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SUMMARY:Finding the water trail of the star and planet formation - Daniel 
 Harsono (Leiden)
DTSTART:20180829T121500Z
DTEND:20180829T124500Z
UID:TALK108802@talks.cam.ac.uk
CONTACT:Dr Giovanni Rosotti
DESCRIPTION:Water is abundant in the solid phase prior to star formation a
 s revealed \nby ice absorption studies of embedded protostars. In contrast
 \, water \ntoward Class II disks is significantly depleted.  Since planets
  are \nformed in those disks\, it is crucial to understand how it is being
  \ntransported there from the large-scale envelope around protostars. Clas
 s \nI protostellar systems have been shown to host well-defined Keplerian 
 \ndisks on similar scales to that of Class II systems. Disks around Class 
 \nI sources thereby provide an interesting link to trace the water \nevolu
 tion. We here present non-detections of spatially resolved warm \nwater li
 nes toward four Class I protostars from the IRAM NOEMA and ALMA. \n  The s
 tringent upper limits suggest that the chemical processing of \nwater due 
 to grain growth and photodissociation are known to take place \nin Class I
 I disks\, already start during the earlier embedded phases. \nDeeper water
  line observations are required to further constrain the \ndependence of t
 he water vapor abundance on the physical structure of the \nClass I disks.
LOCATION:Sackler Lecture Theatre\, IoA
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