Miracle-dz/UniFAR-FTUs huggingface dataset:
DISCOVERY OF A CLOSE SUBSTELLAR COMPANION TO THE HOT SUBDWARF STAR HD 149382—THE DECISIVE INFLUENCE OF SUBSTELLAR OBJECTS ON LATE STELLAR EVOLUTION

Substellar objects, like planets and brown dwarfs orbiting stars, are by-products of the star formation process. The evolution of their host stars may have an enormous impact on these small companions. Vice versa a planet might also influence stellar evolution as has recently been argued. Here, we report the discovery of an 8−23 Jupiter-mass substellar object orbiting the hot subdwarf HD 149382 in 2.391 d at a distance of only about five solar radii. Obviously, the companion must have survived engulfment in the red giant envelope. Moreover, the substellar companion has triggered envelope ejection and enabled the sdB star to form. Hot subdwarf stars have been identified as the sources of the unexpected ultraviolet (UV) emission in elliptical galaxies, but the formation of these stars is not fully understood. Being the brightest star of its class, HD 149382 offers the best conditions to detect the substellar companion. Hence, undisclosed substellar companions offer a natural solution for the long-standing formation problem of apparently single hot subdwarf stars. Planets and brown dwarfs may therefore alter the evolution of old stellar populations and may also significantly affect the UV emission of elliptical galaxies.
THE FAR-INFRARED, UV, AND MOLECULAR GAS RELATION IN GALAXIES UP TO z = 2.5

We use the infrared excess (IRX) FIR/UV luminosity ratio to study the relation between the effective UV attenuation (AIRX) and the UV spectral slope (β) in a sample of 450 1 < z < 2.5 galaxies. The FIR data are from very deep Herschel observations in the GOODS fields that allow us to detect galaxies with star formation rates (SFRs) typical of galaxies with log(M*) > 9.3. Thus, we are able to study galaxies on and even below the main SFR–stellar mass relation (main sequence). We find that main-sequence galaxies form a tight sequence in the IRX–β plane, which has a flatter slope than commonly used relations. This slope favors a Small-Magellanic-Cloud-like UV extinction curve, though the interpretation is model dependent. The scatter in the AIRX–β plane correlates with the position of the galaxies in the SFR–M* plane. Using a smaller sample of galaxies with CO gas masses, we study the relation between the UV attenuation and the molecular gas content. We find a very tight relation between the scatter in the IRX–β plane and the specific attenuation SA, a quantity that represents the attenuation contributed by the molecular gas mass per young star. SA is sensitive to both the geometrical arrangement of stars and dust and to the compactness of the star-forming regions. We use this empirical relation to derive a method for estimating molecular gas masses using only widely available integrated rest-frame UV and FIR photometry. The method produces gas masses with an accuracy between 0.12 and 0.16 dex in samples of normal galaxies between z ∼ 0 and z ∼ 1.5. Major mergers and submillimeter galaxies follow a different SA relation.
(Ga,Mn)As under pressure: A first-principles investigation

Electronic and magnetic properties of ${\mathrm{Ga}}_{1\ensuremath{-}}{}_{x}\text{Mn}{}_{x}\text{As}$, obtained from first-principles calculations employing the hybrid HSE06 functional, are presented for $x=6.25%$ and 12.5% under pressures ranging from 0 to 15 GPa. In agreement with photoemission experiments at ambient pressure, we find for $x=6.25%$ that nonhybridized Mn $3d$ levels and Mn-induced states reside about 5 and 0.4 eV below the Fermi energy, respectively. For elevated pressures, the Mn $3d$ levels, Mn-induced states, and the Fermi level shift toward higher energies, however the position of the Mn-induced states relative to the Fermi energy remains constant due to hybridization of the Mn $3d$ levels with the valence As $4p$ orbitals. We also evaluate, employing Monte Carlo simulations, the Curie temperature $({\mathit{T}}_{\mathrm{C}})$. At zero pressure, we obtain ${\mathit{T}}_{\mathrm{C}}=181$ K, whereas the pressure-induced changes in ${\mathit{T}}_{\mathrm{C}}$ are $d{T}_{\mathrm{C}}/dp=+4.3$ K/GPa for $x=12.5%$ and an estimated value of $d{T}_{\mathrm{C}}/dp\ensuremath{\approx}+2.2$ K/GPa for $x=6.25%$ under pressures up to 6 GPa. The determined values of $d{T}_{\mathrm{C}}/dp$ compare favorably with $d{T}_{\mathrm{C}}/dp=+(2$--3) K/GPa at $p$ $\ensuremath{\le}1.2$ GPa found experimentally and estimated within the $p\text{\ensuremath{-}}d$ Zener model for ${\mathrm{Ga}}_{0.93}{\mathrm{Mn}}_{0.07}\text{As}$ in the regime where hole localization effects are of minor importance [M. Gryglas-Borysiewicz et al., Phys. Rev. B 82, 153204 (2010)].
THE EVOLUTION OF GALAXY SIZE AND MORPHOLOGY AT z ∼ 0.5–3.0 IN THE GOODS-N REGION WITH HUBBLE SPACE TELESCOPE/WFC3 DATA

We analyze the recently released Hubble Space Telescope/Wide Field Camera 3 IR images in the GOODS-N region to study the formation and evolution of quiescent galaxies (QGs). After examining the reliability of two-dimensional light profiles with artificial galaxies, we obtain the morphological parameters with Sérsic profile of 299 QGs and 1083 star-forming galaxies (SFGs) at z ∼ 0.5–3.0, finding the evolution of re and n of massive (M* ⩾ 1010.5 M☉) QGs and weaker evolution of SFGs and less massive (M* < 1010.5 M☉) QGs. The regression of the size evolution of massive QGs follows with (a factor of ∼2.2 increases from z ∼ 2.5 to ∼0.5), which is consistent with the general picture of the significant size growth. For the further understanding of the evolution scenario, we study the evolution of the Sérsic index, n, and find that massive QGs significantly evolve as with αn = 0.74 ± 0.23 (n ∼ 1 at z ∼ 2.5 to n ∼ 4 at z ∼ 0.5), while those of the other populations are unchanged (n ∼ 1) over the redshift range. The results in the present study are consistent with both observations and numerical simulations where a gas-poor minor merger is believed to be the main evolution scenario. By taking the connection with less massive QGs and SFGs into account, we discuss the formation and evolution of the massive QGs over “Cosmic High Noon”, or the peak of star-formation in the universe.
CORONAL SOURCES OF THE SOLAR F10.7 RADIO FLUX

We present results from the first solar full-disk F 10.7 ? > (the radio flux at 10.7 cm, 2.8 GHz) image taken with the S-band receivers on the recently upgraded Karl G. Jansky Very Large Array in order to assess the relationship between the F 10.7 ? > index and solar extreme ultraviolet (EUV) emission. To identify the sources of the observed 2.8 GHz emission, we calculate differential emission measures from EUV images collected by the Atmospheric Imaging Assembly and use them to predict the bremsstrahlung component of the radio emission. By comparing the bremsstrahlung prediction and radio observation we find that 8.1% ± 0.5% of the variable component of the F 10.7 ? > flux is associated with the gyroresonance emission mechanism. Additionally, we identify optical depth effects on the radio limb which may complicate the use of F 10.7 ? > time series as an EUV proxy. Our analysis is consistent with a coronal iron abundance that is four times the photospheric level.
Off-Center Coherent-State Representation and an Application to Semiclassics

By using the overcompleteness of coherent states we find an alternative form of the unit operator for which the ket and the bra appearing under the integration sign do not refer to the same phase-space point. This defines a new quantum representation in terms of Bargmann functions, whose basic features are presented. A continuous family of secondary reproducing kernels for the Bargmann functions is obtained, showing that this quantity is not necessarily unique for representations based on overcomplete sets. We illustrate the applicability of the presented results by deriving a semiclassical expression for the Feynman propagator that generalizes the well-known van Vleck formula and seems to point a way to cope with long-standing problems in semiclassical propagation of localized states.
Entanglement in gapless resonating-valence-bond states

We study resonating-valence-bond (RVB) states on the square lattice of spins and of dimers, as well as SU(N)-invariant states that interpolate between the two. These states are ground states of gapless models, although the SU(2)-invariant spin RVB state is also believed to be a gapped liquid in its spinful sector. We show that the gapless behavior in spin and dimer RVB states is qualitatively similar by studying the Rényi entropy for splitting a torus into two cylinders. We compute this exactly for dimers, showing it behaves similarly to the familiar one-dimensional log term, although not identically. We extend the exact computation to an effective theory believed to interpolate among these states. By numerical calculations for the SU(2) RVB state and its SU(N)-invariant generalizations, we provide further support for this belief. We also show how the entanglement entropy behaves qualitatively differently for different values of the Rényi index n, with large values of n proving a more sensitive probe here, by virtue of exhibiting a striking even/odd effect.
Pixelated Dark Energy

We study the phenomenology of a recent string construction with a quantum mechanically stable dark energy. A mild supersymmetry protects the vacuum energy but also allows O(10−100) TeV scale superpartner masses. The construction is holographic in the sense that the 4D spacetime is generated from “spacetime pixels” originating from five‐branes wrapped over metastable five‐cycles of the compactification. The cosmological constant scales as Λ∼1/N in the pixel number. An instability in the construction leads to cosmic expansion. This also causes more five‐branes to wind up in the geometry, leading to a slowly decreasing cosmological constant which we interpret as an epoch of inflation followed by (pre‐)heating when a rare event occurs in which the number of pixels increases by an order one fraction. The sudden appearance of radiation triggers an exponential increase in the number of pixels. Dark energy has a time varying equation of state with wa=−3Ωm,0(1+w0)/2 , which is compatible with current bounds, and could be constrained further by future data releases. The pixelated nature of the Universe also implies a large‐l cutoff on the angular power spectrum of cosmological observables with l max ∼O(N) . We also use this pixel description to study the thermodynamics of de Sitter space, finding rough agreement with effective field theory considerations.
Clinical outcomes of patients with Liver Imaging Reporting and Data System 3 or Liver Imaging Reporting and Data System 4 observations in patients with cirrhosis: A systematic review

Patients with indeterminate liver nodules, classified as LR‐3 and LR‐4 observations per the Liver Imaging Reporting and Data System, are at risk of developing hepatocellular carcinoma (HCC), but risk estimates remain imprecise. We conducted a systematic review of Ovid MEDLINE, EMBASE, and Cochrane databases from inception to December 2021 to identify cohort studies examining HCC incidence among patients with LR‐3 or LR‐4 observations on computed tomography (CT) or magnetic resonance imaging (MRI). Predictors of HCC were abstracted from each study, when available. Of 13 total studies, nine conducted LR‐3 observation‐level analyses, with the proportions of incident HCC ranging from 1.2% to 12.5% at 12 months and 4.2% to 44.4% during longer study follow‐up. Among three studies with patient‐level analyses, 8%–22.2% of patients with LR‐3 lesions developed LR‐4 observations and 11.1%–24.5% developed HCC. Among nine studies conducting LR‐4 observation‐level analyses, incident HCC ranged from 30.8% to 44.0% at 12 months and 30.9% to 71.0% during study follow‐up; conversely, 6%–42% of observations were downgraded to LR‐3 or lower. Patient‐level factors associated with HCC included older age, male sex, higher alpha‐fetoprotein levels, viral etiology, and prior history of HCC; observation‐level factors included maximum diameter, threshold growth, T2 hyperintensity, and visibility on ultrasound. Studies were limited by small sample sizes, inclusion of patients with prior HCC, short follow‐up duration, and failure to account for clustering of observations in patients or competing risks of transplantation and death. LR‐3 and LR‐4 observations have elevated but variable risks of HCC. Higher quality studies are necessary to identify high‐risk patients who warrant close CT or MRI‐based follow‐up.
The detectability of Lyα emission from galaxies during the epoch of reionization

We study the visibility of the Lyα emission line during the epoch of reionization. Combining galactic outflow models with large-scale seminumeric simulations of reionization, we quantify the probability distribution function of the fraction of Lyα photons transmitted through the intergalactic medium (IGM), . Our study focuses on galaxies populating dark matter haloes with masses of Mhalo= 1010 M⊙ at z= 8.6, which is inspired by the recent reported discovery of a galaxy at z= 8.6 with strong Lyα line emission. For reasonable assumptions, we find that the combination of winds and reionization morphology results in per cent (50 per cent), for the majority of galaxies, even when the Universe is ∼80 per cent (60 per cent) neutral by volume. Thus, the observed strong Lyα emission from the reported z= 8.6 galaxy is consistent with a highly neutral IGM, and cannot be used to place statistically significant constraints on the volume-averaged neutral fraction of hydrogen in the IGM. We also investigate the implications of the recent tentative evidence for an observed decrease in the ‘Lyman alpha emitter fraction’ among drop-out galaxies between z= 6 and 7. If confirmed, we show that a rapid evolution in will be required to explain this observation via the effects of reionization.
GREEN GALAXIES IN THE COSMOS FIELD

We present research on the morphologies, spectra, and environments of ≈2350 “green valley” galaxies at 0.2 < z < 1.0 in the COSMOS field. The bimodality of dust-corrected NUV−r+ color is used to define “green valley”; it removes dusty star-forming galaxies from galaxies that are truly transitioning between the blue cloud and the red sequence. Morphological parameters of green galaxies are intermediate between those of blue and red galaxy populations, both on the Gini–asymmetry and the Gini–M20 planes. Approximately 60%–70% of green disk galaxies have intermediate or big bulges, and only 5%–10% are pure disk systems, based on morphological classification using the Zurich Estimator of Structural Types. The obtained average spectra of green galaxies are intermediate between blue and red ones in terms of [O ii], Hα, and Hβ emission lines. Stellar population synthesis on the average spectra shows that green galaxies are on average older than blue galaxies but younger than red galaxies. Green galaxies and blue galaxies have similar projected galaxy density (Σ10) distributions at z > 0.7. At z < 0.7, the fractions of M* < 1010.0 M☉ green galaxies located in a dense environment are found to be significantly larger than those of blue galaxies. The morphological and spectral properties of green galaxies are consistent with the transitioning population between the blue cloud and the red sequence. The possible mechanisms for quenching star formation activities in green galaxies are discussed. The importance of active galactic nucleus feedback cannot be well constrained in our study. Finally, our findings suggest that environmental conditions, most likely starvation and harassment, significantly affect the transformation of M* < 1010.0 M☉ blue galaxies into red galaxies, especially at z < 0.5.
CHANDRA EVIDENCE FOR EXTENDED X-RAY STRUCTURE IN RY Tau

We report results of a sensitive Chandra ACIS-S observation of the classical T Tauri star RY Tau. Previous studies have shown that it drives a spectacular bipolar jet whose blueshifted component is traced optically along P.A. ≈ 295° at separations of 1. ″5–31″ from the star. Complex X-ray emission is revealed, including a very soft non-variable spectral component (some of which may originate in shocks), a superhot flaring component (T ≳ 100 MK), and faint extended structure near the star. The structure is visible in deconvolved images and extends northwestward out to a separation of 1. ″7, overlapping the inner part of the optical jet. Image analysis suggests that most of the extension is real, but some contamination by point-spread-function-induced structure within the central arcsecond may be present. The predicted temperature for a shock-heated jet based on jet speed and shock speed estimates from optical measurements is too low to explain the extended X-ray structure. Either higher speed material within the jet has escaped optical detection or other mechanisms besides shock heating are involved. Alternative mechanisms that could produce higher temperature plasma at small offsets to the northwest of RY Tau include magnetic heating in the jet, hot plasmoids ejected at high speeds, or X-ray emission from a putative close companion whose presence has been inferred from Hipparcos variations.
Evidence for an axion-like particle from PKS 1222+216?

The surprising discovery by MAGIC of an intense, rapidly varying emission in the energy range 70 - 400 GeV from the flat spectrum radio quasar PKS 1222+216 represents a challenge for all interpretative scenarios. Indeed, in order to avoid absorption of \gamma rays in the dense ultraviolet radiation field of the broad line region (BLR), one is forced to invoke some unconventional astrophysical picture, like for instance the existence of a very compact (r\sim 10^{14} cm) emitting blob at a large distance (R \sim10^{18} cm) from the jet base. We offer the investigation of a scenario based on the standard blazar model for PKS 1222+216 where \gamma rays are produced close to the central engine, but we add the new assumption that inside the source photons can oscillate into axion-like particles (ALPs), which are a generic prediction of several extensions of the Standard Model of elementary particle interactions. As a result, a considerable fraction of very-high-energy photons can escape absorption from the BLR through the mechanism of photon-ALP oscillations much in the same way as they largely avoid absorption from extragalactic background light when propagating over cosmic distances in the presence of large-scale magnetic fields in the nG range. In addition we show that the above MAGIC observations and the simultaneous Fermi/LAT observations in the energy range 0.3 - 3 GeV can both be explained by a standard spectral energy distribution for experimentally allowed values of the model parameters. In particular, we need a very light ALP just like in the case of photon-ALP oscillations in cosmic space. Moreover, we find it quite tantalizing that the most favorable value of the photon-ALP coupling happens to be the same in both situations. Although our ALPs cannot contribute to the cold dark matter, they are a viable candidate for the quintessential dark energy. [abridged]
Pyrophosphoproteomics: extensive protein pyrophosphorylation revealed in human cell lines

Reversible protein phosphorylation is a central signaling mechanism in eukaryotic cells. While the identification of canonical phosphorylation sites using mass-spectrometry (MS) based proteomics has become routine, annotation of non-canonical phosphorylation has remained a challenge. Here, we report a tailored pyrophosphoproteomics workflow to detect and reliably assign protein pyrophosphorylation in two human cell lines, providing the first direct evidence of endogenous protein pyrophosphorylation. Detection of protein pyrophosphorylation was reproducible, specific and consistent with previous biochemical evidence relating the installation of the modification to inositol pyrophosphates (PP-InsPs). We manually validated 148 pyrophosphosites across 71 human proteins, the most heavily pyrophosphorylated of which were the nucleolar proteins NOLC1 and TCOF1. A predictive workflow based on the MS data set was established to recognize putative pyrophosphorylation sequences, and UBF1, a nucleolar protein incompatible with the proteomics method, was biochemically shown to undergo pyrophosphorylation. When the biosynthesis of PP-InsPs was perturbed in a model cell line, proteins expressed in this background exhibited lower levels of pyrophosphorylation. Disruption of PP-InsP biosynthesis also significantly reduced rDNA transcription, potentially by lowering pyrophosphorylation on regulatory proteins NOLC1, TCOF1, and UBF1. Overall, protein pyrophosphorylation emerges as an archetype of non-canonical phosphorylation, and should be considered in future phosphoproteomic analyses.
Pentameric assembly of glycine receptor intracellular domains provides insights into gephyrin clustering

Pentameric ligand-gated ion channels represent a large family of receptors comprising an extracellular domain, four transmembrane helices and a cytosolic intracellular domain (ICD). ICDs play important roles in receptor localization and trafficking, thus regulating synaptic activity and plasticity. Glycine and GABA type A receptor ICDs bind to the scaffolding protein gephyrin, a master regulator of inhibitory synapses. Here we report the use of yeast lumazine synthase as soluble pentameric protein scaffold for the study of receptor ICDs derived from GlyR α1− and β-subunits. We were able to create ICDs assemblies in a homo- (LS-βICD) and hetero-pentameric state (LS-αβICD) and provide first-in-class structural insights on their high structural flexibility using small angle X-ray scattering. We report a high-affinity interaction between the LS-αβICD and gephyrin leading to the in vitro formation of high-molecular mega-Dalton complexes composed of three gephyrin trimers and three pentamers as basic building block. Depending on the stoichiometric ratios between gephyrin and LS-ICDs the formed complexes grow or shrink in size. In cells, LS-ICDs efficiently recruited gephyrin and were able to accumulate gephyrin at GABAergic synapses in neurons. Our findings collectively propose a new, potentially general, mechanistic concept for a gephyrin-dependent bridging of GlyRs at the inhibitory synapse.
Defining transcription factor nucleosome binding with Pioneer-seq

Gene expression requires the targeting of transcription factors (TFs) to regulatory sequences often occluded within nucleosomes. To comprehensively examine TF nucleosome binding, we developed Pioneer-Seq. In Pioneer-seq a library of nucleosomes containing thousands of DNA sequences with TF binding sites in all possible nucleosome orientations is bound to a TF and the protein-nucleosome complex is isolated and quantified. To demonstrate Pioneer-seq we examined nucleosome binding by OCT4, SOX2, KLF4, and c-MYC. Our results demonstrate that KLF4 and SOX2 can bind close to the nucleosome dyad with nucleosome sequence being the major factor regulating TF binding across all studied TFs.