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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20140515T103000
DTEND;TZID=Atlantic/Canary:20140515T113000
UID:iactalks-639
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/639
CREATED:2014-05-15T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Reconstructing the formation 
DESCRIPTION:Reconstructing the formation \nDr. Pablo G. Pérez González\n\
 nOne of the most widely researched topics in Extragalactic Astrophysics in
  the last decades is how early-type galaxies have formed their stars and a
 ssembled. In this context, we now have unequivocal observational evidences
  about the existence of a numerous population of massive galaxies which no
 t only had assembled a considerable amount of stars (~10^11 M_sun) by z~2,
  but were already evolving passively by that time. These galaxies, the lik
 ely progenitors of nearby ellipticals, are also quite compact in compariso
 n with local galaxies of the same mass. These result are mainly based on m
 easurements designed to obtain stellar masses and sizes, and our estimatio
 ns of these parameters are now quite robust. Now we need a more secure det
 ermination of how exactly they formed and assembled their stellar mass in 
 just 2-3 Gyr (z>2). In other words, how was their Star Formation Histor
 y and which are the properties (age, metallicity, dust content) of their s
 tellar populations? And how could they end up with such high masses and sm
 all sizes? In this talk, we will present our results about the SFH (mainly
  ages and duty cycles) of massive galaxies at z=1-3 based on the deepest s
 pectro-photometric data ever taken. These data were gathered by the Survey
  for High-z Absorption Red and Dead Sources (SHARDS), a ESO/GTC Large Prog
 ram aimed at obtaining R~50 optical spectra of distant galaxies. This reso
 lution is especially suited to measure absorption indices such as D(4000),
  Mg_UV, the Balmer break,etc.. for galaxies up to z~3 (merging our SHARDS 
 data with HST/WFC3 grism observations) or emission-line fluxes for faint t
 argets up to z~6. These measurements represent a big step forward for the 
 robust determination of the stellar population properties, providing a muc
 h more certain characterization of the stellar content of distant galaxies
  than the typical broad-band studies. Our results uniquely allow to study 
 the stellar content of red and dead galaxies at z~2 and identify progenito
 rs at higher redshifts, as well as helping to constrain the models of gala
 xy formation.
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