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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20090319T000000
DTEND;TZID=Atlantic/Canary:20090319T010000
UID:iactalks-52
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/52
CREATED:2009-03-19T00:00:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Young stars in Lupus: not as expected, not where expected
DESCRIPTION:Young stars in Lupus: not as expected, not where expected\nDr. 
 Fernando ComerĂłn\n\nMost studies of the stellar and substellar population
 s of star forming regions rely on the identification of the signatures of 
 accretion, outflows, circumstellar dust, or activity characteristic of the
  early stages of stellar evolution. However, the decay of these observatio
 nal signatures with time limits our ability to understand the complete sta
 r forming history of young aggregates, and to obtain unbiased samples of y
 oung stellar objects at different stages of disk evolution.\n\nI will pres
 ent the results of a wide-area study of the stellar population of selected
  clouds in the nearby Lupus star forming region, initially defined to comp
 lement the data obtained by the Spitzer Space Observatory Legacy Program â
 €śFrom molecular cores to planet-forming disks”. When combined with 2MAS
 S photometry, our data allow us to fit the spectral energy distributions o
 f well over 150,000 sources seen in that direction, and to identify possib
 le new members based on their photospheric fluxes alone, with independence
  of the display of signposts of youth. In this way we identify a very clea
 r signature of the existence of a surprisingly numerous and thus far unrec
 ognized population of cool members of Lupus 1 and 3, which is absent from 
 Lupus 4.\n\n\nThe approximately 130 new members that we identify show that
  Lupus 1 and 3 have been forming low mass stars in numbers comparable to, 
 or even exceeding in Lupus 1, those revealed by recent sensitive surveys b
 ased on the signposts of youth. We hypothesize on several possibilities fo
 r the origin of this population that may account for its puzzling properti
 es of general lack of disks, coevality with the disk-bearing population, a
 nd preferential off-cloud location, which hint at a picture more complex a
 nd interesting than the quiescent formation inside dense molecular clouds.
 \n\n
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