Miracle-dz/UniFAR-FTUs huggingface dataset:
The thermal Sunyaev–Zeldovich effect of primordial recombination radiation

It is well known that recombination radiation of primordial hydrogen-helium plasma leads to the distortions of the planckian spectrum shape of the cosmic microwave background radiation (CMB). We discuss the thermal Sunyaev-Zeldovich (SZ) effect with taking into account primordial recombination radiation (PRR). Since in the thermal SZ effect the redistribution of the photons depends on the derivatives of the spectrum, the value of relative correction to SZ effect due to PRR significantly higher than relative corrections due to PRR in the initial spectrum. Calculations of corrections to the thermal SZ effect due to PRR show that depending on the cluster parameters: 1) in the range of frequencies $\nu$ = 0.3 - 700 GHz where the cosmic microwave background (CMB) dominates and spectrum is very close to the planckian one the relative corrections due to PRR have an order of $10^{-9} - 10^{-6}$ of "pure" SZ effect (i.e. SZ effect for pure planckian spectrum). The difference of intensities of PRR coming from different directions (through intracluster and near intercluster medium) reaches values up to 22 mJy/ster at $\nu\simeq 337$ GHz (maximum in considered range). 2) In the range of frequencies $\nu$ = 700 - 5000 GHz where cosmic infrared background (CIB) becomes significant or even dominates the relative corrections due to PRR can reach $10^{-8}$ - $10^{-5}$ of "pure" SZ effect. Corresponding intensity difference reaches values up to 25 mJy/ster (at $\nu\simeq 1700$ GHz). In addition we suggest a modification of the method of electron gas temperature determination using corrections of the SZ effect due to PRR. Such modification allows one to simplify the determination of the cluster electron gas temperature in comparison with known methods.
TeV halos are everywhere: Prospects for new discoveries

Milagro and HAWC have detected extended TeV gamma-ray emission around nearby pulsar wind nebulae (PWNe). Building on these discoveries, Linden et al. [1] identified a new source class -- TeV halos -- powered by the interactions of high-energy electrons and positrons that have escaped from the PWN, but which remain trapped in a larger region where diffusion is inhibited compared to the interstellar medium. Many theoretical properties of TeV halos remain mysterious, but empirical arguments suggest that they are ubiquitous. The key to progress is finding more halos. We outline prospects for new discoveries and calculate their expectations and uncertainties. We predict, using models normalized to current data, that future HAWC and CTA observations will detect in total $\sim$50--240 TeV halos, though we note that multiple systematic uncertainties still exist. Further, the existing HESS source catalog could contain $\sim$10--50 TeV halos that are presently classified as unidentified sources or PWN candidates. We quantify the importance of these detections for new probes of the evolution of TeV halos, pulsar properties, and the sources of high-energy gamma rays and cosmic rays.
Adsorption by design: Tuning atom-graphene van der Waals interactions via mechanical strain

We aim to understand how the van der Waals force between neutral adatoms and a graphene layer is modified by uniaxial strain and electron correlation effects. A detailed analysis is presented for three atoms (He, H, and Na) and graphene strain ranging from weak to moderately strong. We show that the van der Waals potential can be significantly enhanced by strain, and present applications of our results to the problem of elastic scattering of atoms from graphene. In particular we find that quantum reflection can be significantly suppressed by strain, meaning that dissipative inelastic effects near the surface become of increased importance. Furthermore we introduce a method to independently estimate the Lennard-Jones parameters used in an effective model of He interacting with graphene, and determine how they depend on strain. At short distances, we find that strain tends to reduce the interaction strength by pushing the location of the adsorption potential minima to higher distances above the deformed graphene sheet. This opens up the exciting possibility of mechanically engineering an adsorption potential, with implications for the formation and observation of anisotropic low dimensional superfluid phases.
Robust doubly charged nodal lines and nodal surfaces in centrosymmetric systems

Weyl points in three spatial dimensions are characterized by a $\mathbb{Z}$-valued charge---the Chern number---which makes them stable against a wide range of perturbations. A set of Weyl points can mutually annihilate only if their net charge vanishes, a property we refer to as robustness. While nodal loops are usually not robust in this sense, it has recently been shown using homotopy arguments that in the centrosymmetric extension of the $\mathrm{AI}$ symmetry class they nevertheless develop a ${\mathbb{Z}}_{2}$ charge analogous to the Chern number. Nodal loops carrying a nontrivial value of this ${\mathbb{Z}}_{2}$ charge are robust, i.e., they can be gapped out only by a pairwise annihilation and not on their own. As this is an additional charge independent of the Berry $\ensuremath{\pi}$-phase flowing along the band degeneracy, such nodal loops are, in fact, doubly charged. In this manuscript, we generalize the homotopy discussion to the centrosymmetric extensions of all Atland-Zirnbauer classes. We develop a tailored mathematical framework dubbed the $\mathrm{AZ}+\mathcal{I}$ classification and show that in three spatial dimensions such robust and multiply charged nodes appear in four of such centrosymmetric extensions, namely, $\mathrm{AZ}+\mathcal{I}$ classes $\mathrm{CI}$ and $\mathrm{AI}$ lead to doubly charged nodal lines, while $\mathrm{D}$ and $\mathrm{BDI}$ support doubly charged nodal surfaces. We remark that no further crystalline symmetries apart from the spatial inversion are necessary for their stability. We provide a description of the corresponding topological charges, and develop simple tight-binding models of various semimetallic and superconducting phases that exhibit these nodes. We also indicate how the concept of robust and multiply charged nodes generalizes to other spatial dimensions.
The role of cholesterol metabolism in predicting clinical outcome of patients with severe COVID-19

Transcriptomic analysis conducted by us previously revealed upregulation of genes involved in low-density lipoprotein particle receptor (LDLR) activity pathway in lethal COVID-19. Last data suggested the possible role of extracellular vesicles and exomeres in COVID-19 pathogenesis. The aim of the present study was to retro-spectively evaluate parameters of cholesterol metabolism as possible predictors of fatal outcome of COVID-19. Blood from 39 patients with severe COVID-19 (the main cohort) were collected at the time of admission to the intensive care unit (ICU) (T1) and 7 days after admission to the ICU (T2). After 30 days patients were divided into two subgroups according to outcome-21 non-survivors and 18 survivors. 28 patients (13 non-survivors and 15 survivors) with severe COVID-19 were included as the replication cohort. The study demonstrated that plasma low- and high-density lipoprotein cholesterol levels (LDL-C and HDL-C) were decreased and CCL20/MIP3? , IL-10, IL-15, IL-27 concentrations were increased in non-survivors compared to controls in T1. STAB1 gene expression was higher in non-survivors than in survivors (p=0.017) in T2. The conjoint fraction of exomeres and LDL particles measured by dynamic light scattering (DLS) was decreased in non-survivors com-pared to survivors in both the main and replication cohorts. We first showed that change of exomeres fraction may be critical in fatal outcome of COVID-19.
Discovery of a Transiting Adolescent Sub-Neptune Exoplanet with K2

The role of stellar age in the measured properties and occurrence rates of exoplanets is not well understood. This is in part due to a paucity of known young planets and the uncertainties in age-dating for most exoplanet host stars. Exoplanets with well-constrained ages, particularly those which are young, are useful as benchmarks for studies aiming to constrain the evolutionary timescales relevant for planets. Such timescales may concern orbital migration, gravitational contraction, or atmospheric photoevaporation, among other mechanisms. Here we report the discovery of an adolescent transiting sub-Neptune from K2 photometry of the low-mass star EPIC 247267267. From multiple age indicators, we estimate the age of the star to be 120 Myr, with a 68% confidence interval of 100–760 Myr. The size of EPIC 247267267 b (RP = 2.8 ± 0.1 R⊕) combined with its youth make it an intriguing case study for photoevaporation models, which predict enhanced atmospheric mass loss during early evolutionary stages.
Collision and annihilation of relative equilibrium points around asteroids with a changing parameter

In this work, we investigate the bifurcations of relative equilibria in the gravitational potential of asteroids. A theorem concerning a conserved quantity, which is about the eigenvalues and number of relative equilibria, is presented and proved. The conserved quantity can restrict the number of non-degenerate equilibria in the gravitational potential of an asteroid. It is concluded that the number of non-degenerate equilibria in the gravitational field of an asteroid varies in pairs and is an odd number. In addition, the conserved quantity can also restrict the kinds of bifurcations of relative equilibria in the gravitational potential of an asteroid when the parameter varies. Furthermore, studies have shown that there exist transcritical bifurcations, quasi-transcritical bifurcations, saddle-node bifurcations, saddle-saddle bifurcations, binary saddle-node bifurcations, supercritical pitchfork bifurcations, and subcritical pitchfork bifurcations for the relative equilibria in the gravitational potential of asteroids. It is found that for the asteroid 216 Kleopatra, when the rotation period varies as a parameter, the number of relative equilibria changes from 7 to 5 to 3 to 1, and the bifurcations for the relative equilibria are saddle-node bifurcations and saddle-saddle bifurcations.
Metallicity gradients of disc stars for a cosmologically simulated galaxy

We analyse for the first time the radial abundance gradients of the disc stars of a disc galaxy simulated with our three-dimensional, fully cosmological chemodynamical galaxy evolution code GCD+. We study how [Fe/H], [N/O], [O/Fe], [Mg/Fe] and [Si/Fe] vary with galactocentric radius. For the young stars of the disc, we found a negative slope for [Fe/H] and [N/O] but a positive [O/Fe], [Mg/Fe] and [Si/Fe] slope with radius. By analysing the star formation rate at different radii, we found that the simulated disc contains a greater fraction of young stars in the outer regions, while the old stars tend to be concentrated in the inner parts of the disc. This can explain the positive [alpha/Fe] gradient as well as the negative [N/O] gradient with radius. This radial trend is a natural outcome of an inside-out formation of the disc, regardless of its size and can thus explain the recently observed positive [alpha/Fe] gradients in the Milky Way disc open clusters.
QUANTIFYING DISTRIBUTIONS OF THE LYMAN CONTINUUM ESCAPE FRACTION

Simulations have indicated that most of the escaped Lyman continuum (LyC) photons escape through a minority of solid angles with near complete transparency, with the remaining majority of the solid angles largely opaque, resulting in a very broad and skewed probability distribution function (PDF) of the escape fraction when viewed at different angles. Thus, the escape fraction of LyC photons of a galaxy observed along a line of sight merely represents the properties of the interstellar medium along that line of sight, which may be an ill-representation of the true escape fraction of the galaxy averaged over its full sky. Here we study how LyC photons escape from galaxies at z = 4 − 6 ? > , utilizing high-resolution large-scale cosmological radiation-hydrodynamic simulations. We compute the PDF of the mean escape fraction ( ⟨ f esc , 1 D ⟩ ? > ) averaged over mock observational samples, as a function of the sample size, compared to the true mean (if an infinite sample size is used). We find that, when the sample size is small, the apparent mean skews to the low end. For example, for a true mean of 6.7%, an observational sample of (2,10,50) galaxies at z = 4 would have have a 2.5% probability of obtaining the sample mean lower than f esc , 1 D = ? > (0.007%, 1.8%, 4.1%) and a 2.5% probability of obtaining the sample mean greater than (43%, 18%, 11%). Our simulations suggest that at least ∼100 galaxies should be stacked in order to constrain the true escape fraction within 20% uncertainty.
Testing the Etherington distance duality relation at higher redshifts: Combined radio quasar and gravitational wave data

In this paper we analyse the implications of the latest cosmological data sets to test the Etherington's distance duality relation (DDR), which connects the luminosity distance $D_L$ and angular diameter distance $D_A$ at the same redshift. For $D_L$ we consider the simulated data of gravitational waves from the third-generation gravitational wave detector (the Einstein Telescope, ET), which can be considered as standard candles (or standard siren), while the angular diameter distances $D_A$ are derived from the newly-compiled sample of compact radio quasars observed by very-long-baseline interferometry (VLBI), which represents a type of new cosmological standard ruler. Alleviating the absorption and scattering effects of dust in the Universe, this will create a valuable opportunity to directly test DDR at much higher precision with the combination of gravitational wave (GW) and electromagnetic (EM) signals. Our results show that, with the combination of the current radio quasar observations, the duality-distance relation can be verified at the precision of $10^{-2}$. Moreover, the Einstein Telescope ET would produce more robust constraints on the validity of such distance duality relation (at the precision of $10^{-3}$), with a larger sample of compact milliarcsecond radio quasars detected in future VLBI surveys.
Cognitive functions and symptoms predicting later use of psychiatric services following mild traumatic brain injury in school-age

ABSTRACT Objective To investigate whether neuropsychological test performance or presence of some specific injury symptoms at 1–3 months following pediatric mild traumatic brain injury (mTBI) can help to identify the children at risk for developing post-traumatic psychiatric symptoms. Methods Data from 120 children and adolescents aged 7–15 years, treated at Turku University Hospital between 2010 and 2016 due to mTBI, and who had undergone neuropsychological evaluation at 1–3 months following injury, were enrolled from the hospital records. Neuropsychological test performancesand injury symptom reports were retrospectively retrieved from the patient files. Results Slow information processing speed (p = 0.044), emotion regulation deficit (p = 0.014), impulsivity (p = 0.013), verbal processing difficulties (p = 0.042) and headache (p = 0.026) were independent predictors for having later contact in psychiatric care. Conclusions Neuropsychological examination containing measure of information processing speed, injury symptom interview, and parental questionnaires on behavioural issues of the child at 1–3 months following mTBI seems to be useful in detecting children with risk for post traumatic psychiatric symptoms. Targeted support and guidance for this group of children and adolescents and their families are recommended to prevent the development of an unfavorable psychosocial outcome.
Genomic Assembly of Clinical Candida glabrata (Nakaseomyces glabrata) Isolates Reveals within-Species Structural Plasticity and Association with In Vitro Antifungal Susceptibility

The human pathogen Candida glabrata has become a global threat to human health, with infections characterized by high mortality and multidrug resistance. We have obtained nine fully assembled genomes from clinical isolates through a combination of short- and long-read sequencing approaches. ABSTRACT The opportunistic human pathogen Candida glabrata has become an increasingly important threat to human health, with infections globally characterized by high mortality rates and multidrug resistance. To face this threat, more efficient diagnostic and therapeutic approaches are required, underpinning research to help define the intraspecies epidemiology, genetic variability, and therefore, diagnostic and therapeutic target stability. Previous comparative genetics studies conducted on limited numbers of strains only revealed partial resolution of chromosomal settings. In this study, by combining short- and long-read genome sequencing, phenotypic characterization, and comparative genomics over a large set of strains, we detected strict relationships between large chromosomal rearrangements and phylogenetic clades, genes subjected to different selective pressures, and new sets of genes associated with resistance to antifungals. Overall, these results not only provide a fundamental contribution to our knowledge of C. glabrata evolution and epidemiology but may also lay the foundations for the future development of tailored therapeutic approaches. IMPORTANCE The human pathogen Candida glabrata has become a global threat to human health, with infections characterized by high mortality and multidrug resistance. We have obtained nine fully assembled genomes from clinical isolates through a combination of short- and long-read sequencing approaches. The quality and completeness of such genomes and their subsequent comparison to the broadest set of genomes so far allowed us to pinpoint chromosomal rearrangements in several genomes and detect phylogenetic clades that were not associated with geographic location or isolation source. We identified a new set of genes associated with resistance to antifungals coding for adhesin or adhesin-like proteins, suggesting C. glabrata resists antifungals by forming aggregates or adhering to the host tissue. These results, which provide a fundamental contribution to our knowledge of C. glabrata evolution and epidemiology, may initiate the development of precision medicine interventions for patients with suspected or proven invasive fungal infections.
Towards a new paradigm for heavy-light meson spectroscopy

Understanding the hadron spectrum is one of the premier challenges in particle physics. For a long time, the quark model has served as an ordering scheme and brought systematics into the hadron zoo. However, many new hadrons that were observed since 2003, including the lowest-lying positive-parity charm-strange mesons ${D_{s0}^*(2317)}$ and ${D_{s1}(2460)}$, do not conform with quark model expectations. Various modifications to the quark model and alternative approaches have been proposed ever since to explain their low masses and decay properties. Here, we demonstrate that if the lightest scalar and axial-vector open heavy-flavor states, amongst them the ${D_{s0}^*(2317)}$ and the ${D_{s1}(2460)}$, are assumed to owe their existence to the nonperturbative dynamics of Goldstone-Boson scattering off ${D}$ and ${D^*}$ mesons, various puzzles in the spectrum of the charm mesons find a natural resolution. Most importantly the ordering of the lightest strange and nonstrange scalars becomes natural. Furthermore it is demonstrated that the well constrained amplitudes for Goldstone-Boson scattering off charm mesons are fully consistent with recent high quality data on the ${B^-\to D^+\pi^-\pi^- }$ final states provided by the LHCb experiment. This implies that the lowest quark-model positive-parity charm mesons, together with their bottom cousins, if realized in nature, do not form the ground-state multiplet. This is similar to the pattern that has been established for the scalar mesons made from light up, down and strange quarks, where the lowest multiplet is considered to be made of states not described by the quark model. In a broader view, the hadron spectrum must be viewed as more than a collection of quark model states.
Diffuse Ionized Gas in Spiral Galaxies and the Disk-Halo Interaction

Thick layers of warm, low density ionized hydrogen (i.e. , the warm ionized medium or WIM) in spiral galaxies provide direct evidence for an interaction between the disk and halo. The wide-spread ionization implies that a significant fraction of the Lyman continuum photons from O stars, produced primarily in isolated star forming regions near the midplane and often surrounded by opaque clouds of neutral hydrogen, is somehow able to propagate large distances through the disk and into the halo. Moreover, even though O stars are the source of the ionization, the temperature and ionization state of the WIM differ significantly from what is observed in the classical O star H ii regions. Therefore, the existence of the WIM and observations of its properties provide information about the structure of the interstellar medium and the transport of energy away from the midplane as well as place significant constraints on models.
Are we seeing accretion flows in a 250kpc-sized Ly-alpha halo at z=3?

Using MUSE on the ESO-VLT, we obtained a 4 hour exposure of the z=3.12 radio galaxy MRC0316-257. We detect features down to ~10^-19 erg/s/cm^2/arcsec^2 with the highest surface brightness regions reaching more than a factor of 100 higher. We find Ly-alpha emission out to ~250 kpc in projection from the active galactic nucleus (AGN). The emission shows arc-like morphologies arising at 150-250 kpc from the nucleus in projection with the connected filamentary structures reaching down into the circum-nuclear region. The most distant arc is offset by 700 km/s relative to circum-nuclear HeII 1640 emission, which we assume to be at the systemic velocity. As we probe emission closer to the nucleus, the filamentary emission narrows in projection on the sky, the relative velocity decreases to ~250 km/s, and line full-width at half maximum range from 300-700 km/s. From UV line ratios, the emission on scales of 10s of kpc from the nucleus along a wide angle in the direction of the radio jets is clearly excited by the radio jets and ionizing radiation of the AGN. Assuming ionization equilibrium, the more extended emission outside of the axis of the jet direction would require 100% or more illumination to explain the observed surface brightness. High speed (>300 km/s) shocks into rare gas would provide sufficiently high surface brightness. We discuss the possibility that the arcs of Ly-alpha emission represent accretion shocks and the filamentary emission represent gas flows into the halo, and compare our results with gas accretion simulations.