Impact of baryonic streaming velocities on the formation of supermassive
  black holes via direct collapse
  Baryonic streaming motions produced prior to the epoch of recombination
became supersonic during the cosmic dark ages. Various studies suggest that
such streaming velocities change the halo statistics and also influence the
formation of Population III stars. In this study, we aim to explore the impact
of streaming velocities on the formation of supermassive black holes at $z>10$
via the direct collapse scenario. To accomplish this goal, we perform
cosmological large eddy simulations for two halos of a few times $\rm 10^{7}
M_{\odot}$ with initial streaming velocities of 3, 6 and 9 $\rm km/s$. These
massive primordial halos illuminated by the strong Lyman Werner flux are the
potential cradles for the formation of direct collapse seed black holes. To
study the evolution for longer times, we employ sink particles and track the
accretion for 10,000 years. Our findings show that higher streaming velocities
increase the circular velocities from about 14 $\rm km/s$ to 16 $\rm km/s$.
They also delay the collapse of halos for a few million years, but do not have
any significant impact on the halo properties such as turbulent energy, radial
velocity, density and accretion rates. Sink particles of about $\rm \sim 10^5
M_{\odot}$ are formed at the end of our simulations and no clear distribution
of sink masses is observed in the presence of streaming motions. It is further
found that the impact of streaming velocities is less severe in massive halos
compared to the minihalos as reported in the previous studies.
