We present the results of far-infrared spectroscopic observations of the Large Magellanic Cloud (LMC) with FIS-FTS. We covered a large area across the LMC, including 30 Doradus (30 Dor) and N44 star-forming regions, by 191 pointings in total. As a result, we detect the [OIII] and [CII] line emission as well as far-infrared dust continuum emission throughout the LMC. We find that the [OIII] emission is widely distributed around 30 Dor. The observed size of the distribution is too large to be explained by massive stars in 30 Dor, which are assumed to be enshrouded by clouds with the constant gas density estimated from the [OIII] line intensities. Therefore the surrounding structure is likely to be highly clumpy. We also find a global correlation between the [OIII] and the far-infrared continuum emission, suggesting that the gas and dust are well mixed in the highly-ionized region where the dust survives in clumpy dense clouds shielded from energetic photons. Furthermore we find that the ratios of [CII]/CO are as high as 110,000 in 30 Dor, and 45,000 even on average, while they are typically 6,000 for star-forming regions in our Galaxy. The unusually high [CII]/CO is also consistent with the picture of clumpy small dense clouds.

ABSTRACT
1. INTRODUCTION
2. OBSERVATION
3. RESULTS
4. DISCUSSION
REFERENCES

• A. TAKAHASHI(Nagoya University)
• A. YASUDA(Nagoya University)
• H. KANEDA(Nagoya University)
• M. KAWADA(Nagoya University)
• Y. KIRIYAMA(Nagoya University)
• A. MOURI(Nagoya University)
• T. MORI(Nagoya University)
• Y. OKADA(I. Physikalisches Institut, Universitat zu Koln)
• H. TAKAHASHI(Institute of Astronomy, Graduate School of science, University of Tokyo)