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A Multi-Frequency VLBI Total Intensity and Polarization Study of the BL Lacertae Object 0716+714

Published online by Cambridge University Press:  12 April 2016

Y. Y. Kovalev ,
D. C. Gabuzda ,
T. P. Krichbaum ,
W. Alef  and
A. Witzel
Y. Y. Kovalev
Affiliation:
Astro Space Center of the Lebedev Physical Institute, Moscow, Russia
D. C. Gabuzda
Affiliation:
Astro Space Center of the Lebedev Physical Institute, Moscow, Russia
T. P. Krichbaum
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn, Germany
W. Alef
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn, Germany
A. Witzel
Affiliation:
Max-Planck-Institut für Radioastronomie, Bonn, Germany

Abstract

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New polarization-sensitive global VLBI and VLBA images of the BL Lacertae object 0716+714 at 6 cm (1991.4) and 3.6 cm/1.3 cm (1994.2) are presented. The source shows a compact, one-sided core–jet structure in structural position angle ~ 13°. The 3.6 cm total intensity image shows the jet beginning to curve toward the arcsecond-scale structure, which lies in position angle ~ −45°. Comparison with previously published data suggests that the apparent velocity of a 6 cm jet component is > 1.09 ± 0.15c, if the red shift of 0716+714 is z > 0.3. Linear polarization from the VLBI core was detected at all three frequencies; in addition, polarization from the innermost jet component was detected at 1.3 cm. This compact jet polarization appears to be quite high, ~ 50%, and to be aligned with the jet direction, which can be understood if it is a transverse shock. The VLBI core polarization at our earlier epoch was perpendicular to the VLBI jet direction, but had rotated to align with the jet direction by the later epoch, about a year later. This rotation may indicate the imminent birth of a new VLBI component (shock).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 173 - 174
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Eckart, A., et al. 1987. A&AS, 67, 121–146.Google Scholar
Gabuzda, D.C., Wardle, J.F.C., & Roberts, D.H. 1989. ApJ, 336, L59–62.Google Scholar
Gabuzda, D.C., et al. 1994. ApJ, 435, 140–161.Google Scholar
Lobanov, A.P. 1996. Ph.D. Thesis, New Mexico Institute of Mining & Technology.Google Scholar
Wagner, S.J., et al. 1996. AJ, 111, 2187–2211.Google Scholar