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Are IRIS bombs connected to Ellerman bombs?

Recent observations by the Interface Region Imaging Spectrograph (IRIS) have revealed pockets of hot gas ($\sim$2--8$\times$10$^{4}$ K) potentially resulting from magnetic reconnection in the partially ionized lower solar atmosphere (IRIS bombs; IBs). Using joint observations between IRIS and the Chinese New Vacuum Solar Telescope, we have identified ten IBs. We find that three are unambiguously and three others are possibly connected to Ellerman bombs (EBs), which show intense brightening of the extended H$_α$ wings without leaving an obvious signature in the H$_α$ core. These bombs generally reveal the following distinct properties: (1) The O~{\sc{iv}}~1401.156Å and 1399.774Å lines are absent or very weak; (2) The Mn~{\sc{i}}~2795.640Å line manifests as an absorption feature superimposed on the greatly enhanced Mg~{\sc{ii}}~k line wing; (3) The Mg~{\sc{ii}}~k and h lines show intense brightening in the wings and no dramatic enhancement in the cores; (4) Chromospheric absorption lines such as Ni~{\sc{ii}}~1393.330Å and 1335.203Å are very strong; (5) The 1700Å images obtained with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory reveal intense and compact brightenings. These properties support the formation of these bombs in the photosphere, demonstrating that EBs can be heated much more efficiently than previously thought. We also demonstrate that the Mg~{\sc{ii}}~k and h lines can be used to investigate EBs similarly to H$_α$, which opens a promising new window for EB studies. The remaining four IBs obviously have no connection to EBs and they do not have the properties mentioned above, suggesting a higher formation layer possibly in the chromosphere.