Contents of: VI/111/./abstract/GSTACEY_ZZIRBAGN.abs

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.

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