Intrinsic Ultraviolet Absorption in the Seyfert 1 Galaxy NGC 3783

Details Intrinsic Ultraviolet Absorption in the Seyfert 1 Galaxy NGC 3783 Intrinsic Ultraviolet Absorption in the Seyfert 1 Galaxy NGC 3783

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19710911k&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #109.11; Bulletin of the American Astronomical Society, Vol. 32, p.1588

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Scientific paper

We present ultraviolet spectra of the z=0.010 Seyfert 1 galaxy NGC 3783. For wavelengths extending from 920-1185 Å we have obtained high spectral resolution, ~ 20 km s-1, observations with the Far Ultraviolet Spectroscopic Explorer (FUSE). These data are complemented by longer wavelength, 1145-3145 Å, lower resolution Space Telescope Imaging Spectrograph (STIS) spectra. The FUSE and STIS observations were made within three months of one another. Our FUSE spectra exhibit both strong O VI emission and strong associated absorption lines of O VI λ λ 1032, 1038 as well as Lyman β emission and associated absorption. Lyman α , N Vλ 1240, Si IV λ 1398, C IV λ 1549, C III] λ 1909 and Mg II λ 2800 emission are detected in the low resolution STIS spectra. NGC 3783 is one of several Seyfert 1 galaxies which exhibit deep O VII and O VIII absorption edges in the X-ray and intrinsic absorption in the ultraviolet. FUSE observations of O VI are important for characterizing the ionization state of this warm X-ray absorbing gas and providing a link between the lower ionization species, such as N V and C IV, seen in the ultraviolet and the higher ionization X-ray warm absorber. We will discuss the intrinsic absorption present in both our FUSE and STIS spectra. These kinematic components will be compared with the components present in the Chandra X-ray observations (Kaspi et al. 2000, ApJ) and the earlier HST/GHRS/FOS spectra (Crenshaw et al. 1999, ApJ). The FUSE observations were obtained for the Guaranteed Time Team. Financial support for these observations was provided by contract NAS5-32985.

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