Free Access
Issue
Astron. Astrophys. Suppl. Ser.
Volume 128, Number 3, March II 1998
Page(s) 423 - 428
DOI https://doi.org/10.1051/aas:1998153
Published online 15 March 1998
DOI: 10.1051/aas:1998153

A&A Supplement series, Vol. 128, March II 1998, 423-428

Received July 2; accepted August 4, 1997

Observations of the radio emission field around the tex2html_wrap_inline491-ray source 2EG J1834-2138

J.A. Combi tex2html_wrap525tex2html_wrap527 and G.E. Romero tex2html_wrap529

Send offprint request: J.A. Combi, first address

tex2html_wrap531  Instituto Argentino de Radioastronomıa, C.C.5, (1894) Villa Elisa, Bs. As., Argentina
tex2html_wrap533  Theoretical Physics Lab., Department of Physics, University of La Plata, C.C. 67, 1900 La Plata, Argentina
tex2html_wrap535  Instituto Astronômico e Geofısico, Universidade de São Paulo, Av. M. Stefano 4200, CEP 043010-904 São Paulo SP, Brazil

Abstract:

We present results of a study of the radio emission field around the best estimate position of the low-latitude EGRET source 2EG tex2html_wrap_inline497. The identification of this tex2html_wrap_inline491-ray source with the gravitational lensed AGN PKS 1830-211 has been recently proposed by Mattox et al. (1997). Additional support for this identification is provided here. Contamination produced by the diffuse disk emission has been removed from new radio images of the surrounding region of 2EG tex2html_wrap_inline497 allowing a determination of the fine radio structure. Several previously unnoticed supernova remnants have been found within a few degrees from the tex2html_wrap_inline491-ray source. However, the only strong radio source within the 95% source location confidence contour of 2EG tex2html_wrap_inline497 is PKS 1830-211. In addition, both spectrum and variability analysis of the EGRET data support the identification of both sources.

keywords: gamma rays: observations -- radio continuum: galaxies -- galaxies: active -- galaxies: quasars: PKS 1830-211

SIMBAD Objects

Copyright by the European Southern Observatory (ESO)

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