The nature of the seeds of high-redshift supermassive black holes ( SMBHs ) is a key question in cosmology .
Direct collapse black holes ( DCBH ) that form in pristine , atomic-line cooling halos , illuminated by a Lyman-Werner ( LW ) UV flux exceeding a critical threshold J _ { crit } represent an attractive possibility .
We investigate when and where these conditions are met during cosmic evolution .
For the LW intensity , J _ { LW } , we account for departures from the background value in close proximity to star forming galaxies .
For the pristine halo fraction , we account for both ( i ) supernova driven outflows , and ( ii ) the inherent pollution from progenitor halos .
We estimate the abundance of DCBH formation sites , n _ { DCBH } ( z ) , and find that it increases with cosmic time from n _ { DCBH } ( z = 20 ) \sim 10 ^ { -12 } -10 ^ { -7 } cMpc ^ { -3 } to n _ { DCBH } ( z = 10 ) \sim 10 ^ { -10 } -10 ^ { -5 } cMpc ^ { -3 } .
Our analysis shows the possible importance of galactic winds , which can suppress the predicted n _ { DCBH } by several orders of magnitude , and cause DCBH formation to preferentially occur around the UV-brightest ( M _ { UV } \sim - 21 \pm 1 ) star forming galaxies .
Our analysis further highlights the dependence of these predictions on ( i ) the escape fraction of LW photons , ( ii ) J _ { crit } , and ( iii ) the galactic outflow prescription .