Manganese evolution in Omega Centauri: a clue to the cluster formation mechanisms?

We model the evolution of manganese relative to iron in the progenitor system of the globular cluster Omega Centauri by means of a self-consistent chemical evolution model. We use stellar yields that already reproduce the measurements of [Mn/Fe] versus [Fe/H] in Galactic field disc and halo stars, in Galactic bulge stars and in the Sagittarius dwarf spheroidal galaxy. We compare our model predictions to the Mn abundances measured in a sample of 10 red giant members and six subgiant members of ω Cen. The low values of [Mn/Fe] observed in a few, metal-rich stars of the sample cannot be explained in the framework of our standard, homogeneous chemical evolution model. Introducing cooling flows that selectively bring to the cluster core only the ejecta from specific categories of stars does not help to heal the disagreement with the observations. The capture of field stars does not offer a viable explanation either. The observed spread in the data and the lowest [Mn/Fe] values could, in principle, be understood if the system experienced inhomogeneous chemical evolution. Such an eventuality is qualitatively discussed in this paper. However, more measurements of Mn in ω Cen stars are needed to settle the issue of Mn evolution in this cluste

SOLUZIONI TECNOLOGICHE INNOVATIVE PER LA PROSPEZIONE GEOFISICA IN AMBIENTE LAGUNARE

Innovative solutions for carry out geophysical surveys of coastal lagoons are presented

The Chemical Evolution of Phosphorus

Phosphorus is one of the few remaining light elements for which little is known about its nucleosynthetic origin and chemical evolution, given the lack of optical absorption lines in the spectra of long-lived FGK-type stars. We have identified a P I doublet in the near-ultraviolet (2135/2136 A) that is measurable in stars of low metallicity. Using archival Hubble Space Telescope-STIS spectra, we have measured P abundances in 13 stars spanning -3.3 <= [Fe/H] <= -0.2, and obtained an upper limit for a star with [Fe/H] ~ -3.8. Combined with the only other sample of P abundances in solar-type stars in the literature, which spans a range of -1 <= [Fe/H] <= +0.2, we compare the stellar data to chemical evolution models. Our results support previous indications that massive-star P yields may need to be increased by a factor of a few to match stellar data at all metallicities. Our results also show that hypernovae were important contributors to the P production in the early universe. As P is one of the key building blocks of life, we also discuss the chemical evolution of the important elements to life, C-N-O-P-S, together.Comment: Accepted for publication in Astrophysical Journal Letters. 6 pages, 4 figures; reference added to earlier versio

The Evolution of Barium and Europium in Local Dwarf Spheroidal Galaxies

By means of a detailed chemical evolution model, we follow the evolution of barium and europium in four Local Group Dwarf Spheroidal Galaxies, in order to set constraints on the nucleosynthesis of these elements and on the evolution of this type of galaxies compared with the Milky Way. The model, which is able to reproduce several observed abundance ratios and the present day total mass and gas mass content of these galaxies, adopts up to date nucleosynthesis and takes into account the role played by supernovae of different types (II, Ia) allowing us to follow in detail the evolution of several chemical elements (H, D, He, C, N, O, Mg, Si, S, Ca, Fe, Ba and Eu). By assuming that barium is a neutron capture element produced in low mass AGB stars by s-process but also in massive stars (in the mass range 10 - 30 $M_{\odot}$) by r-process, during the explosive event of supernovae of type II, and that europium is a pure r-process element synthesized in massive stars also in the range of masses 10 - 30 $M_{\odot}$, we are able to reproduce the observed [Ba/Fe] and [Eu/Fe] as functions of [Fe/H] in all four galaxies studied. We confirm also the important role played by the very low star formation efficiencies ($\nu$ = 0.005 - 0.5 Gyr$^{-1}$) and by the intense galactic winds (6-13 times the star formation rate) in the evolution of these galaxies. These low star formation efficiencies (compared to the one for the Milky Way disc) adopted for the Dwarf Spheroidal Galaxies are the main reason for the differences between the trends of [Ba/Fe] and [Eu/Fe] predicted and observed in these galaxies and in the metal-poor stars of our Galaxy. Finally, we provide predictions for Sagittarius galaxy for which data of only two stars are available.Comment: 13 pages, 13 figures, accepted for publication in MNRA

Atmospheric fall-out of metals around the Murano glass-making district (Venice, Italy)

Murano\u27s glass-makers have held a monopoly on quality glass-making for centuries known all over the world. Artistic glass manufacture entails exposure to complex mixtures of pollutants, including metals. A few studies have reported high levels of trace elements in marine waters, sediments and mussels around Murano and shown that emissions from Murano glass-making workshops significantly influence air quality in the Venice area. Nevertheless, to date, there is very little information on atmospheric concentrations and virtually none on atmospheric deposition fluxes of trace elements around the island. This study presents data on the distribution of trace elements in the air and atmospheric depositions around Murano, based on a 2-year sampling period. Atmospheric concentrations of As, Cd, Cr, Ni, Pb, Se and Zn were 1-2 orders of magnitude greater on the island of Murano than in the nearest urban areas (Venice and Mestre), with values higher than those reported for European industrial sites. The atmospheric deposition fluxes of all elements were also higher in Murano than those detected by other studies in Venice and Mestre and in the Porto Marghera industrial zone, with As, Cd, Sb and Se 1-2 orders of magnitude higher. As shown by our study, atmospheric loadings of metals around Murano are significant. These observations confirm that emissions from Murano also significantly influence atmospheric deposition in the Venice area. Specifically, the mean daily Cd flux in the most affected area, which includes the whole of the historic city centre of Venice, is ~18 ?g m-2 day-1, i.e. more than 65 times higher than the Dutch limit and more than three times higher than that of Germany

The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

We present the first chemical evolution model for Enceladus, alias the Gaia Sausage, to investigate the star formation history of one of the most massive satellites accreted by the Milky Way during a major merger event. Our best chemical evolution model for Enceladus nicely fits the observed stellar [$\alpha$/Fe]-[Fe/H] chemical abundance trends, and reproduces the observed stellar metallicity distribution function, by assuming low star formation efficiency, fast infall time scale, and mild outflow intensity. We predict a median age for Enceladus stars $12.33^{+0.92}_{-1.36}$ Gyr, and - at the time of the merger with our Galaxy ($\approx10$ Gyr ago from Helmi et al.) - we predict for Enceladus a total stellar mass $M_{\star} \approx 5 \times 10^{9}\,\text{M}_{\odot}$. By looking at the predictions of our best model, we discuss that merger events between the Galaxy and systems like Enceladus may have inhibited the gas accretion onto the Galaxy disc at high redshifts, heating up the gas in the halo. This scenario could explain the extended period of quenching in the star formation activity of our Galaxy about 10 Gyr ago, which is predicted by Milky Way chemical evolution models, in order to reproduce the observed bimodality in [$\alpha$/Fe]-[Fe/H] between thick- and thin-disc stars.Comment: Accepted for publication in MNRAS Letter

Sedimentation and time-of-transition techniques for measuring grain-size distributions in lagoonal flats: comparability of results

A comparative study was performed of three instruments used to measure the grain-size distribution of thirty sediment samples from shallow lagoonal flats: the hydrometer, the Sedigraph 5100 and the CIS-1. The hydrometer and Sedigraph are based on sedimentation whereas the CIS-1 uses the time of transition. The percentage of the samples accounted for by the <8 lm fraction was not affected by the technique used, but this was not the case with the clay fraction (<2 lm). Due to its relative independence from the analytical method applied, the <8 lm fraction can be used in ternary diagram classifications. This fraction also has an environmental significance in coastal lagoons in terms of hydrodynamics, organic enrichment and macrozoobenthos assemblages. The linear relationships obtained in this study may provide useful operational indications for similar studies

A decision-support system in ICZM for protecting the ecosystems: integration with the habitat directive

This paper describes a decision-support system based on landscape ecology and focused on the study of ecosystems\u27 health. System capabilities are illustrated with three cases of integrated coastal zone management(ICZM), in the Adriatic Sea (Italy): the lagoon of and the Rimini and Ancona coastal areas. Indicators and indices are developed with a focus on sub-regional and local problems in coastal management, with a multi- approach based on landscape and seascape ecology. Land-use changes of the coastal areas were detected by analyzing two sets of satellite images. Indices combining satellite imagery, socio-economic and environmental indicators, and landscape and seascape maps created, showing ecological changes, habitat loss and gaps in conservation policy. The approach used provides means for the identification of conflicts and for the assessment of sustainability. Results show that the lagoon of Venice plays an important role in mitigating and compensating the impacts of human activities, and needs to be protected and restored. The Rimini area shows high ecological footprint and development-intensity and low biocapacity. The Ancona area needs the protection of its natural coastal space from potential sources of anthropo-genic impacts to maintain its sustainability. A model of environment changes is critical for formulating effective environmental policies and management strategies. The developed decision-support system provides a suitability map per each area analyzed, which can be used in order to maximize different policy objectives and reduce coastal conflicts

Polycyclic aromatic hydrocarbons in atmospheric depositions around the Venice Lagoon

Studies have revealed the potential risks to which human health and ecosystems are exposed in the Venice Lagoon, due to the atmospheric deposition of persistent pollutants such as trace metals and organic compounds. A total of 77 atmospheric bulk deposition samples were collected monthly from April 2002 to December 2004, from three sites located in the cities of Mestre and Venice, and inside the industrial area of Porto Marghera. Samples were analyzed by HRGC/HRMS for polycyclic aromatic hydrocarbon (PAH) content. Spatial variations of atmospheric fallout were investigated, and source identification was attempted using diagnostic ratios and multivariate statistical analysis. Different conditions were recorded, with three anthropic signatures: i) industrial, mainly affected by local industrial sources and diesel engine emissions, ii) urban, mostly influenced by high traffic density, especially petrol car emissions and iii) lagoonal, characterized by dieselemissions from boat engines and oil burning, with random transport of industrial emissions

Manganese evolution in Omega Centauri: a clue to the cluster formation mechanisms?

We model the evolution of manganese relative to iron in the progenitor system of the globular cluster Omega Centauri by means of a self-consistent chemical evolution model. We use stellar yields that already reproduce the measurements of [Mn/Fe] versus [Fe/H] in Galactic field disc and halo stars, in Galactic bulge stars and in the Sagittarius dwarf spheroidal galaxy. We compare our model predictions to the Mn abundances measured in a sample of 10 red giant members and six subgiant members of ? Cen. The low values of [Mn/Fe] observed in a few, metal-rich stars of the sample cannot be explained in the framework of our standard, homogeneous chemical evolution model. Introducing cooling flows that selectively bring to the cluster core only the ejecta from specific categories of stars does not help to heal the disagreement with the observations. The capture of field stars does not offer a viable explanation either. The observed spread in the data and the lowest [Mn/Fe] values could, in principle, be understood if the system experienced inhomogeneous chemical evolution. Such an eventuality is qualitatively discussed in this paper. However, more measurements of Mn in ? Cen stars are needed to settle the issue of Mn evolution in this cluster