The following document lists the file abstract/TBANIA_TMB_1.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
At 65 pc, MBM-12 is the nearest known molecular cloud. Located far from sources of FUV radiation, it provides an ideal laboratory to study translucent interstellar gas. MBM-12 has been extensively mapped in (13)CO(1->0) and 14 molecular cores have been identified in the complex. Deduced molecular hydrogen densities range from 10E+3 to 10E+4 cm-3 and excitation temperatures are about 10 K. MBM-12 is thus a translucent cloud: densities and temperatures for the cores are typical of dark clouds, while visual extinctions (Av is about 2 mag) are typical of diffuse clouds. Because of the former property, molecules are able to form in abundance in translucent clouds. However, since Av is low, the ambient radiation field plays an important role in their chemistry. MBM-12 cores have visual extinctions such that H2 -> HI and CII -> C -> CO photochemistry is occuring. For MBM-12 most of these species have either already been studied or are currently being investigated. Missing from, and vital to, any complete characterization of the physical state of the atomic and molecular interstellar medium of the MBM-12 complex is any direct measurement of ionized carbon. ISO LWS observations of [CII] will be used in conjunction with existing [CI], CO, and HI data to study the properties of the 14 atomic/molecular cores in the MBM-12 complex. ISO measurements of [CII] emission from MBM-12 can provide important constraints on models for photodissociation regions (PDRs) in translucent clouds near weak FUV radiation fields.