. By impairing exercise capacity, reducing AMP-activated kinase activity, and enhancing insulin resistance, iron deficiency can lead to the development of obesity and type 2 diabetes mellitus. Due to impaired browning of white adipose tissue and reduced mitochondrial iron content in adipocytes, iron deficiency (ID) can cause dysfunction of brown adipose tissue. By reducing ketogenesis, aconitase activity, and total mitochondrial capacity, ID impairs muscle performance. Another important aspect is the effect of ID on the impairment of thermogenesis due to reduced binding of thyroid hormones to their nuclear receptors, with subsequently impaired utilization of norepinephrine in tissues, and impaired synthesis and distribution of cortisol, which all make the body’s reactivity to stress in ID more pronounced. Iron deficiency can lead to the development of the most common endocrinopathy, autoimmune thyroid disease. In this paper, we have discussed the role of iron in the cross-talk between glucocrinology, lipocrinology and myocrinology, with thyroid hormones acting as an active bystander.
The redistribution of matter in the cores of galaxy clusters

We present cosmological N-body resimulations of the assembly of the Brightest Cluster Galaxies (BCGs) in rich clusters. At z = 2 we populate dark matter subhalos with self-gravitating stellar systems whose abundance and structure match observed high-redshift galaxies. By z = 0, mergers have built much larger galaxies at cluster centre. Their dark matter density profiles are shallower than in corresponding darkmatter-only simulations, but their total mass density profiles (stars + dark matter) are quite similar. Differences are found only at radii where the effects of central black holes may be significant. Dark matter density slopes shallower than = 1.0 occur for r/r200 < 0.015, close to the half-light radii of the BCGs. Our experiments support earlier suggestions that NFW-like profiles are an attractor for the hierarchical growth of structure in collisionless systems – total mass density profiles asymptote to the solution found in dark-matter-only simulations over the radial range where mergers produce significant mixing between stars and dark matter. Simulated dark matter fractions are substantially higher in BCGs than in field ellipticals, reaching 80% within the half-light radius. We also estimate that supermassive black hole mergers should create BCG cores as large as rc � 3kpc. The good agreement of all these properties with recent observational studies of BCG structure suggests that dissipational processes have not played a dominant role in the assembly of the observed systems.
Spitzer Planck Herschel Infrared Cluster (SPHerIC) survey: Candidate galaxy clusters at 1.3 < z < 3 selected by high star-formation rate

There is a lack of large samples of spectroscopically confirmed clusters and protoclusters at high redshifts, z > 1.5. Discovering and characterizing distant (proto-)clusters is important for yielding insights into the formation of large-scale structure and on the physical processes responsible for regulating star-formation in galaxies in dense environments. The Spitzer Planck Herschel Infrared Cluster (SPHerIC) survey was initiated to identify these characteristically faint and dust-reddened sources during the epoch of their early assembly. We present Spitzer/IRAC observations of 82 galaxy (proto-)cluster candidates at 1.3 < zp < 3.0 that were vetted in a two step process: (1) using Planck to select by color those sources with the highest star-formation rates, and (2) using Herschel at higher resolution to separate out the individual red sources. The addition of the Spitzer data enables efficient detection of the central and massive brightest red cluster galaxies (BRCGs). We find that BRCGs are associated with highly significant, extended and crowded regions of IRAC sources which are more overdense than the field. This result corroborates our hypothesis that BRCGs within the Planck–Herschel sources trace some of the densest and actively star-forming proto-clusters in the early Universe. On the basis of a richness-mass proxy relation, we obtain an estimate of their mean masses which suggests our sample consists of some of the most massive clusters at z ≈ 2 and are the likely progenitors of the most massive clusters observed today.
QUALITY OF KING SCALLOP (PECTEN MAXIMUS) AND SPRAT (SPRATTUS SPRATTUS SPRATTUS) PACKED IN ICE, CLING FILM AND ALUMINUM FOIL AND STORED AT REFRIGERATED TEMPERATURE (0-4°C )

Comparative study of quality of King scallop (Pecten maximus) and Sprat (Spratus sprattus sprat’s) packed in ice, cling film and alluminium foil at 40C were conducted. Sensory (Inspection) and chemical changes (TVB-N, TMA-N and TMAO-N) were determined for a period of 16 days. In general, TMA-N increased and TMAO-N decreased progressively with increased storage time for both the species. However, significant differences (P<0.05) were observed in the concentrations of TMA-N and TVB-N in fish packed in alluminium foil and cling film compared to fish stored in ice. The biochemical results were in agreement with the sensory score. Ice packed fish showed better quality and longer shelf life compared to fish packed in either aluminum foil or cline film.
Multiple mean motion resonances in the HR 8799 planetary system

HR 8799 is a nearby star hosting at least four ~10 Jovian mass planets in wide orbits up to ~70au, detected through the direct, high-contrast infrared imaging. Large companions and debris disks reported interior to ~10au, and exterior to ~100au indicate massive protoplanetary disc in the past. The dynamical state of the HR 8799 system is not yet fully resolved, due to limited astrometric data covering tiny orbital arcs. We construct a new, orbital model of the HR 8799 system, assuming rapid migration of the planets after their formation in wider orbits. We found that the HR 8799 planets are likely involved in double Laplace resonance, 1e:2d:4c:8b MMR. Quasi-circular planetary orbits are coplanar with the stellar equator and inclined by ~25 degrees to the sky plane. This best-fit orbital configuration matches astrometry, debris disk models, and mass estimates from cooling models. The multiple MMR is stable for the age of the star ~160Myr, for at least 1 Gyr unless significant perturbations to the N-body dynamics are present. We predict four configurations with the fifth hypothetical innermost planet HR 8799f in ~9.7au, or ~7.5au orbit, extending the MMR chain to triple Laplace resonance 1f:2e:4d:8c:16b MMR or to the 1f:3e:6d:12c:24b MMR, respectively. Our findings may establish strong boundary conditions for the system formation and its early history.
Effect of In Ovo Vitamin C Injection against Mobile Phone Radiation on Post-Hatch Performance of Broiler Chicks

Simple Summary The use of mobile phones has become globally widespread and a dependance on them has also increased in recent years. Therefore, the harmful effects of the electromagnetic waves emitted by mobile phones and base stations on humans, animals, and other living organisms have been the subject of many studies. The current study aimed to investigate the effect of in ovo injection of vitamin C to reduce the harmful effects of electromagnetic waves emitted from mobile phones on chicken embryos. In this context, a total of 750 fertilized eggs were exposed to electromagnetic waves for 1050 min during the incubation period. On the 17th day of incubation, vitamin C was injected into the amnion sac of the embryos, and hatched chicks’ performance was observed for 5 weeks after hatching. In ovo vitamin C injection improved the post-hatch performance of chicks but increased the oxidative damage in broiler chicks. The results showed that in ovo vitamin C injection can be a tool to improve carcass weight, production efficiency, and mortality, eliminating the possible negative effects of exposure to electromagnetic waves in the embryonal period on performance. However, the results of the study need to be supported by further investigation. Abstract This study aimed to investigate the effect of in ovo injection of vitamin C to reduce the harmful effects of electromagnetic waves (EMWs) emitted from mobile phones on chicken embryos. In this study, a total of 750 fertilized eggs of Ross 308 were exposed to EMWs for 1050 min during the incubation period. On the 17th day of incubation, the eggs were divided into three groups and solutions were injected into the amnion sac of embryos. The chicks were housed separately in accordance with in ovo treatments for 5 wk after hatching. An in ovo vitamin C injection resulted in a lower hatching weight. The post-hatch mortality or production efficiency factor of birds in the in ovo vitamin C injection group and the intact egg group were comparable, and were better than that of the other negative control group. In ovo vitamin C injection in eggs subjected to EMWs significantly increased their body weight gain, carcass weight, abdominal fat weight, and AST levels, but reduced spleen weight and PON-1 levels. In conclusion, an in ovo vitamin C injection in eggs subject to mobile phone EMWs improved the post-hatch performance of chicks, but low PON and high AST activities indicate an increase in oxidative damage among broiler chicks.
Continuum Kinetic Simulations of Plasma Sheaths and Instabilities

A careful study of plasma-material interactions is essential to understand and improve the operation of devices where plasma contacts a wall. Key contributions of this work include (i) novel continuum kinetic algorithms with novel boundary conditions that directly discretize the Vlasov/Boltzmann equation using the discontinuous Galerkin method, (ii) fundamental studies of a plasma sheath physics with collisions, ionization, and physics-based wall emission, and (iii) theoretical and numerical studies of the linear growth and nonlinear saturation of the kinetic Weibel instability, including its role in plasma sheaths. The continuum kinetic algorithm has been shown to compare well with theoretical predictions of Landau damping of Langmuir waves and the two-stream instability. Benchmarks are also performed using the electromagnetic Weibel instability and excellent agreement is found between theory and simulation. The role of the electric field is significant during nonlinear saturation of the Weibel instability, which was not noted in previous studies. A focus is put on understanding plasma sheath physics which is essential for studying plasma-material interactions. Initial simulations are performed using a collisionless model to match classical sheath theory and the Bohm criterion. A collision operator and volumetric physics-based source terms are introduced and effects of heat flux are briefly discussed. Novel physics-based boundary conditions are developed and included in a general manner with the continuum kinetic algorithm for bounded plasma simulations. These are the first continuum kinetic simulations using self-consistent, wall emission boundary conditions with broad applicability across a variety of regimes.
PRIMUS: ONE- AND TWO-HALO GALACTIC CONFORMITY AT 0.2 < z < 1

We test for galactic conformity at to a projected distance of 5 Mpc using spectroscopic redshifts from the PRism MUlti-object Survey (PRIMUS). Our sample consists of ∼60,000 galaxies in five separate fields covering a total of ∼5.5 square degrees, which allows us to account for cosmic variance. We identify star-forming and quiescent “isolated primary” (i.e., central) galaxies using isolation criteria and cuts in specific star formation rate. We match the redshift and stellar mass distributions of these samples to control for correlations between quiescent fraction and redshift and stellar mass. We detect a significant (>3σ) one-halo conformity signal, or an excess of star-forming neighbors around star-forming central galaxies, of ∼5% on scales of 0–1 Mpc and a 2. 5σ two-halo signal of ∼1% on scales of 1–3 Mpc. These signals are weaker than those detected in the Sloan Digital Sky Survey and are consistent with galactic conformity being the result of large-scale tidal fields and reflecting assembly bias. We also measure the star-forming fraction of central galaxies at fixed stellar mass as a function of large-scale environment and find that central galaxies are more likely to be quenched in overdense environments, independent of stellar mass. However, we find that environment does not affect the star formation efficiency of central galaxies, as long as they are forming stars. We test for redshift and stellar mass dependence of the conformity signal within our sample and show that large volumes and multiple fields are required at intermediate redshift to adequately account for cosmic variance.
Towards a census of the Galactic anticentre star clusters – III. Tracing the spiral structure in the outer disc

In this paper we investigate the nature of 27 star cluster candidates, most of them projected towards the Galactic anticentre. We derive fundamental parameters for 20 confirmed clusters, among these 7 are new identifications. Four of the remaining are uncertain cases that require deeper photometry to establish their nature, and 4 are probably field fluctuations. In addition, we provide a partial census of the open clusters towards the Galactic anticentre. We also include in this study some interesting objects outside the anticentre region, in the second and third Galactic quadrants, mainly in the Perseus and Outer arms. These clusters confirm the extension of the Outer arm along the third quadrant. We also point out that the embedded cluster FSR 486, at a distance of 7.2 +/- 1.3 kpc from de Sun, is projected on the line of sight of the Local Group irregular dwarf galaxy IC 10. Thus, part of the unusual properties of IC 10 may be explained by a Galactic contamination. We point out the importance of embedded clusters in tracing the spiral structure.
Role of FNDC5 gene polymorphism in patients with diabetic nephropathy

: A category of metabolic illnesses known as diabetes mellitus (DM) is characterized by levels of hyperglycemia that persist for an extended length of time. The primary underlying cause of Type 2 diabetes mellitus (DM) is insulin resistance, which may also be accompanied by substantially decreased insulin production. The long-term presence of hyperglycemia causes several problems, including diabetic nephropathy. White adipose tissue (WAT) and brown adipose tissue (BAT) are the two separate compartments that make up adipose tissue. BAT has a thermogenic activity and controls body temperature by dissipating energy through heat generation. It is believed that the browning of adipose tissue will increase insulin sensitivity and lessen weight gain. Muscle-adipose tissue cross-talk may be facilitated by irisin, a newly identified exercise-mediated myokine that controls energy metabolism by transforming white into brown fat. When the precursor plasma membrane protein fibronectin type III domain-containing protein 5 (FNDC5) is broken down, irisin is created and released into the bloodstream. In individuals with diabetic nephropathy and chronic kidney disease (CKD), irisin was discovered to be related to renal functioning. To identify variations in the incidence of diabetic nephropathy among diabetic patients, the role of FDNC5 genetic polymorphism and irisin expression in T2DM nephropathy is being studied
Water masers in bowshocks: Addressing the radiation pressure problem of massive star formation

Abstract Ejection activities in S255IR-SMA1 and AFGL 5142 were investigated by multi-epoch VLBI observations of 22 GHz water masers, tracing bowshocks leading collimated jets. The history of ejections, revealed by the 3D maser motions and supplemented by the literature, suggests that these massive stars formed by episodic accretion, inferred via the accretion-ejection connection. This contribution centers on the role of episodic accretion in overcoming the radiation pressure problem of massive star formation - with maser VLBI and single-dish observations providing essential observational tools.
The K-band luminosity functions of cluster galaxies

We derive the galaxy luminosity function in the $K_s$ band for galaxies in 24 clusters to provide a local reference for higher redshift studies and to analyse how and if the luminosity function varies according to environment and cluster properties. We use new, deep $K$ band imaging and match the photometry to available redshift information and to optical photometry from the SDSS or the UKST/POSS: $>80\%$ of the galaxies to $K \sim 14.5$ have measured redshifts. We derive composite luminosity functions, for the entire sample and for cluster subsamples . We consider the luminosity functions for red sequence and blue cloud galaxies. The full composite luminosity function has $K^*=12.79 \pm 0.14$ ($M_K=-24.81$) and $\alpha=-1.41 \pm 0.10$. We find that $K^*$ is largely unaffected by the environment but that the slope $\alpha$ increases towards lower mass clusters and clusters with Bautz-Morgan type $<$ II. The red sequence luminosity function seems to be approximately universal (within errors) in all environments: it has parameters $K^*=13.16 \pm 0.15$ ($M_K=-24.44$) and $\alpha=-1.00 \pm 0.12$ (for all galaxies). Blue galaxies do not show a good fit to a Schechter function, but the best values for its parameters are $K^*=13.51 \pm 0.41$ ($M_K=-24.09$) and $\alpha=-1.60 \pm 0.29$: we do not have enough statistics to consider environmental variations for these galaxies. We find some evidence that $K^*$ in clusters is brighter than in the field and $\alpha$ is steeper, but note this comparison is based (for the field) on 2MASS photometry, while our data are considerably deeper.