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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20210422T103000
DTEND;TZID=Atlantic/Canary:20210422T113000
UID:iactalks-1439
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1439
CREATED:2021-04-22T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:The evolutionary history of the Milky Way disk(s) and halo from Gai
 a colour-magnitude diagram fitting
DESCRIPTION:The evolutionary history of the Milky Way disk(s) and halo from
  Gaia colour-magnitude diagram fitting\nProf. Carme Gallart\n\nGaia has pr
 ovided distances and photometry, and thus colour-magnitude diagrams in the
  absolute plane, for stars over a large volume in the Milky Way, encompass
 ing significant fractions of the thin and thick disk, and halo. This has a
 llowed us, for the first time, to derive unprecedentedly detailed star for
 mation histories from direct modelling of these colour-magnitude diagrams,
  using the same techniques that have been proven successful for external g
 alaxies in the Local Group. Our first results for a volume of 2 Kpc radius
  from the Sun are extraordinarily promising. Applied to inner halo stars s
 elected kinematically using Gaia proper motions, this technique has allowe
 d us to date the merger of Gaia-Enceladus, to characterise the age profile
  of the accreted stars and of those present in the Milky Way at the time o
 f the merger, and to detect a conspicuous burst of star formation in the t
 hick disk occurred at the time of the merger (Gallart+2019). We have also 
 obtained a representative SFH for the Galactic disk, which clearly shows t
 he presence of up to four epochs of enhanced star formation well constrain
 ed in time, that can be associated with various pericentric passages of th
 e Sgr dwarf galaxy (Ruiz-Lara+2020). Additionally, we are obtaining result
 s of unprecedented clarity regarding the vertical distribution of ages and
  metallicities in the Milky Way disk. I will discuss these results as well
  as future prospects to reach a larger Milky Way volume, and to combine ch
 emodynamical information from spectroscopic surveys with this new approach
  to study the Milky Way evolutionary history. 
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