Other
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...18310508w&link_type=abstract
American Astronomical Society, 183rd AAS Meeting, #105.08; Bulletin of the American Astronomical Society, Vol. 25, p.1447
Other
Scientific paper
We find Broad Absorption Lines (BALs) from high- and low-ionization species (Lyalpha , NV, SiIV, AlIIIlambda1857 , MgII, NaI). Thus IRAS 07598+6508 is a member of the rare class of low-ionization BAL QSOs. Our optical spectropolarimetry shows complex wavelength-dependent percentage polarization, a featureless, power-law polarized flux spectrum (alpha_ nu ~ 0), and wavelength-independent position angle. The emission lines, including FeII, are essentially unpolarized. Unlike the total flux spectrum, the polarized flux spectrum does not show the broad NaI absorption. The Spectral Energy Distribution (SED) is consistent with a standard QSO (or high-ionization BALQSO) spectrum reddened by E(B-V) = 0.12 +/- 0.02 assuming an SMC extinction law, consistent with SEDs of other low-ionization BALQSOs (Sprayberry & Foltz 1992). We use the Boroson & Green (1992) method to deblend the strong optical FeII emission, and find HI equivalent widths among the smallest measured for non-BALQSOs, and Hα /Hβ ~ 6 suggesting a line reddening E(B-V) = 0.45. We explain the polarization with a consistent model in which a typical QSO featureless continuum source and Broad Emission Line Region are partially obscured from direct view by a region (torus) of dusty gas. The direct view of the QSO is highly reddened [E(B-V)~ 0.45] and passes through the BAL region. Continuum emission from a central source emerging at the poles is scattered by dust near the Broad Emission Line Region into our line of sight and does not pass through the BALR. In the observed total light spectrum, the unreddened scattered flux causes us to underestimate the SED reddening, and reduces the HI equivalent widths. A strong 2200 Angstroms ``emission'' feature in the scattered flux spectrum could cancel any 2200 Angstroms feature in the direct spectrum. We suggest that such a scattering model may apply to all low-ionization BALQSOs, and may explain the universally red low-ionization BALQSO SEDs but lack of 2200 Angstroms features.
Hines Dean Carter
Wills Beverley J.
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