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SUMMARY:Models of Diffuse Ionised Gas in star-forming galaxies - Bert Vand
 enbroucke (University of St Andrews)
DTSTART:20190508T124500Z
DTEND:20190508T131500Z
UID:TALK122098@talks.cam.ac.uk
CONTACT:Catrina Diener
DESCRIPTION:Star-forming galactic discs contain an extended layer of diffu
 se gas\nthat is photoionised\, commonly referred to as the Warm Ionised Me
 dium\n(WIM) in our own Milky Way\, and as the Diffuse Ionised Gas in gener
 al.\nLarge Halpha surveys have extensively mapped the properties of the DI
 G\nand found typical scale heights of up to ~kpc above the plane of the\nd
 isc\, and high intensities for forbidden line emission from [NII] 6584\nan
 d [SII] 6725 that indicate an increase in temperature with height\nabove t
 he disc. To understand these properties and to pinpoint the\nsources respo
 nsible for ionising the DIG\, extensive 3D modelling is\nrequired. In this
  talk\, I will briefly review our knowledge of the DIG\nand show how 3D Mo
 nte Carlo radiation transfer and (more recently)\nradiation hydrodynamics 
 models can help us understand (a) the observed\nionisation state of the DI
 G\, and (b) the presence of a diffuse layer at\nthe observed heights above
  the galactic plane
LOCATION:Sackler Lecture Theatre\, IoA
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