Physics
Scientific paper
Jul 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1782b&link_type=abstract
IUE Proposal ID #QSGAB
Physics
Scientific paper
We propose to obtain high-quality, broadened (equivalent to trailed) spectra for 10 Seyfert galaxies with the IUE. Only broadened IUE spectra have sufficient signal-to-noise ratios to allow the detailed fitting of line profiles needed to investigate the kinematics, dynamics, and stratification of the emitting regions. These spectra will also allow more accurate measurements of weak spectral features: OI 1304 and He II 1640 are needed to estimate reddening; N IV] 1486, O III] 1663 and N III] 1749 are needed for abundance analyses; the Mg II 2800 absorption line can be used for estimating ,the covering factor of the broad line region (BLR); and Galactic absorption lines of Si II 1260, O I 1304, C II 1335 and Fe II 1608 can yield additional information on the Galactic halo. There are also broad features superposed on the spectra of Seyfert galaxies: the 2200A dust absorption feature, the emission hump at 3200A and the Fe II emission between 2280 and 2650A. Their detection, measurement and quantitative study also require spectra recorded with high signal-to-noise ratios. Xray fluxes are already available for some of the proposed targets, and these data will be combined with our UV continua to estimate the amounts of available ionizing radiation. We also plan to measure the fluxes of the prominent emission lines L-alpha, SI IV 1400, C IV 1550, C III] 1909 and Mg II 2800, to extend our investigation of the L-alpha/H-beta ratio and to provide a homogeneous set of high quality data to allow the evaluation of models for individual objects instead of, as in the past, for an assumed "typical" Seyfert or quasar. Our previous observations have revealed important differences between the emission line properties of Type 1 Seyferts and high redshift quasars. The results from these Seyferts will greatly strengthen our data base for further investigation.
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