  Ellerman bombs (EBs) have been widely studied over the past two decades;
however, only recently have counterparts of these events been observed in the
quiet-Sun. The aim of this article is to further understand small-scale
quiet-Sun Ellerman-like brightenings (QSEBs) through research into their
spectral signatures, including investigating whether the hot signatures
associated with some EBs are also visible co-spatial to any QSEBs. We combine
H$\alpha$ and Ca II $8542$ \AA\ line scans at the solar limb with spectral and
imaging data sampled by the Interface Region Imaging Spectrograph (IRIS).
Twenty one QSEBs were identified with average lifetimes, lengths, and widths
measured to be around $120$ s, $0.63$", and $0.35$", respectively. Three of
these QSEBs displayed clear repetitive flaring through their lifetimes,
comparable to the behaviour of EBs in Active Regions (ARs). Two QSEBs in this
sample occurred co-spatial with increased emission in SDO/AIA $1600$ \AA\ and
IRIS slit-jaw imager $1400$ \AA\ data, however, these intensity increases were
smaller than reported co-spatial to EBs. One QSEB was also sampled by the IRIS
slit during its lifetime, displaying increases in intensity in the Si IV $1393$
\AA\ and Si IV $1403$ \AA\ cores as well as the C II and Mg II line wings,
analogous to IRIS bursts (IBs). Using RADYN simulations, we are unable to
reproduce the observed QSEB H$\alpha$ and Ca II $8542$ \AA\ line profiles
leaving the question of the temperature stratification of QSEBs open. Our
results imply that some QSEBs could be heated to Transition Region
temperatures, suggesting that IB profiles should be observed throughout the
quiet-Sun.
