We examined retrospectively whether the quantitative morphometric analysis of nuclear shapes in patients with advanced cancer of the larynx could be used as a prognostic factor. In all, specimens were taken from 90 patients treated by surgery in the Department of Otolaryngology, Jagiellonian University, Cracow, Poland, between 1987 and 1988. The follow-up period was no shorter than 5 years. In the group examined there were 59 patients with T3 tumors and 31 with T4 tumors. A neck dissection was performed on one or both sides in each case. Metastases in regional lymph nodes were found in 26 patients. Histologic grading was assessed in all cases. Fourteen parameters of nuclear shape were studied using a computer-assisted system of image analysis. Morphometric data were compared with patients' survival rates. The worse survival rates were found to be linked with a nuclear area (NA) > or = 64.82 micron 2 and its standard deviation (SDNA) > or = 20.10 micron 2, a nuclear perimeter (NP) > or = 32.45 microns and its variation (SDNP) > or = 4.77 microns, nuclear density (ND) > or = 22,215.63 and its variation (SDND) > or = 6930.85 and nuclear roundness (NR) > or = 0.76. By using multivariate Cox regression analysis the SDND, presence of metastases in lymph nodes and low tumor differentiation were found to be independent prognostic factors. No statistically significant correlation was found between the parameters examined, lymph node status and tumor differentiation.

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We report on HST observations of six candidate old globular clusters in the Large Magellanic Cloud: NGC 1754, NGC 1835, NGC 1898, NGC 1916, NGC 2005 and NGC 2019. Deep exposures with the F555W and F814W filters provide us with colourmagnitude diagrams that reach to an apparent magnitude in V of ∼25, well below the main sequence turnoff. These particular clusters are involved with significantly high LMC field star densities and care was taken to subtract the field stars from the cluster colour-magnitude diagrams accurately. In two cases there is significant variable reddening across at least part of the image, but only for NGC 1916 does the differential reddening preclude accurate measurements of the CMD characteristics. The morphologies of the colour-magnitude diagrams match well those of Galactic globular clusters of similar metallicity. All six have well-developed horizontal branches, while four clearly have stars on both sides of the RR Lyrae gap. The abundances obtained from measurements of the height of the red giant branch above the level of the horizontal branch are 0.3 dex higher, on average, than previously measured spectroscopic abundances. Detailed comparisons with Galactic globular cluster fiducials show that all six clusters are old objects, very similar in age to classical Galactic globulars such as M5, with little age spread among the clusters. This result is consistent with ages derived by measuring the magnitude difference between the horizontal branch and main sequence turnoff. We also find a similar chronology by comparing the horizontal branch morphologies and abundances with the horizontal branch evolutionary tracks of Lee, Demarque, & Zinn (1994). Our results imply that the LMC formed at the same time as the Milky Way Galaxy.

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