Synchrotron radiation from the jet of 3C 273. II - The radio structure and polarization

Details Synchrotron radiation from the jet of 3C 273. II - The radio structure and polarization Synchrotron radiation from the jet of 3C 273. II - The radio structure and polarization

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...267..347c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 267, no. 2, p. 347-362.

Astronomy and Astrophysics

Astronomy

51

Polarized Electromagnetic Radiation, Radio Jets (Astronomy), Radio Spectra, Synchrotron Radiation, Astronomical Maps, Faraday Effect, Linear Polarization

Scientific paper

We have collected radio data for the jet of 3C 273 from 151 to 14435 MHz at resolutions of about 1 arcsec. We confirm the major features from earlier work, namely, that a flat-spectrum core coincides with the optical QSO, and that the radio image extends 23 arcsec from the core in p.a. 222 deg. There is no counterjet, to a limit of 10,000:1 in flux density. The intensity rises continuously with radial distance from the core from r = 10 to 21.5 arcsec, leading to a bright head, with three subcomponents, that covers the end of the optical image. For most of its length the half power width of the jet is 1.0 arcsec. The ridgeline of the jet oscillates about the center line by up to 0.5 arcsec. On its southern side the jet is accompanied by an extended steep-spectrum lobe; there is no corresponding feature on the northern side of the jet. The average spectral index of the radio emission is 0.78, and shows rather little variation with position, except that the index between 2 and 6 cm becomes significantly steeper as the head is approached. The linear polarization varies between 10 and 20 percent along the jet, but is essentially the same at 6, 18, and 73 cm. The B-vector follows the (curving) ridgeline out to r = 20.5 arcsec, where it suddenly becomes perpendicular to the axis. It is suggested that the cluster in which 3C 273 lies has an ambient density of no more than 0.0003/cu cm, in contrast to the Virgo cluster containing M 87, where much higher rotation measures are encountered.

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