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SUMMARY:How is  star formation in galaxies quenched? - Asa Bluck (Cavendis
 h)
DTSTART:20191129T113000Z
DTEND:20191129T123000Z
UID:TALK132130@talks.cam.ac.uk
CONTACT:Martin Haehnelt
DESCRIPTION:I will present an overview of my ongoing research into galacti
 c star\nformation and its cessation in the ‘quenching’ process. 
 From an\nanalysis of the SDSS\, we discover that the fraction of quenched\
 ncentral galaxies scales most tightly with estimates of supermassive\nblac
 k hole mass (derived via scaling relations with central\nkinematics). I wi
 ll show that this result is highly consistent with\nmodels which quench ce
 ntrals through AGN-feedback\, particularly in the\n‘radio-mode’.
  However\, satellite galaxies require additional quenching\nmechanisms\, s
 trongly correlated with environment (including local\ndensity and location
  within the group or cluster).\n\nI will also present new work examining r
 esolved star formation and\nquenching in galaxies using the MaNGA IFU surv
 ey. We perform a\ndetailed machine learning analysis of physical propertie
 s derived from\nover 5 million optical spectra\, utilising artificial neur
 al networks\n(ANN). We find that global properties (particularly those mos
 t\nconnected with the central regions in galaxies) are the most\npredictiv
 e of quenching in centrals. Perhaps surprisingly\, the\nconditions at the 
 spaxel location are largely uncorrelated with\nquenching. Conversely\, we 
 find that local/ spatially resolved\nparameters are most effective at pred
 icting the rate of star formation\nin star forming regions. From these res
 ults\, we conclude that: 1)\nquenching is a global process\, impacting ent
 ire galaxies as a whole\;\nyet 2) star formation is a locally governed pro
 cess\, varying\nsignificantly throughout galaxies and depending primarily 
 on local\nconditions. I will conclude by ruling out several quenching mode
 ls on\nthe basis of these results.\n
LOCATION:Kavli Large Meeting Room\, Kavli Building
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