EXCITATION OF THE ARCHED FILAMENTS NEAR THE GALACTIC-CENTER

We present measurements of the far-infrared (FIR) fine structure lines [S III] (33 mu m), [Si II] (35 mu m), [O III] (52, 88 mu m), [O I] (6 3 mu m), and [C II] (158 mu m) and the adjacent continua at these wave lengths in a strip crossing the E2 and W1 thermal radio filaments in t he Galactic center ''are.'' The properties of the two filaments are si milar: the line and continuum fluxes peak in the vicinity of the radio ridges, and the contrast of the ridge fluxes relative to the off-ridg e fluxes is greatest for the FIR continuum and doubly ionized lines, l ower for the single-dish radio measurements (Sofue et al. 1986) and sm allest for the low-excitation lines. The near spatial coincidence of t he line and continuum emission maxima with the radio filaments demonst rates that the same excitation source must be responsible for both the line and the continuum emission. The peak FIR luminosity of similar t o 2.5 x 10(5) L(.) per 30'' beam and the association of [O III] intens ity with the filaments pose difficulties for shock and MHD models. Exc itation by a string of stars is also unlikely, but photoionization of molecular cloud edges by a quasi-uniform distribution of stars is the most plausible excitation source proposed. The peak ionized line inten sity is shifted slightly eastward relative to the FIR continuum emissi on. The deduced excitation, as measured by the [O III] to [S III] line flux ratios, also peaks slightly east of the radio ridges. Together, these two measurements suggest a substantial contribution from an ioni zing source to the east. The strengths of the [O I] and [C II] lines a re consistent with their production in photodissociated molecular mate rial adjacent to the photoionized gas, but the FIR luminosity and the [S II] emission appear to originate predominantly in or very near to t he ionized gas.