  Solar macrospicules are beam-like cool plasma ejections of size in-between
spicules and coronal jets, which can elucidate potential connections between
plasma jetting activity at different scales. With high-resolution observations
from the {\em New Vacuum Solar Telescope} and Solar Dynamic Observatory, we
investigate the origin of five groups of recurrent active-region macrospicules.
Before the launch of each macrospicule, we detect a compact bright patch (BP)
at its base where a newly emerging dipole contacts and cancel with the
pre-existing ambient field. The spectral diagnosis from the {\em Interface
Region Imaging Spectrograph} at one of BPs reveals signatures of reconnection
at the lower atmosphere. Multiwavelength imaging of these BPs show that they
mainly occur at the rising phase of the flux emergence and slowly ascend from
the lower to the upper chromosphere. Remarkable macrospicules occur and fade
out once the BPs appear and decay from the AIA 304 A images, respectively. We
suggest that these macrospicules and related BPs form in a common reconnection
process, in which the increasing reconnection height between the emerging
dipole and the ambient field results in the observed variations from BPs to
macrospicules. Interestingly, most macrospicules show similar characteristics
to larger-scale coronal jets and/or smaller-scale spicules, i.e., the rotating
motions, the presence of minifilaments and BPs before the eruptions, and
magnetic flux emergence and cancellation. We conclude that the formation
mechanism of macrospicules should be the same as spicules and coronal jets,
i.e., solar jetting phenomena at different scales share the same physical
mechanism in association with magnetic reconnection.
