The role of gas fragmentation during the formation of supermassive black
  holes
  We have performed cosmological hydrodynamic simulations to study the effect
of fragmentation on the SMBH seed mass in the direct collapse formation
scenario. We considered different background UV intensities, host halo spin,
and halo merger histories. Our simulations in low-spin halos, in the presence
of a strong UV background are consistent with the Direct Collapse Black Hole
model, in which a single massive object $\sim10^5$ M$_{\odot}$ is formed in the
center of a proto-galaxy. While in our simulations under the presence of a low
UV background, we find fragmentation and the formation of various minor seeds.
These fragments have masses of 10$^3$ - 10$^4$ M$_{\odot}$. These values are
significant if we consider the potential mergers between them, and the fact
that these minor objects are formed earlier in cosmic time compared to the
massive single seeds. In one of our simulations, we observed gas fragmentation
even in the presence of a strong UV intensity. Said structure arose in a dark
matter halo that formed after various merger episodes, and the one with the
highest spin value. The final mass obtained was $\sim 10^5$ M$_{\odot}$ in this
run. From these results, we conclude that fragmentation in fact produces less
massive objects, however, they are still prone to merge. In simulations that
formed many fragments, they all approach the most massive one with time. We see
no uniqueness in the strength of the UV intensity value required to achieve a
DCBH, since it depends in other factors like the system dynamics in our cases.
