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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20190725T103000
DTEND;TZID=Atlantic/Canary:20190725T113000
UID:iactalks-1279
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1279
CREATED:2019-07-25T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Supernova Dust
DESCRIPTION:Supernova Dust\nProf. Mike Barlow\n\nUntil the advent in the la
 te 1990’s of sensitive submillimetre arrays such as SCUBA, it was ge
 nerally thought that the main sources for the interstellar dust found in g
 alaxies were the dusty outflows from evolved AGB stars and M supergiants, 
 although a dust contribution from supernovae had long been predicted on th
 eoretical grounds. The detection at submillimetre wavelengths of very larg
 e dust masses in some high redshift galaxies emitting less than a billion 
 years after the Big Bang led to a more serious consideration of core-colla
 pse supernovae (CCSNe) from massive stars as major dust contributors. KAO 
 and Spitzer mid-infrared observations confirmed that CCSN ejecta could for
 m dust but it was not until the Herschel mission and subsequent ALMA obser
 vations that direct evidence has been obtained for the presence of signifi
 cantly large masses of cold dust in young CCSN remnants. As well as using 
 infrared spectral energy distributions to measure the amounts of dust form
 ing in CCSN ejecta, dust masses can also be quantified from the analysis o
 f red-blue asymmetries in their late-time optical emission line profiles. 
 I will describe current results from these methods for estimating ejecta d
 ust masses, and their implications.
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