  Advancements in instrumentation have revealed a multitude of small-scale EUV
events in the solar atmosphere. Our aim is to employ high-resolution
magnetograms to gain a detailed understanding of the magnetic origin of such
phenomena. We have used coordinated observations from SST, IRIS, and SDO to
analyze an ephemeral magnetic flux emergence episode and the following chain of
small-scale energetic events. These unique observations clearly link these
phenomena together. The high-resolution (0."057/pixel) magnetograms obtained
with SST/CRISP allows us to reliably measure the magnetic field at the
photosphere and detect the emerging bipole that causes the subsequent eruptive
atmospheric events. Notably, this small-scale emergence episode remains
indiscernible in the lower resolution SDO/HMI magnetograms (0."5/pixel). We
report the appearance of a dark bubble in Ca II K related to the emerging
bipole, a sign of the canonical expanding magnetic dome predicted in flux
emergence simulations. Evidences of reconnection are also found: first through
an Ellerman bomb, and later by the launch of a surge next to a UV burst. The UV
burst exhibits a weak EUV counterpart in the coronal SDO/AIA channels. By
calculating DEM, its plasma is shown to reach a temperature beyond 1 MK and
have densities between the upper chromosphere and transition region. Our study
showcases the importance of high-resolution magnetograms to unveil the
mechanisms triggering phenomena such as EBs, UV bursts, and surges. This could
hold implications for small-scale events akin to those recently reported in EUV
using Solar Orbiter. The finding of temperatures beyond 1 MK in the UV burst
plasma strongly suggests that we are examining analogous features. Therefore,
we signal caution regarding drawing conclusions from full-disk magnetograms
that lack the necessary resolution to reveal their true magnetic origin.
