Identification of the region of non-A beta component (NAC) of alzheimer's disease amyloid responsible for its aggregation and toxicity

The non-beta-amyloid (Aß) component of Alzheimer's disease amyloid (NAC) and its precursor a-synuclein have been linked to amyloidogenesis in several neurodegenerative diseases. NAC and a-synuclein both form ß-sheet structures upon ageing, aggregate to form fibrils, and are neurotoxic. We recently established that a peptide comprising residues 3±18 of NAC retains these properties. To pinpoint the exact region responsible we have carried out assays of toxicity and physicochemical properties on smaller fragments of NAC. Toxicity was measured by the ability of fresh and aged peptides to inhibit the reduction of the redox dye 3-(4,5-dimethylthiazol-2-yl)-2,5 diphenyltetrazolium bromide (MTT) by rat pheochromocytoma PC12 cells and human neuroblastoma SHSY-5Y cells. On immediate dissolution, or after ageing, the fragments NAC(8±18) and NAC(8±16) are toxic, whereas NAC(12±18), NAC(9±16) and NAC(8±15) are not. Circular dichroism indicates that none of the peptides displays ß-sheet structure; rather all remain random coil throughout 24 h. However, in acetonitrile, an organic solvent known to induce ß sheet, fragments NAC(8±18) and NAC(8±16) both form ß-sheet structure. Only NAC(8±18) aggregates, as indicated by concentration of peptide remaining in solution after 3 days, and forms fibrils, as determined by electron microscopy. These findings indicate that residues 8±16 of NAC, equivalent to residues 68±76 in a-synuclein, comprise the region crucial for toxicity.

Qutting and restarting smoking: cohort study of patients with angina in primary care

Objective To examine variations in self-reported smoking habit among a cohort of individuals with chronic coronary heart disease over a five year period. Design Cross-sectional cohort; interviews at baseline, 2 years and 5 years. Setting Primary care. Participants A cross-sectional sample of 688 patients previously diagnosed as having angina, identified from 18 general practices in the Greater Belfast Area; a cohort of 487 were followed for five years. Outcome measures Changes in self-reported smoking habits; breath carbon monoxide measurement. Results Initially 92 of the 487 participants (19%) reported smoking, 34 (27%) subsequently reported non-smoking. Of the 395 self-reported non-smokers at baseline, 21 (5%) subsequently reported smoking. The prevalence of self-reported smoking amongst the cohort was 19% and 15% at two and five years respectively. However, changes in reported smoking habits indicating periods of abstinence and resumption were reported by 55/487 (11%) participants. Of the 21 non-smokers who changed their report, 20 had smoked previously, five reported having stopped for less than one year but nine for more than five years. Of the initial sample twice as many smokers as non-smokers had died by 2 years (10% v 5%; p

Chemical composition of B-type supergiants in the OB 8, OB 10, OB 48, OB 78 associations of M 31

Absolute and differential chemical abundances are presented for the largest group of massive stars in M31 studied to date. These results were derived from intermediate resolution spectra of seven B-type supergiants, lying within four OB associations covering a galactocentric distance of 5-12 kpc. The results are mainly based on an LTE analysis, and we additionally present a full non-LTE, unified model atmosphere analysis of one star (OB 78-277) to demonstrate the reliability of the differential LTE technique. A comparison of the stellar oxygen abundance with that of previous nebular results shows that there is an off set of between similar to0.15-0.4 dex between the two methods which is critically dependent on the empirical calibration adopted for the R 23 parameter with [O/H]. However within the typical errors of the stellar and nebular analyses (and given the strength of dependence of the nebular results on the calibration used) the oxygen abundances determined in each method are fairly consistent. We determine the radial oxygen abundance gradient from these stars, and do not detect any systematic gradient across this galactocentric range. We find that the inner regions of M31 are not, as previously thought, very "metal rich". Our abundances of C, N, O, Mg, Si, Al, S and Fe in the M31 supergiants are very similar to those of massive stars in the solar neighbourhood.