L. Spinoglio 1, M.A. Malkan 2, P.E. Clegg 3, J. Fischer 4, M. Greenhouse 5, H.A. Smith 6, D. Péquignot 7, Nguyen-Q-Rieu 7, & S.J. Unger 3
1 Istituto di Fisica dello Spazio Interplanetario-CNR, Frascati, Italy
2 Physics and Astronomy Deptartment, UCLA, Los Angeles, USA
3 Queen Mary and Westfield College, London, UK
4 Naval Research Laboratory, Washington, USA
5 NASA Goddard, Greenbelt, USA
6 Harvard-Smithsonian Center for Astrophysics, Cambridge, USA
7 Observatoire de Paris-Meudon, France
The prototypical Seyfert type 2 galaxy NGC 1068 has been observed with
the LWS
(Long Wavelength Spectrometer) on board the ISO (Infrared Space Observatory,
ESA) satellite from 43 to 197
m. All the expected ionic fine structure
lines have been detected. Also present are OH lines in emission at
79 and 119 m.
The ionic line intensities and ratios in NGC 1068 are discussed in the context of photoionization models of the nucleus and photodissociation regions models of the host-galaxy interstellar medium.