BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//talks.cam.ac.uk//v3//EN
BEGIN:VTIMEZONE
TZID:Europe/London
BEGIN:DAYLIGHT
TZOFFSETFROM:+0000
TZOFFSETTO:+0100
TZNAME:BST
DTSTART:19700329T010000
RRULE:FREQ=YEARLY;BYMONTH=3;BYDAY=-1SU
END:DAYLIGHT
BEGIN:STANDARD
TZOFFSETFROM:+0100
TZOFFSETTO:+0000
TZNAME:GMT
DTSTART:19701025T020000
RRULE:FREQ=YEARLY;BYMONTH=10;BYDAY=-1SU
END:STANDARD
END:VTIMEZONE
BEGIN:VEVENT
CATEGORIES:Galaxies Discussion Group
SUMMARY:How is  star formation in galaxies quenched? - Asa
  Bluck (Cavendish)
DTSTART;TZID=Europe/London:20191129T113000
DTEND;TZID=Europe/London:20191129T123000
UID:TALK132130AThttp://talks.cam.ac.uk
URL:http://talks.cam.ac.uk/talk/index/132130
DESCRIPTION:I will present an overview of my ongoing research 
 into galactic star\nformation and its cessation in
  the ‘quenching’ process. From an\nanalysis of
  the SDSS\, we discover that the fraction of quenc
 hed\ncentral galaxies scales most tightly with est
 imates of supermassive\nblack hole mass (derived v
 ia scaling relations with central\nkinematics). I 
 will show that this result is highly consistent wi
 th\nmodels which quench centrals through AGN-feedb
 ack\, particularly in the\n‘radio-mode’. Howev
 er\, satellite galaxies require additional quenchi
 ng\nmechanisms\, strongly correlated with environm
 ent (including local\ndensity and location within 
 the group or cluster).\n\nI will also present new 
 work examining resolved star formation and\nquench
 ing in galaxies using the MaNGA IFU survey. We per
 form a\ndetailed machine learning analysis of phys
 ical properties derived from\nover 5 million optic
 al spectra\, utilising artificial neural networks\
 n(ANN). We find that global properties (particular
 ly those most\nconnected with the central regions 
 in galaxies) are the most\npredictive of quenching
  in centrals. Perhaps surprisingly\, the\nconditio
 ns at the spaxel location are largely uncorrelated
  with\nquenching. Conversely\, we find that local/
  spatially resolved\nparameters are most effective
  at predicting the rate of star formation\nin star
  forming regions. From these results\, we conclude
  that: 1)\nquenching is a global process\, impacti
 ng entire galaxies as a whole\;\nyet 2) star forma
 tion is a locally governed process\, varying\nsign
 ificantly throughout galaxies and depending primar
 ily on local\nconditions. I will conclude by rulin
 g out several quenching models on\nthe basis of th
 ese results.\n
LOCATION:Kavli Large Meeting Room\, Kavli Building
CONTACT:Martin Haehnelt
END:VEVENT
END:VCALENDAR