Miracle-dz/UniFAR-FTUs huggingface dataset:
How Do Type Ia Supernova Nebular Spectra Depend on Explosion Properties? Insights from Systematic Non-LTE Modeling

We present a radiative transfer code to model the nebular phase spectra of supernovae (SNe) in non-LTE (NLTE). We apply it to a systematic study of SNe Ia using parameterized 1D models and show how nebular spectral features depend on key physical parameters, such as the time since explosion, total ejecta mass, kinetic energy, radial density profile, and the masses of 56Ni, intermediate-mass elements, and stable iron-group elements. We also quantify the impact of uncertainties in atomic data inputs. We find the following. (1) The main features of SN Ia nebular spectra are relatively insensitive to most physical parameters. Degeneracy among parameters precludes a unique determination of the ejecta properties from spectral fitting. In particular, features can be equally well fit with generic Chandrasekhar mass ( ), sub- , and super- models. (2) A sizable (≳0.1 ) central region of stable iron-group elements, often claimed as evidence for models, is not essential to fit the optical spectra and may produce an unusual flat-top [Co iii] profile. (3) The strength of [S iii] emission near 9500 Å can provide a useful diagnostic of explosion nucleosynthesis. (4) Substantial amounts (≳0.1 ) of unburned C/O mixed throughout the ejecta produce [O iii] emission not seen in observations. (5) Shifts in the wavelength of line peaks can arise from line-blending effects. (6) The steepness of the ejecta density profile affects the line shapes, offering a constraint on explosion models. (7) Uncertainties in atomic data limit the ability to infer physical parameters.
Multicomponent H2 in DLA at zabs = 2.05: physical conditions through observations and numerical models★

We perform detailed spectroscopic analysis and numerical modelling of an H_2-bearing damped Lyman-α absorber (DLA) at z_abs = 2.05 towards the quasar FBQS J2340-0053. Metal absorption features arise from 14 components spread over Δv_90 = 114 km s^−1, seven of which harbour H_2. Column densities of atomic and molecular species are derived through Voigt profile analysis of their absorption lines. We measure total N(H i), N(H_2), and N(HD) to be 20.35 ± 0.05, 17.99 ± 0.05, and 14.28 ± 0.08 (log cm^−2), respectively. H_2 is detected in the lowest six rotational levels of the ground vibrational state. The DLA has metallicity, Z = 0.3 Z_|$\odot$| ([S/H] = −0.52 ± 0.06) and dust-to-gas ratio, κ = 0.34 ± 0.07. Numerical models of the H_2 components are constrained individually to understand the physical structure of the DLA. We conclude that the DLA is subjected to the metagalactic background radiation and cosmic ray ionization rate of ∼10^−15.37 s^−1. Dust grains in this DLA are smaller than grains in the Galactic interstellar medium. The inner molecular regions of the H_2 components have density, temperature, and gas pressure in the range 30–120 cm^−3, 140–360 K, and 7000–23 000 cm^−3 K, respectively. Micro-turbulent pressure is a significant constituent of the total pressure, and can play an important role in these innermost regions. Our H_2 component models enable us to constrain component-wise N(H i), and elemental abundances of sulphur, silicon, iron, and carbon. We deduce the line-of-sight thickness of the H_2-bearing parts of the DLA to be 7.2 pc.
Energy loss of charm quarks in the quark-gluon plasma: Collisional vs radiative losses

In considering the collisional energy loss rates of heavy quarks from hard light parton interactions, we computed the total energy loss of a charm quark for a static medium. For the energy range E{approx}5-10 GeV of charm quark, it proved to be almost the same order as that of radiative ones estimated to a first-order opacity expansion. The collisional energy loss becomes much more important for lower energy charm quarks, and this feature could be very interesting for the phenomenology of hadrons spectra. Using such collisional energy loss rates, we estimate the momentum loss distribution employing a Fokker-Planck equation and the total energy loss of a charm quark for an expanding quark-gluon plasma under conditions resembling the energies presently available at the BNL Relativistic Heavy Ion Collider. The fractional collisional energy loss is found to be suppressed by a factor of 5 as compared to the static case and does not depend linearly on the system size. We also investigate the heavy to light hadrons D/{pi} ratio at moderately large (5-10 GeV/c) transverse momenta and comment on its enhancement.
The Pathogenic Role of CD4 D Tissue-Resident Memory T Cells Bearing T Follicular Helper-Like Phenotype in Pemphigus Lesions

In skin lesions caused by pemphigus, a group of life-threatening autoimmune bullous diseases, an over-representation of CD4 þ tissue-resident memory T (T RM ) cells was found. We sought to investigate the contributions of CD4 þ T RM cells to the severity and refractoriness of pemphigus and their role in local immunological pathogenesis. Our data showed that CD4 þ T RM cells accumulated signiﬁcantly in pemphigus skin lesions. These CD4 þ T RM cells expressed a speciﬁc set of T follicular helper cell ‒ related costimulatory molecules. We also found that CD4 þ T RM cells remaining in the lesions produced IL-17A and IL-21. In vitro, CD4 þ T RM cells exhibited strong support and assistance to autoantibody production. Through transcriptomic sequencing and bioinfor-matics analysis, we identiﬁed that the transcription factor IRF4 was responsible for IL-21 overexpression and autoantibody production. Our results showed that T follicular helper-like CD4 þ T RM cells in pemphigus lesions promoted local autoantibody production, resulting in the formation and recurrence of lesions, which supports targeting this cell subset in pemphigus treatment. IRF4 might serve as a potential therapeutic target.
Star-forming content of the giant molecular filaments in the Milky Way

Context. Through observations numerous giant molecular filaments (GMFs) have been discovered in the Milky Way. Their role in the Galactic star formation and Galaxy-scale evolution of dense gas is unknown. Aims. We investigate systematically the star-forming content of all currently known GMFs. This allows us to estimate the star formation rates (SFRs) of the GMFs and to establish relationships between the SFRs and the GMF properties. Methods. We identified and classified the young stellar object (YSO) population of each GMF using multiwavelength photometry from near- to far-infrared. We estimated the total SFRs assuming a universal and fully sampled initial mass function and luminosity function. Results. We uniformly estimate the physical properties of 57 GMFs. The GMFs show correlations between the 13CO line width, mass, and size, similar to Larson’s relations. We identify 36 394 infrared excess sources in 57 GMFs and obtain SFRs for 46 GMFs. The median SFR surface density (ΣSFR) and star formation efficiency (SFE) of GMFs are 0.62 M⊙ Myr−1 pc−2 and 1%, similar to the nearby star-forming clouds. The star formation rate per free-fall time of GMFs is between 0.002−0.05 with the median value of 0.02. We also find a strong correlation between SFR and dense gas mass that is defined as gas mass above a visual extinction of 7 mag, which suggests that the SFRs of the GMFs scale similarly with dense gas as those of nearby molecular clouds. We also find a strong correlation between the mean SFR per unit length and dense gas mass per unit length. The origin of this scaling remains unknown, calling for further studies that can link the structure of GMFs to their SF activity and explore the differences between GMFs and other molecular clouds.
The X-Ray Emission of 3C 346 and Its Environment

We present a detailed spectral and spatial analysis of the X-ray properties of the compact and unusual radio galaxy 3C 346, combining information from ROSAT and ASCA. The dominant component of X-ray emission (~1044 ergs s-1 in each of the 0.5-3 keV and 2-10 keV bands) is unresolved and not heavily absorbed (intrinsic NH ≲ 2 × 1021 cm-2), with evidence for variability of 32% ± 13% over 18 months. We relate the X-ray emission to radio structures on both milliarcsecond scales and the arcsecond scales which Chandra can resolve. The absence of X-ray absorption, and the radio/optical/X-ray colors, when combined with previous radio evidence that the source is a foreshortened FR II, suggest that the radio jets are seen at an angle to the line of sight of about 30°, intermediate between the radio galaxy and quasar classes. Roughly a third of the soft X-ray emission is from a cluster atmosphere, for which we measure a temperature of 1.9 keV, making this the second low-redshift (z < 0.2) powerful radio galaxy, after Cyg A, with a measured cluster temperature. At a jet angle of ~30°, all the radio structures lie within the core radius of the cluster, for which the cooling time is sufficiently long that there is no reason to expect the presence of a cooling flow. The radio lobes of 3C 346 are roughly in pressure balance with the external medium under the assumptions that the energy densities in the magnetic field and radiating particles balance and that a source of excess pressure in the radio lobes, commonly invoked in other radio galaxies, is absent here.
Depth-profiling plasma-induced densification of porous low-k thin films using positronium annihilation lifetime spectroscopy

Positronium annihilation lifetime spectroscopy (PALS) has been used to depth profile the densification induced in a porous low-dielectric constant (k) thin film by typical device integration processing, including exposure to plasmas and oxygen ashing. Such “integration damage” has previously been observed as an undesirable increase in k accompanied by shrinkage in the porous film thickness. PALS confirms that the structural damage is confined to a surface layer of collapsed pores with the underlying pores being undamaged. The dense layer thickness determined by PALS increases with plasma exposure time.
HST Hα grism spectroscopy of ROLES: a flatter low-mass slope for the z ~ 1 SSFR-mass relation

We present measurements of star formation rates (SFRs) for dwarf galaxies (M* ∼ 108.5 M⊙ M⊙) at z ∼ 1 using near-infrared slitless spectroscopy from the Hubble Space Telescope (HST) by targeting and measuring the luminosity of the Hα emission line. Our sample is derived from the Redshift One LDSS3 Emission Line Survey (ROLES), which used [O ii]λ3727 as a tracer of star formation to target very low stellar masses down to very low SFRs (∼0.1 M⊙ M⊙ yr−1) at this epoch. Dust corrections are estimated using SED fits and we find, by comparison with other studies using Balmer decrement dust corrections, that we require a smaller ratio between the gas phase and stellar extinction than the nominal Calzetti relation, in agreement with recent findings by other studies. By stacking the Wide-Field Camera (WFC)3 spectra at the redshifts obtained from ground-based [O ii] detections, we are able to push the WFC3 spectra to much lower SFRs and obtain the most complete spectroscopic measurement of the low-mass end of the SSFR–mass relation to date. We measure a flatter low-mass power-law slope (−0.47 ± 0.04) than found by other (shallower) H α-selected samples (≈−1), although still somewhat steeper than that predicted by the Evolution and Assembly of GaLaxies and their Environments (EAGLE) simulation (−0.14 ± 0.05), hinting at possible missing physics not modelled by EAGLE or remaining incompleteness for our H α data.
RR Lyrae Stars in Galactic Globular Clusters. II. A Theoretical Approach to Variables in M3

We present predicted relations connecting pulsational (period and amplitude of pulsation) and evolutionary (mass, absolute magnitude, and color) parameters, as based on a wide set of convective pulsating models of RR Lyrae stars with Z = 0.001, Y = 0.24, and mass and luminosity suitable for the "old" (age > 8 Gyr) variables observed in globular clusters. The relations are collated with sound constraints on the mass of pulsators, as inferred from up-to-date evolutionary models of horizontal-branch stars, in order to provide a self-consistent theoretical framework for the analysis of observed variables. The theoretical predictions are tested through a detailed comparison with measurements of RR Lyrae stars in the globular cluster M3. We show that the predicted relations satisfy a variety of observed data, thus providing a pulsational route to the determination of accurate distances to RR Lyrae-rich globular clusters with intermediate metal content. We show that current uncertainties on the intrinsic luminosity of up-to-date horizontal-branch models, as due to the input physics used in the computations by the different authors, have a quite low influence (~0.02-0.03 mag) on the pulsational distance modulus. On the contrary, the effect of the different bolometric corrections adopted to convert bolometric luminosity into absolute magnitude is of the order of ~0.05-0.06 mag. The pulsation models are also used to perform some valuable tests on the physics adopted in current stellar evolution computations. We show that the constraints inferred by pulsation theory support the large value of the mixing-length parameter (l/Hp = 1.9-2.0) adopted to fit observed red giant branches, but that, at the same time, they would yield that the luminosity of the horizontal-branch updated models is too bright by ~0.08 ± 0.05 mag, if helium diffusion and metal diffusion are neglected. Conversely, if element diffusion is properly taken into account, then there is a marginal discrepancy of ~0.04 ± 0.05 mag between evolutionary and pulsational predictions.
GW170817 and the Prospect of Forming Supramassive Remnants in Neutron Star Mergers

The gravitational wave data of GW170817 favor the equation of state (EoS) models that predict compact neutron stars (NSs), consistent with the radius constraints from X-ray observations. Motivated by such remarkable progress, we examine the fate of the remnants formed in NS mergers and focus on the roles of the angular momentum and the mass distribution of the binary NSs. In the mass-shedding limit (for which the dimensionless angular momentum equals the Keplerian value, i.e., j = jKep), the adopted seven EoS models, except for H4 and ALF2, yield supramassive NSs in more than half of the mergers. However, for j ≲ 0.7 jKep, the presence or absence of a non-negligible fraction of supramassive NSs formed in the mergers depends sensitively on both the EoS and the mass distribution of the binary systems. The NS mergers with a total gravitational mass ≤ 2.6 M⊙ are found to be able to shed valuable light on both the EoS model and the angular momentum of the remnants if supramassive NSs are still absent. We have also discussed the uncertainty on estimating the maximum gravitational mass of nonrotating NSs (Mmax) due to the unknown j of the precollapse remnants. With the data of GW170817 and the assumption of the mass loss of 0.03 M⊙, we have Mmax < (2.19, 2.32) M⊙ (90% confidence level) for j = (1.0, 0.8) jKep, respectively.
The outcomes of carbon–oxygen white dwarfs accreting CO-rich material

The double-degenerate model, involving the merger of double carbon-oxygen white dwarfs (CO WDs), is one of the two classic models for the progenitors of type Ia supernovae (SNe Ia). Previous studies suggested that off-centre carbon burning would occur if the mass-accretion rate (Macc) is relatively high during the merging process, leading to the formation of oxygen-neon (ONe) cores that may collapse into neutron stars. However, the off-centre carbon burning is still incompletely understood, especially when the inwardly propagating burning wave reaches the centre. In this paper, we aim to investigate the propagating characteristics of burning waves and the subsequently evolutionary outcomes of these CO cores. We simulated the long-term evolution of CO WDs that accrete CO-rich material by employing the stellar evolution code MESA on the basis of the thick-disc assumption. We found that the final outcomes of CO WDs strongly depend on Macc (Msun/yr) based on the thick-disc assumption, which can be divided into four regions: (1) explosive carbon ignition in the centre, then SNe Ia (Macc 1.05*10^-5). Our results indicate that the final fates of double CO WD mergers are strongly dependent on the merging processes (e.g. slow merger, fast merger, composite merger, violent merger, etc.).
Two New Low-Redshift 21 Centimeter Absorbers

As part of a larger program to identify low-redshift radio analogs of the damped Lyα absorbers seen in the spectra of high-redshift quasars, Westerbork Synthesis Radio Telescope observations have discovered two new H I 21 cm absorption lines at z = 0.394 and z = 0.437 in the spectra of the radio sources B0248+430 and B1243-072, respectively. These sight lines and redshifts were selected for study on the basis of the previously known low-ionization absorption lines of Mg II, and neither has been observed in the Lyα line. The 21 cm line observations provide information on the column densities, temperatures, and kinematics of the thickest cold neutral clouds in the absorbers.
MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on Angular Scales of 10'-5°

We present a map and an angular power spectrum of the anisotropy of the cosmic microwave background (CMB) from the first flight of the Millimeter-wave Anisotropy Experiment Imaging Array (MAXIMA). MAXIMA is a balloon-borne experiment with an array of 16 bolometric photometers operated at 100 mK. MAXIMA observed a 124 deg2 region of the sky with 10' resolution at frequencies of 150, 240, and 410 GHz. The data were calibrated using in-flight measurements of the CMB dipole anisotropy. A map of the CMB anisotropy was produced from three 150 and one 240 GHz photometer without need for foreground subtractions. Analysis of this CMB map yields a power spectrum for the CMB anisotropy over the range 36 ≤ l ≤ 785. The spectrum shows a peak with an amplitude of 78 ± 6 μK at l ≃ 220 and an amplitude varying between ~40 and ~50 μK for 400 ≲ l ≲ 785.
Probing strong dynamics with cosmic neutrinos

IceCube has observed 80 astrophysical neutrino candidates in the energy range 0.02 < E_\nu/PeV < 2. Deep inelastic scattering of these neutrinos with nucleons on Antarctic ice sheet probe center-of-mass energies $\sqrt{s} \sim$ 1 TeV. By comparing the rates for two classes of observable events, any departure from the benchmark (perturbative QCD) neutrino-nucleon cross section can be constrained. Using the projected sensitivity of South Pole next generation neutrino telescope we show that this facility will provide a unique probe of strong interaction dynamics. In particular, we demonstrate that the high-energy high-statistics data sample to be recorded by IceCube-Gen2 in the very near future will deliver a direct measurement of the neutrino-nucleon cross section at $\sqrt{s} \sim 1$ TeV, with a precision comparable to perturbative QCD informed by HERA data. We also use IceCube data to extract the neutrino-nucleon cross section at $\sqrt{s} \sim 1$ TeV through a likelihood analysis, considering (for the first time) both the charged-current and neutral-current contributions as free parameters of the likelihood function.
New spectroscopic confirmations of high-redshift galaxy clusters

We present new spectroscopic data in the field of five high-redshift ($z\geq0.6$) candidate galaxy clusters, drawn from the EIS Cluster Candidate Catalog. A total of 327 spectra were obtained using FORS1 at the VLT, out of which 266 are galaxies with secure redshifts. In this paper, we use these data for confirming the existence of overdensities in redshift space at the approximate same location as the matched-filter detections in the projected distribution of galaxies from the EIS I -band imaging survey. The spectroscopic redshifts, associated to these overdensities, are consistent but, in general, somewhat lower than those predicted by the matched-filter technique. Combining the systems presented here with those analyzed earlier, we have spectroscopically confirmed a total of nine overdensities in the redshift range $0.6 < z < 1.3$, providing an important first step in building an optically-selected, high-redshift sample for more detailed studies, complementing those based on the few available X-ray selected systems.
Observation of an anomalous heat current in a Weyl fermion semimetal

The curvature of space-time and its consequences are often far removed from experimental accessibility. A particularly elusive effect is the generation of a heat current by the mixed axial-gravitational anomaly. However, recent theoretical investigations suggest that the magneto-thermal conductivity of condensed matter Weyl systems is linked to such an anomaly-related heat current even in flat space-time. In this paper, we report a positive magneto-thermal conductivity in the semimetal GdPtBi for collinear temperature gradients and magnetic fields ($\nabla T\parallel\mathbf{B}$). The positive magneto-thermal conductivity emerges concurrently with the established anomaly-related magneto-electrical conductivity of Weyl fermions, and is locked to the parallel alignment of $\nabla T$ and $\mathbf{B}$. This observation is consistent with the generation of an anomalous heat current, a fingerprint of the existence of the mixed axial-gravitational anomaly.
ENTANGLED MIXED STATES AND LOCAL PURIFICATION

Linden, Massar and Popescu have recently given an optimization argument to show that a single two-qubit Werner state, or any other mixture of the maximally entangled Bell states, cannot be purified by local operations and classical communications. We generalise their result and give a simple explanation. In particular, we show that no purification scheme using local operations and classical communications can produce a pure singlet from any mixed state of two spin-1/2 particles. More generally, no such scheme can produce a maximally entangled state of any pair of finite-dimensional systems from a generic mixed state. We also show that the Werner states belong to a large class of states whose fidelity cannot be increased by such a scheme.
Knot concordance and von Neumann $\rho$-invariants

We present new results, announced in [T], on the classical knot concordance group C. We establish the nontriviality at all levels of the (n)-solvable filtration · · · ⊆ Fn ⊆ · · · ⊆ F1 ⊆ F0 ⊆ C introduced in [COT1]. Recall that this filtration is significant due to its intimate connection to tower constructions arising in work of A. Casson and M. Freedman on the topological classification problem for 4-manifolds and due to the fact that all previously known concordance invariants are reflected in the first few terms in the filtration. In [COT1], nontriviality at the first new level n = 3 was established. Here, we prove the nontriviality of the filtration for all n, hence giving the ultimate justification to the theory. A broad range of techniques is employed in our proof, including cut-and-paste topology and analytical estimates. We use the Cheeger-Gromov estimate for von Neumann ρ-invariants, a deep analytic result. We also introduce a number of new algebraic arguments involving noncommutative localization and Blanchfield forms. We have attempted to make this article accessible to readers with only passing knowledge of [COT1].
Topological order in the color-flavor locked phase of a (
3+1
)-dimensional 
U(N)
 gauge-Higgs system

We study a (3+1)-dimensional U(N) gauge theory with N-flavor fundamental scalar fields, whose color-flavor locked (CFL) phase has topologically stable non-Abelian vortices. The U(1) charge of the scalar fields must be Nk+1 for some integer k in order for them to be in the representation of U(N) gauge group. This theory has a ZNk+1 one-form symmetry, and it is spontaneously broken in the CFL phase, i.e., the CFL phase is topologically ordered if k≠0. We also find that the world sheet of topologically stable vortices in CFL phase can generate this one-form symmetry.