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D. Casebeer, K. Leighly (The University of Oklahoma)
It has long been thought that the shape of the ionizing continuum of an Active Galactic Nucleus (AGN) should have an effect on its emission-line ratios. This is important since the line ratios then potentially provide a way to infer the shape of the continuum in the unobservable EUV wavelength range. It was suspected that the ratio of \ion{O}{6} to Ly\alpha should be especially sensitive to this shape: \ion{O}{6} should be strong when the continuum in the optical--UV--soft X-ray range is hard. Among the recently presented observational evidence lending support for this idea are the HUT spectra showing that some Seyfert 1 galaxies with strong soft X-ray excesses have also strong \ion{O}{6} lines.
The Seyfert 1 galaxy RE~1034+39 has a remarkable spectral energy distribution. Its optical and UV spectra are very red, but there is no evidence for extinction. Its soft X-rays are very strong, with a steep spectrum. Such a hard ionizing continuum should produce a huge \ion{O}{6} line.
We present the results of a program of coordinated FUSE, EUVE, ASCA and optical observations from the MDM 1.3 meter telescope, as well as a reanalysis of HST FOS observations of RE 1034+39. Our preliminary results from the FUSE observation shows a prominent composite OVI profile including a narrow component with FWHM ~600 km/s. We also detect \ion{C}{3} \lambda 977 and possibly Ly\beta \lambda 1026 as well.
We will present the results of the spectral analysis, as well as photoionization models using the spectral synthesis code Cloudy designed to explicitly test the influence of the unusual spectral energy distribution from RE 1034+39 on the emission line ratios.
This work is supported by NASA grants NAG5-10048 (FUSE) and NAG5-10171 (LTSA).