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| Paper: |
ISOPHOT FIR and SEST molecular line mapping of Chameleon I |
| Volume: |
132, Star Formation with the Infrared Space Observatory (ISO) |
| Page: |
147 |
| Authors: |
Haikala, L. K.; Mattila, K.; Lehtinen, K.; Lemke, D. |
| Abstract: |
The centre and the southern part of the low mass star forming cloud Chameleon I has been mapped using ISOPHOT C_200, C_135, C_100 and C_70 filter bands and in C18O J=1 -> 0 using the 15m Swedish-ESO-Submillimeter-Telescope. The large scale structure of the cloud in FIR and C18O is discussed in this paper. Due to the proximity of the region ISOPHOT provides a spatial resolution of 0.06 and 0.04 pc at C_200/C_135 and C_100/C_70 respectively. This allows a detailed study of star forming and non star forming cores in the region. The mapped part of the cloud is fragmented into five cores of which two are well separated of the known star formation sites in the cloud. In locations separate from IR point sources the dust emission at C_200 and C_135 correlates linearily with each other and with C18O emission. The distribution of the emission in the C_100 band is similar to that observed at longer wavelengths near the star-forming regions of the cloud but is weak in the southern part of the mapped region. The dust temperatures derived from the 161/205 microns ratios in the cloud cores range from 16 K (assuming a λ^{-2} dust emissivity) in the proximity of the star forming sites to 13.5 K in quiescent cores. |
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