Analysis of simulated X-ray line profiles of atomistic models of prismatic dislocation loops and dipoles in α zirconium

We present and analyze the static spectroscopy and radiative dynamics of very high quality, well characterized silver indium gallium sulfide quantum dots. We find that the static spectroscopy and radiative dynamics are very different from those in II-VI and III-V quantum dots. The absorption spectrum is broad and featureless, but sharp, high quantum yield (90%) band edge photoluminescence is observed. Despite the spectrally sharp photoluminescence, the photoluminescence decays are long and nonexponential, having components ranging from 40 to 150ns. The spectroscopy and radiative kinetics are understood in the context of the radial composition profile of each element, as determined by energy dispersive x-ray spectroscopy line profiles. The radially dependent compositions show that the core is largely Ag2S with the fraction of gallium increasing with radial distance. We suggest that random spatial fluctuations in the local silver concentration localize holes at the most silver-rich regions of the particle. The lowest energy transition is nominally parity forbidden and the parity selection rule is relaxed in the random alloy crystal environment. The sites at which holes localize have varying degrees of local crystal asymmetry and varying magnitudes of internal electric fields. Both types of perturbations can break the local symmetry and thereby relax the parity selection rule, giving rise to inhomogeneity in the radiative rates. We also consider the possibility that the nonexponential photoluminescence decay kinetics can be explained by a delayed emission model but consider this to be less likely than the inhomogeneous radiative rate model.

Variable selection plays a central role in spectroscopic calibration. However, most existing methods treat it as a purely data-driven optimization task, without explicitly incorporating the physicochemical mechanisms of spectral responses. Herein, we propose a physics-informed spectral-structure synergy optimization (SSSO) method that integrates characteristic spectral lineshapes (CSLs) with structured synergy effects to enhance consistency and interpretability. First, a physics-informed sparse Bayesian dictionary learning strategy is proposed to explicitly model CSLs using a sparse Gaussian dictionary, while structure-aware priors are employed to characterize the intrinsic properties of distinct spectral components. Variational Bayesian inference (VBI) is then applied to obtain approximate posterior distributions. Based on the solutions, the full spectrum is decomposed into chemically meaningful peak structures, thereby achieving adaptive nonuniform spectral segmentation. To further exploit synergistic effects among these structures, a structure-based bootstrap sampling strategy is introduced. This strategy generates diverse structural combinations and iteratively compresses the number of retained structures based on predictive performance, ultimately selecting the optimal synergistic structural combination. Experimental results demonstrate that SSSO achieves superior predictive performance while ensuring physicochemical interpretability, with the selected variables consistently aligning with the chemical bonds of the target analytes.

Abstract We observed comet C/2025 A6 with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) equipped with the ultra-wideband receiver from 2025 October 23 to November 8, and it was the first detection for this comet with FAST. Through trapezoidal fitting of the OH line profiles, the expansion velocities of the water increase from 1.5±0.3 km s -1 at the heliocentric distance of 0.65 AU to 3±0.9 km s -1 at 0.54 AU. Based on these results, we estimated the OH production rates of C/2025 A6 for October 23, October 26, November 4 and November 5 which were (1.0±0.1)×10 29 , (1.2±0.1)×10 29 , (1.4±0.3)×10 29 , and (1.5±0.4)×10 29 s -1 respectively. The results show a significant upward trend.

Objective.We present the system design and optimization of the ProVision prostate-dedicated time-of-flight, depth-of-interaction, dual-panel positron emission tomography (PET) scanner. Dual-panel PET geometries offer compact and open configuration suitable for prostate-dedicated imaging; yet, they intrinsically suffer from limited-angle sampling. We evaluated two practical strategies providing the same overall scanning time, to improve transaxial angular coverage: (i) large, static panels (3 × 8 detector blocks) optimized through inter-block gap patterns (8 candidate geometries), and (ii) smaller movable panels (3 × 4 blocks) optimized via multi-step motion protocols (4 candidate protocols).Approach.Candidate designs were screened using two complementary frameworks. First, a fast, reconstruction-independent approach proposed to quantify voxelwise sampling characteristics, capturing both the magnitude and isotropy of angular coverage throughout the imaging volume. Second, conventional Monte Carlo simulations followed by image reconstruction and standardized image quality analysis (using a scaled National Electrical Manufacturers Association NU2 image-quality phantom) to assess the resulting imaging performance. The performance was evaluated using contrast recovery (CR), background variability (noise), contrast-to-noise ratio, plus quantification of image elongation through the full-width at half-maximum (FWHM) of line profiles passing through the smallest (4.5 mm diameter) spherical insert.Main results.For static designs, non-uniform gap configuration (smaller at centre, and progressively larger gaps toward the panel edges) were consistently favoured. The top-performing geometry achieved the best overall balance, with +4.3% CR, -2.4% noise, and reduced elongation (7.2 mm vs 8.0 mm FWHM) relative to the minimum-gap reference geometry. For dynamic designs, more complex motion protocols led to improved performance; the best protocol achieved modest gains (+1.6% CR, -3.6% noise) and the smallest elongation among protocols (FWHM 6.3 mm vs 7.4 mm for the reference protocol). Comparing the best of static and dynamic configurations, the moving-panel design improved CR (55.9% vs 53.4%) and elongation (6.3 mm vs 7.2 mm) at the cost of substantially increased noise (8.2% vs 5.7%; +44%), highlighting a clear performance-noise-complexity trade-off. Rankings derived from the proposed reconstruction-independent framework showed overall consistency with those obtained from Monte Carlo simulations, leading to the same winning candidates.Significance.The two evaluation frameworks should be viewed as complementary rather than directly comparable, each offering distinct and valuable insights at different stages of system design and optimization. This study provides a structured basis for examining performance trade-offs, practical design constraints, and methodological implications associated with static and dynamic dual-panel PET configurations for prostate imaging.

ABSTRACT As-quenched lath martensitic steels exhibit a low elastic limit followed by high-strain-hardening without reasonable dislocation multiplication. The role of numerous dislocations in the unique stress–strain behaviour is unclear. Here, we investigated the obstacles to dislocation motion and evolution of dislocation properties (density, fraction of screw dislocations, and distribution parameter) using 0.1 mass%C steel with and without ausforming. X-ray line profile analysis revealed that these dislocation properties were barely changed after tensile tests. Stress relaxation tests indicated that the internal stress, arising from long-range obstacles such as dislocation tangles, constantly accounts for more than 90% of the applied stress. The effective stress, arising from short-range obstacles, was negligibly small at the elastic limit and increased proportionally with the internal stress. This trend implies that the short-range obstacles are dependent on dislocation density, such as dislocation intersections. These findings support two key conclusions: (1) At the elastic limit, dislocations are sufficiently mobile that the distance a dislocation moves is too short to cause dislocation intersections and (2) the strain hardening results from the sequential yielding of soft (low) to hard (high dislocation density) regions. Thus, the elevated flow stress observed in ausformed specimens is attributed to a higher initial screw dislocation density, which intensifies both internal and effective stresses.

Middle ear prostheses are among the smallest implanted medical devices, with diameters as small as 0.25 mm. Accurate postoperative imaging is critical for assessing prosthesis placement, detecting complications such as dislodgement or extrusion, and informing potential revisions. Conventional energy-integrating detector CT (EID-CT) is traditionally used for imaging these implants; however, with the recent clinical use of photon-counting detector CT (PCD-CT), further analysis on multiple parameters is required to assess future utility. This study compares the spatial resolution and visualization quality of middle ear prostheses between EID-CT and PCD-CT. We hypothesize that PCD-CT will provide superior spatial resolution of prostheses, allowing for more accurate postoperative assessments to facilitate improved clinical decision-making. This retrospective study included 10 patients with various middle ear prostheses, including total ossicular replacement prostheses, partial ossicular replacement prostheses (PORP), stapes prostheses, and the middle ear portion of cochlear implants. Each patient underwent temporal bone imaging on both EID-CT and PCD-CT scanners using institutional high-resolution protocols. A total of 30 line profiles were analyzed, with peak intensity (HU) and full width at half maximum (FWHM) calculated from the intensity curves along the prosthetic shafts. Paired t tests were used to assess differences in image-quality metrics between PCD-CT and EID-CT. PCD-CT demonstrated significantly higher mean peak intensity values (4855.8 [SD, 3944.3] HU ) compared with EID-CT (2498.7 [SD, 2135.9] HU), with a mean difference of 2357 HU (95% CI, 77-4638; HU; P = .04). Spatial resolution, measured as FWHM, was significantly better with PCD-CT (mean, 0.4 [SD, 0.2]) than EID-CT (mean, 0.6 [SD, 0.3] mm), with a mean difference of -0.2 mm (95% CI, -0.3 to -0.1; P = .002). PCD-CT demonstrates advantages in spatial resolution and image quality over conventional EID-CT for postoperative evaluation of middle ear prostheses. Enhanced visualization may improve diagnostic confidence and enable more accurate postoperative assessment and complication detection.

Context . Protoplanetary disks around young Sun-like stars are the cradles of the vast majority of detected exoplanets. Probing these disks at multiple spatial scales is key to uncovering how planets form. The inner astronomical unit, the star-disk interaction region, is of utmost importance because most detected exoplanets occupy this zone. Aims . We aim to spatially and spectrally resolve the inner disk and star-disk interaction region of the M0.3 T Tauri star DO Tau by combining two complementary techniques. Methods . We used high-resolution near-infrared spectra from CFHT/SPIRou to constrain the magnetospheric star-disk interaction process and optical long-baseline interferometry with ESO VLTI/GRAVITY to determine the sizes of the K-band continuum and Br γ line emitting regions. From the SPIRou spectra, we measured the veiling in the YJHK bands along with the equivalent widths of the HeI λ 1083, Paβ, and Br γ emission lines, from which we estimated the mass accretion rate. We were able to monitor the time variability of these quantities thanks to our long-sequence of observations over about 40 days. We fit the GRAVITY visibilities in the continuum and the differential quantities in the line with geometrical models to obtain the orientation and the size of the inner disk as well as the size and the on-sky displacement of the Br γ emitting region. Results . We derived a mass accretion rate of ∼10 −8 −10 −7 M ⊙ yr −1 , which confirms that this ∼0.5 M ⊙ star is a strong accretor. The HI and HeI lines exhibit strong variability on a daily timescale, consistent with the burster classification of DO Tau derived from its K2 light curve. We report a periodic modulation of the intensity of the redshifted high-velocity wings of the Br γ line profile. The modulation occurs at the rotational period of the star (5.128 d), which suggests the existence of corotating magnetospheric funnel flows. We derived an upper limit of 0.35 on the ratio between the magnetospheric truncation radius and the disk corotation radius, indicative of an ordered unstable accretion regime. The size of the Br γ line emitting region obtained from GRAVITY is quite small ( R Brγ = 0.011 au ∼ 1.3 R * ), and it is much smaller than the K-band continuum emitting region ( R K = 0.09 au ∼ 11 R * ). Such a compact Br γ emission region suggests that most of the line flux originates from the magnetospheric accretion region and/or from an inner wind close to the magnetosphere-disk interface. The on-sky displacements of the blue and red Br γ line velocity channels suggest a rotation pattern of the emitting gas, as they appear to be nearly aligned along the position angle of the disk. The inclination we derived for the inner disk (∼45-55°) differs from that of the outer disk inferred from the ALMA continuum (∼30°). This points toward a misalignment or warp of the outer disk that may originate from the suspected past encounter with the neighboring HV Tau system. Conclusions . Based on combining high-resolution spectroscopy and long baseline interferometry, we find that the T Tauri star DO Tau appears to be a strong accretor undergoing magnetospheric accretion in an ordered unstable regime, with a Br γ line emitting region as compact (∼0.01 au) as the size of its magnetosphere.

The stria of Gennari (SoG) is a densely myelinated band within layer IVb of the primary visual cortex (V1) and represents the only cortical laminar structure visible macroscopically invivo. Ultrahigh-field MRI may improve its detection and conspicuity. To quantitatively and qualitatively compare the invivo appearance of the SoG at 3 versus 7 T using matched high-resolution T2-weighted fast spin-echo MRI. Prospective. A total of 12 subjects (6 female, 6 male; median age, 17 years; range, 15-24 years) with pediatric-onset epilepsy. 3 and 7 T MRI, T2-weighted fast spin-echo, acquired within 1 month of each other. Cortical line profiles per subject were extracted orthogonally to the calcarine sulcus in V1. Quantitative metrics included peak-valley distance, Δ-signal (peak-valley difference), and contrast ratio (CR). Two blinded neuroradiologists and a radiologist independently rated SoG conspicuity using a 5-point Likert scale. McNemar's test compared detection rates; paired t-tests or Wilcoxon signed-rank tests compared quantitative metrics; reader preferences were analyzed using Wilcoxon tests; inter-reader agreement was assessed using weighted Cohen's κ. No multiple-comparison correction was applied (α = 0.05). SoG-consistent valleys were detected in 31% of profiles at 3 T and 65% at 7 T, significantly. Peak-valley distance remained stable across field strengths (0.45 ± 0.06 depth units; p = 0.37). Mean Δ-signal (33.5 vs. 36.1; p = 0.81) and contrast ratio (0.013 vs. 0.000; p = 0.54) did not differ significantly. Both readers demonstrated a strong preference for 7 T images (pseudo-median +1 to +1.5; significant), with fair inter-reader agreement (κ = 0.36). The SoG can be visualized invivo at both 3 and 7 T, with higher detection frequency and greater subjective conspicuity at 7 T. Quantitative laminar metrics remained stable across field strengths, suggesting that improved detectability at 7 T likely reflects enhanced spatial definition rather than measurable changes in signal contrast. Stage 2.

Abstract The study of Stark broadening of neutral helium lines, despite significant advances over recent decades, has not led to updated large grids of helium line profiles relevant to the spectroscopic study of helium-rich stars. While the semi-analytical approach based on the standard Stark broadening theory is efficient for generating such grids, it presents challenges in incorporating additional physical effects into the model. Motivated by recent studies that highlight potential issues with line profiles in the context of white dwarf stars, this paper leverages advances in computer simulations to create a new grid of line profiles for 13 neutral helium lines in the optical range. These profiles cover densities ranging from 10 14 to 6 × 10 17 cm −3 and temperatures from 10,000 to 40,000 K, with the exception of the narrower He i λ 4713 line, for which the profile grid begins at 10 15.5 cm −3 . The primary goal of this research is to present the new grid and compare it with both the semi-analytical approach and other simulation results. By doing so, corrections to the previous grid will be explored, providing a foundation for future studies that utilize this updated grid. We also examine the impact of these new profiles on the determination of physical parameters for a range of astrophysical objects, including DB white dwarfs and other helium-rich stars.

Abstract Resolved rotation curves (RCs) are our best probe of the dark matter distribution around individual galaxies. However their acquisition is resource-intensive, rendering them impractical for large-scale surveys and studies at higher redshift. Spatially integrated Hi flux profiles on the other hand are observationally abundant and also probe dynamics across the whole Hi disc. Despite this, they are typically only studied using the highly compressed linewidth summary statistic, discarding much of the available information. Here we construct a Bayesian model to infer halo properties from the full shape of the spatially integrated 21-cm line profile of a galaxy, utilising all the available information. We validate our model by assessing the consistency of halo parameters obtained from the flux profile with those obtained from RC fits for a sample of 20 galaxies where both are available, finding good agreement provided the profile is not strongly asymmetric. We study the relative constraining power (quantified using the Kullback–Leibler divergence of the posterior from the prior), finding the flux profile inference recovers posteriors on generalised Navarro–Frenk–White halo parameters on average three times tighter than those from the linewidth, and in some cases as tight as those from resolved RCs. Finally we introduce and validate a probabilistic empirical model for the spatial distribution of Hi, enabling our model to be applied to datasets for which no spatially resolved Hi information is available. As the next-generation of Hi observatories comes online, our framework will enable mass modelling in new regimes, with particular utility for constraining the dark matter content of galaxies across cosmic time.

Abstract The Herbig Ae star AB Aurigae hosts a vast, low-inclination protoplanetary disk that exhibits a plethora of substructures, including the protoplanet candidate AB Aur b. We present M -band spectroscopic data taken with the NASA Infrared Telescope Facility from 2024 February, covering multiple position angles that captured emission from an off-centered, low temperature, and compact source. Analysis of the 12 CO v = 1–0 low- J rovibrational emission line profiles and spectroastrometric signals localizes the source at around an orbital radius of 65 au and a position angle of 143°. These coordinates are distinctly different from those of AB Aur b, which was not detected. Although there is no obvious explanation for the detected source, if we assume it is a circumplanetary disk, then its maximum temperature would be about 550 K and its maximum radius would be about ∼5 au. Our results alludes to a previously unknown companion that may be residing in the AB Aurigae system.

Depth of interaction (DOI) encoding detectors are essential for pre-clinical or organ-dedicated PET scanners to simultaneously achieve high spatial resolution and high sensitivity. Semi-monolithic scintillator PET detectors inherently possess the DOI encoding capability that monolithic scintillator detectors have and can also improve the spatial resolution of the detector by reducing the edge effect. Compared to the widely used lutetium yttrium oxyorthosilicate (LYSO) scintillator, the newly developed gadolinium aluminum gallium garnet (GAGG) scintillator has a higher light output, which may lead to a better energy resolution and higher three-dimensional positioning accuracy in semi-monolithic PET detectors. The semi-monolithic scintillator detectors consisted of 12 long GAGG slabs of 0.96 ⋅ 56 ⋅ 10 mm3, with one using BaSO4 (detector 1) and the other using ESR (detector 2) as the reflector between the slabs. The front and two end surfaces of the slabs were painted with black ink. The detectors were single-ended read out by a 4×16 silicon photomultiplier (SiPM) array with an active pixel area of 3×3 mm2 and a pitch of 3.65mm. A row and column summing signal readout circuit was used to convert the 64 SiPM signals into 4 row and 16 column signals. Different monolthic (y) and DOI (z) positions of the detector were selectively irradiated by using an electronic collimation plus a mechanical collimation. The electronic collimation is realized by using a 0.3mm diameter 22Na point source and a coincidence reference detector consisting of a single LYSO crystal of 1×1×20 mm3. The mechanical collimation is realized by using a 5mm thick tungsten block with a 1mm diameter hole drilled. The centroid of gravity (COG) and squared COG algorithms were used to determine the y position, and the inverse standard deviation algorithm was applied to obtain the DOI information. All slabs are clearly identified from the flood histograms of both detectors. The average peak-to-valley ratios (PVRs), calculated from the line profiles through the center y-axis of the flood histograms, are 3.96 and 3.55 for detectors 1 and 2, respectively. The average energy resolutions are 15.6 ± 1.8% for detector 1 and 14.7 ± 1.2% for detector 2. The COG method provides y-position resolutions of 2.21 ± 0.77mm for detector 1 and 2.16 ± 0.55mm for detector 2, whereas the squared COG method provides y-position resolutions of 1.60 ± 0.32mm and 1.59 ± 0.26mm, respectively. The average DOI resolutions are 2.33 ± 0.68mm for detector 1 and 2.37 ± 0.58mm for detector 2. The average timing resolutions are 4.30 ± 0.57 ns for detector 1 and 4.76 ± 0.56 ns for detector 2. Compared to the detector using LYSO scintillator slabs, the detector using GAGG scintillator slabs provides similar y-position and DOI resolutions, a better energy resolution, a better PVR in the flood histogram and a worse timing resolution. In this work, the performance of two semi-monolithic scintillator detectors composed of GAGG slabs was investigated for the first time. The detector using the ESR reflector achieved similar y-position and DOI resolutions, slightly better energy resolution, and a poorer flood histogram compared to the detector using the BaSO4 reflector. Both detectors clearly identified all scintilator slabs with a thickness of 0.96mm, achieved y-position resolutions of ~ 1.6mm, DOI resolutions of ~ 2.3mm, and energy resolutions of ~ 15%. These detectors are suitable for developing small-animal and high-resolution organ-specific PET scanners.

Abstract This work presents a detailed spectroscopic case study of four long-duration transition-region (TR) explosive events (EEs) observed in NOAA Active Region 13213 on 2023 February 10 using the Interface Region Imaging Spectrograph. The dynamic spectral evolution of each event is tracked through multicomponent Gaussian fitting of the Si iv 1403 Å line profiles. Three recurrent spectral morphologies are identified and characterized: bilateral wing enhancement, exclusive red-wing enhancement, and exclusive blue-wing enhancement, among which bilateral enhancement is the most common in the studied cases. Throughout their lifetimes of 20–25 minutes, these events display sustained and evolving bidirectional flows, with high-velocity components (∣ v ∣ > 100 km s −1 ) emerging in late phases. These spectral signatures are interpreted as evidence of ongoing or recurrent magnetic reconnection, where bilateral profiles correspond to bidirectional outflows, and exclusive wing enhancements represent geometric or evolutionary phases of the same process. In contrast, cotemporal flare ribbons and loop structures exhibit pronounced, unidirectional redshifts. This study underscores that significant non-Gaussian wing enhancement, rather than exclusively high speed, constitutes a defining spectroscopic signature of EEs, and provides detailed kinematic constraints on the dynamics of such TR EEs.

Abstract We present a detailed model atmosphere analysis of hot white dwarfs in the Dark Energy Spectroscopic Instrument (DESI) Data Release 1. Our sample includes 19,321 unique targets with G BP − G RP ≤ 0. We use the DESI spectra along with Gaia parallaxes and Sloan Digital Sky Survey (SDSS), Pan-STARRS, and SkyMapper photometry to perform spectroscopic and photometric fits. We find a significant discrepancy between the photometric and spectroscopic masses for DA white dwarfs (a systematic offset of 0.05–0.06 M ⊙ ), indicating problems with the broad hydrogen line profiles in DESI spectroscopy data. Our photometric fits are consistent with a peak at the canonical mass of 0.6 M ⊙ . A remarkable feature of the mass distribution is the prevalence of magnetic white dwarfs among the ultramassive DA population and that of warm DQs in the non-DA distribution. We identify 70 DQs in the DESI hot white dwarf sample, including nine DAQs with carbon and hydrogen atmospheres. We constrain the ratio of non-DA to DA white dwarfs as a function of temperature, and discuss the implications for the spectral evolution of white dwarfs in the temperature range of 10 5 –10 4 K. We also discuss unusual objects in the sample, including metal-rich white dwarfs and extremely low-mass white dwarfs. This analysis provides the first look at the large sample of Gaia-selected white dwarf candidates that will be observed with multiplexed spectroscopic surveys such as DESI, SDSS-V, the 4 m Multi-Object Spectroscopic Telescope, and the William Herschel Telescope Enhanced Area Velocity Explorer over the next several years.

Abstract Electromagnetically induced transparency (EIT) can greatly reduce the group velocity of light, which has extensive applications in optical sensing, optical storage, etc, and it has been widely studied in visible and microwave wavelengths. In the X-ray regime, EIT was realized in an X-ray thin-film planar cavity, while the detection of the transparency window in the reflection direction is not easy. Due to the interference between the bare cavity reflection and the nuclear resonance, the spectral line profile can be manipulated by adjusting the phases and amplitudes of different channels. By varying the thickness of the top layer, we demonstrate that in the X-ray regime, the spectral line can be transformed from a dip to a peak at the resonant window while maintaining the slow light effect. The slow light ability is evaluated by calculating the group velocity, the interaction strength, and the clarification of EIT and Autler Townes splitting (ATS). As the interaction strength increases, the X-ray cavity transitions from EIT to EIT-ATS crossover regime, which is consistent with the variation of group velocity. The present work would facilitate the detection of slow X-ray light using the cavity system and be helpful for the EIT and ATS clarification studies.

Transmission spectroscopy has advanced our understanding of exoplanet atmospheres, but it can be hindered by contamination originating in stellar heterogeneities, mainly coming from line-of-sight effects. Therefore, probing how stellar spectra vary across the stellar surface is essential to accurately disentangling stellar and planetary spectral contributions in transit observations. Such observations can actually be used to reconstruct the local stellar spectra behind the planet's transit chord. These methodologies can help us learn more about the physics of stellar surface and how to tackle line-of-sight effects. In this paper, we study the centre-to-limb variations of line profiles across the surface of HD 189733 using the ESPRESSO spectrograph. We build on other works by analysing the same sets of lines, allowing for a direct comparison of results and an assessment of the feasibility of applying the Doppler shadow technique with ESPRESSO. We gain a better understanding of the variations in line profiles, while also making a comparison between the data of HD 189733 and synthetic spectra and solar data. Fe I We analysed spectra collected by ESPRESSO during two transits of HD 189733 b as separate sets of data. We performed a cross-correlation of each individual spectrum with two different masks made of selected spectral lines for a total of four sets of cross-correlation functions (CCFs) and employed a Doppler shadow methodology to retrieve profiles for local regions of the stellar surface. We then compared the results with previous works and with solar disc-resolved observations from IAG ATLAS. Finally, we compared the data with two separate transit simulations made using SOAPv4 with Turbospectrum synthetic spectra computed with MARCS stellar atmosphere models under local thermal equilibrium (LTE) and non-LTE (NLTE) conditions. Fe I For the profile depth of three sets of CCFs, we verified a statistically significant increase in line depth from the stellar limb to the centre. This variation was expected from simulations with MARCS models, although the solar data present a smaller gradient in the variation of line depth. In the case of the width of the line profiles, we verified that the profile width decreases from stellar limb to stellar centre for a set of CCFs. This result is consistent with the behaviour observed in solar data, but not reproduced by the simulations. Fe I Fe I These results highlight the abilities of ESPRESSO in providing the necessary precision and resolution to study centre-to-limb variations of spectral line profiles on the surface of other stars with the use of CCFs. The local CCF profiles of HD 189733 agree with the IAG ATLAS data, but disagree with simulations on line widths, indicating that important physical processes are missing and must be included to recover accurate profile widths.

In single-cell spatial phenotyping biology, imaging mass cytometry (IMC) stands out as a cutting-edge, highly multiplexed technology driving discoveries across various disease areas. Invitro profiling relies on tumor-derived cancer cell lines, known for their diverse morphologies and phenotypes. A comprehensive analysis of those cell lines presents a direct challenge in predicting cancer progression and drug treatment responses. We demonstrate in our study an adaptable computational workflow we have named IMC Cell Line Profiler as a suite of versatile open-source tools for visual rendering and quantitative segmentation-based analysis of tumor-derived cell lines profiled by IMC. By leveraging our workflow with IMC resolution and multiplexing capabilities, we scrutinized the morphology, phenotypic traits, and spatial arrangement of 10 cultured cell lines from diverse tissues using custom panels of 20-30 metal-labeled antibodies. This allowed us to generate intricate high-dimensional datasets elucidating diverse cellular states with multiple markers. This computational approach was applied to a cisplatin exposure treatment in a resistant cell line to track morpho-phenotypic changes. Our IMC computational study presents new perspectives and applications to profile cell lines as new types of samples and expand the potential of IMC to new fields of discovery.

Effect of ahfad2 genes on oil profile of advanced breeding lines in groundnut (Arachis hypogaea L.)

The phosphorus abundance distribution in field stars as a function of metallicity reveals a complex pattern. The local thermodynamic equilibrium (LTE) data for P/Fe in the low-metallicity range are sparse and scattered around P/Fe ≈ 0 dex. Near Fe/H $≈ -2$ dex, the relative abundance P/Fe increases and reaches a maximum value of around Fe/H ≈ -1 dex. In this domain, many phosphorus-rich (P-rich) stars and (super)phosphorus-rich stars are observed; the P/Fe value can exceed 1 dex. Until now, no attempts have been made to study the non-local thermodynamic equilibrium (non-LTE) effects on the ultraviolet and infrared phosphorus lines in spectra of cool stars to test the robustness of the observed LTE phosphorus abundance distribution. We developed an atomic model of that can be used to analyze phosphorus lines in the spectra of cool dwarfs and giants in the non-LTE approximation. The model consists of 101 energy levels of and the ground level of ; 1070 transitions between mentioned levels were studied. The model was tested using the solar flux and intensity spectra, as well as the spectra of Procyon and σ Boo. Profiles of 14 phosphorus lines in the infrared regions and equivalent widths were analyzed. Our non-LTE phosphorus abundance in the Sun is (P/H) = 5.35 ± 0.04 dex. P i P i P ii Using our non-LTE model, we selected 12 ultraviolet and infrared phosphorus lines and calculated a grid of non-LTE corrections for the following parameter ranges: T_ = 2$ km s eff from 4000 to 6750 ,K, step 250 ,K; log g from 1 to 5 dex, step 1 dex; and V$_ t -1 $, Fe/H from --3 to +0.5 dex, step 0.5 dex. The non-LTE corrections (Abundance_ ) were calculated for phosphorus abundance ratios of non-LTE -- Abundance$_ LTE P/Fe = --0.4, 0.0, and +0.4 dex. For the Sun, the non-LTE correction is --0.08 dex. The grid of the non-LTE corrections, as well as the direct line profile synthesis, were used to refine the literature data on the phosphorus abundance in metal-poor, intermediate-deficient, and solar-metallicity stars. This sample also includes phosphorus-rich stars. Non-LTE corrections do not qualitatively alter the overall phosphorus abundance distribution over a wide metallicity range, and do not change the characteristic pattern of phosphorus-rich stars. After corrections, the phosphorus abundance distribution became more compact in the low-metallicity range. Overall, the observed phosphorus abundance distribution can be described by the combined effect of phosphorus production in rotating massive stars, Type II supernovae explosions, and oxygen-neon-magnesium novae.