Coalescence of Molecular Filaments

Star-forming molecular filaments are found to display a spectrum of line-masses (mass per unit length)1. This spectrum is thought to influence key observational parameters of star formation2 including the core and stellar initial mass function1. The exact mechanism producing the wide-range of line-masses is unknown, even though, higher surface densities are often observed at the intersection of filaments in hub-filament systems3. Here we show that cascades of lower density filaments coalescing to form higher density filaments and eventually hubs. By performing a multi-scale decomposition of surface density maps of the MonR2 star-forming region, which displays a spiral-shaped hub-filament system4, the coalescence effect is detected in two consecutive cascading steps (the surface density jumps by an order of magnitude at each step) before merging at the central hub which is found to be a dense network of short high-density filaments (as opposed to its view as a massive clump). The radial density structure of the dense-gas component of the hub-filament system shows a power-law dependence of NH2 ∝ r−2 over the scale of ∼5 pc, a feature previously found only at scales of 0.1 pc in star-forming cores5. It appears that the hub-filament system is mimicking the radial profile of an isothermal sphere, at parsec scales, a feature not known until now. This behavior is not seen for the diffuse cloud (NH2 ∝ r−0.5) which holds nearly equal mass. The filamentary nature of the hub implies that only some (embedded in the filaments), and not all, stellar seeds within the hub can become massive stars.

Cirsium Setidens Extracts Abrogate Actin Ring Formation and Bone-Resorbing Osteoclasts Through Inhibition of Core-Linked CD44 and Diffuse Cloud-Associated αvβ3 Integrin

Objectives Since enhanced bone resorption cause skeletal diseases, there is a growing need in therapeutics for combating bone-resorbing osteoclasts. Botanical antioxidants are being increasingly investigated for their health-promoting effects on bone. Cirsium setidens (Korean thistle) contains linarin, luteolin, pectolinarin, hispidulin, and apigenin with antioxidant and hepatoprotective effects. This study examined whether 1–20 μg/ml Cirsium setidens extracts (CSE) inhibited osteoclastogenesis of RANKL-exposed RAW 264.7murine. Methods RAW 264.7 murine macrophages were incubated with 1–20 μg/ml CSE for 5 days in the presence of 50 ng/ml RANKL. Tartrate-resistance acid phosphatase (TRAP) staining and its activity measurement were performed. Western blotting was done with target proteins involved in the osteoclast activation. Results Nontoxic CSE attenuated the RANKL-induced macrophage differentiation into multinucleated osteoclasts, and curtailed bone resorption through reducing lacunar acidification and bone matrix degradation. Linarin and pectolinarin were identified as major components of CSE, where linarin but not pectolinarin were effective in inhibiting formation of TRAP-positive osteoclasts. Linarin-rich CSE diminished the induction of αvβ3 integrin-associated proteins of paxillin, Pyk2 and gelsolin. Additionally, CSE deterred actin ring formation with attenuation of induction of F-actin-enriched podosome core proteins of CD44, Arp2/3 and cortactin. Nontoxic linarin and its aglycone acacetin reduced focal contact of osteoclasts to RGD peptide. The inhibition of integrin-mediated actin ring formation by CSE entailed disruption of TRAF6-c-Src-PI3K signaling of osteoclasts. Conclusions CSE was effective in retarding focal adhesion to bone matrix and active bone resorption of osteoclast via inhibition of core-linked CD44 and diffuse cloud-associated αvβ3 integrin. Funding Sources This work was supported by the National Research Foundation of Korea(NRF) grant funded by the Korea government(MSIT) (2019R1A2C1003218).

Spectral study of scattered light by interstellar dust grains

Interstellar dust is traced by not only thermal emission but also scattered light. The scattered light spectrum observed from ultraviolet (UV) to near-infrared (IR) is useful to constrain some dust properties, such as size distribution, albedo, and composition. Milky Way Galaxy is a unique environment to observe the diffuse scattered light because we can extract it by removing the contribution of starlight. We have observed the UV to near-IR scattered light with space instruments, including Diffuse Infrared Background Experiment (DIRBE), Hubble Space Telescope (HST), and Multi-purpose Infra-Red Imaging System (MIRIS). The scattered light spectrum is marginally consistent with prediction from a recent dust model including carbonaceous and silicate grains with polycyclic aromatic hydrocarbon (PAH). Based on the MIRIS observation of a diffuse cloud, we compare the scattered light color with the dust model with or without grains larger than 1 micrometer. The result shows that the color is consistent with the model without the large grains, which is consistent with recent simulations of dust growth in low-density regions. However, some observations have shown the spectral excess at ∼ 0.6 micrometer wavelength, suggesting the presence of extended red emission (ERE) which cannot be explained by the conventional dust model.

3D AMR simulations of the evolution of the diffuse gas cloud G2 in the Galactic Centre

With the help of 3D AMR hydrodynamical simulations we aim at understanding G2’s nature, recent evolution and fate in the coming years. By exploring the possible parameter space of the diffuse cloud scenario, we find that a starting point within the disc of young stars is favoured by the observations, which may hint at G2 being the result of stellar wind interactions.

Dehydration and cation replacement dramatically improve crystals of large RNAs

Preparation of well-ordered crystals of large RNAs remains a daunting experimental challenge. This probably reflects the relatively undifferentiated molecular surface of folded RNAs (dominated by a regular array of phosphates), the comparatively low free energy of RNA tertiary structure stabilization, and the resulting tendency of RNAs to be conformationally polydisperse. We have found empirically that dehydration and exchange of counterions, can dramatically improve the diffraction properties of some RNA crystals. Two examples from our work are crystals of the glmS ribozyme-riboswitch [1] and of the ternary complex of a T-box riboswitch, its cognate tRNA and an RNA binding protein [2]. Untreated, flash-frozen crystals of the glmS ribozyme diffracted synchrotron X-rays to 3.3 Å resolution. Upon controlled dehydration by soaking into solutions with higher osmolarity, the unit cell contracted by approximately 10%, and diffraction data could be collected that extended to 1.7 Å resolution. Untreated crystals of the T-box ternary complex diffracted X-rays only to 8 Å resolution. A combination of controlled dehydration and exchange of the magnesium an lithium ions needed for crystal growth with strontium (a soft divalent cation), dramatically extended the diffraction limit, allowing the structure to be solved by SAD at 3.2 Å resolution. Because it is a polyanion, RNA is heavily hydrated and surrounded by a diffuse cloud of counterions. It can also site-specifically bind to partially or wholly desolvated metal ions. Hydration and ion binding not only control RNA folding, but also modulate crystallogenesis. Therefore, controlled dehydration and cation exchange are post-crystallization treatments that should be routinely explored for RNA. This work was supported in part by the Intramural Program of the National Heart, Lung and Blood Institute.

Stability of carbonaceous dust analogues and glycine under UV irradiation and electron bombardment

The effect of UV photon (120–200 nm) and electron (2 keV) irradiation of analogues of interstellar carbonaceous dust and of glycine were investigated by means of IR spectroscopy. Films of hydrogenated amorphous carbon (HAC), taken as dust analogues, were found to be stable under UV photon and electron bombardment. High fluences of photons and electrons, of the order of 1019cm−2, were needed for a film depletion of a few percent. UV photons were energetically more effective than electrons for depletion and led to a certain dehydrogenation of the HAC samples, whereas electrons led seemingly to a gradual erosion with no appreciable changes in the hydrocarbon structure. The rates of change observed may be relevant over the lifetime of a diffuse cloud, but cannot account for the rapid changes in hydrocarbon IR bands during the evolution of some proto-planetary nebulae. Glycine samples under the same photon and electron fluxes decay at a much faster rate, but tend usually to an equilibrium value different from zero, especially at low temperatures. Reversible reactions re-forming glycine, or the build-up of less transparent products, could explain this behavior. CO2and methylamine were identified as UV photoproducts. Electron irradiation led to a gradual disappearance of the glycine layers, also with formation of CO2. No other reaction products were clearly identified. The thicker glycine layers (a few hundred nm) were not wholly depleted, but a film of the order of the electron penetration depth (80 nm), was totally destroyed with an electron fluence of ∼1 × 1018cm−2. A 60 nm ice layer on top of glycine provided only partial shielding from the 2 keV electrons. From an energetic point of view, 2 keV electrons are less efficient than UV photons and, according to literature data, much less efficient than MeV protons for the destruction of glycine. The use of keV electrons to simulate effects of cosmic rays on analogues of interstellar grains should be taken with care, due to the low penetration depths of electrons in many samples of interest.

Radio emission from the bow shock of G2

The radio flux from the synchrotron emission of electrons accelerated in the forward bow shock of G2 is expected to have peaked when the forward shock passes close to the pericenter from the Galactic center, around autumn of 2013. This radio flux is model dependent. We find that if G2 were to be a momentum-supported bow shock of a faint star with a strong wind, the radio synchrotron flux from the forward-shock heated ISM is well below the quiescent radio flux of Sgr A*. By contrast, if G2 is a diffuse cloud, the radio flux is predicted to be much larger than the quiescent radio flux and therefore should have already been detected or will be detected shortly. No such radiation has been observed to date. Radio measurements can reveal the nature of G2 well before G2 completes its periapsis passage.