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PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-6332
DTSTART:20210225T213000Z
DTEND:20210225T230000Z
DTSTAMP:20260415T023640Z
LAST-MODIFIED:20210216T180249Z
LOCATION:Zoom meeting(see Abstract ) Coffee and tea 3:30pm\, Talk 3:45
 pm
SUMMARY:PHANGS Results: Connecting the Small Scale ISM Physics to the 
 Galaxy Structures\, Astronomy Colloquium\, Dyas Otomo\, NRAO
DESCRIPTION:The physical and dynamical states of molecular gas are clo
 sely tied to the location and amount of star formation in galaxies. Th
 is interaction between molecular gas and star formation occurs in smal
 l scale (< 100pc)\, therefore\, high resolution observations are neede
 d. PHANGS-ALMA mapped CO line emission in 90 nearby galaxies at 1’â€
 ™ (~100 pc) resolution to quantify the physics of star formation and f
 eedback at the scale of individual giant molecular clouds (GMCs) and c
 onnecting these
\nmeasurements to the galaxy-scale properties. In this
  talk\, I will present recent results from the PHANGS collaboration. F
 irst\, I will show that the molecular gas in roughly in viral equilibr
 ium\, but their properties vary between regions inside galaxies. Secon
 d\, I will present recent measurement of the star formation efficiency
  per free fall time at the GMC scale. Third\, I will explain how we ca
 n estimate the stellar feedback and GMCs lifetime though statistical a
 nalysis. Finally\, I will conclude by showing that the star formation 
 process is self regulated.<br>
\n<br>
\nZoom Link:<br>
\n<br>
\nhttps:
 //uwmadison.zoom.us/j/88513896776?pwd=Y1JtRE1KZllxWkFTamJBSGtGdm9yQT09
 <br>
\n
URL:https://www.physics.wisc.edu/events/?id=6332
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