2003NewA....8..795M

Towards the high-latitude cloud MBM 40, we identify 3 dense molecular cores of M∼0.2-0.5 M, and sizes of ∼0.2 pc in diameter embedded in the HI cloud of ∼8 M which is observed to be extended along the northeast-southwest direction. The molecular cloud is located almost perpendicularly to the HI emission. We confirm the previous result of Magnani et al. that MBM 40 is not a site for new star formations. We found a very poor correlation between the HI and the IRAS 100 mum emissions, but the CO (1-0) and 100 mum emissions show a better correlation of WCO/I100=1±0.2 K km s-1 (MJy sr-1)-1. This ratio is larger by a factor of ≥5 than in dense dark clouds, which may indicate that the CO is less depleted in MBM 40 than in dense dark clouds.