  We explore the implications of the observed low spins aligned with the
orbital axis in Advanced~LIGO~O1 run on binary black hole (BBH)~merger
scenarios in which the merging BBHs have evolved from field binaries. The
coalescence time determines the initial orbital separation of BBHs. This, in
turn, determines whether the stars are synchronized before collapse and hence
determines their projected spins. Short coalescence times imply synchronization
and large spins. Among known stellar objects, Wolf-Rayet~(WR) stars seem the
only progenitors consistent with the low aligned spins observed in LIGO's~O1
provided that the orbital axis maintains its direction during the collapse. We
calculate the spin distribution of BBH mergers in the local Universe and its
redshift evolution for WR progenitors. Assuming that the BBH formation rate
peaks around a redshift of $\sim 2\,$--$\,3$, we show that BBH mergers in the
local Universe are dominated by low spin events. The high spin population
starts to dominate at a redshift of $\sim0.5\,$--$\,1.5$. WR stars are also
progenitors of long Gamma-Ray~Bursts~(LGRBs) that take place at a comparable
rate to BBH mergers. We discuss the possible connection between the two
phenomena. Additionally, we show that hypothetical Population~III star
progenitors are also possible. Although WR and Population~III progenitors are
consistent with the current data, both models predict a non-vanishing fraction
of high aligned spin BBH mergers. If those are not detected within the coming
LIGO/Virgo runs, it will be unlikely that the observed BBHs formed via field
binaries.
