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1999AJ....117.2185P - Astron. J., 117, 2185-2198 (1999/May-0)
Optical and radio polarimetry of the M87 jet at 0".2 resolution.
PERLMAN E.S., BIRETTA J.A., ZHOU F., SPARKS W.B. and MACCHETTO F.D.
Abstract (from CDS):
We do observe significant differences between the radio and optical polarized structures, particularly for bright knots in the inner jet, giving us important insight into the radial structure of the jet. Unlike in the radio, the optical magnetic field position angle becomes perpendicular to the jet at the upstream ends of knots HST-1, D, E, and F. Moreover, the optical polarization appears to decrease markedly at the position of the flux maxima in these knots. In contrast, the magnetic field position angle observed in the radio remains parallel to the jet in most of these regions, and the decreases in radio polarization are smaller. More minor differences are seen in other jet regions. Many of the differences between optical and radio polarimetry results can be explained in terms of a model whereby shocks occur in the jet interior, where higher energy electrons are concentrated and dominate both polarized and unpolarized emissions in the optical, while the radio maps show strong contributions from lower energy electrons in regions with B parallel, near the jet surface.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Active - Galaxies: Individual: Messier Number: M87 - Galaxies: Jets
Nomenclature: Fig.1: [PBZ99] HST-1 N=1. Fig.6: [DAF68] AN (Nos G1-G2) added.
CDS comments: Figs 2, 5: regions HOP and LOP not in SIMBAD.
Simbad objects: 14
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