density obtained from CHIANTI database .  1399 & 1401 [Å]{} lines are found to be blended with other cool lines in the red wings [@2015arXiv150905011Y]. Thus, to obtain the intensity of the two lines, we fitted the average profiles with two Gaussian functions. Cool lines were fitted with narrow Gaussian function with line widths near to thermal and instrumental broadening. The fitted profiles are also over-plotted in the left panel of Figure \[fig:density\]. We obtained the intensity ratio of $\lambda$1399/$\lambda$1401 line pair, which corresponds to an electron number density of 10$^{11.55}$ cm$^{-3}$.

The two ARTBs and the associated hot loop were also observed with EIS using a raster mode. The EIS raster started at 13:02:20 UT and ended at 13:20:23 UT. Although using EIS raster, one can not study the time evolution of the event, various other useful information such as electron density and flows at coronal temperatures of the event can be obtained. As ARTBs, as well as the hot loop, were changing with the time, each EIS raster steps provide different information of the loop and ARTBs at the different time.

Figure \[fig:eis\] show the intensity maps obtained in 195 [Å]{} (top left) and 284 [Å]{} (top middle) 