  Because of its distinctive compositional properties and variability,
low-speed ($\lesssim 450$ km s$^{-1}$) solar wind is widely believed to
originate from coronal streamers, unlike high-speed wind, which comes from
coronal holes. An alternative scenario is that the bulk of the slow wind
(excluding that in the immediate vicinity of the heliospheric current sheet)
originates from rapidly diverging flux tubes rooted inside small coronal holes
or just within the boundaries of large holes. This viewpoint is based largely
on photospheric field extrapolations, which are subject to considerable
uncertainties and do not include dynamical effects, making it difficult to be
certain whether a source is located just inside or outside a hole boundary, or
whether a high-latitude hole will be connected to Earth. To minimize the
dependence on field-line extrapolations, we have searched for cases where
equatorial coronal holes at central meridian are followed by low-speed streams
at Earth. We describe 14 examples from the period 2014--2017, involving Fe XIV
21.1 nm coronal holes located near active regions and having equatorial widths
of $\sim$3$^\circ$--10$^\circ$. The associated in situ wind was characterized
by speeds $v\sim 300$--450 km s$^{-1}$ and by O$^{7+}$/O$^{6+}$ ratios of
$\sim$0.05--0.15, with $v$ showing the usual correlation with proton
temperature. In addition, consistent with other recent studies, this slow wind
had remarkably high Alfv\'enicity, similar to that in high-speed streams. We
conclude that small coronal holes are a major contributor to the slow solar
wind during the maximum and early post-maximum phases of the solar cycle.
