The following document lists the file abstract/WKEGEL_MEGAMAS.abs
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===================================================================== ==> In this proposal, more time is being requested for WKEGEL.OH_MEGA ===================================================================== OH-megamasers and gigamasers are the most luminous masers known.They are related to IR-luminous galactic nuclei.We intend to observe the OH-lines at 34, 53, 119, and 115 micron in in the megamaser galaxy 3Zw 35 in order to determine the pump process and the internal kinematics of the OH-clouds.-The 115 micron line may turn out to be an iraser-line.- For the megamaser Arp220 the 34 micron line has been observed in the central programme (Skinner et al., Nature submitted.). The line shows an absorption of about 20 per cent. If the line is of similar strength in 3Zw35 it will be securely detected. The large depth of the 34 micron absorption towards Arp220 is somewhat puzzling, since it implies an unexpectedly large covering factor of at least 0.2. This means that the OH-absorbing material may be spread over a much larger area than the region containing the masers. Comparison of both absorption and emission lines towards Arp220 (from the central program), 3Zw35 (from this proposal) and the intrinsically much more powerful Gigamaser sources IRAS 14070+0525 and IRAS 20100-4156 (from our active proposal OH_MEGA) will answer this important question. In addition, we will gain insight into the megamaser pump process. This investigation together with our project OH_MEGA is also a contribution to the general goal to determine the physical state of the ISM in the vicinity of the related galactic nuclei. We intend to observe the megamaser galaxy 3Zw 35 which is substantially brighter than the two gigamasers to be observed in our project OH_MEGA. 3Zw 35 was contained in the spring target list of our project OH_MEGA.