No abstract available

[en] The antibiotic, disodium (+)-(Z)-[[[1-(2-amino-4-[2-¹⁴C]thiazolyl)-2-[[(2S,3S)-2-(carbamoyloxymethyl) -4-oxo-1-sulfonato-3-azetizinyl]amino-2-oxoethylidene]-amino]oxy]acetate([¹⁴C]AMA-1080) was synthesized from [¹⁴C]thiourea. Trisodium(+)-(Z)-[[[1-(2-amino-4-[2-¹⁴C]thiazolyl)-2-[[(1S,2S)-3-carbamoyloxy-1-carboxylato-2-sulfonatoaminopropyl]amino]-2-oxoethylidene]amino]oxy] acetate([¹⁴C]AMA-1294) as the principal metabolite of [¹⁴C]AMA-1080 was also prepared. (author)

[en] One of the most challenging open questions in Astrophysics is how Active Galactic Nuclei (AGNs) are fueled. For this to happen, gas has to be driven from the outskirts of the galaxy to the nuclear regions. Different mechanisms such as bars (large-scale and nuclear), lopsided disks, m=1, 2 instabilities or warps have been suggested to remove the gas angular momentum at different spatial scales of galaxy disks. On the other hand, stellar and AGN feedback in the form of outflows prevents galaxies from becoming overmassive. In this work we present the results of interferometric observations of the cold CO(2-1) molecular gas and 1.3 mm continuum obtained with NOEMA of five nearby (mean luminosity distance of 34 Mpc) Seyfert galaxies. The superb angular resolution of the NOEMA data (0.6 100 pc) enables us to study the CO(2-1) morphology and kinematics as well as to measure the molecular gas content of the nuclear regions. Although all galaxies in our sample show evidence of non-circular motions in their nuclear regions, these are detected more clearly in the interacting systems. Our goal is to find out if these motions are related to molecular gas flows.

[en] We report four patients in whom gas was seen in the head on CT shortly after cardiopulmonary resuscitation. The gas was in the posterior cranial fossa, presumably within veins, or in the cavernous sinus. The cause of the cardiac arrest was myocardial infarction in three patients and hanging in one. All had peripheral or central venous lines. The mechanism by which gas appeared in the intracranial veins is discussed. (orig.)

[en] We have demonstrated a GaN growth technique in the Na flux method to confine c-, (a+c)-, and a-type dislocations around the interface between a Na flux GaN crystal and a GaN layer grown by metalorganic chemical vapor deposition (MOCVD) on a (0001) sapphire substrate. Transmission electron microscopy (TEM) clearly revealed detailed interface structures and dislocation behaviors that reduced the density of vertically aligned dislocations threading to the Na flux GaN surface. Submicron-scale voids were formed at the interface above the dislocations with a c component in MOCVD-GaN, while no such voids were formed above the a-type dislocations. The penetration of the dislocations with a c component into Na flux GaN was, in most cases, effectively blocked by the presence of the voids. Although some dislocations with a c component in the MOCVD-GaN penetrated into the Na flux GaN, their propagation direction changed laterally through the voids. On the other hand, the a-type dislocations propagated laterally and collectively near the interface, when these dislocations in the MOCVD-GaN penetrated into the Na flux GaN. These results indicated that the dislocation propagation behavior was highly sensitive to the type of dislocation, but all types of dislocations were confined to within several micrometers region of the Na flux GaN from the interface. The cause of void formation, the role of voids in controlling the dislocation behavior, and the mechanism of lateral and collective dislocation propagation are discussed on the basis of TEM results

[en] We report the detection of a heavily obscured active galactic nucleus (AGN) in the luminous infrared galaxy (LIRG) NGC 6286 identified in a 17.5 ks Nuclear Spectroscopic Telescope Array observation. The source is in an early merging stage and was targeted as part of our ongoing NuSTAR campaign observing local luminous and ultra-luminous infrared galaxies in different merger stages. NGC 6286 is clearly detected above 10 keV and by including the quasi-simultaneous Swift/XRT and archival XMM-Newton and Chandra data, we find that the source is heavily obscured (N_H ≃(0.95−1.32) × 10²⁴ cm⁻²) with a column density consistent with being Compton-thick (CT, $\mathrm{l}\mathrm{o}\mathrm{g}(N_{\mathrm{H}}/{\mathrm{c}\mathrm{m}}^{-<!--\; ???\; -->2})⩾<!--\; ???\; -->24$). The AGN in NGC 6286 has a low absorption-corrected luminosity (L_{2−10 keV} ∼ 3−20 × 10⁴¹ erg s⁻¹) and contributes ≲1% to the energetics of the system. Because of its low luminosity, previous observations carried out in the soft X-ray band (<10 keV) and in the infrared did not notice the presence of a buried AGN. NGC 6286 has multiwavelength characteristics typical of objects with the same infrared luminosity and in the same merger stage, which might imply that there is a significant population of obscured low-luminosity AGNs in LIRGs that can only be detected by sensitive hard X-ray observations.

[en] We used the Atacama Large Millimeter/Submillimeter Array to map the CO(3–2) and the underlying continuum emissions around the type-1 low-luminosity active galactic nucleus (LLAGN; bolometric luminosity $\lesssim <!--\; ???\; -->{10}^{42}$ erg s⁻¹) of NGC 1097 at ∼10 pc resolution. These observations revealed a detailed cold gas distribution within a ∼100 pc of this LLAGN. In contrast to the luminous Seyfert galaxy NGC 1068, where a ∼7 pc cold molecular torus was recently revealed, a distinctively dense and compact torus is missing in our CO(3–2) integrated intensity map of NGC 1097. Based on the CO(3–2) flux, the gas mass of the torus of NGC 1097 would be a factor of ≳2–3 less than that found for NGC 1068 by using the same CO-to-H₂ conversion factor, which implies less active nuclear star formation and/or inflows in NGC 1097. Our dynamical modeling of the CO(3–2) velocity field implies that the cold molecular gas is concentrated in a thin layer as compared to the hot gas traced by the 2.12 μm H₂ emission in and around the torus. Furthermore, we suggest that NGC 1097 hosts a geometrically thinner torus than NGC 1068. Although the physical origin of the torus thickness remains unclear, our observations support a theoretical prediction that geometrically thick tori with high opacity will become deficient as AGNs evolve from luminous Seyferts to LLAGNs.