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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20090428T000000
DTEND;TZID=Atlantic/Canary:20090428T010000
UID:iactalks-4
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/4
CREATED:2009-04-28T00:00:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:The nature of growing bulges within z < 1.3 galaxy disks in the GOO
 DS-N Field
DESCRIPTION:The nature of growing bulges within z < 1.3 galaxy disks in the
  GOODS-N Field\nDr. Lilián de Fátima  Domínguez Palmero\n\nIn this work
  we have tried to verify what types of bulges are the descendants and the 
 precursors of the bulges with blue colors observed at intermediate z. Thes
 e may be the result of intense star formation in the central regions of th
 e disks, related to the phenomenon of pseudo-bulges in the local universe 
 or, alternatively, they may result from rejuvenation processes of old and 
 red classical bulges, formed at high z, perhaps through secular evolution 
 produced by internal or external agents. We can identify and distinguish b
 etween these processes analyzing the central surface brightness of the gal
 axies, &mu;0. For the general bulge population in the local universe, colo
 r is strongly correlated with surface density, in the sense that redder bu
 lges are denser. Classical bulges and pseudo-bulges occupy different regio
 ns in a color-&mu;0 diagram. We have studied the redshift evolution of the
  relation between the colors and the central surface brightness for sample
 s of spiral galaxy bulges selected from HST/ACS GOODS-N survey, and have a
 nalysed the ability of color-&mu;0 diagram to segregate different types of
  bulges at z ~ 1. The results show that, up to z ~ 0.8, galaxy nuclear and
  global colors are strongly correlated with the central surface brightness
  and, therefore, with the central surface density, in the sense that dense
 r bulges are redder. This suggests that these formed the bulk of their sta
 rs at earlier epochs than less dense bulges. For z &gt; 0.8, we find an im
 portant fraction of galaxies with high central surface brightness and nucl
 ear colors much bluer than the rest of the galaxy, which probably correspo
 nds to episodes of strong nuclear star formation that may result in the gr
 owth of the bulges inside the disks. From simple evolution models we can i
 nfer that these nuclei with star formation evolve towards the formation/gr
 owth of moderate central surface brightness, intermediate color z ~ 0 pseu
 dobulges rather than classical bulges. These models also argue against rej
 uvenation processes for z ~ 1 dense and old bulges.
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