Stefano Gallozzi

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Aims. The goal of this work is to measure the evolution of the Galaxy Stellar Mass Function and of the resulting Stellar Mass Density up to redshift ≃ 4, in order to study the assembly of massive galaxies in the high redshift Universe. Methods. We have used the GOODS-MUSIC catalog, containing ∼3000 Ks-selected galaxies with multi-wavelength coverage(More)
We used a proper combination of multiband high-resolution and wide field multi-wavelength observations collected at three different telescopes (HST, LBT and CFHT) to probe Blue Straggler Star (BSS) populations in the globular cluster M53. Almost 200 BSS have been identified over the entire cluster extension. The radial distribution of these stars has been(More)
In the immediate future holographic technology will be available to store a very large amount of data in HVD (Holographic Versatile Disk) devices. This technology make extensive use of the WORM (Write-Once-Read-Many) paradigm: this means that such devices allow for a simultaneous and parallel reading of millions of volumetric pixels (i.e. voxels). This(More)
Aims. We have analysed the physical properties of z ∼ 4 Lyman Break Galaxies observed in the GOODS-S survey, in order to investigate the possible differences between galaxies where the Lyα is present in emission, and those where the line is absent or in absorption. Methods. The objects have been selected from their optical color and then spectroscopically(More)
Context. Deep multicolour surveys are the main tool to explore the formation and evolution of the very faint galaxies which are beyond the spectroscopic limit with the present technology. The photometric properties of these faint galaxies are usually compared with current renditions of semianalytical models to provide constraints on the detailed treatment(More)
Aims. We perform a deep search for galaxies in the redshift range 6.5 ≤ z ≤ 7.5, to measure the evolution of the number density of luminous galaxies in this redshift range and derive useful constraints on the evolution of their Luminosity Function. Methods. We present here the first results of an ESO Large Program, that exploits the unique combination of(More)
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