  We present a comprehensive set of spectral data from two quiescent solar
prominences observed in parallel from space and ground: with the VTT,
simultaneous two-dimensional imaging of H-beta 4862 and Ca II 8542 yields a
constant ratio, indicating small spatial pressure variations over the
prominences. With the Gregory, simultaneous spectra of Ca II 8542 and He I
10830 were taken, their widths yielding 8000< T_kin< 9000 K and v_nth<8 km/s.
The intensity ratio of the helium triplet components gives an optical thickness
of tau < 1.0 for the fainter and tau < 2.0 for the brighter prominence. The
tau_0 values allow to deduce the source function for the central line
intensities and thus the relative population of the helium 3S and 3P levels
with a mean excitation temperature T_ex = 3750 K.
  With SUMER, we sequentially observed 6 spectral windows containing higher
Lyman lines, 'cool' emission lines from neutrals and singly charged atoms, as
well as 'hot' emission lines from ions like O IV, O V, N V, S V and S VI. The
EUV lines show pronounced maxima in the main prominence body as well as
'side-locations' where the 'hot' lines are enhanced with respect to the 'cool'
lines. The line radiance of 'hot' lines blue-wards of the Lyman series limit
(lambda<912 A) appear reduced in the main prominence body. This absorption is
also visible in TRACE images of Fe IX/X 171 as fine dark structure which covers
only parts of the main ('cool') prominence body.
  The Lyman lines show a smooth decrease of line widths and radiance with
increasing upper level k = 5 through 19. For k= 5 through 8 the level
population follows a Boltzmann distribution with T_ex >6 *10^4 K; higher levels
k > 8 appear more and more overpopulated. The larger widths of the Lyman lines
require high non-thermal broadening close to that of 'hot' EUV lines. In
contrast, the He II emission is more related to the 'cool' lines.
