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We investigate the structure of the interstellar medium (ISM) and identifythe location of possible embedded excitation sources from far-infrared (FIR)line and mid-infrared continuum emission maps. We carried out imagingspectroscopic observations of four giant Galactic star-forming regions with theFourier Transform Spectrometer (FTS) onboard AKARI. We obtained [OIII] 88micron and [CII] 158 micron line intensity maps of all the regions:G3.270-0.101, G333.6-0.2, NGC3603, and M17. For G3.270-0.101, we obtainedhigh-spatial-resolution [OIII] 88 micron line-emission maps and a FIR continuummap for the first time, which imply that [OIII] 88 micron emission identifiesthe excitation sources more clearly than the radio continuum emission. InG333.6-0.2, we found a local [OIII] 88 micron emission peak, which isindicative of an excitation source. This is supported by the 18 microncontinuum emission, which is considered to trace the hot dust distribution. Forall regions, the [CII] 158 micron emission is distributed widely as suggestedby previous observations of star-forming regions. We conclude that [OIII] 88micron emission traces the excitation sources more accurately than the radiocontinuum emission, especially where there is a high density and/or columndensity gradient. The FIR spectroscopy provides a promising means ofunderstanding the nature of star-forming regions.

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI