Miracle-dz/UniFAR-FTUs huggingface dataset:
On the structure of hot gas in haloes: implications for the LX-TX relation and missing baryons

We present one-dimensional models of the hot gas in dark matter haloes, which both predict the existence of cool cores and explain their structure. Our models are directly applicable to semi-analytic models of galaxy formation. We have previously argued that filaments of cold (∼104 K) gas condense out of the intracluster medium (ICM) in hydrostatic and thermal equilibrium when the ratio of the thermal instability time-scale to the free-fall time tTI/tff falls below 5–10. This criterion corresponds to an upper limit on the density of the ICM and motivates a model in which a density core forms wherever tTI/tff ≲ 10. Consistent with observations and numerical simulations, this model predicts larger and more tenuous cores for lower mass haloes – while the core density in a cluster may be as large as ∼0.1 cm−3, the core density in the Galactic halo should not exceed ∼10−4 cm−3. We can also explain the large densities in smaller mass haloes (galactic ‘coronae’) if we include the contribution of the central galaxy to the gravitational potential. Our models produce a favourable match to the observational X-ray luminosity–temperature (LX–TX) relation. For halo masses ≲1013 M⊙ the core size approaches the virial radius. Thus, most of the baryons in such haloes cannot be in the hot ICM, but either in the form of stars or in the form of hot gas beyond the virial radius. Because of the smaller mass in the ICM and much larger mass available for star formation, the majority of the baryons in low-mass haloes (≲1013 M⊙) can be expelled beyond the virial radius due to supernova feedback. This can account for the baryons ‘missing’ from low-mass haloes, such as the Galactic halo.
Size and albedo distributions of asteroids in cometary orbits using WISE data

We study the distributions of effective diameter ($D$), beaming parameter ($\eta$), and visible geometric albedo ($p_V$) of asteroids in cometry orbits (ACOs) populations, derived from NASA's Wide-field Infrared Explorer (WISE) observations, and compare these with the same, independently determined properties of the comets. The near-Earth asteroid thermal model (NEATM) is used to compute the $D$, $p_V$ and $\eta$. We obtained $D$ and $p_V$ for 49 ACOs in Jupiter family cometary orbits (JF-ACOs) and 16 ACOs in Halley-type orbits (Damocloids). We also obtained $\eta$ for 45 of them. All but three JF-ACOs (95% of the sample) present a low albedo compatible with a cometary origin. The $p_V$ and $\eta$ distributions of both ACO populations are very similar. For the entire sample of ACOs, the mean geometric albedo is $\bar{p_V} = 0.05 \pm 0.02$, ($\bar{p_V} = 0.05 \pm 0.01$ and $\bar{p_V} =0.05 \pm 0.02$ for JF-ACOs and Damocloids, respectively) compatible with a narrow albedo distribution similar to that of the Jupiter family comets (JFCs), with a $\bar{p_V} \sim 0.04$. The $\bar{\eta} =1.0 \pm 0.2$. We find no correlations between $D$, $p_V$ , or $\eta$. We compare the cumulative size distribution (CSD) of ACOs, Centaurs, and JFCs. Although the Centaur sample contains larger objects, the linear parts in their log-log plot of the CSDs presents a similar cumulative exponent ($\beta = 1.85 \pm 0.30$ and $1.76 \pm 0.35$, respectively). The CSD for Damocloids presents a much shallower exponent $\beta = 0.89 \pm 0.17$. The CSD for JF-ACOs is shallower and shifted towards larger diameters with respect to the CSD of active JFCs, which suggests that the mantling process has a size dependency whereby large comets tend to reach an inactive stage faster than small ones. Finally, the population of JF-ACOs is comparable in number that of JFCs, although there are more tens-km JF-ACOs than JFCs.
Are Internal Capital Markets Ex Post Efficient?

Internal capital markets enable conglomerates to allocate capital to segments throughout the enterprise. Prior literature provides evidence that internal capital markets efficiently allocate capital based predominantly on group member prior performance, consistent with the “winner picking” hypothesis. However, existing research has not examined the critical question of how these “winners” perform subsequent to receiving internal capital—that is, do winners keep winning? We extend the literature by providing empirical evidence on whether or not internal capital markets are ex post efficient. We find, in contrast to mean reversion, that winners continue their relatively high performance. Our study contributes to the literature examining the efficiency of internal capital markets and the conglomerate discount, as well as the literature specifically examining capital allocation in financial firms.
The discrepancy in the mid-infrared continuum and the features of polycyclic aromatic hydrocarbons for Spitzer and Herschel SWIRE-field galaxies

On the basis of observations by Spitzer and Herschel, we present and analyse the correlations between various monochromatic infrared (IR) luminosities for star-forming galaxies, selected from two northern Spitzer Wide-area InfraRed Extragalactic Survey (SWIRE) fields. The 24- and 70 micron luminosities (L[24] and L[70]), which are dominated by the continuum of very small grains (VSGs) and warm dust in thermal equilibrium, respectively, correlate tightly with ongoing star formation. The contribution from cool dust excited by evolved stars also increases as the wavelength increases in the far-infrared (FIR) wavelength range. The spectral features of ionized polycyclic aromatic hydrocarbons (PAHs) around rest-frame 8 micron are excited by the moderated radiation field related to evolved stars as well, rather than by the intensive radiation field related to young stars. Even though the carriers of PAHs could be treated as types of VSG with a smaller scale, the radiation condition between PAHs and classic VSGs seems to be significantly different. The formulae to calculate the total infrared luminosity L[TIR] using L[8(dust)] and L[24] are re-scaled and we find that the L[8(dust)] (L[24]) formula likely underestimates (overestimates) L[TIR] for galaxies with unusual current star formation activity.
The DarkStars code: a publicly available dark stellar evolution package

We announce the public release of the 'dark' stellar evolution code DarkStars. The code simultaneously solves the equations of WIMP capture and annihilation in a star with those of stellar evolution assuming approximate hydrostatic equilibrium. DarkStars includes the most extensive WIMP microphysics of any dark evolution code to date. The code employs detailed treatments of the capture process from a range of WIMP velocity distributions, as well as composite WIMP distribution and conductive energy transport schemes based on the WIMP mean-free path in the star. We give a brief description of the input physics and practical usage of the code, as well as examples of its application to dark stars at the Galactic centre.
Kinesthesia and Temporal Experience: On the ‘Knitting and Unknitting’ Process of Bodily Subjectivity in Schizophrenia

This paper proposes a phenomenological hypothesis that psychosis entails a disturbance of the two-fold process of the indication function of kinesthesia and the presentification function of touch that affects the constitution of bodily subjectivity. Recent functional connectivity studies showed that the increased synchrony between the right anterior insula and the default mode network are associated with psychosis. This association is proposed to be correlated with the disrupted dynamics between the pre-reflective and reflective temporal experience in psychotic patients. The paper first examines the dynamic nature of kinesthesia and the influence touch and vision exert on it, and then the reciprocal influence with temporal experience focusing on the body’s cyclic sense of temporality and its impact on physiology and phenomenology. Affectivity and self-affection are considered in their basic bodily expressions mainly through the concepts of responsivity and receptivity. The overall constitutive processes referred to throughout the article are proposed as a roadmap to develop body-based therapeutic work.
The Early Growth of the First Black Holes

Abstract With detections of quasars powered by increasingly massive black holes at increasingly early times in cosmic history over the past decade, there has been correspondingly rapid progress made on the theory of early black hole formation and growth. Here, we review the emerging picture of how the first massive black holes formed from the primordial gas and then grew to supermassive scales. We discuss the initial conditions for the formation of the progenitors of these seed black holes, the factors dictating the initial masses with which they form, and their initial stages of growth via accretion, which may occur at super-Eddington rates. Finally, we briefly discuss how these results connect to large-scale simulations of the growth of supermassive black holes in the first billion years after the Big Bang.
On the Ubiquity and Stellar Luminosity Dependence of Exocometary CO Gas: Detection around M Dwarf TWA 7

Millimeter observations of CO gas in planetesimal belts show a high detection rate around A stars, but few detections for later type stars. We present the first CO detection in a planetesimal belt around an M star, TWA 7. The optically thin CO (J = 3–2) emission is colocated with previously identified dust emission from the belt, and the emission velocity structure is consistent with Keplerian rotation around the central star. The detected CO is not well shielded against photodissociation, and must thus be continuously replenished by gas release from exocomets within the belt. We analyze in detail the process of exocometary gas release and destruction around young M dwarfs and how this process compares to earlier type stars. Taking these differences into account, we find that CO generation through exocometary gas release naturally explains the increasing CO detection rates with stellar luminosity, mostly because the CO production rate from the collisional cascade is directly proportional to stellar luminosity. More luminous stars will therefore on average host more massive (and hence more easily detectable) exocometary CO disks, leading to the higher detection rates observed. The current CO detection rates are consistent with a ubiquitous release of exocometary gas in planetesimal belts, independent of spectral type.
The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package

The Astropy Project supports and fosters the development of open-source and openly developed Python packages that provide commonly needed functionality to the astronomical community. A key element of the Astropy Project is the core package astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package, as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of interoperable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy Project.
Molecular environment, reverberation, and radiation from the pulsar wind nebula in CTA 1

We estimate the molecular mass around CTA 1 using data from Planck and the Harvard CO survey. We observe that the molecular mass in the vicinity of the complex is not enough to explain the TeV emission observed by VERITAS, even under favorable assumptions for the cosmic-ray acceleration properties of the supernova remnant. This supports the idea that the TeV emission comes from the PWN. Here, we model the spectrum of the PWN at possible different stages of its evolution, including both the dynamics of the PWN and the SNR and their interaction via the reverse shock. We have included in the model the energy lost via radiation by particles and the particles escape when computing the pressure produced by the gas. This leads to an evolving energy partition, since for the same instantaneous sharing of the injection of energy provided by the rotational power, the field and the particles are affected differently by radiation and losses. We present the model, and study in detail how the spectrum of a canonical isolated PWN is affected during compression and re-expansion and how this may impact on the CTA 1 case. By exploring the phase-space of parameters that lead to radii in agreement with those observed, we then analyze different situations that might represent the current stage of the CTA 1 PWN, and discuss caveats and requirements of each one.
The 2008 May burst activation of SGR 1627-41

In 2008 May, the soft gamma-ray repeater (SGR) SGR 1627-41 resumed its bursting activity after nearly a decade of quiescence. After detection of a bright burst, Swift pointed its X-ray telescope in the direction of the source in less than five hours and followed it for over five weeks. In this Letter, we present an analysis of the data from these Swift observations and an XMM-Newton one performed when SGR 1627-41 was still in a quiescent state. The analysis of the bursts detected with Swift/Burst Alert Telescope shows that their temporal and spectral properties are similar to those found in previous observations of SGR 1627-41 and other SGRs. The maximum peak luminosity of the bursts was similar to 2 x 10(41) erg s(-1). Our data show that the outburst was accompanied by a fast flux enhancement and by a hardening of the spectrum with respect to the persistent emission.
WHERE ARE THE LOW-MASS POPULATION III STARS?

We study the number and the distribution of low-mass Population III (Pop III) stars in the Milky Way. In our numerical model, hierarchical formation of dark matter minihalos and Milky-Way-sized halos are followed by a high-resolution cosmological simulation. We model the Pop III formation in H2 cooling minihalos without metal under UV radiation of the Lyman–Werner bands. Assuming a Kroupa initial mass function (IMF) from 0.15 to 1.0 M⊙ for low-mass Pop III stars, as a working hypothesis, we try to constrain the theoretical models in reverse by current and future observations. We find that the survivors tend to concentrate on the center of halo and subhalos. We also evaluate the observability of Pop III survivors in the Milky Way and dwarf galaxies, and constraints on the number of Pop III survivors per minihalo. The higher latitude fields require lower sample sizes because of the high number density of stars in the galactic disk, the required sample sizes are comparable in the high- and middle-latitude fields by photometrically selecting low-metallicity stars with optimized narrow-band filters, and the required number of dwarf galaxies to find one Pop III survivor is less than 10 at <100 kpc for the tip of red giant stars. Provided that available observations have not detected any survivors, the formation models of low-mass Pop III stars with more than 10 stars per minihalo are already excluded. Furthermore, we discuss the way to constrain the IMF of Pop III stars at a high mass range of ≳10 M⊙.
The Role of Angiotensinogen rs699 in Diabetic Nephropathy Among Type 2 Diabetes Mellitus Patients with Uncontrolled Postprandial Glucose Levels

Diabetic Nephropathy (DN) is the most common complication of Type 2 Diabetes Mellitus (T2DM), leading to the highest mortality rate of DM complications. However, its etiology is still questionable. Hyperglycemia, hypertension, and particular genetic susceptibility are associated with DN. Not all patients with uncontrolled hyperglycemia suffer DN. Thus, genetic susceptibility may be a risk factor for DN. The genetic variant of angiotensinogen rs699 is known to be associated with the risk of DN with inconsistent results between ethnicities. This study aims to reveal the correlation between the AGT rs699 with the incidence of diabetic nephropathy among type-2 diabetes mellitus patients with uncontrolled postprandial glucose levels in the Jambi Malay ethnicity. This study was observational analytic research with a cross-sectional design. It used 48 DNA samples from type-2 diabetes mellitus patients with uncontrolled postprandial glucose levels. The authors took 24 DNA samples from patients with DN and 24 without DN (as a control group). The genotyping method used ARMS-PCR specific for AGT rs699. Subjects with the CT genotype had a lower risk for diabetic nephropathy than the CC genotype, but it was not statistically significant (p=0.247; OR=0.508; 95%CI=0.160-1.607). In addition, subjects with the T allele (p=0.331; OR=0.621; 95%CI-0.237-1.630) had a lower risk for diabetic nephropathy than the C allele, but it was not statistically significant. In conclusion, Angiotensinogen rs699 is not a risk factor for diabetic nephropathy among type-2 diabetes mellitus patients with uncontrolled postprandial glucose levels in the Jambi Malay ethnicity.
PROBING THE SOLAR WIND ACCELERATION REGION WITH THE SUN-GRAZING COMET C/2002 S2

Comet C/2002 S2, a member of the Kreutz family of sungrazing comets, was discovered in white-light images of the Large Angle and Spectromeric Coronagraph Experiment coronagraph on the Solar and Heliospheric Observatory (SOHO) on 2002 September 18 and observed in H i Lyα emission by the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) instrument at four different heights as it approached the Sun. The H i Lyα line profiles detected by UVCS are analyzed to determine the spectral parameters: line intensity, width, and Doppler shift with respect to the coronal background. Two-dimensional comet images of these parameters are reconstructed at the different heights. A novel aspect of the observations of this sungrazing comet data is that, whereas the emission from most of the tail is blueshifted, that along one edge of the tail is redshifted. We attribute these shifts to a combination of solar wind speed and interaction with the magnetic field. In order to use the comet to probe the density, temperature, and speed of the corona and solar wind through which it passes, as well as to determine the outgassing rate of the comet, we develop a Monte Carlo simulation of the H i Lyα emission of a comet moving through a coronal plasma. From the outgassing rate, we estimate a nucleus diameter of about 9 m. This rate steadily increases as the comet approaches the Sun, while the optical brightness decreases by more than a factor of 10 and suddenly recovers. This indicates that the optical brightness is determined by the lifetimes of the grains, sodium atoms, and molecules produced by the comet.
CHROMIUM-RICH Zn–Cr ALLOYS: ELECTROCHEMICAL DEPOSITION, STRUCTURE AND CORROSION RESISTANCE

In this work we have done an experimental study of Zinc-Chromium composite coatings. For this the influence of the Chromium concentration was the principal object in order to improve the resistance of the corrosion of the coatings, which has been made by electroplating on steel substrates previously treated, have been studied by several characterization methods, as the Xray diffraction, micro-hardness measurement and scanning electron microscopy (SEM), protection against corrosion properties studied by potentiodynamic polarization measurements (Tafel) . the addition of Cr in the Zn alloys increases the micro-hardness, XRD and SEM results and identify any coatings Zn-Cr alloy composition reveals that zinc phase.
The catalytic effects of monopoles in QCD

We want to find indications that magnetic monopoles in quantum chromodynamics (QCD) exist; therefore, we introduce a monopole and anti-monopole pair in the QCD vacuum of the quenched SU(3) by applying the monopole creation operator on the vacuum. We investigate the catalytic effects of monopoles on chiral symmetry breaking using the Dirac operator of the overlap fermions that preserves the chiral symmetry in the lattice gauge theory. First, we confirm that the eigenstate of the monopole creation operator becomes the coherent state and that the monopole creation operator makes monopoles and anti-monopoles in the QCD vacuum. We have found the catalytic effects of monopoles on observables by varying the values of the magnetic charges of the additional monopole and anti-monopole as follows: (i) The decay constants of the pseudoscalar increase. (ii) The values of the chiral condensate, defined as a negative number, decrease. (iii) The light quarks and the pseudoscalar mesons become heavy. The catalytic effects of monopoles on the partial decay width and the lifetime of the charged pion are estimated using the numerical results of the pion decay constant and the pion mass. (iv) The decay width of the charged pion becomes wider than the experimental result, and the lifetime of the charged pion becomes shorter than the experimental result. These are the catalytic effects of monopoles in QCD, which we find in this research.
Clinical relevance of IL-6 and lactate levels within 24 hours of ICU admission of COVID–19 patients in predicting mortality rate

Background & objective: Patients with COVID-19 have Acute Respiratory Distress Syndrome (ARDS) which progresses to lung edema and disorders of the liver, kidneys and heart associated with cytokine storms, which are the body's immune response to SARS-CoV-2. SARS-CoV-2 patients showed clinical neutrophilia, increased D-Dimer and increased IL-6. In addition, increased lactate dehydrogenase and increased aminotransferase are often found. This study aimed to analyze the clinical relevance of increased IL-6 and lactate in the first 24 hours of ICU-admission of COVID-19 patients in predicting mortality rate. Methodology: This study was a retrospective cohort design. The study was conducted in the Intensive Care Unit (ICU) of Dr. Moewardi Surakarta Hospital. The study was conducted by tracing the medical records of COVID-19 patients treated in the ICU of Dr. Moewardi Surakarta Hospital during the period of March 1, 2020 to March 31, 2021 that met the admission criteria. The patient's mortality assessment is seen as the patient's condition for a maximum of 30 days after discharge from the hospital. Results: Variables that meet the regression model are the lactate levels (OR = 3,143; P = 0.064) as well as the IL-6 levels (OR = 25.41; p<0.001). AUC score of 86.9% with significance of < 0.001. IL-6 levels and lactate levels in the study can be used as predictors of mortality rates with 95.7% sensitivity and 60% specificity. Lactate levels in COVID-19 cases in severe cases can be related to lung damage and tissue damage. Lactate levels have also been recognized as a marker of poor prognosis in patients with COVID-19. IL-6 as a predictor of mortality risk has been recognized and the administration of IL-6 inhibitors in COVID-19 patients may lower the risk of mortality. Conclusion: Raised IL-6 and lactate levels in this study can be a predictor of the mortality rate of COVID-19 patients within 24 hours of ICU-admission. Citation: Nugroho A, Hapsari PP, Santoso SB, Permana SA, Sitompul H. Clinical relevance of IL-6 and lactate within 24 hours of ICU-admission of COVID 19 patient in predicting mortality rate. Anaesth. pain intensive care 2022;26(5):689−694. DOI: 10.35975/apic.v26i5. 2032