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V.I. Harvey (NASA GSFC), S. Satyapal (STScI), M.L. Luhman (Institute for Defense Analysis), J. Fischer (NRL), P.E. Clegg (Queen Mary & Westfield College, U. London, UK), P. Cox (Institut d'Astronomie Spatiale, France), M.A. Greenhouse (NASA GSFC), S.D. Lord (Caltech, IPAC), M.A. Malkan (UCLA), H.A. Smith (Harvard-Smithsonian, CfA), L. Spinoglio (Istituto di Fisica dello Spazio Interplanetario-CNR, Italy), G.J. Stacey (Cornell U.), S.J. Unger (Queen Mary & Westfield College, U. London, UK)
We present far-infrared spectroscopy of the ultraluminous infrared Seyfert 1 galaxy Mrk 231 obtained with the ISO Long Wavelength Spectrometer. These far-infrared observations reveal a far-infrared spectrum different from classical starburst galaxies and lower luminosity infrared bright galaxies. Like the prototypical ultraluminous infrared galaxy Arp 220, the far-infrared spectrum shows weak or absent far-infrared emission lines and many strong absorption lines. Near-infrared 3.3 micron dust feature observations for this source also reveal a LFIR/L3.3 ratio that is higher than that of M82, the prototypical starburst galaxy. We combine these near-infrared imaging observations with the ISO spectroscopy and discuss the origin of the dominant luminosity source in the galaxy.
The author(s) of this abstract have provided an email address for comments about the abstract: harvey@stars.gsfc.nasa.gov