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SUMMARY:Understanding How Star Formation Proceeds in the Perseus and Ophiu
 chus Molecular Clouds - Doug Johnstone (Herzberg Institute of Astrophysics
 \, Canada)
DTSTART:20070424T153000Z
DTEND:20070424T163000Z
UID:TALK7001@talks.cam.ac.uk
CONTACT:Jane Buckle
DESCRIPTION:The nearby Perseus and Ophiuchus molecular clouds are exceptio
 nal laboratories for testing the earliest phases of star formation. Carefu
 l consideration of the multi-wavelength surveys of these clouds (in partic
 ular 2Mass\, Spitzer c2d\, and COMPLETE) allows us to measure the column d
 ensity distributions of the bulk cloud\, the location and kinematics of th
 e dense stellar-massed cores\, and the distribution of the protostars. As 
 such we can now provide strong constraints for theoretical models or simul
 ations wishing to explain the manner in which stars form within a cloud. H
 ighlights of our results are (1) most of the mass of the cloud is at low c
 olumn density\, (2) dense cores form only in high column density regions\,
  (3) the mass distribution of the dense cores is similar to the IMF\, (4) 
 dense cores are mostly thermally supported\, (5) dense cores contain only 
 a few percent of the cloud mass\, (6) the more concentrated cores are most
  likely to contain embedded protostars\, and (7) the dense cores are not r
 andomly located within the the molecular cloud\, suggesting possible trigg
 ering mechanisms for their creation. In this talk\, I will discuss each of
  these important results and place them in context with theoretical models
  and simulations of star formation.
LOCATION:Ryle Seminar Room\, Cavendish Laboratory
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