On the Origin of the UV Continuum Emission from the High Redshift Radio Galaxy 3C256

Details On the Origin of the UV Continuum Emission from the High Redshift Radio Galaxy 3C256 On the Origin of the UV Continuum Emission from the High Redshift Radio Galaxy 3C256

1996-01-19

arxiv.org/abs/astro-ph/9601099v1

Astronomy and Astrophysics

Astrophysics

Uu-encoded compressed gzip tarfile containing 41 page LaTex file, 10 postscript figs, and AASTex style files. To appear in Jul

Scientific paper

10.1086/177409

We report spectropolarimetric observations obtained with the W.M. Keck Telescope of the high redshift z=1.824 aligned radio galaxy 3C256. Our observations confirm that the spatially extended UV continuum emission from this galaxy is polarized (P_V = 10.9% +/- 0.9%) with the electric vector perpendicular to the aligned radio and optical major axes (PA = 48.0 +/- 2.4 degrees). This strongly suggests that a significant fraction of the rest frame UV continuum emission from the galaxy is not starlight, but is instead scattered light from a powerful AGN which is hidden from our direct view. The narrow emission lines, including MgII, are unpolarized. The percentage polarization of the continuum emission and the polarization position angle are roughly constant as a function of wavelength. The present data do not permit us to discriminate between cool electrons and dust as the origin of the scattering. But scattering by hot (T > 10^7 K) electrons cannot be the dominant process, since such a population would overproduce X-ray emission. A large population of cooler T ~ 10^4 K electrons could be responsible for both the line emission and the scattered light, but would require that the dust to gas ratio in the scattering cones is 0.001 times smaller than that in our Galaxy and would imply that a large fraction of the baryonic mass in the galaxy is in the ionized component of its ISM. Dust scattering is more efficient, but would result in detectable extinction of the emission line spectrum unless the dust distribution is more highly clumped than the line emitting gas. Finally, we detect a strong (EW = 12A) broad (FWHM=6500 km/s) absorption line centered at 1477A. We conclude that the most likely explanation is that the absorption is due to a high velocity BAL cloud near the nucleus of 3C256.

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