Staphylococcus aureus from patients with chronic rhinosinusitis show minimal genetic association between polyp and non-polyp phenotypes

Background: Staphylococcus aureus has a high prevalence in chronic rhinosinusitis (CRS) patients and is suggested to play a more etiopathogenic role in CRS patients with nasal polyps (CRSwNP), a severe form of the CRS spectrum with poorer surgical outcomes. We performed a microbial genome-wide association study (mGWAS) to investigate whether S. aureus isolates from CRS patients have particular genetic markers associated with CRS with nasal polyps (CRSwNP) or CRS without nasal polyps (CRSsNP). Methods: Whole genome sequencing was performed on S. aureus isolates collected from 28 CRSsNP and 30 CRSwNP patients. A mGWAS approach was employed using large-scale comparative genomics to identify genetic variation within our dataset. Results: Considerable genetic variation was observed, with >90,000 single nucleotide polymorphisms (SNPs) sites identified. There was little correlation with CRS subtype based on SNPs and Insertion/Delection (Indels). One indel was found to significantly correlate with CRSwNP and occurred in the promoter region of a bacitracin transport system ATP-binding protein. Additionally, two variants of the highly variable superantigen-like (SSL) proteins were found to significantly correlate with each CRS phenotype. No significant association with other virulence or antibiotic resistance genes were observed, consistent with previous studies. Conclusion: To our knowledge this study is the first to use mGWAS to investigate the contribution of microbial genetic variation to CRS presentations. Utilising the most comprehensive genome-wide analysis methods available, our results suggest that CRS phenotype may be influenced by genetic factors other than specific virulence mechanisms within the S. aureus genome

Metal Abundances and Kinematics of Bright Metal-Poor Giants Selected from the LSE Survey: Implications for the Metal-Weak Thick Disk

We report medium-resolution (1-2 A) spectroscopy and broadband (UBV) photometry for a sample of 39 bright stars (the majority of which are likely to be giants) selected as metal-deficient candidates from an objective-prism survey concentrating on Galactic latitudes below |b| = 30 deg, the LSE survey of Drilling & Bergeron. Although the primary purpose of the LSE survey was to select OB stars (hence the concentration on low latitudes), the small number of bright metal-deficient giant candidates noted during this survey provide interesting information on the metal-weak thick disk (MWTD) population. The kinematics of the LSE giants indicate the presence of a rapidly rotating population, even at quite low metallicity. We consider the distribution of orbital eccentricity of the LSE giants as a function of [Fe/H], and conclude that the local fraction (i.e., within 1 kpc from the Sun) of metal-poor stars that might be associated with the MWTD is on the order of 30%-40% at abundances below [Fe/H] = -1.0. Contrary to recent analyses of previous (much larger) samples of non-kinematically selected metal-poor stars, we find that this relatively high fraction of local metal-poor stars associated with the MWTD may extend to metallicities below [Fe/H] = -1.6, much lower than had been considered before. We identify a subsample of 11 LSE stars that are very likely to be members of the MWTD, based on their derived kinematics; the lowest metallicity among these stars is [Fe/H] = -2.35. Implications of these results for the origin of the MWTD and for the formation of the Galaxy are considered. (abridged)Comment: 41 pages, 9 tables, 6 figures, accepted for publication in The Astronomical Journa

The Spectroscopic Orbit of the Evolved Binary HD 197770

We have used spectra taken between 1992 and 1997 to derive the spectroscopic orbit of the eclipsing double-lined spectroscopic binary HD 197770. This binary has a period of 99.69 +/- 0.02 days and K amplitudes of 31.2 +/- 0.8 and 47.1 +/- 0.4 km s^{-1} for components A & B, respectively. The msin^{3}i values for A & B are 2.9 and 1.9, respectively, and are close to the actual masses due to the eclipsing nature of this binary. Both components of HD 197770 have spectral types near B2 III. This means both components are undermassive by about a factor of five and, thus, evolved stars. Additional evidence of the evolved nature of HD 197770 is found in 25, 60, and 100 micron IRAS images of HD 197770. These images show 2 apparent shells centered on HD 197770; a bright 60 micron shell with a 14' diameter and a larger (1.2 degeree diameter) bubble-like feature. At least one of the components of HD 197770 is likely to be a post-AGB star.Comment: will be published in the AJ (1998 June), also availible at http://snake.phys.lsu.edu/~gordon/papers/hd197770.htm

Lovemore Park (formerly Buffelsfontein), 8 km west of Port Elizabeth central

At least 12 white milkwood Sideroxylon inerme trees on a small-holding. Cleared of its dense surrounding natural bush

The ultraviolet extinction curve for circumstellar dust formed in the hydrogen-poor environment of V348 Sagittarii

New International Ultraviolet Explorer (IUE) spectra with high signal-to-noise ratios have been obtained during the recovery of the hot R Coronae Borealis star, V348 Sgr, from its 1992 minimum. These spectra have been combined with spectra from the IUE archives to obtain a definitive extinction curve for dust recently ejected from this star, and make available for the first time an extinction curve of high accuracy in the far-UV for circumstellar dust formed in a hydrogen-poor environment. We find that a Drude profile with a central wavelength of 2425 Å and a full width at half-maximum of 1.342 μm-1 is able to satisfactorily represent the circumstellar dust ejected from V348 Sgr, not just during one ejection episode, but in general. We calculated theoretical extinction curves for comparison with the observed data using 400 Å graphite grains and 300 Å amorphous carbon grains. It is clear that scattering is very important at short wavelengths. Neither type of grain works very well when scattering is not included. The amorphous carbon fits are somewhat better than the graphite fits. The data seem to be more consistent with a cloud covering the entire star, and not just lying in our line of sight. This contradicts other empirical evidence that points toward the formation of patchy clouds around R Coronae Borealis stars. © 1997. The American Astronomical Society. All rights reserved

The efficacy and safety of chitosan dextran gel in a burr hole neurosurgical sheep model

BACKGROUND Achieving and maintaining haemostasis is of paramount importance in neurosurgery. Chitosan has been shown in both animal and human models to be significantly effective in haemostasis as well as in reducing adhesion formation. OBJECTIVES To evaluate the haemostatic potential and to study histopathological changes caused by novel chitosan dextran gel in a neurosurgical sheep model. METHOD Ten sheep underwent neurosurgical burr hole procedure. Bleeding control was tested at the level of bone, dura and brain separately with both chitosan gel and Gelfoam paste on separate burr holes. Baseline bleeding was measured at the time of injury using the Boezaart scale, and then every 2 min after the application of each agent until complete haemostasis or 10 min, whichever was earlier. Safety was assessed through MRI scans and histopathological analysis. RESULTS Mixed modeling showed no statistical difference in time to haemostasis between chitosan gel and Gelfoam paste (means of log-normalized areas under the curve were 1.3688 and 1.3196 respectively) for each burr hole (p  = 0.7768). Logistic regression modeling showed that Chitosan significantly decreased the incidence of bleeding beyond the first time point measured after application of the treatment when compared to Gelfoam (OR = 2.7, p = 0.04). Average edema volume (cm3) on post-operative MRI was 0.97 for Gelfoam and 1.11 for (p = 0.49) while average histology scores were 2.5 for Gelfoam versus 3.3 for chitosan (p = 0.32). CONCLUSION Chitosan dextran gel is an effective haemostatic agent to control bleeding in brain tissue. It is safe and nontoxic to neural tissue.Sukanya Rajiv, Marguerite Harding, Ahmed Bassiouni, Camille Jardeleza, Amanda Drilling, Craig James, Thanh Ha, Steve Moratti, Simon Robinson, Peter-John Wormal

Seismic structure across the rift valley of the Mid-Atlantic Ridge at 23020 ' (MARK area)' Implications for crustal accretion processes at slow spreading ridges

International audienceThe results from a 53‐km‐long, wide‐angle seismic profile across the rift valley of the Mid‐Atlantic Ridge south of the Kane transform (near 23°20′N, MARK area) provide new constraints on models of tectonic extension and magmatic accretion along slow spreading mid‐ ocean ridges. Anomalously low middle and lower‐crustal P wave velocities beneath the neovolcanic Snake Pit ridge are consistent with elevated axial temperatures and with the presence of 4±1% partial melt evenly distributed within the lower crust in preferentially oriented, elongated thin films. If the melt inclusions have larger aspect ratios, melt fractions can be up to 17±3%. This and other geological observations suggest that the study area is presently in a magmatically active period. The igneous crust is anomalously thin beneath both flanks of the median valley (≤2.3–2.5 km). Thus the mantle rocks observed along the western rift valley wall at Pink Hill were probably emplaced at shallow levels within the valley floor during a period of very low magma supply and were later exposed on the valley walls by normal faulting. The crust within the eastern rift valley and flanking rift mountains is seismically heterogeneous, with igneous crustal thickness variations of ≥2.2 km over horizontal distances of ∼5 km. This heterogeneity indicates that the magma supply in the area has fluctuated during the last ∼2 m.y. Thus magmatic and amagmatic periods at slow spreading ridges may alternate over much shorter temporal scales that previously inferred from sea surface gravity data