Infrared Polarizations of High-Redshift Radio Galaxies by G. Leyshun

By G. Leyshun

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Centaurus A can hence be explained by the usual scattering model. Other NLRG imaging polarization measurements rapidly followed 3C 234 in the literature. 028) (di Serego Alighieri et al. 132) radio galaxy successfully analysed, 3C 368 (Scarrott, Rolph & Tadhunter 1990; di Serego Alighieri et al. 1989). 766) (di Serego Alighieri et al. 1988). Results published in other papers were as follows: Antonucci & Barvainis (1990) attempted to measure the polarization of several other NLRGs but obtained only large upper limits in most cases (they blame obscuring kpc-scale dust lanes for their failure to detect nuclear light in these cases).

The continuum and emission lines) are polarized in the same direction and with comparable strength, the polarization mechanism is probably one which polarizes light in transit rather than anything intrinsic to the emission of light at the source. [Were we to find polarization angles which systematically changed with wavelength, one interpretation might be a relativistic effect violating the Einstein Equivalence Principle; conversely, the observed constancy of the orientation angle in galaxies at various different redshifts provides further reinforcement for General Relativity, as noted by Cimatti et al.

There is evidence (Kormendy & Richstone 1995; Willott et al. 1998; Serjeant et al. 1998) that the radio and optical luminosity of the active nucleus may be correlated with the mass of the galaxy, and hence its stellar luminosity; but we will assume that the relative contributions of the stellar and nuclear components can be varied freely with a wide dynamic range. We postulate that dust and/or electrons may be present in the outer regions of the galaxy, and that these particles are capable of scattering light into the line of sight to the Earth.

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