I ZW 1: A Detailed Look at a Narrow Line Quasar with HST

Details I ZW 1: A Detailed Look at a Narrow Line Quasar with HST I ZW 1: A Detailed Look at a Narrow Line Quasar with HST

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.1802l&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #18.02; Bulletin of the American Astronomical Society, Vol. 26, p.1337

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Scientific paper

The prominent broad emission lines of quasars are typically blended with weaker emission features (e.g. Fe II multiplets). This blending prevents a reliable study of the prominent line profiles, the measurement of weaker lines, and the identification of very weak lines. Blending effects are minimized in the rare class of narrow line quasars (i.e. with FWHM ~ 1000 km s(-1) ). Such objects therefore provide us with the opportunity to make a significantly more accurate study of quasar emission line properties. We report here the results of an HST study of I Zw 1 which is both a narrow line quasar and a very strong Fe II emitter. High S/N spectra (50-120 per resolution element) were recently obtained with the FOS from 1150 Angstroms to 3250 Angstroms. The spectra are very rich in emission lines. There is essentially no wavelength range free of emission features. Preliminary analysis indicates the presence of significant C III(*) lambda 1176 emission, and possibly also Fe III (UV 34), together with a large number of strong Fe II UV multiplets, and other emission features whose likely identification is discussed. The Mg II lambda lambda 2796, 2804 and the Si IV] lambda lambda 1394, 1403 doublets are resolved, which allows constraints on the optical depth in these lines. We also compare the prominent line profiles and find significantly different line peak velocities for some of the lines. We plan to use the I Zw 1 Fe II spectrum as a template for measuring the UV Fe II emission in HST spectra of other quasars with broader lines. This will allow us to study in detail the UV Fe II emission properties of quasars and their relation to the optical Fe II emission. The subtraction of the Fe II emission will allow a more accurate measurement of weak lines, and of strongly blended lines, such as Mg II, C III] lambda 1909 and He II lambda 1640. Support for this work is provided by NASA through Grant No. GO-5486.01-93A from the Space Telescope Science Institute.

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