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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20200625T103000
DTEND;TZID=Atlantic/Canary:20200625T113000
UID:iactalks-1408
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1408
CREATED:2020-06-25T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Probing black hole-galaxy co-evolution from de-biased scaling relat
 ions
DESCRIPTION:Probing black hole-galaxy co-evolution from de-biased scaling r
 elations\nProf. Francesco Shankar\n\nIt has been claimed for decades that 
 almost all galaxies in the local Universe host at their centre a supermass
 ive black hole (SMBH) the mass of which appears to be tightly correlated w
 ith the stellar mass and the random motion ("velocity dispersion", sigma) 
 of the stars in the host galaxy. In this talk I will first review the stat
 e of the art in this field. I will then highlight that significant biases 
 affect local black hole-galaxy correlations.  I will specifically sho
 w that the majority of quiescent early-type galaxies with central black ho
 le dynamical mass estimates have significantly higher velocity dispersions
  than local typical galaxies of similar stellar mass. Through aimed Monte 
 Carlo simulations, residual analysis, and the comparison with latest AGN c
 lustering measurements, I will then illustrate that present data sets of a
 ctive and quiescent galaxies strongly favour on average lower SMBH masses 
 than previously thought, and point to velocity dispersion as more ``fundam
 ental'' than galaxy stellar mass, galaxy size or Sérsic index. I wi
 ll then move on discussing the main implications of these findings, in par
 ticular: 1) The implied black hole radiative efficiencies and obscured fra
 ctions; 2) the consequences on feedback from active black holes and SMBH b
 inary gravitational waves; 3) the connection to cosmological models that r
 ely on velocity dispersion, rather than stellar mass, as main driver of bl
 ack hole growth.\nZoom link:  https://rediris.zoom.us/j/97154760
 685
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