The Relative Contributions of BLR and NLR Gas to the Fe II Pseudo-continuum in the Narrow-lined Type 1 Seyferts, Ark 564 and I Zw 1

Details The Relative Contributions of BLR and NLR Gas to the Fe II Pseudo-continuum in the Narrow-lined Type 1 Seyferts, Ark 564 and I Zw 1 The Relative Contributions of BLR and NLR Gas to the Fe II Pseudo-continuum in the Narrow-lined Type 1 Seyferts, Ark 564 and I Zw 1

Publishing date

Jan 2010

URL

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543302e&link_type=abstract

Journals

American Astronomical Society, AAS Meeting #215, #433.02; Bulletin of the American Astronomical Society, Vol. 42, p.370

Science

Astronomy and Astrophysics

Field

Astrophysics

Type

Scientific paper

Abstract

Because of the rich atomic structure of Fe II, it has the potential of being the single most important atomic probe of physical conditions in astrophysical objects. It has atomic transitions accessible from the far UV through the IR. In this work, we use the spectra of low-redshift, narrow-line Seyfert 1 (NLSy1) galaxies, Ark 564 and I Zw 1, as laboratories for modeling the Fe II emission features in the wavelength range 1200-6700 Å. We utilize data acquired by the Hubble Space Telescope and that obtained by the 2.7 m telescope at McDonald Observatory. We compare these data with predictions from newly computed grids of Fe II emission spectra, representative of both BLR and NLR clouds, using a 830-level model for Fe II. Our comparisons for I Zw 1 and Akn 564 show relatively good agreement, but also reveal Fe II lines where better atomic data are needed. This work further confirms previous results which indicate that spectral modeling must include contributions from both BLR and NLR gas, even in the 2000-3000 Å region, where the Fe II emission from the BLR is most prominent. We further show that the Fe II emission in the 4000-6000 Å region is an important diagnostic for determining the relative contributions of NRL and BLR gas.

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