Effects of the amphibian skin-derived bradykinin B2 receptor antagonist peptide, kinestatin, on the proliferation of human prostate cancer cell lines

Bradykinin and related peptides are found in the defensive skin secretions of many frogs and toads. While the physiological roles of bradykinin-related peptides in sub-mammalian vertebrates remains obscure, in mammals, including humans, canonical bradykinin mediates a multitude of biological effects including the proliferation of many types of cancer cell. Here we have examined the effect of the bradykinin B2 receptor antagonist peptide, kinestatin, originally isolated by our group from the skin secretion of the giant fire-bellied toad, Bombina maxima, on the proliferation of the human prostate cancer cell lines, PC3, DU175 and LnCAP. The bradykinin receptor status of all cell lines investigated was established through PCR amplification of transcripts encoding both B1 and B2 receptor subtypes. Following this demonstration, all cell lines were grown in the presence or absence of kinestatin and several additional bradykinin receptor antagonists of amphibian skin origin and the effects on proliferation of the cell lines was investigated using the MTT assay and by counting of the cells in individual wells of 96-well plates. All of the amphibian skin secretion-derived bradykinin receptor antagonists inhibited proliferation of all of the prostate cancer lines investigated in a dose-dependent manner. In addition, following incubation of peptides with each cell line and analysis of catabolites by mass spectrometry, it was found that bradykinin was highly labile and each antagonist was highly stable under the conditions employed. Bradykinin signalling pathways are thus worthy of further investigation in human prostate cancer cell lines and the evidence presented here would suggest the testing of efficacy in animal models of prostate cancer as a positive outcome could lead to a drug development programme for the treatment of this disease.

Nebular and auroral emission lines of [Cl III] in the optical spectra of planetary nebulae

Electron impact excitation rates in Cl III, recently determined with the R-matrix code, are used to calculate electron temperature (T-e) and density (N-e) emission line ratios involving both the nebular (5517.7, 5537.9 Angstrom) and auroral (8433.9, 8480.9, 8500.0 Angstrom) transitions. A comparison of these results with observational data for a sample of planetary nebulae, obtained with the Hamilton Echelle Spectrograph on the 3-m Shane Telescope, reveals that the R-1 = /(5518 Angstrom)/I(5538 Angstrom) intensity ratio provides estimates of N-e in excellent agreement with the values derived from other line ratios in the echelle spectra. This agreement indicates that R-1 is a reliable density diagnostic for planetary nebulae, and it also provides observational support for the accuracy of the atomic data adopted in the line ratio calculations. However the [Cl III] 8433.9 Angstrom line is found to be frequently blended with a weak telluric emission feature, although in those instances when the [Cl III] intensity may be reliably measured, it provides accurate determinations of T-e when ratioed against the sum of the 5518 and 5538 Angstrom line fluxes. Similarly, the 8500.0 Angstrom line, previously believed to be free of contamination by the Earth's atmosphere, is also shown to be generally blended with a weak telluric emission feature. The [CI III] transition at 8480.9 Angstrom is found to be blended with the He I 8480.7 Angstrom line, except in planetary nebulae that show a relatively weak He I spectrum, where it also provides reliable estimates of T-e when ratioed against the nebular lines. Finally, the diagnostic potential of the near-UV [Cl III] lines at 3344 and 3354 Angstrom is briefly discussed.

Nebular and Auroral Emission Lines of [Ar IV] in the Optical Spectra of Planetary Nebulae

Recent R-matrix calculations of electron impact excitation rates in Ar IV are used to calculate the emission-line ratio: ratio diagrams (R₁, R₂), (R_1, R₃), and (R_1, R₄), where K₁ = I(4711 Å)/I(4740 Å), R₂ = I(7238 Å)/I(4711 + 4740 Å), R₃ = I(7263 Å)/I(4711 + 4740 Å), and R₄ = I(7171 Å)/I(4711 + 4740 Å), for a range of electron temperatures (T_e = 5000-20,000 K) and electron densities (N_e = 10-10⁶ cm^-3) appropriate to gaseous nebulae. These diagrams should, in principle, allow the simultaneous determination of T_e and N_e from measurements of the [Ar IV] lines in a spectrum. Plasma parameters deduced for a sample of planetary nebulae from (R_1, R₃) and (R_1, R₄), using observational date obtained with the Hamilton echelle spectrograph on the 3 m Shane Telescope at the Lick Observatory, are found to show excellent internal consistency and to be in generally good agreement with the values of T_e and N_e estimated from other line ratios in the echelle spectra. These results provide observational support for the accuracy of the theoretical ratios and, hence, the atomic data adopted in their derivation. In addition, they imply that the 7171 Å line is not as seriously affected by telluric absorption as previously thought. However, the observed values of R₂ are mostly larger than the theoretical high-temperature and density limit, which is due to blending of the Ar IV 7237.54 Å line with the strong C II transition at 7236 Å. 

Fluorescence (FISH) and chromogenic (CISH) in situ hybridisation in prostate carcinoma cell lines: comparison and use of virtual microscopy

Chromogenic in situ hybridisation (CISH) has become an attractive alternative to fluorescence in situ hybridisation (FISH) due to its permanent stain which is more familiar to pathologists and because it can be viewed using light microscopy, The aim of the present study is to examine reproducibility in the assessment of abnormal chromosome number by CISH in comparison to FISH. Using three prostate cell lines - PNTIA (derived from normal epithelium), LNCAP and DU145 (derived from prostatic carcinoma), chromosomes 7 and 8 were counted in 40 nuclei in FISH preparations (x100 oil immersion) and 100 nuclei in CISH preparations (x40) by two independent observers. The CISH slides were examined using standard fight microscopy and virtual microscopy. Reproducibitity was examined using paired Student's t-test (P