  Ellerman Bomb-like brightenings of the hydrogen Balmer line wings in the
quiet Sun (QSEBs) are a signature of the fundamental process of magnetic
reconnection at the smallest observable scale in the solar lower atmosphere. We
analyze high spatial resolution observations (0.1 arcsec) obtained with the
Swedish 1-m Solar Telescope to explore signatures of QSEBs in the H$\beta$
line. We find that QSEBs are ubiquitous and uniformly distributed throughout
the quiet Sun, predominantly occurring in intergranular lanes. We find up to
120 QSEBs in the FOV for a single moment in time; this is more than an order of
magnitude higher than the number of QSEBs found in earlier H$\alpha$
observations. This suggests that about half a million QSEBs could be present in
the lower solar atmosphere at any given time. The QSEB brightening found in the
H$\beta$ line wings also persist in the line core with a temporal delay and
spatial offset towards the nearest solar limb. Our results suggest that QSEBs
emanate through magnetic reconnection along vertically extended current sheets
in the solar lower atmosphere. The apparent omnipresence of small-scale
magnetic reconnection may play an important role in the energy balance of the
solar chromosphere.
