SIMBAD references

We report here the results of [CII]158 and [OI]63µm fine-structure line observations along two cuts across a molecular clump of L1457 (MBM12) carried out with ISO-LWS. [CII] emission was detected at all positions observed. It can be assigned to the cooling of the diffuse atomic interstellar medium. We observed excess [CII] emission from the dense clumpy molecular component. It is likely to originate from molecular gas that is irradiated by an interstellar FUV-radiation field of order χ=(1-2)χ₀. Using PDR models for a spherical symmetry we find the molecular gas of L1457 consists of clumps with a density n_H∼10⁵cm^–3. Their masses range between 10^–4 and 10^–3M_☉ consistent with the clump distribution derived from high resolution CO observations. [OI]63µm emission was not detected toward L1457.