Chandra X-ray Spectroscopy of NGC 4151

Details Chandra X-ray Spectroscopy of NGC 4151 Chandra X-ray Spectroscopy of NGC 4151

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.1109o&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #11.09; Bulletin of the American Astronomical Society, Vol. 34, p.1110

Astronomy and Astrophysics

Astronomy

Scientific paper

NGC 4151 (z=0.00332) is a bright, nearby Seyfert 1.5 active galaxy. It has an extended, photoionized optical and X-ray narrow-line region. We previously explained the strong resonance lines in the Chandra HETGS spectrum by invoking a hot, collisionally ionized intercloud medium (Ogle et al. 2000). We show in this poster that photoexcitation (resonance scattering) is a more consistent explanation. We have also made new LETGS observations which extend this result to longer wavelengths. We show a detailed photoionization model fit of all H-like and He-like K-shell and Fe L-shell emission lines and recombination continua. We also explore the strong continuum spectral variability to see if it can be explained by a variable absorber. This research is based on data taken with the Chandra X-ray Observatory and funded by Smithsonian grant G02-3146X.

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