Search for: All records

Supercritical CO2-assisted impregnation (SCI) offers a sustainable route for embedding functional small molecules into polymer substrates, but its capacity to direct additive localization, interfacial organization, and solid-state structure, key determinants of optical, barrier, and controlled-release performance in multifunctional polymer composites and coatings, remains insufficiently understood. Herein, we elucidate how SCI processing governs the sorption, interfacial interactions, spatial localization, and release kinetics of vanillin, a model solid-phase bioactive compound, within semicrystalline cellulose. SCI enabled vanillin loadings ranging from 0.15 to 0.60 g g–1, with addition of polar cosolvents enhancing uptake by nearly 10-fold relative to neat CO2. By adjusting cosolvent environment and batch time, SCI directs the formation of distinct additive domains: surface-confined crystalline deposits at short times, bulk-dispersed amorphous regions at intermediate times, and recrystallized nanostructured domains once local additive concentrations exceed the dispersive capacity of cellulose. FTIR spectroscopic, X-ray photoelectron spectroscopic, X-ray diffraction, calorimetric, and electron microscopic characterization reveal that these SCI-driven interfacial interactions and phase states govern cellulose composite hydration, moisture-sorption hysteresis, and UV-shielding performance, where UVB transmittance ranges from 4–6% (surface crystalline) to 13–15% (matrix-embedded crystalline). Release experiments conducted in FDA/EU food simulants show that amorphous vanillin exhibits rapid, diffusion-controlled dissolution, reaching equilibrium (∼33 μg mL–1) within 180 min, whereas crystalline vanillin dispersed throughout the matrix exhibits delayed, anomalous release, showing a 30 min lag and ∼90 μg mL–1 equilibrium concentration after ∼10,000 min. Collectively, these results establish SCI as a versatile materials engineering platform that couples supercritical-fluid processing with control over interfacial chemistry and solid-state organization, enabling the design of sustainable cellulose-based composites with programmable optical, hygroscopic, and transport properties. 

Abstract While the cohesin complex is a key player in genome architecture, how it localizes to specific chromatin sites is not understood. Recently, we and others have proposed that direct interactions with transcription factors lead to the localization of the cohesin-loader complex (NIPBL/MAU2) within enhancers. Here, we identify two clusters of LxxLL motifs within the NIPBL sequence that regulate NIPBL dynamics, interactome, and NIPBL-dependent transcriptional programs. One of these clusters interacts with MAU2 and is necessary for the maintenance of the NIPBL–MAU2 heterodimer. The second cluster binds specifically to the ligand-binding domains of steroid receptors. For the glucocorticoid receptor (GR), we examine in detail its interaction surfaces with NIPBL and MAU2. Using AlphaFold2 and molecular docking algorithms, we uncover a GR–NIPBL–MAU2 ternary complex and describe its importance in GR-dependent gene regulation. Finally, we show that multiple transcription factors interact with NIPBL–MAU2, likely using interfaces other than those characterized for GR. 

Context.The archetypal blazar 3C 279 has a prominent relativistic jet and strong broadband variability across the electromagnetic spectrum. In April 2017, the Event Horizon Telescope (EHT) observed 3C 279 with an unprecedented angular resolution of about 20 μas, accompanied by one of the most extensive quasi-simultaneous multiwavelength (MWL) campaigns ever conducted, spanning from radio to TeVγ-ray energies. Aims.Taking advantage of this comprehensive MWL dataset, we investigated the physical processes governing 3C 279, with a particular focus on the formation, collimation, and acceleration of its relativistic jet and on the origin of its high-energy emission, including the underlying particle-acceleration mechanisms. Methods.We analyzed individual observations and multiband light curves. We also constructed a new quasi-simultaneous spectral energy distribution covering frequencies from the radio band to very high-energy (VHE)γrays. We further performed a phenomenological modeling using the turbulent extreme multi-zone (TEMZ) model to constrain the fundamental physical properties of the source. Results.The EHT observations reveal a clear flux increase in the innermost core between April 5 and 11, 2017. Over a broader time span, radio observations at longer wavelengths reveal concurrent enhancements in the core flux and polarization around mid-April, coinciding with the ejection of a superluminal knot moving at (25 ± 2)c. Record UV–optical flares with strong polarization variability occurred in late March, followed by high-energyγ-ray activity that declined before the end of the EHT observing period. During this time, the source remained in a low X-ray state and exhibited no detectable VHE emission. Conclusions.The results of the TEMZ modeling indicate that the broadband spectrum and variability of 3C 279 might be explained with a jet scenario in which turbulent plasma cells are compressed by a stationary conical shock. Nonetheless, alternative interpretations, such as magnetic reconnection or a moving shock-in-jet event, remain possible. This coordinated MWL campaign advances our understanding of the origin of the jet andγ-ray emission in the blazar 3C 279, and it also provides a comprehensive publicly available dataset that will serve as a valuable reference for future studies. 

In very-long baseline interferometric arrays, nearly co-located stations probe the largest scales and typically cannot resolve the observed source. In the absence of a large-scale structure, closure phases constructed with these stations are zero and, since they are independent of station-based errors, they can be used to probe data issues. Here, we show how these trivial closure phases become nonzero with a brightness distribution on smaller scales than their short baseline would suggest. When applied to sources that are made up of a bright compact and large-scale diffuse component, the trivial closure phases directly measure the centroid relative to the compact source and higher-order image moments. We present a technique to measure these image moments with minimal model assumptions and validate it on synthetic Event Horizon Telescope (EHT) data. We then apply this technique to 2017 and 2018 EHT observations of M87^*and find a weak preference for extended emission in the direction of the large-scale jet. We also apply it to 2021 EHT data and measure the source centroid about 1 mas northwest of the compact ring, which is consistent with the jet observed at lower frequencies. 

Context.Sagittarius A* (Sgr A^*), the supermassive black hole at the center of the Milky Way, provides a unique laboratory to study accretion dynamics and plasma processes near the event horizon. Aims.We investigated the variability and polarization properties of Sgr A^*using ALMA observations during the 2018 Event Horizon Telescope campaign. Methods.We analyzed high-cadence full-polarization light curves from ALMA at millimeter wavelengths, performed time-series analysis, and investigated the temporal behavior during an X-ray flare observed byChandraon 2018 April 24. The variability characteristics are compared with expectations from standard accretion flow models. Results.We find low variability in total intensity (σ/μ < 10%), but significantly higher variability in linear and circular polarization (∼30% and ∼50%, respectively). A time-series analysis reveals red-noise variability, with power spectral densities between −2 and −3 across all Stokes parameters. Polarized intensity shows stable intra-day timescales, while total intensity exhibits more variable timescales, suggesting distinct emission regions, with polarization likely arising from a coherent structure. On April 24, a statistically significant inter-band delay in polarized intensity coincides with a near-simultaneous X-ray and millimeter peak that deviates from the typical delayed flare scenario. This event also features enhanced millimeter variability and coherent polarization loop evolution. The observed simultaneity challenges standard models of transient synchrotron emission with cooling delays, favoring instead a scenario of continuous energy injection in an optically thin region. Conclusions.Our results offer new constraints on the physical mechanisms driving variability in Sgr A^*, and provide key observational input for refining theoretical models of accretion and plasma behavior in the vicinity of supermassive black holes. 

Abstract Event Horizon Telescope (EHT) images of the supermassive black hole M87* depict an asymmetric ring of emission. General relativistic magnetohydrodynamic (GRMHD) models of M87* and its accretion disk predict that the amplitude and location of the ring’s peak brightness asymmetry should fluctuate due to turbulence in the source plasma. We compare the observed distribution of brightness asymmetry amplitudes to the simulated distribution in GRMHD models, across varying black hole spina_*. We show that, for strongly magnetized (MAD) models, three epochs of EHT data marginally disfavor ∣a_*∣ ≲ 0.2. This is consistent with the Blandford–Znajek model for M87’s jet, which predicts that M87* should have nonzero spin. We show quantitatively how future observations could improve spin constraints and discuss how improved spin constraints could distinguish between differing jet-launching mechanisms and black hole growth scenarios.