[C-II] 158 MICRON AND [O-I] 63 MICRON OBSERVATIONS OF THE GALACTIC-CENTER REGION

Using the balloon-borne infrared telescope (BIRT) incorporated with a liquid-helium-cooled double-channel Fabry-Perot spectrometer, intensit ies and velocity profiles of [C II] 158 mum and [O I]63 mum fine-struc ture lines have been observed in the Galactic center region within \l\ less-than-or-equal-to 0.7-degrees. Intense [C II] line emission has b een detected ubiquitously in almost all of the observed points. The di stribution of the [C II] intensity shows a central peak at Sgr A West together with two prominent peaks at DELTA1 = +/- 0.6-degrees, which c orrespond to Sgr B1 (not Sgr B2) and Sgr C, respectively. The intensit y distribution resembles but is not identical to, that of far-infrared emission. The velocity profiles of the [C II] line are resolved and c an be deconvolved into multiple components, many of which can be trace d to the features observed by molecular lines. The [O I]63 mum line ha s been detected at Sgr A West and at some other points. The [O I]63 mu m/[C II] 158 mum ratios are always less than 3 in the beam of 3'.7 The se observed results can be explained as the emission generated in phot odissociation regions formed in the molecular clouds complexes illumin ated by intense UV radiation field in the Galactic center regions. How ever, contribution from ELD region is possibly present and cannot be r uled out.