  Ellerman bombs (EBs) are a kind of solar activities that is suggested to
occur in the lower atmosphere. Recent observations using the Interface Region
Imaging Spectrograph (IRIS) show connections of EBs and IRIS bombs (IBs),
implying that EBs might be heated to a much higher temperature ($8\times10^{4}$
K) than previous results. Here we perform a spectral analysis of the EBs
simultaneously observed by the Fast Imaging Solar Spectrograph (FISS) and IRIS.
The observational results show clear evidence of heating in the lower
atmosphere, indicated by the wing enhancement in H$\alpha$, Ca II 8542 \r{A}
and Mg II triplet lines, and also by brightenings in the images of 1700 \r{A}
and 2832 \r{A} ultraviolet continuum channels. Additionally, the Mg II triplet
line intensity is correlated with that of H$\alpha$ when the EB occurs,
indicating the possibility to use the triplet as an alternative way to identify
EBs. However, we do not find any signal in IRIS hotter lines (C II and Si IV).
For further analysis, we employ a two-cloud model to fit the two chromospheric
lines (H$\alpha$ and Ca II 8542 \r{A}) simultaneously, and obtain a temperature
enhancement of 2300 K for a strong EB. This temperature is among the highest of
previous modeling results while still insufficient to produce IB signatures at
ultraviolet wavelengths.
