Astronomy and Astrophysics, volume 514, A13-13 (2010/5-1)
Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI.
OKADA Y., KAWADA M., MURAKAMI N., OOTSUBO T., TAKAHASHI H., YASUDA A., ISHIHARA D., KANEDA H., KATAZA H., NAKAGAWA T. and ONAKA T.
Abstract (from CDS):
We investigate the structure of the interstellar medium (ISM) and identify the location of possible embedded excitation sources from far-infrared (FIR) line and mid-infrared continuum emission maps. We carried out imaging spectroscopic observations of four giant Galactic star-forming regions with the Fourier transform spectrometer (FTS) onboard AKARI. We obtained [OIII] 88µm and [CII] 158µm line intensity maps of all the regions: G3.270-0.101, G333.6-0.2, NGC 3603, and M 17. For G3.270-0.101, we obtained high-spatial-resolution [OIII] 88µm line-emission maps and a FIR continuum map for the first time, which imply that [OIII] 88µm emission identifies the excitation sources more clearly than the radio continuum emission. In G333.6-0.2, we found a local [OIII] 88µm emission peak, which is indicative of an excitation source. This is supported by the 18µm continuum emission, which is considered to trace the hot dust distribution. For all regions, the [CII] 158µm emission is distributed widely as suggested by previous observations of star-forming regions. We conclude that [OIII] 88µm emission traces the excitation sources more accurately than the radio continuum emission, especially where there is a high density and/or column density gradient. The FIR spectroscopy provides a promising means of understanding the nature of star-forming regions.
infrared: ISM - HII regions - ISM: lines and bands
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