Purpose: The survival rate of non–small cell lung cancer patients is very low, and knowledge of predictors of outcome is inadequate. To improve the curability of lung cancer, we need to identify new specific molecules involved in tumorigenesis and progression. The purpose of this study was to better define the role of osteopontin in non–small cell lung cancer biology by determining its prognostic significance. Experimental Design: Osteopontin expression was evaluated by immunohistochemistry, as percentage of neoplastic cells with cytoplasmic immunoreactivity, in a wide series of patients with stage I-IIIA non–small cell lung cancer (207 cases). The median value of this series (20% of positive cells) was used as the cutoff value to distinguish tumors with low (<20%) from tumors with high (≥20%) osteopontin expression. Results: Taking the series of patients as a whole (207 cases), osteopontin expression was associated with neither overall survival (P = 0.14) nor disease-free survival (P = 0.074). However, among patients with at least 6 years of follow-up (163 cases), 6-year overall survival and disease-free survival were significantly reduced if osteopontin expression was high (P = 0.0085 for overall survival, P = 0.0023 for disease-free survival). Moreover, a statistically significant correlation between high levels of osteopontin and shorter overall survival (P = 0.034) and disease-free survival (P = 0.011) in patients with stage I tumors (136 cases) was shown. Conclusions: Our results support the hypothesis of an association between high osteopontin expression and poor survival of patients with stage I non–small cell lung cancer, suggesting that osteopontin could be a candidate target for cancer therapy.

Context. The last decade showed an impressive observational effort from the photometric and spectroscopic point of view for ancient stellar clusters in our Galaxy and beyond, leading to important and sometimes surprising results. Aims. The theoretical interpretation of these new observational results requires updated evolutionary models and isochrones spanning a wide range of chemical composition so that the possibility of multipopulations inside a stellar cluster is also taken also into account. Methods. With this aim we built the new “Pisa Stellar Evolution Database” of stellar models and isochrones by adopting a well-tested evolutionary code (FRANEC) implemented with updated physical and chemical inputs. In particular, our code adopts realistic atmosphere models and an updated equation of state, nuclear reaction rates and opacities calculated with recent solar elements mixture. Results. A total of 32 646 models have been computed in the range of initial masses 0.30 ÷ 1.10 M ⊙ for a grid of 216 chemical compositions with the fractional metal abundance in mass, Z, ranging from 0.0001 to 0.01, and the original helium content, Y, from 0.25 to 0.42. Models were computed for both solar-scaled and α-enhanced abundances with different external convection efficiencies. Correspondingly, 9720 isochrones were computed in the age range 8 ÷ 15 Gyr, in time steps of 0.5 Gyr. The whole database is available to the scientific community on the web. Models and isochrones were compared with recent calculations available in the literature and with the color–magnitude diagram of selected Galactic globular clusters. The dependence of relevant evolutionary quantities, namely turn-off and horizontal branch luminosities, on the chemical composition and convection efficiency were analyzed in a quantitative statistical way and analytical formulations were made available for reader’s convenience. These relations can be useful in several fields of stellar evolution, e.g. evolutionary properties of binary systems, synthetic models for simple stellar populations and for star counts in galaxies, and chemical evolution models of galaxies.

A parasitologic study on 129 red foxes (Vulpes vulpes) from Tuscany (central Italy) was carried out in 2004-2006. Five intestinal species were found at necropsy: Dipylidium caninum (prevalence 57.3%), Mesocestoides lineatus (45.4%), Uncinaria stenocephala (39.1%), Toxocara canis (9.1%), and Toxascaris leonina (5.4%). Other parasites not associated with the intestine included Crenosoma vulpis (14.7%), Capillaria aerophila (7.0%), Angiostrongylus vasorum (7.0%), and filarial parasites (17.8%). Coprologic tests were less sensitive and less specific in identifying parasites than direct examinations at necropsy. Trichinella larvae were not found in muscles submitted to artificial digestion. By immunologic assay, antigens of Echinococcus spp. were detected in fecal samples of 20 foxes, but results could not be confirmed by fecal examination or molecular tests.

Osteopontin (OPN) is a multifunctional protein, which has recently been shown to be linked to tumorigenesis, progression and metastasis in different malignancies. Since non-small-cell lung cancer (NSCLC)'s prognosis remains bad, with few predictors of outcome, the purpose of this study was to evaluate if OPN might be involved in NSCLC's biology and therefore represent a prognostic marker and a target for new therapeutic trials. Immunohistochemistry was used to detect OPN expression, evaluated as percentage of neoplastic cells with cytoplasmic immunoreactivity, in a wide cohort of patients with stage I NSCLC (136 cases). The median value of this series (20% of positive cells) was used as the cutoff value to distinguish tumours with low (<20%) from tumours with high (20%) OPN expression. A statistically significant correlation between high levels of OPN and shorter overall (P=0.034) and disease-free (P=0.011) survival in our patients was shown. Our results support the hypothesis that high OPN expression is a significantly unfavourable prognostic factor for the survival of patients with stage I NSCLC. This conclusion has notable importance in terms of the biological characterization of early-stage tumours and therapeutic opportunities.

Context. The availability of high-quality astero-seismological data provided by satellite missions stimulated the development of several grid-based estimation techniques to determine the stellar masses and radii. Some aspects of the systematic and statistical errors affecting these techniques have still not been investigated well.Aims. We study the impact on mass and radius determination of the uncertainty in the input physics, in the mixing-length value, in the initial helium abundance, and in the microscopic diffusion efficiency adopted in stellar model computations.Methods. We consider stars with mass in the range [0.8−1.1] M ⊙ and evolutionary stages from the zero-age main sequence to the central hydrogen exhaustion. To recover the stellar parameters, a maximum-likelihood technique was employed by comparing the observations constraints to a precomputed grid of stellar models. Synthetic grids with perturbed input were adopted to estimate the systematic errors arising from the current uncertainty in model computations.Results. We found that the statistical error components, owing to the current typical uncertainty in the observations, are nearly constant in all cases at about 4.5% and 2.2% on mass and radius determination, respectively. The systematic bias on mass and radius determination due to a variation of ± 1 in ΔY/ΔZ is ±2.3% and ± 1.1%; the one due to a change of ± 0.24 in the value of the mixing-length α ml is ± 2.1% and ± 1.0%; the one due to a variation of ± 5% in the radiative opacity is ∓ 1.0% and ∓ 0.45%. An important bias source is to neglect microscopic diffusion, which accounts for errors of about 3.7% and 1.5% on mass and radius. The cumulative effects of the considered uncertainty sources can produce biased estimates of stellar characteristics. Comparison of the results of our technique with other grid techniques shows that the systematic biases induced by the differences in the estimation grids are generally greater than the statistical errors involved.