Cool stars are fossils from the history of the universe and their properties can provide unique insights on the formation and evolution of the Milky Way. We are now systematically studying stellar populations in the broader Galactic contex t, and thanks to transformational facilities we will soon be able to bridge between the Milky Way and other galaxies. Measuring the chemistry of resol ved stellar populations up to a few million of parsecs will open up science cases that so far could only be addressed with nearby stars, and transform our ability to test and to use the Milky Way as a template to study other galaxies. I review some of the main results obtained in this quest, present ongoing efforts and highlight future directions with upcoming observationa l facilities.
I obtained a Master's degree in physics at the University of Torino (Italy) and PhD i n astronomy at the University of Turku (Finland). In 2008 I was awarded a f ellowship from the Max Planck Institute for Astrophysics (Munich, Germany). I stayed there for three years, before taking up a Stromlo Fellowship at t he ANU Research School of Astronomy & Astrophysics (RSAA). I was awarde d an ARC Future Fellowship in 2016 and I am now a member of the Faculty at RSAA.
His field of research are stellar and Galactic astronomy, working on the determination of stellar parameters and the use of stellar populations to understand the formation and evolution of the Milky Way. Among his resu lts, he has solved a decade long problem by firmly set the zero-point of th e stellar effective temperature scale, and he has provided the first observ ational evidence that stellar radial migration is responsible for broadenin g the metallicity distribution of stars as function of age. He is actively involved to improve inclusion, diversity and equity in astronomy, he is a m ember of the European Astronomical Society, the Astronomical Society of Aus tralia and an elected member of the Commission on photometry and polarimetr y of the International Astronomical Union.
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Cool stars are fossils from the history of the universe and their properties can provide unique insights on the formation and evolution of the Milky Way. We are now systematically studying stellar populations in the broader Galactic contex t, and thanks to transformational facilities we will soon be able to bridge between the Milky Way and other galaxies. Measuring the chemistry of resol ved stellar populations up to a few million of parsecs will open up science cases that so far could only be addressed with nearby stars, and transform our ability to test and to use the Milky Way as a template to study other galaxies. I review some of the main results obtained in this quest, present ongoing efforts and highlight future directions with upcoming observationa l facilities.
I obtained a Master's degree in physics at the University of Torino (Italy) and PhD in astronomy at the University of Turku (Finland). I n 2008 I was awarded a fellowship from the Max Planck Institute for Astroph ysics (Munich, Germany). I stayed there for three years, before taking up a Stromlo Fellowship at the ANU Research School of Astronomy & Astrophys ics (RSAA). I was awarded an ARC Future Fellowship in 2016 and I am now a m ember of the Faculty at RSAA.
His field of research are stellar and Galact ic astronomy, working on the determination of stellar parameters and the us e of stellar populations to understand the formation and evolution of the M ilky Way. Among his results, he has solved a decade long problem by firmly set the zero-point of the stellar effective temperature scale, and he has p rovided the first observational evidence that stellar radial migration is r esponsible for broadening the metallicity distribution of stars as function of age. He is actively involved to improve inclusion, diversity and equity in astronomy, he is a member of the European Astronomical Society, the Ast ronomical Society of Australia and an elected member of the Commission on p hotometry and polarimetry of the International Astronomical Union.
DTSTAMP:20260619T223148 DTSTART;TZID=Australia/Sydney:20221201T193000 DTEND;TZID=Australia/Sydney:20221201T213000 SEQUENCE:0 TRANSP:OPAQUE END:VEVENT END:VCALENDAR