Maurizio Salaris

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We present a large and updated stellar evolution database for low-, intermediate-and high-mass stars in a wide metallicity range, suitable for studying Galactic and extragalactic simple and composite stellar populations using population synthesis techniques. The stellar mass range is between ∼ 0.5M ⊙ and 10M ⊙ with a fine mass spacing. The metallicity(More)
This paper is the 4th in a series describing the latest additions to the BaSTI stellar evolution database, which consists of a large set of homogeneous models and tools for population synthesis studies, covering ages between 30 Myr and ∼20 Gyr and 11 values of Z (total metallicity). Here we present a new set of low and high resolution synthetic spectra(More)
Hipparcos parallax measurements of stars in the Pleiades notoriously result in a cluster distance of 118 pc, which is approximately 10% shorter than the 'classical' result obtained from earlier main sequence (MS) fitting studies. In an earlier paper we developed a purely empirical MS-fitting method in an attempt to address this problem. This work produced(More)
We present accurate relative ages for a sample of 55 Galactic globular clusters. The ages have been obtained by measuring the difference between the horizontal branch and the turnoff in two, internally photometrically homogeneous databases. The mutual consistency of the two data sets has been assessed by comparing the ages of 16 globular clusters in common(More)
We present homogeneous age determinations for a large sample of 55 Galactic globular clusters, which constitute about 30% of the total Galactic population. A study of their age distribution reveals that all clusters from the most metal poor ones up to intermediate metallicities are coeval, whereas at higher [Fe/H] an age spread exists, together with an(More)
NGC 6791 is a well studied open cluster that it is so close to us that can be imaged down to very faint luminosities. The main-sequence turn-off age ( approximately 8 Gyr) and the age derived from the termination of the white dwarf cooling sequence ( approximately 6 Gyr) are very different. One possible explanation is that as white dwarfs cool, one of the(More)
In the old, populous, and metal-rich open cluster NGC 6791 we have used deep HST/ACS images to track the white dwarf cooling sequence down to m F606W ≃ 28.5. The white dwarf luminosity function shows a well defined peak at m F606W ≃ 27.4, and a bending to the blue in the color–magnitude diagram. If this peak corresponds to the end of the white dwarf cooling(More)
White dwarfs are the remnants of stars of low and intermediate masses on the main sequence. Since they have exhausted all their nuclear fuel, their evolution is just a gravothermal process. The release of energy only depends on the detailed internal structure and chemical composition and on the properties of the envelope equation of state and opacity; its(More)
We introduce and discuss the properties of a theoretical (B−K)-(J −K) integrated colour diagram for single-age, single-metallicity stellar populations. We show how this combination of integrated colours is able to largely disentangle the well known age-metallicity degeneracy when the age of the population is greater than ∼ 300 Myr, and thus provides(More)