2002/08/27 by S. B. Kraemer, D. M. Crenshaw, T. Yaqoob +7 · 41 citations
Physics and Astronomy · #Absorption (acoustics) #Absorption spectroscopy #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Doubly ionized oxygen #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Hubble space telescope #Ion #Ionization #Line (geometry) #Optics #Photoionization #Physics #Radial velocity #Redshift #Space Telescope Imaging Spectrograph #Spectral line #Spectrograph #Stars #astro-ph
paper · pdf · doi:10.1086/344542
published in The Astrophysical Journal 582(1), 125-132 (IOP Publishing) · 30 pages, three figures (Figure 1 is in color). Accepted for publication in the Astrophysical Journal
arxiv created 2002/08/27 · openalex publication_date 2003/01/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present observations of the UV absorption lines in the luminous Seyfert 1 galaxy Mrk 509, obtained with the medium-resolution (λ/Δλ ≈ 40,000) echelle gratings of the Space Telescope Imaging Spectrograph on the Hubble Space Telescope . The spectra reveal the presence of eight kinematic components of absorption in Lyα, C IV, and N V, at radial velocities of -422, -328, -259, -62, -22, +34, +124, and +210 km s -1 with respect to an emission-line redshift of z = 0.03440, seven of which were detected in an earlier Far Ultraviolet Spectrographic Explorer (FUSE) spectrum. The component at -22 km s -1 also shows absorption by Si IV. The covering factor and velocity width of the Si IV lines were lower than those of the higher ionization lines for this component, which is evidence for two separate absorbers at this velocity. We have calculated photoionization models to match the UV column densities in each of these components. Using the predicted O VI column densities, we were able to match the O VI profiles observed in the FUSE spectrum. Based on our results, none of the UV absorbers can produce the X-ray absorption seen in simultaneous Chandra observations; therefore, there must be more highly ionized gas in the radial velocity ranges covered by the UV kinematic components.