Nitric oxide donors inhibit 5-hydroxytryptamine (5-HT) uptake by the human 5-HT transporter (SERT)

1 The aim was to test the hypothesis that nitric oxide ( NO) donor drugs can inhibit the 5-hydroxytryptamine (5-HT) transporter, SERT. 2 The NO donors, MAHMA/NO ( a NONOate; (Z)-1-[N-methyl-N-[6-(N-methylammoniohexyl)amino]]diazen- 1-ium-1,2-diolate), SIN-1 ( a sydnonimine; 5-amino-3-(4-morpholinyl)-1,2,3-oxadiazolium chloride), FK409 ( an oxime; (+/-)-(4-ethyl-2E-(hydroxyimino)-5-nitro-3E-hexenamide)) and peroxynitrite, but not Angeli's salt ( source of nitroxyl anion) or sodium nitrite, caused concentration-dependent inhibition of the specific uptake of [H-3]- 5-HT in COS-7 cells expressing human SERT. 3 Superoxide dismutase (150 U ml(-1)) plus catalase ( 1200 U ml(-1)), used to remove superoxide and hence prevent peroxynitrite formation, prevented the inhibitory effect of SIN-1 ( which generates superoxide) but not of MAHMA/NO or FK409. 4 The inhibitory effects of the NO donors were not affected by the free radical scavenger, hydroxocobalamin (1 mM) or the guanylate cyclase inhibitor, ODQ (1H-[ 1,2,4] oxadiazolo[4,3-a] quinoxalin-1-one; 3 muM). 5 L-Cysteine ( 1 mM; source of excess thiol residues) abolished or markedly reduced the inhibitory effects of MAHMA/NO, SIN-1, FK409 and peroxynitrite. 6 It is concluded that inhibition of SERT by the NO donors cannot be attributed exclusively to NO free radical nor to nitroxyl anion. It does not involve guanosine-3',5'-cyclic monophosphate, but may involve nitrosation of cysteine residues on the SERT protein. Peroxynitrite mediates the effect of SIN-1, but not the other drugs. 7 Data in mice with hypoxic pulmonary hypertension suggest that SERT inhibitors may attenuate pulmonary vascular remodelling. Thus, NO donors may be useful in pulmonary hypertension, not only as vasodilators, but also because they inhibit SERT, provided they display this effect in vivo at appropriate doses.

Optical precursors and Beer's law violations; non-exponential propagation losses in water

We develop a model for exponential decay of broadband pulses, and examine its implications for experiments on optical precursors. One of the signature features of Brillouin precursors is attenuation with a less rapid decay than that predicted by Beer's Law. Depending on the pulse parameters and the model that is adopted for the dielectric properties of the medium, the limiting z-dependence of the loss has been described as z(-1/2), z(-1/3), exponential, or, in more detailed descriptions, some combination of the above. Experimental results in the search for precursors are examined in light of the different models, and a stringent test for sub-exponential decay is applied to data on propagation of 500 femtosecond pulses through 1-5 meters of water. (C) 2005 Optical Society of America.

A Cochrane review (update 2004): Hylan G-F 20 vs placebo for knee OA

Aim of study: As part of a Cochrane review of viscosupplementation in knee OA, randomised controlled trials (RCT) were reviewed to evaluate evidence for the efficacy of viscosupplementation with Hylan G-F 20 compared to placebo. Methods: Electronic searches were conducted of MEDLINE, EMBASE, Premedline, Current Contents, and CENTRAL. Human, RCT involving Hylan G-F 20 compared to placebo, published prior to 1Q2004, were included. Trials were selected and data extracted by two independent reviewers. Methodological quality was assessed with the Jadad criteria by two reviewers. Data on the OARSI and OMERACT core set clinical outcome measures were extracted where possible. Weighted mean difference (WMD), based on post-test scores, and 95% confidence intervals (CI) were calculated for continuous outcome measures and relative risk (RR) for dichotomous outcome measures. Results: Seven RCT met the inclusion criteria. Median methodological quality was 4 (range 1–5). A further two studies were only reported in abstract form (Jadad score Z 1) and contained insufficient extractable data for inclusion in the analysis. Nine RCT, which compared Hylan G-F 20 to other interventions such as intra-articular corticosteroid, physiotherapy, NSAID, appropriate care, intra-articular gaseous oxygen and other hyaluronan, are not reported here. Twenty-three studies failed to meet inclusion criteria and were excluded. Hylan G-F 20 was more efficacious than placebo at 1–4 weeks post-injection for pain on weight-bearing WMD (random effects [RE]) 13 mm on a 0–100 mm VAS (P Z 0.002) based on 6 RCT. This difference was even greater at 5–13 weeks post-injection, 22 m (RE) (P Z 0.001) based on 5 RCT, and at 14–6 weeks postinjection, 21 m (RE) (P Z 0.006) based on 4 RCT. Hylan G-F 20 was more efficacious than placebo at 1–4 weeks post-injection for pain at night, WMD 7 mm on a 0–100 mm VAS (P Z 0.003) based on 5 RCT. This difference was even greater at 5–13 weeks post-injection, 11 mm (P Z 0.008) based on 4 RCT, and at 14–26 weeks post-injection, 17 mm (P ! 0.00001) based on 3 RCT. There was no significant difference (WMD 8 mm) between Hylan G-F 20 C oral placebo and arthrocentesis C oral placebo at 5–13 weeks post-injection for WOMAC Pain, but Hylan G-F 20 C oral placebo was more efficacious than arthrocentesis C oral placebo for WOMAC Function, WMD 9 mm on a 0–100 mm VAS (P Z 0.01) (Dickson, 2001). Hylan G-F 20 was more effective than placebo at 1–4 weeks postinjection for the variable designed treatment efficacy, WMD 22 mm on a 0–100 mm VAS (P ! 0.00001) based on improvement in 4 RCT. This difference was even greater at 5–13 weeks post injection, 35 mm (P ! 0.00001). Conclusions: Evidence from this updated Cochrane review supports the superior efficacy of Hylan G-F 20 compared to placebo on weight-bearing pain, night pain, function and treatment efficacy in the treatment of knee OA.

The 2dF-SDSS LRG and QSO (2SLAQ) survey: the z < 2.1 quasar luminosity function from 5645 quasars to g=21.85

We have used the Two-Degree Field (2dF) instrument on the Anglo-Australian Telescope (AAT) to obtain redshifts of a sample of z < 3 and 18.0 < g < 21.85 quasars selected from Sloan Digital Sky Survey (SDSS) imaging. These data are part of a larger joint programme between the SDSS and 2dF communities to obtain spectra of faint quasars and luminous red galaxies, namely the 2dF-SDSS LRG and QSO (2SLAQ) Survey. We describe the quasar selection algorithm and present the resulting number counts and luminosity function of 5645 quasars in 105.7 deg(2). The bright-end number counts and luminosity functions agree well with determinations from the 2dF QSO Redshift Survey (2QZ) data to g similar to 20.2. However, at the faint end, the 2SLAQ number counts and luminosity functions are steeper (i.e. require more faint quasars) than the final 2QZ results from Croom et al., but are consistent with the preliminary 2QZ results from Boyle et al. Using the functional form adopted for the 2QZ analysis ( a double power law with pure luminosity evolution characterized by a second-order polynomial in redshift), we find a faint-end slope of beta =-1.78 +/- 0.03 if we allow all of the parameters to vary, and beta =-1.45 +/- 0.03 if we allow only the faint-end slope and normalization to vary (holding all other parameters equal to the final 2QZ values). Over the magnitude range covered by the 2SLAQ survey, our maximum-likelihood fit to the data yields 32 per cent more quasars than the final 2QZ parametrization, but is not inconsistent with other g > 21 deep surveys for quasars. The 2SLAQ data exhibit no well-defined 'break' in the number counts or luminosity function, but do clearly flatten with increasing magnitude. Finally, we find that the shape of the quasar luminosity function derived from 2SLAQ is in good agreement with that derived from Type I quasars found in hard X-ray surveys.

The Las Campanas/Anglo-Australian Telescope Rich Cluster Survey - III. Spectroscopic studies of X-ray bright galaxy clusters at z similar to 0.1

We present the analysis of the spectroscopic and photometric catalogues of 11 X-ray luminous clusters at 0.07 < z < 0.16 from the Las Campanas/Anglo-Australian Telescope Rich Cluster Survey. Our spectroscopic data set consists of over 1600 galaxy cluster members, of which two-thirds are outside r(200). These spectra allow us to assign cluster membership using a detailed mass model and expand on our previous work on the cluster colour-magnitude relation ( CMR) where membership was inferred statistically. We confirm that the modal colours of galaxies on the CMR become progressively bluer with increasing radius d( B - R)/dr(p) = - 0.011 +/- 0.003 and with decreasing local galaxy density d( B - R)/dlog ( Sigma)= - 0.062 +/- 0.009. Interpreted as an age effect, we hypothesize that these trends in galaxy colour should be reflected in mean H delta equivalent width. We confirm that passive galaxies in the cluster increase in Hd line strength as dH delta/dr(p) = 0.35 +/- 0.06. Therefore, those galaxies in the cluster outskirts may have younger luminosity-weighted stellar populations; up to 3 Gyr younger than those in the cluster centre assuming d( B - R)/dt = 0.03 mag per Gyr. A variation of star formation rate, as measured by [ O II]lambda 3727 angstrom, with increasing local density of the environment is discernible and is shown to be in broad agreement with previous studies from the 2dF Galaxy Redshift Survey and the Sloan Digital Sky Survey. We divide our spectra into a variety of types based upon the MORPHs classification scheme. We find that clusters at z similar to 0.1 are less active than their higher-redshift analogues: about 60 per cent of the cluster galaxy population is non-star forming, with a further 20 per cent in the post-starburst class and 20 per cent in the currently active class, demonstrating that evolution is visible within the past 2 - 3 Gyr. We also investigate unusual populations of blue and very red non-star forming galaxies and we suggest that the former are likely to be the progenitors of galaxies which will lie on the CMR, while the colours of the latter possibly reflect dust reddening. We show that the cluster galaxies at large radii consist of both backsplash ones and those that are infalling to the cluster for the first time. We make a comparison to the field population at z similar to 0.1 and examine the broad differences between the two populations. Individually, the clusters show significant variation in their galaxy populations which we suggest reflects their recent infall histories.