Multiline CO observations of MBM 32

We present a detailed study of the high latitude cloud MBM 32. Observations were made in the J = (1 - 0), (2 - 1), and (3 - 2) transitions of (CO)-C-1 2 and in (CO)-C-13(1 - 0) and (2 - 1). These data were complemented by 21 c m HI data and by IRAS 60 and 100 mu m data. Our data show that MBM 32 consists of a main cloud component at V-lsr > 2 k m s(-1) (mass about 16.9 M.), and a smaller component at V-lsr < 0 km s(-1) (4.1 M.), in ad dition to some emission in between those two velocities (< 0.5 M.). We study the gas distribution and the CO line ratios within MBM 32, the lat ter also along a cut through both cloud components. We find that the ratios of different rotational transitions are constant within each cloud part. O nly the ratio (CO)-C-12(1 - 0)/(CO)-C-13(1 - 0) is lower in the cloud cente r. This suggests equal excitation conditions through MBM32 and line tempera tures determined through clump filling factors. All CO components show associated HI emission, but small velocity differenc es of typically 1 km s(-1) exist between the HI and CO gas. The mass of ass ociated HI gas is similar to the molecular mass for all components. There is a good correlation between FIR, CO, and HI emission. The dust mass is about 0.073 M., and the ratio of gas and dust mass (280) is lower than found from similar (IRAS) data for denser clouds, suggesting that the amoun t of dust colder than 20 K is relatively small. We subdivide the CO data cubes in Gaussian shaped clumps; 40 - 50% of the C O emission can be assigned to the larger clumps. The remaining emission com es from either more extended clumps or from overlapping unresolved clumps.