and we are back from lunch

J. Johnson (LANL) talking about supermassive stars as seeds for supermassive black holes – going to be getting more technical

supermassive star has a gas mass ~ 105 solar masses (as oppesed to few hundredish solar masses for standard Pop III stars that could provide low mass seeds)

form later than Pop III – maybe ~ 4-500 Myr after Big Bang

something like that may be needed for observed high luminosity quasars at redshift > 6.

radiative feedback, still not doing it right
but are we they doing it well enough…?

argues supermasive star formation common at z ~ 8-12
#JWST will tell, if true

Whalen, Heger et al finds disruptive (e+/e- pair) detonation for ~ 50,000 Msun stars (Z?) –

if true gives 1055 erg SNe – ~ 10,000 more luminous than nomral type II SNe.
those would be rather IR bright – (NB how fast, incl. 1+z dilation? – check)
also chemical signature
NB – other issue, explosion calculations start with static equilibrium model for zero age assembled star – in reality these cannot be in equilibrium, must be undergoing significant accretion – does that matter for detonation? how fragile are these?

talks about IR signature at Z ~ 20-30 – but, but
argued earlier they formed later than Pop III – so should only be seen at lower z – something wrong here

interesting, if true
Note-to-self – what is He yield in these conjectured events? Check.

Next John Wise (Georgia Tech): black hole seeds from first stars

beautiful graphics – check out the pdf of the slides when they are up on the KITP web

so after a decade of ever improving research we conclude we don’t actually know Pop III IMF at all… well, it is definitely tipped to massive-ish

and radiative feedback rears, again, its ugly head

cute plot – with no radiative feedback M_BH incresaes by factor of 100 with radiative feedback M_BH increases by factor of 1.001 or so

naked IMBH floating around halos of proto-galaxies, many such
– sounds familiar –

caution – the supermassive stars may not be following sims long enough to see fragmentation – possible post-collapse of core – get fragmentation in angular momentum supported outer parts of proto-supermassive star (Greif et al ’12? – check) – what do fragments go into? real interesting if clumps make many lower mass BH already bound to central SMBH – total wishful thinking for grav rad detection… timescales matter, hard problem

Elena Rossi (Leiden) – Connecting growth of galaxies to black hole seeds
Mass loss as critical ingredien to massive BH seed formation

switcheroo, not the talk we were expecting

ok, I didn’t catch that sorry
time for a break

PS: much later – my laptop was being used for couple of talks in last part of session, talk on IMBH/SMBH as analogous to jovian/stellar systems

I blathered on a bit about black holes in globulars and what possible relevance they might have

Melvyn gave a jolly nice talk on runaway collapse in nuclear star clusters and whether (v/c) is a critical parameter – per Davies & Miller etc.

Amy Reines presented latest results on sub million solar mass SMBH in dwarf galaxies in LMC-SMC mass range
there are some

now we rest