By G. Leyshun
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Extra resources for Infrared Polarizations of High-Redshift Radio Galaxies
Angel & Stockman (1980, §IV) wrote before the Unification Hypothesis had be- come popular, and reviewed numerous mechanisms which might account for the low visible/infrared polarizations observed in many Seyferts. Originally, Seyfert polarizations (of order 1%) were attributed to the visible high-frequency tail of synchrotron radiation. Multicolour and spectroscopic studies of Seyfert polarization, however, showed that in most Seyferts, both the core continuum light and the emission lines were polarised, and the polarization (corrected for the stellar contribution) was stronger in the blue than in the red, but with little rotation of position angle.
1998, 10%) or even dominant (Cimatti et al. 1997, 3C 368). 37 Neither nebular emission nor stellar blackbody emission is intrinsically polarized, so we expect these sources to contribute only to the unpolarized spectrum, while the nuclear component may be partially polarized. This nuclear contribution may itself consist of several features with different polarization strengths, indicative of the various mechanisms at work within the nucleus. The presence of an unpolarized stellar (and nebular) component together with a substantially polarized nuclear component is indicative of the fact that the polarizing mechanism is contained inside the host galaxy (otherwise the stellar emission would also become polarized) but does not consist of many independent cells of polarized emission (Antonucci 1984) which, if independently oriented, would tend to cancel out one another’s polarization and produce a low overall figure.
2 3C 226 FSC 10214+4724 MRC 2025-218 B/N N N ? B B B N N N ? 3 θ ± σθ (◦ ) 152 ± 5 10 ± 8 n/a 119 ± 22 66 ± 2 180 ± 16 169 ± 7 84 ± 13 75 ± 3 93 ± 8 δo−r 58 93 n/a 5 42 n/a 108 120 145 63 Ref S+ S+ CA S+ S+ S+ A+ A+ L+ C+ Key: Source: Common name of object; B/N: BLRG / NLRG classification; z: redshift; Band: waveband of observation, Johnson-Cousins or Gunn designation [Ø denotes no filter, effective passband 400–1000 nm]; λr : central wavelength of observed frame transformed into source’s rest-frame; P ± σP : percentage polarization (debiased) with 1σ error [e indicates corrected for suspected emis- sion line contamination; ℓ indicates largest of cited nucleocentric apertures taken; w indicates whole galaxy, not nucleus]; θ ± σθ : Electric vector orientation E of N (◦ ); δo−r : Orientation offset of optical polarization minus radio position angle (◦ ); Ref: Data source, as follows: A+ (di Serego Alighieri, Cimatti & Fosbury 1994); C+ (Cimatti et al.