Don't necessarily expect them to be up to date. Note that the low noise of the new array means that background noise-limited conditions are obtained at JHK with exposure times of only a few seconds. For each wavelength, two tables are given.
Spectral profile is roughly rectangular.
For extended objects the sensitivities will be 0.4 magnitudes less. The line fluxes are for unresolved lines. With these low order gratings the slit width is 3 arcseconds and each row on the array is 3 arcseconds in the spatial direction. The total slit length is 90 arcseconds. At these resolutions and integration times, it can be assumed that the observations are background noise limited.