STIS Echelle Observations of NGC 4151. I. Measurements of the Intrinsic Absorption

Details STIS Echelle Observations of NGC 4151. I. Measurements of the Intrinsic Absorption STIS Echelle Observations of NGC 4151. I. Measurements of the Intrinsic Absorption

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19711009c&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #110.09; Bulletin of the American Astronomical Society, Vol. 32, p.1590

Astronomy and Astrophysics

Astronomy

Scientific paper

We present echelle observations of the intrinsic UV absorption lines in the Seyfert galaxy NGC 4151, which were obtained with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST) on 1999 July 19. The UV continuum flux at 1450 Å decreased by a factor of about four over the previous two years and there was a corresponding dramatic increase in the column densities of the low-ionization absorption lines (e.g., Si II, Fe II, and Al II), presumably as a result of a decrease in the ionizing continuum. In addition to the absorption lines seen in previous low states, we identify a large number of Fe II absorption lines that arise from metastable levels as high as 4.1 eV above the ground state, indicating high densities (> 106 cm-3). We find that the transient absorption feature in the blue wing of the broad C IV emission, seen in a Goddard High Resolution Spectrograph (GHRS) spectrum and thought to be a high-velocity C IV component, is actually a S II fine-structure absorption line. We also demonstrate that the ``satellite'' emission lines of C IV found in International Ultraviolet Explorer (IUE) spectra are actually regions of unabsorbed continuum plus broad emission that become prominent when the UV continuum of NGC 4151 is in a low state. Finally, we show that there is a significant contribution of scattered light that is intrinsic to NGC 4151, and the broad kinematic component of absorption at -490 km s-1 (relative to the nucleus) is heavily saturated in most lines.

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