The following document lists the file abstract/GSTACEY_ZZIRBAGN.abs
from catalogue VI/111.
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The following is a proposal solicited by the ISO OTAC chairmen via email on September 25, 1997 to provide detailed follow-up work in the area of "Detailed SWS/LWS/PHOT-S spectroscopy of bright starburst galaxies". After many iterations within the program team, we have decided on the following program. (1) Our top priority is that ISO should search for the "confining molecular torus" in NGC 1068 via deep integrations in selected SWS rotational transitions of CO near 40 um, and the vibrational transitions of CO at 4.6 um. NGC 1068 is unusual in that there are several OH lines seen in emission there, suggesting, perhaps, collisional population of the levels in the dense torus. High priority observations are deep integrations in the 34.6 and 163 um OH lines to test this hypothesis. (2) We believe that ISO should perform deep integrations in selected transitions of OH, CO and CH in the archetypical starburst galaxy NGC 253. Past guaranteed and open time proposals indicate that the molecular ISM in NGC 253 is unusually warm and dense, even compared with other starburst galaxies such as M82. The proposed OH and CO observations will confirm these results. (3) In addition, we have concluded that ISO should observe the NeII(12.8 um)/NeIII (15 um) lines in a group of 17 IRAS galaxies selected as starbursters with 60 um fluxes in excess of 20 Jy. These observations constrain the hardness of the ambient radiation fields (age of the starburst) in a manner relatively free from extinction, depletion, temperature and density effects. (4) Finally, we plan to identify the 74.56 um UIR feature we observe from the nucleus of NGC 1068. The rest wavelength of this feature is near that of a UIR 74.22 um line in the planetary nebula, NGC 7027. This line of interest to the entire community, but is particularly so for observers of NGC 1068. For post ISO line identification, it is important to obtain the best value possible for the rest frequency of the line. Since the NGC 1068 line is weaker, and much broader than that in NGC 7027, we propose to measure the line rest frequency by obtaining an LWS Fabry-Perot spectrum on NGC 7027.