AstroFIt 2 – COFUND fellow since October 1, 2016.
Project ended on September 30, 2019.
INAF Research Centre: Osservatorio Astronomico di Trieste
Email: gabriele.cescutti at inaf.it
Curriculum vitae (Dec 2016)
List of publications (Dec 2016)
In the Media:
Espansione cosmica, il manganese sulla contesa (Media INAF, 16/03/2020)
- Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations (MNRAS, 25/5/2017)
- Phosphorus Abundances in FGK Stars (The Astrophysical Journal, 26/4/2017)
- The oldest stars of the bulge: new information on the ancient Galaxy (Proceedings of the IAU Symposium 334 “Rediscovering our Galaxy”, Potsdam, 10-14 July 2017)
- Abundance Uncertainties Obtained With the PizBuin Framework For Monte Carlo Reaction Rate Variations (Proceedings of OMEG 2017, Daejeon, Korea, June 27-30, 2017)
- The chemical signature of SNIax in the stars of Ursa minor? (Mem. S.A.It. Vol. 75, 282, 2/8/2017)
- The s-process nucleosynthesis: impact of the uncertainties in the nuclear physics determined by Monte Carlo variations (Mem. S.A.It. Vol. 75, 282, 2/8/2017)
- Manganese spread in Ursa Minor as a proof of sub-classes of type Ia supernovae (Astronomy & Astrophysics, 31/8/2017)
- Abundance Uncertainties Obtained With the PizBuin Framework For Monte Carlo Reaction Rate Variations (AIP Conf. Proc. 1947, 03/09/2017)
- Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations (MNRAS, 13/12/2017)
- Uncertainties in s-process nucleosynthesis in low-mass stars determined from Monte Carlo variations (MNRAS, 05/05/2018)
- Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient (MNRAS, 01/08/2018)
- 7Li evolution in the thin and thick discs of the Milky Way (MNRAS, 27/11/2018)
- A new delay time distribution for merging neutron stars tested against Galactic and cosmic data (MNRAS, 08/04/2019)
- 2D chemical evolution model: the impact of galactic disc asymmetries on azimuthal chemical abundance variations (Astronomy & Astrophysics, 25/6/2019)
- Uncertainties in νp-process nucleosynthesis from Monte Carlo variation of reaction rates (MNRAS, 02/08/2019)
- The contribution from rotating massive stars to the enrichment in Sr and Ba of the Milky Way (MNRAS, 05/09/2019)
- Neutron star binary orbits in their host potential: effect on early r-process enrichment (MNRAS, 13/09/2019)
- Phosphorus Abundances in the Hyades and Galactic Disk (The Astronomical Journal, 06/11/2019)
- Modelling the chemical evolution of Zr, La, Ce, and Eu in the Galactic discs and bulge (MNRAS, 09/01/2020)
Project title: RNFS – Revealing the Nature of the First Stars: the role of the chemical signatures in the primordial stars of our Galaxy
The First Stars shaped the evolution of the primordial Universe through their energy feedback and they enriched the pristine interstellar medium with elements heavier than lithium. Nowadays, these stars are long dead and only when the next generation facilities push the observational frontier to extremely high redshifts, will it be possible to detect the First Stars and it will be crucial to know what to search for. The scientific community therefore has an important task to fulfill in this period: constraining their nature. Without this input the possibility of finding these primordial stars will be seriously hampered. At the present, the only way to constrain our theoretical understanding of the formation of the first stars is to search for their imprints left in the oldest, still surviving, stars in our own backyard: the Milky Way and its satellites. The strategy taken so far by the Galactic Archaeology community has been to look for the most metal-poor stars, and directly compare their individual chemical abundances with the outputs of the different stellar models proposed for the first stars. The time is ripe to replace this approach with a more sophisticated one. I intend to investigate the large parameter space given by alternative nucleosynthesis scenarios with a stochastic chemical evolution model. The ultimate goal is to provide constraints on the nature of the First Stars (their mass spectrum, their chemical and energetic outputs) and to achieve that the theoretical predictions will be compared to the large amount of data now available thanks to ongoing observational campaigns.
These data cover not only the MW halo, but also other nearby regions hosting old stars with different star formation histories such as the bulge and the satellites of the MW. This is crucial because it improves the constraints on the nature of the First Stars. We are just entering an era where a robust and statistical comparison between models and abundance data is possible, hence making our project feasible.
Here I am: